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KOSMOS Instrument Manual - National Optical Astronomy Observatory

1. C KOSMOS I nstrument Manual Authors Sean Points Jay Elias Paul Martini and Timothy Beers C KOSMOS Instrument Manual V1 7 Revision History Version Version Date Description Authors 0 1 PM JE SP Dec 15 2013 Initial draft 1 0 JE SP PM Feb 28 2014 First release to users 1 1 JE SP Mar 2 2014 Various updates 1 2 TB Mar 10 2014 Various checks 1 3 JE Mar 14 2014 Addressed comments from staff link to troubleshooting pages 1 4 JE SP Sept 17 2014 Updates for COSMOS deleted some material now in operations manual other edits 1 5 JE Sept 18 2014 Updated NOCS screen captures 1 6 JE Oct 7 2014 Updates to troubleshooting section correlation with operations manual 1 7 JE SP Nov 14 2014 Link to mask design software and related info Page 2 of 100 C KOSMOS Instrument Manual V1 7 Table of Contents UR regere eren oj TP 9 2 Instrument Ch haracteristiCS sroine a idos 11 2 1 Basic Pafamipters AAA ACI AA LAA AICA AAA RTN Da de 13 Zie2 THROU I PU ERIN 14 2 2 1 Imaging E FOUGITDUE tl lla 14 2 2 2 Spectroscopic ThrOUHl DUOC vete veter neta beber veio eh in 14 2 3 PIGS VS AS 15 A SA A b gall an b E oa werent 17 24 1 Blue VPH GEIST sus nal aid citrico 17 24 2 Red VP GPS nee A eR eut Puit is 18 2 4 3 Additional GOISIiS ads et ees eo e a ea 18 29 ECO DESC c r TT 19 2 6 E A O Oe a ae 21 2 5 L Faciliby LOngSlitS sio a ad OS 21 2 6 2 Cu
2. sssssssss 81 Figure 29 He Ne Ar spectra for red VPH grism blue offset slit ssssssssse 83 Figure 30 He Ne Ar spectra for red VPH grism center slit l enn 85 Figure 31 He Ne Ar spectra for red VPH grism red offset slit sssssssss 87 Figure 32 Location of access ports for slits top and filters bottom 92 Figure 33 Mask holder with retaining ring removed ssse 93 Figure 34 Typical multislit task 3 oce eruere dert rk rin OR P PR YR eg YA Re yea 94 Figure 35 Mask installed in holder Note black side facing up sse 94 Figure 36 Longslits in holders left ooa I eere Evo eH VE RH gna ERE ea dO ena 95 Figure 37 Filter in holder right eseeen mmn 95 Page 7 of 100 C KOSMOS Instrument Manual V1 7 Tables Table 1 Imaging Zero Points ssssss m 14 Table 2 KOSMOS FIlterS oooococooccocooococnooccnn corro nono menn 15 Table 3 Detector Parameters sssseseee mme 20 Table 4 Recommended I maging Flat Exposures sssssesssss 68 Table 5 Recommended Spectroscopic Calibration Exposures 69 Page 8 of 100 C KOSMOS Instrument Manual V1 7 1 Introduction KOSMOS is the Kitt Peak Ohio State Multi Object Spectrograph a visible wavelength spectrograph and imager at the 4 m Mayall telescope at Kitt Peak National
3. 6912 close image expID 2456669 737888 obsID null 1 EndReadout 6912 Number of open KW databases 0 4 EndReadout 691 2 ette 1 1 EndReadout 6912 Complete Time 6 sec EndReadout 6912 Jekki a ma HE HA HH HIH i 1 Figure 15 The mayall 2 upper right hand monitor containing the VNC window of the KOSMOS DHS The lower right hand window should look similar to this Page 36 of 100 C KOSMOS Instrument Manual V1 7 ae S KALIQNIS ha lign py ugcAMS ka INIQNTI MAT Fits NIght 96338 fits NIST 00054 PIERO 72006 288 Ingo Night 06850 Fitsl2 at Focus 1999 99 reb E Figure 16 The mayall 2 lower right hand monitor contains an IRAF xgterm window and SAO mage ds9 window to permit the observer to examine their data as they are taken Starting with the lower left screen these windows contain Page 37 of 100 C KOSMOS Instrument Manual V1 7 1 NOAO MONSOON Supervisor Layer NMSL The main instrument status window with countdown clock detector information gain selection and exposure control e g Pause Resume Stop and Abort Exposure X NOCS Monsoon Supervisor Layer NMSL kosmos Fle Options Help rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 78 375 A rmslDramaGpxStartExp INFO GPX_STARTEXP 1 READINGOUT 79 375 rmslDramaGpxStar
4. Zero Images You create bias images using the ZERO script Since there are no photons involved the only parameters you need to specify are the number of images 10 is a good number binning 1x1 2x2 2x1 and the region to be read out 1k x 1k 2k x 2k 320 x 4k full frame 2k x 4k Page 67 of 100 C KOSMOS Instrument Manual V1 7 6 4 Flat Fields All flat fields should be done with the dome flat Someone from the day crew will position the telescope for you pointed at the white spot The dome lights should be off and the shades in the control room should be pulled down before taking dome flats The dome flats are controlled either by switches on the telescope console or a gui on the observer s computer Ask the person doing the instrument start to show you the switches These control a high low setting and an intensity 4 4 1 Imaging Flats Imaging flats are normally done with the low lights and usually with the intensity setting about halfway 25 Experiment with the exposure times but normally you should be taking 5 20 seconds and getting 50 000 counts Stay under 100 000 counts Some recommended settings follow If you are using the GUI to set the lamps 52 units is 100 and 24 units is 50 The dome flat lamps are not controlled by the scripts created by the NOCS so if you are doing flats with various lamp settings you need to enable the prompts and adjust the settings for the individual flat sequences Table 4
5. C KOSMOS Instrument Manual V1 7 References 1 The Ohio State Multi Object Spectrograph Martini Paul Stoll Rebecca Derwent Mark A Zhelem R Atwood B Gonzalez R Mason J A O Brien T P Pappalardo D P Pogge R W Ward B Wong M H PASP 129 187 Page 98 of 100 C KOSMOS Instrument Manual V1 7 I nstrument Team Page 99 of 100 C KOSMOS Instrument Manual V1 7 KOSMOS Observing Cheat Sheet Note this document is not a substitute for reading the manual at least once Afternoon Verify that all filters and slits required for the start of the night have been installed In general filters should have been requested n advance of your run Reference Operations Manual Section 7 With telescope pointed at white spot o Prepare required calibration scripts zero flats arcs User Manual Section 4 o Verify instrument focus User Manual Section 3 5 o Initiate execution of scripts User Manual Section 3 3 Start of night o KOSMOS only fill dewar o Check telescope pointing and focus User Manual Section 3 6 see also Section 3 6 on scripts as needed During the night o Imaging observing User Manual Section 3 10 see also Section 7 on efficient observing o Long slit observing User Manual Section 3 8 see also Section 7 on efficient observing o Multi slit observing User Manual Section 3 9 see also Section 7 on efficient observing Slit mask changes if required Operations Manual Section 7 Vo f
6. KOSMOS Optical Layout The telescope focal surface is at the far left and the detector is at the far right KOSMOS may be used with either a relatively blue sensitive e2v CCD or a more red sensitive LBNL CCD At present only the first detector is available Both devices are 2048 x 4096 arrays of 15 micron pixels Basic parameters are listed below section 2 4 The layouts of the imaging and spectroscopic fields are outlined below also see Section 2 6 Page 11 of 100 C KOSMOS Instrument Manual V1 7 S 5 o e 5 y E spectral direction Figure 3 KOSMOS imaging field of view in relation to the detector The width of the field is 10 in the spatial field direction The normal image display mode see Section 5 2 for details has the long axis as the Y vertical axis and the short axis as the X horizontal axis That is the display is rotated 90 degrees relative to Figure 3 When imaging with the instrument the relation between what you see on the ds9 display and celestial coordinates is as follows At PA 90 degrees KOSMOS default North is up and East is to the left e At PA 270 degrees COSMOS default North is down and East is to the right In spectroscopic modes blue is at the bottom small Y values and red is at the top higher Y values See Section 2 6 Page 12 of 100 C KOSMOS Instrument Manual V1 7 2 1 Basic Parameters Optical Design Collimator f 7 9 14 degree FOV Double Gauss
7. Writing observation 1 1 as 3 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 4 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 5 7 with DP S init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 6 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 7 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS nguiSetExecClose INFO wrote script home observer exec CAMSFOCUS sh cx LI E EXIT E INNEN NGUI v20140611 c 2006 2014 AURA Inc Contact Philip N Daly pnd noao edu 4 Figure 18 The NGUI window provides for the creation of observing scripts Detector Page 39 of 100 C KOSMOS Instrument Manual V1 7 3 An xterm terminal window that allows an observer to execute scripts that were created by the KOSMOS NGUI Ti 90x2 M dhsSendMetaData sent mdConfig xbfabb840 size 32776 stat 32776 istat 0 DITSCMD 2c6e nohs nohsDramaNewObs DONE OK SUCCESS TASK nohs ACTION nohs newobs ARGS headers DITSCMD 2c6f nmsl nmslOramalnit DONE OK DITSCMD 2c70 nmsl nmslDramaGpxSetAVP DONE OK SUCCESS TASK nmsl ACTIONsnasl gpxSetAVP ARGS xpID 2456669 7391684874892235 DITSCMD 2c71 nmsl nmslDramalnit DONE OK DITSCMD 2c72 nmsl nmslDramaGpxStartExp DONE OK SUCCESS TASKenmsl ACTION nasl gpxStartExp ARGS none D
8. 47 EE Azimuth 0 00 1 12 2014 Dome Error 0 00 0 42 09 Dome Tracking off s um 0 41 27 50 Telescope Focus um 11150 00 DEEST 8000 Declination 2 10 00 5 Guider Mode off dosed Epoch 2014 0 South Guide X mm 119 86 Hour Angle 0 00 00 00 South Guide Y mm 28 92 EN Distance 0 20 Mirror Position thru 1 00 Lamp A Source quartz 0 00 Lamp A Status off 735 50 Lamp B Source henear 180 00 Lamp B Status off 90 10 Lamp C Source bright kosmos Lamp C Status off Optical Prescription For Illustrative Purposes Only KCMID Software Author s Bob Marshal rmarshall amp noao edu Phil Daly pnd amp noso edu KCMID Software Date 20131220 KCMID Software Version IEB Version 0 5 Figure 20 KOSMOS Status Monitor window alias kccd that shows the filter disperser and slit information as well as telescope telemetry data 000 X Truss temp Trs Change gt CST Click tt Figure 21 Mayall environmental temperature display This is not part of the NOCS and is not present on the Blanco telescope Continuing with the upper right hand screen we find the Page 41 of 100 C KOSMOS Instrument Manual V1 7 5 VNC KOSMOS 4m 1 monsoon The VNC window with the Data Handling System DHS control and image display X VNG kosmos 4m 1 Process Status Shared Henory Cache Real Time Display Pathe 8 Files Paths Ports amp Modes NOINE Xintcol Version 1 309081 Meg low Norm Mox Aeg Rex Cur O Ri
9. 90 deg Page 24 of 100 C KOSMOS Instrument Manual V1 7 y pixels x pixels Figure 11 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure Data are for COSMOS The points are relative to zenith Z measured three times and correspond to two and four hours East and West at constant declination and 85 60 0 and 25 deg declination along the meridian These measurements were obtained with the instrument rotator at PA 270 deg The data should be similar to those in the preceding figure difference may reflect differences in the dewar flexure between the two dewar designs There is also flexure between the guide probe and the slit this appears to be roughly comparable about Y pixel hour in the direction of changing gravity Our recommendation is that you should re check centering of the object on the slit after 2 hours Note that for both guider slit and slit detector flexure orientation at the parallactic angle tends to put the direction of maximum flexure along the slit Page 25 of 100 C KOSMOS Instrument Manual V1 7 2 8 Shutter The shutter is located at the front of the instrument between the entrance hatch and slit wheel It is a model PS 500 from Sci in Tech with a square 5 aperture There are two carbon fiber blades that provide even illumination with high accuracy over the entire field Exposure times at least as s
10. AI D E 4 E 7000 7200 7400 7600 7800 8000 8200 Wavelength A HeNeAr KOSMOS Red Grating Blue Slit 1 M A e i 4 OZMO 8200 8400 8600 8800 9000 Wavelength A Figure 29 He Ne Ar spectra for red VPH grism blue offset slit Page 83 of 100 Rel Intensity Rel Intensity Rel Intensity Rel Intensity 6000 5500 5000 4500 4000 5x10 4x10 3x10 2x10 10 8000 5500 6000 4500 4000 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Center Slit 5748 299 Nel 5764 418 Nel 6852 4876 Nel 5875 618 6143 0823 Ne _ 8163 5939 Nel 6217 2813 Nel 6266 495 Nel 6304 7892 Nel 63344279 Ne 6382 9914 Ne 6402 246 Nel 6508 5279 Nel 6532 8824 Nel 6598 9529 Nel 6678 2 blend LC 5600 5800 6000 6200 6600 Wavelength A HeNeAr KOSMOS Red Grating Center Slit iid HM I 6400 6600 6800 7000 7200 7400 7600 Wavelength A Page 84 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Center Slit h t 4 Ei E jg 3 R A e li il 6000 5500 i 2 5000 A El 4500 4090 7 LI T NEN 7600 7800 8000 B200 8400 8600 8800 Wavelength A HeNeAr KOSMOS Red Grating Center Slit m 2 z amp 5000 3 E 4000 H 8600 8800 9000 9200 9400 9600 Wavelength A Figure 30 He Ne
11. Ar spectra for red VPH grism center slit Page 85 of 100 Rel Intensity Rel Intensity Rel Intensity Rel Intensity C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Red Slit 5x10 gt x 9 gt 3x10 2x10 6143 0623 Nel _ 6163 5939 Nel 8217 2813 Ne 4 6304 7892 Nel 83344279 Ne _ 6266 495 Nel 10 6000 5500 5000 4500 4000 as a 6200 638289814 Nel __ 8402 246 Nel 6506 5279 Nel 0632 8824 Nel __ 6598 9529 Nel 6676 2 blend 6717 0428 Nel __ 0752 832 AI 8400 6600 Wavelength A HeNeAr KOSMOS Red Grating Red Slit 2 3 E 50 o o 45 o o E 7000 A a 7200 7400 7600 7800 Wavelength A 8000 B103 682 AI 8115 311 AI 7147 041 Al 8200 Page 86 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Red Slit 8115 311 AI 6000 5500 5000 450 4000 E 8000 8200 8400 8600 8800 9000 9200 Wavelength A Rel Intensity o HeNeAr KOSMOS Red Grating Red Slit 5x10 4x10 3x10 2x10 Rel Intensity 10 6000 5500 5000 4500 Rel Intensity 4000 9000 9200 9400 9600 9800 10000 10200 Wavelength A Figure 31 He Ne Ar spectra for red VPH grism red offset slit Page 87 of 100 C KOSMOS Instrument Manual V1 7 Appendix C Multi Slit
12. Camera f 2 7 26 degree FOV Petzval Grisms Fixed position zero net deviation at blaze peak Filters n collimated beam tilted 8 to avoid ghost images Wavelength Coverage Full wavelength coverage is 3600 10000 Field of View 12 diameter cropped to 100 sq arcminutes by detector Pixel Scale 0 292 arcseconds per pixel Operating Modes Direct I maging KPNO facility 4 inch filters dedicated blocking filters Grism Spectroscopy Blue VPH grism Red VPH grism with blocking filters as required Disperser Resolution and Wavelength Coverage see Appendix B Blue VPH Grism R 2100 Blue Slit 3500 6200 Center Slit 3800 6600 Red Slit 4300 7000 Red VPH Grism R 2100 Blue Slit 5000 9000 Center Slit 5800 9400 Red Slit 6100 10000 Long slits Facility 0 6 0 9 1 2 1 5 3 0 wide All slits are 10 long Multi Object Masks Custom laser machined slit masks Minimum Recommended Exposure Time 0 01 sec 0 5 sec for accurate photometry see section 2 7 Page 13 of 100 C KOSMOS Instrument Manual V1 7 2 2 Throughput 2 2 1 Imaging Throughput Table 1 Imaging Zero Points Filter g R i ZP 1 DN s 27 20 27 23 27 08 e s 0 mag 5 00e10 5 13e10 4 47e10 Table 1 lists zero points for representative filters on the AB magnitude system These measurements were obtained with the e2v detector 2 2 2 Spectroscopic Throughput Overall System Efficiency KOSMOS
13. If you want to do this read the ccdproc help Page 50 of 100 C KOSMOS Instrument Manual V1 7 The minimum recommended processing steps comprise e Removal of the bias level for each amplifier using the detector overscan section e Trimming the result since the overscan isn t needed e Combining the outputs from the individual amplifiers into a single image You are certainly free to perform additional processing but it is not needed to carry out any of the observing tasks outlined below Note also that the processing only affects the data on the local machine kosmos or cosmos data in the archive are stored as raw data To process the data type mscred epar mscred View the parameters and confirm that backup once backuproot Raw note the instrument home observer kosmos dat Exit with q Now type epar ccdproc For the basic processing merge into a single image all steps should be set to no except Apply overscan strip correction Trim the image Merge amplifiers from same CCD CCD image type to process should be blank Additional relevant settings are biassec BIASSEC Page 51 of 100 C KOSMOS Instrument Manual V1 7 trimsec TRIMSEC the is required Overscan removal settings should use the default values which are listed below You can reset these if they appear to have been tinkered with by typing unlearn ccdproc and then going back to epar ccdproc Starting with Fit
14. KOSMOS Instrument Manual V1 7 6 5 Wavelength Calibration Wavelength calibrations are set up doing the TELESCOPE ARC scripts Arcs are observed by moving a mirror in the rotator into the beam which sends light from the arc lamp into the instrument The field of view of the comparison system is smaller than the KOSMOS FOV but close enough to be useful for most purposes Recommended exposure times are shown in the table above Note that these do not scale with slit width because the lines are unresolved NOTE If you have the lamp control enabled in NGUI scripts that you create will move the mirror in and out and turn the lamps on and off as necessary This is normally a good thing but if you are stringing together a series of arc scripts it wastes time So for those situations only turn the lamp control and prompt off Then in the higher level script within which you nest your comparison scripts include the pre existing COMPSTART sh and COMPEND sh scripts to start and end the sequence Alternatively you can have someone from observer support set the lamps and mirror as needed If you need to get arc spectra while observing for example because you are trying to get precise radial velocities you can run arc scripts at any position of the telescope However there scripts should be created with the lamp control on so that things are positioned correctly and the lamps are turned off at the end of the arc observation NOTE FOR ADVANCED USERS
15. Mask Design When designing multi slit masks there are several considerations including differences between the two telescopes C 1 Basic Considerations Slits can in principle be placed anywhere in the imaging field of view of the instruments However slits that are displaced significantly in the dispersion direction may produce spectra that are missing a relevant portion at one end Also the VPH gratings efficiency curves are strongly position dependent so a blue shifted slit will also have the peak efficiency blue shifted This can be advantageous in long slit mode see discussion of offset slits above but may be less desirable in multi slit mode In general therefore we recommend restricting slits to within a rectangle roughly 5 x 10 arcmin In addition mask layout should allow for alignment stars Square boxes are designed into the mask centered on relatively bright stars which are used to check mask alignment While 2 stars are in principle all that is needed we generally recommend 3 5 stars to provide some redundancy The alignment stars should be distributed widely over the mask to provide optimal alignment Note that the alignment boxes do produce spectra when observing through the mask so you must be careful to avoid interference with science slits C 2 KOSMOS Constraints The Mayall rotator is capable of rotation over position angles from 0 to 180 degrees Do not design masks for position angles between 180 an
16. Oe 1 EOS Escollect z collect _amemyr u s mm mm m ms ms IL EST Minas pt j CTI T ais el WC cord i Figure 22 The VNC DHS window where images are displayed and when observers can select the Image Root Name file prefix Finally we have the lower right hand screen which contains an xgterm window for the observer to run IRAF and a SAOI mage ds9 window to display images There is one more screen that is normally minimized but which can be useful at times xyerm sym Page 42 of 100 C KOSMOS Instrument Manual V1 7 6 NICS 000 X NOCS Instrument Control System NICS KOSMOS File Options Help Thu Sep 18 05 53 17 PM MST2014 kosmos thermal templ 20 7 4m gwe kpno noao edu 2347 kpno 4m IEB Air C Opt Bench C 16 6 Internal C Extemal C Camera Focus Qm 21000 O Camera Detta qum PI Camera zero m 555 catimator Focus m 5000 Gimator Deita um T0 Colimator zero m B GG395 GG455 GG495 065 06570 SDSS g SDSS r SDSS i Gunn z Irvin z Open b2k l r2 riple A eeren ne Figure 23 This NICS shows mechanism status and also allows manual control Here the text window in the upper part has been minimized and the control buttons for the mechanisms have been enabled otherwise they would be grayed out This is normally minimized look for it at the bottom of the lower left monitor If you open it it show
17. Position thru Optical Bench 2 C 3 1 00 Lamp A Source quartz Ambient Air C RA Offset 0 00 Lamp A Status off Last CfgAll Command Dec Offset 735 50 Lamp B Source henear Filter Demand i _Parallactic Angle 180 00 Lamp B Status E eff Disperser Demand Rotator Angle 90 10 Lamp C Source bright Slit Demand Instrument Name kosmos Lamp C Status off Optical Prescription For Illustrative Purposes Only KCMID Software Author s Bob Marshall rmarshall amp noao edu Phil Daly pnd noao edu KCMID Software Date 20131220 KCMID Software Version IEB Version 0 5 X Truss temp Trs Change gt 1 deg 3 7 Click to Reset Mir 6 4C Figure 14 The mayall 2 upper left hand window showing the KOSMOS status display i e the KOSMOS Observing Monitor and the Mayall temperature monitor The upper right hand window should look similar to Figure 14 This display contains the VNC Viewer that shows the KOSMOS Data Handling System DHS Page 35 of 100 C KOSMOS Instrument Manual V1 7 X VNC kosmos 4m 1 monsoon lata Handling Sustem Supervisor le z Super Sending EndReadout Heim File Help Quit dhsEndReadout readout finished with no errors seqno 6912 ICA Complete ending readout 2456669 737888 SHCMar ending Expl 2456669 737888 Process Status Tine Di i setOption rdirname data2 observer 20140111 Shared Henory Cache Real Time Display Paths 8 Files
18. Recommended I maging Flat Exposures Filter Lamp setting Exposure SDSS g Low 52 units 10 sec SDSS r Low 52 units 15 sec SDSS i Low 52 units 20 sec Ha all filters High 24 units 10 sec O 111 all filters High 52 units 2 sec These recommendations apply to 1x1 binning if you are taking data with different binning you should reduce exposure times by the appropriate factor 2 or 4 or adjust lamp intensities Note that flux is not proportional to the numerical intensity setting 6 4 1 Spectroscopic Flats Spectroscopic flats are done with the high illumination and maximum intensity Recommended exposure times for 3 pixel slits are given below Page 68 of 100 C KOSMOS Instrument Manual V1 7 Table 5 Recommended Spectroscopic Calibration Exposures Type Red disperser Blue disperser Flat high max int 7 sec 40 sec Arc 5 sec 120 sec Exposure times for flats scale inversely with slit width less time for wider slits Normally 10 images configuration is reasonable It does no harm to take a sample image or two before setting up a complete calibration series NOTE If you are creating scripts to be run in sequence unattended turn off the lamp control and lamp prompt options in NGUI before creating the scripts and turn them on again when you are done Otherwise you will come back from dinner and find the whole sequence waiting for a prompt Page 69 of 100 C
19. The commands to control lamps rotator mirror etc from the observer s xterm are all of the form testntcs item command where the item is something like gcccompb for comparison lamp B gccmirror for the rotator mirror and command is a position or status like thru or on These commands are useful to have in reserve during the afternoon during the night the telescope operator can set these items for you more quickly 6 6 Standard Stars Lists of standard stars can be found on the KPNO web site http www kpno kpno noao edu Info standard catalogs html Some additional sources of information are listed below They are current at the time of this writing 6 6 1 Imaging Photometric Standards Additional sources beyond what s listed on the KPNO catalogs page include Page 70 of 100 C KOSMOS Instrument Manual V1 7 http www gemini edu q node 10445 6 6 2 Spectrophotometric Standards Additional sources beyond what s listed on the KPNO catalogs page include http www gemini edu sciops instruments gmos calibration spectroscopic stds http www eso org sci observing tools standards spectra stanlis html http www astronomy ohio state edu MODS Calib index html specphot The standards listed on these sites are mostly the same the last two sites include finding charts Page 71 of 100 C KOSMOS Instrument Manual V1 7 7 Efficient Observing with KOSMOS This section is intended to help observers minimize o
20. The first approach leads to less clutter in the exec directory but you have to be careful not to over write a script that is still executing The second approach fills up the directory with single use scripts you may wish to clean them out every afternoon You can run into trouble if you end up with scripts with similar names and forget which one is current e g TARC B sh and TARC B sh In either case don t forget to specify the object name Note that for some actions e g pointing checks or telescope focus you probably don t care what the object was and can leave it as something generic Pointing Star Page 48 of 100 C KOSMOS Instrument Manual V1 7 e f you are doing more than one spectral configuration make sure you change a relevant parameters when you create the script for each configuration e f you decide to change file prefixes when you change objects not recommended but it s up to you in the end remember to do this before starting execution of a script e Scripts in home observer sysexec should not be modified or deleted e Scripts in home observer exec are not archival They may also be modified or deleted during the day if trouble shooting is performed If you want to protect them during your run e mail or copy them Copying them for safe keeping to home observer lt yourname gt will protect them during your run 5 3 8 Automated Observation Logging klog A program that creates a log of your observations
21. ace RAUDIR set to data2 observer 20140111 setOption pdirname data2 observer 20140111 F ik PROCDIR set to data2 observer 20140111 Ku Ruit Update M Show Activity JF Verbose Mode SHC CLEAN ExpID 2456669 737888 time 6 done 1 Transferring data scp kosnosdhs 4n home data Night2 06912 data2 observer 20140111 Night2 06912 dat 100 60KB 60 1KB s 00 00 Night2 06912 fits 100 34MB 33 6MB S 00 01 Triggering iSTB for data2 observer 20140111 Night2 06912 fits Abonar Postproc DONE ExpID 2456669 737888 Raw Filet kosmosdhs 4m home data Night2 06912 Fits Local File data2 observer 20140111 Night2 06912 fits Date Sat Jan 11 17 43 35 MST 2014 Aaa N R 4154 1 t lb y j J NOAO IRAF XIntool Version 1 3EXPORT ial 06912 RTD Norm Match AReg Reg Cue Q Reset Update Clean SHC Page Usage kosnosdhs dm kosmosdhs dn Disk Usage 17 _ Connect Status Exp Status y i j z mosdca J dal 1 EndReadout 6912 Updating image headers 1 EndReadout 6912 Number of open keyword dbs 3 2 EndReadout 6912 Updating header for kudb phu image 0 1 EndReadout 6912 Closing phu 2 EndReadout 6912 Updating header for kwdb imi image 1 1 EndReadout 6912 Closing imi 2 EndReadout 6912 Updating header for kudb im2 image 2 1 EndReadout 6912 Closing im2 1 EndReadout 6912 close image status 0 iostat 0 1 EndReadout
22. are displayed are usually Page 44 of 100 C KOSMOS Instrument Manual V1 7 whatever was set when that particular script type was last created All scripts require you to specify an object name and a script name If a script with the same name exists when you try to create the new script you will be prompted to over write it Do not over write a script that is being executed The available scripts and their purposes are ZERO This takes a zero bias image or images and therefore has few parameters You will probably want zero images for each region of interest mode with which you are taking data DARK This takes a dark image or images For most observing programs dark images are not necessary SKY TWILIGHT FLAT This will take twilight or sky flats With the e2v CCD these don t appear to be necessary They are not expected to be needed with the LBNL CCD either DOME FLAT This will take dome flats you should plan to take a dome flat with each disperser slit filter configuration you will observe with See the calibration section for details TELESCOPE FLAT This takes a flat using the continuum lamp in the rotator guider It is not very flat and is not recommended TELESCOPE ARC This takes spectra using the arc lamp installed in the rotator guider See the calibration section for details You will want to take an arc for each configuration you observe with TELESCOPE FOCUS This takes a series of exposures with the telescope foc
23. central slit Note that Y is North at PA 90 and Y is South at PA 270 See Appendix E for the physical layout of the slits in the slit holders 2 6 2 Custom Multi Object Slit Masks Multi slit masks can be designed and fabricated for KOSMOS These are laser cut from special shim stock Users are responsible for designing their own masks see Appendix C and links therein for details There are significant differences between the two telescopes that affect mask design as summarized below Page 21 of 100 C KOSMOS Instrument Manual V1 7 The range of rotator angles on the two telescope is different o The available range on the Mayall is 0 180 degrees o The available range on the Blanco is 0 360 degree excluding 87 93 degrees The plate scales on the two telescopes are slightly different Note that the instruments are installed so that at a given position angle the physical orientation NSEW of the instrument is the same on both telescopes Because of the first 2 differences KOSMOS masks cannot be used on COSMOS and vice versa The Mayall does not have an atmospheric dispersion corrector that covers the full field of view of KOSMOS so masks should be designed considering the likely parallactic angle at the time of observation The Blanco in contrast does have an ADC with sufficient field of view Page 22 of 100 C KOSMOS Instrument Manual V1 7 2 7 Flexure The figures below show flexure at two different rotator position
24. general appearance for the COSMOS masks will be similar to those for KOSMOS except that neither side will be shiny The black side of the KOSMOS masks faces the collimator to reduce ghost images While both sides of the COSMOS masks are black the alignment pins in the mask holders ensure that the orientation is always correct Page 93 of 100 Figure 34 Typical multislit mask The black side of the mask is facing the detector not the telescope secondary when installed in the instrument see Figure 35 Figure 35 Mask installed in holder Note black side facing up Page 94 of 100 C KOSMOS Instrument Manual V1 7 A longslit holder is shown below These are permanently configured so all that needs to be done for use is to installed the selected holder s into the instrument Filters are installed by daytime support staff Figure 36 Longslits in holders left The slit holders shown are for a centered slit top and a blue displaced slit bottom marked by the arrows The red displaced slits have the slit in the position near the handle of the holder Slit mask mounted in wheel Figure 37 Filter in holder right Je After changing slits or filters it is necessary to update the configuration files These are in home logs The configuration file for the slits is kosmos slits conf same name for COSMOS the file for the filters is Kosmos filters conf e Open the file for editing e f you have replac
25. image of the sequence for one or more stars on the display Avoid stars that are saturated overlapping with other stars or that run off the edge of the field Then type q to exit and see a display of focus parameters You can re run the routine omitting or adding stars to see if you get a better result There is a focus widget at the Mayall at least than monitors telescope truss temperature and recommends focus adjustments You can make use of this to tweak the focus but you will likely want to re check focus if the temperature has changed by a large amount if the seeing has gotten better or if you re concerned that the correct focus has drifted Page 56 of 100 C KOSMOS Instrument Manual V1 7 5 7 Guiding The telescope operator will select and acquire guide stars You don t need a guide star for focus checks or pointing checks but it s recommended for all other observations The usable field for the guider is shown below IMPORTANT It may in fact be possible to observe spectra with the guide probe inside the vignetted area since the slits only occupy a portion of the focal plane If the probe is vignetting the imaging field you will see its shadow in the acquisition image and will be able to see whether it is occulting your slit or slit mask If it is not you can take spectra KOSMOS Guider Patrol Area X 95mm 10 5 X 90mm 9 9 Actual x Imaging Field Y 100 mm 11 Y Guider Patro
26. is available To run it type nocs start klog in an xterm open on the kosmos or cosmos machine The program then starts a log for every new observation that appears in the data directory files created through ccdproc or other IRAF tasks are not logged You can add comments on the mountain you can automatically enable printing as pages complete The pages are also saved in the data directory so you can re print them or copy them Page 49 of 100 C KOSMOS Instrument Manual V1 7 5 4 Data KOSMOS data are multi extension fits files where data from each amplifier are stored in a separate extension 1 2 for e2v 1 4 for LBNL The extensions can be combined using the ccdproc command within the mscred IRAF package 5 4 1 Data Storage Data obtained by KOSMOS are simultaneously sent to the NOAO archive and stored locally in the data subdirectory This is actually an alias for a subdirectory labeled by date so each night if you restart the NOCS data will be stored in a new subdirectory full path data2 observer YYYMMDD IMPORTANT if you leaving the NOCS running continuously this data directory will not update from night to night It is possible to change the directory setting in the DHS VNC window Paths amp Files tab change both paths but we strongly recommend you re start the NOCS every afternoon instead after noon Files are identified by a prefix set in the DHS VNC window see above and a file number The file number
27. trying to abort during an integration while the countdown is proceeding o type CNTRL C cr then let the integration run to completion with DONE in the NMSL window The script will stop when the integration has finished but leaves the last integration unterminated in the data system o Issue this command in the shell window to terminate the last integration ditscmd nohs nohs endobs cr o Inthe DHS VNC monitor see Fig 22 check that an image processed to disk o You are ready to take data again 5 3 7 Script Management There is more than one way to manage your scripts and the following should be taken as suggestions rather than mandatory It is very convenient to create a master script for your afternoon calibrations Note that if you are working in MOS mode this script may be different every afternoon since the MOS masks will be different There is limited advantage to creating all your night time observing scripts during the afternoon you can usually create the scripts acquisition and observing for your next object during the preceding observation Or you can try to stay ahead by a couple of objects Once you are reasonably familiar with the process you can probably create scripts while the operator is moving to your next target but in general allow enough time to check your work before saving You can operate either by over writing the same basic scripts or by creating a new script name or names for each object
28. using the labels next to the handle Figure 12 KOSMOS dark slide handle location In the figure the dark slide is shown in the open position Pull down slightly on the handle arrow before you move it in or out Page 32 of 100 C KOSMOS Instrument Manual V1 7 If the NOCS software has been started before the Torrent controller has been turned on NMSL window background see Fig 17 below will be yellow or orange this is not the only reason it can change color however You will need to call someone to turn the controller on in this case Please see Appendix D which addresses common KOSMOS problems and their solutions If KOSMOS has been started before the dark slide has been removed all observations will look like bias frames The solution is to open the KOSMOS dark slide 5 1 3 NOCS Startup The observer should first logon to either maya 2 or mayall 3 using the 4meter account if this has not already been done the account password is located in the Mayall control room For COSMOS login on observer2 as kosmos get the password from your support contact The steps required to start the NOCS are 1 Open an xterm window on mayal 2 or mayall 3 2 On the command line type the following ssh X Y observer kosmos The observer should now be logged into kosmos as observer and ready to start the NOCS In the observer kosmos xterm window the observer should then type the following at the command prompts waiting for each
29. 00 5000 5100 5200 5300 5400 5500 5600 Wavelength A Page 80 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Blue Grating Red Slit j g z Rel Intensity A a e e 4000 5600 5700 5800 5900 6000 6100 6200 6300 Wavelength A HeNeAr KOSMOS Blue Grating Red Slit 5000 5000 4500 Rel Intensity 4000 6300 6400 6500 6800 6700 6800 6900 7000 Wavelength A Figure 28 He Ne Ar spectra for blue VPH grism red offset slit Page 81 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Blue Slit TON 2ve8 ypo69 IPH 8199489 IPN 8L8Y 2988 ION GT 94G PN 662 8v4S IV 040c90 77 IV 2629099 IV evg 2499 7 Tv 212298 IV 99424819 4x10 3x10 E 2x10 31sue1ug eU 4200 4000 Aysusyu 194 3800 5200 5400 5600 5800 6000 6200 Wavelength A 5000 HeNeAr KOSMOS Red Grating Blue Slit 5x10 IPN 421260 7 7000 Tv y 9969 TeN 896269 77 Iv 821499 Iv 2082949 PN 82502149 pusiq 28499 TON 63969699 IPN y308 2899 6400 PN E183 2129 EN 8883 8918 WN Ake VIS 6600 6800 Wavelength A x x e q ysu 7 U 194 o o 10 8000 5500 000 o A x Page 82 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Red Grating Blue Slit 8014 786 AI 8103 692 AI 8115 311 AI Rel Intensity 7147 041 AI 7948 175 AI B008 156
30. 1 slit 17 Figure 6 Red VPH grism Scale and resolving power with a hypothetical 1 slit 18 Figure 7 Nominal quantum efficiency curves for the KOSMOS and COSMOS care L OC 19 Figure 8 Location of the Red Center and Blue long slits relative to the detector and field Of VIEW nannan te ei Qu Ra e taba uv a deo RON e Se Gant Rai Ced n ceca eres CY ene ee 21 Figure 9 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure oooccooccccccncoccncncnnononcnannos 23 Figure 10 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure ooccocccccccncocnnoncnnnnoncnnnnos 24 Figure 11 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure eeeeeeees 25 Figure 12 KOSMOS dark slide handle location n 32 Figure 13 The mayall 2 lower left hand monitor with the necessary KOSMOS windows shown NMSL NGUI and xterm lead mete do 34 Figure 14 The mayall 2 upper left hand window showing the KOSMOS status display i e the KOSMOS Observing Monitor and the Mayall temperature monitor 35 Figure 15 The mayall 2 upper right hand monitor containing the VNC window of the KOSMOS DAS iaa os 36 Figure 16 The mayall 2 lower right hand monitor contains an
31. A Mac mini computer in the Mayall 4 m control room from which all programs are launched The observer should be logged into mayal 2 or mayall 3 using the 4meter account The password for the 4meter account is available in the control room or can be provided by Observer Support Both mayall 2 and mayall 3 have four 4 attached monitors If you are observing remotely you will most likely connect to mayall 2 by a Virtual Private Network VPN and display the mayall 2 screens remotely For COSMOS a similar capability is provided through a Linux workstation again with multiple monitors kosmos kosmos 4m The main computer that runs the NOCS and co ordinates the data acquisition for the observer COSMOS computers are the same except named COSMOS XXxX kosmospan kosmospan 4m The MONSOON pixel acquisition node PAN computer kosmosahs kosmosdhs 4m The main data handling system DHS machine that ingests data from the PAN performs various data management tasks and produces the final FITS image on disk This image is transferred back to kosmos 4m and to the NOAO archive In addition to the NOCS a number of the observing tasks make use of the IRAF image analysis facility While the manual specifies relevant IRAF commands for most tasks a general familiarity with the software is extremely helpful Information and tutorials can be found at http iraf net Page 29 of 100 C KOSMOS Instrument Manual V1 7 Page 30 of 100 C KOSMO
32. Blue and Red Gratings 4000 5000 6000 7000 8000 9000 Wavelength A Figure 4 Total spectroscopic efficiency with the blue and red VPH grisms The three solid lines for each grism represent the blue center and red slit options Efficiency includes the instrument telescope and atmosphere at Zenith Page 14 of 100 C KOSMOS Instrument Manual V1 7 2 3 Filters KOSMOS has 2 filter wheels with 6 positions each of which 1 should be kept open Thus a total of 10 filters can be installed KOSMOS has a set of 5 order blocking filters These are listed in Table 2 KOSMOS may also be used with any of the KPNO 4 inch square filters COSMOS may be used with the CTIO 4 inch filters There are two important stipulations First since the filters are in the collimated beam any filters that do not meet specific flatness criteria will distort the wavefront and thus compromise the image quality Second because the filters are tilted by 8 degrees to avoid reflection ghosts all narrowband filters are significantly blue shifted The table below includes filters that have been tested with KOSMOS it will be expanded to include CTIO filters KPNO filters are also listed on the Kitt Peak web page where transmission curves for narrowband filters with the 8 degree tilt are presented when available Table 2 KOSMOS Filters Filter Filter Name Comments ID GG395 KOSMOS dedicated blocker GG455 KOSMOS dedicated blocker G
33. Ez New Integration Time s Gain Amp 1 e ADU 0 66 Read Noise Amp 1 e 6 84 Gain Amp 2 e fADU 0 65 Read Noise Amp 2 e 6 69 Saturation e 140000 Read Out s 75 Binning ixi Pixel Scale pix 0 29 y Code Version ROIV206 Latest Dewar Temp K 242 0 X NOCS Monsoon Supervisor Layer NMSL kosmos Thu Sep 18 03 40 52 PM MST 2014 Integration timer 1 0 0 1 4m gwc kpno noao edu 2347 kpno 4m New Integration Time s Status DONE Exposure Vector i Gain Amp 1 e ADU 0 66 Read Noise Amp 1 e 6 84 Gain Amp 2 e ADU 0 65 Read Noise Amp 2 e 6 69 _Pause Exposure Saturation e 140000 Read Out s 75 Binning ixi Pixel Scale pix 0 29 Code Version ROIV206 Latest Dewar Temp K 242 0 A Figure 17 The NOAO MONSOON Supervisor Layer NMSL window shows the instrument status countdown clock detector information and exposure control The top image shows it with the text window open the bottom image is with it closed The appearance of this screen may be slightly different with continuing improvements to the software For normal operation you can hide the upper text window using the Options menu you can restore it if needed Page 38 of 100 C KOSMOS Instrument Manual V1 7 2 NOAO KOSMOS Spectrograph Mayall 4m Telescope Aka NGUI the script editor window lt CAMSFOCUS gt Writing observation 1 1 as 4 7 with DPOS in
34. G495 KOSMOS dedicated blocker 0G530 KOSMOS dedicated blocker 0G570 KOSMOS dedicated blocker 1584 SDSS g 1585 SDSS r 1586 SDSS i 1590 O III Shifts to rest frame Need to refocus telescope by 500 redshifted microns 1564 Ha Shifts to red frame H alpha http www noao edu kpno filters 4Inch_List html and 1 ttp http www ctio noao edu noao content ctio 3x3 inch and 4x4 inch filters Page 15 of 100 C KOSMOS Instrument Manual V1 7 The order sorting filters are dedicated filters and therefore always available the other 4 inch filters may be used on other telescopes so make sure to request them in advance if they are essential to your program We prefer to have the dedicated filters always installed in the instrument but they can be removed if your program requires more than 5 additional filters Filter changes are normally done only during regular work days and should have been requested in advance Last minute requests may not be honored if the personnel or the requested filters are not available Page 16 of 100 2 C KOSMOS Instrument Manual V1 7 4 Dispersers 2 4 1 Blue VPH Grism dA dx nm pix R 2 3 33d 0 075 0 07 0 065 0 06 0 055 2600 2400 2200 4 1 4 4 4 4 L 4 L 4 4 L 4 4 4 0 4 0 6 0 6 Wavelength microns Figure 5 Blue VPH grism Scale and resolving power with a hypothetical 1 slit Page 17 of 100 C KOSMOS
35. IRAF xgterm window and SAOI mage ds9 window to permit the observer to examine their data as they are A 37 Figure 17 The NOAO MONSOON Supervisor Layer NMSL window shows the instrument status countdown clock detector information and exposure control 38 Figure 18 The NGUI window provides for the creation of observing scripts 39 Figure 19 The xterm window used to execute the scripts created by the observer AM p e P 40 Figure 20 KOSMOS Status Monitor window alias kccd that shows the filter disperser and slit information as well as telescope telemetry data 41 Figure 21 Mayall environmental temperature display This is not part of the NOCS and is not present on the Blanco telescope ssi e ia te GA e reda ad 41 Page 6 of 100 C KOSMOS Instrument Manual V1 7 Figure 22 The VNC DHS window where images are displayed and where observers can select the Image Root Name file prefix eseeeem 42 Figure 23 NI CS s ame e ni eo qtti e hai s 43 Figure 24 Mayall guider patrol area relative to the KOSMOS field of view 57 Figure 25 Blanco guider patrol area relative to the KOSMOS field of view 58 Figure 26 He Ne Ar spectra for blue VPH grism blue offset slit sssssssssse 17 Figure 27 He Ne Ar spectra for blue VPH grism center slit aaneen 79 Figure 28 He Ne Ar spectra for blue VPH grism red offset slit
36. ITSCMD_2c89 nohs nohsDramaInit DONE OK M dhsSendMetaData starting Observation Number 10 expID 2456669 739168 stat 0 istat 0 M dhsSendMetaData send 0x9548ec0 size 120 stat 0 istat 0 M dhsSendMetaData sent 0x9548ec0 size 120 stat 120 istat 0 M dhsSendMetaData send metadata size 21120 stat 0 istat 0 M dhsSendMetaData sent metadata size 21120 stat 21120 istat 0 M dhsSendMetaData send mdConfig Oxbfabb840 size 32776 stat 0 istat 0 M dhsSendMetaData sent mdConfig OxbfabbB40 sizes32776 stat 32776 istat 0 DITSCMD 2c8a nohs nohsDramaEndObs DONE OK SUCCESS TASKenohs ACTION nohs endobs ARGS none DITSCMD 2c8b nmsl nmslDramalnit DONE OK DITSCMD 2c8c nmsl nocsDramaWgui DONE OK SUCCESS TASK nmsl ACTION namsl wgui ARGS Finished script home observer exec DFLAT U430 4 5 sh observer amp kosmos 4m exec I Figure 19 The xterm window used to execute the scripts created by the observer using NGUI The path needed to execute the scripts is home observer exec Continuing with the upper left hand screen we have the Page 40 of 100 C KOSMOS Instrument Manual V1 7 4 KOSMOS Status Monitor This window shows instrument and telescope telemetry nan X KOSMOS Observing Monitor cD y Sat Jan 11 05 42 47 PM MST2014 tcs target ra 0 41 27 50 2347 4m gwc kpno noao edu ji Universal Time 0 42
37. Image Focus Sky Twilight Flat Camera Spectra Focus o E Dome Flat Slit Acquisition Telescope Flat MOS Acquisition Telescope A Spectra Status DONE Exposure vector 1 Gain vr 1 emmy 0 66 Peat Mose Pep 1 e 6 84 rro Read Hase amp 2 e 6 69 e 72900 tens Out 5 75 76 istat d Pret Scale pix 0 29 Latest Dewar Temp Ke 136 0 Terminal sih 90x25 y l bservergkoraos n execls B ET EE Y Figure 13 The mayall 2 lower left hand monitor with the necessary KOSMOS windows shown NMSL NGUI and xterm The upper left hand window should look similar to this Page 34 of 100 C KOSMOS Instrument Manual V1 7 eene X KOSMOS Observing Monitor Hie Options Help 1 O9 tes target ra 0 41 27 50 O om 2347 4m gwc kpno noao edu Universal Time 0 42 47 Dome Azimuth 0 00 Sat Jan 11 05 42 47 PM MST 2014 Disperser Position Filter Position 1 12 2014 Dome Error 0 00 Slit Position 0 42 09 Dome Tracking off Camera Focus um 0 41 27 50 Telescope Focus um 11150 00 Collimator Focus um 32 10 00 5 Guider Mode off Shutter j 2014 0 South Guide X mm 119 86 IEB Air C 14 30 0 00 00 00 South Guide Y mm 28 92 Optical Bench 1C i Zenith Distance 0 20 Mirror
38. Instrument Manual V1 7 2 4 2 Red VPH Grism 0 105 0 1 0 085 F dA dx nm pix 0 085 2800 2800 2400 R A 3 33d 2200 2000 0 6 0 7 0 6 0 8 Wavelength microns Figure 6 Red VPH grism Scale and resolving power with a hypothetical 1 slit 2 4 3 Additional Grisms The disperser wheel has space for 3 additional dispersers leaving an open position for imaging Page 18 of 100 C KOSMOS Instrument Manual V1 7 2 5 CCD Detectors The table below summarizes basic parameters for both detectors At present only the e2v detector is available The LBNL detector would see use when available for programs that focus on observation at redder wavelengths Once a choice is available considerations are as follows e The e2v detector provides better blue response but its response is somewhat less in the red and decidedly lower in the far red e The LBNL is a thicker detector and therefore has a much higher cross section to cosmic rays Will add a couple of comparison figures when we have them e The LBNL detector will support nod and shuffle However implementation of this mode is not planned on any particular schedule e Dewar changes are a day time operation that must be scheduled in advance and which may not be possible on weekends TBC The detector or detectors required for the program must be identified on the telescope time request e2v typical QE 100 C Deep depletion silicon astr
39. Observatory This instrument was built to provide a modern high efficiency spectrograph for the U S community that meets many of the scientific needs described in the ReSTAR Renewing Small Telescopes for Astronomical Research Report KOSMOS was commissioned in October 2013 Figure 1 shows KOSMOS mounted in the Cassegrain Cage of the 4 m Mayall telescope t Figure 1 KOSMOS mounted in the Cassegrain Cage of the 4 m Mayall telescope KOSMOS was built by a partnership between Ohio State and NOAO and is largely based on the OSMOS Ohio State Multi Object Spectrograph instrument at the MDM 2 4m Hiltner telescope The heritage from OSMOS includes an all refractive optical design that enables imaging longslit and multi slit spectroscopy over a wide field rapid reconfiguration between observing modes and the capability to have a wide range of slits filters and dispersers mounted simultaneously Page 9 of 100 C KOSMOS Instrument Manual V1 7 KOSMOS has a nearly identical twin named COSMOS Cerro Tololo Ohio State Multi Object Spectrograph at the 4 m Blanco Telescope of the Cerro Tololo Inter American Observatory Except where noted otherwise explicitly all contents of this manual apply to both instruments even if only KOSMOS is named Page 10 of 100 C KOSMOS Instrument Manual V1 7 2 Instrument Characteristics The Kitt Peak Ohio State Multi Object Spectrograph KOSMOS is an imager and low to moderate resolution spec
40. S Instrument Manual V1 7 5 1 Startup Most of this section is devoted to starting the observing software but some additional tasks are listed at the end don t overlook these 5 1 1 Directory Structure The NOCS software runs on the computer Kosmos kosmos 4m at the Mayall 4 m telescope but is displayed on the computer mayal 2 or mayall 3 Mayall 2 and mayall 3 are Mac mini computers with 4 monitors and a small web camera You will operate the instrument logged into Kosmos Normally you will do any image processing needed to support your observations on this computer as well not the observer workstation When you are logged into kosmos your home directory will be home observer Type cd to return to this if you re not quite sure where you are You should also start IRAF in this directory since that s where the login cl file is located Some relevant sub directories are home observer exec observing scripts are created and run here home observer bin a few specialized commands are located here home observer data active data sub directory The data sub directory is actually an alias for data2 observer data YYYMMDD where YYYYMMDD is the date of the start of the night It is re evaluated whenever you restart the NOCS see below If you need to look at previous nights data you can navigate using the direct path listed above just specify the desired night s sub directory Directories on cosmos
41. angles In both cases the flexure perpendicular to the slit is small In general flexure will be 0 2 pixels hour in the dispersion direction For realistic exposure times this is far below the level that would degrade resolution but caution is required if you are trying to measure radial velocities to better than 0 1 pixel 5 km sec or so y pixels 3 2 1 0 1 2 3 x pixels Figure 9 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure Data are for KOSMOS The points are relative to zenith Z measured three times and correspond to two and four hours East and West at constant declination and 30 17 orientation for the dome s white spot 0 60 and 85 deg declination along the meridian These measurements were obtained With the instrument rotator at PA 0 deg Page 23 of 100 C KOSMOS Instrument Manual V1 7 y A pixels 3 2 1 0 1 2 3 X pixels Figure 10 Movement of the image of a central pinhole relative to the detector at different telescope orientations due to instrument flexure Data are for KOSMOS The points are relative to zenith Z measured three times and correspond to two and four hours East and West at constant declination and 30 17 orientation for the dome s white spot 0 60 and 85 deg declination along the meridian These measurements were obtained with the instrument rotator at PA
42. are organized in the same way The data directory on kosmos 4m will change if you restart after local noon Data are stored under a new date in the NOAO archive starting at 9 am regardless of whether the NOCS has been restarted You can specify the directory where new data are stored from the DHS window don t do this unless you are sure you know what you are doing Page 31 of 100 C KOSMOS Instrument Manual V1 7 5 1 2 Tasks in the Cage Before starting the NOCS software it is important to make sure that the Torrent controller for KOSMOS is turned on and that the dark slide has been moved to the open position Both the Torrent power switch and the KOSMOS dark slide are located in the Mayall Cassegrain cage Turning on the Torrent controller must be performed by a KPNO CTIO staff member Normally the controller is left on during the day but it may be turned off if there is a risk of lightning or because of engineering or maintenance activities The observer is allowed to open the dark slide if they have been instructed the dark slide is normally closed by the telescope operator at the end of the night The dark slide is located on the far side of the instrument from the cage door near the top see Figure 12 Pull down on the handle slightly and slide in or out Note that the slide is somewhat counter intuitive in that it is opened by pushing the handle in and closed by pulling it out Confirm that you ve set the dark slide correctly
43. ch you zeroed the telescope pointing Use the smallest reasonable region of interest for each step This can save you up to 30 seconds image and can therefore cut telescope time used by 2 3 minutes per object Note that the short slit spectral region 320x4k is 90 arcsec long which should be more than enough for point sources and compact targets For most long slit acquisition 1k x 1k should be enough It is always tempting to look at the last image before slewing to the next target Recognize that this costs time and decide for yourself whether you gain anything by doing this 7 2 Step by Step Observing 1 Once the shutter closes on the current observation you can start slewing to the next position If you are using KOSMOS and need to adjust the rotator that next position is the zenith If you are not changing the rotator skip to step 3 2 Atthe zenith the OA will go into the cage and adjust the rotator For long slit observations he she can set it to the required accuracy in the cage for MOS Page 72 of 100 C KOSMOS Instrument Manual V1 7 observations it will need to be tweaked from the control room but this can be done away from zenith 3 Slew to the target If you need to tweak the rotator the OA can do it now larger adjustments are possible with COSMOS Also the OA can identify a guide star and direct the guide probe to move to that position Unless it s a very short slew both the rotator and guider will be wh
44. command to fully execute before typing the next cd nocs start hardware nocs start all If you need to perform other tasks for example run IRAF on the kosmos computer open another xterm and issue the same ssh command as above then start IRAF or whatever else you want to do If you are observing with COSMOS the everything described here and in the rest of this section except that the kosmos is replaced with cosmos in accessing computers 5 1 4 Shutdown To shut down the NOCS at the end of the night type nocs stop all nocs stop hardware You do not need to be in any particular directory to do this The telescope operator will close the dark slide when he she fills the dewar on the Mayall only the COSMOS dewar does not need to be filled at the end of the night the dark slide should still be closed Page 33 of 100 C KOSMOS Instrument Manual V1 7 5 2 User I nterface After KOSMOS has been initialized a variety of windows will open to enable observing with KOSMOS Upon successful completion of starting the KOSMOS user interface the lower left hand monitor should look similar to this dl Terminal Shell Edi View Window Help D EB O 4 Sat 5 46 17 PM 4meter_Q X NMSL kosmos on N NOAO KOSMOS Spectrograph Mayall 4m Telescope pe Help ay Sat Jan 11 05 4424 PM MST 2014 integration timer 7 0 7 0 wocswe Finished script home observer exec DFLAT U4305 sh Telescope Focus Image Camera
45. d 360 degrees The only available atmospheric dispersion corrector on the Mayall has a field of view substantially less than 10 arcminutes and the guide probe needs to work within this field when the ADC is used Thus use of the ADC in multi slit mode is generally impractical You should therefore plan to observe close to zenith or else design masks to be used at a position angle close to the parallactic angle of the observations C 3 COSMOS Constraints The Blanco rotator is capable of rotation over a larger range than the Blanco but has a zone of exclusion between 88 and 92 degrees Also the atmospheric dispersion corrector available on the Blanco has a field of view large enough to allow use of the full field and the guider Its use is therefore recommended Page 88 of 100 C KOSMOS Instrument Manual V1 7 C 4 Mask Design The program currently recommended for mask design is adapted from the program used for OSMOS It is a very basic program and may eventually be replaced by something with greater versatility The program will only run on Linux based computers and older Macs This is because it relies on the ESO Skycat utilities which is no longer being updated and thus is incompatible with recent versions of OSX Information on the mask design software can be found at http www ctio noao edu points CKOSMOS ckosmos_mos html The web page includes links to download the KMS software and the ESO SkyCat tool A link to a Ge
46. d Mask Changes This information is included for completeness observers are not expected to perform mask or filter changes Filter changes are normally performed only during the day mask changes can be carried out at night by the telescope operator but the observer may be able to help Filters or multislit masks should be installed in holders Longslits are pre assembled into holders so it s a matter of selecting the longslits to be installed Filters are installed in holders by the day crew since there are spare filter holders any filters you may have requested should be already installed in holders At the Mayall they will be kept in the loading room old plate loading room outside the control room Access to the instrument for this purpose is shown in the figures below Figure 32 Location of access ports for slits top and filters bottom Page 92 of 100 C KOSMOS Instrument Manual V1 7 A disassembled multislit mask holder is shown below it consists of the holder itself and a retaining ring that clamps the mask into place The 4 clamps can be seen around the inner edge of the holder Alignment pins can also be seen at approximately the 6 11 and 12 o clock positions The KOSMOS masks are cut from stainless steel shim stock that is coated black on one side One such mask is shown in Figure 34 COSMOS masks are cut either from aluminum shim stock that is blackened on both sides or a thin carbon fiber sheet The
47. d be used in creating and using nested scripts In particular do not attempt to scripts that are more complex than a sequence of scripts and NOCS commands Also be aware that aborting a script that is running inside a higher level script will likely not work properly there is a good chance you will have to re start the NOCS afterward Consequently this approach is recommended only for sequences of observations that will run unattended such as calibrations over dinner and that you are confident will execute correctly 5 3 5 Running Scripts After you ve created scripts by whatever means you should type rehash to allow them to executed just by typing the name e g Spectra sh If you haven t done a rehash after the script was created precede the name by e g Spectra sh You will then see the contents of the script displayed in the xterm as it executes and there should be activity in the appropriate windows of the NOCS 5 3 6 Aborting Scripts If your script contains only one or two exposures it may be simpler to abort the individual exposures use the Abort button on the righthand side of the NMSL window Fig 16 Page 47 of 100 C KOSMOS Instrument Manual V1 7 If your script is about to finish minute or two just let it run to completion as the recovery after an abort will take about the same time If however neither of these apply Type CNTRL C cr in the shell window If you are
48. e new focus Page 53 of 100 C KOSMOS Instrument Manual V1 7 You must reset the camera to the best focus whether it s unchanged or a new value This is because it s currently set to the value at the end of the focus sequence The command to do so is testnics camfocus xxxx where xxxx is the desired focus value The instrument status display will update after a few seconds and should show the correct value Note you can also set focus from the NICS window see section 5 2 You can adjust focus based on the temperature change using the nominal coefficient of 10 microns degree You need to keep track of record the bench temperature for which you measured focus If the temperature seems to be changing systematically in a particular direction and has changed by 2 C or so calculate the new focus and then apply it using testnics camfocus xxxx For example if your focus was 2020 determined at a temperature of 10 0 C and the bench temperature is now 8 0 C and declining steadily change the focus to 2040 testnics camfocus 2040 Don t do this in the middle of an exposure and preferably not in the middle of an observing sequence Page 54 of 100 C KOSMOS Instrument Manual V1 7 5 6 Pointing and Telescope Focus 5 6 1 Pointing Check At the start of the night the observing assistant will point to a moderately bright star which should be centered in the middle of the field You should do the following e Create an a
49. ed something edit the line for the item you removed to substitute what you ve installed For filters the KPNO or CTIO filter ID goes in the last column For multislit masks the 6 digit ID goes in the last column TBC Page 95 of 100 C KOSMOS Instrument Manual V1 7 Make sure there is an open position in the wheel and that it is called Open You can change which physical location in the wheel this is Save the file When you ve made all the changes type bin change hardware to update the NOCS Starting the NOCS automatically uses the updated files so the change hardware command isn t required If you want to verify that everything is correct open the NICS window see section 5 2 and confirm that the filters and slits displayed there are what you expect you can then try moving to the position of one of the new items enable command buttons to do so Page 96 of 100 C KOSMOS Instrument Manual V1 7 Appendix F Basic Data Reduction We will eventually add more detail but for the time being users can get most of the guidance they need for both imaging data and longslit spectral data using the cookbooks and tutorials at http iraf net irafdocs http iraf noao edu iraf web tutorials tutorials html While these are 20 years old they are by no means outdated F 1 Imaging Data more F 2 Long Slit Data more F 3 Multi Slit Data Here the IRAF tutorials are of less assistance Page 97 of 100
50. ensity HeNeAr KOSMOS Blue Grating Blue Slit 5500 5600 5700 5800 5900 6000 6100 6200 Wavelength A Figure 26 He Ne Ar spectra for blue VPH grism blue offset slit Page 77 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Blue Grating Center Slit 1 5x10 Rel Intensity 5000 5000 y 4500 Rel Intensity 4000 3800 3900 4000 4100 4200 4300 4400 4500 4600 Wavelength A HeNeAr KOSMOS Blue Grating Center Slit 5000 5000 4500 Rel Intensity 4000 e Me UL TL Eae a e a dae do 4500 4600 4700 4800 4900 6000 5100 5200 5300 Wavelength A Page 78 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Blue Grating Center Slit 33 i 83 E t 4 E amp 5000 5000 2 F 4500 4 El 4000 5200 5300 5400 5500 5600 5700 5800 5900 6000 Wavelength A HeNeAr KOSMOS Blue Grating Center Slit z z gt P ll Er 2 10 E 5000 La MI al A LL A 5000 gt E 4500 E E 4000 5900 6000 6100 6200 6300 6400 6500 6600 Wavelength A Figure 27 He Ne Ar spectra for blue VPH grism center slit Page 79 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Blue Grating Red Slit 10 Rel Intensity 5000 5000 4500 Rel Intensity 4000 4200 4300 4400 4500 4600 4700 4800 4900 Wavelength A HeNeAr KOSMOS Blue Grating Red Slit 1 5x10 10 Rel Intensity 5000 5000 4500 Rel Intensity 4000 49
51. ere they are needed by the time you get to the target 4 f you are carrying out a program where you really need to get an arc spectrum at the position of the telescope start the rotator mirror moving to the comparison position Don t do this unless using night sky lines for zero point adjustments is really not sufficient If you can skip this go to step 7 5 Take an arc spectrum If you aren t using a generic arc script for example you want the object name in the header define the script beforehand 6 Move the rotator mirror back to the through position If the arc script is set up with mirror control enabled this will be automatic Note the script will also move the mirror into the comparison position but it s preferable to do that manually while the telescope is slewing and then start the script once the telescope is on target 7 Once the telescope has completed the slew and if necessary the rotator mirror is back in the through position the OA can verify that the guide star is visible This can be done once the dome is close to its final position even if there is some vignetting 8 Assuming the telescope is pointing fairly reliably the OA should move the guide star to the center of the guider field and then lock on it turn on guiding 9 Now execute the appropriate NOCS acquisition script Again if you aren t using a generic script prepare it beforehand 10 Run ccdproc on the images you will save a few seconds
52. hort as 0 01 seconds are possible although the accuracy of such short exposures is poor It is recommended that exposures be kept to 0 5 second or longer if photometric accuracy of 196 is required For short exposures repeatability and accuracy across the field are better than the absolute timing accuracy which may be off too long by as much as 7 msec The shutter actually takes about 1 second to open or close for short exposures one leaf of the shutter is open while the other leaf follows it and closes thus for very short exposures a narrow slot moves across the focal plane The time when photons first arrive at the detector will therefore come several tenths of a second after the nominal start of the exposure and this time will vary across the detector along the length of the slit The shutter delays are taken into account when starting the readout of the CCD Note that the actual duration of the exposure exposure to light is correct and accurate Page 26 of 100 C KOSMOS Instrument Manual V1 7 3 Proposing for KOSMOS In order to write an observing proposal for KOSMOS you should understand the available instrument configurations section 2 above You should also think through how you will actually observe In particular Which instrument modes will you need imaging longslit multislit Note that some imaging is required for acquisition but you don t need to calibrate these images If you are doing multislit observati
53. however since they won t run properly if filter names differ slightly or instrument configurations are at all different Page 28 of 100 C KOSMOS Instrument Manual V1 7 5 Observing with KOSMOS Section 5 this one and Section 6 describe the KOSMOS observing procedures in detail Please read through them carefully you may then want to read Section 7 which provides suggestions for optimizing your observing efficiency The software used to control KOSMOS is called the NOAO Observation Control System NOCS The NOCS is a script based software package meaning that a script that has most likely been created by the observer performs all of the data acquisition A script editor the NOAO Graphical User Interface NGUI is part of the software package making it simple to create scripts as you observe The NGUI software can be downloaded by visiting astronomers here The NGUI is discussed in more detail in section 5 2 NOAO may provide some basic scripts related to calibrations but for the most part you will need to create the scripts you will use The predefined scripts will be discussed in more detail in the calibration section 6 Several computers work together to obtain KOSMOS data The list below is specific to KOSMOS but the arrangements for COSMOS are very similar Although the observer should only need to access kosmos and mayall 2 or mayal 3 we list the full complement of computers for completeness mayall 2 or mayall 3
54. if you process each frame of the sequence once it s written to disk 11 Now run the appropriate alignment script kalign for MOS koffset for long slit 12 Give the resulting offsets to the OA 13 If you don t need to check the result skip to step 15 In general it s recommended that you check the alignment if the offset was gt 10 arcsec or involved a change in the rotator angle of any size 14 If you want to recheck the alignment take an image of the field on y You can use the slit image you took on the first iteration Go back to step 11 NOTE the long slit alignment script currently doesn t support this you have to take the slit image right before the field image 15 Now you are ready to take spectra Run the spectra script which you should have prepared beforehand Page 73 of 100 C KOSMOS Instrument Manual V1 7 16 It is recommended that you recheck the alignment every 90 120 minutes Since there is both flexure between slit and detector and slit and guider you need to get both the slit and field images That is go back to step 9 You should find that any offsets are small If you ran an arc spectrum at the beginning of the observation you may want to take another at this point See steps 18 20 if you really want to do this 17 0nce you have finished with the spectra you are done go to step 1 for your next object unless you need to get an arc spectrum in which case continue with the next steps 18 Advise the OA wh
55. ify pathnames appropriately and or locate the kms files differently the approach described here works as efficiently as any alternative Page 62 of 100 C KOSMOS Instrument Manual V1 7 5 10 I maging Acquisition Acquisition for imaging is performed in the same way as for the initial pointing zero determination 3 4 above If you are doing long exposures or working with narrowband filters you may want to position the telescope using short exposures through a broadband filter If you are only interested in a single object or a small area you can generally skip the pointing check and just start observing Page 63 of 100 C KOSMOS Instrument Manual V1 7 5 11 Observing Once you have properly centered the object or field you can then execute the prepared script You can verify that you are using the configuration you really wanted by looking at the status display Unless this is a very short observation this is a good time to make sure you have the scripts you need for the next observation but remember that you should not over write a script that it is in the midst of execution Page 64 of 100 C KOSMOS Instrument Manual V1 7 6 KOSMOS Calibrations Most calibrations can be carried out in the afternoon so you don t use much of the night observing light bulbs This is practical because instrument flexure is modest see Section 2 7 and because the mechanisms are extremely repeatable There are two cautions however e f
56. ign ir cvi P rk RR RACE RA AR 88 Page 4 of 100 C KOSMOS Instrument Manual V1 7 Col Basic Considerations O Var Oed DIN CLAN 88 G2 KOSMOS CONSTA tl cades pa ondas 88 ES COSMOS CORSA ae 88 CA MSDS trado ONARE 89 Appendix D Basic Troubleshooting ice a 90 DIL Problems With PhOotOns xci Pa dial 90 D 2 Problems with Electrons Including Instrument Start Up seseeeese 90 D 3 Problems Not Covered ADOVE so ed ive rfr sr e a C eR EE c ri ad 91 Appendix E Filter and Mask Changes oi orn e nen tr enr a v ey ed a c 92 Appendix F Basic Data Reduction ice mii re i ce ec em d en d a 97 FI maging Dalla esaet es edvseg da dit da aera 97 P 2 Longest Dad AAA A oa ratu a a iL SCC 97 Pos ulus SINE A a oa dr i tta uiua ra od ue ra eU dera 97 References sce a ob a ORI ERRAT RD cR Reda EU cus lest iD eda ada E s da S aa 98 instrument TeaM NE DIL NI DL T 99 KOSMOS Observing Cheat Shegbs cine ww yx peer a onu road aa Ea E NS Et 100 Page 5 of 100 C KOSMOS Instrument Manual V1 7 Figures Figure 1 KOSMOS mounted in the Cassegrain Cage of the 4 m Mayall telescope 9 Figure 2 KOSMOS Optical EayOUL iiio iceo uro d sien eni ii Pe DINE YR a YA Rte yp a 11 Figure 3 KOSMOS imaging field of view in relation to the detector 12 Figure 4 Total spectroscopic efficiency with the blue and red VPH grisms 14 Figure 5 Blue VPH grism Scale and resolving power with a hypothetical
57. ilter changes during the night End of night o KOSMOS only fill dewar o Initiate execution of additional calibrations normally needed only if you have done slit changes during the night Page 100 of 100
58. increments with each exposure and is never reset so every image will have a unique name Because the data are sent to the archive separately you can delete or process images in the local directory without losing the ability to recover the raw data later Note that it takes a few typically 6 seconds after the script completes for the data to be written to disk you will see a message in the lower left window on the DHS VNC window when that happens 5 4 2 Data Management For many of the tasks described below it is very helpful to do some processing on the data for simplicity we recommend that you process all data using the basic steps below You need to decide how you want to handle the products of this processing There are a couple of options e You can over write the raw data with the processed data The raw data are copied first to a sub directory default name Raw You can change where and whether the raw data are copied using the mscred parameters epar mscred This is the recommended approach If you adopt this approach note that a command along the lines of ccdproc Night1 fits will process any fits files beginning with Night1 that have not already been processed See below for more e You can instead process data and specify where the processed files are to go and what they are named This requires that you create a list of files to be processed and another list of processed files before each time you run ccdproc
59. ip it After you are done with the selection the field image is selected and you will be prompted to select the matching alignment stars in the same order Once you are done the script will output values for RA and Dec offsets and rotation The RA and Dec offsets can be done with the guider in follow mode but the rotational adjustment doesn t support this so you are normally better off performing the rotational adjustment with the guider off then re acquiring the guide star You will almost certainly need to repeat the procedure you don t need to take another mask image if you do Page 61 of 100 C KOSMOS Instrument Manual V1 7 At the time of writing neither telescope has a working fine encoder so it s not possible to set the rotator to better than the nearest 0 1 degree On the Mayall we have found that setting the rotator to the nominal mask PA plus 0 1 degree will get you within measurement errors on the rotational adjustment On the Blanco there is not currently a single offset that works for all rotation angles Once you are done you should close the ds9 window you had open for IRAF reductions the window created by kalign shou d work but if it doesn t close that as well and open a brand new ds9 window for use with IRAF Note if you just type python kalign py you will see a description of the command options You can run the alignment procedure from a different directory e g the data directory if you spec
60. it TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 5 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 6 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 7 7 with DP S init TYPE FOCUS DHS CAMSFOCUS nguiSetExecClose INFO wrote script home observer exec CAMSFOCUS sh nquiSetExecOpen lt INFO gt opened file home observer exec CAMSFODUS sh nquiSet bs lt CAMSFOCUS gt Writing observation 1 1 as 1 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS i lt CAMSFOCUS gt Writing observation 1 1 as 2 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 3 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 4 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 5 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 6 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt Writing observation 1 1 as 7 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS nguiSetExecClose INFO wrote script home observer exec CAMSFOCUS sh nquiSetExecOpen lt INFO gt opened file home observer exec CAMSFOCUS sh nquiSet bs lt CAMSFOCUS gt Writing observation 1 1 as 1 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS i lt CAMSFOCUS gt Writing observation 1 1 as 2 7 with DPOS init TYPE FOCUS DHS CAMSFOCUS lt CAMSFOCUS gt
61. it does notturn red it will probably correct itself don t restart the NOCS until you verify you cannot take data usually a bias frame is a good quick test e Image appears to read out normally but never appears in the data directory The image may be hung up in the DHS Sometimes taking another image try a bias as that s quick will push the image through If not see the NEWFIRM troubleshooting suggestions referenced in D 3 below e Mechanism error This is infrequent but if a mechanism has stalled you can reset it using the command sequence cd bin change_hardware cd exec If the mechanism continues to malfunction you need to call for assistance as mechanism stalls should be isolated and infrequent D 3 Problems Not Covered Above If simple software re starts do not work power cycling the instrument and detector electronics may be necessary The observer should not do this on his her own Call for assistance if someone qualified is not present already Try the following resources e Mosaic manual Appendices F and G http www noao edu kpno mosaic manual e NEWFIRM manual Appendix http www noao edu ets newfirm documents NEWFIRM user rev3 4 pdf Use with caution As noted above stopping and restarting the system will solve most problems and is often quicker than trying to check through the documentation to find a more focused solution Page 91 of 100 C KOSMOS Instrument Manual V1 7 Appendix E Filter an
62. l Field Y 200 mm 22 X 128mm 14 1 128mm 14 1 Figure 24 Mayall guider patrol area relative to the KOSMOS field of view Selection of guide stars within the gray rectangle can cause the guide probe to vignette the KOSMOS field The size of the region that leads to vignetting is somewhat conservative particularly for longslit spectroscopy At PA 90 deg N is Y and E is X Page 57 of 100 C KOSMOS Instrument Manual V1 7 70 Vignetted 90 99 70 120 Figure 25 Blanco guider patrol area relative to the KOSMOS field of view Selection of guide stars within the lower region can cause the guide probe to vignette the COSMOS field The size of the region that leads to vignetting Is somewhat conservative particularly for longslit spectroscopy Page 58 of 100 C KOSMOS Instrument Manual V1 7 5 8 Longslit Acquisition Longslit acquisition can be done using three IRAF scripts described below The basic process performed by the acquisition consists of taking an image through the slit you want to observe with followed by an image of the field you want to observe Guiding must be on The observations can be done with any filter not necessarily the blocking filter for your spectra For most acquisition the script to use is koffset1 In the IRAF xgterm type epar koffset1 The file prefix needs to match what you are using for the acquisition images if you keep the same prefix all night or all run yo
63. lit image If you type j when looking at the slit image while running the script you will see how it is centered along the slit the counts you see should be comparable to the peak counts in the field image if you are close to being centered Note that they are not likely to equal the peak because of the way the IRAF algorithm works Page 59 of 100 C KOSMOS Instrument Manual V1 7 The other two scripts that can be of assistance with acquisition are kosmos offset and slitmove kosmos offset allows you to handle offsets in situations where you don t have a slit image It can be useful in moving around in an imaging field In particular you need to specify the position you want to move to X and Y You must also specify the rotator position angle the pixel scale may need to be entered as well use 0 292 as the value Then type g and the image will be displayed for you to centroid on your target you will again get offsets for the telescope operator The third script slitmove is used to offset between the nominal longslit positions the command is slitmove current new where the two positions can be blue center red So if you are currently at the blue slit position and want to go to the center slit you would type slitmove blue center I mportant This offset is approximate but will get you close to the correct position you must re acquire the object on the new slit Page 60 of 100 C KOSMOS In
64. lthough you can change the prefix as often as you want for example to match object names it s very easy to forget to do it every time We recommend picking a more generic prefix that you won t need to change as often e g raw or Night1 e Also within the NGUI Options menu are several boxes that can be checked or unchecked Confirm that the Parallelize Mechanisms and Include Temperature Readback boxes are checked and the Include Gain Control box is NOT checked The lamp control boxes are discussed in more detail in the section on calibrations for the purposes of startup it doesn t matter whether they are checked or not It s also helpful to position the various windows in a way that allows you to observe efficiently the layout described about is one we have found helpful 5 3 2 Creating Scripts A few basic calibration scripts should already be available to you a list is provided below A more extensive set of scripts has not been provided because they rely on having all elements with the same exact names in the current configuration and in the script since you can only check this by viewing the script in a text editor or trying to run it it s usually quicker to create what you need To create a script select one of the buttons on NGUI the grayed out options are not supported A new window appears allowing you to select parameters for the script including both the script name and the object name The parameters that
65. mode but at the time of writing the ability to dither along the slit is not fully functional Because the script creating windows normally recall parameters from the last time they were used the SPECTRA I and II scripts can be used to remember parameters for 2 different configurations for example a red and a blue set up so that you only need to update object names and exposure times times Things that are easy to overlook when creating scripts e Dont forget to specify the object name e f you are taking spectra with more than one disperser configuration check the disperser filter and slit when creating the script The SPECTRA and II options are intended to help out here WARNI NG Do not create scripts before you come to the telescope with the intention of using them to observe proper execution of scripts requires the instrument configuration used in creating the script to be the same as the instrument configuration actually present 5 3 3 Lamp Control If you click on the NGUI options menu you will see two check boxes for lamp control and lamp prompt If the lamp control box is checked any script you generate will make sure that comparison lamps in the rotator are turned on or off as appropriate and also that the comparison mirror is in the correct position either comp or thru If this box is selected the status of the lamp prompt isn t relevant This does not control the dome flat lamps If the lamp control bo
66. o needs to turn off the guiding 19 Execute the arc script it should move the rotator mirror for you both in and out but if you didn t set it up that way have the OA move the mirror and then start the script once the mirror is in place this is less efficient obviously 20 If you are done with the object go to step 1 for the next object If you are not done have the observer turn the guider back on once the guide star is visible Then go back to step 9 or step 15 depending on whether the alignment needs to be checked Page 74 of 100 C KOSMOS Instrument Manual V1 7 Appendix A KOSMOS FI TS Header Page 75 of 100 C KOSMOS Instrument Manual V1 7 Appendix B Calibration Lamp Spectra The images in this appendix are organized according to slit position and disperser 4 panels for each configuration HeNeAr KOSMOS Blue Grating Blue Slit d E Rel Intensity 4168 59 Al __ 5000 5000 y 4500 Rel Intensity 4000 3500 3600 3700 3800 3900 4000 4100 4200 Wavelength A HeNeAr KOSMOS Blue Grating Blue Slit 10 po 4713 143 Hel__ Rel Intensity 5000 5000 Rel Intensity gt a e o 4000 I 4200 4300 4400 4500 4600 4700 4800 4900 Wavelength A Page 76 of 100 C KOSMOS Instrument Manual V1 7 HeNeAr KOSMOS Blue Grating Blue Slit 5187 746 Al __ 5000 5000 4500 4000 4900 5000 5100 5200 5300 5400 5500 5600 Wavelength A Rel Int
67. o process 100 90 80 70 sd uu 90 O 40 30 20 10 0 300 500 700 900 1100 Wavelength nm D42 default LBNL Figure 7 Nominal quantum efficiency curves for the KOSMOS and COSMOS detectors Additional detector parameters are summarized below Page 19 of 100 C KOSMOS Instrument Manual V1 7 Table 3 Detector Parameters Detector e2v LBNL Read Noise 5 electrons TBD Gain 0 6 e ADU Regions of Interest Read 4k x 2k 46 sec TBD xxx time 1x1 binning 2k x 2k 26 sec lk x 1k 13 sec 4k x 320 13 sec Binning 1x1 2x2 1x2 TBD Nod and Shuffle No For most observing programs the detectors will be operating unbinned 1x1 binning This is because the unbinned mode is matched to both the resolution of the spectrograph and reasonable seeing The software supports 2x2 binning and 2x1 binning The 2x1 mode bins a ong the slit this is potentially of interest to someone trying to take a series of spectra with minimum readout time probably also using the 4k x 320 ROI Page 20 of 100 C KOSMOS Instrument Manual V1 7 2 6 Slits 2 6 1 Facility Longslits Center Slit Blue Slit Y 4 mdi Figure 8 Location of the Red Center and Blue long slits relative to the detector and field of view The blue and red slits are offset by 160 25mm physical units at the focal surface relative to the
68. ons where will you get the imaging data to create your masks What filters will you need to acquire your objects or for any imaging data you need Once there is a choice of CCDs is one preferred to the other Does your program benefit from switching detectors partway through the run For KOSMOS which does not have an atmospheric dispersion corrector available can you manage to orient your multislit masks so atmospheric dispersion runs along the slits more or less If you require more than one spectroscopic configuration how will you handle this The choices are either to do all configurations at each target setting or to observe all targets with one setting then repeat the targets with another Overheads are likely to be somewhat lower with the first approach but if one configuration is more important than the others the second approach may still be preferable If you are using both CCDs once they are available the second approach is the only possibility The mechanisms are highly repeatable so for almost all programs switching configurations for each object is reasonable Page 27 of 100 C KOSMOS Instrument Manual V1 7 4 Observing Preparation Once you ve been allotted time consult the relevant web page s for KPNO and CTIO respectively http www noao edu kpno observer info shtml http www ctio noao edu noao content Planning Executing Wrapping your run CTI O Both observatories will ask you to specify the ins
69. operator s point of view but what you have to do with the instrument will be the same advising the operator when the star is centered 5 6 2 Telescope Focus The telescope focus script will take a single image where the telescope focus is incremented and the charge is shifted along a column Y axis for e2v X axis for LBNL with an extra offset for the final focus setting You need a star or stars that are bright enough to give good profile measurements but not so bright that you need a really short exposure to avoid saturation because you want to average the seeing somewhat Exposure times in the few second range are optimal The image is analyzed using the starfocus routine in the obsutil package Settings for the routine are use epar starfoc to access them Page 55 of 100 C KOSMOS Instrument Manual V1 7 images image with focus sequences focus 1x1 fstep focus step e g 50 or 100 gt nexposure number of exposures e g 7 step step set in script in pixel e g 30 direction 2 line gap end coords mark1 You can also tinker with the measurement parameters further down if you want and have an idea of what you are doing but it s not essential If you want the FWHM in arcsec the pixel scale to use is 0 292 Before running starfoc on the image you should run ccdproc on the image When you run the routine it will display the image and you should use the m key to identify the starting
70. overscan interactively the settings should read no minmax 1 1 1 3 3 0 If you type ccdproc fits ccdproc will only process images that haven t been previously processed However it does take time to check the already processed images so this can be rather slow if you ve already taken a lot of images that night You are therefore better off specifying a small range of images to check process or if you are doing long exposures just the single most recent image For example ccdproc Night1 0905 fits ccdproc data 08755 fits If you are an experienced IRAF user you are obviously free to handle your images differently but in that case you are relying on your experience and not this manual Page 52 of 100 C KOSMOS Instrument Manual V1 7 5 5 Camera Focus The camera focus should be checked and reset if necessary before doing afternoon calibrations The camera focus does have a temperature dependence of approximately 10 microns degree Focus shifts of 25 microns will start to affect image quality so it is recommended that you re check focus if the bench temperature shown on the status monitor changes by much more than 2 C The external ambient temperature provides some guidance on how the bench temperature might change in the future You can use the temperature coefficient to adjust focus without checking see below but it is not recommended you do this for changes gt 3 C To check focus Set up a spectral camera foc
71. ppropriate image script if you don t have one already It should have a short exposure time perhaps 0 1 sec but 0 01 sec is acceptable for a bright star and an appropriate filter SDSS r for example If you name the script something like Pointing it can be re used as needed e Run the script e Run ccdproc on the resulting image after loading the mscred package this will create a composite image e From the IRAF xgterm o Execute epar kosmos offset you will need to specify the desired position e g 512 512 for a 1k x 1k image the image with the star field the rotator angle and perhaps the pixel scale 0 292 if not already at this value o Type g it will display the field and then ask you to center the star If the star image is not too badly saturated center the cursor on the star and type a if it is saturated center as best you can and type m e Give the resulting offset values to the operator There is no point in trying to center better than a few arcsec for this purpose so it is not necessary to iterate these steps t may be convenient at times to re zero the telescope coordinates for example if you are working in a particular area of sky away from zenith in that case follow the same procedure If you are observing the first night the instrument is installed the operator may need to do additional pointing checks just repeat the process above The procedure for COSMOS may not be identical from the telescope
72. rber viewer program also free is included at the end this lets you view your mask designs Page 89 of 100 C KOSMOS Instrument Manual V1 7 Appendix D Basic Troubleshooting D 1 Problems with Photons Problems and solutions No light on images Check for the following o Is the dark slide open Unfortunately there s no way to check without going out to the cage but if you were seeing light previously the dark slide will not have closed spontaneously That is this is a start up problem not a problem in the middle of the night o Is the rotator mirror in the correct position For arcs it should be in the comp position check the instrument status display for any other image including flats it should be in the thru position This can occur if you have disabled lamp control for a script and then did not set the lamps and mirror manually o Are the telescope mirror covers open o Is the detector operating properly Check for errors in the NMSL window I mages are saturated Usually a problem if you were trying to take spectra o Check that a slit or mask is in the beam and not the open position see instrument status display o For imaging flats check that dome flat lamp is set correctly usually on low Spectra badly out of focus Did you run a camera focus script and forget to reset the focus afterward Check that the focus displayed on the instrument status display is correct and if not set the correct value
73. s you current mechanism status You can also control the mechanisms if you open the Options menu and select Enable command buttons You can then move the mechanisms by clicking on the position for the wheels or entering a number and then clicking on the mechanism focus button focus stages You can hide the upper text panel from the Options menu Page 43 of 100 C KOSMOS Instrument Manual V1 7 5 3 How to Take Data All data are taken by executing a script that you or someone else have previously created The script defines the observing parameters including object name Scripts are located in the home observer exec directory You can practice creating scripts with NGUI but scripts created elsewhere may or may not work at the telescope because the filter or slit configurations may be different 5 3 1 Getting Started At the start of your run you need to specify some basic parameters These are preserved even if you restart the NOCS so you only need to do this once or if something changes e In the NGUI window upper left corner select Options gt Set Project This allows you to specify the proposal 1D observer and telescope operator e Then issue the command nocs set project e Inthe VNC window for the DHS in the window on the upper left select the Paths amp Files You can then specify the prefix that is applied to all your data files The prefix you specify is followed by a and a file number A
74. see section 5 5 D 2 Problems with Electrons Including nstrument Start Up Many problems can be solved by stopping and starting the NOCS see section 5 1 4 and 5 1 3 respectively However not all problems are best solved this way though stopping restarting is a good generic solution Specifically NMSL display window shows orange text box background The detector computer is in simulation mode and the detector is not being read out If the problem is a communications issue stopping and restarting the NOCS may cure it If there are problems with communications links issuing the command Sbin fixlink before issuing the NOCS startup commands may solve the problem If not the controller electronics may be powered off call electronics support for assistance in checking this and for further troubleshooting if required Relevant procedures are listed in the operations manual Section 4 2 as these require manipulation Page 90 of 100 C KOSMOS Instrument Manual V1 7 of the Torrent controller and other electronics users should not attempt these on their own e Error messages in NMSL window Usually accompanied by inability to take data If this occurs try issuing the command nmslReset and see if the error messages stop and you can take data Again if this doesn t solve the problem call electronics support for help e Readout time counter runs through zero and turns red and negative Stop and restart the NOCS Note that if
75. stom Multi Object Slit Masks 4 eren ran dara 21 A A E S 23 A dines dis tans eos an aos anya en d MU d D RO aaa a ada ea eae ohana CER A Rd 26 3 Proposing TORI O SMS ss ees costes auan edo s facet estie etus a a ea et ies 27 4 Observing Preparation acces onte ta Ceteri ad 28 5 Observing With KOSMO Sua 29 A A II o 31 5 Ll Directory StRUGtu re usarios 31 51 2 Tasks MINE Cara a aan a N a a 32 5 13 NOCS StartUp aos oria e eot 33 5 14 ShUEBOWELT vesicae bed icis eo VE he wea per re ne vec v e b PE E s 33 5 2 USEF Interface oda oda 34 5 3 How A i eed at e d e ud ve o 44 5 3 Getting Started ner seq otv O A Vv te i 44 5 3 2 Creabllig SCH DES riada di 44 5 3 3 Hamp CONTRO Iz seus euo delito A 46 5 3 4 NESTING SCHIDES usos ordeo Ee ire ai EP dede nce Pa b o tede tv n end 46 5 3 5 RUNNING SCHIDES iia id 47 Page 3 of 100 C KOSMOS Instrument Manual V1 7 5 240 Aborting Scripts vasteratera oM a A itu aU EYE RPM OUR ELMAR 47 bo Script Mana deme Cati 48 5 3 8 Automated Observation Logging klog ooooocccccocccnnncccnnnnocononarononarononanons 49 oS ADI E O MH Natoetes 50 5 1 I Data Storage uie doi AR OL AD Cd e DR RR asa D D ARD dax At DNA 50 5 4 2 Data Management tado cis caigo os eade Dundee Settee aay 50 5 9 CalhiBra FOCUS esce aE boit lb te veeipute a 53 5 6 Pointing and Telescope FOCUS sedie aera e aca ore ee EIER E ee E da 55 5 5 L Polnting Gelesen Veen ween d car On or Pelo ca oxyde efc D
76. strument Manual V1 7 5 9 Multi slit Acquisition The data for multi slit acquisition are taken in the same way as for longslit acquisition but the subsequence procedure is quite different You must acquire images using the 2k x 2k ROI and then process them with ccdproc You should also have copied the kms files associated with your masks to the KALIGN sub directory You may find it convenient to open a separate xterm to kosmos for mask alignment only read on and you ll see why Type cd cd KALIGN python kalign py mask kms lt maskimage fits gt lt fieldimage fits gt where mask kms is the file for the mask you are trying to align and the two images are the images taken through the mask and without the mask respectively Since you are in the KALIGN directory you must specify the full path names for the images these will be of the form data2 observer yyyymmdd XXXXXX fits Alternatively you can copy the images to the KALIGN directory but this is generally more time consuming Note that if you have a dedicated xterm for mask alignment you recover and edit the command using the up arrow key and thus don t need to type in the path name every time you run the command The command will open a new ds9 window unfortunately and display the mask image You will be prompted to select alignment boxes on the image you do not need to select all of them for example if one of the alignment stars is saturated you may want to sk
77. tExp INFO GPX STARTEXP 1 READINGOUT 80 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 81 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 82 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 83 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 84 375 nnslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 85 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 86 375 nnslDramaGpxStartExp lt INFO gt GPX STARTEXP 1 READINGOUT 87 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 88 375 rmslDramaGpxStartExp INFO GPX_STARTEXP 1 READINGOUT 89 375 nnslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 90 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 91 375 rmslDramaGpxStartExp INFO GPX_STARTEXP 1 READINGOUT 92 375 rmslDramaGpxStartExp INFO GPX STARTEXP 1 READINGOUT 93 375 rmslDramaGpxStartExp INFO GPX_STARTEXP 1 READINGOUT 94 375 nocsSockRead lt RECV gt asyncMsq OK gpxStartExp Exposure is done expID 2456919 6533779446035624 nnslDrama pxStartExp INFO GPX_STARTEXP 0 0K 95 375 rmslDramaGpxStartExp DONE OK nocsGpxReset lt INFO gt Resetting GPX commands nmslDramaInit DONE OK nocsDramaWgui DONE OK t 1 1 D Thu Sep 18 03 40 52 PM MST 2014 Integration timer 1 0 0 1 4m gwc kpno noao edu 2347 kpno 4m nocs staus Finished script home observer exec CAMSFOCUS sh Status DONE Exposure Vector
78. trograph for the 4 m Mayall telescope that operates from approximately 3500 to 10000 KOSMOS has an approximately 10 arcminute circular field of view at a scale of 0 29 per pixel This same field is available for spectroscopy with multi object slit masks There are presently two VPH grisms hereafter named the Blue VPH grism and the Red VPH Both provide a resolving power of approximately R 2000 with a 1 wide slit The nominal wavelength ranges are 3800 to 6600 for the Blue VPH and 5800 to 9400 for the Red VPH grism although somewhat shifted wavelength coverage is possible with offset slits KOSMOS has an all refractive design see Figure 2 The collimator is f 7 9 and contains five lenses including a doublet The first collimator element is 73mm from the telescope focal surface which provides ample space for the slit wheel The collimated beam diameter is 54mm and the pupil is located 68mm from the vertex of the last collimator element The disperser wheel is coincident with the pupil The total collimated beam space is 170 mm and also includes two tilted filter wheels The camera is f 2 7 and includes 9 lenses in the form of two triplets one doublet and a field flattener The final optical element is the flat window of the CCD Dewar The full field of view has a radius of 5 82 When imaged on a 2048 x 4096 detector with 15 micron pixels the total field of view is approximately 100 square arcminutes Figure 2
79. trument set up http www noao edu cgi bin kpno OrpForm pl http www ctio noao edu forms supportforms visitor support html In specifying the set up consider the following e Your request for CCD must match your proposal once there is a choice of CCD e Filter requests in addition to those specified in your proposal may or may not be accommodated if there is a conflict with another telescope where the filters were requested in the original proposal you will lose out Also since the filter wheels will only handle 5 filters in addition to the standard blocking filters requesting too many filters will create support problems e Make sure you correspond ear y with your assigned staff contact if you are going to observe in multislit mode e NOAO may set a limit on the number of masks it will manufacture without cost to the observer per night for the time being we only ask that people be realistic about how many masks they will plausibly use Other recommendations e Until we have an alternative procedure make sure you bring or have the ability to download the mask design files you create if you are using multislit mode e See recommendations for coordinate caches at the respective telescopes e Download install and practice with NGUI in order to familiarize yourself both with the process of script creation and the variety of observing parameters available to you It is not worth trying to create all the scripts you might use
80. u won t need to change that often The file number is for the firstfile of the pair you observed and must include any leading zeros Then type g The script will bring up the slit image and ask you to identify the place on the slit where you want the object Type k to determine an accurate centroid perpendicular to the slit and then type q to exit you can repeat the centroiding if needed before quitting The position along the slit is determined by the cursor position you may want to zoom the image to position it precisely Now your field will be displayed Put the cursor on the object you want to observe and type a to centroid or type a space to just record the cursor position not recommended use only if you can t centroid your object for some reason Then type q to exit The script will now give you offsets in RA and Dec which you should communicate to the telescope operator The telescope will perform the offset with the guide probe compensating for the motion If the offset is large it may push the guide probe outside its allowable range so it will not move to compensate In this case the operator needs to find another guide star Unless you have done a very small offset it is highly advisable to repeat the acquisition sequence Take the images and re run the koffset1 script as above Note that if you are almost in the correct position and if your object is not too faint it will likely appear through the slit in the s
81. us adjusted according to the parameters specified in the script Focus units are microns and a reasonable step size is 100 microns 50 if seeing is good At the Mayall there is a temperature monitoring widget that recommends focus changes as the telescope truss temperature changes consult with the operator for details Vote there is an option to start the focus sequence at the mid point do not use this as it does not take out focus backlash properly CAMERA SPECTRA FOCUS This focuses the slit on the detector using the camera focus See the calibration section for more details SLIT MOS ACQUISITION This takes an image of the slit or MOS mask looking at sky through an appropriate filter and then another image with the same filter and no slit The offsets to get the target s seen in the sky image on the slit s can then be determined using an appropriate IRAF script see below for slit and MOS acquisition IMAGE This takes an image or images For imaging mode you will normally want to specify less than the full frame 2k x 2k ROI typically This script supports an optional dither mode SPECTRA and II These take a spectrum or spectra using a specified configuration You will normally want to use the full frame unless you are looking only at stars or compact objects in which case the 320 x 4k ROI will save you Page 45 of 100 C KOSMOS Instrument Manual V1 7 some readout time This script also supports an optional dither
82. us script using the narrowest slit you have available If you are just re checking focus use steps of 25 microns and 7 positions centered on or close to your current focus Once you have the images run ccdproc on them Create a list of the images Note that you can just list the images directly within the specfocus task but it s tedious to do and it s easy to make typing errors It s easier to create the list in a file using vi or your favorite text editor Run the specfocus routine in the obsutil package with the list file as the source of the input files Settings epar specfoc as below images list of images if it s a file precede the file name with e g listl gt focus KSCAMFOC slitl lt lower slit edge use a value near the middle like 1000 gt slit2 lt upper slit edge use a value near the middle like 1050 gt Other values should be unchanged from the defaults when in doubt type unlearn specfoc Also if you are using the narrow ROI 320 x 4k use appropriate values for the slit edges like 140 and 180 The output should provide a value for best focus If it is significantly different from the current nominal focus do the following o Goto home logs and open kosmos camera conf for editing note that the file will be named this way for COSMOS also o Change the focus and zero values to the new best focus value and save the file This ensures that if you restart the NOCS the camera will be set to th
83. vd eve vica d 55 5 6 2 Telescope FOCUS sister eb vh ode dde 55 SA ER ETE ET N LUDERE 57 le MI e bau tta d eee LA A 59 DESEA E QUISO vs cc da ca ene uda reel orar d Ed 61 5 10 Magma Acquisito Nessa RE REA UE MR REDI AOL Ico Sa eds Ad amas 63 5 LL ODSETVING rta a E Face wot ta esa e qut dia do n c dct eus 64 p KOSMOS Calibracion RECEN YR GRON n NS CU ESOS an RO ce NN RN RI V B PRO S AR RR A 65 Ge CaliDratlOn Blaise E veo etc t eat E te ud 66 6 1 1 Imaging Calibrations qs oce oci aad ra re 8 eto o pe S PS Qoa S QA RC IER D a A Y Vds 66 6 1 2 Spectroscopic Calibrations ride 66 6 3 Bias Zero MATOS is AI eo vedo n va d AAA e as 67 OA Flat FIelds nace E aaa ln ld a a eee 68 4 4 imaging Flats enere en E EEEE T i ava a re ERE SE 68 QI 1 SpectroSc DIC Flats oiov etie vetere t bct eben ue coole PU Rod 68 6 5 Wavelength Calibration xxiii e ER Eo e e ea GU ae cts aot 70 6 6 Standard GAS ssi slt NS tsa ren mta a aan Ay Rr ced nt PR o nS i PRA ON 70 6 6 1 Imaging Photometric Standards sede ad Fg ee ei ee eias deis 70 6 6 2 Spectrophotometric Staliddal Ss vue e EYE Pin RA EK E EY EXE Y PRA EE e 71 7 Efficient Observing with ROS MOS ia ASS ne e rb e co e 72 Tob General PANNING iris one EY yp fai atone KEEN ERU earl era eu PEEL 72 Tid Step A aO E DIE ON RES OY AO NR IER ON US Laas 72 Appendix A KOSMOS FITS Header sseeeem nennen nnn nnns 75 Appendix B Calibration Lamp Pedi ia a A xr erbe P e ny ade 76 Appendix C Multi Slit Mask Des
84. verhead time at the telescope While a couple of minutes here and there may not look like much if you observe a dozen objects per night including standards and waste a couple of minutes on each one that s potentially one more target you didn t get to observe that night The following suggestions are intended to help minimize this wasted time 7 1 General Planning A few things to keep in mind when planning the night The dome is often the slowest thing involved in a slew this is especially true if a large rotation is involved as may be the case if you are pointing relatively close to the zenith Note that you can get comparison arc spectra while the dome is moving if you have a program that requires them many will not If you are using the instrument rotator to match the slit to the parallactic angle see if you can organize your observations so that you don t have to go to zenith before each observation to set the rotator Small rotations few degrees can be done without going to zenith but on the other hand small rotations won t affect your spectrophotometry anyhow This is a concern primarily for KOSMOS Make sure you ve submitted your coordinates in advance or give them to the OA early to input If you are going to observe with an offset slit e g blue long slit make sure you use that position to zero the telescope pointing If you are using more than one slit position it s most efficient to always start with the slit for whi
85. x is not check but the lamp prompt box is then you will be prompted at the start of any script requiring a lamp including dome flats you will have to use the enter key to proceed During the night you will want to have both boxes selected for any scripts you create but for scripts you are going to run during the afternoon in series you probably want them both unchecked See the flat and spectral calibration descriptions in Section 6 for more details 5 3 4 Nesting Scripts You can create script files that execute a series of scripts This is very useful if you want to set up a series of calibrations in the afternoon that will execute over dinner for example This is less useful for observations during the night see the warning below You could also create a script that observes a series of filters or both red and blue spectra However if the individual scripts take a while to execute you may not find you Page 46 of 100 C KOSMOS Instrument Manual V1 7 save much time by concatenating them To do so in the xterm window in the exec directory create your new script file with a text editor e g vi BigScript sh You can then type in the commands for the scripts you want to execute and then save the file You can also include additional NOCS commands see the calibration section for some examples Then save the script You will need to make the file executable e g chmod a x BigScript sh WARNING Some caution shoul
86. you are trying to get precise radial velocities it may be helpful to take arc spectra before and after observing each object e Flexure can introduce low level effects into flat fields in the red if you are trying to achieve very high signal to noise 2100 you may need to take additional steps Page 65 of 100 C KOSMOS Instrument Manual V1 7 6 1 Calibration Plan Except as noted above the calibration images you need are as follows 6 1 1 Imaging Calibrations For calibrating direct imaging you need e Zero bias images e Flat field images in each filter being used for imaging If you are doing direct imaging only for the purpose of acquisition you can omit the calibrations but unless you are absolutely sure of this you might as well acquire the calibration images Calibration images should be obtained in the same formats ROI region of interest as the science images In addition during the night you will likely want to observe standard star fields 6 1 2 Spectroscopic Calibrations For calibrating spectra you need e Zero bias images e Flat field images for each configuration where you plan to take spectra Thus if you are planning to observe through 5 multi slit masks with both red and blue dispersers you must take a total of 10 flat fields e Arc spectra for each configuration Again during the night you will want to observe spectrophotometric standards Page 66 of 100 C KOSMOS Instrument Manual V1 7 6 3 Bias

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