Home

here - PANIC

1. ccccccccnnnnonononononcnononnccnnnnnnnnnnnos 105 Figure 3 3 2 14 Rotating field stop in two positions with the housing upper part hidden left field stop for 0 25 arcsec pixel in use right field stop for 0 45 arcsec pixel in use 106 Figure 3 3 2 15 Both optics assemblies have been replaced by point masses the rest of the CIS OSEE TS moho WI nr mb taste tM en 107 Figure 3 3 2 16 Displacement of cold bench with the telescope pointing to zenith gravity Eeer NIENTE K 108 Figure 3 3 2 17 Cryostat displacement with the telescope pointing to zenith gravity vector in z re E E T m Um 108 Figure 3 3 2 18 Displacement of cold bench with the telescope pointing to horizon gravity a o AAA 109 Figure 3 3 2 19 Cryostat displacement with the telescope pointing to horizon gravity vector in sa ME 109 Figure 3 3 2 20 Displacement of cold bench and optics with the telescope pointing to horizon gravity vector in y direction pineda ev 110 Figure 3 3 2 21 Displacement of cold bench and optics with the telescope pointing to horizon gravity vector in 2 dtecton rne ne e nnnnnennne nennen eene eee 111 Figure 3 3 2 22 Displacement of cold bench and optics with the telescope pointing to zenith gravity vector mz direc la 111 Figure 3 3 2 23 Simulation of entrance window deformation due to a differential pressure of 1 bz T H 112 Figure 3 3 2 24 Deformation
2. oooccccccnnnnnnnnononnnononnnoninonos 129 gt IVIDUOTEODHIEOLE ee 130 D WO MEE CC RU Em 130 JAL Principle ol motion contol Sy Mercator ee Qu ato 130 34233 Motion controller board MOGC DIN Lasa 131 SALA Stepper Motor Driver Ee EE 131 SU INT MO 132 e MR Uo dm m m ee 132 202 9 TPaSIHOB OD EE Me Mares atando 132 L Suae RETI E o m D RT 132 A ase ae tae cre O M 133 3 4 2 5 3 Resolver Module RESMOD sisi siiis 133 3420 EE 134 OE T MME TSP uu EE S nu A act tay aoeete ee AN E EE 134 3 4 2 6 2 Optics and field Stops wheel EE 134 Ser O a MEOS CH RU UR AMD MONDE RM ENEMIES 135 3 4 2 7 1 Power consumption and Welght ococcccccnnncnnnnnnnnnnnonnnnnnnnnnnnnnnnnononnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnos 135 3252 02 Neu te 135 A An saceciconsioasaqantooese sareqnaesosacuac on soeceanreemsscaseqeansosegeacoasonncesomeessesaree 136 2o N A A 136 SG 136 eo SS An 136 3 5 3 1 Guides to understanding the requirements esses nono non nono nro nn nnns 136 SE ll U Ot SAN ST nn 136 3 5 3 1 2 Unconfirmed and undefined regurements eren 136 3 5 3 2 General Require Hielils ars 136 SUN AE Cu c PH 136 CRX MERO Sra S SIE UU T 136 SO nn E E 137 D E E ON 137 3 5 3 3 1 Hardware minimum requirements oooccccccnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnninininess 137 EE 137 0 sument S TAL
3. Next tables show the integration tolerances for the different barrel which contain the singlets Barrel 1 is in Table 3 2 35 Lens mount 2 is in Table 3 2 36 Lens mount 3Ba is in Table 3 2 37 Lens mount 3Bb is in Table 3 2 38 and Barrel 4B is in Table 3 2 39 Note that Barrel 1 and Lens mount 2 are common for the two pixel scales For Barrel 1 the 0 25 px scale do not violates the values given for them in the 0 45 px scale In the case of the Lens mount 2 the L2 values are imposed by the 0 25 px scale but do not represent tight values The others barrel have values quite relaxed The range obtained for the compensator in dectenter for L2 and L5B are shown in the tables PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 82 of 183 Barrel 1 L0 M1 M2 M3 Lope pem ose s o ow xw ex um sm mm Table 3 2 35 Integration tolerances within the barrel 1 for the 0 25 px scale Lens mount 2 L1 L2 L3 L4 Cold Stop DECENTER X DECENTER Y TILT X TILT Y POSITION Z um arc min arc min um um Lu pese ium 3 10 03x49 Compensator Compensator L2 200 400 600 Table 3 2 36 Integration tolerances within the lens mount 2 for the 0 25 px scale SINGLET Lens mount 3Ba L5B L6B SINGLET TILT X TILT Y DECENTERX DECENTER Y POSITION Z um arc min arc min um um Compensator Compensator 500 400 Table 3 2 37 Integrat
4. 3 4 2 7 2 Instrumentation rack Communication Unit Read Out Electronics Temperature Monitor DADAS E Temperature Controller Da AAA ICH Gr Motion Control Vacuum Measurement System Figure 3 4 2 10 Instrumentation rack PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 136 of 183 3 5 Software 3 5 1 Summary This section contains the requirements of the SW of the PANIC instrument and the design report for fulfilment of that requirements After the introductory part the requirements for the SW which were derived from the applicable documents are presented This document forms part of the documentation set to be revised by the review panel at the PDR 3 5 2 Introduction The PAnoramic Near Infrared camera for Calar Alto PANIC is planned as a wide field NIR camera for the 2 2m telescope at Calar Alto Observatory PANIC will be built by a consortium formed by two institutions with proved experience in R D developments These institutions are MPIA Heidelberg Germany and IAA Granada Spain The PANIC SW is divided into two main parts the Instrument Control Software ICS and Data Handling Software DHS The ICS is divided into two systems GEIRS and the Observation Tool OT and the DHS is again divided into the data reduction software DRS and the Quicklook 3 5 3 Requirements 3 5 3 1 Guides to understanding the requirements 3 5 3 1 1 Use of shall should
5. 78 Table 3 2 27 Integration tolerances within the lens mount 2 for the 0 45 px scale 78 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 24 of 183 Table 3 2 28 Integration tolerances within the lens mount 3A ooccccnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnos 78 Table 3 2 29 Integration tolerances within the barrel 4A oo cc cece cccccceeeeeeeeseeeeseeeeeseeees 78 Table 3 2 30 Integration tolerances within the Optics mount 1 79 Table 3 2 31 Integration tolerances within the Optics wheel in the 0 45 px scale 79 Table 3 2 32 Assembly tolerances for the different units in the 0 45 px scale 79 Table 3 2 33 Tolerances for whole instrument to the telescope in the 0 45 px scale 80 Table 3 2 34 Manufacturing tolerances for individual elements for the 0 25 px scale 8l Table 3 2 35 Integration tolerances within the barrel 1 for the 0 25 px scale 82 Table 3 2 36 Integration tolerances within the lens mount 2 for the 0 25 px scale 82 Table 3 2 37 Integration tolerances within the lens mount 2bRa 82 Table 3 2 38 Integration tolerances within the lens mount 3Bb 000000000000ns0nososnnsssssssssssssssseeee 82 Table 3 2 39 Integration tolerances within the barrel Ap 83 Table 3 2 40 Integration tolerances within the Optics mount 1 for 0 25 px
6. PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 40f183 List of acronyms and abbreviations 2MASS Two Micron All Sky Survey Analog Digital Converter Asymptotic Giant Branch AIV Assembly Integration Verification Anti Reflection CDR Critical Design Review CPU Central Processor Unit OOS o CSE CircumStellar Enveloppe ooo Distortion Data Handling Software 000000 Data Handling Software Direct Memory Access DRS Data Reduction Software EE Ensquared Energy length square side EFL Effective focal length ElectroMagnetic Compatibility EN Eurpaische Norm EPICS Experimental Physics and Industrial Control System Electrostatic Discharge FEA Finite Elements Analysis FIFO First In First Out FOV Field of View Focal Plane Assembly FPGA Field Programmable Gate Array FWHM Full Width Half Maximum GEIRS Generic Infrared Software PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 50f183 Gamma Ray Burst Graphical User Interface H2RG HAWAII 2RG HAWAIORG o Lens number 1 of the PANIC optics system Lens number 2 of the PANIC optics system Lens number 3 of the PANIC optics system Lens number 4 of the PANIC optics system Lens number 4 of the PANIC optics system o A E um Lens number 8 of the PANIC optics system in the 0 25 px scale L7B LAS M2 Second folding mirror inside the instrument M3 Third
7. PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 48 0f 183 3 2 6 Optics Layout 3 2 6 1 PANIC General Optics layout Figure 3 2 6 1 shows the location of PANIC in the telescope EN 1 5 AA 1 Y k Ab A i 1 E i i 1 A d x p i is L L d V i N A L1 rs y A 1 M M k i i VW d A UE KAN i V k A A WV A i i Cha a d LI Y SC Figure 3 2 6 1 PANIC location in the RC focus of the 2 2 m telescope Figure 3 2 6 2 shows the optics model solution for the two scales of PANIC PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 49 of 183 Figure 3 2 6 2 Optics layout of PANIC left the 0 45 px camera and right the 0 25 px camera The PANIC optics design presented in this document has been modelled at cryogenic temperatures and vacuum A separate Technical Note ORD4 describes in details the models considered to obtain the glass catalogue at 80 K produced for PANIC The camera consists of two separate lens systems which will be alternatively inserted after the cold stop mask keeping the total distance between the cold stop and the detector fixed and equal to 437 30 mm A deep study has been made to evaluate the best solution for the implementation of that second pixel scale in PANIC and a separate Technical Note ORD3 describes m details this second pixel scale study Finally we decided to implement the classical
8. PRELIMINARY DESIGN REPORT Page 59 of 183 3 2 6 2 6 0 45 px Distortion The distortion has been calculated in with respect to the FOV centre which does not have distortion In Table 3 2 10 we present the values for the central wavelength of the filters For simplicity we only present in Figure 3 2 6 14 the plot of the maximum distortion obtained in the work photometric band of PANIC Notice that all the bands are in requirements D lt 1 5 94 Wavelength um Distortion 76 0 82 0 99 1 32 0 99 1 08 1 31 1 08 1 34 1 31 J H 1 50 1 80 1 97 2 42 Table 3 2 10 Distortion data in the 0 45 px scale GRID DISTORTION Y BAND INSTITUTO ASTROFISICA ANDALUCIA FIELD 8 5320 W 4 5320 H DEGREES CONCHI CARDENAS IMAGE 76 49 W 76 49 H MILLIMETERS MAXIMUM DISTORTION 1 31H67 PANIC1_V1_TP_045_MULTIBAN ZMX SCALE 1 000X WAVELENGTH 0 9880 Gm CONFIGURATION 3 OF 6 Figure 3 2 6 14 Distortion plot for the 0 45 px camera 3 2 6 2 7 0 45 7px Transmission The preliminary estimation for the average throughput in PANIC is done using the transmittances given by the glasses manufacturers they have been introduced in the glass catalogue of PANIC used in Zemax for the lenses and the cryostat window It has been considered AR coating given by Zemax both sides and the thickness of any element We expect better performance in transmission due to the optimization of the AR coating of the lenses with the manufacturers In Table 3
9. Shall is used for requirements whereas should is reserved for guidelines Requirements are mandatory and guidelines are not mandatory although their fulfilment should be strongly pursued 3 5 3 1 2 Unconfirmed and undefined requirements A TBC or a TBD identifies unconfirmed or undefined requirements respectively 3 5 3 2 General Requirements 3 5 3 2 1 Parts The System shall be divided in the following main parts 1 Instrument Control Software ICS 1 1 GEIRS 1 2 Observation Tool OT 2 Data Handling Software DHS 2 Data Reduction Software DRS 2 2 Quick look 3 5 3 2 2 Operating System All the computer system involved in PANIC ICS and DHS shall work on a personal computer PC running 64 bit Suse 10 x Linux distribution This requirement is in compliance with CAHA staff PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 137 of 183 3 5 3 2 3 System Log The errors faults and warnings shall be logged properly and used as input for system maintenance giving as minimum the timestamp code and description of the error 3 5 3 3 GEIRS The generic infrared camera software of the MPIA and Calar Alto shall offer the same capabilities for PANIC like for Omega2000 with some extensions and add ons It shall implement all instrument hardware interfaces and shall offer the telescope interface It shall still support the previous interactive usage of the
10. Focus mm Table 3 2 15 Bandwidths of evaluation of the PANIC optical design and their change in focus for the 0 25 px scale The image quality of the instrument is specified in terms of the 80 EE EE80 for each photometric band The EESO is evaluated in Table 3 2 16 using the greater value given in the FOV analyzed Note that all the bands are in requirements EE80 lt 3 pixels 54um 0 75 EE80 um EESO pix EESO arcsec Table 3 2 16 EE80 in the 0 25 px scale For simplicity it has been presented only the polychromatic EE in Figure 3 2 6 25 where it is represented the fraction of energy enclosed as a function of the half side length square It is indicated with an horizontal line the 80 of the EE In dark it is shown the diffraction limit of the system For simplicity as well it has been presented only the polychromatic spot diagram in Figure 3 2 6 26 This figures shows the geometrical structure of the image at all points of the field for all the wavelengths considered Better figures are obtained when the system is refocusing in the photometric bands The squared boxes indicate the dimension of two pixels in the focal plane 36 um and the Airy disk for this configuration is indicated with the dark circle PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 67 of 183 DIFF LIMIT H 0880 0 0880 DEG 0 008080 6 0008 DEG 0 1888 0 1088 DEG 0 0620 0 0628 DEG FRR
11. PANIC PRELIMINARY DESIGN REPORT Code Issue Rev Date No of pages PANIC GEN SP 01 0 1 22 October 2007 183 PANIC PANoramic Infrared camera for Calar Alto PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 2 of 183 Approval control Vianak Naranjo Harald Baumeister Werner Laun Ulrich Mall Matthias Alter Prepared by Clemens Storz Jens Helmling M Concepcion Cardenas Vazquez Jos Miguel Ibanez Mengual Matilde Fernandez Josef W Fried Josef W Fried Revised by Julio Rodriguez Max Planck Institut fur Astronomie MPIA Instituto de Astrof sica de Andalucia IAA PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 3 of 183 Changes record Issue Date Section Page Change description EE AA E WE WE E A ll Applicable documents JN Documenttitle Code Issue 02000 User s Manual 2 6 Oct 2005 PANIC SCIENTIFIC REQUIREMENTS PANIC GEN RQ 00 Reference documents N Documenttile Code Issue ORD2 Signalto Noise cases PANIC OPT TN 00 00 ORD4 GlassCatalogue PANIC OPT TN 04 00 ORDS Toleranceanalysis PANICOPTTN 05 00 Optical AIV Preliminary Design AIV PANIC OPT TN 06 00 Fruchter A S Hook R N 1997 A method for the Linear Reconstruction of undersampled Images PASP astro ph 9808087
12. SCHLE APERTURE DIAMETER 247 8888 p FOOTPRINT DIAGRAM RAYS THROUGH 64 69 INSTITUTO ASTROFISICA ANDALUCIA SURFACE CONCHI CARDENAS FAY X MIN RAY Y MIN MAX RRDIUS ke Te PANTC1_01_COMPLETE_TF_TAMA 0S ZMK LONFLGURATLON 2 0 E Sa Figure 3 2 6 17 Footprint of the 0 25 px camera FOV on the Entrance window left on the L0 right TURE OLAMETER 276 2647 RAYS THROUGH 84 68 FOOTPRINT DIAGRAM INSTITUTO ASTROFISICA ANDALUCIA x MIN Y MIH RADIUS PPHICI VI CDHPLETE TP TRHH D ZHX CLONPFLCGURMATLON lt UF aF LL Pe p EIT A E ia w HI ka J ki a La Le e La SCRLE Sei AFERTUEE DLAME TER 219 043 FODTPELNI SURFRCE 17 FAY X MIN RAY Y MIN MAX RRDIUS 0736 RAY X MAX 56 BB REY Y MAX 5954 WAVELENGTH ALL 8868 MILLIMETERS zu La SCALE Sei AFERETUEE DIAMETER 246 F244 FODTPRELINI FATS THEUUGH 84 68 DIAGRAM INSTITUTO ASTROFISICA ANDALUCIA SURFACE 14 CONCHI CARDENAS RAY X MIN RAY Y MIN MAX RRDIUS x HRX Y Y MAX IAVELENGTH 66 9555 46 2830 ALL PANICI WI COMPLETE TP TAHA 05 24x COMPLGURATLONM OF Z RAYS THEOUGH 84 48 DIAGRAMA INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS 76 1538 Ee 2398 PANIC1_41_CONPLETE_TP_TAMA D5 ZHX CONFIGURATION 2 Of Ta Figure 3 2 6 18 Footprint of the 0 25 px camera FOV on the M1 left up on the M2 right up and on the M3 bottom PANIC Cod
13. and a peak of 200GByte per night 3 5 3 7 2 Data storage 3 5 3 7 2 1 Disk The data should be copied to the data reduction system from the data acquisition computer The data reduction system should have a minimum total capacity of 4 TeraBytes about 30 full operation nights 3 5 3 7 2 2 Access Raw data monitor data calibration data and images shall be easily accessible to the users for copy to DVD USB disk or any other removable supports 3 5 3 7 3 Delivering format FITS shall be the default format for delivering the results to the scientific community so both raw and final data shall be FITS files 3 5 3 7 3 1 FITS headers One separate document shall specify contents of FITS headers The CAHA FITS document of Mr Roeser MPIA shall be taken into account 3 5 3 7 4 Saving Modes PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 148 of 183 Data files shall at least not exceed the 2 Gbytes size limit to allow data storage and handling of data also on 32bit limited file systems Therefore a configuration shall be available to limit the max FITS file size to a proper size and the software shall split larger exposure files into multiple files For a single exposure buffer of 125 full size images the storage size as 16bit data is gt 125 32Mbytes 4000Mbytes 3 9 Gbytes In the fast photometrie mode a 15 minutes continuous run of 1 kHz of 36 36 pixels the single sub
14. Figure 3 TEE 151 ac ANNO A O ON PO Duns UM I osea SAA DX Hu eE iSi 152 Figure 5 5 4 Computer EES 153 Figure 3 5 4 4 Overview of the PANIC control software tasks the access to data the data flow the connection to the hardware and to Observation Tool and to the on line pipeline ao A A A PI a asieran aoid 154 Pisute 5 50 Dala DRESS oa tools ica 159 ac O NI oe dio A e O ON SOU A 163 Figure 3 5 4 7 Browser interface Conceptual Diagram eere 164 t 3o A S Data TOW RT E 166 Figure 3 5 4 9 Quick reduction SCHEME sse eene eene nnn nennen 170 PPCM gt 4 10 Science mode scheme ee 171 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 23 of 183 LIST OF TABLES Table 3 1621 H2RG Major Characteristic asirios 38 Table 3 2 1 Summary of the PANIC General Specifications ooooooccccccnnnnnnnnnnnnnnonnnnnnnnnnnnnnnonoss 45 Table 3 2 2 Mass estimation for the PANIC optics system oooocccccnccnnnncnnnnnnnnnnnnnnnnnnnnnnnnnnnnnonoss 50 Table 3 2 3 Raw mass estimation for the folding mrorg cc ceeeeeeeceeeeeeeeeeeeeeeeeeeeeees 50 Table 3 2 4 Prescriptions data of the common elements of the optical system at its nominal desioi CANIN A A 51 Table 3 2 5 Prescriptions data of the elements that only belong to the 0 45 px scale 52 Table 3 2 6 Summary of the PANIC performance in the OA3ipsscale eecseteeeeeees 55 Table 3 2 7 Fields used in
15. PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 26 of 183 1 2 General Requirements The general requirements that were clear from the start are Detector size 4096x4096 pixel Spectral range NIR 1 e minimum YJHK Image scale 0 45 arcsec pixel 2 2m telescope Additional obvious requirements are Instrument must not exceed limits set by the telescope in size and weight Flexure of the instrument must not degrade optical quality Power dissipation should be kept as low as possible goal 200W The standard guiding unit on the telescope can not be used since it would vignette the field of PANIC So PANIC must have its own guiding system 1 3 Design Aspects These requirements have direct consequences on the design of PANIC The optical train is much longer than the maximum allowable length of the instrument along the optical axis This requires a folded design The lateral dimension is not critical The weight limit is a very severe one According to the original ZEISS documentation the weight limit is 300kg at the focus This has led us not to follow the commonly used design with two nested tanks rather our design uses one super isolated tank with one small tank to cool the detector However both CAFOS and WFI at the twin telescope on LaSilla exceed this limit without any degradation in telescope performance Including the guider unit CAFOS weighs 400kg and has a torque of 1860Nm
16. 2 11 and Figure 3 2 6 15 are the values and the plot respectively of the expected transmission as function of the wavelength In the transmission calculation all the mirrors has been considered the two telescope mirrors and the three folding mirrors of PANIC For the telescope mirrors we have modelled an aluminium coating and for the PANIC folding mirrors a gold coating PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 60 of 183 H L I un H L TRANS a HW BEHOL 1 650006 WAVELENGTH IN um TRANSMISSION VS WAVELENGTH INSTITUTO ASTROFISICA ANDALUCIA IS UNPOLARIZED PANIC V COMPLETE TP CORTINC ZHX CONFIGURATION 1 OF 2 Figure 3 2 6 15 Expected transmission for the 0 45 px camera 3 2 6 3 0 25 px camera 3 2 6 3 1 0 25 px Optics Layout Figure 3 2 6 16 shows the unfolded optics layout of the 0 25 px scale of PANIC Filters K SS A NAE L1 L3 us Dewar e Wip MO mes M3 o window Field Stop 3 Mirrors Cold Stop mask mask T Figure 3 2 6 16 Optics layout of de PANIC the 0 25 px camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 61 of 183 3 2 6 3 2 0 25 px optical prescriptions The prescription of the system is listed in Table 3 2 4 and Table 3 2 12 In Table 3 2 4 are listed all the common elements of the two pixel scales and in Table 3 2 12 there are listed the elements of the scale
17. 4 Overview of the PANIC control software tasks the access to data the data flow the connection to the hardware and to Observation Tool and to the on line pipeline reduction software 3 5 4 5 1 GEIRS integration time and data specifications GEIRS most important expressions and how they shall be interpreted are e exposure is the result of a single start read out command sent to the ROE This will result in the execution of cycle repeat times of cycle type executions by the ROE e exposure time is the sum of the pixel integration time in all cycle types done as result of a single start readout command sent to the ROE e integration type for the HAWAII2 RG this 1s always the integration while read type IWR To start with a well defined detector state new IWR cycle the detector is normally reset pixel by pixel or line by line or in the 2RG eventually also frame wise e integration time is the time that each pixel of a single cycle type image is exposed to photons Because of the IWR property of the detector this 1s for single correlated images the time between the reset of the pixel and the readout of the pixel for double correlated images PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 155 of 183 the time between the Ist readout and the 2nd readout of the pixel for multiple correlated images the time between the Ist readout and the correlated readout of the pixel diffe
18. COP I mseg Ji fis 2 fs a a lis fis 1 os ln Software p 2 2 2 2 2 2 14 MPIA Management 31 MPIA Management AA PRELIMINARY DESIGN REPORT PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date Page 22 October 2007 181 of 183 2075 4 6 Cost and Financial plan 2825 The cost listed below 1s exact for detectors and electronics First offers for filters are 10000 each Only crude estimates can be made at this stage for cryostat and optics This table does not include cost for man power Optics Filter Cryostat Electronics Computers etc miscellaneous 1 050 000 _ 1 490 000 260 000 150 000 150 000 30 000 10 000 miscellaneous 30000 30 000 1 710 000 According to the schedule this results in the following financial plan 2007 255 000 250 000 detectors 5 000 travel 765 000 680 000 550 000 150 000 60 000 5 000 250 000 260 000 150 000 10 000 10 000 detectors cryostat electronics misc travel detectors optics filters computers travel 2010 10 000 10 000 travel PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 182 of 183 The dates of the rates for the detectors are as requested by Teledyne in their offer The other expenses have to be distributed over the years 2008 and 2009 1f these are outside the budget one might consider to buy only a subset of the filters or aim at delivery of filters early 201
19. GEIRS does not know the correct entries This shall be based on a flexible FITS keyword dictionary of the instrument Telescope and mountain informations from the observatory the PANIC instrument informations as well as the PANIC OT and data reduction informations shall be specified in this keyword dictionary and used in the FITS header e write the data into FITS files Preferred format is a single multi extensions FITS file per exposure with the integral image of each detector stored as FITS image extension e write each resulting data file name and information into a data log file which might be used for accessing data files from software parts outside GEIRS store the data files alternating on multiple hard disks in parallel if speed of a single disk or RAID partition is a limiting factor 3 5 3 3 4 Filter focus PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 140 of 183 The different telescope focus offsets for each filter shall be characterized and available to the instrument control system The GEIRS shall focus the telescope secondary mirror automatically when a new filter 1s selected by the user 3 5 3 3 5 Guiding Due to the telescope tracking performances and planned observing modes guiding shall not be needed at first light but it should possible to implement after first light Although guiding will not be necessary for most observations because typical exposure tim
20. PRELIMINARY DESIGN REPORT Page 14 of 183 Sele Quek ET 144 A E OE A 144 noz Observing BIN RIED 144 BN GUUS sagas CO E 144 E e o MM E MIRI 144 ee o accuser E arene tpn emmre ceased aaa nonteettetencteseouneeac cet 144 o ER e E 144 OE EC S MEE B data EEGENEN 144 33306 M Ee SOMW ate TT 144 S0 D T XOUICE it E EE 144 2 912945 Ll Dark Ccurent SUDIDICHOD E 145 Ge NN Pae AM ccm 145 So os I Badeprxel E e ME 145 SEINE ME C SI 145 E GN o HI EE 145 o LAS ASOC oca 145 o A aiu IN eM en dox dMiP ata mua me Mes d curet adeft idees 145 2 5 9 0 2 T Master calibration MIMO S dee 145 Jaaa Date Current Subs AOGLIO E 145 225 023 ER E Ee e 145 305 4202 eene 145 co ER ee ET o e A 146 0 30 20 COSMICTAYS e 146 ME e DDR m em 146 3 5 3 6 2 8 Shift and align Dithering and Stacking cccccncncnnncnonnnocononenininenininininininnninaninnnanananannnnnns 146 CSS IA MEME E A 146 o O AAA o un A O eee eee re 146 co IA a is AA 146 5 5 552 LI de li ON ae ti eee eee ce 146 30 0 0 2 MZ SIA ASI Actas 146 3 5 3 6 2 11 3 World Coordinate System WCS 146 3 5 3 6 2 12 Photometric Requirements oocccccccccnnnncnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnns 146 3 5 3 6 2 12 1 Absolute Photometric in J HkKe een nennen nennen nenne 146 3 3 3 6 2 12 2 Absolute Photometric Ih Y Zi 146 SESS ELM MEC PP MM 147 a A oo ae eaccamguenccsaest 147 55 A e AA Ee
21. SCHLE f 5 APERTURE DIAMETER 91 2757 X RAYS THROUGH 64 68 APERTURE DIAMETER 33 06 X RATS THROUGH 64 623 FOOTPRINT DIAGRAM FOOTPRINT DIAGRAM 25 INSTITUTO ASTROFISICA ANDALUCTA Y lt S INSTITUTO ASTROFISICA ANDALUCTA SURFACE 27 L CONCHI CARDENAS SURFACE 29 LAB CONCHI CARDENAS RAY X HIH 11 6338 RAY X MAX 41 6398 RAY X MIN 37 3533 RAY X MAX 37 353 RAY Y MIN 6338 RAY Y MAX 1 6338 PRNICI VI COMPLETE TP TRMR 05 2 Mx RAY Y MIN 37 3533 RAY OY MAX 37 3533 PRNICI VI COMPLETE Ip mn OS ZHx MAX RADIUS 3 gt WAVELENGTH ALL COMFIGUEATION OF 7 MAX RADIUS 39 d WAVELENGTH ALL CONFIGURATION 2 OF 2 Figure 3 2 6 21 Footprint of the 0 25 px camera FOV on the L5B left on the L6B right PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 64 of 183 d bw r ER a e Fo Ta ia ee ee i ech i bel Zei IMETERS LIMETERS e QU mw noni A eg e ea ETC d Sp Bonn AA AAA A aoe ei weil MII AA EEE TI Rh i W LL ep IT COIITITITFETILLEI MAMA bai je e al e e DAA E a Be 56 000 D0 GG MN A P 4 m E RT T n d A Ki n D ki x KE X ET ET AS cu d d Xa dug urge vum og dara Pr Pee oe eae aa SGH eee ge Pe ews wn vi K APO mn La Be 1 B E De n ki Ki E OK Ki EI n m T Ki TINAA Rn n CAMARO HE AEERa Mr a K 4 S Harary Be LKE HL AAA ADA E
22. SEU A E E 166 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 16 of 183 JASI Dotoctor C3 Mod 1 8 0 EE 167 A 167 3 5 4 8 3 1 3 Sky modelling and extractnon eee nennen 168 CREW E callo REO L 168 3 5 4 8 3 1 5 Electronic Crosstalk correction oooooooccccnnnnooccccnononononancnncnnnnnonnnnnncnnnnnanoncnnnnnnnannnnnncnnnns 169 3 5 4 8 3 1 6 Optical ghosts TM ss 169 o A o APA 169 S ey P NON e e 169 3 5 4 8 3 1 9 Astrometry and Photometry sse eene eene enne enne nnne 170 SI os Quick NS A aeudedenoadssaeeades omencusedaaedesamsecweceseetes 170 De o idu mr 170 30404 Implenientallon gedet A a Ye UAM Us tu Padus d n 172 30 WEIN EN ANGE E EE 173 S E GE 173 5509 LUO Oee E E E 173 36 3 Technical Requirements ii ai orde 173 3 6 3 1 gt o ee eee ee ee 173 e e E 173 Lo O O O o oO E ee eee ee er eee Sree eee eee reer ene ree 174 3 6 3 3 1 The electronics Rack can be mounted under the mirror cell independent of the cryostat This means that the cable length between the electronics rack and the cryostat will be about 4m 174 3 6 3 3 2 To guarantee the best technical support CAHA needs a full spare electronics set 174 3 6 3 3 3 Before first light Calar Alto staff needs a full documentation set in English 174 3 6 3 3 4 Regarding electronics the docume
23. We take these values as safe limits The operating temperature of the detectors is in the range 77 80K the optimum temperature has to be found by experiment From experience with other Rockwell detectors we expect that the operating temperature should be stable to 0 1K The cooling system should require as little attention as possible Since liquid Nitrogen cooling requires only refilling we decided to use nitrogen cooling We are aiming at holding times longer than 24 hours although Calar Alto would accept refilling twice a day We try to benefit from experience gained with Omega2000 as much as possible PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 27 of 183 o Mechanical detail solutions such as lens holders and filter wheel mechanics will be taken over with minimal changes o The read out electronics is a further development of the older MPIA ROE using newer and cheaper ICs Furthermore the new ROE will read out 132 channels compared to 36 in Omega2000 o The control electronics will use modules which are standard at MPIA CAHA and are in use not only in Omega2000 but also in several other instruments on Calar Alto This will reduce not only the time required for development but also has obvious advantages for documentation spare parts stock and know how on Calar Alto 1 4 Additional Features While designing PANIC several additional features were proposed which go beyond t
24. are manufactured very precisely and that friction can be neglected This mounting method has been successfully used in both OMEGA2000 for lenses with diameters between 106 mm and 155 mm and in PYRAMIR for lenses with diameters of about 20 mm between T 293K and 77K L OECD IEA a aa uc osm 1 9 o Es H 98 nm B M 19 o Bh ow 4 19 Lua lm o 00 mw ow 0 uA seme gt 1M 9 LB Bh x6 9 1 SS iB m o 9 18 ws B ww o M Table 3 3 4 Material list of cryogenic optical elements and their mounts The cold optics parts are made of at least nine different materials each material having different thermal expansion properties eight optical materials for the lenses and mirrors and aluminium AlMg4 5Mn for the mount parts Table 3 3 4 shows that the fused silica FS lens actually PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 98 of 183 becomes slightly larger when cooled down to 80 K whereas the BaF lens shrinks by about 0 3 This behaviour 1s nonlinear for all the materials used which means that e g the fused silica lens shrinks and expands again while temperature changes from 300 K to 80 K Of course cooling of the mount parts and the lenses does not start simultaneously because the lenses are cooled by the mount and the retainer rings are cooled by the corresponding lenses and by the scre
25. as well as on the size and quality of contact surfaces A rough surface will slide less easily and give poorer thermal contact to another part than a smooth one For this reason the chamfers are diamond turned Note that low thermal conductivity will lead to an inhomogeneous temperature distribution inside one part Measurements during the development of OMEGA2000 have shown that in the case of the CaF lens the maximum temperature difference between the lens and the mount during the whole cooling period is about 40 K In the case of fused silica this difference is about 60 K The maximum temperature gradient in the lens from its centre to its edge is 5 K and 12 K respectively This does not cause much thermal stress The larger temperature difference in the case of a fused silica test plate is mainly due to the fact that the surface quality and angle of its chamfer being hand polished are less accurate than the surface and angles of the diamond turned CaF test plate Although the chamfers of all parts were machined with the highest possible accuracy both shape and surface quality it is not possible to simply put the parts together to meet the optical PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 99 of 183 specification for lens alignment Radial holes in the lens mount allow the measurement and adjustment by fine pitch threaded screws of each lens In principle the lens adjustment can a
26. bulge disk decomposition Rare objects as T dwarfs and z gt 6 QSOs could be other science goals The NIR part of COMBO 17 4 could be completed in 12 5 clear nights A deep NIR photometric survey for sample selection and characterization would be also of interest as a previous step for the exploitation of the EMIR NIR multi object spectrograph a common user instrument for Grantecan Characterization of distant galaxies will also benefit from a high resolution imaging mode 2 1 2 GRBs 2 1 2 1 GRBs at high redshift The detection of GRBs at redshifts beyond zz 7 is currently one the major astrophysical challenges due to its deep implications in the reconstruction of the history of the Universe However at redshifts z gt 5 the Lyman a blanketing prevents the detection of their optical afterglows so near IR observations are required for their identification The determination of photometric redshifts is viable with simultaneous multiband observations carried out with medium class telescopes like the 2 2m Calar Alto telescope 2 1 2 2 GRB host galaxies A dedicated multicolour imaging program running at the 2 2m would allow for the first time to compile a homogeneous large sample of GRB host galaxies and to apply statistical methods to construct the SED of GRB host galaxies brighter than R 24 using photometric points From the fit of the SED we would infer information about the following quantities the photometric redshift the a
27. but it s assumed that the actual Nitrogen production is good enough for the Panic needs A few days before Panic comes to the telescope Calar Alto staff will make the necessary vacuum and will cool down the instrument with the Nitrogen produced in the 3 5 Telescope to its nominal values For that purpose Calar Alto will use its own vacuum pumps On the day when the instrument comes to the telescope it will be properly cooled down and the mechanics group will mount it and prepare the telescope balance for observation After installing Panic at the telescope the Electronics group will make all necessary connections and a functional test to ensure the correct working conditions from all motors and detectors After this the Astronomers group will prepare the instrument for the observer and if necessary they will give an introduction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 177 of 183 The normal operation place will be the remote observation room situated in the laboratory building The observer will have a backup possibility for copying his files to an appropriate data media which must be decided in future During the normal operation the instrument will be filled with Nitrogen at least once a day When the observing run is over and if it will not be used it will be stored in the Coud room in the 2 2m Telescope In case of technical problems during the observing run
28. can be relaxed significantly This means that certain optics groups have to be measured interferometrically and corrected before they are mounted to the complete optics assembly These compensators are e Axial distance between L1 and L2 e Decentre in x and y of L2 e Decentre in x and y of L6A Retainer ring of L1 Retainer ring of L2 Mount of L2 can be DN shifted in x direction j PS Intermediate ring can be shifted in y direction Micrometer screw for x direction Lens Ll Lens L2 Mount of L1 can be machined for axial distance adjustment Micrometer screw for y direction Optics mount 2 Figure 3 3 2 25 Optics mount 2 with mechanical decenter adjustment of lens L2 with micrometer screws exploded view PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 116 of 183 Screw access holes for sliding rings Lens Ll Mount of L1 can be Retainer ring of L1 machined for axial distance adjustment Lens L2 Dowel pin Retai l f L2 etainer ring o Mount of L2 can be shifted in x direction Micrometer screw for y direction y Micrometer screw for x direction Intermediate ring can be shifted in y direction Pupil stop mask Optics mount 2 Figure 3 3 2 26 Section of optics mount 2 The axial distance between L1 and L2 can be adjusted by machining one of the mount parts The centricity adjustment of L2 and L6A requires som
29. data It will be also possible to detect intermediate age populations in spiral arms by identifying AGB stars their stellar photometry is of crucial importance for understanding and quantifying the importance of the AGB star contribution to the integral light of unresolved stellar populations in distant galaxies Global progression of star formation throughout galaxies could be characterized obtaining accurate maps of the old stellar population mass and comparing them with star formation measurements 2 1 3 3 Magnetic field Polarimetric observations of nearby galaxies allow determining the large scale distribution of the magnetic field At a nuclear level information on the geometry of the narrow and broad band line regions could be inferred Polarimetric studies of extragalactic star forming regions will provide information on the dust distribution as well as on the energizing mechanism of the magnetic field in the thermal structure of the nebulae 2 1 4 Distance scale A measure of the near IR period luminosity relation of Cepheids in nearby galaxies as a function of the metallicity would improve the accuracy of extragalactic distance scales 2 1 5 Searches for high redshift quasars A by product of large area multiband imaging could come the detection of high redshift z gt 7 quasars based on the position of the Lyman a break between the z and K bands at z gt 7 The high redshift quasar candidates would be subject of specifically p
30. fail procedures How to s 3 6 3 4 6 In case it will be needed by CAHA staff training of software operation will be required 3 6 3 4 7 It is recommendable to have a RAID system to prevent data losses as well as a DAT unit 3 6 3 4 8 If possible the hardware should be acquired in Spain for warranty issues 3 6 3 5 Optics and cryogenics 3 6 3 5 1 In case that the optical fine adjustments will be done on Calar Alto it would be desirable to mount a clean room This room can later be used for filter changes and all works to be done on the cryostat 3 6 3 5 2 Transmission curves including red leaks beyond 2 5 um for all filters and the other optical elements should be supplied in paper and electronic ASCII format 3 6 3 5 3 The drawings of the optics shall be delivered in electronic form in a format agreed upon with CAHA PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 176 of 183 3 6 3 6 Acceptance Fulfillment of all these technical requirements together with fulfillment of science operations requirements separate document and successful commissioning are necessary conditions for final CAHA acceptance PANIC Acceptance and Commissioning Team Calar Alto August 2007 CAHA requirements for PANIC August 2007 Approved by CAHA director on 17 of October of 2007 3 6 4 Operation Before first light CAHA needs to know how much Nitrogen will be needed for normal operation
31. folding mirror inside the instrument MBE Molecular Beam Epitaxy MOCON Motion Controller MPIA Max Planck Institute for Astronomy MSPS Mega Sample Per Second Non Applicable Near InfraRed PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 6o0f 183 ORD Optics Reference Document Observation Tool PC PCI PANIC Detector Control System PDR Preiliminary Design Review Preliminary Optical Design PSF Point Spread Function Puls Width Modulation QSO Quasi Stellar Object RC Ritchey Chr tien Resolver Module Root Mean Square Radius of Curvature ReadOut Electronics Telescope Primary mirror S1 Telescope Secondary mirror SDSS Sloan Digitized Sky Survey SE D Spectral Energy Distribution SMDS Stepper Motor Driver for 8 Axis SRAM Static Random Access Memory Software TBC Unified Modeling Language ooo Unified Modeling Language UNIMOD Universal Module WFCAM Wide Field Camera UKIRT PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 70f183 CONTENTS 1 FANK GENERA H E 25 1 1 INTRODUCTION rotura raro 25 Ufer GENERAL REQUIREMENT KC 26 1 3 DE GIN FSP TO ee 26 1 4 EE 27 2 v 8s FOE GL ON GU NL o ecc cT 28 2 1 PXTRAGALACTIC ASTRONOMY E 28 E GE EE 28 LT MEE e a e OO 28 2 1 2 1 A A cU nen d ansR aM d QU DS LANE MEM RE IU RERO 28 221 2 2 ORB EE 28 2 1 5 Mapping of nearby galaxies cesses essen enne nnn
32. has a complete knowledge of the instrument This contact person should be reachable also during vacations and occasionally but rarely during the night and weekends 174 3 6 3 3 8 The first PANIC observations will be done during instrument commissioning and in contact with the hardware and software designers if possible present at Calar Alto 174 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 17 of 183 SX ST MES i EE 174 3 6 3 4 1 The disk organization will be as follow 174 3 6 3 4 1 1 One disk for the system installation boot swap and partitions ooocnnnnnnnnnnnnnnnnnnninininn 174 3 6 3 4 1 2 One disk for the whole instrument software Odtsk at 175 3 6 3 4 1 3 Ome or more disks for data Gdekb A 175 sp ESA A a amu I sep e ae EL MEME eT 175 3 6 3 4 2 The system installation will be done by Calar Alto staff according to its own standards SuSE Operating system and Pc based computer 175 3 6 3 4 3 Before first light Calar Alto needs a full backup of all necessary software installed in the computers necessary for the normal operation This backup system will be tested before first light CAHA requirements Tor PANIC August iesse 175 3 6 3 4 4 Any non standard part in the Pc shout be acquired together with a spare part 175 3 6 3 4 5 Regarding software the final documentation should include occcccccnnnnnnnnnnnnnnnnnnnnnnnnnnnos 175 P
33. image at all points of the field for all the wavelengths considered Of course better figures are obtained when the system is refocusing in the photometric bands The squared boxes indicate the dimension of two pixels in the focal plane 36 um and the Airy disk for this configuration is indicated with the dark circle PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 58 of 183 DIFF LIMIT 0 2188 0 2189 DEG 0 0000 0 0004 DEG 0 26680 0 26680 DEG 9 1540 0 1548 DEG FRACTION OF ENCLOSED ENERGY 0 000 9 888 18 000 HALF WIDTH FROM CENTROID IN 4m FFT DIFFRACTION ENSQUARED ENERGY 0 45 INSTITUTO ASTROFISICA ANDALUCTA WAVELENGTH POLYCHROMATIC CONCHI CARDENAS SURFACE IMAGE CCAMERA FOCUS PRNIC1 U1 COMPLETE TP ZMX CONFIGURRTION 1 OF 2 Figure 3 2 6 12 Polychromatic EE of the 0 45 px camera 087 B 0000 0 0900 DEG OBT 0 1540 0 1548 DEG 95090 x 1 4300 9180 2 ARR IMA 0 004 8 8088 MM IMA 22 254 22 251 MM OBJ 8 2188 8 21880 DEG DBT 0 2660 0 2664 DEG IMA 38 744 38 744 MM INSTITUTO ASTROFISICA ANDALUCIA ae ARE ee RIRY EE X EXE P a j CONCHI CARDENAS RMS RADIUS 7 578 6 784 7 155 7 420 GED RADIUS 16 589 15 735 23 162 20 761 PANIC1_V1_COMPLETE_TP_COATING ZMX BOX WIDTH 36 REFERENCE CENTROID CONFIGURATION 1 OF 2 Figure 3 2 6 13 Polychromatic spot diagram of the 0 45 px camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007
34. lt science gt Flat sky flat dome Tat where meaning is defined as is a optional set of elements 0 N is a optional set of elements but at least one element 1 N mean single and optional element 0 1 meaning or lt gt angle brackets used to surround obligatory entities 3 5 4 6 4 Workflow Firstly the observer shall define the observation program according to his her scientific program proposal It can be done on line or off line using the OT After the observer has defined his her observation program with the OT Editor it should validate it to ensure that it is compliant with the operational instrument rules avoiding wrong parameters values or nonsense sequences Then OT shall generate a script commands sequence that shall be sent to GEIRS command server over a socket connection If these commands are accepted by GEIRS it will execute them and reply to OT about the success or failure of them So on the OT side there is a listening event handler that manages the GEIRS reply commands The OP can also be submitted to the observation repository for a further execution The general workflow of the OT is presented in the next figure PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 163 of 183 Program Set Constraints No Define Observation Define Targets Blocks sequences frames Validate OP Generate Script Fixerrors and w
35. maximum in position f the inner mask due to the S2 obstruction must have a diameter of 36 87 mm for the minimum in position and 36 24 mm for the maximum in position g itis not necessary the implementation of the obstruction due to the S2 spiders h if we decided to implement the four arms then they can be 1 4 mm of thickness or less PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 73 of 183 Notice that the degradation in the pupil re imaging diameter shall be 3 maximum in K band as it 1s required in 3 2 5 1 5 We can calculate the degradation in the diameter for K band due to positioning the pupil at the polychromatic position 13 53 mm which is 1 73 3 Also we have calculated that degradation due to the decentring 200 um in X or Y axis perpendicular to the optical axis and tilt 3 arcmin the pupil is 0 63 Adding the three contributions the total degradation 1s 2 99 which is nearly the 3 as maximum permitted So we conclude that the pupil fulfils the requirement even in the polychromatic position A footprint at the polychromatic position of the cold stop for the central and the external fields 1s shown in Figure 3 2 6 32 To avoid maximum background suppression losing minimum flux in K band we propose to place the pupil at the distance of 22 30 mm from the L4 with the dimensions shown in Table 3 2 20 But we can placed it at the polychromatic position being
36. plane At the detector plane the image spots analyzed are located in the coloured points as it is shown in the Figure 3 2 6 24 The box indicates the total size of the whole detector including gap of 167 pixels between detectors SURFACE IMA CAMERA FOCUS INSTITUTO ASTROFISICA ANDALUCIA JUNCHI CARDENAS NIC1_V1_TP_025_MULTIBAN ZMX REFERENCE CHIEF RAY CONFIGURATION 1 OF Figure 3 2 6 24 Complete FOV of the 0 25 px PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 66 of 183 The performance of the design is evaluated at the wavelength and bandwidths shown in Table 3 2 15 Notice that the design has been optimized to this bands except the z band The requirement for z band is not optical quality it is only for transmission in this band Instead of this it can be seen that there is optical quality in z band so the system is able to work in this photometric band As the filters will be placed in convergent beam it has been decided to simulate them by inserting a plate of IR fused silica with a thickness of 12 5 mm between the L7B and L8B it is possible to refocus the system by a movement of the telescope S2 along the optical axis so the measurements in defocus is referred to the displacement of the S2 from the nominal position in the polychromatic configuration and gives the sense forward 1 e sense toward the entrance window backward opposite
37. position is detect by an micro switch Part Motor Resolver Ref Switches Table 3 4 2 2 Summary of motion controlled filter wheels 3 4 2 6 2 Optics and field stops wheel Part Motor Reslover Gear Ref Switches Second Pixel Scale Optic VSS52 200 xx RE 15 1 A14 Harmonic Drive 100 1 Field Stops Wheel VSS52 200 xx RE 15 1 A14 Harmonic Drive 100 1 Table 3 4 2 3 Summary Both wheels are driven by a stepper motor in combination with an 100 1 harmonic drive gear The detection of a reference position comes from a micro switch Harmonic drive gears mounted on Phytron motors have the following advantages High reduction ratio in a small volume Very low weight Very low mass inertia High permissible torque in comparison to the size High drive speed Very low backlash in comparison to conventional gears High efficiency PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 135 of 183 3 4 2 7 Resources 3 4 2 7 1 Power consumption and weight consumption VA Temp Monitor Lake Shore 2198 TL AITOR Compact Rack Components 195 300VA 53kg Table 3 4 2 4 Summary of power consumption and weight The calculated power 1s the maximum power consumption from manufacturer datasheets 195 300VA The calculated weight is 53kg We are investigating ahead possibilities exist to reduce the power dissipation e g switching off devices not in use
38. scale 83 Table 3 2 41 Integration tolerances within the Lens mount 3B cccccnnncnnnnnnnnnnnnnnnnnnnnnnnnnniness 83 Table 3 2 42 Integration tolerances within the Optics wheel in the 0 25 px scale 83 Table 3 2 43 Assembly tolerances for the different units in the 0 25 px scale 84 Table 3 2 44 Tolerances for whole instrument to the telescope in the 0 25 px scale 84 Table 3 3 1 Grouping of the optical elements of PANIC for the 0 45 arcsec pixel scale 94 Table 3 3 2 Grouping of the optical elements of PANIC for the 0 25 arcsec pixel scale 94 Table 3 3 3 Mass estimation of the cryogenic opto mechanics oooccccnnncnnnnnnnnnnnnnnnnnnnnnnnnninons 95 Table 3 3 4 Material list of cryogenic optical elements and their mounts 97 Table 3 3 5 Tilts and displacements of optical bench and optical groups 110 Table 3 3 6 Overall mass estimation of PANIC with two pixel scales 117 Table 3 3 7 Overall mass estimation of PANIC with only one pixel scale 119 Table 3 4 2 1 Summary of electronic COVICES nennen 129 Table 3 4 2 2 Summary of motion controlled filter Wheels ooooooocconcnonnnnnononnnnnnnnns 134 Table E S UTIWTIBEV E 134 Table 3 4 2 4 Summary of power consumption and weight cccccccccccccccceeeeeeeeeeeeeeeeeeeeee
39. slightly different positions shifted by the dithering offsets they have to be aligned prior to the summation The approximate offsets can be calculated from the observing position stored in the image header or directly from the PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 169 of 183 known dither pattern used For high quality images the alignment precision should be on a sub pixel scale which is beyond the pointing accuracy of the telescope The exact shifts of the images can be obtained by matching the positions of corresponding point sources in the frames Once the offsets are known the frames can be superimposed to the master sum frame in different ways Well sampled images can just be summed with integer pixel shifts whereas in the under sampled case a more elaborate summation process e g the DRIZZLE RD7 algorithm for the PSF reconstruction might be more appropriate Both methods will be implemented in the pipeline system The summation process also offers the possibility to effectively eliminate cosmic ray events in the data Since cosmics usually affect individual pixels and are statistically distributed in the different images they can be removed by filtering high pixel count levels that are detected in a single frame only 3 5 4 8 3 1 5 Electronic Crosstalk correction Images from one detector channel may produce secondary images ghosts on other channels either positive o
40. solution which consist in a optics wheel that interchanges all the optics elements after the cold stop as it is shown in the next pages in this document The straight layout shown in the Figure 3 2 6 3 and Figure 3 2 6 16 shows a long instrument 21925 mm Due to the mechanical constrains in length and weight it has been searched alternatives to make the system more compact and finally the packaging solution adopted shown in the Figure 3 2 6 2 introduces three folding flat mirrors in the optical path between LO and L1 From the optical performance point of view this packaging proposed has not effect The distances between mirrors have been fixed as shows the Table 3 2 4 which is an optimum mirror separation with no possible interference and vignetting and optimizes the cold volume of the system PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 50 of 183 In Table 3 2 2 it 1s shown the mass estimation for the lenses of PANIC calculated from the Zemax model In the calculations are included the cryostat window and the lenses of the two pixel scales Element Weight Kg Window 2 93 7 51 LO to L4 L5A to L8A 2 96 L5B to L8B 2 84 Total 16 24 Table 3 2 2 Mass estimation for the PANIC optics system A raw estimation for the folding mirrors mass shown in Table 3 2 3 could be made assuming circular mirrors with a clear aperture diameter and a thickness of the 10 of its dia
41. the filling level and the orientation Also this vessel will be filled from the side through the central ring There are three tubes with functionality similar to the tubes of the large vessel 3 3 1 2 4 Spacers The spacers connect the cold and the warm parts of the cryostat They have to be stiff to fulfill the requirements on flexure and they have to have a very low heat conductivity Furthermore they have to compensate the thermal shrinking of the cold structure We therefore use GRP glass fibre reinforced plastic With a ring of 12 sheets which are flexible in radial direction and stiff in all other directions we solved this problem PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 90 of 183 Central ring of vacuum can One of 12 spacers Cold optical bench Figure 3 3 1 3 Cold warm spacers from the central ring to the optical bench 3 3 1 2 5 Thermal connection of the detector The detector package will be connected to a separate small nitrogen vessel This will bring a temperature stability which is almost independent from the ambient conditions The expected stability 1s better than 0 2 K The required stability of 0 1 K makes a controller necessary This controller will also be used to control the warm up and cool down of the detector The heat dissipation of the detector will be compensated by the Nitrogen inside the small vessel The heat dissipation of the preamplifier
42. the read noise of 15 electrons for the detector 3 4 1 3 3 H2RG CB HAWAII2RG Clock Bias board The H2RG CB board generates all supply and bias voltages needed by the 4 HAWAII2RG detectors The bias voltages are generated with a DAC and can be adjusted remotely Further the H2RG CB board does a level translation of the pattern coming from the ROCon to appropriate levels At last this board houses a FPGA The FPGA provides 4 synchronous serial interfaces to set up the HAWAII2RG internal registers Some of the pattern lines are routed to the FPGA in order to trigger the change of detector internal register values via a serial write H2RG CB Ext Data Address DAC Bias Voltages Reference Voltage Detector Supply Detector Serial Interface n y O p O qo n G O y E Level Clocks to Detector Pattern Figure 3 4 1 4 H2RG CB block diagram PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 124 of 183 3 4 1 3 4 BP6 6 slot backplane The BP6 connects the above three boards There are 4 slots for AD36 boards 1 slot for 1 ROCon and 1 for the H2RG CB board The backplane also connects to the power supplies and delivers the power to the different boards The BP6 is layouted impedance controlled and has termination circuitry onboard This provides optimum signal integrity for high speed signals 3 4 1 3 5 OPTPCI fiberlink interface The OPTPCI board re
43. the science images 3 5 3 6 2 6 Shift and align Dithering and Stacking Since the images will be shifted by the dithering offsets they shall have to be aligned prior to the summation image stacking This should be done with choice of several schemes drizzle SWARP MONTAGE 3 5 3 6 2 9 Gap elimination The detectors will be spaced about 147 pixels on focal plane so the DRS shall eliminate that gap in the full image when enough frames are taken with the suitable dither offsets 3 5 3 6 2 10 Scale Modes The two different pixel scale modes shall be considered into the data reduction software both quick and science pipeline mode 3 5 3 6 2 11 Astrometry Requirements 3 5 3 6 2 11 1 Absolute Astrometry Absolute astrometry accuracy shall be lt 0 3 arcsec rms for any processed multi frame 3 5 3 6 2 11 2 Relative Astrometry Differential astrometry accuracy shall be lt 0 1 arcsec rms for any processed multi frame 3 5 3 6 2 11 3 World Coordinate System WCS Final astrometry calibration from the catalogue with an appropriate and agreed World Coordinate System WCS shall be written in all FITS headers 3 5 3 6 2 12 Photometric Requirements 3 5 3 6 2 12 1 Absolute Photometric in J H Ks Absolute photometric accuracy should be x 0 02 mag in J H Ks bands with pixel size of 0 25 arcsec and 0 04 mag with pixel size of 0 45 arcsec It will depend on the quality of the input data 3 5 3 6 2 12 2 Absolute Photom
44. 0 4 7 Schedule The schedule is shown on the next page An important date is the assembly of the instrument early 2009 This requires that the cryostat including all interior parts is finished and the detectors and the read out electronics are working at least in a non optimized way For integration of the whole system and laboratory tests we have foreseen 1 year Since MPIA has much experience gained from the Omega2000 project we are confident that the cryostat and the wheels will not cause major problems So most of this time will be devoted to optimization of the read out First light will be in 2010 and we plan to optimize the instrument during about 3 commissioning runs so that it will be available for the astronomical communities in 2011 The schedule rests on three assumptions 1 the manpower required is actually allocated to the project 11 the time of delivery of the detectors is 18 months as promised by Teledyne in their offer and 111 the detectors fulfil the specifications Assumption 1 may be optimistic since the design office at MPIA is currently overbooked by a factor of about 2 The schedule assumes that the design of the cryostat to the level required by industry can be finished until about march 2008 and the design of the interior parts lens holders wheels mirror mounts is finished during summer so that the manufacturing of these parts can start in September and be finished early 2009 so we can proceed with the a
45. 0 25 px that only belong to that pixel scale The curvature radius and thicknesses of the lenses are given at 80 K working temperature of PANIC For manufacturing and assembly those parameters have to be replaced by warm parameters using thermal expansion coefficients defined in OR D Curvature radius Thickness or Separation AMEE meos eS 139 a 7 Bar 271 923 i 195 6231 L6B IR Fused Silica 83 1 180 2618 AA a 248 5058 L61B SR E SF03 2339 343 7706 AA CECR 173 621 L7B 40 0 BaF 60 7 57 76894 160 495 LSB 14 6 IR Fused Silica 81 0 90 66532 AA a 0 Bee Rar p S Table 3 2 12 Prescriptions data of the elements that only belong to the 0 25 px scale 3 2 6 3 3 0 25 px descriptions In this section we present all the footprint for the optical components in the 0 25 px scale configuration from Figure 3 2 6 17 to Figure 3 2 6 23 264 4608 MILLIMETERS SCALE Si HPERT SURFA kn RAY MAX X Y R 200 0000 MILLIMETERS HAFER sE e LIE RAY EFT HAX PANIC PRELIMINARY DESIGN REPORT URE DIAMETER 291 1694 FOOTPRINT DIRGERM Xx PAYS THROUGH INST LUTO RSTRURISICA ANURLUCTH CE S ENTRANCE WINDOW CUONCHI CARDENAS MHIN 61 8195 EMY X MIN 61 8195 RAY Y MAX 61 8 ADTUS 74 4693 WAVELENGTH ALL MAX PPHIL V LUMPLETE Ip DR US Mx LCOMFIGUREHRMIIOPM QI Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 Page 62 of 183 ti D Lli i MILL THE
46. 0 kHz 1 MHz 074 Hz 7 14 Hz 0 024 Hz 0 24 Hz 15 2 Hz 588 Hz 15 2 Hz 588 Hz subwin 36x36 lir ieff 100 37 6 Hz 294 Hz 37 6 Hz 294 Hz inside der ieff gt 50 37 6 Hz 294 Hz 37 6 Hz 294 Hz area ofa msr 1 single channel 75 2 Hz 588 Hz 75 2 Hz 588 Hz eff 100 subwin 36x36 single frame rate 139 Hz 1000 Hz coneria lir Geff 100 69 4 Hz 500 Hz WE the edge der ieff gt 50 69 4 Hz 500 Hz Y between 2 channels msr ieff 100 139 Hz 1000 Hz MO msr looses 1 frame time at each cycle restart in a cycle repeat loop Table 3 5 1 Expected image rates compared for the subwindow size of 36x36 read pixels asked for in AD 2 3 5 4 5 3 Read noise reduction For small narrow band filter observations of faint stars a read noise reduction with non destructive read outs should be available The table below lists the expected read noise and integration times based on Rockwell s general specification of the Hawaii 2RG depending on the correlation of nondestructive reads l single Expected Overhead T multi pixel expected Read clock correlated multi Read uim sup Usage reads n samples Noise time SC 1MHz e 100 kHz high background bright objects 100 kHz medium background 1 5 medium bright objects Exposure 10 30s 0 14 high background very l bright objects 0 44 better to use a 100 kHz read not recommended use 100 kHz read Table 3 5 2 Table with expected read noise suppression in case of limitation by
47. 1296 36 36 5184 36 36 10368 e GEIRS source package e GEIRS control configuration files for PANIC e GEIRS ROE engineering configuration files for PANIC e GEIRS FITS configuration files for PANIC PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 158 of 183 e PANIC read out electronic including fibers and cables serial line NPORT terminal server and data lines or running PLX data generator or running in data simulation e MPIA PLX PCI 64bit 66MHz interface PLX driver extensions running in multi threaded code or running in data simulation e Linux PC system to run GEIRS multiple CPUs enough RAM e Connection to PANIC instrument IP network Expected additional software gnuplot X for installation g X subversion All this is available in the standard openSuSE distribution 3 5 4 6 Observation Tool description 3 5 4 6 1 Purpose The aim of the OT is to provide a higher abstraction level for the users of PANIC at the observatory providing easier observation procedures and a set of extra keywords to be saved on FITS headers to be used by the data reduction software DRS The OT will allow the astronomical users to specify the observations in a user friendly way avoiding to remember large commands or building complicated scripts They should choose a predefined observing template or build their own observation template using high level commands to PANIC It is intended t
48. 183 The high background in infrared data must be carefully estimated to retrieve the science information In imaging mode the observations are done in dither mode with small offsets around a central position for each exposure to allow to estimate the sky background variations directly by filtering the images and separate astronomical from sky signal Apart from this difficult sky estimation the frames are recombined with some cross correlation techniques to precisely determine the offsets between the images The main role of the Data Reduction Software DRS will be this data reduction For this purpose an on off line pipeline will be considered Automatic pipeline reduction of PANIC data is predicated on the assumption of a well defined set of observing protocols that forward the relevant meta data to the pipeline reduction system Besides the pipeline should not only deliver science quality products but also provide feedback on the health of the camera and on the overall data quality The DRS will have two main operational modes quick and science The quick operational mode is used for quick look purposes and for on site quality control It will process all raw data sequentially i e as they arrive from the instrument It produces calibration products and reduced science data but will usually not obtain the best possible results This 1s due to the sequential operation post observation day time calibrations are not available during nig
49. 2 Telescope Interface The interface of the OT with the telescope shall be provided through the GEIRS interface 3 5 3 4 3 3 3 On line star catalog Remote communication between OT and on line star catalogs shall be carried out via http PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 141 of 183 3 5 3 4 4 Display The frames coming from the camera shall be shown in GEIRS real time display tool the OT shall not show them 1t has no own frame display 3 5 3 4 5 Observing definition The OT shall allow the definition of all observing information This shall include but not be limited to Science program information PI observer program title email observation constraints seeing airmass distance from moon time intervals target coordinates and epoch scale mode 0 45arcsec pixel or 0 25 arcsec pixel filter detector setup dithering pattern for sparse fields or extended objects exposure time each position number of cycles readout mode saving mode separate disk FITS files for each exposure integrated image only a multi extension FITS file guiding stars TBC 3 5 3 4 6 Calibration definition The OT shall allow the definition of calibrations observations This shall include but not be limited to calibration series darks dome flat fields with a fixed lamp power and filter providing automatic exposition time calculation twiligh
50. 200 400 400 Table 3 2 27 Integration tolerances within the lens mount 2 for the 0 45 px scale Lens mount 3A L5A L6A L7A DECENTER X DECENTER Y SINGLET amis a ee a ah in POSITION Z um arc min arc min um um Compensator Compensator L6A 3 00 3 00 T 152 150 300 350 Table 3 2 28 Integration tolerances within the lens mount 3A Barrel AA L8A DECENTER X DECENTER Y SINGLET Mein a in gt in EN POSITION Z um arc min arc min um um E eo eow m xm 3x4 Table 3 2 29 Integration tolerances within the barrel 4A PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 79 of 183 Next tables show the integration tolerances for the sub barrels and finally the instrument We show them as they are nested First there are the Optics mount 1 Table 3 2 30 and the Optics wheel Table 3 2 31 them the whole instrument assembly Table 3 2 32 and finally the alignment of the instrument with the telescope Table 3 2 33 Note that Optics mount is common for the two pixel scales We have considered a default ranges for the tolerated parameters for Tilt 3 arc min for decenter 100 um and for position 200 um also The only available adjust once the system 1s cooled will be the telescope refocusing using the S2 although for integration a detector adjustment in position and tilt is possible The tilt in the detector will be required to co
51. 4 A PANIC CA 2 2m CAMERA Telescope Figure 3 5 4 1 Software architecture 3 5 4 3 Network Layout In regard the layout of the main parts of the system there will be tree main areas properly network connected the telescope are where the instrument will be the computer room next to the telescope area and the control room that is where the user will handle the instrument using a Thin Terminal connected to the ICS workstation The data reduction workstation will also be in the Control Room with a fast network link to the ICS data storage unit A general overview of the network layout is described in the next figure PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 152 of 183 Instrument Devices E ComPort Detector Computer Room ICS workstation Ethernet 100Mb s Fiber Figure 3 5 4 2 Network layout 3 5 4 4 Computer Architecture The PANIC software will be divided in two main systems one for the Instrument Control Software and other for the Data Reduction Software Both systems will be Linux PC based with multiple CPU enough RAM and a fast network links For the data storage a system based on local disk RAID arrays to prevent data losses as well as a DAT DVD for backup should be installed by Calar Alto staff as archive server PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 153 0f 183 Data Reduction Workstat
52. 56 x 156 mm It is machined into the housing of the field stop wheel When PANIC is used with the 0 25 arcsec pixel scale a field stop mask of 63 x 63 mm is turned into the optical beam It rotates by 75 and it has two positions which are defined by mechanical limit switches from Saia For simplicity the same motor Harmonic Drive gear and ball bearing is used as for the optics wheel So identical spare parts can be used for both units The distance between both field stops axial direction 1s 2 mm Rotating field stop Harmonic Drive gear Stepper motor Figure 3 3 2 13 Rotating field stop total view and section PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 106 of 183 Figure 3 3 2 14 Rotating field stop in two positions with the housing upper part hidden left field stop for 0 25 arcsec pixel in use right field stop for 0 45 arcsec pixel in use 3 3 2 2 6 Detector mount The detector unit is mounted directly to the housing of the optics wheel unit Tip Tilt and focus position 1s adjusted once by shimming or machining without additional actuators However details about the detector assembly are not yet available 3 3 2 2 7 FEM simulation results 3 3 2 2 7 1 Simulation of cryostat with optics replaced by point masses For the first FEM simulation the whole opto mechanics was replaced by two point masses representing one optics assembly each Figure 3 3 2 15 The point m
53. 8 This circuit prevents damages caused by electrostatic discharge and ensures that no voltage greater than 4 7 volts is applied to any detector pin from Clock Bias board D gt to detector S 4V7 GND GND Figure 3 4 1 8 preamplifier protection circuit Last but not least the detector manual states that there are some protection diodes at the input pads but doesn t reveal any details 3 4 1 3 9 Troubleshooting Diagnostics For troubleshooting purposes there are some built in diagnostics The first diagnostics facility is on the OPTPCI board The FPGA can be switched to a data generator mode In this mode errors on the PCI side of the OPTPCI can be discovered PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 127 of 183 The second facility is on the AD36 board The FPGA on this board can also be switched to a data generator mode In this mode the data transfer mechanism from the ROE to the OPTPCI can be checked A device that simulates a HAWAII2RG detector will soon be available This device has read only memory 32 DACs and a FPGA onboard In response to the clocking pattern it outputs a test picture on the DAC outputs and thereby allows to check the complete signal path from thecryogenic preamplifiers to the shared memory PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 128 of 183 3 4 2 Control Electronics 3 4 2 1
54. A 2 which starts at the completion of conversion of the AD36 boards This sequencer is programmable via commands It reads the conversion results of the AD36 boards in the desired order and transmits them to the PANIC workstation via Fiber 1 and 2 Fiber 1 and 2 can transmit 132 Mbyte sec each 3 4 1 3 2 AD36 36 channel analog to digital converter The AD36 board houses 36 ADCs with suitable differential drivers and a FPGA The synchronous serial outputs of the ADCs are connected to the FPGA When conversion is completed all 36 conversion results are present in FPGA internal registers and can be read from the ROCon PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 123 of 183 ADC Data Channelselect Cardselect Trigger Figure 3 4 1 3 AD36 block diagram The ADCs have 16 bits resolution and a throughput of 1 MSPS For more information refer to the data sheet of the AD7677 With a scale of 0 45 pixel an area of 15 x 15 of the detector can be read in about 1 1 ms On the prototype the noise performance for a single correlated read with shorted inputs of the AD36 board results in a standard deviation of 0 8 counts Adding the noise of the cryogenic preamplifiers will result in about 1 0 Assuming a charge storage capacity of 100 000 electrons this would be a noise of approximately 2 1 electrons for a double correlated read This value is small compared with
55. AS 23 RAY X MIN 52 5879 RAY X MAX 58 5879 RAY X MIN 51 9827 RRY X MRX 51 9827 RAY Y MIN 58 5879 RAY_Y MAX 58 5879 PRNICI VI COMPLETE TP pp DS znx RAY Y MIN 8827 RRY Y MAX 51 8827 PRNICI VI COMPLETE TP TRMR 0S ZMX MAX RADIUS 60 7972 WAVELENGTH ALL CONFIGURATION 2 OF 2 MAX RADIUS WAVELENGTH ALL CONFIGURATION 2 OF 2 Figure 3 2 6 20 Footprint of the 0 25 px camera FOV on the L3 left on the L4 right Ba are e Pus Re E 9S we ew ee a D MM e w Ce E e WR ER SS y ewei d ER ES E E LAA EKEERRREEXEEXZZEXR EXERNEENSEENEEXNX EUA ADA DN Le IHET md De m on Bim a E EN h E 2 my e S el EPR a am RARAAAZ amp t HIL LIRE vs ial PA b PL noc IA d im aui Co gt A di 3x ar aw BBB MILL a y amp i A wwNNEWwNBN CEA UE WugpGGEGSMEGEHMN Ej EMER ee ee ee ar HEDERRRR Sus AER kr Ze ein Tr bi Ex a A oa prem Ta Zum Qu ww rrpp E a o Dl NN NN a Mal wow de ee a ee de EE BERERERE SA SS SAAR BARR REE cree 2 EE e s 8 X a e PREABAPRARR IS F e OR aif t Fa WEE FAMA PREX eee SPER sERREX PREM EERE FAR six ath WEEK Ki 146 2000 HREEZZALEM c Be 56 FOBIA Sa Fal i Kg r Fa Pa eee ee a ri a Ki x E LI x LI RS x x E x E x RI a K x x x Ke al Le EJ E LJ ALE A Ag F Apr eee eee ee rj d
56. Alto Instrumentation Committee recommended to build such an instrument In October 2006 the project PANIC Panoramic Near Infrared Camera for Calar Alto was started It 1s a joint project between IAA and MPIA One may argue that an instrument like PANIC should be installed at the 3 5m telescope Obviously the 3 5m telescope is more powerful however observation time is much more readily available at the 2 2m telescope so the disadvantage in light collecting power by a factor of 2 2 3 5 2 0 4 can be compensated by integration time Omega 2000 at the 3 5m telescope is clearly a competing instrument However Omega 2000 does not have a cold entrance pupil and hence has a high thermal background in the K bands It is expected that PANIC which will have a cold stop will be more sensitive than Omega2000 and since PANIC has a four times larger FOV it will be more efficient by factors of a few than Omega2000 in the K bands PANIC will not be the first instrument of its kind Competing instruments at telescopes lt 4m are WFCAM at UKIRT NEWFIRM at Kitt Peak 4m telescope and WIRCAM at CFHT In the southern hemisphere VISTA 4m telescope has a 64 Mpixel camera that will cover 2154 square arcmin its operation shall start mid 2008 It is obvious that because of these competing instruments the development of PANIC should be fast However the proposed science cases for PANIC show that interesting science can be done with it even if it 1s not unique
57. CTION OF ENCLOSED ENERGY 13 500 27 100 HALF WIDTH FROM CENTRDID IN 4m FET DIFFRACTION ENSQUARED ENERGY 00 INSTITUTO ASTROFISICA RNDRLUCTR WAVELENGTH POLYCHROMATIC CONCHI CARDENAS SURFACE IMAGE CCAMERA FOCUS PANIC1_V1_COMPLETE_TP ZMX CONFIGURATION 2 OF 2 Figure 3 2 6 25 Polychromatic EE of the 0 25 px camera 087 B 0000 0 0900 DEG OBT 8 8620 0 0624 DEG 25090 x 1 4300 9100 4000 IMA 0 0AA H DH MM IMA 16 059 16 859 MM OBJ B 0880 B8 DEG OBI 8 1888 8 1888 DEG IMA 22 818 22 810 MM IMA 28 012 28 812 MM SURFACE IMA CAMERA FOCUS po SPOT DIRGRRM 0 INSTITUTO ASTROFISICA ANDALUCIA 3 q CONCHI CARDENAS 0 25 UNITS ARE 4a AIRY RADIUS 11 76 xi FIELD l 2 RMS RRDIUS 5 214 fered 6 191 7 el GED RADIUS Sarti 15 356 16 909 25 372 PANIC1_V1_COMPLETE_TP_COATING ZMX BOX WIDTH 36 REFERENCE CENTROID CONFIGURATION 2 OF 2 Figure 3 2 6 26 Polychromatic spot diagram of the 0 25 px camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 68 of 183 3 2 6 3 6 0 25 px Distortion The distortion has been calculated in with respect to the FOV centre which does not have distortion In Table 3 2 17 we present the values for the central wavelength of the filters For simplicity we only present in Figure 3 2 6 27 the plot of the maximum distortion obtained in the work photometric band of PANIC Of course all the bands a
58. CTION OF ENCLOSEO ENERGY 0 OR HALF WIDTH FROM CENTROLO IN gm FFT OLFFRACTION ENSQUAREO ENERGY 45 INSTITUTO ASTROFISICA ANDALUCIA WAVELENGTH POL YCHROMAT IC CONCHI CARDENAS Figure 3 2 7 1 Montecarlo overlay of the EE80 for the tolerances in the 0 45 px PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 81 of 183 3 2 7 1 2 Tolerances for the 0 25 px scale In Table 3 2 34 are the values for manufacturing considering the 0 25 px scale We have considered the same ranges as in the 0 45 px analysis in the tolerated parameters We can conclude that this scale impose the value in wedge of LO and L2 since result lower values in this scale although the difference 1s not to much There not limitation to the rest of values obtained The values in blue emphases result as the values more restrictive and they must be the limit in that cases The range obtained for the compensator in L6B L61B distance 0 3 mm MANUFACTURING ERRORS OF SINGLETS FIRST STAGE ITEM WINDOW l L61B FILTER winnow si L7B R1 mm 0 420 0 470 0 260 0 150 0 210 t 0 140 t 0 200 t 0 250 t 0 170 t 0 160 R2 mm 0 300 0 430 0 120 3 000 0 280 0 180 0 350 0 060 0 090 Thickness um Wedge arc min 100 Table 3 2 34 Manufacturing tolerances for individual elements for the 0 25 px scale Flatness fringes 632 8 nm
59. Courtesy of Teledyne Scientific and Imaging IC 38 Figure 3 2 6 1 PANIC location in the RC focus of the 2 2 m telescope cc ccceeeeeeeeeeees 48 Figure 3 2 6 2 Optics layout of PANIC left the 0 45 px camera and right the 0 25 px camera 49 Figure 3 2 6 3 Optics layout of de PANIC the 0 45 px camera occccccnnnnnnnonnonononcnnnnnccnncnnnanannnos 50 Figure 3 2 6 4 Footprint of the 0 45 px camera FOV on the Entrance window left on the LO tarn 52 Figure 3 2 6 5 Footprint of the 0 45 px camera FOV on the MI left up on the M2 right up and On TiS MI DOMON coxcasiesscstasedeoneteperioessuecusudacuassaatenidenddeyciensauniuerdiselacsetenedencneddeoesgantaleeds 53 Figure 3 2 6 6 Footprint of the 0 45 px camera FOV on the L1 left on the L2 right 53 Figure 3 2 6 7 Footprint of the 0 45 px camera FOV on the L3 left on the L4 right 54 Figure 3 2 6 8 Footprint of the 0 45 px camera FOV on the LSA left on the L6A right 54 Figure 3 2 6 9 Footprint of the 0 45 px camera FOV on the L7A left on the L8A right 54 Figure 3 2 6 10 Footprint of the 0 45 px camera FOV on the detector plane 55 Figure 3 2 6 11 Complete FOV of the 0 45 Pri iaids 56 Figure 3 2 6 12 Polychromatic EE of the 0 45 px camera esee 58 Figure 3 2 6 13 Polychromatic spo
60. EN SP 01 Iss Rv 0 1 Date Page 22 October 2007 53 of 183 218 e244 FOOTPRINT OTAGRAM Mz 185 7Y 114 7326 RAY X MAX 5483 RAY Y MAX 350 WAVELENGTH LBH 1 60H 4 5483 ALL RAYS THROUGH 83 98 INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS PANIC Mi _COMPLETE_TFP_TAMA 05 Mx CONFIGURATION 1 OF 2 RAYS THROUGH 82 98 INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS wt VI COMPLETE TP eg 0S ZER CONFIGURATION 1 OF 2 J Figure 3 2 6 5 Footprint of the 0 45 px camera FOV on the M1 left up on the M2 right up and on the M3 bottom METERS pop MILLI E 5 APERTURE DIAMETER SURFACE 19 RAY x MIN RAY Y MIN MAX EBHLL ILS a agar did RAY x MAX card RAY 1901 METERS galas MILL Log l z Haas FOOTPRINT DIAGRAM 5 RAYS TAROUGH Ba Sax CG up INSTITUTO ASTROF SICA ANDALUCTA CONCHI CAROENAS lt uerace 21 RAY x MIN RAY Y MIN MAX EBHLD ILSsz v1 36 el dey ALL Y PANIC YI COMPLETE TP THHR DE zHX MAX z CONFIGURATION 1 OF 2 WAVELENGTH APERTURE OLANETER 1524 14r 13 FOOTPRINT OLAGRAM Lz 5r 67 T2 amp HB3 RAY s MAX Z amp LHB3 RAY Y MAX 60335 WAVELENGTHS 67 6489 67 6489 ALL Figure 3 2 6 6 Footprint of the 0 45 px camera FOV on the L1 left on the L2 right 5 RAYS TAROUGH 83 98 INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS PRHICI Mi _COMPLETE_TP_TAMA DE Mx CO
61. F SINGLETS FIRST STAGE Flatness fringes R1 mm R2 mm Thickness um Wedge arc min 632 8 nm www 3m xs M w sem o s s 4 w la a o o loa m dq la u sem soe xm x9 uw onoo roov om e o n Tamara ce anm uw aen om am ox 0 0 um sem Luca zm ox o i osoaz ronson om wo o o ooo sux x 9 0 0 om TI m 3x lu im sem sume xm 339 Table 3 2 25 Manufacturing tolerances for individual elements for the 0 45 px scale Next tables show the integration tolerances for the different barrel which contain the singlets Barrel 1 is in Table 3 2 26 Lens mount 2 is in Table 3 2 27 Lens mount 3A is in Table 3 2 28 and Barrel 4A is in Table 3 2 29 Note that Barrel 1 and Lens mount 2 are common for the two pixel scales We have considered a default ranges for the tolerated parameters for Tilt 3 arc min for decenter 100 um and for position 200 um The range obtained for the compensator in dectenter for L2 and L6A are shown in the tables PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 78 of 183 Barrel 1 L0 M1 M2 M3 Table 3 2 26 Integration tolerances within the barrel 1 for the 0 45 px scale Lens mount 2 L1 L2 L3 L4 Cold Stop SINGLET TILT X TILT Y DECENTER X DECENTER Y POSITION Z um arc min arc min um um Compensator Compensator 3 00 3 00
62. IM Io IM SDEDE 147 3 5 9 6 2 10 Catalog BeBDerdlODi ous c o EHE ss 147 GER Hardware Eet 147 3 5 3 7 Data Collection And Data Rates Requirements c oooooooooocooooooooooooononnnonnnnnnnnnnnnnonononnnnn nnns 147 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 15 of 183 ON O O o 147 Go E EE NEE e e A 147 EA A E OE S ET 147 SONNEN e O 147 3 5 3 7 3 Delivering 0 6 002 E 147 Boada H KEE 147 gt ae Ret E A ee een 147 sod 4I A 148 e E PCT A 148 A MEE O A 149 A 149 cr NUS MER nn PP 149 os A O o PA Oo A E 149 o E Ei E II A 149 An A 150 3 5 4 1 DAS DRUG nt EE 150 GE E RER Tee 150 CRT onto ay OU E 151 5544 XORDUIGFJATCRIIEE iones 152 3545 GEIRS Design ucsetIpilOfi eeneg 153 3 5 4 5 GEIRS integration time and data opecfceatonsg enne nnns 154 3 5 4 5 2 Read out with high speed 155 SOA O do alo iones alii Aa li o A 156 SES SE MERCURIUS 157 Dro A ro E A m 157 3 0446 Observation I OOlCeSCMp s uoo nene cieduec esaet On aetas cedes oca enata dO enen 158 3 98 Ee 158 ERST EN Di A ene See RT EAER een eee tan a ene 158 O e E 159 E A E T A E 162 Sos Ine Obermano Ke RE 163 3 5 4 6 6 Programming language and components occccccnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnns 164 Sm di A PA 164 es A og 0 6 A 164 3 9 2 7 enee E 164 S545 Data eduction Software es CAPO si A iia 164 O e o MEE MEM MEE 164 O EN E 165 224053 HEH 166
63. INARY DESIGN REPORT Page 101 of 183 Lens LSA Shaft Lens L8B Lens mount Retainer ring Phytron motor Counter weight Wheel mount Figure 3 3 2 6 Optics wheel without housing PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 102 of 183 Mounting surfaces for filter wheel unit Ball bearing Housing Bellow Labyrinth coupling Wheel mount Figure 3 3 2 7 Section view of optics wheel unit Stainless steel bearing support ring Double row ball bearing Figure 3 3 2 8 Optics wheel ball bearing detail view of Figure 3 3 2 7 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 103 of 183 Detector unit Filter wheel unit Labyrinth Figure 3 3 2 9 Detail view of optics wheel and filter unit 3 3 2 2 4 Filter wheel unit Each of the four filter wheels has an external toothing and is driven by a Phytron VSS 65 stepper motor and a backlash free gear The transmission ratio is 12 8 1 Therefore the positioning accuracy of the wheel is 360 200 steps turn 12 8 8 arcmin which corresponds to 0 32 mm in the centre of a filter The filter wheels have preloaded double row ball bearings WAD937ZZ from ADR outer diameter 73 mm which are very similar to the bearings of the optics wheel see section 3 942 2 3 The wheels are very well balanced by counter weights so there w
64. L I E T E I E nom ED wA FR HU 5 5 D a e P FF P p Mk Ki Ki LT a KN 8 n Ld T T F L KI w d A UP WEE ER e t SCALE SCALE Iu LE j eem veer AFERI URE DIAMETER Ss DI 5 RAYS TAROUGH 84 684 APERTURE DIAMETER 66 6542 5 RAYS TAROUGH BA 68 FOOTPRINT DIAGRAM FOOTPRINT DIAGRAM 0 25 INSTITUTO ASTROF SICA ANDALUCIA 8 29 INSTITUTO ASTROFISICA ANDALUCIA SURFACE 31 LIB CONCHI CARDEMAS syupeace 33 178 CONCHI CARDENAS RAY X MIN 33 6351 RAY X MAX 33 RAY X MIN 26 0549 RAY X MAX 26 0549 PRNIC _V1_COMPLETE_TP_TAHA Ds zMX PAY Y MIN 26 549 RAY Y MAX 26 0549 PANICI UI COMPLETE TP TRHR 05 2 33 6351 RAY Y MIN 33 6351 RAY Y MAX 33 4351 NICH Ui J TR MAX RADIUS 35 8986 WAVELENGTH2 ALL CONFIGURATION 2 OF 2 MAX RADIUS 28 8162 WAVELENGTI i ALL CONFIGURATION 2 OF 2 Figure 3 2 6 22 Footprint of the 0 25 px camera FOV on the L61B left on the L7B right On the detector plane is box indicates the dimension of the detector mosaic and the circle the FOV optimized for the 0 25 px scale 4 9300 1 4308 1 9108 pg zc NDOO LIMETERS 52 0988 MII SCALE APERTURE OTAMETEE 68 9947 RAYS TARUUGH DH GD SURFACE IHR CRHEER FOCUS OUTPRIWT DIAGRAM FULL FIELO SPOT OLAGRAM 0 25 INSTITUTO ASTROFISICA ANDALUCIA oe INSTITUTO ASTROFISICA ANDALUCIA SURFACE 37 LEE CONCHI CARDEMAS Zeg u SC CONCHI CARDENAS RAY x MIN cari HCH RAY a MAX ar Det EMS PADIUS 3 gb t
65. MPLETE_TP_TAMA OS Zur CONFIGURATION I OF e RAYS THROUGH EZ Sex FOOTPRINT DIAGRAM INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS RAY X MAX De B8946 RAY Y ARH Sy Bue WAVELENGTH ALL PANICI VI COMPLETE TP TAMA OS Zur CONFIGURATION 1 OF Zz Figure 3 2 6 8 Footprint of the 0 45 px camera FOV on the ESA left on the L6A right IMETERS DO MILL 4009 Q SCALE APERTURE DIAMETER 144 6016 RAYS THROUGH 63 987 FOOTPRINT DIAGRAM INSTITUTO ASTROFISICA ANDALUCIA SURFACE CONCHI CARDENAS RAY X MIN RAY Y MIN MAX RADIUS 33 74 RAY X MAX RAY Y MAX WAVELENGTH AL PRNICI U1 COMPLETE TP TRMR OS 2MX CONFIGURATION 1 OF 2 IMETERS 00 MILL 3 3 e DO 100 APERTURE DIAMETER 0 45 SURF RAY RAY MAX ACE 237 X MIN Y MIN RADIUS 105 1706 RAYS THROUGH FOOTPRINT OIAGRAM INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS d RAY X MAX 167 RAY MAX Y PRNICI UI COMPLETE TP TRMR OS 2MX WAVELENGTH CONFIGURATION 1 OF 2 Figure 3 2 6 9 Footprint of the 0 45 px camera FOV on the L7A left on the L8A right PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 55 of 183 1 5509 1 43000 e 1 9160 r 2 M i SURFRACE IMA CAMERA FOCUS FULI FIELU SPOT D0OLAGRAMA DNE INSTITUTO ASTROFISICA ANDALUCIA FIELD nu a CONCHI CARDENAS RMS RADIUS Y EE P84 CED PRDIUS 5 EE Dnu PANICI VI COMPLE
66. N SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 173 0f 183 3 6 Maintenance Operation 3 6 1 Summary This document will present Calar Alto Technical requirements and Operations for the Panic instrument 3 6 2 Introduction The main reason for this part of the document is to guarantee the best integration for Panic in the Calar Alto Observatory and its standards As known Panic will be operated in the 2 2m Telescope at Calar Alto and in order to guarantee the best possible operation and integration in the instrument park and at the telescope the instrument needs to be as compatible as possible with the rest of the instruments In item 3 Technical requirements you will find all what we consider important to obtain the best results and the best possible service in case of problems separated in 4 different sections these are mechanics electronics software optics and cryogenics This is a copy from the CAHA Technical requirements for PANIC prepared by Calar Alto staff and the Calar Alto director This document will be revised by the PDR In item 4 Operation we describe how we will prepare the instrument for the observation and what we will do in case of technical problems 3 6 3 Technical Requirements CAHA Technical requirements for PANIC 3 6 3 1 Synopsis This document presents CAHA s technical requirements for the PANIC instrument Science operations requirements are not part of thi
67. NFIGURATION 1 OF 2 PANIC PRELIMINARY DESIGN REPORT 00686 MILLIMET A oa RPERFIURE DImMEIER 146 1 RAYS THROUGH Ba Sex FODTPRLMI DIPFLDEPFI 0 45 SURFACE 23 L3 RAY X MIN 65 9366 RAY Y MIN 65 34386 MAX RRDIUS 69 4786 INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS RAY x MAX 65 9386 RAY Y MAX 6S 9386 WAYVELENGTH ALL PANICI VI COMPLETE_TP_TAMA 05 Zur LONFIGURATLION 1 OF e TERS K L aged MILLIHE 160 SCALE APERTURE DIAMETER 118 3411 RAYS THROUGH Ba Sex FOOTPRINT OLAGRAM AL SURFACE 27 RAY Ox MIN RAY Y MIN HAX RADIUS INSTITUTO ASTROFISICA ANDALUCIA LEA CONCHI CARDENAS Ho 6607 RAY x MAX 49 6607 49 66607 RAY Y MAX Ha 6607 D6 2330 WAVELENGTH ALL PANICI VI COMPLETE_TP_TAMA 0S Zur CONFIGURATION 1 OF Zz MILLIMETERS aono a 16 SCALE ri ER I E HS LIFE SURFACE 25 RAY Ox MIN RAY Y MIN HAX RADIUS aged MILLIMETERS ea SCHLE FIF ER i LIRE d HS SURFACE 29 RAY Ox MIN RAY Y MIN MAS RADIUS DlMMETIER 116 54 rora RHY X SH ore 55 H440 WAVELENGTH DIAMETER 145 9688 x 5r 8946 Sr Be 69 3332 Code PANIC GEN SP 01 Iss Rv 0 1 Date Page 22 October 2007 54 of 183 Ces A if e wi e Ae i PE SS VE di Sai 8 ees rc See eg Ge Leit eg Ce KS THROUGH Ba SEX FODIPELNT 0D LALEFIMA INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS MEX Y MAX RAY PANIC VI CO
68. OE SAMEDI esc T 175 36 34 32 Directory structure fot the SOM W erkene re NENNEN RaR Reo 175 545 104 3 3 Start and E ee 175 3 6 3 4 5 4 Test scripts help programs and debug 175 50 54 09 Description about E 175 3 6 3 4 5 6 Changes done in the standard operating system cocccccncnncncnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnns 175 3 6 3 4 5 7 Normal programs installed in the awvstem nennen 175 3 6 3 4 5 8 Description for the different versions if available 175 3 6 3 4 5 9 Description about the network structure 175 3 6 3 4 5 10 Hardware and software fail procedures HOW t0 S cccccccccccceeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeees 175 3 6 3 4 6 Incase it will be needed by CAHA staff training of software operation will be required 175 3 6 3 4 7 It is recommendable to have a RAID system to prevent data losses as well as a DAT unit 175 3 6 3 4 8 If possible the hardware should be acquired in Spain for warranty issues 175 3 6 3 5 Optics and CrYOQCNICS cc ceeeeeeeesesesessesesseeeeeeeeseeeeseseeeseeeeeeseeeeseeeeeeeseeeeeeeeeeessessssassasaaassaasasaasaaagas 175 3 6 3 5 1 In case that the optical fine adjustments will be done on Calar Alto it would be desirable to mount a clean room This room can later be used for filter changes and all works to be done on the cryostat 175 3 6 3 5 2 Transmission curves including red leaks beyond 2 5 um for
69. ON Features Control of up to 8 axes Motion profiles include S curve trapezoidal velocity contouring and electronic gearing Asymmetric acceleration and deceleration to custom program a trapezoidal motion profile Incremental encoder quadrature input and parallel input for absolute encoder or resolver for on the fly motor stall detection Trace capabilities for system performance checks maintenance and diagnostics Advanced breakpoint capability allows precise sequencing of events Two directional limit switches index input and home indicator per axis Serial Interface RS232 CAN Bus Ethernet Figure 3 4 2 3 Motion Controller Board 3 4 2 3 4 Stepper Motor Driver SMD6 The stepper motor driver board SMD8 contains the power amplifiers to power the stepper motor coils The SMDS board 1s capable to carry eight IM481H amplifier modules The IM481H is a PWM chopper type sinusoidal micro step bipolar stepping motor driver Sinusoidal micro step operation is generated by means of built in hardware and is outputted for operation by clock signal inputting The micro stepping rate 1s selectable from 1 1 1 256 Steps which enables individual application related microstep switching smooth and constant running and reduces considerably system resonance Current down system eliminates motor power losses and heating during standstil Figure 3 4 2 4 SMD8 Board PANIC Code PANIC GEN SP 01 Iss R
70. PANIC readout electronics allows a fine tuning of all components in order to achieve best performance For cross checks a spare set of readout electronics will be available 3 1 7 1 Tests The standard parameters of the Omega2000 detector provide a good starting point for optimization 3 1 7 1 1 Detector sensitivity and system gain The system gain relates the output digital numbers ADU to the corresponding input electrons collected at the pixel unit cell The system gain is expressed in units of electrons ADU With the knowledge of system gain and gain in the signal processing chain pre amp gain the detector internal conversion gain in units of uV electron can be determined Since system gain G and read noise R are constant this leads to a linear correlation between variance of the signal N and the signal itself S PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 41 of 183 S R N G G A linear regression fit y mx b leads to R 1 4 DE G G The actual MPIA detector readout software GEIRS supports a set of statistical functions that allow the data calculation from a stack of images for various integration times 1 e flux levels Since PANIC detector readout software is based on GEIRS these statistical functions will also be available 3 1 7 1 2 Full well capacity The full well capacity 1s estimated from the photon transfer plot vari
71. RP Also mounted to this ring there are all connections like electrical feedthroughs LN feedthroughs vacuum pumping flange safety valve and vacuum gauge To the telescope side there will be a dished flange with the entrance window here called Vacuum upper part At the opposite side there will be a dome flanged to the central ring called lower part The dome uses a dished boiler end All parts of the vacuum can are made from aluminium for weight reduction All flanges and walls are weight optimized to meet the weight limitations of the telescope For the handling of the cryostat we have to add a mounting structure and feet to handle the instrument with a cart 3 3 1 2 2 Nitrogen vessel for cold bench cooling To cool the cold bench we use a Nitrogen vessel The upper part of the vessel is a dished boiler end The light path goes right through the vessel which makes a vertical tube welded into the vessel necessary The vessel will have a geometrical volume of about 107 litres Due to the movement of the telescope it is only possible to fill it half The usable volume has to take into account that the vertical tube could be completely in the liquid The resulting max filling will be PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 89 of 183 about 46 1 We will have a filling and an exhaust gas tube Besides there will be an additional third tube for the safety valve The vessel wi
72. Requirements Positioning of filter wheels Positioning Accuracy 800um outer dimension of filter wheel Motor 1 8 stepper motor 200 steps rev Driver microstepping driver 1 5A RMS 2 1A peak Reference mark micro switch Feedback resolver in 16 bit incremental encoder mode Gear 10 1 reduction ratio gear wheel to gear ring Positioning of optic wheel Positioning Accuracy 70um outer dimension of optic wheel Motor 1 8 stepper motor 200steps rev with harmonic drive gear 100 1 reduction ratio Driver microstepping driver 1 5A RMS 2 1A peak Reference mark micro switch Feedback resolver in absolute encoder mode with angle accuracy 0 2 Positioning of field stops wheel Motor 1 8 stepper motor 200steps rev with harmonic drive gear 100 1 reduction ratio Driver microstepping driver 1 5A RMS 2 1A peak Reference mark micro switch Feedback resolver in absolute encoder mode with angle accuracy 0 2 Monitoring of temperature inside the cryostat Temperatur accurancy Including electronic and sensor accurancy 1K Measurement device 8 channel temperature monitor Lake Shore 218S Temperatur sensor Silicon temperature diode DT 670 wide useful temperature range from 1 4K to 500K Detector temperature controlling max fall rise time 0 5K min Temperatur accurancy Including electronic and sensor accurancy 0 1K Controller device Temperature controller Lake Shore 3318 Temperatur sensor Silicon tem
73. S1 which gives the maximum light collecting power and not the secondary as any Infrared Telescope in which the secondary is undersized The cool stop is used to control undesirable light that could reach the detector it prevents the detector from seeing anything but the optics and the imaged scene especially the warm interior of the system In the optical design of PANIC we have generated a good image quality of the SI in the middle of the optical track and we have determined the optimal pupil imaging position in function of the photometric bands as Table 3 2 20 shows We proposed a mask with an outer hole which corresponds to the re imaging S1 diameter and a inner mask which corresponds to the S2 obstruction as the figure shows Figure 3 2 6 31 Pupil mask shape Distance from L4 rear to Cold Stop Outer hole Inner mask Wavelengths de optimal position mm diameter mm diameter mm Polychromatic 13 53 92 18 36 87 11 37 92 52 36 99 15 40 91 79 36 71 22 30 90 61 36 24 Table 3 2 20 Position and size of the Cold Stop mask The results are a the pupil mask is the same for the two pixel scales b it shall be positioned between L4 and L5 c the position from the L4 in the optical axis direction will be 13 53 mm min and 22 30 mm max see the Figure 3 2 6 3 or Figure 3 2 6 16 d the pupil mask is accessible e the outer hole must have a diameter of 92 18 mm for the minimum in position and 90 61 mm for the
74. T S of EE wn E ep e E Mtt Dr hour e 0 08 Comparison 6 0 1 T 0 12 ap e e ep ap Ap Ap ef 9 a FT s d Ap at e Es eg af en Af kel ZA a 0 14 0 16 std dev 0 0031 mag L J 0 5 0 00 0 6 0 85 JD 2453543 0 Figure 2 2 Observations done with the 3 5m telescope at Calar Alto using the infrared camera Omega Cass and the 0 2 pixel scale The upper panel shows the light curve of a young variable star and the lower panel shows the light curve of a reference star the standard deviation of the second star 1s 3 millimagnitudes PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 35 of 183 3 REQUIREMENTS AND DESIGN 3 1 Detectors 3 1 1 Summary PANIC will use a mosaic of four 2k x 2k HAWAII 2RG arrays from Rockwell now Teledyne in order to cover a field of view of approximately 30 arcmin 3 1 2 Requirements The following section lists the technical requirements for the PANIC Science Detector based on the PANIC Scientific Requirements Ref 01 3 1 2 1 Number of pixels The detector shall have a total of 4096 x 4096 pixels 3 1 2 2 Spectral Range The detectors should be responsive from 0 82 to 2 42 um In the worst case a minimum spectral range from 0 95 to 2 42 um shall be achieved 3 1 2 3 Guiding Since the actual autoguider at the Calar Alto 2 2m Telescope vignettes the FOV of PANIC and it will have to be removed whenever PANIC is attache
75. TA DH 4 DEG HH DEG MU cm D A 0000 FRACTION OF ENCLOSED ENERGY 13 566 HALF WIDTH FROM CENTROLO IH m FFT OLFFRACTION ENSQUAREO ENERGY H 5 WAVELENGTH i POLYCHROMATIC SURFACE IMAGE LEAMERA FOCUS 1 HLL cb hx CONFICURATION 1 OF 1 Figure 3 2 7 2 Montecarlo overlay of the EE80 for the tolerances in the 0 25 px PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 850f 183 It has been presented the tolerances for image quality up to date which shows values that are not too tight if we use the compensator proposed The results are detailed in the ORDS and feed the opto mechanical and alignment strategy of the instrument In the following phase of PANIC a complete image quality error budget will be develop to include thermal errors glass parameters index melt glass homogeneity and surface irregularity and image stability as well and its effect on tolerances 3 2 8 AIV A preliminary optical AIV plan has been made for PANIC A separate technical note OR D describes in detail this complete AIV plan for the instrument and only covers engineering tests regarding the optics We hardly recommend to read it The aim of that document is to determine the procedures and equipment required for integration of the instrument and verification tests These tools will have to be available for the PANIC team as the integration in subsystem and system level will be an in house task
76. TE TP pp Q5 ZHY BOX WIDTH 7 573E BB EEFEFENCE CENTROID COHFIGLUFRRTIOM 1 OF 2 Figure 3 2 6 10 Footprint of the 0 45 px camera FOV on the detector plane 3 2 6 2 4 0 45 px optical performance The Table 3 2 6 lists a summary of the characteristics that describe the performance of PANIC in the 0 45 px scale In this table are the figures of merit that provides a rough idea about the design quality 31 9 x 31 9 Scale at detector 0 45 px 0 45 px Pupil image Cold stop available Mechanical available Pupil image quality lt 10 loss in flux for K band lt 2 loss in flux all bands Optimized 0 95 2 5 um Wavelength range Good transmission from 0 8 um Image Quality EES0 x 2 pixels 36 um 0 90 EESO 29 8 um 0 75 1 7 pix max 1 50 corner 1 32 max corner As much as possible 45 window 9 lenses Gap between detectors 167 pixels minimum Broad band YJHK Broad band zYJHK Filters Narrow band 1 Narrow band 1 Table 3 2 6 Summary of the PANIC performance in the 0 45 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 56 of 183 3 2 6 2 5 0 45 px Ensquared Energy and Spot diagrams The FOV has been sampled from the centre to the external field in a radial configuration following the equal area rule The system has been optimized for the following fields see Table 3 2 7 to cover the complete detector surfa
77. To get an idea of what we have to expect we made some finite element FE calculations We calculated the temperature distribution with maximum filling when pointing to horizon and with an almost empty vessel in the same orientation These are extreme positions which almost never will be used for observation PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 92 of 183 With the full vessel we have a gradient of about 1 5 K the almost empty vessel has a gradient of about 5 5 K A temperature change of 1 K at 80 K results in a change in dimension of about 10 um on 1 m The temperature changes are very slow so that a large effect only happens if the instrument does not move BONS E w i Le AF PESTS AN A KN y daad AU E Figure 3 3 1 4 Temperature distribution with half filled vessel maximum filling pointing to 0 000 20 9 900 m 0 200 0 600 horizon Figure 3 3 1 5 Temperature distribution with almost empty vessel pointing to horizon PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 93 of 183 3 3 1 2 7 Telescope adapter The cryostat is mounted to the telescope mirror cell by an adapter shown in Figure 3 3 1 6 It 1s made from steel and it has two flanges with diameters of 720 mm and 1240 mm which are eccentric by 245 mm The off straight sheet metal cone in between the flanges has a wall thickness of only 1 mm The s
78. US eearri AE UUPA GERE HR RERO AR RERO IR OREMED ds E DDR TAB PHA NU GU PUES 137 E D Ee 2 Conrol sie eire NR 138 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 13 of 183 3 5 3 3 2 3 Readout Electronics ROE nennen enne eene nennen enne 138 3 05 92 e A A 139 EA A e IE O ea daecee ip aoa hence E E 139 DESC A IR mm 139 A o A 139 DS MEE D Dc Y 140 SES MES SS RON T cc 140 A 140 Bedok Hardware TO QUISO Sito 140 EA 140 3 5 2 4 3 1 1 Graphical User Intetface GUD ui 140 DRE MEN i CH Ke RETE 140 o o Oae E A OI PIC ES 140 Nm A A o aedeay eeaucencoumeeans 140 aoka Telescope MERETUR E TTE 140 SENE AES RTE SEA CAVA OO RR T u 140 A 141 3 90990 ao A oom dE tum nem REM iR MM REMEM 141 DAE MEE ic OUI A Eent E 141 35 594 a as MM o UR a 141 O Lis 141 E A A 142 Seer E A y RR 142 ERI SEED D coire We 142 3 9 412 OU SCEIDIS EE 142 Ao Er NO a a nt acest ea E EE E EE 142 E GEIR PUCHA ET 142 ao la Secondary aio OU sonia 142 a A O P 143 cd A E viU la NOTI PqIgsgI rte eter re nr E E eee ere 143 SX DIS EE 143 OL O o DS AP oo E o A nest 143 E O E dera cias 143 Seog Timeline ANC Ee 143 35 34 22 Exposure Time Calculator E 143 3 5 3 4 23 Engineering support 143 S550 E E e E 143 A e DEUM EUM Ue phen cee UIM Eun iiaii 144 3 5 3 5 irre dio Eemere 144 o O i CIE ESI NETTO 144 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007
79. all filters and the other optical elements should be supplied in paper and electronic ASCII Tomat 175 3 6 3 5 3 The drawings of the optics shall be delivered in electronic form in a format agreed upon with CAHA 175 S eS E e 176 S MES PSP In 176 4 MANAGEMEN ies rcc T 178 SEE E RY eer sta 178 2M MEE 0 Uu TAGE ERR oem 178 4 3 LOEB PANIC TEAM ee 179 AA ASSEMBLY AND INTEGRA TION siii dia ia 180 4 5 hu NEO GE 180 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 18 of 183 4 6 COST AND FINANCIAL PLAN EE 181 4 7 SCTE DULT 182 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 19 of 183 LIST OF FIGURES Figure 2 1 Improvement of the photometric precision if a small pixel size compared to the A A eee ene eee 33 Figure 2 2 Observations done with the 3 5m telescope at Calar Alto using the infrared camera Omega Cass and the 0 2 pixel scale The upper panel shows the light curve of a young variable star and the lower panel shows the light curve of a reference star the standard deviation of the second star is 3 millimagnitudes ooooooooooonncnnnnnnnnnnnnnnnnnnnnnnononononononononoss 34 Figure 3 1 6 1 The mosaic assembly plate left and four H2RG s mounted into it right
80. ally Positions P number of images with an exposition time of T Repeats seconds This parameter determines the total exposition time for the target and the final limiting magnitude of the pointing P Positions images are taken at different dither positions Number of Exposures N Perhaps we need for the same dither position also a repeat of exposures at least for the shorter wavelengths where we do not need to get often the current sky sampled multiple exposures at the same dither position will be faster then often dithering and more sure than a very long exposure time It is expected that it should be interesting for a field of acquisition which has also saturated stars to be able to do multiple and perhaps different exposures for the same position to get different dynamic ranges and be able to use it for the resulting deep image result Filter the selected filter PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 161 of 183 e Observation Block An Observation Block OB is the smallest entity that contains all the information necessary to obtain a single observation The changes to one of the parameters of a OB in a given OP do not affect all OBs of the OP Each OB consist of o Target Name Type Epoch RA hr mm sec Dec dec aremin arcsec Proper motion e RA milli arcsec year e Dec milli arcserc year o Sequence Instrument Configurati
81. ance versus signal The noise increases linearly with the flux signal Once the signal level approaches the full well capacity a noise roll over 1s reached due to pixel saturation effects where the noise no longer obeys Poisson s statistics 3 1 7 1 3 Read noise e Spatial read noise measurement Two CDS dark frames each with minimum detector integration time are subtracted from each other pixel by pixel The standard deviation estimated from a defect free region of the resultant frame is divided by V2 and multiplied by the system gain to get the spatially averaged temporal read noise in electrons rms This noise is referred as read noise in a CDS frame Temporal noise A series of dark frames are obtained with minimum detector integration time and without any time interval between individual frames A noise frame in ADU is generated by measuring the noise in every pixel from all the dark frames on a pixel by pixel basis The resultant noise frame is converted into electrons by multiplying by the system gain The result 1s a histogram of the noise frame in electrons The mean of the histogram is the temporal read noise The standard deviation of the histogram shows the noise uniformity The actual MPIA detector readout software GEIRS supports a set of statistical functions to perform these tests Since PANIC detector readout software is based on GEIRS these statistical functions will also be available 3 1 7 1 4 Linearity The mean an
82. ape and dimension The maximum degradation in the pupil re imaging diameter shall be 3 which is less than a 10 loss in flux for K band The central obstruction of the S2 image at the re imaging pupil plane shall be avoid It is not necessary to avoid the structure of the S2 spiders 3 2 5 1 6 Stray light and Ghosts Parent requirements 4 1 5 1 and 4 1 5 2 in RDI 3 2 5 1 6 1 Image Ghost ratio The intensity ratio between a ghost image and its source shall be lower than 1e 4 this means that for a point source at the detector and at the limit of saturation there shall not be a single ghost structure contributing more than 6 counts 3 2 5 1 6 2 Individual Ghost diameter The diameter of any individual ghost shall be larger than 10 in case the requirement of Image Ghost ratio is not fulfilled 3 2 5 1 6 3 Stray light The total stray light shall be minimized 3 2 5 1 7 Band passes Parent requirements 4 1 6 1 4 1 6 2 and 4 1 6 3 in RDI PANIC shall be designed to allow use of broad and narrow band filters PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 470f 183 3 2 5 1 7 1 Broad band filters Filters shall be provided for Y J H and K bands A z filter should also be provided 1f the 0 82 2 42 um range is achieved 3 2 5 1 7 2 Tolerance for narrow band filters Parent requirement 4 1 6 3 in RDI Since the narrow band filters have widths on average of 1 of the
83. arger cryostat with thicker walls requiring additional Nitrogen because of increased heat input We are currently testing the performance of the telescope with additional weights A design with only one pixel scale is also presented this clearly avoids the weight problem and exceeds the torque only slightly and the mechanical tolerances are relaxed PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 28 of 183 2 SCIENCE CASES We list below potential scientific cases that would benefit from the panoramic imaging mode of this camera More details for some of them can be found in the Phase A document section 2 A non exhaustive compilation of science cases that would benefit from the other TBC observing modes 1s also given 2 1 Extragalactic Astronomy 2 1 1 Extragalactic Surveys Cosmic evolution in the z range 1 5 2 0 can be studied through surveys of specific areas in the sky in the clean windows of z and J bands which enormously reduce the background sky contained in the OH lines originated in the high levels of the atmosphere as compared with the corresponding broad band filters Photometric redshifts would then be systematically derived in the so called redshift desert A wide field survey covering the SDSS area not contained in the UKIDSS LAS would provide highly resolved NIR images of the local galaxy population including studies of bars lopsidedness population gradients and
84. arnings Run Obs Program now Sent Script Commands to GEIRS Server Submt OP into Repository Figure 3 5 4 6 OT Workflow 3 5 4 6 5 The Observation Tool Editor As a main GUI component the observation tool editor will be implemented containing three main areas a button frame on the left side a navigator area on the middle which shows the components in a hierarchical structure and editors for each observation component on the right side This seems to be a natural design since a OP has a hierarchical structure This structure is show in the next figure PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 164 0f 183 PANC Observing Tool A a Buttons Navigation Component Frame Frame Frame Contains View Editor for current selected item Hierarchical view in the Navigation Frame The GUI tool varies of OP depending on the item type components Figure 3 5 4 7 Browser interface Conceptual Diagram 3 5 4 6 6 Programming language and components The programming language will be the Java language based on the Java Virtual Machine which has a great deal of power and flexibility The Observing Tool will extensively use the classes that are part of the JSky Java Components for Astronomy Project started at ESO That tool is freely available for the community 3 5 4 7 Quicklook description 3 5 4 7 1 Purpose When observing with infrared
85. assembly plate This mosaic integrates four HAWAII 2RG arrays as separate modules into one single thermal and vibration stable structure allowing precision alignment and physical flatness between all 4 detectors The following figure shows a picture of the detectors mounted into the mosaic package followed by a table with the major characteristics of these detectors PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 38 of 183 Figure 3 1 6 1 The mosaic assembly plate left and four H2RG s mounted into it right Courtesy of Teledyne Scientific and Imaging LLC Table 3 1 6 1 H2RG Major Characteristics Parameter Specification 2048 x 2048 100 kHz to 5 MHz 32 2 guide window Charge storage capacity gt 100000 e Read noise CDS Quantum efficiency Dark current lt 0 1 e sec Spectral range 0 3 2 5 um Pixel operability 2 95 Operating temperature lt 4 mW 100 kHz 350000 each The mosaic package and the science detectors are already ordered A Bare Multiplexer and an Engineering Grade detector will also be available for test purposes PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 39 of 183 3 1 6 2 Requirements verification The following section presents the calculations needed to determine the feasibility of the critical technical requirements So far the most critical requirement regarding the detect
86. asses are located in the corresponding centre of gravity In the following the deformation of the instrument by gravitational forces is shown for both horizontal and vertical telescope pointing horizon and zenith PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 107 of 183 0 00 250 00 500 00 mm 125 00 375 00 Figure 3 3 2 15 Both optics assemblies have been replaced by point masses the rest of the cryostat is not shown 3 3 2 2 7 1 1 Telescope pointing to zenith The maximum deformation of the optical bench due to bending is 0 094 mm The effect on the optical components has to be further investigated Figure 3 3 2 16 and Figure 3 3 2 17 show both the same results although in Figure 3 3 2 16 the cryostat is not shown PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 108 of 183 X 0 00 250 00 500 00 mm 125 00 375 00 e Figure 3 3 2 16 Displacement of cold bench with the telescope pointing to zenith gravity vector in z direction 0 00 600 00 mm SCH 8 150 00 450 00 Z Figure 3 3 2 17 Cryostat displacement with the telescope pointing to zenith gravity vector in z direction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 109 of 183 3 3 2 2 7 1 2 Telescope pointing to horizon The maximum absolute displacement of the bench with respect to the telescop
87. ating would decrease the intensity ratio about one order of magnitude If finally we would decide to avoid the ghost 2 and or 5 it 1s possible to change a little the ROC of the lenses involved in those ghosts 3 2 7 Tolerance Analysis A preliminary study of the tolerances for PANIC has been done In a separate technical note ORDS it is described Tolerances need to be defined for optical manufacturing position accuracy during assembly and stability during operation The nominal criterion to evaluate the acceptance of the degraded system is the half EE80 lt 2px 18um for the 0 45 px and the half EE80 x 3px 27um for the 0 25 px 80 The system has been evaluated in terms of the rms spot radius at five fields FOV centre and 4 external situated at 9096 of the FOV corner and in three wavelengths to cover the complete spectral range The tool used to verify the fulfilment of the criterion has been the Overlay Montecarlo during the tolerances runs The tolerances for the elements and sub systems are done for the following features For the elements fabrication has been tolerated the folding mirrors are included the ROC of the two surfaces front and rear in the case of flat surfaces it has been tolerated the flatness in fringes the thickness of the element except for the mirrors and the wedge of the element And for the barrels and the whole instrument has been tolerated the position in the axial directio
88. ation sequence defined by the user taking into account the overheads and delays That estimation should be available before any start of observation at the instrument 3 5 3 4 22 Exposure Time Calculator The OT should integrate an exposure time calculator in order to estimate exposure times The total integration time should be taken and automatically divided into several exposures 3 5 3 4 23 Engineering support The OT should provide templates and observation blocks for engineering purposes during the different stages of the instrument development integration commissioning maintenance The necessary engineering tests should be packed at commissioning time into maintenance OBs for easier verifications 3 5 3 4 24 Errors amp Warnings The OT should handle errors reported by the systems controlled by it It will pause the observation in execution in response to such errors and report the error to the user Warnings shall only be reported to the user in a suitable way Both Errors and Warnings shall be written into the log file PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 144 0f 183 3 5 3 4 25 Repository The OT should allow to submit the observation definitions and user defined templates as XML files to a repository through the net A submitted observation could be retrieved and modified later 3 5 3 5 Quicklook Tool 3 5 3 5 1 General requirements The quicklook operat
89. by the current two pixel scale design Since we do not see a way to reduce weight or to reduce the distance between the centre of gravity and the telescope flange while keeping the same instrument performance the only possibility seems to be to have only one pixel scale In this case the optics wheel and the rotating field stop mask would not be necessary anymore and the cryostat could by significantly smaller Figure 3 3 2 27 and Figure 3 3 2 28 show the design of the instrument with one pixel scale Table 3 3 7 shows a mass estimate for this option PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 118 0f 183 UDS Figure 3 3 2 27 Section of the one pixel scale design similar to Figure 3 3 2 1 Figure 3 3 2 28 Cold bench and optics of the one pixel scale design similar to Figure 3 3 2 2 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 119 of 183 Patorunt mass kg Cryostat oS d S O NF NN ee LN half filling 35 Optics and Opto Mechanics NENNEN A Detector Package E WE Electronics O 0 0 0 0 0 E A Cabling rack Miscellaneous screws cables etc Contingency Sum 385 Table 3 3 7 Overall mass estimation of PANIC with only one pixel scale It is obvious that even with a one pixel scale design the original ZEISS limit is exceeded The weight is less than the CAFOS limit the moment of 2000 Nm is slightl
90. camera with GEIRS GUIs and commands It shall log all commands and maintenance relevant logging levels with the timestamp 3 5 3 3 1 Hardware minimum requirements The computer system PC shall e use a 64bit PCI data interface for the detector data read out to be able to read the expected max data rate of 256 Mbytes sec peak and 250 Mbytes sec mean This data speed arises from the number of 16bit data channels 128 the maximal clocking speed 1 MHz and the subtraction of some overhead for example line reset lt 10 microseconds of 2048 lines per channel e have multiple CPU cores on probably at least 2 processor sockets to support the concurrent multiprocessing and multithreading of tasks of all software parts e have about 16 to 32 Gbytes of RAM to allow the buffering of a single data sequence which is done by the detector read out electronic ROE with a single trigger and to have additionally enough space for caching of disk transfers The 16 Gbyte RAM will allow to buffer a single integration count of an exposure of double correlated images of about 125 for full frames about 340 sec of min integration time at 100kHz pixel clock and 11000 for the 36x36 window size about 11 sec of min integration time at 1MHz pixel clock Always all rawdata from the detectors are buffered e not delay the optimal efficiency for the detector usage This is also supported by the double exposure buffering logic of GEIRS e have multiple hard d
91. ce 0 266 0 266 38 30 38 30 Table 3 2 7 Fields used in the 0 45 px scale The origin of coordinates 1s the centre of the detector mosaic The second column is the fields on the sky and the third column is the coordinates at the detector plane At the detector plane the image spots analyzed are located in the coloured points that shows the Figure 3 2 6 11 The box indicates the total size of the whole detector including gap of 167 pixels between detectors 1 8200 1 8900 s 2 4000 76734 00 SURFACE IMA CAMERA FOCUS FULL FIELD SPOT DIAGRAM NOMINAL INSTITUTO ASTROFISICA ANDALUCIA UNITS ARE ja RMS RADIUS 3 9E 001 GED RADIUS 5 5E 084 PANIC _Vil_TP_ 4S_MULTIBAN ZMX BOX WIDTH 7 673E 884 REFERENCE CHIEF RAY CONFIGURATION 1 OF 6 Figure 3 2 6 11 Complete FOV of the 0 45 px The performance of the design is evaluated at the wavelength and bandwidths shown in Table 3 2 8 Notice that the design has been optimized to this bands except the z band The requirement for z band is not optical quality 1t is only for transmission in this band Instead of PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 57 of 183 this 1t can be seen that there is optical quality in z band so the system 1s able to work in this photometric band As the filters will be placed in convergent beam 1t has been decided to simulate them by inserting a plate of IR fused s
92. ceives the data sent by the ROCon Receiver 1 and 2 parallelizes the data stream and writes it to the corresponding FIFOs If an adjustable threshold is reached a DMA request is produced and the data is written to the memory of the PANIC workstation Receiver 1 Fiber 1 En FIFO 1 i SES EE ER B PCI 64 bit 8 66MHz Figure 3 4 1 5 OPTPCI block diagram The OPTPCI should be installed in a PCI slot with 64 bits 66MHz to reach the maximum data rate of approximately 250 Mbytes per second However the OPTPCI can be run in a PCI slot with 32 bits 33 MHz This will reduce the achievable data rate to approximately 100 Mbytes per second PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 125 of 183 3 4 1 3 6 CA36 36 channel cryogenic preamplifier The CA36 board translates the detectors single ended output signal to a differential signal TVCC Out1 Y Figure 3 4 1 6 single channel of the CA36 board There are four preamplifier boards in the cryostat located close to the detectors The schematics for the CA36 are done but due to missing information from Teledyne formerly known as Rockwell and missing information of the mechanical details the cryogenic preamplifier board cannot be layouted at the moment 3 4 1 3 7 Power Supply The ROE in this configuration needs two supplies of 5 volts One supplies the digital circuits of the ROE the second supplies the analog circu
93. central wavelength of the filter the maximum shift allowed for this central wavelength shall be 0 396 3 2 5 1 8 Field distortion requirement Parent requirement 4 1 8 in RD Field distortion shall be less than 1 5 from the field centre 3 2 5 1 9 Transmission Parent requirements 4 1 6 1 4 1 6 2 and 4 1 6 3 in RD There is no number requirement defined for the transmission of PANIC There is only the goal to be as high as possible to optimize the materials to maximize transmission in the 0 95 2 45 um range and to work in the z band from 0 82 um 3 2 5 1 10 Environmental conditions Parent requirement 5 3 in RD PANIC shall be designed to operate and have optical quality under cryogenic conditions temperature 80 K and vacuum 3 2 5 1 11 High resolution mode Parent requirements 4 3 in RD Requirements 3 2 5 1 2 3 2 5 1 5 3 2 5 1 6 3 2 5 1 7 3 2 5 1 8 3 2 5 1 9 and 3 2 5 1 10 apply to this mode 3 2 5 1 11 1 Pixel scale A second pixel scale of 0 25 pixel shall be implemented in PANIC 3 2 5 1 11 2 FOV PANIC when observing with the 0 25 px scale shall have a FOV of at least a circle with a diameter of 8 arcmin The goal is a FOV with a diameter of the circle inscribed in the detector dimension which is a diameter of 17 76 arcmin 3 2 5 1 11 3 Image quality The image quality shall be such that an 80 of the energy is ensquared EE in a 0 75 3 pixels over the full FOV for each of the broad bands
94. d in a 19 inch 7 height units case whereas the new ROE is housed in a 13 inch 3 height units case PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 121 of 183 Figure 3 4 1 1 new ROE left versus old ROE right The left side in Figure 3 4 1 1 shows the new ReadOut Electronics the right side the former one The new development was started in summer 2006 The complete ReadOut Electronics consists of the following electronic boards e ROCon ReadOutController e AD36 36 channel analog to digital converter e H2RG CB HAWAII2RG Clock Bias board e BP6 6 slot backplane connecting the above three boards e OPTPCI feeds the data from the fiberlink to the PCI bus e CA36 36 channel cryogenic preamplifier All boxes boards and cables are specifically designed and built according to the EMC criterion for more information refer to IEC EN 61000 4 The central board of the new ROE is the ReadOutController ROCon It generates the pattern needed for clocking the detector and has circuitry for data transmission via fibers The Clock Bias board transforms the clocks from the ROCon board to the levels required by the detectors and generates programmable detector supply voltages The AD36 board has 36 analog to digital converters with 16 bit resolution and a sampling rate of 1 million samples per second The AD36 boards are connected to the detectors via CA36 cryogenic preamplifier boards The co
95. d or median output signal vs integration time is measured and plotted The output signal in ADU is converted into electrons by multiplying it with the system gain PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 42 of 183 A least squares fit to the data from 10 to 80 of the full well gives the linearity behavior 3 1 7 1 5 Persistence and cross talk Will not be measured at MPIA 3 1 7 1 6 Quantum efficiency This test will not be performed Values will be taken from the manufacturer s data sheets 3 1 7 1 7 Flatness The flatness of each detector s surface will be measured by means of a triangulation method using an xy stage to map the detector area MPIA owns such an xy stage and it will be used to perform the measurements 3 1 8 Handling storage and transportation The main purpose of this section is to describe a series of safe procedures that shall be followed when handling the science detectors during acceptance delivery inspection storage transportation integration and maintenance 3 1 8 1 Electrostatic Discharge Detectors can be damaged by ESD The science detectors shall be handled only in an ESD protected area MPIA counts with integration halls and dedicated labs in which ESD protected conditions are fulfilled 3 1 8 2 Clean room conditions The detector should be handled under clean room conditions class 10000 For assembly and integration the det
96. d to the telescope the detector shall support fast readout rates in order to implement a guiding mode using a subframe of the detector 3 1 2 4 Flatness The physical flatness of the detector should be better than 40 um peak to valley from the best fit plane in order to avoid image degradation 3 1 3 Introduction The selection of the science detector was mostly based on cost availability and of course technical requirements There were 3 options investigated the 2K x 2K VIRGO detector from Raytheon the 4K x 4K new development from Teledyne and a mosaic of four HAWAII 2RG detectors also from Teledyne The HAWAII 4RG Teledyne s new development was discarded at an early stage of the project because of cost and risk The capital cost of the project would have increased in approximately 0 4 MEuro and the array was only at a design stage On the other hand the VIRGO detector was more expensive than the HAWAII 2RG and since MPIA has gained a lot of experience working with Teledyne detectors it was decided to use a mosaic of four 2k x 2k HAWAII 2RG arrays These arrays were also preferred because they have a special guide mode in which a programmable window may be read out continuously at high pixel rates for stable tracking of guide stars allowing interleaved readout with the full frame science data PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 36 of 183 3 1 4 Scope T
97. da 20 the upper limit for the RMS deflection would be max RMS deflection 0 8 um 20 40 nm CH ES 0 3 5e 004 7e 004 um 1 75e 004 5 258 004 Figure 3 3 2 24 Deformation of mirror M1 due to gravity in z direction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 114 of 183 3 3 2 2 8 Error budget The error budget calculation for the optical elements and groups see section 3 2 shows critical decentre values for the lenses L5 and L6 0 45 arcsec px and for the tilt of lenses L1 L2 L4 L5 and L7 Realistic values from a manufacturing point of view are 25 um for decentre and roughly 60 arcsec for tilt for a 100 mm diameter lens The most difficult requirement however is the decentre value of the optics wheel The decentre of the lens group L5A to L8A 0 45 arcsec pixel must not exceed 39 um The following list shows several potential decentre effects of this group and their expected values a Positioning accuracy of the wheel due to gear transmission errors The transmission accuracy of the Harmonic Drive gear HD14 100 1 is less than 2 arcmin With a distance between the optical axis and the axis of rotation of 140 mm the positioning accuracy of the optics is 80 um b Positioning accuracy of the motor The Phytron stepper motor needs 200 steps for a full turn With a gear transmission ratio of 100 1 one step of the motor gives a rotation of the wheel of 1 08 arcm
98. dg RAY Y MIN car dr rea RAY Y MAS rr DE PANIC V1 COHPLETE_TP_TAHA DE Hx LEO EADIUS 4 BC Ann PANIC U1 COHFLETE_TP_TAHA 05 Hx OF 2 MAX RADIUS 38 5464 WAVELENGTH ALL CONFIGURATION 2 OF 2 BOX WIDTH 7 573E 88 4 REFERENCE CENTROID CONFIGURATION 2 Figure 3 2 6 23 Footprint of the 0 25 px camera FOV on the L8B left on the detector plane right 3 2 6 3 4 0 25 px optical performance The Table 3 2 13 lists the characteristics that describe the performance of PANIC in the 0 25 px scale In this table are the figures of merit that provides a rough idea about the design quality PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 65 of 183 EESO x 3 pixels 54 um 0 75 EESO 41 4 um 0 58 2 3 pix max Transmission 43 window 10O lenses Table 3 2 13 Summary of the PANIC performance in the 0 25 px scale 3 2 6 3 5 0 25 7px Ensquared Energy and Spot diagrams The FOV has been sampled from the centre to the external field in a radial configuration following the equal area rule The system has been optimized for the following fields see Table 3 2 14 to cover the maximum circle inscribed in the detector dimension X Y coordinate mm Table 3 2 14 Fields used in the 0 25 px scale The origin of coordinates 1s the centre of the detector mosaic The second column is the fields on the sky and the third column is the coordinates at the detector
99. dimensions axis x y windows of identical size detector time In case of multiple windows of different sizes multiple FITS files are created each of the according window size x y detector time as special case the original raw data as buffered in the shared memory can be dumped directly into a lt name gt dump file An header file is also be written in the FITS header format as lt name gt info file All these file structures have the advantage of easy writing the FITS file immediately and parallel to the incoming data arriving in the same order In a FITS file should only be data of a single exposure That means dithered data will not be in a single FITS file because each dithering is a new tele position and a new exposure 3 5 3 7 5 Archive and VO 3 5 3 7 5 1 Archiving Following Scientific Advisor Committee SAC recommendations the PANIC data should be compliant with the future CAHA Archive implementing when the Archive 1s defined the necessary modules to support it and to allow data retrieval and data queries in concordance with the pipeline outputs 3 5 3 7 5 2 Virtual Observatory The PANIC Archive should be VO compliant 3 5 3 7 5 2 1 VO data model A data model for PANIC should be defined for VO integration 3 5 3 8 Caha Sw Requirements The section 3 6 3 about CAHA technical requirements includes some specific requirements concerning the software So they complete the software requ
100. e PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 63 of 183 c ops MILLIMETERS MILLIMET oo b s PEPA d oo 100 00 100 090 APERTURE OIRMETER 162 4335 Y RAYS THROUGH 84 68 APERTURE OIAMETER 152 7713 X RAYS THROUGH FOOTPRINT DIAGRAM FOOTPRINT OIAGRAM 0 25 INSTITUTO ASTROFISICA ANDALUCIA Y 25 INSTITUTO ASTROFISICA ANDALUCIA SURFACE 19 L1 CONCHI CRHRDENRS sugrRCE 21 L2 CONCHI CARDENAS RAY X MIN D RAY X MAX 60 6846 RAY X MIN 528 6587 RAY X MAX S8 65987 RAY Y MIN 6 RAY Y MAX 68 6846 PRNICI VI COMPLETE TP TRMR OS zMx RAY Y MIN 58 6587 RAY_Y MAX 58 6587 PRNICI V1 COMPLETE TP TRMA 0S ZMX MAX RRDIUS 63 WAVELENGTH ALL CONFIGURATION 2 OF 2 MAX RADIUS 61 2569 WAVELENGTH ALL CONFIGURATION 2 OF 2 gt ES E RS WE LEEPER EF a PERA kt MILL IMHE MILLIMETERS mp CI AA BN ee LiL pp 1a PEF ee am da a ad EUER ee a FARRER RRB T a F Sd SR Ge a eee REL UE St P hae AAA AAA mm na auum s ar an b LUE RUE CHE am d db dl db d EL Go WA GR RR Sr xw op 146 4000 ud dem s RE ER a 100 090 GELEET RRR a E eee TT Tr ER Sg CT ee a TT a woe d ED RRR A RAD A ALE Le HPERTURE DIAMETER 146 1259 RATS THROUGH 84 65 APERTURE OIRMETER 116 536 X RAYS THROUGH FOOTPRINT DIAGRAM FOOTPRINT DIRGRRM 0 25 INSTITUTO ASTROFISICA ANDALUCIA 0 25 INSTITUTO PSTROFISICA ANDALUCIA SURFACE 23 13 CONCHI CARDEMAS suerace 25 Ly CONCHI CARDEN
101. e with the telescope pointing to horizon is 0 120 mm This can be split into a radial displacement of about 0 070 mm and a tilt of about 4 8 arcsec q 0 00 250 00 500 00 mm 125 00 375 00 Figure 3 3 2 18 Displacement of cold bench with the telescope pointing to horizon gravity vector in y direction Y 0 00 350 00 700 00 mm 175 00 525 00 0 Figure 3 3 2 19 Cryostat displacement with the telescope pointing to horizon gravity vector in y direction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 1100f183 3 3 2 2 7 2 FEM simulation of a detailed model In this simulation the point masses of chapter 3 3 2 2 7 1 were replaced by detailed models which use the optics mounts lenses mirrors and wheels By this the displacement and tilt of each individual optical element and optical group due to gravity can be investigated Table 3 3 5 summarizes the simulation results All values are absolute values with respect to the telescope flange The tilt and shift values for individual lenses and mirrors as well as the lens mounts as described in Table 3 3 1 in respect to their corresponding units are very small and can be neglected Optical dd Remark ul bench shift direction Telescope pointing to horizon 77 um y Telescope pointing to horizon 80 um x z Telescope pointing to zenith 30 um C Table 3 3 5 Tilts and displacements of optical bench and optical gr
102. e additional mount parts which can be moved by micrometer screws Figure 3 3 2 25 shows how this could look like for L2 Lens L2 is mounted to a ring which can by moved along a groove in x direction by a pair of micrometer screws e g Mitutoyo 148 207 An intermediate ring can slide in a groove of lens mount 2 in x direction controlled by another pair of micrometer screws This design allows to adjust the lens decenter in both directions independently Once the correct position is found both rings can be fixed by M3 screws through access holes in the ring in front of them PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 117 of 183 3 3 2 2 9 Total weight limit and possible solutions An overall mass estimation of PANIC is given in Table 3 3 6 The total mass is 463 kg With the centre of gravity located about 630 mm away from the telescope interface flange the instrument adds a moment of about 2530 Nm to the telescope assuming that most of the electronics is mounted close to the mirror cell of the telescope EE O masso o oo oo Cryostat a ss sisi n o Ta causter tom CAD mesa LN half filling 461 28 7 Optics and Opto Mechanices Detector Package Electronics ll O Contingency S Contingency Estimated 453 Table 3 3 6 Overall mass estimation of PANIC with two pixel scales So both the weight and the moment limit of the 2 2m telescope are well exceeded
103. e encase eee 87 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 11 of 183 A A M 88 3 3 1 2 2 Nitrogen vessel for cold bench coolmg eene n nnn nnn nnns 88 3 3 1 2 3 Nitrogen vessel for detector cooling oooooccococcncnonononnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnos 89 NS NN E MER OL gt OPE A ee ee re ee eee eee ert eee ee ere meee ee 89 3 3 1 2 5 Thermal connection of the detector eene n E KE S EKn TE nnne 90 35 3 L2 5 VThermal10y 6 SUP eier dereen degen 91 3 3 1 2 6 1 Nitrogen vessel for cold bench w sc ccccccceccsceeseccntesscncneneazsasndndasdesnenesecanetansedantensaassdanseneeresneansne 9 3 3 1 2 6 2 Nitrogen vessel for detector coolmg nennen eene 91 o A EMI is TNT 91 Alu Tee one AC Ap Maeght A A 93 SG OUI NN 94 e CNR Ee 94 a ESOS DO e 94 Sd a Ae OOO a O no A RUN EREU NM QAM cans cence MEM GU IM EO DEUM 96 3 3 2 2 Mounting of cryogenic lenses and mrorg nn nnnnn nn nn rn nnn nnns neis 97 o AOS eo LU bai 100 SE ME It 103 3 9 2 2 Rotating field OP unan 105 900220 E Ee aaa ao 106 Sd SEENEN 106 3 3 2 2 7 1 Simulation of cryostat with optics replaced by point masseg 106 3 3 2 2 7 1 1 Telescope pointing to zenith ccccccccnnnnnnnnnnnnnnnnnnnnnnnninnnnnnnnnnnannnnnnnnrnn nr nn enne nennen nennen 107 3 3 2 2 7 1 2 Telescope pointing to NOrZOM 2c cc ccccccicccecdssesescadseseecsdseaiecesteseesiasaseecsdes
104. e for a Lyot stop at the telescope image pupil placed at the primary mirror 3 2 3 Scope The Preliminary Optical Design is described in this optics section 3 2 4 Simulations The PANIC optical design has been developed using ZEMAX EE Version January 2007 The model includes the optical components of the 2 2 m telescope The optical surfaces are defined with respect to the optical axis which is always parallel to the Z axis of the local frame of reference by the optical design program The distance between optical surfaces is measured along the optical axis and it is defined by a thickness parameter 3 2 5 OPTICS Requirements This section summarizes the Requirements established imposed by the science goals and the Technical Requirements that derivate of the operational conditions and design choices A separate document describes the Science Requirements RD1 for PANIC PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 45 of 183 The Table 3 2 1 summarizes the General Specifications for PANIC 0 45 arcsec pixel Pixel scales 0 25 arcsec pixel Direct Imaging Over the whole FOV Pupil image available Cold stop 0 95 2 45 um with IQ Wavelength range 0 82 0 95 um able to transmit Broad band z YJHK Filters Narrow band 1 System focusing mechanism Telescope S2 Table 3 2 1 Summary of the PANIC General Specifications The optical system is a monobeam design all r
105. ector should be handled in a laminar flow area 3 1 8 3 Detector handling The handling of the detectors is restricted to well trained persons Only persons with permission from MPIA are allowed to handle the detectors The handling of the detectors is only allowed with sufficient ESD protection equipment The detectors shall not be cleaned In case cleaning is necessary contact the responsible person at MPIA Avoid any mechanical shock to the detectors and mosaic package PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 43 of 183 3 1 8 4 Storage The detectors must be stored in their original case under correct environmental conditions Temperature the storage temperature must be between 50 K and 310 K 220 C and 30 C Humidity the case shall contain humidity absorbent materials Only qualified people shall have access to the storage cabinet 3 1 8 5 Transportation The detectors must be transported in its original case The previous rules must also be fulfilled during transportation For transportation across countries ensure that all custom regulations are fulfilled Before shipping the detectors contact the responsible person at MPIA PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 44 of 183 3 2 Optics 3 2 1 Summary This optics section contains a description of the PANIC Preliminary Optical Design The repor
106. eees 135 Table 3 5 1 Expected image rates compared for the subwindow size of 36x36 read pixels asked a MR Mo a E ahaa esas 156 Table 3 5 2 Table with expected read noise suppression in case of limitation by read noise instead of Dac TOMA ito 156 Table 3 5 3 Some estimated timings for multiple guiding windows embedded between normal ic MACS scoscasssensodectcototandantesensnniaetusosneasatonieniadsiiesoadentgasuonhedeatabendundontecandas 157 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 25 of 183 1 PANIC GENERAL 1 1 Introduction The greatest strength of the Calar Alto observatory is its up to date instrumentation Whereas the 3 5m telescope is well equipped with modern instruments the 2 2m telescope is lacking modern instrumentation an exception is the lucky imager Astralux but this is a special purpose instrument for a limited range of applications A survey on instrumentation wanted for Calar Alto at MPIA and IAA came independently to the same result 1 e a NIR 0 9 to 2 5 microns imager for the 2 2m telescope It is obvious that an instrument with a single 2x2 k detector is not state of the art so a mosaic of 4 detectors was envisaged Science applications would obviously be wide field gt 1 square degree imaging and surveys but a collection of ideas at AA and MPIA showed that there are many very interesting applications also for single pointed observations The Calar
107. efractive being the only mirrors of the system the ones used for folding and packaging The design has not been required to have an internal collimated beam 3 2 5 1 GENERAL REQUIREMENTS 3 2 5 1 1 Pixel scale Parent requirement 4 1 1 in RDI The optimum scale shall be 0 45 pixel 3 2 5 1 2 Wavelength range Parent requirement 4 1 2 in RD PANIC shall work in the wavelength range 0 95 2 42 um and should work in the range 0 82 2 42 um 3 2 5 1 3 Image quality Parent requirement 4 1 3 in RD The image quality shall be such that an 80 of the energy 1s ensquared EE in a 0 9 2 pixels over the full FOV for each of the broad bands PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 46 of 183 3 2 5 1 4 FOV Parent requirements 4 1 1 and 5 4 1 in RDI PANIC when observing with the 0 45 px scale shall have a FOV of at least 30 arcmin x 30 arcmin 3 2 5 1 5 Pupil re imaging quality Parent requirement 4 1 4 in RDI A separate Technical Note ORD2 describes in details the signal to noise study for PANIC and imposes the following requirements in the pupil quality 3 2 5 1 5 1 System pupil The PANIC pupil has to be placed at the telescope primary mirror S1 3 2 5 1 5 2 Accessible pupil image The Optical design shall provide an accessible pupil image so that a suitable cold mask shall be used to minimize stray thermal radiation 3 2 5 1 5 3 Pupil sh
108. electronics This includes temperature and pressure sensors temperature controller for the detector controller for the wheels This will be build by MPIA e Integration lab tests MPIA has the facilities for this so these work packages will be done at MPIA IAA will participate e Observation tool data retrieval pipeline archiving this will be developed by IAA The experience during the first year of cooperation is excellent and shows that this division is very reasonable PANIC PRELIMINARY DESIGN REPORT Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 Page 179 of 183 4 3 The panic team The following people form the PANIC team Mathias Alter Harald Baumeister Concepcion Cardenas Josef Fried Jens Helmling Jose Miguel Ibanez Julio Rodriguez Werner Laun Ulrich Mall Marcos Ubierna Matilde Fernandez Jose Ramos Ralf Rainer Rohloff Clemens Storz Vianak Naranjo Karl Wagner Control Electronics Design Optics PI Calar Alto feedback Software Project Management Cryotechnique Read Out Electronics Design CoPI Science Read Out Electronics Design Software Detectors Electronics Former team members Lourdes Verdes Montenegro and Bernhard Grimm PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 180 0f 183 4 4 Assembly and integration The logical place for lab tests assembly and integration of PANIC is clearly MPIA since the ha
109. er the filters for the 0 25 px camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 71 of 183 3 2 6 5 Stray Light In order to minimize the stray light in PANIC in this stage of the instrument design we have done the following considerations from the point of view of the Optics and Opto mechanics The opto mechanics design of PANIC has implemented an optical labyrinth in both optical assemblies and all the system 1s encapsulated to minimize stray light effects and the light interaction between both scales The optical design of PANIC A Has been baffled with the two naturally stops the field stop and the pupil stop They are explained respectively in 3 2 6 5 1 and 3 2 6 5 2 sections B All the lenses have been over dimensioned a 5 over their clear aperture in order to avoid stray light coming from the lens edges C The contribution in the stray light due to the ghost has to be minimizing taking into account the ghost analysis in section 3 2 6 6 D The micro roughness of the lenses and mirrors surfaces will contribute in the total amount of stray light So the aim of the design has been not use diamond turned surfaces In this way first there is not any aspheric surface in the optical design of PANIC and second we propose to use gold coated glass folding mirrors to reduce imaging errors and scattered light A complete stray light analysis will be done in the followi
110. es Po On omens sosaesad cet becmesaemetebecensemeemeer peemesoeneers 35 TS S 00007000 AAA e E E E E A E E 35 SE COG AP y 5 o 36 S e e CANON sire 36 3 1 5 1 rme Ke 36 AA dr A Pe paenctencte euch eneccececheneens poeccreascecenecce 36 5 1 5 2 E and Spectral ET 36 ISLS et ee 36 L P E A 36 Ge Ar OT D ee ege 36 EN EE Ro O E 36 E M Kurt EE 36 SN MEE e E 36 E APU usse etras eraslsste atlbx ustatantu instet oU A E E cr e D de Ende DEM REN Ed UNE 36 ILLI Venue Sr ETT m T 37 LLA Temperature Cuca IOD sou erate cedars piece ta iia 37 DN DN e COOMAG Wii and Warm UB E 37 Sl a A M dad 37 Sl WE OSibrapedompetature e EE 37 alo DESC Ee E 37 s e lo Pat EO PR O o coeunt io et tees be sube oue Dip DM cd COS eee 37 ENS VOS MEME 1 E E ee ere eee ne rT erry ee ere ey ene ere ee eee er 37 CNN A m 37 A 37 3 1 6 1 SCICMCE Bio O m A EE aa secncmoneponeesqucnencoce EE 37 3 1 6 2 Requirements verficeaton ono nono nono nono nono nono nono nono nono nn nn nennen enne ene naar nennen eene 39 3 1 7 EE EI PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 9 of 183 3 1 7 1 jc e ORO A Q 40 3 1 7 1 1 Detector sensitivity and system gan 40 SN PLN MEE DUBIE NINE IET mE 4 SNP MEE ET 41 AE o E 41 24 7 15 o o RM A ING 52 oc cei acedecntnduedasoncemecmsecuiedentecemsmescmecsesadenctunes A NU uU RUE DU URURUD s
111. es are on the order of a few tens of seconds narrow band imaging clearly requires guiding At least in the beginning it is sufficient to select the guide star manually by clicking on it an automatic routine might be implemented later on The guide star should not be lost during a dithering sequence and guiding should continue automatically on the new position 3 5 3 4 Observation Tool OT 3 5 3 4 1 Functionality The OT should allow access to all of the astronomical observing functionalities of the instrument 1 e for normal astronomical observing it should not be necessary to access any engineering functionality of any other system 3 5 3 4 2 Hardware requirements The OT shall have a PC with enough CPU to run the Java Virtual Machine at least 1 GByte of RAM and a hard disk with at least 20 GByte of available space The OT should be able to run on the same GEIRS PC 3 5 3 4 3 External Interfaces 3 5 3 4 3 1 Graphical User Interface GUI The OT shall be a PANIC high level control based on a GUI which shall allow the users to make the observations in a simple and user friendly way 3 5 3 4 3 2 Hardware Interfaces No hardware interfaces are required for OT 3 5 3 4 3 3 Software Interfaces 3 5 3 4 3 3 1 GEIRS Interface OT shall have a well defined interface with GEIRS This interface will be based on the current GEIRS command server interface Likely some new internal commands between GEIRS and OT will be needed 3 5 3 4 3 3
112. etector has to be slower than 0 5 K min 3 3 1 1 2 Cooling system The cooling system should be convenient to use on Calar Alto This means that it should run at least one observing night without any maintenance service or any other interrupt Refilling should be necessary only once a day 3 3 1 1 3 Flexure The flexure of the cryostat due to the movement of the telescope has to meet the requirements defined by the optics 3 3 1 2 Design Report The cryostat is a nitrogen bath cryostat with a large vessel to cool the complete structure To reduce LN consumption and thermal gradients we use 30 layers of multilayer insulation MLI on the cold surface This should reduce the heat load from radiation to about 5 W m For a constant detector temperature we use a second small LN vessel exclusively to cool the detector For weight reduction we will use dished ends on the vacuum can instead of flat thick walled plates PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 88 of 183 Entrance window Vaccum vessel upper part Nitrogen vessel Central ring Optical bench Nitrogen vessel for detector Radiation shield Vacuum vessel lower part Figure 3 3 1 1 PANIC cryostat setup 3 3 1 2 1 Vacuum can The vacuum can consists out of 3 parts There is a central ring where we have the cold warm connections to the optical bench with spacers from glass fiber reinforced plastics G
113. etectors spaced 147 pixels for projects needing contiguous coverage and analysis of large areas of sky it is necessary to take dithered images with offsets of 4167 pixels 75 15 arcmin or greater In such cases the reduction software will implement an algorithm to generate a large area image removing the cross between each detector SWARP software and algorithms from Terapix might be used into the pipeline PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 170 of 183 3 5 4 8 3 1 9 Astrometry and Photometry Since astrometry and photometry are not a requirements at first light methods will be defined further on However a raw astrometry based on distortion parameters determined from the optical design should be ready at first light 3 5 4 8 3 2 Quick look Mode The quick look mode will have the following main tasks 1 Detector calibration for instrument signature removal a Dark subtraction b Flatfield division c Bad pixel correction mask frame 2 Sky modelling and extraction Shift and align 4 Mosaicing Master Detector Target Raw Calibratrion Calibration Frames Frames Sky Modelling Shift amp Align 4 frames SE Reduced EE SuperFrame Reduced p Frame Figure 3 5 4 9 Quick reduction scheme 3 5 4 6 3 3 Science Mode The science mode will have the main tasks described in 3 5 4 8 3 Main steps as shown in the next figure PANIC Code PANIC GEN SP 01 Iss R
114. etric in Y z PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 147 of 183 Absolute photometric accuracy should be 0 03 mag in Y z bands with pixel size of 0 25 arcsec and 0 05 mag with pixel size of 0 45 arcsec It will depend on the quality of the input data 3 5 3 6 2 13 Ghosts The reduction pipeline shall remove the ghost images created the different filters To do that it will be necessary that they are characterized 3 5 3 6 2 14 Field distortion The reduction pipeline shall correct the field distortion To do that it will be necessary that it 1s characterized The corrected images shall be suitable for mosaicing 3 5 3 6 2 15 Image stability The reduction pipeline shall correct the image motion by the instrument during an exposure run To do that it will be necessary that it is previously characterized 3 5 3 6 2 16 Catalog generation The pipeline shall provide a basic catalogue generation including astrometric photometric shape and data quality information 3 5 3 6 3 Hardware Requirements The DRS should run on a fast system based on Linux PC with multi CPU at least 16 32 GByte of RAM and using disk RAID arrays for local storage with at least 4 TB of capacity for about 30 full operation nights 3 5 3 7 Data Collection And Data Rates Requirements 3 5 3 7 1 Data volume PANIC control system shall be able to handle an average data volume of 100GBytes per night
115. fined rules In this way the classified data will be processed more easily by the quicklook tool and the on off line pipeline Quicklook Tool QT This tool shall provide a fast preview of the data being acquired by GEIRS It will perform a rough and ready data reduction to the observation at the telescope and shall allow to check that the right objects are being observed This package will use some parts of the pipeline procedures quick reduction mode Data Reduction Software DRS The data produced by the observation run shall be calibrated and processed in a on off line TBC pipeline Automatic pipeline reduction of the instrument data is predicated on the assumption of a well defined set of observing protocols that supply the relevant meta data of the pipeline reduction system These meta data should be provided by the Observation Tool to GEIRS to be saved in FITS headers Besides the pipeline will not only delivered a product with scientific quality product but also provides feedback on the health of the camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 151 of 183 Data Reduction Software x User PN Template N defined i Template Quicklook Tool Observation Tool Data Classifier Observation Setup User defined AS PIPELINE Scripts Keyword IDs amp science Ve i quick me ee Ss ees Ss E
116. from the bench and the cold shields Both optics assemblies do not touch each other An optical labyrinth ensures light tightness between them The arrangement scheme of all optical elements of PANIC is shown in Table 3 3 1 and Table 3 3 2 The detector array 1s mounted directly to the optics wheel unit complete optics Table 3 3 1 Grouping of the optical elements of PANIC for the 0 45 arcsec pixel scale complete optics Table 3 3 2 Grouping of the optical elements of PANIC for the 0 25 arcsec pixel scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 95 of 183 Mass Table 3 3 3 Mass estimation of the cryogenic opto mechanics Mounting structure LN vessel Field stop wheel Optics assembly 2 optics wheel with mount Optics assembly 1 optics group 1 with mount Figure 3 3 2 1 Section through PANIC the vacuum window and the detector unit are not shown PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 96 of 183 Lens mount 3 Optics wheel Filter unit Lens mount 2 Rotating field stop Cold bench Mirror M3 Mirror M1 Mirror M2 Lens LO Figure 3 3 2 2 Cold bench and optics 3 3 2 2 1 Entrance window The entrance from Infrasil has a diameter of 330 mm and a thickness of 20 mm As shown in Figure 3 3 2 3 it is mounted to a cylindrical flange of the vacuum vessel by a retainer rin
117. g It 1s sealed by an o ring The FEM results of the window deformation due to atmospheric pressure are shown in section 3 3 2 2 7 3 Retainer ring Entrance window O ring Figure 3 3 2 3 Entrance window PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 97 of 183 3 3 2 2 2 Mounting of cryogenic lenses and mirrors The most difficult task of the lens mount design is to make sure that the lenses survive cooling and at the same time achieve the tight tolerances required by the optical design If the lenses mirrors were mounted in a conventional way e g with a threaded retainer ring the different thermal expansion properties of the materials used might lead to severe damage during cooling Therefore a mounting method is employed that uses chamfers at both the lenses mirrors and the mount parts In this case a chamfer angle of 40 1s chosen for both outer edges of each lens mirror the lens mount and the retainer ring Figure 3 3 2 4 shows how this principle was used for the cold optics of OMEGA2000 The lenses sit in the conical surfaces of the mount The retainer rings keep the lenses in this position by the forces of eight disk spring packages each Temperature changes result in diameter changes of the parts These changes lead to an axial displacement of the lenses and retainer rings because the parts can slide on the chamfer surfaces relatively to each other assuming that the chamfers
118. ge of the dominant stellar population the extinction Ay the galaxy type the favoured IMF the total stellar mass of the host galaxy and the host galaxy environment PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 29 of 183 2 1 3 Mapping of nearby galaxies It is well known that at NIR wavelengths the effects of extinction are mitigated while galaxy phenomena are hidden at shorter wavelengths The following studies could be performed 2 1 3 1 Morphological characterization Multiple nuclei bars and boxy peanut shaped bulges become visible at NIR wavelengths The wide field of PANIC is also particularly suitable for mapping the outer parts of galaxies where flaring or warping occur Extremely low surface brightness halo structures in nearby galaxies could be traced using red giants A high resolution imaging mode will provide access to nuclear parts of galaxies e g photometric cusps used to measure the mass of the black hole 2 1 3 2 Star formation and stellar populations Studying dust embedded star formation in nearby galaxies Mapping in SIII 0 9069 0 9532 um Paschen amp Brackett series H2 FelI CO band head and their corresponding continua would allow to study the excitation mechanisms in regions of active star formation as well as detection of the shock effects and possible impact on the dust attenuation law They could also be an interesting supplement to Spitzer
119. gle introduced when the decentering compensator are used Sub barrels integration Optics mount 1 DECENTER X DECENTER Y BARREL wi s id SE EN POSITION Z um arc min arc min um um Table 3 2 40 Integration tolerances within the Optics mount 1 for 0 25 px scale Sub barrels integration Lens mount 3B DECENTER X DECENTER Y BARREL ree E b o POSITION Z um arc min arc min um um Table 3 2 41 Integration tolerances within the Lens mount 3B Sub barrels integration Optics wheel DECENTER X DECENTER Y BARREL min A MA b POSITION Z um arc min arc min um um Table 3 2 42 Integration tolerances within the Optics wheel in the 0 25 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 84 0f 183 Assembly errors whole instrument Table 3 2 43 Assembly tolerances for the different units in the 0 25 px scale Alignment telescope whole instrument BARREL TILT X TILT Y DECENTER X DECENTER Y POSITION Z um arc min arc min mm mm Table 3 2 44 Tolerances for whole instrument to the telescope in the 0 25 px scale Whole instrument i Figure 3 2 7 2 shows the overlay EE for the montecarlo systems generated with the values of tolerances that we have summarized More than 97 of the systems are inside the criterion half EE80 lt 27 um as required OIFF LIMIT 0 0972 BATS DEL H WM H OR DEL 4 082 0 972 DEL E
120. hall be 0 1 e sec at operating temperature 3 1 5 1 9 Pixel operability PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 370f 183 The number of functional pixels shall be gt 95 3 1 5 1 10 Operating temperature The operating temperature shall be 77 K 5 K 3 1 5 1 11 Temperature fluctuation The temperature fluctuation should be less than 0 1 K This specification was not given by Teledyne 1t was rather defined by the PANIC team 3 1 5 1 12 Cool down and warm up The cool down and warm up rates of the detectors shall be lt 0 5 K min 3 1 5 1 13 Physical flatness The surface of each detector shall be flat to 40 um peak to valley 3 1 5 1 14 Storage temperature limits The detectors shall be stored safely between 50 K and 310 K 3 1 5 1 15 Detector identification Each detector shall be identified by a unique serial number 3 1 5 2 Mosaic Package The mosaic package consists of an assembly plate made of molybdenum where the 4 detectors will be mounted to 3 1 5 2 1 Flatness The flatness over the surface of the whole array 4 detectors shall be 40 um peak to valley from the best fit plane 3 1 5 2 2 Dead space The dead space between the detectors shall be lt 3 mm approx 167 pix which correspond to about 75 arcsec from one active area edge to the other 3 1 6 Design 3 1 6 1 Science Detectors The science detectors are mounted into a molybdenum mosaic
121. has to be cooled by the large Nitrogen vessel PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 91 of 183 3 3 1 2 6 Thermal investigations 3 3 1 2 6 1 Nitrogen vessel for cold bench 1 Radiation on surface 4 3 m with multilayer insulation 5 W m 21 5W 2 Radiation through the window 22 W 3 Conductivity through spacers 5W 4 Conductivity through filling tubes 0 1 W 5 Conductivity through cables 3W 6 Power consumption detector preamplifier and electronics 5W Complete heat input 57W Evaporation rate 1 3 l h Hold time with 45 LN2 35 5 h 3 3 1 2 6 2 Nitrogen vessel for detector cooling l Radiation on surface 0 09 m 0 03 W 2 Conductivity through spacers 0 05 W 3 Conductivity through filling tubes 0 05 W 4 Power consumption detector 0 05 W Complete heat input 0 18 W Evaporation rate 4 10 3 I h Hold time with 1 1 LN2 250h 3 3 1 2 6 3 Thermal gradient Because we want to save weight we use only one Nitrogen vessel to cool the cold bench In other instruments we enclosed the inner vessel with a second outer actively cooled shield The use of only one Nitrogen vessel results in a thermal gradient and temperature changes over the cold bench due to the filling level and the orientation of the cryostat To keep the Nitrogen consumption small and to reduce the gradient we will use multilayer insulation MLI Nevertheless there 1s still a small resulting temperature change
122. he basic requirements The ones we followed up are e Extend the spectral range to 0 82 microns so PANIC will cover all spectral bands from the z to K The z band has been included for convenience of the observers in order to allow z band observations to complement NIR observations without changing instrumentation or waiting for another instrument to be mounted The applications of PANIC however are in the NIR e The use of narrow band bandwidth 1 of central wavelength filters This requires that the angle of incidence of the beam does not exceed a certain value Our optical design takes this into account e A second pixel scale of 0 25 arcsec pixel This image scale will allow higher spatial resolution and will be very useful under good seeing conditions which prevail frequently since the median seeing at Calar Alto is 0 89 arcsec in the R band which corresponds to 0 65 arcsec in the K band An optics wheel to exchange some parts of the optics allows to change between the two image scales A major difficulty imposed by the optics 1s the high mechanical precision required in positioning this wheel 0 45 microns see mechanics section However close to the date of submitting the PDR documents it finally turned out that PANIC with 2 image scales well exceeds the 400kg limit We estimate the difference in mass between a single and two pixel scale instrument to 80 100 kg This is so because not only additional hardware is need but also a l
123. his document presents the specifications of the NIR Detectors for PANIC In addition the test procedures for the characterization process and the general handling of the detectors are described 3 1 5 Specifications The following specifications apply under normal operating conditions and correspond to the ones given by Teledyne in their offer 3 1 5 1 Science Detectors PANIC will use a mosaic of four 2k x 2k HAWAII 2RG MBE grown HgCdTe AR coated substrate removed devices from Teledyne 3 1 5 1 1 Number of pixels Each detector shall have 2048 x 2048 pixels 3 1 5 1 2 QE and Spectral Range The detectors shall be responsive from 0 3 um to 2 5 jum The QE shall be gt 75 in all photometric bands Y J H and K 3 1 5 1 3 Uniformity of OE The non uniformity of QE shall be lt 10 o mean in the QE histogram in all bands 3 1 5 1 4 Pixel Pitch The pixel pitch shall be 18 0 um square format 3 1 5 1 5 Number of Outputs Each detector shall have 32 outputs that can be operated in parallel in order to reduce frame times 3 1 5 1 6 Read Noise The read noise shall be lt 20 e CDS 100 kHz 3 1 5 1 7 Timing In subarray mode an area of 15 x 15 of the detector shall be read out at a rate of 8 ms frame with a goal of 1 ms frame for fast photometry This specification was not given by Teledyne it was rather defined by the PANIC team based on the scientific requirements 3 1 5 1 8 Dark current The dark current s
124. ht time The science operational mode becomes possible when all data of a night including the associated day time and twilight calibrations have been collected Then the calibration data are sorted and assessed independently of their timestamp The best possible master calibration data are created Their quality is checked They are finally applied to the science data of a night In this report both the first after light and after first light requirements will be considered for the preliminary design description however for first light only OT and quicklook shall be operative 3 5 4 8 2 Data Flow The next figure shows how the data flows in the system from the ROE to the data repository after the data processing into the DRS The data quickly reduced will be able to show in the quicklook display tool The main tasks of the data receiver and the data collector are detailed bellow Data Receiver 1 Detect when new data arrive from the data acquisition system ICS 2 Inspect the data header classify the data and put it into the corresponding directory calib science tests Some new keywords may be inserted into the header and or file conversion could be done Multi extension FITS cubes to single FITS or whatever 3 If quicklook is activated by the user run the quick reduction mode pipeline with the new science data as they arrive 4 Provide the new data calib and science to the science reduction mode pipeline 5 Remove per
125. ials not using high index refraction materials in order to include all the photometric bands even the z band in the system avoiding some critical materials The correction of off axis aberrations due to the wide field available the correction of chromatic aberration due to the wide spectral coverage the introduction of narrow band filters 1 in the system minimizing the degradation in the filter pass band have been achieved with this optical design An important point is the production of the internal cold stop with good optical quality which reduces the background in K band considerably It has been presented the feasibility of the two pixel scales 0 45 px and 0 25 px in the FOV required being the two systems independent each other Notice that the optical design of the 0 45 px scale will not be affected if the other scale is suppressed PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 87 of 183 3 3 Cryostat and Mechanisms 3 3 1 Cryostat 3 3 1 1 Requirements 3 3 1 1 1 Temperature Due to background radiation the local temperature inside the shield should not exceed 100 K This 1s also valid for local spots like cable feed throughs or motors Temperature changes should be in a range that the tolerances of the optics are met The detector has a working temperature of about 77 to 80 K which has to be investigated The required stability is 0 1 K Warm up and cool down of the d
126. ich produce the ghost images The Table 3 2 21 and Table 3 2 22 summarize the results obtained for the two pixel scales A lot of values are not included because they were too far out of focus for the simulation to make sense The higher results in intensity ratio between a ghost image and its source are the ghost 1 and 73 respectively the instrument window and the filters but always 1s lower than 1 10 in all the cases 1n requirement There are three ghosts out of the 10 diameter requirement they are 2 field 1 and 5 fields 3 and 4 But they do not represent any problem because the requirement of Image Ghost ratio is completely fulfilled In the 0 45 px scale 10 are equal to 400 um so in principle the ghost Z2 violates this condition but notice that this ghost has a central hole of 60 um and both the source and the ghost are centred in the 0 0 coordinates The source has a diameter of 29 84 um so there will not real superposition In the 0 25 px scale 10 are equal to 720 um so in principle the ghost 5 fields 3 and 4 violates this condition If we calculate the contribution of the ghost in relative energy in the source area we can notice that it is in the order of 10 or 10 We can conclude that in all the cases the contribution in intensity is insignificant instead of the violation in diameter so the impact of the ghosts in the total PSF of the system 1s negligible First reflecting Second reflecti
127. ilica with a thickness of 12 5 mm between the L7A and L8A It is possible to refocus the system by a movement of the telescope S2 along the optical axis so the measurements in defocus are referred to the displacement of the S2 from the nominal position in the polychromatic configuration and gives the sense forward 1 e sense toward the entrance window backward opposite Focus mm oso s277 3009 Table 3 2 8 Bandwidths of evaluation of the PANIC optical design and their change in focus for the 0 45 px scale The image quality of the instrument is specified in terms of the 80 EE EE80 for each photometric band where EE80 is expressed as the square side length which contains the 80 of the image energy This EESO is evaluated in Table 3 2 9 using the greater value obtained in the FOV analyzed Note that all the bands are in requirements EE80 lt 2 pixels 36um 0 90 EE80 um EE80 pix EESO arcsec Polychromatic Table 3 2 9 EE80 in the 0 45 px scale For simplicity it has been presented only the polychromatic EE in Figure 3 2 6 12 the X axis 1s the half side length square of EE and the Y axis represents the fraction of energy enclosed where there is indicated with an horizontal line the 80 In dark it is shown the diffraction limit of the system For simplicity as well it has been presented only the polychromatic spot diagram in Figure 3 2 6 13 This figures shows the geometrical structure of the
128. ill be very little moment around both axes which are perpendicular to the rotation axis Figure 3 3 2 11 shows that there are six positions in each filter wheel five of them can hold filters and one remains empty This hole is bigger than the others to access the filters in the wheels below through an opening in the housing This opening is normally covered and light tight A set of three spring clips hold the filters in their position To avoid scratching of the filters there are thin protection rings between the filters and the spring clips For feeding back the wheel position resolvers RE 15 from LIN Servotechnik are mounted on the back side of the motors not shown in Figure 16 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 104 0f 183 Stepper motor Double row ball bearing Filter access ns hole cover Ge Jm not shown CN Bellow coupling Pair of ball bearings Shaft Figure 3 3 2 10 Filter wheel unit with four filter wheels Figure 3 3 2 11 Filter wheel with drive unit PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 105 of 183 Bail e all bearing Protection ring Spring clip Filter Figure 3 3 2 12 Detail view of filter wheel 3 3 2 2 5 Rotating field stop The field stop is located between LO and M1 The field stop mask for the 0 45 arcsec pixel scale has a free opening of 1
129. in or a optics decentre of 44 um c Ball bearing true run tolerance The true run tolerance of the ball bearing WAD933ZZ from ADR is 12 um d Optics shift due to thermal gradient As shown in section 3 3 1 2 6 3 the cold bench can have a thermal gradient under certain conditions This means that the optics wheel and the optics group 1 can move with respect to each other by up to 15 um e Deformation of the cold structure due to varying gravitation vectors The Finite Element Analysis shows deformations which can result in decentre of the optics wheel of up to 20 um f Positioning accuracy of the optics wheel on the bench The manufacturing accuracy on a conventional CNC milling machine is about 10 um This means that the positioning accuracy of the wheel on the cold bench is about 20 um in each direction For the current mechanical design it seems to be unrealistic to meet the specifications since the expected decentre values of a and b are already higher than what is acceptable for the optical quality Only f could by compensated by adjustment A mechanical design which allows to position the optics with the required precision in a cryogenic environment would be much more complex PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 115 of 183 However optical tolerance calculations show that if certain compensators are introduced in the optical design most tolerances
130. instruments it is often necessary to reduce the images in real time to adapt to varying conditions and to adopt the correct observing strategy The quick look facility is intended to allow a fast examination of raw frames and pre processed images It will be used to visualize sets of images and monitor in real time the observation It shall offer a wide variety of graphical resources as well as preliminary inspection tools specific to the observation mode such as simple statistics zooms cuts radial profiles among others Therefore a quick look data reduction mode will be implemented into PANIC DRS specifically designed to reduce in a fast mode the infrared observations The quick pipeline will allow the observer to clean up the images cosmetically using a set of calibration files darks flat fields etc to examine the images in many modes to compute image quality parameters FWHM SNR and to put various images together in mosaics or shift and add Furthermore the quick look pipeline shall accept data acquired with various observing techniques dithering separate sky exposure etc 3 5 4 7 2 Implementation The quicklook will be based on display tool like SkyCat or DS9 They are freely available and provide a powerful programming interface for our purposes 3 5 4 8 Data reduction software description 3 5 4 8 1 Purpose PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 165 of
131. iodically the old quick reduced data and temporary files created Data Collector 1 Detect when new quick reduced data are produced and send them to the quicklook display tool and save them into the quick data temporary directory PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 166 of 183 2 Detect when new science reduced data are produced and save in the data repository in the corresponding directory for data delivery 3 If data archiving is working in CA insert new data raw and reduced into the archive Data Reduction Software ICS data acquisition DATA Repository Figure 3 5 4 8 Data flow 3 5 4 8 3 General data reduction schemes 3 5 4 8 3 1 Main steps The standard IR image reduction process involves several steps from the raw frames to the reduced image which contains the calibrated astronomical signal The data reduction software will implement the following processes 1 Detector calibration for instrument signature removal a Linearity correction b Dark subtraction c Flatfield division m Bad pixel correction mask frame PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 167 of 183 2 Fringing correction 3 Sky modelling and extraction 4 Shift and align 5 Electronic Crosstalk correction 6 Optical ghosts removal 7 Field distortion correction 8 Mosaicing 9 Astrometry 10 Photo
132. ion uick Look Control Electronic Figure 3 5 4 3 Computer Architecture 3 5 4 5 GEIRS Design description For general GEIRS description see the manual of Omega2000 ADI or other IR instrument manuals using GEIRS This description concentrates on the specific functionality of PANIC and its requirements PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 154 0f 183 gt initiate action Es GEIRS task gt data access SE HW data buffers data flow Inside PANIC Dewar control lines d 128 channels Motor MPIA ROE3 Temperature uso Pressure Schematic 4 detector array showing mM NEN 2 data lines expected standard scanning directions and Electronic reference pixels around sensitive pixels SEH Ei MPIA PLX PCI device port wheel aio 2 DMA channels Read buffers healthy sU scanner Ge Ls read AP guiding raw data SOEN 7 processing i XR science raw data TA action ER guiding processing deeg ER amp i ES emdServer ee and or J TUN ay PU interface controlGUI A A die T ETE RT display RT display healthy science guiding E A monitor image image A RS Observation Online tool i pipelinef i PANIC workstation l OT reduction CN a EM mmm Figure 3 5 4
133. ion tolerances within the lens mount 3Ba Lens mount 3Bb L61B L7B ECENTER X DECENTER Y SINGLET AA NS PEN EN POSITION Z um arc min arc min um um Table 3 2 38 Integration tolerances within the lens mount 3Bb PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 83 of 183 Barrel 4B L8B SINGLET TILT X TILT Y DECENTERX DECENTER Y POSITION Z um E HET min CN min um um Table 3 2 39 Integration tolerances within the barrel 4B Next tables show the integration tolerances for the sub barrels and finally the instrument We show them as they are nested First there are the Optics mount 1 Table 3 2 40 second the Lens mount 3B Table 3 2 41 and the Optics wheel Table 3 2 42 them the whole instrument assembly Table 3 2 43 and finally the alignment of the instrument with the telescope Table 3 2 44 Note that Optics mount 1 is common for the two pixel scales but this scale do not impose values to the other scale The same happens with the alignment to the telescope The alignment for Barrel 3B can be completely relaxed 1f we verify this barrel with 1ts sub barrels completely attached The others barrel have values quite relaxed In this scale the only available adjust once the system 1s cooled will be the telescope refocusing using the S2 too So the same consideration is done with respect to the detector adjustment in position and tilt to compensate for the an
134. ions shall be all accessible from an GUI with a display tool There must be communication with the image display for the purposes of specifying positions with the cursor and for overlaying graphics The general requirements are 3 5 3 5 1 1 Quick feedback The quicklook shall be able to provide quick feedback on the quality of the raw data to the user 3 5 3 5 1 2 Quality control The quicklook system should be able to provide the Quality Control required to monitor the quality of the data That should include mean sky brightness sky noise image detection threshold average FWHM seeing average stellar ellipticity and average saturation level 3 5 3 5 2 Observing Utilities 3 5 3 5 2 1 Focus A utility to enable determination of best focus from a series of frames taken at different focus positions shall be provided by the quicklook 3 5 3 5 2 2 Seeing A utility to enable determination of seeing from a frame should be provided by quicklook 3 5 3 5 3 Data reduction tasks The quicklook pipeline shall do the data reduction tasks defined in the quick pipeline mode 3 5 3 3 4 Extensions The quicklook pipeline could be extended to produce coloured images with different filters or mosaic images if possible 3 5 3 5 5 Quick data persistence Quick look reduced data should only be kept until the beginning of the next observing night 3 5 3 6 Data Reduction Software 3 5 3 6 1 Quick pipeline PANIC Code PANIC GEN SP 01 Iss R
135. irements However some of those software requirements should be revised after PDR PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 150 of 183 3 5 4 Design Report The software architecture of PANIC shall be divided in two main packages the Instrument Control Software ICS and the Data Handling Software DHS Each one is composed as follows 3 5 4 1 Instrument Control Software GEIRS It is an already existing GEneral InfraRed instrument Software once intended to control all MPIA CAHA in house infrared cameras It shall control all PANIC hardware like in other CAHA instruments and the telescope interface The main part shall be the control of the detector and the data readout Observation Tool OT This software package will allow high level control of the instrument based on a GUI This tool shall provide a higher level of abstraction to the user in order to allow an easier observation procedure It will provide a set of predefined observation templates with some parameters to be set by the user The user can choose some of these templates define his her own observation template or control directly the observation using high medium level commands 3 5 4 2 Data Handling Software Data Classifier DC It will be composed of two main tasks the data receiver and the data collector The aim of these packages is to inspect the FITS headers and classify the data files using a set of prede
136. isks as data storage to allow data saving with full speed of the read out and the DHS data access The disks should be RAID protected if that solution is fast enough 3 5 3 3 2 Interfaces All interfaces should be provided additionally in simulation 3 5 3 3 2 1 Instrument Status GEIRS shall support e an instrument status GUI e monitoring of all available temperature and pressure sensors of the PANIC dewar PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 138 of 183 e and monitoring of external conditions if information is accessible dry liquid nitrogen protection flow of the entrance window temperatures of electronic rack houses etc e logging of the temperature and pressure values as history to allow to be checked and visualized at any time by plotting tools e writing of the necessary status information temperature pressure other conditions into the FITS header 3 5 3 3 2 2 Control Electronics The interface to the motor electronics 6 cryogenic motor units controlled by a MPIA motor electronic shall optimize the moving time and the position reliability for instrument efficiency The motor devices shall be configurable as disabled enabled fixed to position simulated be configurable for the position of the elements the element objects and the dependencies defined by the elements wavelength focus offset etc do for each device during home initialization
137. its At the moment there are two 5 volts 8 Amps switching supplies in use We estimate a maximum power consumption of about 50 watts 3 4 1 3 8 Detector protection circuitry Since the used detectors are not inexpensive protection circuitry is included in the ROE to avoid damage The first part is located on the Clock Bias board the second part on the 36 channel cryogenic preamplifier All biases and clocks needed by the detectors are generated by the Clock Bias board In Figure 3 4 1 7 the zener rectifier limits the detector supply voltage to 4 7 volts in case of a circuit failure All other supplies and clocks are clamped via a Schottky rectifier to that voltage This ensures that no detector input voltage can be greater than VDD 0 2 volts and prevents latchup PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 126 0f 183 of detector input pins The remote controlled DAC has a power on reset input This guarantees that all biases are at 0 volts after power on 5 VA A VRef1 25 gt 3 6 R 2 A gt VDD AGND AGND AGND AGND LLL LC Wh gt VDDA 5VA A BI D VBiaspower t vai 4 Y s 1 oe BE CLK OUT1 V lo 2 x 45 NC FL S IN CLK OUT Figure 3 4 1 7 Protection circuitry on Clock Bias board More protection circuitry is integrated to the 36 channel cryogenic preamplifier Each detector input pin is protected with the circuit in Figure 3 4 1
138. ius in this case 150 mm E Young s modulus 70000 N mm t window thickness 20 mm The reason for the difference between the FEM and the calculated results is unclear Only measurements can show which of both values 1s closer to reality To calculate the minimum thickness various equations can be found in the web see 2 3 and 4 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 113 of 183 Using the following equation from 2 the minimum window thickness is 14 3 mm Tmin sqrt 1 1 p 17 S M psi with S safety factor in this case 4 M rupture modulus for fused silica 7000 psi r effective radius in inches p differential pressure in psi The equations from 3 and 4 give similar results So a window thickness of 20 mm seems to be sufficient 3 3 2 2 7 4 Bending of mirror M1 due to gravity For the biggest of the three cryogenic mirrors the bending due to gravity has been simulated using ANSYS The mirror was placed horizontally with the gravity vector in y direction see Figure 3 3 2 24 The maximum value in the center is 47 nm peak to valley PTV This corresponds to a RMS value of 13 3 nm when the following worst case relationship for defocus e g from 5 1s used PTV 2 sqrt3 RMS The wavelength range of PANIC is 0 8 2 5 microns Thus if we specify the maximum deflection RMS of the reflecting surfaces to be lamb
139. lanned spectroscopic observations 2 1 6 Clusters and Superclusters of galaxies Broad band observations of clusters and superclusters of galaxies would allow to search for objects with strong IR excess and or the selection of candidates to supermassive starbursts in clusters at intermediate redshift making use of deep narrow band filter imaging matching their redshifted Ha line PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 30 of 183 2 2 Galactic Astronomy 2 2 1 Galactic survey A proper motion survey is proposed using 2MASS as the first epoch over a quarter of the sky which will not be covered by any NIR imager The larger depth of the survey would allow obtaining a better star galaxy separation and photometry for all 2MASS objects and proper motion down to 10 mas yr This catalogue would allow searching for population II very low mass stars and brown dwarfs This project is completed by the case explained in 2 3 4 2 2 2 Galactic plane and bulge The wide field of PANIC will allow mapping selected areas of the galactic plane and bulge NIR imaging permits a detailed exploration of the large scale structure of the Milky Way and the Galactic components in hidden areas of the Milky Way There are still controversial or totally unknown parameters in the description of the detailed stellar structure e g concerning the radial and vertical distribution of the Galactic disc and its s
140. le of the sky extraction 1s the following Several dithered images are stacked in the pixel coordinate system 1 e the values in the third dimension of the image cube all result from the same detector pixel Due to the small telescope offsets in between the image sequence the astronomical objects are slightly shifted from image to image Thus the pixel columns the values for the same pixel in the different images contain mostly sky signals even at the position of a stellar object in one image A suitable value for the actual sky level in such a pixel column is the median The median 1s a less sensitive function concerning outliers than the average and is thus less influenced by a high star signal An accurate sky frame is obtained by determining the median for each pixel column of the image Besides a real median process other techniques can be applied to extract the best local sky value for a pixel 3 5 4 8 3 1 4 Shift and align After the background contribution has been removed and the individual image is fully reduced all frames belonging to the same pointing have to be added up in order to create a master image with an improved signal to noise ratio When summing N images with a given SNR of an object the signal to noise ratio of the superimposed frame will be improved by a factor NN For the detection of very faint objects a large number of images has to be co added in order to reach a sufficiently high SNR since the images were taken at
141. lified block diagramm of instrument control electronics ETHERNET PANIC Control System Simplified Block Diagram Cryostat Workstation Cryostat i Stepper Motors Resolvers Fiber Link Read Out Electronics ANAL Heater Figure 3 4 2 1 PANIC Control System Simplified Block Diagram PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 130 of 183 3 4 2 3 Motion control electronics 3 4 2 3 1 General The heart of the PANIC Motor Controller is the standard MPIA MoCon board with a phyCORE XC161 Single Board Computer module on it This MoCon board is a multi functional device which is able to control a huge variety of motors Due to the modular concept the MoCon electronics is capable to drive stepper motors as well as servo loop motors Core of the hardware is a 16 bit Infineon Controller which contains the firmware managing the communication and command functions For motion controlling the electronics 1s equipped with two motion processors from Performance Motion Devices 3 4 2 3 2 Principle of motion control system Cryostat Motor Controller Referenos Switch TT Limit Switches Motor Driver 4 i Stepper Motor Resnlver Resolver Interface Figure 3 4 2 2 Principle of motion control system PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 131 of 183 3 4 2 3 3 Motion controller board MOC
142. ll be filled from the side through the central ring Filling will be done by pointing the telescope to zenith The filling tube from the side goes to the bottom of the LN vessel The exhaust gas line ends in the centre of the vessel It will be filled until LN2 is spilled out of the exhaust gas line The third tube will end about in the centre of the LN vessel When the vessel is full the filling line will be closed and the exhaust gas line opened If it is necessary to drain the vessel the filling line is opened and the exhaust gas line 1s closed The pressure of the evaporating gas will press the LN out of the filling line when pointing to zenith The thermal contact area to the cold bench is ring shaped on the rim of the bottom flange This is due to the deformation of the nitrogen vessel from pressure inside which should not have any influence on the optical bench The extremely weight reduced LN vessel for the cold bench could not be calculated in a standard way So we had to use FEM Due to the risk of this calculations we are going to have a crosscheck of the results from an external company Th contact Eer ermal contact area Vertical tube for the Flat lower part light path Figure 3 3 1 2 Nitrogen vessel for cold plate 3 3 1 2 3 Nitrogen vessel for detector cooling The detector will be cooled by a separate nitrogen reservoir This 1s necessary in order to have a constant temperature which in other case would change with
143. lso be done by cooling down and warming up again However this self centering only works for radial misalignments of more than about 0 1 mm For values smaller than that the centering forces seem to be too low to overcome friction In the case of OMEGA2000 the manufacturing tolerances for the chamfer angle were 3 arcmin for the mount parts and 2 arcmin for the lenses The tolerances of the chamfer position were 0 01 mm retainer ring lens lens mount a mount cools lens cooles retainer ring cools d Figure 3 3 2 5 Displacements of lens and retainer ring due to thermal shrinkage during cooling from room temperature to 77 K The arrows in axial direction show movements relative to the lens mount supporting surface a All parts at room temperature b Lens mount cooling lens and ring still much warmer c Cold lens mount lens cooling retainer ring still much warmer d Cold lens and lens mount retainer ring cooling The radial force component Fg of the spring force Fp which centres the lens can be calculated as Fr Fr sina cos al with a being the chamfer angle relative to the optical axis assuming that friction can be neglected Tests with the focal reducer of OMEGA2000 have shown that once the lenses were aligned as accurately as possible e g to 0 01 mm changes in the lens position introduced by multiple cooling cycles and changes in cryostat orientation could not be measured The accurac
144. lto in the V band is 0 9 S F Sanchez J Aceituno U Thiele D Perez Ramirez J Alves arX1v 0709 0813 The night sky at the Calar Alto Observatory that is 0 67 in the K band From Sanchez et al s Fig 5 one can compute that 51 of the nights have seeing lt 0 67 in the K band During these nights the images will be undersampled In order to avoid this situation a smaller pixel scale has been proposed and the optical design has incorporated it PANIC PRELIMINARY DESIGN REPORT Code PANIC GEN SP 01 Iss Rv 0 1 Date Page 22 October 2007 33 of 183 Different kind of scientific projects that will profit from a such a pixel scale 0 25 pixel Morphological studies of extended objects galaxies planetary nebulae etc Differential photometry with precision of millimagnitudes Since the light will be spread over more pixels differences in their response will be averaged besides partial aperture techniques can be easily applied Detection of faint sources close to bright objects low mass companions objects with planetary masses etc because if the point spread function is oversampled the saturation level and saturation effects will be reached only after longer exposure times In order to compute the effect of the pixel size on the photometric precision we have analyzed a set of 226 K band images taken with Omega2000 for the Alhambra project Mariano Moles et al on a certain field Differential pho
145. ly be lost under the wings of the stellar PSF It 1s possible to obtain information on the grain size distribution extinction equator to pole ratio density contrast and structure of the CSE via modelling the observations This case would benefit from a high resolution imaging mode Measures of stellar sizes Lunar occultations in the IR allow to derive very high angular resolution 1 mas information to be used for close binaries resolution direct measure of stellar diameters resolving objects with extended envelopes T Tauris carbon stars etc Narrow band filters will complement broad band ones as they allow a better resolution of diffraction 2 3 4 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 31 of 183 fringes for bright stars Fast read out mode should be implemented for these applications Low mass objects exoplanets The wide field provided by this camera will allow performing efficient searches of faint brown dwarfs and specially objects with planetary masses either isolated or far from their parent star in open clusters 2 3 4 1 Probing the IMF down to 1 Jupiter mass A deep star forming region survey The closest not farther than 300 pc and densest star forming regions will be surveyed in order to detect 1 Jupiter mass objects and to extend the IMF of those regions to that limit The different regions should also provide a wide range of initial condition
146. mation associated with one proposal Each OP consists of multiple Setup Elements SE and Observation Blocks at least one An OP shall be also completed with the following fields o Name ofthe OP o Purpose PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 160 0f 183 o Name or the PI o Institution o E mail e Setup Element SE A SE contains the information associated with one of the following subjects o Observing Constraints Site quality sky background seeing Schedule data airmass elevation constraints o Data store Setup File name prefix Save mode raw FITS cube integrated individual o Data reduction Setup Reduction Mode No reduction Quick Science Quicklook display True False o Instrument Setup Readout mode cycle type CDS LIR MSR Scale Mode 0 45 arcsec or 0 25 arcsec Frame size Full subwindow Integration Time IT is the single integration time for a single image result it is time that each pixel of a single cycle type image is exposed This parameter is to be optimized for each filter to allow background limited observations Repeats cycle repeat count number of single integration single images done They can be added up in memory before the final single image with an exposition time of IT Repeats seconds is saved on disk or otherwise they can be saved each single integration individu
147. meter Notice that this 1s only a first estimation and the final mirrors could be elliptical shape see Figure 3 2 6 5 and with the minimum thickness needed to assure not degradation in the optical quality That thickness will be determined for a FEA taking into account also the holder design for that element So the final mirrors weight surely will be less of this estimation Element Weight Kg M 4 46 10 47 ow am Table 3 2 3 Raw mass estimation for the folding mirrors 3 2 6 2 0 45 px camera 3 2 6 2 1 0 45 px Optics Layout Figure 3 2 6 3 shows the unfolded optics layout of the 0 45 px scale of PANIC Telescope flange Pupil Detector D o LUX 5 A LA Filters P IE AF UE em E A LE _ p TT Mil 118 OSS gt SC eg a nn an im Se a me NM e AAA I E LI L3 pon D L8A 4 da Ml amie M aaa M3 oc H Dewar L6A EN window Field Stop 3 Mirrors Cold Stop mask mask Figure 3 2 6 3 Optics layout of de PANIC the 0 45 px camera PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 51 of 183 3 2 6 2 2 0 45 px optical prescriptions The prescription of the system is listed in Table 3 2 4 and Table 3 2 5 In Table 3 2 4 are listed all the common elements of the two pixel scales and in Table 3 2 5 here are listed the elements of the scale 0 45 px that only belong t
148. metry 3 5 4 8 3 1 1 Detector Calibration It includes the following processing to remove the detector signature 1 Linearity correction The data obtained from NIR arrays may be strongly non linear although the linearity curve can be derived through observations of a stable light source for a range of exposure times e g a sequence of dome flats Potentially because each PANIC detector is read out in 32 parallel channels 64x2048 pixels each 32 separate linearity correction functions may be needed for each detector At the moment of writing this document we do not know what effect non linearity will have but in case a noticeable effect exists 7196 the suitable correction should be implemented into the GEIRS correlated image result function due the readout mode that is the resulting image pixel we get as raw image pixel is already a subtraction of pixel integration frame pixel reset frame where depending from the light the reset frame might already have a significant level which means we might have a pixel value of 100 as result of 43100 43000 or as result of 1100 1000 2 Dark subtraction from target and calibration frames Darks will be routinely computed from the daily observations by combining as many darks as are generally available for each exposure time and readout mode If a particular combination is not available the nearest suitable calibration dark frame from nearby nights will be used instead If this still d
149. mpensate for the angle introduced when the decentering compensator are used Sub barrels integration Optics mount 1 DECENTER X DECENTER Y BARREL un A oe gt POSITION Z um arc min arc min um um Table 3 2 30 Integration tolerances within the Optics mount 1 Sub barrels integration Optics wheel BARREL TILT X TILT Y DECENTER X DECENTER Y POSITION Z um arc min arc min um um Table 3 2 31 Integration tolerances within the Optics wheel in the 0 45 px scale Assembly errors whole instrument DECENTER X DECENTER Y BARREL ndn e mn gt POSITION Z um arc min arc min um um www Laang aso Table 3 2 32 Assembly tolerances for the different units in the 0 45 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 80 of 183 Alignment telescope whole instrument BARREL TILT A TILT Y DECENTER X DECENTER Y POSITION Z um arc min arc min mm mm Whole instrument 6 00 6 00 1 00 1 00 200 Table 3 2 33 Tolerances for whole instrument to the telescope in the 0 45 px scale Figure 3 2 7 1 shows the overlay EE for the montecarlo systems generated with the values of tolerances that we have summarized More than 97 of the systems are inside the criterion half EE80 lt 18 um as required DIFF LIMIT 4 2491 2 2394 OEG 4 4080 2 0648 DEG 8 2394 2394 DEG 2 2394 4 2994 DEG a 2394 0 2394 DEG FRA
150. mplete ROE thus consists of 4 AD36 1 ROCon and 1 Clock bias board these are connected PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 122 of 183 by a 6 slot backplane BP6 The OPTPCI is installed in the PC workstation and receives the data via fiber link 3 4 1 3 1 ROCon ReadOutController The ReadOutController board controls the activities of the whole ROE The ROCon is populated with two FPGAs two fiber transmitters and a microcontroller module One FPGA together with 8 MegaByte SRAM forms the pattern generator The second FPGA together with the two fiber modules do the data gathering and transmission to the PANIC workstation The microcontroller module handles the commands from the serial line or ethernet RS232 Microcontroller FPGA 1 px Module Data Address Ethernet Fo s Ex Data Address free Card and Channelselect ADC Data 1 Fiber Fiber 1 Module 1 ADC Data 2 Fiber 2 Module 2 Figure 3 4 1 2 ROCon block diagramm To run the pattern generator you first have to send commands containing the different chunks of the pattern The pattern also contains the trigger for the AD36 boards Next you have to send a program table The program table contains the sequence of the patterns and the number of repetitions of each pattern If the pattern generator is running the AD36 boards are triggered periodically This trigger arms a sequencer in FPG
151. mredinesvevaasioens 42 A MEE Gn ir AA ctsacae EEE E EAER EER ENER 42 A O A 42 3 1 8 Handling storage and transportation e eeessssssseeeeeeee seen nnne nnns 42 3 1 8 1 EE Eege 42 3 59 2 Tee Oe re 42 2S9 o AAA uE Deas mtd Ma Es tdiu te RUNE IER UR taMS nud 42 SX II Cu O O REO omoes 43 S15 IAN PO Soto 43 SCENE 44 SG o AAA o EEE EE TO 44 O A on os dead nse cnet adenaea Savas eoasasasenaveteuerss 44 55228 A Y 44 5 AME A 44 229 de ET E EE 44 323l SGBNERADREQUIREMEN Re pro E trasera 45 SR EN WM Ec em O M 45 A E A Ems 45 S SES MEN or OD CLA NET ccc c 45 pM TEM IP M 46 22 5 15 lc ene ne nee me oar ae et ner enn cer weer ey tae eae eee 46 De EN We E 46 3 2 5 1 5 2 Accessible pupil Ia 46 Sl P pilshape and ee E 46 32 5 10 Eet EE 46 SOS O e o quie pus titediemi idet E iE ENNNU NNI MENO ATEM c ODIT DEM eG 46 3 2 5 16 2 Individual Ghost diami GE sedeo nte aene Ron Hep RR aeu ES EEA EGRE ME ONE en E SERE E MEME 46 A ui c a a o PH 46 2 clc Ee E 46 A O o A nn peo E TUE DU ee MIU EU REN Rr dus 47 2 540152 SEolerdnce tor narrow band Eet E 47 52 518 o ao AMA 47 225 EC Ok E A MEME M wate E uae meee 47 3231 10 Environmental condi ds 47 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 10 of 183 3 2 5 1 11 High res
152. n and the decenter and tilt in X and Y being X and Y contained in the plane perpendicular to the Z axis The results for the barrels have been presented here in the order of they are nested The opto mechanical arrangement and grouping made for the mechanics for the two pixel scales 1s shown in Table 3 2 23 and Table 3 2 24 Groups complete optics Table 3 2 23 PANIC camera groups for the 0 45 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 76 of 183 lens mount 3Ba complete optics Table 3 2 24 PANIC camera groups for the 0 25 px scale The study has been performed as follows First a sensitivity analysis was performed to identify the critical elements in the optical system and define the tolerances in manufacturing and assembly of the lenses and the barrels for the two pixel scales At this stage there are two distances which need compensation due to manufacturing errors gt L1 L2 distance and L6B L61B distance These distances will be done after the factory report of the as built singlets such as thicknesses radii wedges and lens distances are measured A new optimization is then carried out and final values of these compensators are evaluated and fixed Thus this compensator will only compensate for symmetrical aberrations Second it has been assigned tolerances to the elements and the barrels and allowing some degradation in the nomi
153. n eser nne nsns 29 2 1 3 1 Morphological EE e EE 29 2 1 3 2 Star formation and stellar populations 0 29 2 1 3 3 Mascotas 29 A is An In E E see 29 2 1 5 Searches for high redshift quasars ooccccooooonnnnnnnnnonnnnnnnonnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnancnnnnnnns 29 2 1 6 Clusters and Superclusters of galaxies eese enne 29 2 EE RE Re LOU EE 30 2 2 EUA A MT 30 LEE GAMER plane ahd DUN LE ERROR 30 2 3 STELLAR EVOLUTION STAR FORMATION EXOPLANETS ooccoocccnoccnnoccnnancnnccnnnccnnaccnnnncnnanos 30 EST MEE oo PLE E Dia mi m ra 30 E COME PQ IA 30 2 09 9 Measures of Stellar SUZCS ia 30 2 0944 LOW EE 31 2 3 4 1 Probing the IMF down to 1 Jupiter mass A deep star forming region sure 31 2 3 4 Testing the brown dwarf ejection scenario a survey around Bok globules ooooooooccnnnnnnnnnn 31 2 5 2 ATAY Diniary COUNT DOT oa iio tic 31 ZII ooo uoa PES 31 E 31 2 3 8 SE 32 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 8 of 183 2 4 DOLAR a4 quz MT 32 2 4 1 Trans Neptunian s minor bodies enne 32 A A a APA e RE UU Un II ace ee oe se aoe tessa aged eee 32 2 5 JUSTIFICATION FOR A SECOND PIXEL SCALE en 32 3 REQUIREMENTS AND DESIGN RE 35 3 DETECTOR rar iO 35 SG ER WE er ee 35 A E 35 EE 35 AE PP o 35 E O A A o T 35 SIE FIANE EE o c
154. n set in English 3 6 3 3 4 Regarding electronics the documentation should include 3 6 3 3 4 1 Block schematics for cabling between different electronic units 3 6 3 3 4 2 Block schematics for each electronic board 3 6 3 3 4 3 Detailed schematics for each electronic board 3 6 3 3 4 4 Detailed electrical cabling for each electronic subsystem 3 6 3 3 4 5 Cabling through the telescope to be decided together with Calar Alto staff 3 6 3 3 4 6 Documentation about non standard components 3 6 3 3 4 7 Documentation about test programs and adjusting procedures 3 6 3 3 4 8 Extended users manual with all necessary for trouble shooting including serial and parallel port configuration 3 6 3 3 5 The maximum acceptable power dissipation under the mirror cell will be 100W If more is needed a cooling system should be implemented 3 6 3 3 6 Before first light at least 2 technicians from Calar Alto staff need a complete training about the electronics and software 3 6 3 3 7 For at least the first year Calar Alto needs a contact person to solve the unforeseen problems that will appear until the system is stable and Calar Alto staff has a complete knowledge of the instrument This contact person should be reachable also during vacations and occasionally but rarely during the night and weekends 3 6 3 3 8 The first PANIC observations will be done during instrument commissioning and in contact with the hardware and software designers if possible p
155. nal system performance With the Overlay Montecarlo and with some iteration has been established a limit in degradation for a 97 of the simulated system being inside the criterion The results obtained in this stage showed some elements with tight tolerances in the two pixel scales both in position and tilt So we have chosen the following decentring compensators to relax as much as possible the critical values L2 decenter gt L6A decenter and L5B decenter Those elements will be adjusted in decenter while placing an interferometer to cancel the non symmetrical aberrations due to lens wedges and mounting tilts These compensators have the effect of correcting non symmetrical aberrations due to Finally 1t has been performed a final analysis to determine the tolerances with the compensators implemented and the ranges needed for the compensators as well From Table 3 2 25 to Table 3 2 44 we summarize the values for the tolerances after the compensator has been introduced PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 77 of 183 3 2 7 1 1 Tolerances for the 0 45 px scale In Table 3 2 25 are the values for manufacturing We have considered a default ranges for the tolerated parameters for ROC the 0 1 of ROC for thickness 100 um for wedge 3 arc min and for flatness 1 fringe The range obtained for the compensator in L1 L2 distance 0 8 mm MANUFACTURING ERRORS O
156. ng T Ghost Geometrical rms Diameter um Relative intensity 5 1 1622 with hole 600 field 1 1643 with hole 622 field 2 Window rear Window front l l Hu 7 1655 with hole 622 field 3 1661 with hole 622 field 4 LO_front 329 8 with hole 60 field 1 2 10 107 Table 3 2 21 PANIC ghost analysis for the 0 45 px scale First e rtiad Second inr d T Ghost Sr Ea Gr inr d ae Geometrical rms Diameter um Relative intensity 5 3 2596 with hole 1000 field 1 2527 with hole 978 field 2 Filter rear Filter front l l 2504 with hole 961 field 3 2486 with hole 961 field 4 L6B_front 2981 4 field 1 3 2510 an 1999 with hole 666 field 1 1132 field 2 Lob front LO rear l u Hu 477 field 3 52 field 4 Table 3 2 22 PANIC ghost analysis for the 0 25 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 75 of 183 We also looked to see if any ghost pupil images are formed on the detector and we did not find anything significant These could potentially be a problem if the image of the pupil 1s near the detector and is smaller than the field of view But that does not happen in PANIC In conclusion the effects of the L8A L8B and LO dominate this analysis So the best way to deal with the ghosts will be put good AR coatings on those lenses and possibly in the filters and in the entrance window We have estimated that improvement of the AR co
157. ng phase of the project 3 2 6 5 1 Field Stop In order to achieve a good shielding from off axis sources of light that would be outside the desired FOV a Field Stop is placed at the position of the RC focal plane as shown Figure 3 2 6 3 between LO and M1 This aperture is usually located at an image to limit and define the FOV without adding radiating flux from warm surfaces which is critical in the K band In PANIC the Field Stop mask needed has been calculated for the two pixel scales as it is shown in Table 3 2 19 The free opening proposed is square shape with the same orientation as the detector The optimal positions in axial direction of the Field masks from the rear surface of LO are not coincident there is a space close to 3 mm This makes possible a mechanical solution which has the 0 45 px mask fixed and introduces a mobile 0 25 px mask Distance from LO rear to Field Stop Square length side of the Plate scale a i optimal position mm free opening mm 0 45 px 35 16 155 37 156 0 25 px 38 10 62 31 63 Table 3 2 19 Position and size of the Field Stop masks PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 72 of 183 3 2 6 5 2 Cold Stop A main feature in the optical design of an infrared camera is its cold aperture stop to reduce the thermal background overall in the K band In PANIC the entrance pupil or entrance stop is the telescope primary mirror
158. ntation should include oocccccnnnnnnnnnnnnnnnnononnnnninononos 174 3 6 3 3 4 1 Block schematics for cabling between different electronic units sesessssse 174 3 6 3 3 4 2 Block schematics for each electronic board eee ceescecceeeeeeeeneeeeeeeeeeenneeeeceeseeennaeeeeeeees 174 3 6 3 3 4 3 Detailed schematics for each electronic board essere 174 3 6 3 3 4 4 Detailed electrical cabling for each electronic subsystem ooccnnnnnnnnnnnnnnnnnnnninininnnininnnnnn 174 3 6 3 3 4 5 Cabling through the telescope to be decided together with Calar Alto staff 174 3 6 3 3 4 6 Documentation about non standard components oocccccccnnnnncnnnnnnnnnnnnnnnnnonnnnnnnnnnnnnininininininns 174 3 6 3 3 4 7 Documentation about test programs and adjusting procedures 0000ssoeeosseeeeeeeeeeeeeee 174 3 6 3 3 4 8 Extended users manual with all necessary for trouble shooting including serial and parallel a 174 3 6 3 3 5 The maximum acceptable power dissipation under the mirror cell will be 100W If more is needed a cooling system should be implemented iino ee 174 3 6 3 3 6 Before first light at least 2 technicians from Calar Alto staff need a complete training about the electrons and SOTUVOEE ege 174 3 6 3 3 7 For at least the first year Calar Alto needs a contact person to solve the unforeseen problems that will appear until the system is stable and Calar Alto staff
159. o be the sole instrument user interface at the telescope as well as remotely capable of configuring and sequencing instrument and telescope motions and of integrating the data processing pipeline with data acquisition Once a observation is defined it will be executed by astronomers or and operators users when they believe that the conditions are most favourable 3 5 4 6 2 Observing strategies A typical observing strategy carried out with an infrared camera like PANIC 1s shown bellow 1 Instrument setup this includes read mode RRR CDR Fast saving modes FITS cubes individual integrated saving paths filenames log files etc 2 Darks before starting observations we take dark images using several integration times and coadds 3 Twilight dome flat fields we take flat images for each filter that we are going to use during our observation 4 Focus we measure the focus in one filter for the other filters the telescope computes the focus using the programmed offsets Usually the GUI provides different fields for focus and the user select a field close to the zenith During the night we can check the seeing and repeat the focus procedure if needed 5 Calibration stars That loads the standard object list and observes the standard stars in each filter we are going to use Then a dithering sequence for these observations number of positions and offsets is selected 6 Target fields That loads project objects lis
160. o that pixel scale The nominal length from the external part of the window to the detector is 1925 36 mm for both scales The curvature radius and thicknesses of the lenses are given at 80 K working temperature of PANIC For manufacturing and assembly those parameters have to be replaced by warm parameters using thermal expansion coefficients defined in ORD4 Curvature radius Thickness or Separation Element mm at 80 K mm at 80 K Aperture mm PI Cryostat window E 20 0 IR Fused Silica 291 2 Plane 424 9674 LO 33 6 IR Fused Silica 247 0 Plane O ee 145 0 MI Plane 28 0 TBD BK7 276 3 Zerodur or BK7 pe fe geg UE IBD ei 1 Dan 0 Vacum NN 027 281 1478 Sg AAA wem 251 2363 qo oou ovem 00 144 1806 E o a 217 6609 6469 551 eg Table 3 2 4 Prescriptions data of the common elements of the optical system at its nominal design temperature PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 52 of 183 Curvature radius Thickness or Separation BRE M oo 1 82 2 Vacum ma 6815 IR Fused Silica 118 4 121 EE Vacum a 4817 S FPL51 146 0 212 RS Vacum ee 7703 E SFO3 144 6 SE 1 29 124 a S FTM16 105 2 EN 5234 Vacuum Fee RS LIM DO MIIL ag Table 3 2 5 Prescriptions data of the elements that only belong to the 0 45 px scale 3 2 6 2 3 0 45 px descriptions In this sec
161. oes not produce all the required darks to process a night s data a suitable combination of closely related dark frames will be created and used instead 3 Flatfield division in order to correct for pixel response non uniformity in the detector Twilight or dome flatfields can be routinely taken from the daily observations by combining as many flats as are generally available for each time and readout mode Also weekly flatfield sequences can be taken dark corrected and then stacked to form intermediate master flats 4 Bad Pixel Correction The bad pixel values dead hot or cold pixels will be replaced by a representative count level determined from good pixels in the local neighbourhood The defect pixels will be marked in a bad pixel mask by a value 1 whereas the position of good pixels shall be indicated by 0 3 5 4 8 3 1 2 Fringing PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 168 of 183 At the time of writing we have no way of knowing what effect fringing will have on data from PANIC Some infrared detectors are badly affected by 1t and some are not affected at all WFCAM It appears to depend upon the final f ratio of the optical system the properties of the top layer of material in the detectors and the presence or not of atmospheric emission lines in a particular waveband It 1s also true that a background sky correction may remove any fringing that 1s present 1f the sky es
162. of mirror M1 due to gravity in z direction 113 Figure 3 3 2 25 Optics mount 2 with mechanical decenter adjustment of lens L2 with micrometer screws exploded view sess 115 Fiare 3 9 2260 5660 Or ODUCS MOUNT Zi eege 116 Figure 3 3 2 27 Section of the one pixel scale design similar to Figure 3 3 2 1 118 Figure 3 3 2 28 Cold bench and optics of the one pixel scale design similar to Figure 3 3 2 2 et 118 Figure 3 4 1 1 new ROE left versus old ROE oeh 121 Figure 5 4 12 ROCom block dar E 122 Figure 5 3 1 5 AD936 block Olarra ici 123 Figure 34 1 4 AH2RG CB block dilata narran 123 Fi ure 3 4 1 5 OPTPCI block aa EE 124 Figure 3 4 1 6 single channel of the CA36 board cocooooocccccooocococnnononococononanananonononononnnnccnnnnanannnns 125 Figure 3 4 1 7 Protection circuitry on Clock Bias board essere 126 Figure 3 4 1 8 preamplifier protection circuit 126 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 22 of 183 Figure 3 4 2 1 PANIC Control System Simplified Block Duaoeram ccc cccccceeeeeeeeeeeees 129 Figure 3 4 2 2 Principle of motion control gwsatem eene 130 Figure 3 4 2 5 Vacuum stepper motor Via 132 Figure 34 2 8 Resolver Type RE rodada li asd a Yuri gud desde ec 133 AA on 133 Figure 3 4 2 10 Instrumentation rock 135
163. oftware team will try to have some of them ready at first light 3 5 3 6 2 1 Master calibration frames The science pipeline shall compute maintain and update a series of master calibration frames darks flats skys hot bad pixels masks to provide a basic instrumental signature removal for the quick pipeline 3 5 3 6 2 2 Dark current substraction Dark current frame shall be scaled to the real integration time and subtracted from the science image 3 5 3 6 2 3 Flatfielding correction The pipeline shall divide the science image through a normalized flatfield image to correct the sensitivity variations across the detector 3 5 3 6 2 4 Bad hot pixel removal The bad pixel values dead hot and cold pixels shall be replaced by a representative count level PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 146 of 183 3 5 3 6 2 5 Fringe correction It is not clear that PANIC will have fringes but in case it has they should be removed by the pipeline Fringing correction should be considered at the commissioning stage 3 5 3 6 2 6 Cosmic rays removal When present the cosmic rays shall be removed using a suitable algorithm 3 5 3 6 2 7 Sky modeling The high background from the environment and the sky with additional temporal and spatial variability of the latter produce the main background signal A fast computing of sky modeling shall be computed and it shall be subtracted from
164. oiding wrong parameters values or nonsense sequences In any case the checking process should not block user entries it should only warn about them 3 5 3 4 11 Execution Control Once the observation 1s defined by the user and validated the OT shall allow users to execute pause resume or abort the observation sequence at any time 3 5 3 4 12 Output scripts For each observation defined this tool shall produce a list of GEIRS instructions commands 1 to carry out the planned sequence but they should not be managed directly by the user 3 5 3 4 13 Extra keywords The OT shall provide a set of extra info keywords to write in FITS files In that way we can ensure that the quicklook tool and the pipeline will work in an appropriate way These extra keywords should also facilitate the data archiving and subsequent data searching 3 5 3 4 14 GEIRS Functionalities The OT should provide the same GEIRS functionalities and new ones with higher abstraction level for the observer In one way the aim of this tool is to replace the current O2k MIDAS scripts and GEIRS commanding and provide and enhanced graphical tool to edit and build new observation scripts using GEIRS command via a well defined TCP interface 3 5 3 4 15 Secondary mirror focusing OT should provide an item to program a focus sequence but it shall not calculate best focus offsets for the secondary mirror for each filter it shall be done by quicklook utilities Be
165. olution mode nn nnnnnnnnnnnnnnnnnnnnnnnnnnnh nnns siiis sss isis sisi siii iis 47 EA LI Evi m TES 47 ENS an A Vr 47 NEE MS CANA TEE D nn E 47 De OCS TOIT a esata tosses ea E A 48 3 2 6 1 PANIC Geperal Optics lay OU sata 48 20 9 2 A ne ee eee ne ee ee oe eee 50 Pe EN WT Ee Ope ec OE 1 eee eae eee S eee ey nea ee ee eee ee eee 50 3 2 5 2 2 10 45 EIERE onda 51 A E te macnaseuascniconngatesosmacniensaaceeceenacs 52 320 24 QA px optical perl ormante sirasi R E E 55 3 2 6 2 5 0 45 px Ensquared Energy and Spot duagrams 56 EA E A oe eee re ee eee eee eee 59 e E AS EN ARSS e EE 59 3 2 6 3 A A A EE 60 SL DIS POPE O sis 60 EE 61 E TT EE 61 3 2 0 4 20 25 px optical ee EE 64 3 2 6 3 5 0 25 px Ensquared Energy and Spot duagrams nennen 65 225 2 0 U23 S US EE 68 3 2 6 3 7 0 25 px Transmission ccccccccccccceeeeeceeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeess 68 DA MEME D mem T ieee antes 69 3 2 6 5 SE ET oe ae ey eer erence ae eee ee 71 SES SM NEME io RE 71 ERE S CO 3 A 72 EE EE 73 du A 75 3 14 Tolerances forthe 0 45 PSA isos er IEEE Ei 77 Jal Tolerances Torthe 0 25 EE 81 UD EP 0 O ES PUE O e o ee er 85 E GG 7 86 3 3 CRYOSTAT AND VWIECHANISM KEE 87 3 3 1 OC OST AA sense ae gaa cee E sete aetna seeds esata aes teeta 87 3 3 1 1 MM E E A 87 PA T EE 87 ENN A 87 Saeba TE EE 87 CNN P Pe eee cas eon ees c
166. on Iterator To perform any complex observations iterators are required They are placed into a sequence of an observation and are used to define the series of actions that will be performed to collect the data It will allow you to change in a single step any configurable attributes of an item For instance with an iterator we can set up a series of iteration steps each of which simultaneously changes the selected filter readout mode integration time repeats and positions as defined for a instrument setup e Filter e Scale Mode 0 45 arcsec or 0 25 arcsec e Readout mode e Integration Time IT e Repeats R e Positions P Offset Pattern dithering pattern mosaic pattern e Number of points e Offset p q Observation Frame dark sky flat dome flat focus seq science e Number of Exposures N An Observation Program OP can be defined using a notation described below This description aims to show all the possibilities feasible with the OT PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 162 0f 183 OP Setup Element Target Observing Block Setup Element Observation Constraint gt lt Instrument Setup lt Data Store Setup gt lt Data Reduction Setup gt Observation Block lt Target gt Sequence y Sequence Instrument Config Iterator Offset Pattern Observation Frame gt Observation Frame lt dark gt flat focus
167. or component level allowing a quick engineering and science verification The barrels with decentering compensator will be assembled with an interferometric adjustment and during the integration the compensator in distance will be adjusted For Barrel 1 which does not have adjustments proposed the alignment will be verify All the sub barrels will be cryogenically verified Finally the whole instrument will be assembled and tested as we do not expect to need further adjustments than the mounting tolerances the only adjustment to be done 1s the one for the detector in position and tilt A more detail explanation has been done in the technical note referenced about the AIV PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 86 0f 183 BARREL 1 BARREL FILTER WHEEL Figure 3 2 8 1 Opto mechanical layout showing the main assemblies regarding the optical elements 3 2 9 Conclusions The nominal optical design meets desired performance criteria and contains margin to be applied to fabrication and alignment tolerances To achieve this an specific control plan during integration phases should be considered In the following phase a deeper study of the tolerances and quality compensators environmental change and stray light will be done The design contains only spherical surfaces i e no conic or aspheric surfaces and special care has been taken in the selection of lens mater
168. ors 1s the physical flatness of 40 um peak to valley from the best fit plane and its effect on the optical quality Calar Alto 2 2 Telescope Focal ratio f 8 Plate scale 11 7 mm gt 1 85 um PANIC Scale 18 1 E 40 um 0 45 Then the focal ratio at the detector 1s 40 8 f 3 76 118 m fl On the other hand Then PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 40 of 183 66099 Now considering different r values With a physical flatness of 40 um peak to valley from the best fit plane the blurr will be of approximately 10 um Considering also the seeing at Calar Alto 0 6 at 40 um the blurr is 24 um Adding this values leads to Total blurr 24 10 26 um Which means that the optical quality is mostly dominated by the seeing and not by the factor introduced by the physical flatness of the detectors 3 1 7 Characterization The detector characterization will be done at MPIA using the existing cryogenic test equipment for IR detectors and the real PANIC readout electronics The final detector control system PDCS computer and software shall be used The cryogenic test equipment allows to change detector temperature insert a filter and blank off any light by cold light tight baffles This setup has also been used for other projects using HAWAII 2 detectors e g LUCIFER I amp IL LINC NIRVANA Omega2000 etc Using the real
169. ot nog A M 95 Iagure s 2 2 2 Cold bench and opis eene 96 Figure 3 3 2 3 Entrance WIOdOW oooooooccncnnnnccnnnnnnnnnnonnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnn ono nnn nnns nnns eren enne nnn 96 Figure 3 3 2 4 Cold optics of OMEGA2000 with spring loaded cryogenic lens mount 98 Figure 3 3 2 5 Displacements of lens and retainer ring due to thermal shrinkage during cooling from room temperature to 77 K The arrows in axial direction show movements relative to the lens mount supporting surface a All parts at room temperature b Lens mount cooling lens and ring still much warmer c Cold lens mount lens cooling retainer ring still much warmer d Cold lens and lens mount retainer ring cooling 99 Figure 3 3 2 6 Optics wheel without housing eese 101 Figure 3 3 2 7 Section view of optics wheel unt 102 Figure 3 3 2 8 Optics wheel ball bearing detail view of Figure 3 3 2 7 ssssss 102 Figure 3 3 2 9 Detail view of optics wheel and filter unt 103 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 21 of 183 Figure 3 3 2 10 Filter wheel unit with four filter wheels 00 0 0 cccceceeessseeeeeeeeeeeeeeeeeeeens 104 FHiette 5 2 21 T Pier wheelwithdnive EE 104 Fistte 3 3 2 12 Detail View of ler Wheel eodera meut e enit deu rior ici 105 Figure 3 3 2 13 Rotating field stop total view and section
170. oups o 3 5e 005 7e 005 um d x 1 75e 005 5 25e 005 Figure 3 3 2 20 Displacement of cold bench and optics with the telescope pointing to horizon gravity vector in y direction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 111 of 183 zl Figure 3 3 2 21 Displacement of cold bench and optics with the telescope pointing to horizon gravity vector in x direction 3e 005 6e 005 um 1 5e 005 4 5e 005 Y 2 5e 005 Se 005 um tC e 1 25e4 005 3 75e 005 Z Figure 3 3 2 22 Displacement of cold bench and optics with the telescope pointing to zenith gravity vector in z direction PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 112 of 183 3 3 2 2 7 3 Bending of entrance window The entrance window from Fused Silica has a diameter of 330 mm and a thickness of 20 mm The FEM analysis shows a maximum displacement of 33 2 um due to a differential pressure of 1 bar and a maximum stress of about 4 3 N mm2 which is about 1 11 of the rupture modulus of fused silica 0 5e 004 1e 005 um z 2 5e 004 7 5e4 004 e Y Figure 3 3 2 23 Simulation of entrance window deformation due to a differential pressure of 1 bar The following equation from 1 gives a max deformation of 63 um max deformation 0 696 p r E with p differential pressure 10 Pa r effective rad
171. pattern control PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 139 0f 183 e the handling of the reference pixels which surround the detectors and are automatically clocked together with the data only 2040 of the 2048 pixels in each detector direction are science data e the saving of the 4 detector science data units in an appropriate FITS format the guiding processing directly with the science detector in the science FOV some time after the first light 3 5 3 3 2 4 Telescope GEIRS shall provide a telescope interface which e allows all necessary telescope commands e contains a GUI to show and control the telescope activities focussing positioning e should show the status information of the open dome segment limitation the dome segment shifting is not done automatically but has to be started manually e allows the control of the focus depending on the used optical elements in the beam 3 5 3 3 2 5 OT GEIRS shall provide a complete command interface via external shell commands and or via the command server interface to the OT GEIRS should provide a status interface informing regularly about a configurable parameter set on a selectable time base of the order of seconds 3 5 3 3 3 Data GEIRS shall e offer a FITS keyword interface which allows to configure the FITS header keywords specific to the instrument and add externally supplied keywords about
172. pecific morphology Halo streams across the galactic plane would be traced using colour selected M stars as has recently been demonstrated to have spectacular effect by 2MASS 2 3 Stellar evolution star formation exoplanets 2 3 1 Accretion disks of young stars NIR monitoring of young stars most of them low mass stars show variations due mainly to changes of the innermost parts of the disk Simultaneous zJHK photometry would allow studying the variability of the disk H and K bands and maybe the J band at the same time that the stellar photosphere is monitored in the z band Hot stellar spots thought to induce the changes observed in the inner disk leave also a fingerprint on the H and K bands that would be removed before that data are fitted by theoretical models of the disks Polarimetric measures can provide in these systems information on the geometry of the system since light becomes polarized after dispersion reflection in structures like the inner cavities of the disk etc 2 3 2 Search for post AGBs 2 3 3 Post AGB stars are enshrouded by a dusty CSE which becomes optically thinner at NIR wavelengths NIR emission is primarily emitted from the reddened photosphere and from light scattered by dust grains Polarimetry would also allow discriminating between the faint polarised scattered light from the dusty envelope and the bright unpolarized emission from the central star This enables the imaging of material that would normal
173. perature diode DT 670 wide useful temperature range from 1 4K to 500K Heating Element Power resistor Quality of vacuum preasure inside the cryostat Device Vacuum measurement system dual channel device pfeifer TPG262 connection for two gauges measurement range from 5x10 11mbar up to 55bar PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 129 0f 183 Transfer of data between serial interfaces and ethernet Device Serial device server Nport 5610 xx up to 16 ports supporting RS232 10 100 Mbps Ethernet 15kV ESD surge protection for all serial signals 3 4 2 2 General electronics concept 3 4 2 2 1 Overview The PANIC instrument control electronics is based on the computer infrastructure of Calar Alto Standarized Calar Alto instrumentation boards and devices are forseen The connection to the instrument workstation 1s realized via a Local Area Network The central process computer for PANIC is a x86 multicore PC Most of the other function units are independent intelligent devices The following table shows the chosen devices and their manufacturers x86 multicore PC Nport server Nport 5610 xx MOXA Motion Controller MPIA Read Out Electronics MPIA Temperature Monitor Model 218S Lake Shore Vacuum measurement system TPG 261 Pfeiffer Vacuum GmbH Temperature Controller Model 3318 Lake Shore Table 3 4 2 1 Summary of electronic devices 3 4 2 2 2 Simp
174. r and schedule 4 2 Work Packages Since PANIC is build by two institutions it is necessary to split the whole project into well separated well defined work packages in order to minimize internal friction and traveling We have also assigned the work packages according to the experience of each institution The project was split into the following work packages e Optics the optics calculations are done by IAA under guiding by MPIA since this is new to IAA IAA will also contact the manufacturers monitor the test protocols during fabrication and will also take care of specifying and ordering of the filters Since MPIA has more experience in these affairs MPIA will be contacted and informed at each step e Mechanics MPIA will make the design of the whole instrument detail the drawings of the cryostat as required by industry and take care of fabrication of the cryostat by local industry Wheels and lens holders will be designed and manufactured at MPIA IAA has already participated in the design process and has interest to continue e Instrument hardware and detector control Will be included in MPIA GEIRS software MPIA will also take care of testing and optimizing the read out of the detectors e Read out electronics The read out electronics is build at MPIA based on previous systems This includes also firm software to store the data in the computer memory so there is a clear cut division to the data retrieval software e Control
175. r and the screws For a true run tolerance of the wheel a very tight fit between the ball bearing and its surrounding parts has to be achieved This is hard to achieve with the surrounding parts made from an aluminium alloy and the bearing made from steel A slightly too tight fit e g between the bearing outer ring and the wheel mount see Figure 3 3 2 7 will lead to a damage of the bearing because the steel has a shrinkage from ambient to liquid nitrogen temperature of about 0 3 whereas AIMg4 5Mn shrinks by 0 39 This problem 1s solved by two stainless steel bearing support rings both inside and outside the ball bearing see Figure 3 3 2 8 These rings are solid enough to keep the stress away from the bearing which the shrinking wheel mount tries to introduce So a high true run accuracy of the wheel can be realized by tight bearing fits over the whole temperature range In most cryogenic wheels the ball bearings are the thermal bottle neck for the cooling down or warming up process This 1s because the bearings are made from stainless steel which has a rather poor heat conductivity and because there are only point contacts between the bearing rings and the balls From experiments which were made during the development of the cryogenic wheels of LINC NIRVANA we can estimate that the whole unit will be cooled down from ambient temperature to 77 K after about 30 35 hours PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIM
176. r negative in sign and may also even cross from one detector to another In a stable environment it is feasible to measure the contribution of crosstalk from one channel to another by using bright point like sources and thereby define a comprehensive crosstalk matrix C Since this is environment specific determining the final form of this matrix will be one of the commissioning tasks although earlier laboratory based measurements will be used to characterise its likely impact and to investigate ways of minimising the effect Providing the cross talk terms are small 1 e lt 1 the most likely scenario then the following simple single pass additive correction scheme will be used to correct for this problem l l 2lCu where I is the observed frame and I the corrected version 3 5 4 8 3 1 6 Optical ghosts removal At the time of writing this document we have no way of knowing what effect ghost images created by the different filters will have on the data from PANIC However if they are present and they shall be characterized and available to the data reduction pipeline to remove them 3 5 4 8 3 1 7 Field distortion correction Due the large field of view of PANIC it 1s supposed that a field distortion correction will be needed To do that is necessary the field distortion created by the optics 1s characterized and available for the data reduction software 3 5 4 8 3 1 8 Mosaicing As the focal plane of PANIC is populated with d
177. rdware is build and or assembled here Thus we will have the support from MPIA s well equipped mechanical and electronics shops In addition MPIA has laboratories suited for such purposes and a large park of all kinds of equipment both electronical and mechanical For the tests of detectors MPIA has a test dewar which is large enough to house the FPA Influence of gravity on the instrument functionality of movable parts optical quality can be checked by means of a mechanical mounting system which allows the instrument to be moved in any direction We intend to hire a student in the lab test phase probably also for the commissioning runs IAA will participate in this phase 4 5 Manpower In the following table we list the manpower required for the progress of the project according to the schedule in units of man months The numbers for 2006 and 1 2007 are really allocated time the rest of the table estimates The listing corresponds to the departments at the institutes Instrumentation group at MPIA comprises participation in the grand design of the cryostat test of the detectors individually and optimization of the read out process for the array Software MPIA includes read out of the array and hardware control Design IAA means participation of Marcos Ubierna during design and integration 2006 2007 2007 2008 2008 2009 2009 2010 2010 2011 2011 Optics SEENEN 42 se co MPIA a AA Mech Mechshop POIS PORO
178. re in requirements D x 1 5 GRID DISTORT LON INSTITUTO ASTROFISICA ANDALUCIA H MILLIMETERS LA O 0 PANICI MI TR Qz5 MULTIBRM ZMX 2 2080 um CONFIGURATION amp OF Figure 3 2 6 27 Distortion plot for the 0 25 px camera 3 2 6 3 7 0 25 px Transmission In Table 3 2 18 and Figure 3 2 6 28 are the values and the plot respectively of the expected transmission as function of the wavelength which has been calculated with the same considerations as the 0 45 px scale Table 3 2 18 Values of the expected transmission for the 0 25 px scale PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 69 of 183 MISI MISSION m TRANS au id Bleu 1 6566 WAVELENGTH IN Aa TRANSMISSION VS WAVELENGTH m INSTITUTO ASTROFISICA ANDALUCTA FIELD POS 8 08000 0 0000 DEG CONCHI CARDENAS FIELD IS UNPOLARIZED PANIC V1 COMPLETE TP CDRTIMG ZHX CONFIGURATION z OF 2 Figure 3 2 6 28 Expected transmission for the 0 25 px camera 3 2 6 4 Filters The filters are placed close to the detector between L7 and L8 in the convergent beam and we have proposed filters with 125 mm of diameter The thickness is not jet exactly determined because we have found some different criteria and we have not had the confirmation of the manufactures to achieve completely the optical quality requirements that we have asked for the filters depending on the filter thickness That filters location
179. read noise instead of background 7 0 low background faint objects 100 kHz 16 16 1 5 26 4 Exposure gt 30s PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 157 of 183 3 5 4 5 4 Guiding Guiding requirements shall be supported by the development of the ROE and the pattern development for the read out modes The extensions of the Hawai 2RG allow to use 2 nested clockings without skipping needs and the possibility to reset only a part of the detector But the clocking 1s not parallel and the photon sensitive pixels are accessed by both clocks The 2 nested clocked data output from the detector shall be splitted by GEIRS into 2 independent data streams The guiding processing part should be implemented after commissioning of PANIC itself but shall be foreseen and the ROE shall be in principle prepared for these nested clocking patterns and first tests shall be done Software modules for CCD cameras already exist to calculate the centroid of the guide star e g LAICA minimal minimal always each of maximal e E S full fix full 100 kHz win size guide science win rate science clocking win rate unc Gan wins done each full Bl wins done at fix rate line 418 Hz 418 Hz 329 Hz 1024 83 Hz Table 3 5 3 Some estimated timings for multiple guiding windows embedded between normal full frame read out lines 3 5 4 5 5 Parts 6 36 1296 36 36
180. remove most of the field dependence of any wavelength shift due to the change in incidence angle with field over the filters For interference filters because the focal ratio of the camera and the change in the incidence angle with field over the filters the expected filter performance will suffer a broadening of the apparent band pass a depression of transmittance values and a shift to shorter wavelengths For broadband filters the effect is negligible For narrowband filters we have to calculate carefully this effect and determine the incidence angle which is a flux weighted mean of the final converging beam to specify to manufacturers the filter to operate at that angle In Figure 3 2 6 29 and Figure 3 2 6 30 we show the angle over the filters in the position that they are located the angle on top is the semi cone due to the focal ratio of the camera and on the bottom is the angle variation over the filter due to the field Due to the constrains imposed during the optical design we do not expect any problem with this even for 1 narrowband filters PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 70 of 183 3D LAYOUT PANIC1_V1_COMPLETE_TP_FILTERS ZMX KT aleet LOM 1 Figure 3 2 6 29 Angle over the filters for the 0 45 px camera e LBEOUI INSTITUTO ASTROFISICA ANDALUCIA CONGHI CARDENAS PANIC1_V1_COMPLETE_TP_FILTERS ZMX CONFIGURATION 2 Figure 3 2 6 30 Angle ov
181. rent behaviour for msr and sar see ADI e cycle type also called read out cycle mode type is a specific read out pattern of clocking logic The result of a single read out is normally a single image but the read out raw data might consist of multiple frames exception msr which has multiple images as result of a read out cycle e cycle time is the time of the total cycle type pattern It is always larger or equal to the integration time e single correlated image means that the read out type produces no time correlated read out frames but only a single read out frame normally after a detector reset which still contains typical detector properties e double or multiple correlated image means that the read out type produces two or more read out frames correlated in time which are used to get rid of the pixel dependent time and offset properties Only amplification dependencies of the pixels and imaging dependencies of the instrument or photonic sources as well as some kind of noise remain in the correlated images 3 5 4 5 2 Read out with high speed The detector shall be clocked at minimum speed with 100kHz pixel clock rate Additionally 1t shall be clocked with a faster maximal speed because a 1 kHz image rate for a sub window of the size of about 35x35 pixels is required in Ad2 To prevent edge effects to the rest of the detector the pixel count for this requirement 1s increased by an additional pixel read around the
182. resent at Calar Alto 3 6 3 4 Software 3 6 3 4 1 The disk organization will be as follow 3 6 3 4 1 1 One disk for the system installation boot swap and partitions PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 175 of 183 3 6 3 4 1 2 One disk for the whole instrument software disk a 3 6 3 4 1 3 One or more disks for data disk b 3 6 3 4 1 4 Filesystem ext3 3 6 3 4 2 The system installation will be done by Calar Alto staff according to its own standards SuSE Operating system and Pc based computer 3 6 3 4 3 Before first light Calar Alto needs a full backup of all necessary software installed in the computers necessary for the normal operation This backup system will be tested before first light CAHA requirements for PANIC August 2007 3 6 3 4 4 Any non standard part in the Pc shout be acquired together with a spare part 3 6 3 4 5 Regarding software the final documentation should include 3 6 3 4 5 1 Disk structure 3 6 3 4 5 2 Directory structure for the software 3 6 3 4 5 3 Start and user scripts 3 6 3 4 5 4 Test scripts help programs and debug 3 6 3 4 5 5 Description about Log files 3 6 3 4 5 6 Changes done in the standard operating system 3 6 3 4 5 7 Normal programs installed in the system 3 6 3 4 5 8 Description for the different versions if available 3 6 3 4 5 9 Description about the network structure 3 6 3 4 5 10 Hardware and software
183. ric mode since the IR emission from X ray binaries can be intrinsically polarised because of light scattered within the system or because there is a significant synchrotron emission at high frequencies from a compact jet 2 3 6 Asteroseismology Phase shifts between different colours increases significantly toward the infrared for non radial pulsating stars Time series analysis extended to the NIR increases dramatically the pulsation modes identification allowing real asteroseismology of main sequence stars 2 3 7 Supernovae searches The large FOV of PANIC will allow observing large portions of individual clusters of galaxies or even whole ones at the same time boosting the rate of supernova detections Once detected multiband light curves YJHK could be constructed a relevant issue for the calculation of the total SN luminosity PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 32 of 183 2 3 8 Active stars Photometric time series extended to the NIR constrain the theoretical models of active stars showing photospheric solar like activity cycles and give information about differential rotation and temporal and or spatial correlations between inhomogeneities at different atmospheric levels 2 4 Solar system 2 4 1 Trans Neptunian s minor bodies A survey to study NIR colors and short term variability of a good sample of TNOs centaurs and other minor planets could be performed
184. s It has been divided in three main categories related to the optical integration process from components manufacture and tests barrel integration subassemblies and tests and system integration and final engineering tests To design this plan it has been necessary the identification of the adjustments and compensators which come from the tolerance analysis given in section 3 2 7 The different tasks and tests regarding each integration stage are described at each level components subsystem or system The optical elements of PANIC are grouped in five main units as shown in Figure 3 2 8 1 e Barrel 1 LO M1 M2 M3 e Barrel 2 L1 L2 L3 L4 cold stop e Barrel 3A and 3B L5A L6A L7A and L5B L6B L61B L7B respectively e and Barrel 4A and 4B L8A and L8B respectively e The fifth unit is the Optics Wheel Barrel 3A Barrel 4A and Barrel 3B Barrel 4B respectively which place the optics according to the desired plate scale The optical AIV process will have two independent responsibilities The optical elements manufacture will be accepted at the optical shop as individual elements and the integration of these lenses in the barrels and in the full instrument will be done by the PANIC team The rationale behind the integration process 1s to test the functionality of the different pieces at each integrating step as these are being integrated In that sense the system integration and verification should not display any fault at the subsystem
185. s stellar density presence of hot stars total mass and or age The long integration times will be split into several epochs along a few years in the way of a photometric monitoring This variability survey could detect new eclipsing binaries transiting planets stellar variability rotational periods etc 2 3 4 2 Testing the brown dwarf ejection scenario a survey around Bok globules Since in large star forming regions there is a problem in distinguishing the early brown dwarf halo from mass segregation due to interactions it is advantageous to study the distribution of brown dwarfs around more isolated and much less massive systems containing only a few objects like Bok globules A dozen Bok globules would be observed in three bands J H and Ks depending on sensitivity and contaminant rejection potential Escaping brown dwarfs detections will be confirmed by spectroscopic and astrometric follow up 2 3 5 X ray binary counterparts Identification of counterparts of X rays binaries can be performed at NIR wavelengths particularly of massive ones so that high extinction areas towards the galactic disk and or centre can be searched Ellipsoidal variations due to perturbations in the shape of the donor star can be detected and multiwavelength photometric data can be modelled to infer whether the emission is due to the companion star accretion disc or a possible relativistic jet This scientific case would also benefit from a polarimet
186. s document 3 6 3 2 Mechanics 2 1 The maximum measurements for PANIC including transportation car are limited by the elevator dimensions namely 190 cm wide 130 cm deep and 200 cm high 2 2 Maximum height at the telescope flange is 165 cm without car 2 3 Filling and vacuum pipes should face North 2 4 The vacuum valve should be similar to the one used on Omega2000 2 5 Transport car requirements 2 5 1 Inflatable wheels for a smoother transport 2 5 2 Hydraulic elevation system for an easier mounting at the telescope 2 5 3 Good access to vacuum and N2 filling pipes 2 5 4 Good access to electronic plugs for diagnostics in the lab 2 5 5 Possibility to tilt the instrument is desirable 2 6 Maximum weight for PANIC is 400Kg 2 7 The instrument must adapt to the telescope flange Specifications can be found in the Engineering Book where the flange drawings are numbered as 563951 drawings 1 to 3 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 174 of 183 3 6 3 3 Electronics 3 6 3 3 1 The electronics Rack can be mounted under the mirror cell independent of the cryostat This means that the cable length between the electronics rack and the cryostat will be about 4m CAHA requirements for PANIC August 2007 3 6 3 3 2 To guarantee the best technical support CAHA needs a full spare electronics set 3 6 3 3 3 Before first light Calar Alto staff needs a full documentatio
187. seeseceeacseeesiaces 109 3 3 2 2 7 2 FEM simulation of a detailed model 110 3 3 2 2 7 3 Bending of entrance Window nn rra nennen nennen nns 112 3 3 2 2 7 4 Bending of mirror M1 due to oravity nennen eene 113 A MEME uda A PERO 114 3 3 2 2 9 Total weight limit and possible solunonsg ccc ccccceeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeeess 117 O A 120 Se GE 8 Ope EE O ro ee ee ee etre ere ee 120 3 4 1 1 DODDE uc puis UM EE 120 A E 120 SON MEE e IOMA e M 120 34 131 ROCon R adOut eu EE 122 3 4 1 3 2 AD36 36 channel analog to digital converter 22 cccccccccecceeeeeeeeeeeeeeeeeeeeeeeeeeeseeeeeeeeeeeeess 122 3 4 1 3 3 H2RG CB HAWAII2RG Clock Bias board ooocccccccccnccncncnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnos 123 S134 BPO 6510 WACK AIG eerte EH pps end oe Tcl ao hes at E EEEa 124 A o Alaro oe oeaeug eateceumontsaraatencien cane te RON IRVIUNI E DEPNN SEU EUUUE 124 3 4 1 3 6 CA36 36 channel cryogenic preamplifier ooooccccccnncnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnss 125 A Tone I PE 125 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 12 of 183 24111 5 8 Detector E eeh EEN 125 3 1 1 2 9 Troubleshooting Did nos stees 126 za e 128 3 4 2 1 a MM A MEME ted iium E in Ehe Uer 128 2 122 General electronics e E 129 A O od Nm 129 3 4 2 2 Simplified block diagramm of instrument control electronics
188. sides GEIRS shall include offsets for each filter into its configuration parameters but the calibration of the focus offsets for each optical element should be a maintenance calibration template PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 143 of 183 3 5 3 4 16 Simulation It should be possible to use the OT in two simulation modes 1 GEIRS and therefore the camera and telescope is not present In this mode it should be possible to carry out a observing sequence simulation 2 GEIRS is present and in simulation mode too so a full testing of the OT can be done 3 5 3 4 17 Observing Modes It shall be possible to execute PANIC observations in situ and in service mode A remote mode outside CAHA should only be available via ssh X tunneling for engineering support 3 5 3 4 18 Efficiency The OT shall not compromise the efficiency of the observations 1t shall only improve the efficiency of the observations 3 5 3 4 19 Flexible The OT shall be flexible enough to allow running of different types of scientific programs and engineering tests 3 5 3 4 20 On Off line The OT shall work online by the astronomer at CAHA control computers and off line at astronomer computer When offline the user will be only able to define pre plan and save them for a further execution 3 5 3 4 21 Timeline Calculator The OT should generate a estimation of the time required for the observ
189. ssembly and integration of the instrument Any delay here clearly leads to a delay of the whole project Assumption 11 is delivery of the detectors until February 2009 as promised by Teledyne Past experience however has shown that this might be optimistic Furthermore it is also very important that all channels of all detectors work well assumption 111 Past experience however has shown that this too might be optimistic PANIC GEN SP 01 Code 22 October 2007 183 of 183 Date Page E z O Z 2 un EQ gt 2 lt Z 2 an z A mpeedjopu E ve uopezumdo E ee Sun BUILOIS SILOS Ei ze vru Er 83 a2uejda22 v EE o O we E e Bugeeu yoo A ez A INN E Oo qe ez paunu jo jquiass y amp Jo4 uo2 4jsul aJeA os El 1 no peal aJeAa pos OE 0 S33110453 9 O4UOS Ei a e 200 Em DIBSOW ydo 33 s10Jpajap Th lenpaipu ysay suoayap se vr ua sysay suopayep EE vi Hanap Ge LE A A O qM aanjoejnueu Seay Jayi El o aanjoejnueui sJapjou sus eunjoejnueui je1so 42 sjejap saiueu2aui 3 ubisap 24340 saiueuaaul A pos Sa sondo E anjoejnueur 4apa4o sondo E uoreziundo sondo loz mofe sdo v o auieusbuebJ0A AN
190. t otary Transformer 2 Figure 3 4 2 8 Resolver Type RE 15 S4 Figure 3 4 2 7 Principle of operation Operating principle A resolver is a rotary transformer that provides information on the rotor position angle 0 The stator bobbin winding is energized with an AC voltage R1 R2 This AC voltage is transferred to the rotor winding with transformation ratio Tr The AC voltage then induces the voltages S1 S3 and S2 S4 into the two output windings of the stator The magnitude of the output voltages vary with the sine and the cosine of the rotor position angle 0 because the two secondary windings are shifted by 90 3 4 2 5 3 Resolver Module RESMOD The ResMod V2 is a piggyback module designed for use with the UniMod board It contains a resolver to digital converter RD19230 and a frequency generator to drive the primary side of the resolver The resolution of the converter can be programmed to 10 12 14 or 16 bit The RD19230 has 3 digital outputs that emulate an incremental encoder l La ZA 00WMSs38 ur 83 E y Figure 3 4 2 9 RESMOD V2 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 134 of 183 3 4 2 6 Motion controlled units 3 4 2 6 1 Filter unit The filter unit has four filter wheels Each wheel is driven by a stepper motor The position feedback comes from an angular resolver that is mounted on the stepper motor axis Each wheel has one fixed reference position This
191. t and perform an observation of each field with each of the desired filters and then a dithering sequence for these observations number of positions and offsets is selected Each filter and field may require a different observing setup like exposition time coadds or dithering sequence PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 159 of 183 7 Twilight dome flat fields At the end of the night we can take flats for each of the filter that have been used during our observation 8 Data storage The data should be copied from the data repository to a removable device 3 5 4 6 3 Data Entities In order to get a set of accurate and unambiguous PANIC observation programs that allow to follow the general observing strategies described before we consider a hierarchical structure of the observation program with the following main entities shown in the next figure Observation Observation Program Constraints Data Store Setup Setup Element SE Data Reduction Setup Instrument Setup Observation Block Sequence Instr Config Iterator Offset Pattern Calibration Frame Observation Frame D ya Science Frame Figure 3 5 4 5 Data Entities where each entity is defined as follow e Observation Program An Observation Program OP is defined as a full set of observations that the observer sets up to achieve the scientific goal It contains most of the infor
192. t diagram of the 0 45 px camera 58 Figure 3 2 6 14 Distortion plot for the 0 45 px camera 59 Figure 3 2 6 15 Expected transmission for the 0 45 px camera 60 Figure 3 2 6 16 Optics layout of de PANIC the 0 25 px camera occccncnnnoooooooncnonnnnnnnnncnnnnnnnnnnos 60 Figure 3 2 6 17 Footprint of the 0 25 px camera FOV on the Entrance window left on the E A M M S 62 Figure 3 2 6 18 Footprint of the 0 25 px camera FOV on the M1 left up on the M2 right up and on Me M3 AE 62 Figure 3 2 6 19 Footprint of the 0 25 px camera FOV on the L1 left on the L2 right 63 Figure 3 2 6 20 Footprint of the 0 25 px camera FOV on the L3 left on the L4 right 63 Figure 3 2 6 21 Footprint of the 0 25 px camera FOV on the L5B left on the L6B right 63 PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 20 of 183 Figure 3 2 6 22 Footprint of the 0 25 px camera FOV on the L61B left on the L7B right P 64 Figure 3 2 6 23 Footprint of the 0 25 px camera FOV on the L8B left on the detector plane fabu d 64 Figure 3 2 6 24 Complete FOV of OheO25ipnx nennen nnne nnns 65 Figure 3 2 6 25 Polychromatic EE of the 0 25 px camera sse 67 Figure 3 2 6 26 Pol
193. t includes the optics requirements the optics layout and image quality a preliminary ghost analysis and stray light considerations optical tolerances analysis and a preliminary AIV 3 2 2 Introduction PANIC shall be a wide field infrared imager for the Ritchey Chr tien RC focus of the Calar Alto CAHA 2 2 m telescope The camera optical design is a single optical train that images the sky onto the focal plane at an optical speed of f 3 74 with a plate scale of 0 45 arcsecond per 18 um pixel The detectors are four Hawaii 2RG of 2k x 2k made by Teledyne mounted in a mosaic giving a field of view FOV of 31 9 arcmin x 31 9 arcmin The camera has been provided with a second smaller pixel scale of 0 25 arcsecond per pixel optimized for a 18 arcmin diameter FOV Special care has been taken in the selection of the standard IR materials used for the optics in order to include the z band and to maximize the instrument throughput This cryogenic instrument has been optimized for Y J H and K bands The mains challenges of this design are the correction of off axis aberrations due to the wide field available the correction of chromatic aberration due to the wide spectral coverage the introduction of narrow band filters 1 in the system minimizing the degradation in the filter pass band and the mechanical constrains in mass and torque at the Ritchey Chr tien focus of the telescope The optical design produces an internal pupil availabl
194. t sky flat fields with recommended sky flat fields focus test with recommended focus fields 3 5 3 4 7 Survey Mosaic definitions The OT shall allow to define a sequence of observations to make a survey mosaic observation 3 5 3 4 8 Templates The user can choose some of these templates or define his her own template for the observation In any case the observer can always do the observation without any specific defined template In this case he she will handle the observation with the PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 142 of 183 GEIRS control GUI or with the command line commands available also into GEIRS dither read save focus or other macros as in Omega2000 and new ones The OT shall provide a set of predefined observation templates There shall be at least three types of templates e calibration templates darks dome sky flat fields e science templates source and calibration objects e test templates used for technical maintenance of the instrument not available to users 3 5 3 4 9 Dome segments shift The dome segments shifting during an observation shall not be managed by the OT The OT shall only show a warning about these kind of events if they are provided by the telescope control system to GEIRS 3 5 3 4 10 Validation The OT shall check that the observation program specified by the user complies with the operational instrument rules av
195. the 0 45 ri E 56 Table 3 2 8 Bandwidths of evaluation of the PANIC optical design and their change in focus for A PP 57 Table 3 229 BESO inthe 0 45 TEE 57 Table 3 2 10 Distortion data in the 0 45 px scale nennen 59 Table 3 2 11 Values of the expected transmission for the 0 45 px scale 60 Table 3 2 12 Prescriptions data of the elements that only belong to the 0 25 px scale 61 Table 3 2 13 Summary of the PANIC performance in the 0 25 px scale 65 Table 5 2 14 Fields used 1n h6 0 25 DX SC 65 Table 3 2 15 Bandwidths of evaluation of the PANIC optical design and their change in focus A O AMA eed E 66 Table 5 215 EFESO mihe 25 PX Scale ainia 66 Table 3 2 17 Distortion data in the 0 25 px scale eene 68 Table 3 2 18 Values of the expected transmission for the 0 25 px scale 68 Table 3 2 19 Position and size of the Field Stop masks 71 Table 3 2 20 Position and size of the Cold Stop make 12 Table 3 2 21 PANIC ghost analysis for the 0 45 px scale 74 Table 3 2 22 PANIC ghost analysis for the 0 2Z5ipnxscale 74 Table 3 2 23 PANIC camera groups for the OA3ipnsscale 75 Table 3 2 24 PANIC camera groups for the O ipnsscale 76 Table 3 2 25 Manufacturing tolerances for individual elements for the 0 45 px scale Zu Table 3 2 26 Integration tolerances within the barrel 1 for the 0 45 px scale
196. the Calar Alto staff will try to solve this problems by themselves if necessary during the night with the possibility to change the whole electronics rack After this emergency repair they will try to solve the problem in the lab and if they need help they will contact the appropriate engineers at MPIA Heidelberg or at IAA Granada System backup copies will be made by the informatics group on DAT tapes or any other media if necessary as often as necessary normally once per month Programs backup will be made when there is a new program version The idea is to use the instrument computers pc only for Panic operation other activities like data reduction should be done on other computers and on separate disks in order to avoid interferences in the instrument operation In case that operating system patches must be installed Calar Alto staff will make a system backup before installing patches especially if they include the kernel In case that the Panic cryostat must be opened Calar Alto staff will take the maximum possible care to ensure a clean and electrostatic sure environment in consideration that actually there is no clean room available PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 178 of 183 4 MANAGEMENT 4 1 Summary In this document we describe management issues how the project 1s split into work packages how assembly and integration are planned cost manpowe
197. the range of 16bit or by storing the data in a data type of 32bit width 3 5 3 7 4 2 File structure GEIRS shall store an exposure independent of single image or integral image saving in a single FITS file But PANIC will have 32 Mbytes or 64 Mbytes of data per full detector array field and should ensure that the resulting file sizes does not get too large to handle GEIRS shall allow to configure the maximal size of a data file e g 1 GByte size limit and split larger exposure results into multiple files The preferred default file structure shall be the integral images of each detector stored as distinguished image extensions into a single multi extensions FITS file format But this implies proper quality in all single images without artefacts in one of them PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 149 of 183 On request it shall also allow to store the exposure image s into single FITS files or FITS cubes FITS files with NAXIS gt 2 GEIRS shall write single extended FITS file in the multiple extensions format MEF Each single or integral image is written in a single FITS header data unit HDU Each extension has its own FITS header but might inherit the primary FITS header This allows to add any count of HDUs to the file The order of the written HDUS are the same like above x y HDU window detector time single standard FITS file with 2 3 4 or 5
198. the verification of the configured backlash correction size which is used for correct positioning use a second reference switch additional to the home position switch as backup in case of problems with the single home switch in the not accessible dewar if no encoders or element position sensors are used for the device 3 5 3 3 2 3 Readout Electronics ROE GEIRS shall support the new MPIA PLX PCTI Interface to the ROE3 using a single device port with 2 data lines DMA channels the new Rockwell IR detector Hawai 2RG properties according to the requirements for PANIC 100kHz to 1 MHz pixel clock limited by the used ADCs read noise reduced read out modes full frame and sub window readouts nested with different frame speeds into each other for parallel guiding in the science focus field of view the read out of 4 detectors simultaneously via the 2 PLX data lines in full arrays and in fast sub windows and combined with the nested guiding readouts the acquisitions in time without losing data also for small 36x36 frames until about 200 to 256 Mbytes sec data rate from the detector the detector engineering and maintenance tasks by allowing detector patterns to be configured and handled by detector engineers during runtime without recompilation of the control software detector pattern engineering interface a data protocol added to the frame read out in front and at the end of a logical pattern clocking frame by the ROE3 via
199. tiffness of the cone is increased by 24 gusset plates The total mass of this structure is 33 kg The results of various FEM simulations including this telescope adapter are shown in section 319 227 Figure 3 3 1 6 PANIC telescope adapter PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 94 of 183 3 3 2 Mechanisms 3 3 2 1 Requirements All mechanical and optical components inside the cryostat have to be designed for a temperature of 77 K Their position and the position tolerances are defined in section 3 2 For test purposes all mechanisms have to work at room temperature also However there are no requirements for the position tolerances at this temperature The mechanics should be stiff enough to work for all telescope orientations with the required precision 3 3 2 2 Design Report The optical elements of PANIC are arranged in two groups These groups are mounted directly to the cold bench The first assembly optics group 1 consists of the mirrors M1 to M3 the lenses LO to L4 and the cold stop The lenses L5 to L8 are different for each of the two pixel scales and therefore mounted onto an optics wheel This wheel has two positions and is driven by a geared stepper motor The filter unit has four filter wheels with 6 positions each So in total 20 filters or 19 filters and a dark can be installed The opto mechanics is completely encapsulated to minimize stray light effects
200. timate 1s sufficiently local both spatially and temporally First we note that fringing 1s an additive effect so 1f removed as part of a procedure that used night sky data as a flat field source this would introduce a systematic error in the photometry To perform sky fringe removal effectively requires the flat fielding to be decoupled from the defringing by for example using twilight sky exposures to construct the flat field frames where the contribution from sky emission lines is negligible The basic method to remove fringing from images is to fit the fringe pattern from a library fringe frame to that of an observation frame by iteratively minimising the median absolute deviation of the difference of the two images This should work in principle so long as the fringe pattern is stable with time However experience shows that this 1s not the case The flux of the emission lines that lead to the fringe patterns can vary in a complex temporal manner which means the relative intensity of parts of the fringe pattern will also alter with time The way to get around this problem is to use data from the night in question to form mean fringe frames rather than to rely on a library frame which may be days or even weeks old As this can only be done once the whole night of data has been at least partially reduced this method of fringe correction will only be possible in the science pipeline 3 5 4 8 3 1 3 Sky modelling and extraction The princip
201. tion we present all the footprint for the optical components in the 0 45 px scale configuration from Figure 3 2 6 4 to Figure 3 2 6 10 LIME 20 MIL ETE 200 008 APERTURE DIAMETER 257 0000 FOOTPRINT DIAGRAM INSTITUTO ASTROFISICA RNDRL UCI IR D up INSTITUTO ASTROFISICA RNORLUCTR CONI HI CARDENA SURFACE 7 ONCHI CARDENAS PANICI V1 COMPLETE TP TRMR 0S ZNN 2AY Y MIN 84 5506 RAY Y MAX 64 5506 PANIC T U1_COMPLETE_TP_TAMA 0S SH CONFIGURATION 1 OF 2 MX RADIUS 17 5913 WAVELENGTH AL FIGURATION 1 OF 2 Figure 3 2 6 4 Footprint of the 0 45 px camera FOV on the Entrance window left on the L0 right METERS HE MILL CA aL 2601 AE CALE 5 APERTURE LITHMETER a HE SURFACE 11 RAY X MIN RAY Y MIN MAX RADIUS HI T 109 1 31 PANIC PRELIMINARY DESIGN REPORT ETERS H BE MILLI CA W zm D rob 60 A FOOTPRINT OLAGRAM RAYS THROUGH 63 98 A 45 INSTITUTO ASTROFISICA ANDALUCIA CONCHI CARDENAS cupeeace 1 RAY X MIN RAY Y MIN MAX RADIUS 166 RAY 1038 RAY arc JC X MAX Y MAX WRIUELENGTH 1089 96 PRNICI V1 COMPLETE TP Rn DS ZMK Ce Br L CONFIGURATION 1 OF 2 AL METERS 0000 MILL 200 SCALE AFERI URE DIAMETER 219 0239 FOOTPRINT DIAGRAM Fi 45 SURFRCE 17 RAY X MIN RAY Y MIN MAX RADIUS J5H3 RAY x MAX RAY Y MAM 161 WAVELENGTHS APERTURE LITHMETER 4 Code PANIC G
202. tometry was performed on a bright star of the field taking as a reference star the weighted average of another 7 stars on the same field Figure 2 shows the brightness difference between the bright star and the reference star for different values of the seeing that is for different ratios of seeing pixel size the pixel size of Omega2000 being 0 45 The scatter of the data points decreases as the ratio of the seeing over the pixel size increases The larger scatter is obtained for values of this ratio between 1 and 2 a seeing below the pixel size cannot be measured therefore 1 is a lower limit for this ratio A pixel size half of the seeing value or smaller ensures the best photometric precision Since a seeing of lt 0 67 is expected at Calar Alto for 51 of the nights a pixel size lt 0 33 should be available P LU or s aa E 2 Ro L tA s Te m L e E E u li m Fw e RE dum p Ze al e t e e d bL eques 2e j l z E r ae z L2 a a a amp E gef ez a L O e L b Sech Fm LU 1 4 d Seeing Pixel size Figure 2 1 Improvement of the photometric precision if a small pixel size compared to the seeing is used AKc mag PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 34 of 183 Cass om CAHA Original data E OBa AS dod 0 8 e 9 Se Se e Be B a e C kel A
203. under requirement because for a degradation of 3 maximum in the diameter the thermal contribution in the K band is negligible 9500 4388 9188 3687 MM 2 4000 SE JE AR 100 0000 MILLIMETERS ru SY Sch SCALE APERTURE DIAMETER 92 Del A RAYS THROUGH 80 717 o up INSTITUTO ASTROFISICA ANDALUCIA SURFACE 28 PUPIL CONE AT CARDENAS RAY X MIN 47 0651 RAY X MAX 47 M651 RAY Y MIN Sot Goal EAT 7 MAA if Gost EHNILIT VI IE E EE uk MAX RADIUS 47 4938 WAVELENGTH ALL CONFIGURATION 1 DF 2 Figure 3 2 6 32 Footprint at the Pupil position 3 2 6 6 Ghost analysis A preliminary analysis of ghost reflections was performed for PANIC in its two pixel scales The analysis of ghost images has been made by tracing first order all combinations of two reflections within a lens 1 e a ray from the axial object point is traced to the second surface from which it reflects back to the first surface and then reflecting from it travels on to the image This process is iterated for all the possible combinations of two surfaces The telescope surfaces are not taken into account in this analysis A 1 reflective coating has been applied to PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 74 of 183 all optical surfaces including the filter surfaces this consideration will aid in accurate computation of total ghost energy in Zemax We have analyzed the most critical components wh
204. v 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 132 of 183 3 4 2 4 PANIC motors 3 4 2 4 1 General Extreme Environment Stepper Motors from the company Phytron will be installed inside the PANIC cryostat These two phase hybrid stepper motors are build with special windings insulating material and adhesive This motor drives successfully the filter wheels of infrared camera 02000 Figure 3 4 2 5 Vacuum stepper motor VSS 3 4 2 5 Position and reference marks 3 4 2 5 1 Microswitches Microswitches will be used to indicate the reference position of all motorized units The selected switches are manufactured by Saia Burgess AG This type of switches have been successfully used in past cryogenic projects for example the infrared camera 02000 Characteristics Wide range of forces and variants Long mechanical and electrical life Solder PCB and faston terminals Rating 250 VAC 10 A max Dimensions mm 19 9x9 5x 6 4 Figure 3 4 2 6 Micro switch PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 133 0f 183 3 4 2 5 2 Resolver An angular resolver Type RE 15 1 A14 from LTN Servotechnik will be mounted on the motor axis of each filter wheel The resolver monitors the angular position of motor axis With a simple rotor modification of LIN Servotechnik this type 1s suitable for cryogenic projects S1 e esch R1 Mf D 4 T R2 Ro
205. v 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 145 of 183 The quick pipeline mode shall be operative at first light providing the following main features 3 5 3 6 1 1 Dark current subtraction Dark current frame shall be scaled to the real integration time and be subtracted from the flat field images 3 5 3 6 1 2 Flatfielding By dividing the science image through a normalized flatfield image the sensitivity variations across the detector shall be corrected 3 5 3 6 1 3 Bad pixel correction The bad pixel values have to be replaced by a representative count level determined from good pixels in the local neighborhood The defect pixels shall be flagged in a bad pixel mask by a value 1 whereas the position of good pixels shall be indicated by 0 3 5 3 6 1 4 Raw sky modeling The high background from the environment and the sky with additional temporal and spatial variability of the latter produce the main background signal A fast computing of sky modeling shall be computed and it shall be subtracted later from the science images 3 5 3 6 1 5 Shift and align Since the images will be shifted by the dithering offsets they shall have to be aligned prior to the summation 3 5 3 6 1 6 Fast Astrometry The quicklook should provide the possibility to make a fast raw astrometry of the images 3 5 3 6 2 Science pipeline The following tasks should be provided after first light by the science pipeline mode but the s
206. v 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 171 of 183 Calibra Detector Science tion Ma Raw Frames SEE Frames Sky Modelling Defringing Shift amp Align ione Frame Crosstalk correction Ghost and field distortion correction Reduced SuperFrame Astrometry Photometry 1 1 I 1 1 1 1 I 1 1 1 1 1 1 ee I Mosaicing 1 1 1 1 1 I 1 we e en en en en e e eee wm om em em em em em ee em em em em em em em After first light Reduced Catalogue Figure 3 5 4 10 Science mode scheme PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 172 of 183 3 5 4 8 4 Implementation overview For the implementation of the DRS we will use already publicly available software modules wherever possible and others will be own implemented Some of the main pillars of our pipeline will be the following software modules e TERAPIX software SExtractor SCAMP SWarp SkyMaker MissFITS e CFITSIO library for FITS file manipulation e Eclipse ESO C Library for an Image Processing Software Environment e Others common libraries PANIC Code PANIC GE
207. wanted sub window 36x36 In the multi channel mode of the detector it should be possible to reduce the necessary reading time by centering the sub window on the edge between 2 channels The table below summarizes some expected image rates for the different cycle read types The fast sub window 36 36 results in a maximal data rate out of the ROE of about 200Mbytes sec to 250Mbytes sec in the mean in the multichannel read out mode 1 MHz 128 channels 16bit 2048 line resets lt 10 microseconds 250 Mbytes sec The science data to store in that small sub window case will be much less 2 Mbytes sec if there is no interest at the additional data of the other detectors or channels in terms of cheap sky references A maximum of 250 Mbytes sec shall be in principle achievable as read out speed as first tests of the MPIA PLX interface in a 64bit 66MHz PCI slot showed which is the data interface for the ROE3 using data read tests from a data generator on the interface itself Fast small single frames or data units should be possible at maximal speed of about 10kHz frame rate over each of the 2 DMA channels of the PLX board in parallel the interrupt reaction speed of the low level driver itself PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 156 of 183 EN cycle type 32 channel output detector efficiency between single 1 channel output detector pixel clock images 100 kHz 1 MHz 10
208. window alone has 2 2 Gbytes of data when stored together with a second window of another detector channel area as sky saving it 1s already 4 4 Gbytes 3 5 3 7 4 1 Data type size single images are in GEIRS always the correlated result of 1 2 or more single frames which are based first on a reset and then read out non destructive An integral image is the summation of 1 or more single images acquired in the same exposure sequence GEIRS e shall write an integral image of all selected single images of the exposure The resulting depth will be stored at least as 32bit data type e shall write single images as FITS standard BITPIX 16 which is a signed 16bit data type Because there is no unsigned 16bit format in FITS available it involves using the FITS keywords BZERO 32768 0 and BSCALE 1 0 according to the equation real value fits value BSCALE BZERO Data types shall be selected in a way to minimize the needed storage space The BITPIX 16 format is not 100 percent data type safe for a double correlated image Normally the subtraction of a l6bit unsigned reset frame from the 16bit unsigned integrated frame results in an unsigned 16bit But it might happen by bad pixels or very short images or integrations of less then the noise level or strange first reset images that the single image might have already some negative results This problem should be solved either by adapting BZERO if the range of minimum and maximum is still in
209. with PANIC together with a search for very slowly moving objects in the largest possible fraction of the sky at least 30 degrees above the ecliptic For that goal the 2MASS archive would be used as the initial epoch 2 4 2 Comets The most visible and distinctive features of comets are the dust coma and tail the refractory material reflects the solar radiation at every wavelength from the near UV to the sub mm range Systematic observations of comets belonging to different families can be performed in order to follow the comet activity the dynamical and compositional evolution of the dust coma and tail and gas coma as a function of the heliocentric distance In the case of the dust by fitting the observed image with images synthetically generated by a dust dynamical model it is possible to put constraints in the distribution of the dust size and terminal velocity Making use of cometary images in several continuum filters the dust colour can be measured as a function of the projected cometocentric distance as well as a function of the heliocentric distance The dust colour combined with similar measurement in the optical range allow constraining the mineralogical composition of the dust grains If polarimetry is also provided most of the uncertainties arising from the dust colour analyses can be cleared up 2 5 JUSTIFICATION FOR A SECOND PIXEL SCALE The need of a smaller pixel scale is given by the fact that the average seeing at Calar A
210. ws in the spring packages To understand the movements of the lens mount parts while being cooled from 300 K to 77 K Figure 3 3 2 5 shows a sequence of snapshots of thermal conditions In Figure 3 3 2 5a the lens mount the lens and the retainer ring are at room temperature 300 K When the cryostat 1s filled and the cold plate and the filter unit are cooling the mount starts cooling only after a certain delay This means that the lens mount shrinks as shown in Figure 3 3 2 5b The lens and the retainer ring are shifted upwards because the lens can slide on the 40 chamfer relatively to the mount In the next phase see Figure 3 3 2 5c the lens changes its diameter and thickness since its cooling via the chamfer contact surface to the mount Therefore lens and retainer ring move downwards Finally in Figure 3 3 2 5d the retainer ring cools down and shrinks causing an upward movement relative to the lens E tube CaF lens disk spring retainer ring assembly lens mount _ gt 45 chamfer FS lens BaF2 lens Zn5e lens Figure 3 3 2 4 Cold optics of OMEGA2000 with spring loaded cryogenic lens mount This cooling model is of course very schematic The real process is much more complicated because the parts change their dimensions simultaneously after a certain time The delay depends very much on material properties like thermal conductivity which is a function of the temperature itself and thermal expansion
211. y of the measuring device was 0 005 mm PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 100 of 183 3 3 2 2 3 Optics wheel unit Since PANIC offers two different pixel scales the optics wheel carries two sets of lenses one set of four and one set of five lenses These are the lenses L5A to L8A and L5B to L8B see Figure 3 3 2 6 The optics wheel is driven by a cryogenic stepper motor Phytron VSS 52 and a modified Harmonic Drive gear PMG 14A with a ratio of 100 1 The distance between the optical axis and the rotation axis is 140 mm The motor needs 200 steps to do a full turn This means that one motor step rotates the optics wheel by 1 08 arcmin which corresponds to a lateral lens shift of 44 um which is the positioning accuracy At the beginning the wheel has to be initialized by a mechanical reference switch from Saia After that both positions of the optics wheel are reached by turning the motor by a certain number of full steps A feedback of the actual position is given by a resolver RE 15 from LTN Servotechnik The wheel has a preloaded double row ball bearing WAD933ZZ from ADR outer diameter 66 7 mm The bearing is very stiff and since the wheel is very well balanced there will be very little moment around both axes which are perpendicular to the rotation axis All metal parts of this unit are made of AIMg4 5Mn except the ball bearing the bearing support rings the moto
212. y over the CAFOS value 1860Nm but this will not cause problems Details of the mechanical design general layout lens holders filter wheels and the mechanical tolerances are similar and or identical to the two pixel scale design Since the most critical part of the two pixel scale design the optics wheel is not needed the mechanics can meet the requirements set by the optics PANIC Code PANIC GEN SP 01 Iss Rv 0 1 Date 22 October 2007 PRELIMINARY DESIGN REPORT Page 120 of 183 3 4 Electronics 3 4 1 ROE 3 4 1 1 Scope This document describes the design of PANIC s readout electronics 3 4 1 2 Requirements e the ROE shall operate four HAWAII2 RG detectors e a possibility to read an area of 15 x 15 33 x 33 pixels at 0 45 pixel of the detector at an minimal rate of 8 ms frame in this mode PANIC could be used for fast photometry Final goal is 1ms frame This mode will also be used for guiding but at much lower frame rates e the ROE noise shall be small compared with the ReadOut noise of the detector e the ROE shall be low power e all voltages on detector shall be in allowed range during power on off 3 4 1 3 General Information The ROE used with Omega2000 could operate 40 channels in total Since PANIC uses four HAWAII2 RG detectors with a total of 128 channels a new design of the standard MPIA ReadOut Electronics is required The new ROE uses new parts which are smaller and cheaper So the old ROE was house
213. ychromatic spot diagram of the 0 25 px camera 67 Figure 3 2 6 27 Distortion plot for the 0 25 px camera 68 Figure 3 2 6 28 Expected transmission for the 0 25 px camera 69 Figure 3 2 6 29 Angle over the filters for the 0 45 px camera 70 Figure 3 2 6 30 Angle over the filters for the 0 25 px camera oocccccnnnnnnnoonononnnnnnnnnncnnnnnnnnnnnnns 70 Figure 3 2 6 31 Pupil mask Shape esses eene eene nnne eene nennt 72 Figure 3 2 6 32 Footprint at the Pupil position coonnnnocooooocococcnononononononananononononnnnnnnnnccnnnnnnannnnnos 79 Figure 3 2 7 1 Montecarlo overlay of the EE80 for the tolerances in the 0 45 px 80 Figure 3 2 7 2 Montecarlo overlay of the EE80 for the tolerances in the 0 25 px 84 Figure 3 2 8 1 Opto mechanical layout showing the main assemblies regarding the optical SiS IS A e o POP E O Polo ES OU DEE E cemedaanadunrae EEA OE ETTET 86 PG Ue 5 5 l 1 PANIC cryostat SOL Dentro rre 88 Figure 5 5 1 2 Nitrogen vessel for cold plate erre n vete a ege 89 Figure 3 3 1 3 Cold warm spacers from the central ring to the optical bench 90 Figure 3 3 1 4 Temperature distribution with half filled vessel maximum filling pointing to ere 92 Figure 3 3 1 5 Temperature distribution with almost empty vessel pointing to horizon 92 Figure 2 5 1 0 PANIC Ee En EE 93 Figure 3 3 2 1 Section through PANIC the vacuum window and the detector unit are n

here - PANIC

Contents

Download Pdf Manuals

Related Search

Related Contents