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paKo. The Observer`s User Interface to the NCS

1. demo rx spectrometers demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP SET ANGLE arcsec 1 SWTOTAL select total power TPHASE 0 5 time per phase data sample CALIBRATE Sol AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start ONOFF 40 0 30 0 offsets of on position NSUBSCANS 12 number of subscans REFERENCE 600 0 0 0 projection offsets of off source reference SYSTEM projection system for offsets SYMMETRIC symmetric subscan sequence TSUBSCAN 30 time per subscan PAUSE ONOFF SWTOTAL OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source In its first form ONOFF is used with TOTAL POWER Subscans are taken alternating between a position that s considered to be ON source and a reference position that s normally assumed to be OFF source 5 NCS USER S GUIDE 72 i e free of emission The source signal is then calculated as the difference between ON and OFF The basic parameters are the offsets for the ON position parameters of the options are the offsets for the reference position the
2. backend BACKEND pause 1 backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 1 backend BACKEND 1 1 pause backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 1 backend 4MHZ 1 4MHZ 2 clear FTS clear FTS FTS FTS FTS FTS FTS FTS FTS ONOOFRWNK clear FTS clear FTS FTS FTS FTS FTS FTS FTS FTS ANoanFWN Ee clear Receiver E090 Horiz LI Receiver E230 Verti LI Fine Fine Fine Fine Fine Fine Fine Fine Fine Default Receiver Receiver Receiver Receiver Receiver Receiver Receiver Receiver Default Receiver Receiver Receiver Receiver Receiver Receiver Receiver Receiver E090 E090 E230 E230 E090 E230 E090 E230 E090 E090 E230 E230 E090 E230 E090 E230 hor ver hor ver ver ver hor hor hor ver hor ver ver ver hor hor LI LI LI LI LO LO LO LO LI LI LI LI LO LO LO LO 63 the first 2 EMIR subbands connect 1 part to E090 Ho LI 2nd part to E230 Ve LI EMIR FTS wide bandwidth mode Fine is NOT present connect 1 part to each selected EMIR subband plus 1 part to each of the 4 outer subbands of E090 short syntax still wide EMIR FTS fine resolution because Fine is present connect 1 part to each selected EMIR subband plus 1 part to each of the
3. Real tCalibrate time 7 4 CATALOG CATALOG SOURCE LINE fileName Select a source or line catalog Character kind SOURCE or LINE Character fileName file name Selects a file with name fileName as source or line catalog Source Catalog The format of a line in the source catalog is the same as that of the parameters of the SOURCE command without the keyword SOURCE and without any options see HELP SOURCE Example W30H EQ 2000 02 27 03 8812 61 52 24 572 LSR 45 0 FLUX 3 73 1 00 IMPORTANT NOTE sourceName is limited to 12 characters 7 PAKO LANGUAGE INTERNAL HELP 109 Line Catalog The format of a line in the line catalog is same as that of the 2nd 3rd and 4th parameter of the RECEIVER command lineName frequency SB with frequency in unit GHz see HELP RECEIVER Example 12C0 1 0 115 271204 UI for EMIR 12C0 2 1 230 537990 LI for EMIR 12C0 2 1 230 537990 LSB for HERA IMPORTANT NOTE lineName is limited to 12 characters NB Don t use amp lt gt in names of sources lines projects PI observer operator etc Don t use in source names 7 4 1 CATALOG SOURCE Source Catalog The format of a line in the source catalog is the same as that of the parameters of the SOURCE command without the keyword SOURCE and without any options see HELP SOURCE Example W30H EQ 2000 02 27 03 8812 61 52 24 572 LSR 45 0 FLUX 3 73 1 00 IMPORTANT NOTE sourceName is li
4. TPHASE 0 5 time per phase data sample CALIBRATE AMBIENT ambient load 5 NCS USER S GUIDE 74 COLD cold load SKY 500 0 400 0 sky at offsets 500 0 400 0 SYSTEM projection system for SKY offset TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start OTFMAP 300 15 300 15 offsets at start and end of first OTF CROLOOP ROR subscans reference OTF reference NOTF 4 number of on the fly subscans REFERENCE 500 400 projection offsets of off source reference STEP 0 10 step shift between OTF subscans SYSTEM projection system for offsets TOTF 120 0 time per on the fly subscan TREFERENCE 20 0 time per off source reference ZIGZAG go back and forth PAUSE OTFMAP SWTOTAL OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source l 11 11 11 11 CROLOOP ROR means that there will be an 1 off source reference subscan R pl before and after each OTF suscan 0 1 Therefore with NOTF 4 on the fly subscans the complete 11 subscan sequence will be 1 R OTF 1 R R OTF 2 R R OTF 3 R R OTF 4 R 11 11 11 1 1I with CROLOOP ROOROOR it would be R OTF 1 OTF 2 R OTF 3 OTF 4 R In OTFMAP on the fly observations the antenna moves relative to the source while recording its positio
5. To use this line catalog enter at the prompt PAKO gt 97 3012085 97 980968 100 076392 102 031906 104 711385 109 782182 110 201370 112 359277 113 490982 115 271204 136 464400 144 617147 145 602952 146 969049 219 560319 220 398686 220 747263 222 166970 224 714370 225 697772 230 537990 241 016176 244 935606 265 886432 267 557625 CATALOG LINE demo EMIR lin HERA c180 2 1 13C0 2 1 CH3CN220 CH3CCH222 c170 2 1 H2C0225 12C0 2 1 C348 5 4 CS 5 4 HCN 3 2 Line Frequency Band 219 560319 220 398686 220 747263 222 166970 224 714370 225 697772 230 537990 241 016176 244 935606 265 886432 LI LI LI LI LI UI UI UI UI UO LI LI LI LI LI LI LI LI LI LI LI LI LI LI LI Id demo lin v 1 1 1 2009 05 08 Hans Ungerechts LSB LSB LSB LSB LSB LSB LSB LSB LSB LSB 29 4 PAKO S COOK BOOK 30 HCO 3 2 267 557625 LSB To use this line catalog enter at the prompt PAKO gt CATALOG LINE demo lin With this command we select the line catalog a special file in which information about the spectral lines is stored Each line contains 3 items the name identifier of the line the frequency in GHz and a code for the side band or EMIR sub band NOTES For the EMIR bands we distinguish up to 4 sub bands each of 4 GHz bandwidth e the lower outer sub band LO from about 12 GHz to 8 GHz frequency shift relative t
6. 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 800 000 000 500 000 200 FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL ONLY FL FL FL FL FL FL Oo0oo0o0oooo O O O TOO O O Ome TO O OO QOTO O OCG OGN O O aO OTOT OO 000 0 0 000 000 0 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 Ooo0oooo OO OR OO OOOO o0o0D0DOOO0O0O0O0O0O0O0O0O0O0O000000000000000000 26 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 4 PAKO S COOK BOOK 27 RLMI EQ 2000 09 45 34 1308 34 30 44 068 LS 3 000 FL 0 000 0 000 RLEO EQ 2000 09 47 33 4669 11 25 44 288 LS 3 000 FL 0 000 0 000 RXBOO EQ 2000 14 24 11 6772 25 42 12 934 LS 1 500 FL 0 000 0 000 UHER EQ 2000 16 25 47 6952 18 53 33 188 LS 16 800 FL 0 000 0
7. SAVE SWITCHING FILE track 2 SAVE TRACK FILE track 2 APPEND Notes IMPORTANT FREQUENCY SWITCHING is very powerful and efficient for some projects e g mapping of narrow spectral lines in cold dark clouds outside the plane of the Milky Way However before deciding to use frequency switching one should consider some potential drawbacks The target lines should be narrow enough so that line signals from the 2 phases of the switching cycle are well separated The spectral baseline will generally be less flat than in other switching modes Some spectral lines are also emitted in the earth s mesosphere e g the mesopheric lines from 12 CO are rather strong and they will be seen in FREQUENCY SWITCHING spectra taken toward astronomical sources with a low Doppler shift The mesospheric lines will appear at a frequency and velocity that corresponds to the rest frame of the athmosphere i e the observatory Care must be taken that they are not confused with the lines from the astronomical source Information computed by the ASTRO software can help with this decision When observing sources near the plane of the Milky Way line emission from clouds at other velocities than the target source e g other spiral arms can cause confusion In case of doubt consult the special memo on FREQUENCY SWITCHING or ask an experienced FRE QUENCY SWITCHING observer 4 3 9 ON OFF Position Switching and Wobbler Switching Id demo onoff pa
8. to be that of the project account Submission from other projects will not be accepted by the NCS enter at the prompt PAKO gt SET doSubmit yes to activate submission of observing commands to the NCS observing queue SET doSubmit no is useful for debugging so that scripts including START can excute without actually trying to submit observations To start any observation in the NCS enter at the prompt PAKO gt START which actually generates an XML file with a full and detailed specification of all subscans that will be excuted by the NCS coordinator software This is done by the scanAnalyzer which is an integral part of the pako software If you are looking for an adventure you are encouraged to explore these XML files e g using a recent version of Mozilla the XML editor oxygen or emacs Several instances of pako should not be run in the same working directory of the same project account Also at most one instance of pako should try to send observations to the observation queue 2 PAKO GUIDE OF THE PERPLEXED 13 2 8 Source and Line Catalogs The format of the source catalog e g iram sou is similar to source catalogs at PdB A source catalog for the NCS can be generated from standard old 30m catalogs cat using ASTRO The example source catalog demo sou was generated from a historic version of IRAM CAT using ASTRO The format of the line catalog e g model lin is as in the old control
9. 073 359 054 837 271 985 525 110 LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR yet support pointing on Si0 masers 02 02 03 05 05 05 09 09 14 16 18 19 19 19 19 20 21 CATALOG SOURCE demo sou 19 22 53 11 35 55 45 47 24 25 08 06 15 50 57 46 09 20 bl 28 19 14 49 34 33 tdi 247 04 222 223 233 36 20 32 7066 7287 8025 7492 4740 2761 1308 4669 6772 6952 0790 2515 3656 8831 7728 5768 3331 02 58 11 52 05 20 34 11 25 18 22 08 07 32 01 40 68 58 35 24 52 22 10 30 25 42 53 13 13 02 36 095 713 689 30 12 20 27 30 12 25 51 59 28 165 157 768 44 44 934 33 313 49 49 54 53 06 29 068 288 188 187 766 226 04 381 440 855 LS LS LS LS LS LS LS LS LS LS LS LS LS LS LS LS LS OO OO OO OO OO OO OOO OOO Ome 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 800 000 000 500 000 200 000 3 000 500 800 500 000 500 300 800 100 800 FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL ONLY FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL oe E e
10. 700 all in system radio projection OTFMAP 300 300 300 300 REFERENCE 600 700 projection SYSTEM projection 7 For special purposes it is possible to overrule this with swWobbler no e g ONOFF 44 swWobbler no 6 NCS EXPLAINED 83 Example ii Observe an OTF map with first OTF subscan from offsets 300 300 to 300 300 in system trueHorizon and no off source reference This is typical for bolometer OTF maps OTFMAP 300 300 300 300 REFERENCE no SYSTEM trueHorizon NOTES Visiting observers have also used ONOFF in trueHorizon combined with OFFSETS SYS TEM projection with TOTAL POWER apparently with success NOTES e one should not specify offsets for the same system with the observing mode and OFFSETS and there is not need to do this If the observing mode uses SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode uses SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used e in the commands for the observing modes the offsets for off source reference positions must be in the same system as those of the on source or OTF positions i e REFERENCE and SYSTEM must select the same system normally PROJECTION Details at a technical level about these and more offsets can be found in the documentation of NCS Antennna Mount Drive by Alain Perrigouard NOTES More explanations about coordinate systems projections an
11. History of this Document 1 2 10 11 12 13 14 15 v 0 HU v 1 0 0 2005 12 16 HU v 1 0 1 2005 12 22 HU v 1 0 2 2006 01 22 HU v 1 0 4 2006 08 07 HU v 1 0 6 3 2007 02 22 HU v 1 0 7 2007 06 28 HU v 1 0 9 2007 10 24 HU v 1 1 1 2009 05 12 HU v 1 1 4 2010 12 01 HU v 1 1 5 2011 04 25 BBC HU v 1 1 6 2011 07 31 FTS 32GHz HU v 1 1 11 2011 11 11 EMIR E230 E330 upgrade HU v 1 1 12 2012 04 01 GISMO Lissajous HU v 1 1 14 2012 12 01 NIKA E150 switch box HU Pending Items 2006 08 07 TBD v1 2 WE PRODUCED THIS DOCUMENT USING PDF ETRX WITH THE STANDARD PACKAGE HYPERREF AND OUR OWN PROTOTYPE PACKAGE NCS HU CONTENTS Contents 1 paKo Introduction and Overview 2 1 La 2 3 2A 2 5 2 6 21 2 8 29 2 10 2 11 2 12 2 13 2 14 2 15 2 16 2 17 2 18 2 19 2 20 2 21 2 22 2 paKo Guide of the Perplexed PARO AMO SIO c s en s ca ERG A RA RR a PARO and lame 2 aes saaa Lae BOR RG aa e Ree a Running PAKO offline and several instances of PAKO 2 2 ee ee Help 24546 Bae eee FOG 4 GE a a EER ERA Re Ee ee eS SET LEVEL for Errors Warnings and Infos 2 4 Saving and Restoring 0 22 45 2256 5 dowa os ae sa ws Observation Queues and Starting 2 00000 eee eee Source and Line Catalogs o o ca a d oa a RP ae Switches Modes o cate Gan wok ae a A ee Cibservas Modes e a ro ete gus BR epa m poe Te aoea kai ee ee ee i Combinations of Switching and Obser
12. IMPORTANT NOTE ON VELOCITY One should not use very large Doppler velocities thousands of kilometers to achieve red shift corrections of frequencies Instead one should enter the red shifted frequencies in the line catalog or with the RECEIVER command and use Doppler velocity of 0 0 The alternative approach with very large Doppler velocities needs special methods and attention in the data processing which are not implemented in CLASS because it is better to observe in such a way that minimum modification to the data is done later on J Pety For a full discussion of this question see Gordon et al 1992 A amp A 7 PAKO LANGUAGE INTERNAL HELP 178 264 337 in Sect 6 7 27 40 OPTIONS VERTICAL VERTICAL sb1 sb2 VERTICAL n one EMIR subbands for Vertical polarization This option applies only to EMIR Character sbi sb2 for EMIR LO LI UI UO This option selects which EMIR subband s of this polarization will be transmitted through IF cables 1 to 4 Note that some backends NBC 4MHz WILMA VESPA can only be connected to IF cables 1 to 4 i e only to the EMIR subbands selected with the RECEIVER command For each EMIR band and polarization at most 2 subbands can be transmitted through IF cables 1 to 4 Which combinations of EMIR bands polarizations and subbands are possibble is determined by the hardware of the EMIR IF switching box See the EMIR documentation for details If no subband is explicitl
13. PAUSE ONOFF SWWOBBLER OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source IMPORTANT NOTE ONOFF with SWWOBBLER wobbler switching on off requires that the subscans are offset relative to the source in the trueHorizon system by 1 the Wobbler elongations offsets With the commands above paKo recognizes this and automatically sets the correct values In this case OFFSETS can be used to set additional mapping offsets in the projection of the astronomical coordinate system These mapping offsets in the projection apply to all ONOFF subscans When ONOFF is used with WOBBLER SWITCHING command SWWOBBLER the position offsets must be set to very specific values in TRUE ANGLE HORIZON depending on the parameters of SWWOBBLER This is achieved by using the special option SWWOBBLER of the command ONOFF Subscans are then taken alternating between 2 positions in such a way that a in some subscans one position of the antenna the source is in the first of the two Wobbler phases b in the other subscans the other position of the antenna the source is in the second of the two Wobbler phases During the data processing the source signal is computed as a double difference 1st the difference of the 2 Wobbler phases 2nd the difference between ONOFF subscans a and 6 This form of ONOFF is also called Wobbler Onoff or sometimes simpl
14. Project 111 22 I SHOW PI Dr Jane D Doe I SHOW Observer John Doe I SHOW Operator Pako I SHOW Topology LOW I SHOW Pointing azimuthCorrection 0 0000000E 00 I SHOW Pointing elevationCorrection 0 0000000E 00 0 I SHOW Focus focusCorrection 0 0000000E 00 PAKO gt Figure 1 Screen shot of PAKO runing in a terminal window 2 paKo Guide of the Perplexed 2 1 paKo and SIC PAKO uses the usual SIC command line interpretor and can be run in any X windows terminal see Figure 1 It includes the GREG and GUI languages for plotting and of course adding GUI widgets 2 2 paKo and Linux PAKO and the NCS run on Linux Any files that are prepared off line e g command scripts and source or line catalogs should follow Linux standards Files prepared on other operating systems may contain non compliant control characters 2 3 Running paKo offline and several instances of paKo PAKO can run independently of the NCS This is useful e g to prepare command scripts and source or line catalogs Several instances of pako should not be run in the same working directory of the same project account Also at most one instance of pako should try to send observations to the observation queue other instances should SET DOSUBMIT NO see below 2 4 Help There is help available e g enter at the prompt PAKO gt HELP CALIBRATE 2 PAKO GUIDE OF THE PERPLEXED 11 The display for most commands correspon
15. Set minimal level for paKo messages to be written 1 interactively to the standard output i e the terminal window 2 to the message log file pako mes All paKo messages have an associated severity number With SET LEVEL we can select that only messages with severity higher than minimalForStandard0ut minimalForFile are written Very serious messages with severity 9 and higher can NOT be turned off The severity number for messages of kind I is 1 or 2 Informational message W is 3 or 4 Warning message E is 5 or 6 Error message F is 7 or higher Fatal Error message Example SET LEVEL 5 3 Has the effect that I messages are not shown at all and only E and F messages are shown in the terminal window 7 PAKO LANGUAGE INTERNAL HELP 145 7 15 4 SET POINTING SET POINTING azimuthCorrection elevationCorrection Real azimuthCorrection arc sec Real elevationCorrection arc sec Set pointing corrections in units of arc sec in place of a number leave the value unchanged Example SET POINTING 1 1 2 2 7 15 5 SET 2NDROTATION SET 2ndRotation rotation Real rotation rotation angle deg Set rotation angle for the secondary mirror and Wobbler mechanism deg The angle is limited to be between 50 and 50 deg NOTE Its sense is opposite to the mathematical convention this will be changed in a future release of the NCS The rotation angle is relative to the horizontal system A value of 0
16. if the receiver is tuned to the Si0 line EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 NOTE NCS does not OCET SPER NMLTAU IRC 50137 ORIA UORI RLMI RLEO RXBOO UHER VXSGR RAQL WAQL XCYG RRAQL NMLCYG TCEP To use this source catalog enter at the prompt PAKO gt EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 21 21 21 21 21 21 21 15 23 31 34 36 39 48 22 22 22 22 22 22 22 22 22 22 22 23 23 02 03 13 18 25 32 36 20 229 44 235 10 238 201 4509 43 14 02 52 47 36 22 46 53 56 58 13 05 3850 4941 2540 3053 5791 3021 2793 9665 4963 0315 2570 4015 4627 18 57 17 05 45 44 2309 7438 9320 9656 3867 8503 29 05 12 01 00 14 06 42 31 25 03 04 11 28 12 16 62 27 61 05 233 235 07 53 241 23 57 16 245 29 35 57 243 28 06 08 49 01 58 28 13 38 38 40 38 30 36 01 50 57 51 648 545 312 316 085 53 21 10 50 540 22 04 17 54 36 192 725 163 319 108 710
17. xOffsetR x offset Real yOffsetR y offset Character systemNameRef name of system see SYSTEM for choices NOTE with the usage REFERENCE xOffsetR yOffsetR both parameters are requi but you can replace either parameter with to leave it unchanged 7 10 4 ONOFF SWWOBBLER SWWOBBLER yes no 7 PAKO LANGUAGE INTERNAL HELP 121 option of command ONOFF set parameters appropriate for on off Wobbler switching Logical doSwWobbler If switching mode SWWOBBLER has been selected the following parameters of ONOFF are set according to wOffseti and wOffset2 ONOFF xOffset is set to w0ffset1 yOffset is set to 0 0 REFERENCE is set to Yes xOffsetR is set to wOffset2 yOffsetR is set to 0 0 systemNameRef is set to TRUEHORIZON SYSTEM systemName is set to TRUEHORIZON NOTE in this case the values selected by SWWOBBLER overrule the corresponding values specified directly in the command NOTE To do ONOFF with Wobbler switching and other unconventional values for the parameters listed above simply specify the values using command ONOFF with option SWWOBBLER NO not recommended NOTE If the selected switching mode is SWWOBBLER and if the option SWWOBBLER is no explicitly given it will be assumed to be True Yes If the selected switching mode is not SWWOBBLER and if the option SWWOBBLER is no explicitly given it will be assumed to be False No 7 10 5 ONOFF SYMMETRIC SYMMETRIC yes no
18. 14 4701 2431 1540 0022 9336 7464 9795 2682 7959 8226 4231 0894 3565 1634 8003 9268 8992 4348 9895 7409 6922 9611 0222 1010 1082 3910 0300 1316 6602 6704 5274 0034 2441 3546 2094 3819 8748 0102 3341 8762 2617 0622 0817 1009 6375 6157 5968 2988 3922 2966 8339 6892 6971 7983 47 41 32 01 50 13 38 01 00 37 05 36 23 01 16 36 13 07 48 34 42 51 44 20 41 42 37 00 56 50 51 22 52 09 16 53 06 02 39 15 33 01 34 54 243 09 33 34 57 58 14 245 03 47 39 08 15 44 30 71 11 17 01 24 09 49 07 42 55 03 20 70 20 39 40 25 65 23 29 80 71 19 01 12 18 39 29 es 02 25 16 30 18 46 57 08 01 20 36 56 2d 06 24 59 03 2k 31 32 31 16 28 35 50 35 08 19 15 52 52 13 07 31 55 43 49 49 40 16 19 36 12 18 23 36 10 45 42 59 41 30 20 15 54 16 02 39 35 35 58 41 17 43 08 49 387 42 762 755 230 14 574 33 702 460 549 668 367 756 614 373 160 345 124 173 314 125 988 476 585 569 392 692 980 04 580 988 34 658 481 051 337 585 24 530 760 572 692 44
19. 7 2 3 BACKEND DEFAULTS DEFAULTS yes no Set default values If EMIR sub bands have been selected with the RECEIVER command this option has a special function for some Backends BACKEND BBC Defaults connects one BBC part to each sideband of each selected EMIR band up to 8 BACKEND NBC Defaults connects one NBC part to each selected EMIR sub band up to 4 BACKEND 4MHZ Defaults connects one 4MHz part to each of the ist and 2nd selected EMIR sub band BACKEND WILMA Defaults connects one WILMA part to each selected EMIR sub band up to 4 BACKEND FTS Defaults connects one FTS part in wide bandwidth to each EMIR sub band up to 4 selected for IF cables 1 to 4 and additionally one part to each of the available Outer subbands up to 4 on IF cables 5 to 8 BACKEND FTS Fine Defaults connects one FTS part in fine resolution to each EMIR sub band up to 4 selected for IF cables 1 to 4 and additionally one part to each of the available Outer subbands up to 4 on IF cables 5 to 8 7 2 4 BACKEND CLEAR CLEAR yes no Completely clear a list of connected hardware e g receivers backends or parameters of the associated command After changing the receiver configuration BACKEND CLEAR is recommended followed by the backend setup for the new receivers without that it is 7 PAKO LANGUAGE INTERNAL HELP 100 possible that pako will not accept BACKEND commands because of unresolved conflicts between the
20. E230 E230 E090 E230 E090 E230 hor ver hor ver ver ver hor hor LI LI LI LI LO LO LO LO 33 clear all backend setups EMIR BBC connect 1 part to both polarizations of each sideband of each selected EMIR band EMIR NBC connect 1 part to each selected EMIR subband EMIR WILMA connect 1 part to each selected EMIR subband EMIR 4MHz NOTE 4MHz has only 2 parts with EMIR connect 1 part to each of the first 2 EMIR subbands connect 1 part to E090 Ho LI 2nd part to E230 Ve LI EMIR FTS wide bandwidth mode Fine is NOT present connect 1 part to each selected EMIR subband plus 1 part to each of the 4 outer subbands of E090 short syntax still wide 4 PAKO S COOK BOOK pause backend BACKEND pause 1 backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 1 1 backend BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND say pause 11 EMIR backend BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 34 EMIR FTS fine resolution because Fine is present clear FTS Fine Default connect 1 part to each selected EMIR subband plus 1 part to each of the 4 outer subbands of E090 clear short syntax fine FTS 1 Fine Receiver E090 hor LI FTS 2 Fine Receiver E090 ver LI FTS 3 Fine Receiver E230 hor LI FTS 4 Fine Receiver E230 ver LI FTS 5
21. EMIR subband to connect to backend part Character sideband EMIR sideband to connect to backend part Choices for receiverBand are compare RECEIVER command E090 E150 E230 E330 HERA1 HERA2 Choices for polarization are for EMIR compare RECEIVER command Horizontal Vertical Choices for subband sideband when observing with EMIR are LO LI UI UO LSB USB LSB and USB apply only to EMIR bands with 8 GHz bandwidth E090 E230 and E330 and Backend BBC 7 2 12 BACKEND EXAMPLES Id demo backend pako basic BACKEND EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts swTotal default select a switching mode compatible with all backends one example of a complex EMIR setup pako RECEIVER pako RECEIVER clear RECEIVER E090 CS 2 1 97 980965 LI horizontal LI vertical LI RECEIVER E230 CO 2 1 230 537994 LI horizontal LI vertical LI l BACKEND CLEAR clear all backend setups EMIR BBC BACKEND BBC Default connect 1 part to both polarizations 7 PAKO LANGUAGE INTERNAL HELP backend BACKEND pause backend BACKEND backend BACKEND pause BACKEND BACKEND pause 1 backend BACKEND 1 1 pause backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 1 backend clear NBC clear WILMA clear 4MHz 4MHZ 1 4MHZ 2 clear FTS clear FTS FTS FTS FTS FTS FT
22. Figure 3 The range of mapping offsets for these plots can be set with the usual GREG command limits e g enter at the prompt PAKO gt 3 For special purposes it is possible to overrule this with swWobbler no e g ONOFF 44 swWobbler no 2 PAKO GUIDE OF THE PERPLEXED XxX paKo name system longitude latitude velocity SOURCE W30H eq J2000 0 02 27 03 881 61 52 24 57 LSR 0 000 h 2 451078 low SETNS6SGbMIE NO F deg 36 766172 61 873492 0 0 0 0 rad 0 64169075 1 07989616 0 00 mm A iram J2000 LSR sou CATALOGIEINE model lin lineName frequency GHz SB doppler width gain dB tempLoad efficiency scale E090 12C0 1 0 115 271204 UO Doppler 0 050 13 L L 0 95 0 75 antenna Horizontal UO Wertical UI E230 12C0 2 1 230 537990 LI Doppler 0 050 13 L L 0 91 0 52 antenna Horizontal LI Nertical LI OTFMAP On The Fly OTF Map arcsec BMEREGUENCY Frequency Switching xStart yStart 300 000 300 000 fOffset1 fOffset2 MHz xEnd yEnd 300 000 300 000 3 900 3 900 receiver E090 gt length0tf 600 000 11 700 11 700 receiver E230 system projection reference F tPhase 0 100 xOffsetR yOffsetR 600 000 0 000 systemNameRef 0 000 croLoop notf 12 BACKEND nPart resolu bandw fShift receiver mod perc lineName step dx dy 0 000 10 000 4mMHz 1 4 000 4024 0 248 0 E090 hor UO speed sStart sEnd 5 000 5 000 4MHz 2 4 000 4024 0 248 0 E090 ver UI FtOtf 120 000 WILMA 1 2 000 3720 0 265 0 E090 hor UO 100 0 tReferen
23. HORIZONTAL 170 MODE 171 NOTF 171 NSUBSCANS 171 PERCENTAGE 171 RECEIVER 172 REFERENCE 172 SCALE 172 SKY 172 SPEED 173 STEP 173 SWWOBBLER 173 SYMMETRIC 174 SYSTEM 174 TCALIBRATE 175 TEMPLOAD 176 TOTF 175 TPHASE 176 TREFERENCE 176 TSUBSCAN 176 VELOCITY 177 VERTICAL 178 WIDTH 178 181 INDEX ZIGZAG 179 OTFMAP 125 CROLOOP 127 DEFAULTS 127 NOTF 127 REFERENCE 128 SPEED 128 STEP 128 SYSTEM 128 TOTF 129 TREFERENCE 130 ZIGZAG 130 EXAMPLES 130 POINTING 132 DEFAULTS 132 DOUBLEBEAM 132 NOTF 133 TOTF 133 EXAMPLES 133 RECEIVER 134 CLEAR 136 CONNECT 136 DEFAULTS 136 DEROTATOR 136 DISCONNECT 136 DOPPLER 137 EFFICIENCY 137 GAINIMAGE 137 HORIZONTAL 137 SCALE 138 TEMPLOAD 138 VERTICAL 139 WIDTH 139 EXAMPLES 140 SAVE 141 APPEND 142 FILE 142 EXAMPLES 142 SET 143 2NDROTATION 145 DOSUBMIT 144 EMIRCHECK 146 EXAMPLES 147 FOCUS 144 LEVEL 144 LIMITCHECK 146 POINTING 145 TOPOLOGY 145 USERLEVEL 147 SHOW 148 SOURCE 148 CATALOG 151 GREP 151 VELOCITY 151 EXAMPLES 152 START 153 SUBSCAN 153 CROFLAG 155 RAMP 155 SYSTEM 156 TOTF 156 TSUBSCAN 157 TUNE 157 TYPE 157 SWBEAM 157 SWFREQUENCY 158 DEFAULTS 159 RECEIVER 159 TPHASE 159 EXAMPLES 159 SWTOTAL 160 DEFAULTS 160 TPHASE 160 SWWOBBLER 160 DEFAULTS 161 TPHASE 161 TIP
24. Integer nOtf number of OTF on the fly subscans 7 27 22 OPTIONS NSUBSCANS NSUBSCANS nSubscans Integer nSubscans number of subscans 7 27 23 OPTIONS PERCENTAGE PERCENTAGE percentage Real percentage percentage of bandwidth to use This is a special option for the autocorrelators VESPA and WILMA For autocorrelators normally some channels at both ends of the band are blanked because they do not contain usable data and only the central percentage of the theoretical bandwidth is used typically about 90 Reasonable conservative defaults are automatically applied in general 90 but 82 for VESPA with bandwidth 640 This option allows the observer to adjust the percentage for special purposes 7 PAKO LANGUAGE INTERNAL HELP 172 For WILMA connected to EMIR the useful bandwidth is 3720 MHz and counted as 100 See VESPA user s guide for details 7 27 24 OPTIONS RECEIVER RECEIVER receiverBand Character receiverBand receiver EMIR band Choices for receiverBand are E090 E150 E230 E330 HERA1 HERA2 7 27 25 OPTIONS REFERENCE REFERENCE xOffsetR yOffsetR systemNameRef or REFERENCE NO no reference position of off source reference subscans Real xOffsetR x offset Real yOffsetR y offset Character systemNameRef name of system see SYSTEM for choices NOTE with the usage REFERENCE xOffsetR yOffsetR both parameters are requi but you can replace either paramete
25. Logical doSymmetric default no For ONOFF select a subscan sequence that is symmetric in time This requires that the number of subscans is a multiple of 4 Example for ONOFF with SYMMETRIC no SYMMETRIC yes 1st subscan OFF OFF 2nd ON ON 3rd OFF ON 4th ON OFF and so on NOTE that this does not in anyway change the positions of the ON source and OFF source subscans 7 PAKO LANGUAGE INTERNAL HELP 122 7 10 6 ONOFF SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM pr
26. NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 7 PAKO LANGUAGE INTERNAL HELP 117 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yO
27. NCS Explained subsection Switching Modes 5 4 3 POINTING Id demo bolometer pointing pako v 0 2 2005 07 14 by Hans Ungerechts RECEIVER BOLOMETER SWWOBBLER 22 22 TPHASE 0 5 select Wobbler switching 5 NCS USER S GUIDE 77 SET ANGLEUNIT arcsec make sure angle unit is arc sec POINTING 60 pointing with subscan length 60 CALIBRATE no no calibration NOTF 4 4 OTF subscans TOTF 15 0 15 seconds per OTF subscan PAUSE POINTING OK to start c q a chance to check START start RETURN To execute this script simply enter demo bolometer pointing POINTING observations are done to optimize the positioning of the telescope in Azimuth and Elevation This is normally done by continuum observations of a cross scan in azimuth and elevation on a point source or at least a small source near the intended target source It is normally used with BEAM SWITCHING or WOBBLER SWITCHING it is also possible with TOTAL POWER With the bolometer POINTING is done with WOBBLER SWITCHING A calibration is not needed for POINTING if one is only interested in the pointing corrections and not in the source intensity After a pointing the data processing software displays the results and you can enter a correction for the observed pointing offsets with the command SET POINTING azimuthCorrection elevationCorrection Note that this is the total correction i e the previous correction plus the additiona
28. SYSTEM setae pa g EE roem D se Pee ee ee dg 156 7194 SUBSCAN JEOTE a a4 dg pa A Se he A Se BS 156 7194 SUBSCAN TSUBSCAN sose 2 oe sor ag i n aa og dee A a os 157 1 198 SUBSCAN TUNE osea e aa ae ia Berek 157 7 19 7 SUBSCAN TYPE e ee bee s a E pa aa h A 157 SWBBEAM o seneg nme p canpa e g eaa ie Da ka ERE A ee aa ES 157 SWHRREQUENOY pas weage neia d a OR eR RE RR EEO 158 721 1 SWFREQUENCY DEFAULTS 6 ect aX eee aw meee ew REE BA 159 fale SWEREQUENCY RECEIVER ses es toce ca sie 852454 545 159 Tala SWFREQUENCY TPHASE 2025248844544 44424 488 e285 159 7 214 SWFREQUENCY EXAMPLES 159 SWTOTAL cosita e 160 7 22 1 SWTOTAL DEFAULTS gt cs2e5 Bb aoa nr e wee 160 7 22 23 SWTOTAL TPHA E lt ooe cepen nb oR Ree eee ete 160 SWWOBBLER lt s osaig a a E ein a ka Be ooh ee e 160 T231 SWWOBBLER DEFAULTS osa A E a 161 asa SWWOBBLER TPHASE 6822 4548604 eee he ee Oe TA es 161 UP pete E 162 A este t eae heh OE ee ee Ree oe ee he 162 T242 TIP AIRMASS oc oir ee a AA ee Reg ewe OS 162 AS TIP TSUBSCAN co eee gia A A Se ee ee ee aw OE 162 PEALE AA EE 163 Vo TRACK DEFAULTS ee po bbs ad Ra E A 163 1282 TRACE JOYSTEM lt o erised Ade ee rr era A 163 1223 TRACK NSUBSCANS e ee ce mg teda Ree a 164 dl FRACR I TSUBSCAN ce tene ari a oe Se Ge EH RY 164 CONTENTS 8 Pand TRACK EXAMPLES 2 0 ee Poe ek Swe A ek o ee ee PO ee 164 Wee NEED atar eed cee Ke eee eee see ec a ee ee a we ee we 165 Veet OPTION eaaa
29. Wobbler Switching 2 26 0286645 ces ee ee oe ee es The Fly Mapping with Wobbler Switching 6 1 Coordinate Systems Map Projections and Position Offsets 62 Anmuth Topology lt oe Sk wk e eR ee ee el Re we ie eg we pi 6 3 Switching Modes Gal BEAM SWITCHING lata Sts a ee doe eo 6 3 2 FREQUENCY SWITCHING 2245 cas ma eR Pe ae 6 3 3 WOBBLER SWITCHING sos 2 5 sae Bed BOS Se Ae eG Sw AE we Ss 6 3 4 Toral P OWER e A a a ai T AE ie A ho ARA ee es 64 iserving Modes s a sr sa racs s gaea ee da ERE SA ee G 64 1 CALIBRATE o iceren recrea o ap a e e a BAD POINTING cs s seaga s fead Pa a a a Bo 6 4 3 FOCUS 6 4 4 TIP 6 4 5 ONOFF 646 OTFMAP 22 666 po ds e eana i a 6 4 7 RASTER 6 4 8 TRACK 6 4 9 VLBI 6 5 Receivers 6 6 Backends 46 46 AT 53 53 55 62 67 67 68 69 71 73 76 76 76 76 76 77 78 78 79 CONTENTS 5 7 PAKO Language Internal Help 90 Val LAMAS Bao a el il A BO ek A a Bet Bh Ae 91 TLL Language NEWS cia a A e A A a aS 92 7 1 2 Language HELP dce sc rara ee ee ae 94 72 BACKEND lt cas 508 he eo Fa Re eee oe ak Aw ade Re ew as 95 LaL BACKEND BBG eco 4 ee aba Sw oe ao OE a a 97 G22 BACKEND FITS se 22442 22 eee Sea W Ae e ee hel ew wo 97 20 BACKEND DEBATLTS gt socios ERLE BE RR EE OR 99 128 BACKEND CLEAN lt gt racer Ghee dees eee eae 99 125 BACKEND CONNECT isos Pe ke RH RA me wR ES 100 7126 BACKEND DISCONNECT o 62d 4 eRe Be eR e
30. resolution MHz bandwidth MHz frequency shift MHz receiver band EMIR polarization and EMIR sub band The receiver band and subbands must have been previously selected with RECEIVER For some backends the resolution bandwidth and or frequency shift are fixed and a shorter syntax is possible See the HELP BACKEND for complete information CLEAR completely clears the backend setup Normally the continuum backends are used only for POINTING FOCUS and TIP antenna tipping or skydip For VESPA only a selected few possibilites are shown for more information see the VESPA user s guide After you enter a backend setup manually we recommend to save it optionally to a named file SAVE BACKEND FILE backend 1 It can then at any later time be reloaded with backend 1 see HELP SAVE 5 NCS USER S GUIDE 67 5 3 4 CALIBRATE Id demo calibrate pako CALIBRATE EXAMPLE v 1 1 5 2011 04 25 Hans Ungerechts CALIBRATE AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for sky offset TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start Comments we assume here that source receivers and backends already have been selected and setup see demo source demo receiver demo backend NOTE this is a generic calibrate for any heterodyne
31. total number of subscans and the time per subscan in s After you enter an ON OFF setup manually we recommend to save it optionally to a named file SAVE ONOFF FILE onoff 1 It can then at any later time be reloaded with onoff 1 see HELP SAVE You may want to save the switching mode seperately or with ONOFF into the same file SAVE SWITCHING FILE onoff 2 SAVE ONOFF FILE onoff 2 APPEND SYMMETRIC selects a subscan sequence that is symmetric in time for details see HELP ONOFF SYMMETRIC This requires that the number of subscans is a multiple of 4 This form of ONOFF is also called Position Switching but it should be noted that the switching here is realized by a sequence of subscans at different positions i e in a way completely different from switching in the sense of BEAM SWITCHING WOBBLER SWITCHING and FREQUENCY SWITCHING Id demo onoff swwobbler pako ONOFF SWWOBBLER EXAMPLE v 1 1 6 2011 07 31 Hans Ungerechts WOBBLER SWITCHING demo rx spectrometers demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP SET ANGLE arcsec select wobbler switching SWWOBBLER 120 0 120 0 wobbler 120 arc sec TPHASE 1 0 1 seconds per phase CALIBRATE AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration
32. 10 and 20 in system radio projection typically used with FREQUENCY SWITCHING TRACK 10 20 SYSTEM projection Example 2 Observe ONOFF position switching with TOTAL POWER with ON position at 30 40 and off source reference at 600 700 both in system radio projection ONOFF 30 40 REFERENCE 600 700 projection SYSTEM projection Example 3 Pointing with subscans of length 120 POINTING 120 NoTEs For POINTING the OTF offsets are always in system trueHorizon and are specified implicitly though the angular length of the subscans Example 4 ONOFF observations with WOBBLER SWITCHING are a special case because the offsets for the subscans must be in system trueHorizon and their values must be selected according to the offsets of the WOBBLER SWITCHING E g SWWOBBLER 33 33 ONOFF 33 O REFERENCE 33 0 trueHorizon SYSTEM trueHorizon This can also be achieved simply by saying SWWOBBLER 33 ONOFF PAKO knows the special requirements for onoff wobbler switching and will set the offset parameters for ONOFF accordingly if SWWOBBLER has been previously selected 7 In this special case in order to map the source the observer may add offsets on the source and b using the command OFFSETS with the system projection e g SWWOBBLER 33 OFFSETS 110 120 SYSTEM projection ONOFF Example i Observe an OTF map with first OTF subscan from offsets 300 300 to 300 300 and off source reference at 600
33. 50 41 3193 09 29 05 122 LSR 0 000 FL 0 000 0 000 0106 013 EQ 2000 01 08 38 7684 01 35 00 421 LSR 0 000 FL 0 000 0 000 0112 017 EQ 2000 01 15 17 0917 01 27 04 456 LSR 0 000 FL 0 000 0 000 0113 118 EQ 2000 01 16 12 5176 11 36 15 412 LSR 0 000 FL 0 000 0 000 0119 041 EQ 2000 01 21 56 8557 04 22 24 842 LSR 0 000 FL 0 000 0 000 0133 476 EQ 2000 01 36 58 5910 47 51 29 164 LSR 0 000 FL 0 000 0 000 0135 247 EQ 2000 01 37 38 3418 24 30 53 698 LSR 0 000 FL 0 000 0 000 0202 149 EQ 2000 02 04 50 4141 15 14 11 214 LSR 0 000 FL 0 000 0 000 0212 735 EQ 2000 02 17 30 7735 73 49 32 845 LSR 0 000 FL 0 000 0 000 0221 067 EQ 2000 02 24 28 4237 06 59 23 499 LSR 0 000 FL 0 000 0 000 W30H EQ 2000 02 27 03 8812 61 52 24 572 LSR 0 000 FL 0 000 0 000 0224 671 EQ 2000 02 28 50 0655 67 21 03 123 LSR 0 000 FL 0 000 0 000 0234 285 EQ 2000 02 37 52 3845 28 48 09 782 LSR 0 000 FL 0 000 0 000 0235 164 EQ 2000 02 38 38 9268 16 36 59 287 LSR 0 000 FL 0 000 0 000 0239 108 EQ 2000 02 42 29 1773 11 01 00 856 LSR 0 000 FL 0 000 0 000 5 NCS USER S GUIDE 0300 471 0316 413 0333 321 0336 019 0355 508 0403 132 0415 379 0420 014 0422 004 0426 380 0430 052 0439 360 0454 234 0458 020 0514 161 0521 365 0528 134 0529 075 0552 398 0605 085 0607 157 0642 449 0646 306 0716 714 0727 115 0735 178 0736 017 0745 241 0754 100 0804 499 0805 078 0814 425 0820 560 0823 033 0834 201 0836 710 0851 202 0923 392 0945 408 0953 254 0954 658 1012 232 1034 293
34. 77 37 31 33 51 03 42 247 20 38 57 19 20 23 29 52 05 22 37 27 29 12 51 08 20 46 48 56 41 10 36 04 57 243 04 591 700 473 849 04 089 484 496 049 034 11 50 00 39 04 04 28 49 51 44 03 09 06 14 06 58 31 44 48 32 48 52 10 53 43 19 41 14 29 21 43 59 07 23 39 30 59 19 01 10 07 47 26 23 45 36 39 26 51 38 49 51 28 00 01 21 28 01 46 40 25 54 838 26 29 01 48 02 547 518 622 294 640 395 265 687 381 10 57 43 43 59 02 00 12 31 695 621 257 24 868 251 601 14 080 238 845 431 069 400 666 TOT 770 04 874 979 958 698 852 478 684 502 398 410 616 423 604 022 989 106 592 585 101 183 LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR oo UDOOO0O0O0O0O0O0O0O0O0O0O0000000000000000000000000000000000000o00o00o00o 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 00
35. 901 408 446 666 454 914 319 788 965 860 549 712 34 608 583 453 292 085 LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR oo UDOOO0O0O0O0O0O0O0O0O0O0O0000000000000000000000000000000000000o00o00o00o 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL o0D0DOOO0OO0O0O0O0O0O0O0O0O0O0O00000000000000000000000000000000000000000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 DO O TOG OU O O QU O O OO OO O O
36. E E E o E o E E DE o A eo E m E e E a E e D o a E E w E o O OQO O O O RO O O O O O OOTO O 00 0 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 OO OO OO OO OOOO OOO ome ooooooo0oqo0qoq0qo0qo0o0oo ooo oc o 50 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 With this command we select the source catalog a special file in which information about the sources is stored The syntax of the parameters in the source catalog is like that for the parameters of the source command see HELP SOURCE Lines starting with a are comments The standard file extension for source catalogs is sou NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names 5 NCS USER S GUIDE 51 Note that the format of the source catalog is meant to be like the source catalog format used at PLATEAU DE BURE Id demo source pako basic SOURCE EXAMPLES v 1 1 1 2009 05 08 by Hans
37. E330 are the 4 EMIR Eight MIxer Receiver bands 7 PAKO LANGUAGE INTERNAL HELP 135 HERA1 and HERA2 are the 2 parts of HERA HEterodyne Receiver Array If only receiverBand and lineName are specified we try to read the frequency and sideband subband from the line catalog specified with CATALOG LINE fileName The local oscillator for the receiverBand will be set so that the frequency corrected for the Doppler shift will be in the requested sideband subband SB See receiver documentation for the exact values of the IF NOTE EMIR subbands IF cables and Backends The output signals from EMIR are transmitted to the spectrometers and NBC through 8 IF cables Each IF cable carries one subband of bandwidth 4 GHz LO LI UI or UO NBC 4MHz WILMA and VESPA can only be connected to IF cables 1 to 4 FTS parts 1 to 4 can also be connected to IF cables 1 to 4 The command options RECEIVER HORIZONTAL and RECEIVER VERTICAL allow to select up to 4 EMIR subbands that will be transmitted through IF cables 1 to 4 compare HELP RECEIVER HORIZONTAL and the EMIR user documentation This selection can include Outer subbands In addition for EMIR bands E090 E230 and E330 the IF cables 5 to 8 carry the 4 Outer subbands corresponding to the subbands selected for IF cables 1 to 4 E g if we select for IF 1 to 4 E230 ver UO E090 ver UI E230 hor UI E090 hor UI then the IF cables 5 to 8 will transmit E230 ver UO E090 ver UO E230
38. EMIR LO LI UI UO This option selects which EMIR subband s of this polarization will be transmitted through IF cables 1 to 4 Note that some backends NBC 4MHz WILMA VESPA can only be connected to IF cables 1 to 4 i e only to the EMIR subbands selected with the RECEIVER command For each EMIR band and polarization at most 2 subbands can be transmitted through IF cables 1 to 4 Which combinations of EMIR bands polarizations and subbands are possibble is determined by the hardware of the EMIR IF switching box See the EMIR documentation for details If no subband is explicitly specified with this option paKo will assume that for this polarization the same single subband SB is requested as specified for the main parameters frequency tuning of the RECEIVER command for this EMIR band HORIZONTAL n one means that from this polarization no subband 7 PAKO LANGUAGE INTERNAL HELP 171 will be transported through IF cables 1 to 4 7 27 20 OPTIONS MODE MODE mode Character mode backend mode Choices for mode are SIMPLE simple standard PARALLEL parallel mode POLARIZATION polarimetry Select special mode for VESPA See VESPA user s guide for details For EMIR MODE PARALLEL or MODE POLARIZATION connect VESPA to the same band and subband in both polarizations they must previously have been selected with the RECEIVER command For exmples see HELP BACKEND Examples 7 27 21 OPTIONS NOTF NOTF nOtf
39. EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 01 01 01 01 01 01 02 02 02 02 20 20 20 20 20 20 20 20 21 21 21 21 21 21 21 213 21 22 22 22 22 23 23 08 15 16 21 36 37 04 17 24 27 00 01 07 05 15 23 25 38 01 07 15 23 31 34 36 39 48 22 22 22 22 22 22 22 46 53 56 58 13 02 03 13 18 25 32 36 20 38 ry 12 56 58 38 4141 30 28 03 50 Ti 45 44 30 28 19 10 37 38 01 29 44 235 10 238 01 05 43 14 4963 52 47 36 22 02 7684 0917 5176 8557 5910 3418 7735 4237 8812 0848 6989 9340 9646 7151 0066 8256 0188 8275 5931 3850 4941 2540 3053 5791 3021 4509 2793 9665 0315 2570 4015 4627 18 57 17 05 45 44 2309 7438 9320 9656 3867 8503 01 01 11 04 47 24 15 73 06 61 17 33 40 77 37 31 33 51 03 42 29 05 12 01 00 14 06 42 31 25 03 04 11 28 12 16 62 27 61 05 235 27 236 22 51 30 14 49 59 52 48 32 48 2
40. Fine Receiver E090 ver LO FTS 6 Fine Receiver E230 ver LO FTS 7 Fine Receiver E090 hor LO FTS 8 Fine Receiver E230 hor LO 1 EMIR WILMA 4MHz VESPA clear WILMA Default 4MHz Default VESPA 1 0 040 40 0 0 0 E090 Horiz LI VESPA 2 0 040 40 0 0 0 E090 Verti LI VESPA 3 0 040 40 0 0 0 E230 Horiz LI VESPA 4 0 040 40 0 0 0 E230 Verti LI 1 backends can be combined VESPA autocorrelator basic mode with fShift optional line name clear VESPA 1 0 040 40 0 120 0 E090 Horiz LI line EOHUO M VESPA 2 0 040 40 0 120 0 E090 Horiz LI line EOHUO P VESPA 3 0 040 40 0 100 0 E090 Verti LI line myLine3 VESPA 4 0 040 40 0 110 0 E090 Verti LI line myLine4 VESPA 5 0 040 80 0 150 0 E230 Horiz LI line VESPA 6 0 040 80 0 150 0 E230 Horiz LI line apple VESPA 7 0 040 80 0 200 0 E230 Verti LI line orange VESPA 8 0 040 80 0 200 0 E230 Verti LI line red EMIR VESPA autocorrelator basic and parallel modes backend BACKEND clear VESPA 1 0 320 240 0 0 0 E090 Horiz LI 4 PAKO S COOK BOOK 30 BACKEND VESPA 2 0 320 240 0 0 0 E090 Verti LI BACKEND VESPA 3 0 320 240 0 0 0 E230 Horiz LI mode parallel pause NOTE BACKEND VESPA E230 Horiz LI mode parallel 11 connects one VESPA part in parallel to 11 E230 Horiz LI and E230 Verti LI 1 both must be selected in RECEIVER command 11 HERA with FTS wide bandwidth receiver clear RECEIVER HERA1 WIDTH wide RECEIVER HERA2 WIDT
41. MIR Choices for backend name are BBC NBC 4MHz WILMA FTS VESPA Broad Band Continuum subband sideband polarization polarization polarization polarization polarization polarization frequency shift MHz receiver band EMIR polarization to E E to connect to connect to to connect to to connect to Backend Narrow Band Continuum Backend filter spectrometers with fixed resolution autocorrelation spectrometers Fourier Transform Spectrometer autocorrelator with variable resolution Choices for receiverBand are compare RECEIVER command E090 E150 E230 E330 HERA1 HERA2 sideband subband subband subband subband subband backend part backend part backend part backend part Choices for polarization are for EMIR compare RECEIVER command Horizontal Ve Choices for s LO LI rtical ubband UI UVO sideband when observing with EMIR are LSB USB 95 7 PAKO LANGUAGE INTERNAL HELP 96 LSB and USB apply only to EMIR bands with 8 GHz bandwidth E090 E230 and E330 and Backend BBC fShift can be used to shift offset the backend band within the receiver band this only applies to some backends in particular VESPA For VESPA the range for fShift is much smaller than the 4GHz subbands of EMIR For wide bandwidth backends fShift is fixed corresponding to the frequency pattern of the EMIR subbands and backend bands See EMIR and backend documentation CLEAR comp
42. NOTE this is a generic calibrate for any heterodyne receiver s and backends Remember to select the appropriate backend before Calibrate normally a continuum backend for POINTING and FOCUS and spectrometer s for TRACK ONOFF and heterodyne OTFMAPs In a standard calibration for heterodyne receivers we observe 3 subscans SAC on a Sky posi tion an Ambient temperature load a k a hot load and a Cold load Calibrations are always and automatically done in TOTAL POWER A calibration needs to be done for any heterodyne observation in order to get data with a calibrated intensity scale It is normally done before the target observations It must always be done after changing receiver and or backend setups It should also be done when changing sources and often enough to follow any variation of the athmosphere about every 15 minutes After you enter a calibrate setup manually we recommend to save it optionally to a named file SAVE CALIBRATE FILE calibrate 1 4 PAKO S COOK BOOK 37 It can then at any later time be reloaded with calibrate 1 see HELP SAVE 4 3 6 POINTING POINTING EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts Id demo pointing pako SOURCE Mars OFFSETS CLEAR demo rx 1 BACKEND CLEAR BACKEND BBC Default SET ANGLEUNIT arcsec 1 SWBEAM POINTING DEFAULT POINTING 120 NOTF 4 TOTF 30 0 PAUSE POINTING OK to star
43. OCO O OO O O OO CT O AO OO On OOO OO OO OO Oa OOO OOO O 48 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 5 NCS USER S GUIDE 1253 055 1308 326 1313 333 1334 127 1354 195 1413 135 1418 546 1502 106 1504 167 1510 089 1514 241 1546 027 1548 056 1606 106 1611 343 1622 297 1633 382 1637 574 1638 398 1641 399 1642 690 1655 077 1657 261 1716 686 1730 130 1732 389 1739 522 1741 038 SGRA 1749 096 1757 240 1800 440 1803 784 1807 698 1823 568 1828 487 1830 211 1842 681 1908 202 1921 293 1923 210 1928 738 1954 513 CYGA 1958 179 K3 50A 2005 403 2007 776 2013 370 2021 317 2023 336 2037 511 2059 034 NGC7027 EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 12 13 1
44. OPTIONAL mapping offsets in system projection ONOFF for Wobbler switching number of subscans symmetric subscan sequence time per subscan a chance to check start been selected IMPORTANT NOTE ONOFF with SWWOBBLER wobbler switching on off requires that the subscans are offset relative to the source in the trueHorizon system by 1 the With the commands above paKo recognizes this and automatically Wobbler elongations offsets In this case OFFSETS can be used to set additional mapping offsets in the projection of the astronomical coordinate system These mapping offsets in the projection apply 7 PAKO LANGUAGE INTERNAL HELP 7 11 O OTFMA TFMAP P xStart yStart xEnd yEnd Specify an On The Fly OTF map with linear OTF subscans Real Real Real Real The sequence of subscans is determined by xStart yStart xEnd yEnd x offset y offset x offset y offset croLoop n0tf reference step zigzag croL nOtf refe step zigz of of of of start start end end of first OTF of first OTF of first OTF of first OTF oop sequence of R off source Reference O on source OTF number of OTF subscans rence off source reference position step in x and y between OTF subscans translation of one OTF subscans to the next ag option to scan back and forth subscan subscan subscan subscan The scan analysis loops through the letter codes in croLoop u
45. RECEIVER and BACKEND setups 7 2 5 BACKEND CONNECT CONNECT yes no connect or disconnect the specified hardware e g backend or backend part gt DEPRECATED PROTECTED needs SET userLevel 7 2 6 BACKEND DISCONNECT DISCONNECT disconnect the specified hardware e g backend or backend part gt DEPRECATED PROTECTED needs SET userLevel 7 2 7 BACKEND FINE FINE for BACKEND FTS select the fine mode with a resolution of 0 049 MHz Note with the option DEFAULT or the short syntax this allows to select the fine resolution without explicitly entering the values of resolution and bandwidth 7 2 8 BACKEND MODE MODE mode Character mode backend mode Choices for mode are SIMPLE simple standard PARALLEL parallel mode POLARIZATION polarimetry Select special mode for VESPA See VESPA user s guide for details 7 PAKO LANGUAGE INTERNAL HELP 101 For EMIR MODE PARALLEL or MODE POLARIZATION connect VESPA to the same band and subband in both polarizations they must previously have been selected with the RECEIVER command For exmples see HELP BACKEND Examples 7 2 9 BACKEND LINENAME LINENAME lineName Character lineName name of line don t use lt gt gt OPTION OF BACKEND COMMAND FOR USE WITH EMIR This allows to set a line name for each backend part If a line name is set for a backend part it will be used in the CLASS header of the spectrum from
46. With the bolometer FOCUS is done with WOBBLER SWITCHING A calibration is not needed for FOCUS anyhow it will probably already have been done before the POINTING before the FOCUS After a focus the data processing software displays the results and you can enter a correction for the observed focus offset with the command SET FOCUS focusCorrection Note that this is the total correction i e the previous correction plus the additional offset found with the FOCUS observation The optiomal focus correction for different receiver bands may be slightly different by a few times 0 1 mm and the observer can decide to optimize for one particular band or use a compromise value After you enter a focus setup manually we recommend to save it optionally to a named file SAVE FOCUS FILE focus 1 It can then at any later time be reloaded with focus 1 see HELP SAVE 5 3 7 TRACK Single Position with Frequency Switching Id demo track pako TRACK EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo rx demo setup of receivers BACKEND CLEAR clear previous backends BACKEND VESPA 1 0 040 40 090 hor LI high spectral resolution BACKEND VESPA 2 0 040 40 090 ver LI with VESPA BACKEND VESPA 3 0 080 80 230 hor LI BACKEND VESPA 4 0 080 80 230 ver LI REPLACE WITH YOUR SETUP SET ANGLE arcsec oooo 5 NCS USER S GUIDE 70 setup frequency switching SWFREQUENCY 3 9 3 9 receiver E090 fo
47. angle unit is arc sec SHBEAM to select beam switching POINTING DEFAULT reset all options POINTING 120 pointing with subscan length 120 NOTF 4 4 OTF subscans TOTF 30 0 30 seconds per OTF subscan PAUSE POINTING OK to start c q a chance to check START start RETURN NOTE if you use NASMYTH offsets for an off center pixel of a mutlibeam receiver don t use OFFSETS CLEAR If you want the intensity of the Pointing data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before the pointing POINTING observations are done to optimize the positioning of the telescope in Azimuth and Elevation This is normally done by continuum observations of a cross scan in azimuth and elevation on a point source or at least a small source near the intended target source It is normally used with BEAM SWITCHING or WOBBLER SWITCHING it is also possible with TOTAL POWER With the bolometer POINTING is done with WOBBLER SWITCHING A calibration is not needed for POINTING if one is only interested in the pointing corrections and not in the source intensity After a pointing the data processing software displays the results and you can enter a correction for the observed pointing offsets with the command SET POINTING azimuthCorrection elevationCorrection Note that this is the total correction i e the previous correction plus the additional off
48. any case it is recommended to use ONOFF instead of RASTER with several ON per OFF gt gt 6 4 8 TRACK The TRACK observing mode simply tracks one position relative to the source It is normally used with FREQUENCY SWITCHING and offsets in SYSTEM projection 6 NCS EXPLAINED 89 The basic parameters are the offsets for the position to track parameters of the options are the total number of subscans and the time per subscan in s After you enter a track setup manually we recommend to save it optionally to a named file SAVE TRACK FILE track 1 It can then at any later time be reloaded with track 1 see HELP SAVE You may want to save the switching mode seperately or with TRACK into the same file SAVE SWITCHING FILE track 2 SAVE TRACK FILE track 2 APPEND 6 4 9 VLBI VLBI a special observing mode to track the source position specified with SOURCE during VLBI scans It should only be used for VLBI and is always used with TOTAL POWER 6 5 Receivers This section remains to be written For the time being please refer to the information available on the web pages about the 30 M Telescope 6 6 Backends This section remains to be written For the time being please refer to the information available on the web pages about the 30 M Telescope 7 PAKO LANGUAGE INTERNAL HELP 90 7 PAKO Language Internal Help From here follows a reproduction of the Internal Help available in paKo with HELP PAKO Please consult t
49. at 0 5 sec 7 24 1 TIP DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 24 2 TIP AIRMASS AIRMASS airmassStart TO airmassEnd BY airmassStep range of airmass for TIP Real Real Real NOTE 1 NOTE 2 airmassStart airmassEnd airmassStep elevation ASIN 1 airmass for slew tips TIP SLEW airmassStep has no effect airmassStart gt airmassEnd is allowed this implies elevation at start lt elevation at end i e TIP from low to high elevation for traditional TIP with SLEW no airmassStart lt airmassEnd i e they go from high to low elevation 7 24 3 TIP TSUBSCAN TSUBSCAN tSubscan time per subscan 7 PAKO LANGUAGE INTERNAL HELP 163 Real tSubscan time 7 25 TRACK TRACK xOffset yOffset specify tracking of a single position Real xOffset x offset of on source position Real yOffset y offset of on source position NOTES TRACK is normally used for observations with frequency switching SWFREQUENCY also for some special observations e g of pulsars There is a built in limit to the time per subscan currently 2006 07 it is 3600 seconds 1 hour If for special purposes one needs to track a source for a longer time this can easily be done by using several subscans 7 25 1 TRACK DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 25 2 TRACK SYSTEM SYSTEM systemName N
50. but different elevations spaced by equal steps in air mass It is ESSENTIAL that the switching mode is TOTAL POWER during TIP This is in particular an important step in the calibration of observations with the bolometer The basic parameters of this observing mode and its options are the azimuth the range and step in airmass and the time per subscan 6 45 ONOFF In its first form ONOFF is used with TOTAL POWER Subscans are taken alternating between a position that s considered to be ON source and a reference position that s normally assumed to be OFF source i e free of emission The source signal is then calculated as the difference between ON and OFF The basic parameters are the offsets for the ON position parameters of the options are the offsets for the reference position the total number of subscans and the time per subscan in s After you enter an ON OFF setup manually we recommend to save it optionally to a named file SAVE ONOFF FILE onoff 1 It can then at any later time be reloaded with onoff 1 see HELP SAVE You may want to save the switching mode seperately or with ONOFF into the same file 6 NCS EXPLAINED 88 SAVE SWITCHING FILE onoff 2 SAVE ONOFF FILE onoff 2 APPEND When ONOFF is used with WOBBLER SWITCHING command SWWOBBLER the position offsets must be set to very specific values in TRUE ANGLE HORIZON depending on the parameters of SWWOBBLER This
51. clear l RECEIVER E150 RECEIVER E330 say say say pause say receiver clear I RECEIVER E150 RECEIVER E330 say say say pause RETURN Horizontal LI UI Vertical none HCN 1 0 Hor LI UI Ver none 12C0 2 1 Horizontal none Vertical LI UI CS 3 2 Horizontal LI Vertical LI 13C0 3 2 Horizontal LI Vertical LI CS 3 2 Horizontal none Vertical LI 13C0 3 2 Horizontal UI Vertical LI NOTE NOTE E090 V UI 1 E230 H LI UI E090 V UO for FTS E230 H LO U0 for FTS E090 E230 full BW single pol LSB Inner LI USB Inner UI LSB Inner LI USB Inner UI NOTE NOTE NOTE NOTE NOTE NOTE NOTE NOTE E090 H LI UI 2 4 GHz BW E090 H L0 U0 for FTS E230 V LI UI 2 4 GHz BW E230 V LO U0 for FTS E150 LI E330 8 GHz i E150 H V LI 4 GHz BW E330 H V LI 4 GHz BW E330 H V LO for FTS E150 LI E330 full BW E150 V LI 4 GHz BW E330 H UI V LI 4 GHz BW E330 H UO V LO for FTS 60 5 NCS USER S GUIDE 61 Normally we use the RECEIVER command with 2 parameters a receiver name and a line name The line name must be the name of a line in the line catalog selected earlier The frequency and sideband or EMIR sub band are then taken from the line catalog Alternatively the frequency and sideband or sub band can be specified directly as the 3rd and 4th parameter NOTES For the EMIR bands
52. hand the idiomatic usage SAVE ALL C FILE LAST allows to save really everything in order to recover it with LAST SAVE SWITCHING saves the currently selected switching mode total power beam frequency wobbler to file switching pako or to a different file specified with FILE NOTE the parameters of unused unselected hardware switching modes and observing modes are never saved 7 14 1 SAVE APPEND APPEND yes no Append to existing file do not create a new one Logical doAppend default false 7 14 2 SAVE FILE FILE fileName Specify file name Character fileName 7 14 33 SAVE EXAMPLES SAVE EXAMPLES v1 0 0 2005 12 19 Hans Ungerechts SOURCE SWFREQUENCY SWTOTAL ONOFF OTFMAP SAVE saves OTFMAP to file otfmap pako SAVE ALL saves everything to file all pako 7 PAKO LANGUAGE INTERNAL HELP 143 SAVE ONOFF saves ONOFF to file onoff pako SAVE SOURCE saves SOURCE to file source pako SAVE SWITCHING saves SWTOTAL to file switching pako SAVE SWFREQUENCY saves SWFREQUENCY to file swfrequency pako 7 15 SET SET keyword value valuex Set values for some general parameters Character keyword Character Integer Real value Keywords Type of Value s Level Integer Integer minumum value s for warning and error messa Project Character len 24 project ID PI Character len 24 PI Don t use amp lt gt Observer Character len 24 Obs
53. hardware e g backend or backend part 7 PAKO LANGUAGE INTERNAL HELP 137 gt DEPRECATED PROTECTED needs SET userLevel 7 13 6 RECEIVER DOPPLER DOPPLER doppler Character doppler apply doppler correction choices DOPPLER FIXED 7 13 7 RECEIVER EFFICIENCY EFFICIENCY forwardEfficiency beamEfficiency specify forward and beam efficiencies Real forwardEfficiency Real beamEfficiency 7 13 8 RECEIVER GAINIMAGE GAINIMAGE gainImage dB Specify the gain ratio of image to signal sidebands Real gainImage If dB is added after the value the ratio is assumed to be in dB otherwise a decimal fraction gt A standard value for EMIR is 13 db for HERA 10 db 7 13 9 RECEIVER HORIZONTAL HORIZONTAL sb1 sb2 HORIZONTAL n one EMIR subbands for Horizontal polarization This option applies only to EMIR Character sbi sb2 for EMIR LO LI UI UO This option selects which EMIR subband s of this polarization will be transmitted through IF cables 1 to 4 Note that some backends NBC 7 PAKO LANGUAGE INTERNAL HELP 138 4MHz WILMA VESPA can only be connected to IF cables 1 to 4 i e only to the EMIR subbands selected with the RECEIVER command For each EMIR band and polarization at most 2 subbands can be transmitted through IF cables 1 to 4 Which combinations of EMIR bands polarizations and subbands are possibble is determined by the hardware of the EMIR 1F switching box S
54. hor FTS 4 Fine Receiver E230 ver FTS 5 Fine Receiver E090 ver FTS 6 Fine Receiver E230 ver FTS 7 Fine Receiver E090 hor FTS 8 Fine Receiver E230 hor clear WILMA Default 4MHz Default VESPA 1 0 040 40 0 0 0 VESPA 2 0 040 40 0 0 0 VESPA 3 0 040 40 0 0 0 VESPA 4 0 040 40 0 0 0 VESPA autocorrelator basic clear VESPA 1 0 040 40 0 120 0 VESPA 2 0 040 40 0 120 0 VESPA 3 0 040 40 0 100 0 VESPA 4 0 040 40 0 110 0 VESPA 5 0 040 80 0 150 0 VESPA 6 0 040 80 0 150 0 VESPA 7 0 040 80 0 200 0 VESPA 8 0 040 80 0 200 0 VESPA autocorrelator basic clear VESPA 1 0 320 240 0 0 0 VESPA 2 0 320 240 0 0 0 VESPA 3 0 320 240 0 0 0 BACKEND VESPA LI LI LI LI LO LO LO LO E090 E090 E230 E230 E090 E090 E090 E090 E230 E230 E230 E230 E090 E090 E230 E230 Horiz LI mode backends can be combined connect 1 part to each selected EMIR subband plus 1 part to each of the 4 outer subbands of E090 short syntax fine EMIR WILMA 4MHz VESPA LI LI LI El Horiz Verti Horiz Verti LI LI LI LI LI LI LI LI Horiz Horiz Verti Verti Horiz Horiz Verti Verti and parallel modes LI LI LI Horiz Verti Horiz parallel line line line line line line line line mode mode with fShift optional line name EOHUO M EOHUO P myLine3 myLine4 apple orange red parallel 104 7 PAKO LANGUAGE INTERNAL HELP 7 3 connects one VESPA part i
55. letter L instead of a number In this case during the execution of the observations the NCS will 176 7 PAKO LANGUAGE INTERNAL HELP 177 use the best known values for the corresponding load temperature s For tempColdLoad this is based on a lookup table for tempAmbientLoad it is derived from a measurement of the physical temperature The lookup table for tempColdLoad normally is valid for the standard calibration system with a closed cycle cooling system A can be substituted for tempColdLoad which means to leave the value for tempColdLoad unchanged from the previous RECEIVER command IF THE OBSERVERS HAVE ANY DOUBT ABOUT THIS THEY SHOULD ASK A RECEIVER ENGINEER FOR THE CORRECT VALUE AND ENTER IT EXPLICITLY NOTE FOR HERA The new logic is not yet available However for HERA best known values are always used during the execution of the observations This is the same logic as in pevious versions of paKo NCS 7 27 39 OPTIONS VELOCITY VELOCITY referenceFrame velocity Specify reference frame and source radial velocity Character referenceFrame reference system for velocity Real velocity in units km s Choices for referenceFrame LSR barycentric heliocentric lt lt TBD not yet supported gt gt lt lt TBD 3K gt gt lt lt TBD galactocentric gt gt lt lt TBD body gt gt lt lt TBD geocentric gt gt lt lt TBD topocentric gt gt lt lt TBD null gt gt
56. need more parameters and more explicit BACKEND commands see the following sections 4 PAKO S COOK BOOK 24 4 PakKo s Cook Book This section provides a basic step by step cook book for standard observations in an interactive session It only gives simple examples details on all the parameters and options can be found in later sections If you only need to refresh your memory of what standard commands in a typical observation run look like it may be sufficient to look at the examples without reading the explanations Also note that a later section NCS User s Guide follows the same general outline repeats most of the information in Pako s Cook Book but provides more detailed explanations and more elaborate examples in the form of PAKO scripts This section starts with some general commands and the selection of a source catalog The next subsection explains how to do Spectral Line Observations with Heterodyne Receivers Remember that in command language scripts based on SIC starts a comment indicates that a command is continued on the next line PAUSE pauses the execution of the script e g in order to allow the user to review the param eters set RETURN ends the execution of the script and returns to the level from which the script was called you have to delete or comment RETURN in order to execute the rest of the script Generally the case UPPER lower or Mixed doesn t matter To execute a
57. observed focus offset with the command SET FOCUS focusCorrection Note that this is the total correction i e the previous correction plus the additional offset found with the FOCUS observation The optiomal focus correction for different receiver bands may be slightly different by a few times 0 1 mm and the observer can decide to optimize for one particular band or use a compromise value After you enter a focus setup manually we recommend to save it optionally to a named file SAVE FOCUS FILE focus 1 It can then at any later time be reloaded with focus 1 see HELP SAVE 5 4 5 TIP Antenna Tipping or Skydip Id demo bolometer tip pako v 0 2 2005 07 14 by Hans Ungerechts RECEIVER BOLOMETER SWTOTAL TPHASE 0 5 select Total Power IMPORTANT TIP 180 tip at azimuth 180 deg AIRMASS 1 1 4 1 0 6 air mass from to by step TSUBSCAN 12 0 time per subscan s PAUSE TIP OK to start c q a chance to check START start To execute this script simply enter demo bolometer tip TIP antenna tipping or skydip observations are done to measure the transmission of the Earth s athmosphere by taking data at several points with the same azimuth but different elevations spaced by equal steps in air mass It is ESSENTIAL that the switching mode is TOTAL POWER during TIP This is in particular an important step in the calibration of observations with the bolo
58. phases b in the other subscans the other position of the antenna the source is in the second of the two Wobbler phases During the data processing the source signal is computed as a double difference 1st the difference of the 2 Wobbler phases 2nd the difference between ONOFF subscans a and b This form of ONOFF is also called Wobbler Onoff or sometimes simply Wobbler Switching The combination of ONOFF and WOBBLER SWITCHING provides a very high sensitivity in continuum bolometer observations of compact sources and excellent baselines for spectroscopy It has the disadvantage that the emission free off source positions are very close to the source limited by the maximum Wobbler throw Also the Wobbler direction is fixed in the horizontal system relative to the telescope and therefore in the source system the off source positions rotate around the source position For continumm observations usually a short time per Wobbler phase 0 25 s is used with small Wobbler offsets throws for spectroscopy largest possible Wobbler offsets throws up to 120 are preferred but then the time per phase must be longer 1 2 s 5 3 9 OTF On The Fly Mapping Id demo otfmap pako OTFMAP SWIOTAL EXAMPLE v 1 1 6 2011 07 21 Hans Ungerechts demo rx spectrometers demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP SET ANGLE arcsec 1 SWTOTAL to select total power
59. project number SET PI Dr Lilo D Doe principal investigator SET Observer John Doe SET Operator Pako SET Topology low topology for azimuth SET Level 3 3 suppress informational message I messages from paKo DEVICE image w for plots SHOW show the values set with set 1 NOTE don t use special characters like lt gt amp accents in the names 11 Id demo set2 pako additional SET EXAMPLES v 1 1 1 2009 05 08 Hans Ungerechts 7 PAKO LANGUAGE INTERNAL HELP 148 11 SET doSubmit YES to allow submission to Queue SET Pointing 1 1 2 2 pointing corrections SET Focus 2 3 focus correction mm SHOW show the values set with set 7 16 SHOW SHOW List all parameters that can be set with command SET as well as their current values 7 17 SOURCE SOURCE sourceName systemName epoch lambda beta referenceFrame velocity 1 SOURCE Body sourceName perihelionEpoch ascendingNode argumentOfPerihelion inclination perihelionDistance eccentricity Select a source from the source catalog or specify source parameters directly on command the line Character 12 sourceName don t use amp lt gt Character systemName C Real epoch in units years NOTE epoch should be J2000 0 Coordinate lambda longitude Coordinate beta latitude Character referenceFrame reference system for velocity Real velocity in units km s IMPO
60. s sas RON e a ee RE 112 Ro ODAJU cw oe eh Ree ew ee PEER eh ESO Re bee ES 112 TSL IIBSAJOUOS CENTER et eb oes deeb bee eee Ree oe ee NS 113 182 LISSAJOUS PREQUE NOY os cos soe bela a ee a as 114 183 LISSAJOUS PHASES o io os ane eee wea Sede ee a Be 114 24 LISSAJQUS SYSTEM bee bh obs eh ee ERE a ee eee t 114 100 LISSAJOUS TOTE o ack ot be he s Di ER oe ee Se eee Ee Ok 115 TO OFFSETS opa co alk wee a Rk Be ARG we RR Ee hee ee eh ee 115 791 OFFSETS DEFAULTS 6 sc ca mg beh 0 Ree ee eR A 117 T92 OFFSETS CLEAR scce trene t be eee e be Ge EE SS 117 CONTENTS 6 7 10 q Dl FL 7 13 7 14 ES OFFSETS Fore e cre o ee ee ee 117 ONORE ce RAN 118 FUE ONOFF DEFPA ULIS oxicorte e SH He 120 F102 ONOFF NSUBSCANS 225 s a aoga eee Dede aue he ee hee ees 120 7 10 3 ONOFF REFERENCE oso o 044 oe 44a wa dee Bae ae Sw oe 120 7 104 ONOFF SWWOBBLER vo s cacr aca 2a dae eS ee ee Sw as 120 7 105 ONOFF SYMMETNIG sosa gore sor a be eo Ke Oda De daw Ws 121 JOB ONOFF SYSTEM ep ee eh eee Vee Ree EROS BE REE EE ee 122 7 10 7 ONOFF TSUBSCAN vrs devra a ee araa 123 10 8 ONOFF EXAMPLES s s soo 48 Pee Rss ce p E e Re 123 OTEMADB sar rr A BAG OR A a 125 ILL OTEMAP DEFAULTS ec cec eb Sed tribales LESH ES 127 ALA OTFMAP CROLOOP cesar Oe eee oe hE See eee bares 127 TALS OTEMAP NOU coord a eRe Sea 127 TALA OTFMAP REFERENCE cosacos coros See Se ee ee Se ri 128 PILO ATT ASE candor e eee ee eh aS Oe pe eee eee eee 128 7 116 OTP MA
61. saved files is that of a valid script in the command language Therefore you can restore it later enter at the prompt PAKO gt POINTING In a similar way you can save the parameters of the source receiver and backend setup and of the switching mode SAVE ALL saves nearly all current parameters as well as the current switching and observing modes It saves the pointing and focus corrections only if used in the form SAVE ALL C ORRECTIONS 2 PAKO GUIDE OF THE PERPLEXED 12 Normally SAVE ALL is meant to generate a paKo script that can be used to re produce the setup at a later time when one probably wants to use different pointing and focus corrections On the other hand the idiomatic usage SAVE ALL C FILE LAST allows to save really everything in order to recover it with LAST The parameters of unused unselected hardware switching modes and observing modes are never saved Tip check out the options of command save enter at the prompt PAKO gt HELP SAVE FILE HELP SAVE APPEND After using O to restore a saved observing mode e g otfmap the graphic display may look confused To clean it up enter at the prompt PAKO gt CLEAR PLOT BOX OTFMAP i e the observing mode 2 7 Observation Queues and Starting In the NCS all observations are handled through an observation queue So far this is rather simple first in first out The operator has to set the current observation queue
62. start c ql source already has pako Hans Ungerechts demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP select total power time per phase data sample ambient load cold load sky at offsets 600 0 0 0 system for SKY offsets time per calibration subscan a chance to check start offsets of on position number of subscans offsets of off source referen system for offsets symmetric subscan sequence time per subscan a chance to check start been selected 123 7 PAKO LANGUAGE INTERNAL HELP 124 ONOFF SWWOBBLER EXAMPLE v 1 1 6 2011 07 31 Hans Ungerechts WOBBLER SWITCHING demo rx spectrometers SET ANGLE arcsec SWWOBBLER 120 0 120 0 TPHASE 1 0 CALIBRATE AMBIENT COLD SKY 600 0 0 0 SYSTEM projection TCALIBRATE 5 0 1 PAUSE CALIBRATE OK to start c q START 11 1 OFFSETS 20 30 SYSTEM projection ONOFF SWWOBBLER NSUBSCANS 12 SYMMETRIC TSUBSCAN 30 PAUSE ONOFF SWWOBBLER OK to start c q Comments see demo source sets the correct values to all ONOFF subscans we assume here that the source already has demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP select wobbler switching wobbler 120 arc sec 1 seconds per phase ambient load cold load sky at offsets 600 0 0 0 system for SKY offsets time per calibration subscan a Chance to check start
63. subscan PAUSE CALIBRATE OK to start c q a chance to check START start 1 OPTIONAL OFFSETS 20 30 mapping offsets in SYSTEM projection system projection ONOFF SWWOBBLER NSUBSCANS 12 SYMMETRIC TSUBSCAN 30 ONOFF for Wobbler switching number of subscans symmetric subscan sequence time per subscan 5 NCS USER S GUIDE 73 PAUSE ONOFF SWWOBBLER OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source IMPORTANT NOTE ONOFF with SWWOBBLER wobbler switching on off requires that the subscans are offset relative to the source in the trueHorizon system by 1 the Wobbler elongations offsets With the commands above paKo recognizes this and automatically sets the correct values In this case OFFSETS can be used to set additional mapping offsets in the projection of the astronomical coordinate system These mapping offsets in the projection apply to all ONOFF subscans When ONOFF is used with WOBBLER SWITCHING command SWWOBBLER the position offsets must be set to very specific values in TRUE ANGLE HORIZON depending on the parameters of SWWOBBLER This is achieved by using the special option SWWOBBLER of the command ONOFF Subscans are then taken alternating between 2 positions in such a way that a in some subscans one position of the antenna the source is in the first of the two Wobbler
64. system and at PdB NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names 2 9 Switching Modes In the NCS we distinguish the following 4 Switching Modes TOTAL POWER BEAM SWITCHING WOBBLER SWITCHING FREQUENCY SWITCHING only with heterodyne receivers The corresponding commands are SWTOTAL SWBEAM SWWOBBLER SWFREQUENCY BEAM SWITCHING WOBBLER SWITCHING and FREQUENCY SWITCHING are realized by a system with hardware synchronization signals that allow a precise and fast switching within subscans TOTAL POWER simply means that none of the other 3 switching modes is active The system switches through a regular cycle with several 1 2 or 4 switching phases The 4 switching modes are mutually exclusive 1 e at any time the system uses only one of them During the transitions between phases e g while the Wobbler is moving between its positions no data are taken during the short blanking time The switching mode and its parameters should normally be set before choosing an observing mode because for some observing modes details of the setup depend on the switching mode 2 10 Observing Modes The NCS supports the following Observing Modes CALIBRATE POINTING FOCUS TIP ONOFF OTFMAP lt lt TBD RASTE
65. the EMIR user guide CLEAR completely clears the receiver setup RECEIVER must be specified before BACKEND After you enter a receiver setup manually we recommend to save it optionally to a named file SAVE RECEIVER FILE receiver 1 It can then at any later time be reloaded with receiver 1 see HELP SAVE Option DEROTATOR angle system sets the derotator angle for HERA DOPPLER controls whether Doppler corrections will be applied for that receiver WIDTH allows to select narrow or wide mode for HERA Note that simple standard VESPA setups require narrow This option does not apply to EMIR GAIN allows to set the gain ratio I S between image and signal sidebands With the syntax GAIN 13 db you can specify the image gain directly in dB TEMP LOAD allows to set the effective temperatures of the cold and ambient loads TEMP L L implies that during the execution of the observations the NCS will use the best known values For the cold load this is based on a lookup table for the ambient load it is derived from a measurement of the physical temperature EFF ICIENCY allows to set the forward and main beam efficiencies Gain ratio load temperatures and efficiencies describe physical parameters of the system which can not really be controlled by the observer However the options are available here to specify these values because they are important for the calibration of the data
66. the antenna moves relative to the source while recording its position and taking data a high rate thus performing scans in the strict sense of the word This is a very fast mode for mapping The basic parameters of the command are the position offsets of the start and end of the first OTF subscan the basic parameters of the options are the number of OTF subscans the offsets of an off source reference position the step shift in x and y offsets between subsequent OTF subscans the time per OTF subscan in s and the time per off source reference subscan s This observing mode is normally used either with i TOTAL POWER with an off source reference for spectral line observations or ii FREQUENCY SWITCHING without off source reference for spectral line observations see below or iii WOBBLER SWITCHING and TRUE ANGLE HORIZON offsets for continuum mapping with the bolometer After you enter an OTF map setup manually we recommend to save it optionally to a named file SAVE OTFMAP FILE otfmap 1 It can then at any later time be reloaded with otfmap 1 see HELP SAVE You may want to save the switching mode seperately or with OTFMAP into the same file SAVE SWITCHING FILE otfmap 2 SAVE OTFMAP FILE otfmap 2 APPEND 6 4 7 RASTER lt lt RASTER not yet implemented will be similar to ONOFF and TRACK but allow to observe several ON positions To be used with ToTAL POWER or maybe FREQUENCY SWITCHING In
67. to 3600 000 2 standard range If you enter a value outside the standard range you get a warning message but the value is accepted e g enter at the prompt PAKO gt POINTING TOTF 3000 W TOTF value 3000 000 outside standard range 10 00000 to 600 0000 2 20 Independence of Command Parameters The parameters of each observing mode are independent from the parameters of other observing modes The same is true fop the different switching modes For example if you first enter at the prompt PAKO gt OTFMAP NOTF 12 and later POINTING NOTF 4 the number of OTF subscans for OTFMAP is still at 12 as you can see with OTFMAP Some options exist for several observing modes E g options NOTF and TOTF exist for POINTING and OTFMAP The syntax parameters and meaning of these options is then almost the same for all observing modes 2 21 Option keywords Options that start with t refer to times durations e g tOtf time per OTF subscan n refer to number of something e g nOtf number of OTF subscans f refer to frequency of something temp refer to temperature of something 2 22 Logical YES NO or ON OFF Options Several options of commands are logicals which can have only one of 2 values TRUE YES shown in the display as T or FALSE NO shown in the display as F The command syntax and logic for ALL these options is the same e g enter at the prompt PAKO gt OTFMAP ZIGZAG
68. to 420 degrees SET TOPOLOGY HIGH selects to use the azimuth range 100 to 460 degrees About SET TOPOLOGY also see Section 6 2 and Figure 4 in that section DEVICE is a standard command to open a graphics window for plots It is used by PAKO to provide a preview plot for some observing modes SET LEVEL can be used to control the amount of messages written by PAKO in the terminal window SET LEVEL 3 3 is a good choice in most cases because it suppresses many informational I messages but lets all warnings and serious errors through All these commands should normally be executed in the same way each time observations for a project start Therefore it is a good idea to put them in a script SET doSubmit yes is needed to activate submission of observing commands to the NCS observing queue SET doSubmit no default is useful for debugging so that scripts including START can excute without actually trying to submit observations NOTE the operator also has to set the current observation queue to be that of the project account Submission from other projects will not be accepted by the NCS SET POINTING and SET FOCUS are used to set pointing and focus corrections 5 2 Specify your Source Catalog and or Source Id demo sou v 1 0 1 2006 01 03 by Hans Ungerechts generated by ASTRO from IRAM CAT pointing sources 0003 380 EQ 2000 00 05 57 1352 38 20 14 869 LSR 0 000 FL 0 000 0 000 0048 097 EQ 2000 00
69. true angle horizontal syste with throw ABS wOffset2 wO0ffset1 7 PAKO LANGUAGE INTERNAL HELP 119 Data from 1 are treated as source signal data from 2 and 3 as off source reference signal Note that in the astronomical coordinates positions 2 and 3 will rotate around the source position 1 Therefore one must normally be sure that the extent of the source is less than throw beamWidth 2 REFERENCE xOffsetR yOffsetR systemNameRef or REFERENCE NO no reference position of off source reference subscans Real xOffsetR x offset Real yOffsetR y offset Character systemNameRef name of system see SYSTEM for choices NOTE with the usage REFERENCE xOffsetR yOffsetR both parameters are requi but you can replace either parameter with to leave it unchanged SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NA
70. used with FREQUENCY SWITCHING TRACK 10 20 SYSTEM projection Example 2 Observe ONOFF position switching with TOTAL POWER with ON position at 30 40 and off source reference at 600 700 both in system radio projection ONOFF 30 40 REFERENCE 600 700 projection SYSTEM projection Example 3 Pointing with subscans of length 120 POINTING 120 NOTES For POINTING the OTF offsets are always in system trueHorizon and are specified implicitly though the angular length of the subscans Example 4 ONOFF observations with WOBBLER SWITCHING are a special case because the offsets for the subscans must be in system trueHorizon and their values must be selected according to the offsets of the WOBBLER SWITCHING E g SWWOBBLER 33 33 ONOFF 33 O REFERENCE 33 0 trueHorizon SYSTEM trueHorizon This can also be achieved simply by saying SWWOBBLER 33 ONOFF 2 PAKO GUIDE OF THE PERPLEXED 16 PAKO knows the special requirements for onoff wobbler switching and will set the offset parameters for ONOFF accordingly if SWWOBBLER has been previously selected In this special case in order to map the source the observer may add offsets on the source and b using the command OFFSETS with the system projection e g SWWOBBLER 33 OFFSETS 110 120 SYSTEM projection ONOFF NOTES SOURCE does not clear offsets set with OFFSETS NOTES If you are unsure about any of this read the additional information in Sectio
71. vi 1 1 SUPPORT FOR EMIR gt major changes in CALIBRATE BACKEND RECEIVER modifications of some commands FOR MAMBO BOLOMETER OBSERVATIONS see OFFSETS SYSTEM NASMYTH OFFSETS SYSTEM NASMYTH CLEAR TIP TPADDLE TIP SLEW paKo v1 0 9 paKo v1 0 8 IMPORTANT CHANGE NEW LOGIC FOR RECEIVER TEMPLOAD L L for details see HELP RECEIVER TEMPLOAD 93 GENERAL paKo Lock Sequence of Commands Checks NEW COMMANDS SET 2ndRotation SHOW NOTE NEW OPTIONS POINTING DOUBLEBEAM NOTE lt lt TBD gt gt lt lt aro A 7 1 2 Language HELP 7 PAKO LANGUAGE INTERNAL HELP 94 There is a new lock file mechanism to prevent that 2 instances of pako run in the same working directory It is now enforced for the purpose of consistency che scan analysis i e for the translation to subsan BACKEND must be specified after RECEIVER Observing Mode must be specified after Switching Mode Observing Mode must be specified after SET 2ndRotatio ONOFF must be specified after OFFSETS START will not work without SOURCE RECEIVER and BAC There are various stricter limit checks and more cons checks set rotation angle for secondary mirror and Wobbling mechamism This is ONLY for Bolometer with Wobbler Switching and POINTING FOCUS and OTFMAP now also shows the pako version revision number and and the 2ndRotation the character is NOT allowed in source names to avoid confusion
72. w for plots SHOW show the values set with set 1 11 NOTE don t use special characters like lt gt amp accents in the names 11 Id demo set2 pako additional SET EXAMPLES v 1 1 1 2009 05 08 Hans Ungerechts SET doSubmit YES to allow submission to Queue SET Pointing 1 1 2 2 pointing corrections SET Focus 2 3 focus correction mm SHOW show the values set with set 1 5 NCS USER S GUIDE 47 SIC PRIORITY 1 PAKO assures that PAKO commands have priority over similar other commands e g POI will be understood as PAKO POINTING and not as GREG1 POINTS With the SET commands we specify some basic information the project number the principal inves tigator PI the names of the observer and telescope operator NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names SHOW lists everything previously set with SET SET TOPOLOGY deserves special attention The 30m antenna has azimuth limits of 60 and 460 degrees Azimuth 360 degrees is due North Therefore there is an overlap range approximately toward East Northeast which the antenna can reach at a low azimuth 60 to 100 from the South or at a high azimuth 420 to 460 from the North SET TOPOLOGY LOW selects to use the azimuth range 60
73. 0 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL FL o0D0DOOO0OO0O0O0O0O0O0O0O0O0O0O00000000000000000000000000000000000000000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 DO O TOG OU O O QU O O OO OO O O OCO O OO O O OO CT O AO OO On OOO OO OO OO Oa OOO OOO O 49 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 000 5 NCS USER S GUIDE 2113 293 2121 053 2128 123 2131 021 2134 004 2136 141 2145 067 2200 420 2201 315 2210 257 2216 038 2223 052 2230 114 2234 282 2243 123 2251 158 2254 617 2255 282 NGC7538 2318 049 The following sources are SiO masers and are useable for pointing
74. 0 corresponds to the Wobbler switching purely in Azimuth i e normal Wobbler switching Observers must inform the operator if they want to use this feature A non zero values is up to know only meaningful and supported for bolometer observations with Wobbler switching and the observing modes POINTING FOCUS and OTFMAP The OTF map must be set to be in the true angle horizontal system and the direction of the OTF subscans must agree with that of the 2ndRotation There is a special pako script available in the bolometer pool to do this To avoid un intentional errors this feature can only be used by privileged users ask the AOD or the NCS team 7 15 6 SET TOPOLOGY SET TOPOLOGY topology topology Character len 24 Topology for the overlapping azimuth range Choices for topology are LOW HIGH 7 PAKO LANGUAGE INTERNAL HELP 146 Select a topology for sources in the overlapping azimuth range 60 to 100 degrees 420 to 460 degrees The 30m antenna has azimuth limits of 60 and 460 degrees Azimuth 360 degrees is due North Therefore there is an overlap range approximately toward East Northeast which the antenna can reach at a low azimuth 60 to 100 from the South or at a high azimuth 420 to 460 from the North SET TOPOLOGY LOW selects to use the azimuth range 60 to 420 degrees SET TOPOLOGY HIGH selects to use the azimuth range 100 to 460 degrees Note this is shown in a figure in paKo s manual Section NCS Explai
75. 0 CS 3 2 H LI V LI RECEIVER E330 13C0 3 2 H LI 56 clear all receivers previously set NOTE E090 band line f SB from catalog SB from catalog SB from catalog f frequency SB sideband subband NOTE E090 band line f SB explicit SB explicit SB explicit NOTE E090 H amp V 4 GHz BW NOTE E090 E150 bands LSB Inner LSB Inner LSB Inner LSB Inner NOTE E090 H V 4 GHz BW E150 H V 4 GHz BW NOTE E090 E230 bands LSB Inner LSB Inner LSB Inner LSB Inner NOTE E090 H V 4 GHz BW E230 H V 4 GHz BW NOTE E150 E330 bands LSB Inner LSB Inner LSB Inner 5 NCS USER S GUIDE V LI say wog say w pause Hitt RECEIVER clear REC HERA1 12C0 2 1 230 537990 LSB REC HERA2 12C0 2 1 230 537990 LSB pause 1 Id demo receiver pako more demos v 1 1 11 2011 11 CATALOG line 24 demo EMIR lin say Mal RECEIVER CLEAR RECEIVER E090 pause 1 Bay ae receiver clear temp 30 260 eff 0 95 0 75 scale beam RECEIVER E090 HCN 1 0 pause l say oI RECEIVER E090 HCN 1 0 Horizontal LI UI Vertical LI UI dop dop gain 13 db 1 pause l say oie receiver clear RECEIVER E090 HCN 1 0 Horizontal LI UI Vertical LI UI n p lt NOTE 57 LSB Inner NOTE E150 H V 4 GHz BW NOTE E330 H V 4 GHz BW clear all receivers previously set Hans Ungerechts specify
76. 000 VXSGR EQ 2000 18 08 04 0790 22 13 25 313 LS 7 500 FL 0 000 0 000 RAQL EQ 2000 19 06 22 2515 08 13 49 187 LS 47 000 FL 0 000 0 000 WAQL EQ 2000 19 15 23 3656 07 02 49 766 LS 25 500 FL 0 000 0 000 XCYG EQ 2000 19 50 33 8831 32 54 51 226 LS 8 300 FL 0 000 0 000 RRAQL EQ 2000 19 57 36 7728 01 53 04 855 LS 30 800 FL 0 000 0 000 NMLCYG EQ 2000 20 46 25 5768 40 06 59 381 LS 1 100 FL 0 000 0 000 TCEP EQ 2000 21 09 32 3331 68 29 28 440 LS 3 800 FL 0 000 0 000 To use this source catalog enter at the prompt PAKO gt CATALOG SOURCE demo sou With this command we select the source catalog a special file in which information about the sources is stored The syntax of the parameters in the source catalog is like that for the parameters of the source command see HELP SOURCE Lines starting with a are comments The standard file extension for source catalogs is sou NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names Id demo source pako basic SOURCE EXAMPLES v 1 1 1 2009 05 08 by Hans Ungerechts CATALOG SOURCE demo sou select source catalog SOURCE NGC7027 select source from catalog OFFSETS Clear optional clear previously set offsets PAUSE OTHER WAYS TO SPECIFY A SOURCE SOURC
77. 1039 811 1044 719 1045 188 1055 018 1116 128 1124 186 1144 402 1156 295 1213 172 1226 023 1244 255 EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 2000 03 03 03 03 03 04 04 04 04 04 04 04 04 05 05 05 05 05 05 06 06 06 06 07 07 07 07 07 07 08 08 08 08 08 08 08 08 09 09 09 09 10 10 10 10 10 10 11 11 11 12 03 19 36 39 59 05 18 23 24 28 33 42 57 01 16 22 30 32 55 07 09 46 48 53 19 07 18 36 06 39 15 16 47 50 39 24 48 03 55 249 47 47 16 23 27 06 29 DT 04 58 31 46 06 46 21 30 38 39 48 57 08 08 18 24 25 36 41 54 27 48 56 58 14 37 44 48 48 58 18 27 46 11 12 12 46 59 15 29 35 48 30 30 29 33 21 15 46 40 11 53 03 12 15 Pots 56 38 30 59 40 32
78. 162 AIRMASS 162 DEFAULTS 162 TSUBSCAN 162 TRACK 163 DEFAULTS 163 NSUBSCANS 164 SYSTEM 163 TSUBSCAN 164 EXAMPLES 164 VLBI 165 182
79. 3 13 13 14 14 15 L5 15 15 15 15 16 16 16 16 16 16 17 18 56 10 16 3T 57 15 19 04 07 12 17 49 50 08 13 26 35 38 40 16 16 16 17 17 17 17 dos 17 45 17 18 18 18 18 18 18 18 42 42 58 00 16 33 34 40 43 51 00 01 00 06 24 29 33 42 19 19 19 19 19 19 20 20 20 20 20 20 20 20 21 21 11 24 25 27 55 59 00 01 07 05 15 23 25 38 01 07 d 28 07 39 04 58 46 24 04 50 41 29 35 46 41 06 4848 4457 29 58 07 09 53 13 02 20 36 58 40 32 30 32 45 50 07 2315 39 233 09 51 59 48 42 28 250s 245 44 30 28 19 10 37 38 01 15 13 1688 6573 9949 7841 4305 8108 5784 9752 7876 5321 8190 4326 2658 1974 0330 0237 6235 8001 8336 0340 1591 9209 7019 5664 9634 8510 0313 8104 4267 2950 6222 6518 0480 8047 9093 7085 6517 0545 5932 4595 7230 3546 0848 6989 9340 9646 7151 0066 8256 0188 8275 5931 05 32 33 1 2 19 13 54 10 16 09 24 02 05 10 34 29 38 57 39 39 68 07 26 68 13 38 52 03 29 09 24 44 78 69 56 48 21 68 20 29 21 73 51 40 17 33 40
80. 4 outer subbands of E090 short syntax fine EMIR WILMA 4MHz VESPA 5 NCS USER S GUIDE Ooooo BACKEND WILMA Default BACKEND 4MHz Default BACKEND VESPA 1 0 040 40 0 0 BACKEND VESPA 2 0 040 40 0 0 BACKEND VESPA 3 0 040 40 0 0 BACKEND VESPA 4 0 040 40 0 0 say pause l EMIR VESPA autocorrelator basic 1 backend clear BACKEND VESPA 1 0 040 40 0 120 BACKEND VESPA 2 0 040 40 0 120 BACKEND VESPA 3 0 040 40 0 100 BACKEND VESPA 4 0 040 40 0 110 BACKEND VESPA 5 0 040 80 0 150 BACKEND VESPA 6 0 040 80 0 150 BACKEND VESPA 7 0 040 80 0 200 BACKEND VESPA 8 0 040 80 0 200 pause 11 EMIR VESPA autocorrelator basic 1 backend clear BACKEND VESPA 1 0 320 240 0 O BACKEND VESPA 2 0 320 240 0 O BACKEND VESPA 3 0 320 240 0 O pause NOTE BACKEND VESPA 0 0 0 1 E090 Horiz LI E090 Verti LI E230 Horiz LI E230 Verti LI 1 backends can be combined mode with fShift optional line name E090 E090 E090 E090 E230 E230 Horiz LI line EOHUO M Horiz LI line EOHUO P Verti LI line myLine3 Verti LI line myLine4 Horiz LI line Horiz LI line apple E230 E230 Verti LI line orange Verti LI line red OO ORO o E ae E e AE ae and parallel modes E090 Horiz LI E090 Verti LI E230 Horiz LI mode parallel E230 Horiz LI mode parallel 1 connects one VESPA part in parallel to 1 E230 Horiz LI and E230 Verti LI 1 both must be selected in RECEIVER
81. 6 SWBEAM SWWOBBLER SWFREQUENCY During typical observations different switching modes are used with different observing modes e g for some spectral line project we might use BEAM SWITCHING for POINTING and FOCUS FREQUENCY SWITCHING with TRACK or OTFMAP and TOTAL POWER with ONOFF or OTFMAP The following examples for doing observations contain the specification of an appropriate Switching Mode as well as the Observing Mode For more details on Switching Modes see Section NCS Explained subsection Switching Modes After you enter the setup of a complex switching mode like frequency switching manually we recom mend to save it optionally to a named file SAVE SWITCHING FILE switching 1 The setup can then at any later time be reloaded with switching 1 see HELP SAVE Note that you can also save each switching mode specifically e g SAVE SWFREQUENCY 4 3 5 CALIBRATE Id demo calibrate pako CALIBRATE EXAMPLE v 1 1 5 2011 04 25 Hans Ungerechts CALIBRATE AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for sky offset TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start Comments we assume here that source receivers and backends already have been selected and setup see demo source demo receiver demo backend
82. 6 LI cs 5 4 244 935606 LI HCN 3 2 265 886432 LI HCO 3 2 267 557625 LI To use this line catalog enter at the prompt PAKO gt CATALOG LINE demo EMIR lin Id demo lin v 1 1 1 2009 05 08 Hans Ungerechts 5 NCS USER S GUIDE 55 Line Frequency Band HERA c180 2 1 219 560319 LSB 13C0 2 1 220 398686 LSB CH3CN220 220 747263 LSB CH3CCH222 222 166970 LSB c170 2 1 224 714370 LSB H2C0225 225 697772 LSB 12C0 2 1 230 537990 LSB C348 5 4 241 016176 LSB CS 5 4 244 935606 LSB HCN 3 2 265 886432 LSB HCO 3 2 267 557625 LSB To use this line catalog enter at the prompt PAKO gt CATALOG LINE demo lin With this command we select the line catalog a special file in which information about the spectral lines is stored Each line contains 3 items the name identifier of the line the frequency in GHz and a code for the side band or EMIR sub band NOTES For the EMIR bands we distinguish up to 4 sub bands each of 4 GHz bandwidth e the lower outer sub band LO from about 12 GHz to 8 GHz frequency shift relative to the local oscillator e the lower inner sub band LI from about 8 GHz to 4 GHz e the upper inner sub band UI from about 4 GHz to 8 GHz and e the upper outer sub band UO from about 8 GHz to 12 GHz If we select LO LI UI UO as EMIR sub band in the line catalog or directly in RECEIVER the localoscillator will be adjusted so that the
83. 9 52 10 53 43 19 41 14 33 3b 07 53 241 23 57 16 245 29 35 57 243 28 06 08 49 01 58 28 13 00 15 53 11 32 23 57 43 43 59 02 00 12 31 38 38 40 38 30 36 01 50 57 51 648 545 312 316 085 53 21 10 50 421 04 412 24 29 698 214 845 499 24 456 842 164 572 547 518 622 294 640 395 265 687 381 10 540 22 04 17 54 36 183 192 725 163 319 108 710 073 359 054 837 271 985 525 110 LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR LSR NOTE MIRA does not yet support pointing on Si0 masers if the receiver is tuned to the Si0 line OCET SPER NMLTAU IRC 50137 ORIA UORI EQ EQ EQ EQ EQ EQ 2000 2000 2000 2000 2000 2000 02 02 03 05 05 05 19 22 53 11 35 55 20 51 28 19 14 49 7066 7287 8025 7492 4740 2761 02 58 11 52 05 20 58 35 24 52 22 10 36 095 7113 689 30 768 12 20 27 30 165 157 LS LS LS LS LS LS 46 38 33 16 40 O O ORO OM OM OOM Ome OO OO OO OO OO OOO OOO OO OOOO OR OM OM OM OO Oe 000 000 000 000 000 000 000 000 000 000
84. BE ee EP OR BAD Ea Se ee BY 166 For OPTIONS AIRMASS e ec pura eee Pe be Peer a eee RES ESS 166 272 OPTIONS AMBIENT ooo we oe eke wa eee Gee ae aw os 167 T210 OF TIONS APPEND po eae eae es oa ee OE ee A Sa 167 tA OPTIONS CLEAN cosa oe oe BO ES dee A ws 167 IO OPTIONS GOLD serp he eh eee eee EOL ae BERR EES 167 7 27 6 OPTIONS CONNBDOT sv eee ewe BES ER SRS Be ee araa 167 tard OPTIONS CROLOOP cesos Re ke RE SA ee AA 167 1278 OPTIONS DEFAUTES 2 4 we be dee oe ORE Be OR ee a 168 fore OPTIONS DEROTATOR 2 8 82254 682462544862 64 484454 168 7 27 LOOPTIONS DISCONNELT 2 score aeaii tees bi bbe eee tees 168 LA LIL OPTIONS DOPPLER sc eoe diod ca tamara pated ig eeeua 168 7 27 12 OPTIONS DOUBLEBEAM 2 4 445428 244 See Se aa ee ed 168 TITAISOPTIONS EFFICIENCY 22665 sca eh eS Cae ed eee ee ee 169 oe aOR TIONS PURE e ae ae ep ed BA ee ORS RES Kee eee 169 T2 A5 OPTIONS FINE soma ara RS ORR SKE e EAE ERs 169 fe IGOPTIONS GAINIMAGBE og ba Ye wee Ree ee es ee E Re 169 Got OPTIONS IS a eh ee ee BR eR 170 TIS OPTIONS PORTE oo cat dd ee Ee ES ERS 170 7 2119 OPTIONS JRORIZAUNTAL pora bee se pee ee Eee ES 170 T2 0 OPTIONS MODE cs oa ee OO Sh eS EE Sm 171 Te 2LOV TIONG NOP o eiei ae oe ew ee OO Ee dew deta w Bs 171 7 21 22 OPTIONS NSUBSCANS ook eo Shoe Ree ERR BE RE EE ek 171 7 21 23 OPTIONS PERCENTAGE 2 hehe a eee be eb a ee eee 171 72T A OPTIONS RECEIVER 5 a 6 Pe ke ROH RA AA 172 12 23 OPTIONS REFERENCE 26424446 eR ERR R
85. Book already provided a good part of the information in the NCS User s Guide Here we provide more details and more elaborate examples in the form of PAKO scripts that can be edited and used for actual observations This section starts with some general commands and the selection of a source catalog The next subsection explains how to do Spectral Line Observations with Heterodyne Receivers Remember that in command language scripts based on SIC starts a comment indicates that a command is continued on the next line PAUSE pauses the execution of the script e g in order to allow the user to review the parameters set RETURN ends the execution of the script and returns to the level from which the script was called you have to delete or comment RETURN in order to execute the rest of the script Generally the case UPPER lower or Mixed doesn t matter To execute a script in a file named yoda pako enter at the prompt PAKO gt yoda 5 1 Set General Information Id demo set pako basic SET EXAMPLES v 1 1 1 2009 05 18 Hans Ungerechts SIC PRIORITY 1 PAKO PAKO commands get precedence over similar GREG commans SET Project 111 22 project ID project number SET PI Dr Lilo D Doe principal investigator SET Observer John Doe SET Operator Pako SET Topology low topology for azimuth SET Level 3 3 suppress informational messages I messages from paKo DEVICE image
86. CE must match those of a source name in the source catalog or a name of a special source like a planet However the case of the source name is ignored for matching For example W30H woh W3oh all match W30H in the source catalog Mars Mars and mars all are recognized as the planet Mars however W30 does not match W30H 4 3 Spectral Line Observations with Heterodyne Receivers 4 3 1 Specify your Line Catalog A line catalog is a special file containing information about spectral lines to be observed in particular their frequencies The line catalog can be prepared with any text editor Here is an example Id demo EMIR lin v 1 1 1 2009 05 06 Hans Ungerechts this is a special version for EMIR using sub bands LI UI and UO Line Frequency EMIR sub band E090 CH30H 84 52121 LI OCS 7 6 85 139108 LI SIO V1 86 243350 LI H13CN 86 342274 LI H13C0 86 754330 LI SIO VO 86 846891 LI HCN 1 0 88 6316024 LI HCO 1 0 89 188523 LI HNC 1 0 90 663574 LI HC3N 10 9 90 9789933 LI C348 2 1 96 412982 LI 4 PAKO S COOK BOOK OCS 8 7 CS 2 1 HC3N 11 10 34802 13C180 1 0 C180 1 0 13C0 1 0 C170 1 0 CN F1 1 0 12C0 1 0 E150 HC3N 15 14 C348 3 2 H2C0 146 CS 3 2 E230 c180 2 1 13C0 2 1 CH3CN220 CH3CCH222 c170 2 1 H2C0225 12C0 2 1 C348 5 4 CS 5 4 HCN 3 2 HCO 3 2
87. CHING is very powerful and efficient for some projects e g mapping of narrow spectral lines in cold dark clouds outside the plane of the Milky Way However before deciding to use frequency switching one should consider some potential drawbacks The target lines should be narrow enough so that line signals from the 2 phases of the switching cycle are well separated The spectral baseline will generally be less flat than in other switching modes Some spectral lines are also emitted in the earth s mesosphere e g the mesopheric lines from 12 CO are rather strong and they will be seen in FREQUENCY SWITCHING spectra taken toward astronomical 5 NCS USER S GUIDE 71 sources with a low Doppler shift The mesospheric lines will appear at a frequency and velocity that corresponds to the rest frame of the athmosphere i e the observatory Care must be taken that they are not confused with the lines from the astronomical source Information computed by the ASTRO software can help with this decision When observing sources near the plane of the Milky Way line emission from clouds at other velocities than the target source e g other spiral arms can cause confusion In case of doubt consult the special memo on FREQUENCY SWITCHING or ask an experienced FRE QUENCY SWITCHING observer 5 3 8 ON OFF Position Switching and Wobbler ON OFF Id demo onoff pako ONOFF SWIOTAL EXAMPLE v 1 1 1 2009 05 05 Hans Ungerechts POSITION SWITCHING
88. E CALORI catalog lines J2000 select source from another catalog PAUSE SOURCE OCET EQ J2000 02 19 20 71 02 58 36 17 LSR 46 800 command line specification of source PAUSE SOURCE Mars planet Mars PAUSE SOURCE Moon our Moon PAUSE SOURCE Io Jupiter s satellite Io PAUSE 4 PAKO S COOK BOOK 28 SOURCE Body Pako 2455000 0 22 2 33 3 44 4 55 5 0 66 solar system body orbital elements PAUSE SOURCE w3oh will match W30H in demo sou NOTES source names must match 11 full source name in catalog or 1 full name of planet or satellite 1 the case is ignored for source name matching RETURN We use the command SOURCE to select a source for observations Normally it is used after CATALOG SOURCE to select one of the sources from the source catalog Alternatively the parameters of the source can be specified directly on the command line using the same format as in the source catalog Pluto the planets and some of their Satellites are recognized directly by their name NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names For a full explanation of the parameters of the source command see HELP SOURCE Notes IMPORTANT All characters of the source name in the command SOUR
89. E230 SWFREQUENCY tphase 0 20 same for all receivers bands CALIBRATE AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for offset TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start OTFMAP 300 300 300 300 offsets at start and end of first OTF CROLOOP 0 only OTF subscans NOTF 4 number of on the fly subscans REFERENCE no no off source reference subscans STEP 0 10 step shift between OTF subscans SYSTEM projection system for offset TOTF 120 0 time per on the fly subscan ZIGZAG go back and forth 4 PAKO S COOK BOOK 45 PAUSE OTFMAP SWFREQUENCY OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source 4 4 Continuum Observations with Bolometers NOTES Most bolometer observations are done in the bolometer observing pool which has its own special in structions Observers in the bolometer pool should follow these special instructions NOTE 2011 07 14 the MAMBO bolometers are out of operation For other notes on bolometer observations see section 5 4 5 NCS USER S GUIDE 46 5 NCS User s Guide This section contains an extended guide explaining how to setup and execute observations Also note that an earlier section Pako s Cook
90. EED SPEED speedi speed2 speed of OTF subscans Real speedl speed at start Real speed2 speed at end For OTFMAP speed2 speedl In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 11 7 OTFMAP SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION 7 PAKO LANGUAGE INTERNAL HELP 129 TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM
91. H wide backend clear BACKEND FTS 1 RECEIVER HERA1 BACKEND FTS 2 RECEIVER HERA2 HERA narrow bandwidth with FTS fine resolution receiver clear RECEIVER HERA1 WIDTH narrow RECEIVER HERA2 WIDTH narrow backend clear BACKEND FTS 1 FINE RECEIVER HERA1 BACKEND FTS 2 FINE RECEIVER HERA2 The command BACKEND has up to 8 parameters backend name logical part number resolution MHz bandwidth MHz frequency shift MHz receiver band EMIR polarization and EMIR sub band The receiver band and subbands must have been previously selected with RECEIVER For some backends the resolution bandwidth and or frequency shift are fixed and a shorter syntax is possible See the HELP BACKEND for complete information CLEAR completely clears the backend setup Normally the continuum backends are used only for POINTING FOCUS and TIP antenna tipping or skydip For VESPA only a selected few possibilites are shown for more information see the VESPA user s guide After you enter a backend setup manually we recommend to save it optionally to a named file SAVE BACKEND FILE backend 1 It can then at any later time be reloaded with backend 1 see HELP SAVE 4 3 4 Switching Mode Always specify one of the Switching Modes TOTAL POWER BEAM SWITCHING WOBBLER SWITCHING FREQUENCY SWITCHING before an Observing Mode The corresponding commands are SWTOTAL 4 PAKO S COOK BOOK 3
92. HIGH Az 100 460 460 420 ae Control room Control room Figure 4 Azimuth Topology The left side shows in blue the range for SET TOPOLOGY LOW the right side shows in red the range for SET TOPOLOGY HIGH Compare Section 6 2 figure prepared by Joaquin Santiago The 4 switching modes are mutually exclusive i e at any time the system uses only one of them During the transitions between phases e g while the Wobbler is moving between its positions no data are taken during the short blanking time The switching mode and its parameters should normally be set before choosing an observing mode because for some observing modes details of the setup depend on the switching mode Id demo switching pako v 1 1 1 2009 05 05 Hans Ungerechts SWTOTAL tphase 0 2 Total Power PAUSE SWBEAM Beam Switching PAUSE SWFREQUENCY default Frequency Switching PAUSE SWFREQUENCY 3 3 3 3 for all RXs PAUSE SWFREQUENCY 3 9 3 9 receiver E090 select frequency switching SWFREQUENCY 11 7 11 7 receiver E230 for EMIR band E230 SWFREQUENCY tphase 0 20 same for all receivers PAUSE SWWOBBLER 22 22 tphase 0 25 Wobbler Switching 6 NCS EXPLAINED 85 PAUSE NOTE 1 after changing the switching modes always re execute a command 1 for an observing mode because internal parameters and error checks 1 of the observing modes depend on the switching mode 6 3 1 Beam Swit
93. K to start c ql START To execute this script simply enter demo bolometer otfmap 80 no off source reference subscans step shift between OTF subscans system for offset true horizon offsets time per on the fly subscan s go back and forth a chance to check start For bolometer observations OTFMAP is used with WOBBLER SWITCHING command SWWOBBLER In OTFMAP on the fly observations the antenna moves relative to the source while recording its position and taking data a high rate This is a very fast mode for mapping extended regions The basic parameters of the command are the position offsets of the start and end of the first OTF subscan the basic parameters of the options are the number OTF subscans the step shift in x and y offsets between subsequent OTF subscans the time per OTF subscan in s This mode is normally used with WOBBLER SWITCHING and the true horizon system for continuum mapping with the bolometer 6 NCS EXPLAINED 81 6 NCS Explained In this section we explain in more detail some general aspects of the NCS 6 1 Coordinate Systems Map Projections and Position Offsets The NCS will support a variety of astronomical coordinate systems and projections as well as descriptive coordinate systems defined by the user Up to now 2012 12 01 only equatorial coordinates J2000 0 are well tested and available for use Map Projections and Offsets In general a map pro
94. M Nasmyth are specified in pako the values xOffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 11 1 OTFMAP DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 11 2 OTFMAP CROLOOP CROLOOP croLoop sequence of R off source Reference 0 On source subscans Character croLoop Example croLoop ROOR 7 11 3 OTFMAP NOTF NOTF nOtf 7 PAKO LANGUAGE INTERNAL HELP 128 Integer nOtf number of OTF on the fly subscans 7 11 4 OTFMAP REFERENCE REFERENCE xOffsetR yOffsetR systemNameRef or REFERENCE NO no reference position of off source reference subscans Real xOffsetR x offset Real yOffsetR y offset Character systemNameRef name of system see SYSTEM for choices NOTE with the usage REFERENCE xOffsetR yOffsetR both parameters are requi but you can replace either parameter with to leave it unchanged 7 11 5 OTFMAP STEP STEP dx dy Step shift or translation between lines in a map Real dx shift in x offsets Real dy shift in y offsets 7 11 6 OTFMAP SP
95. MIR bands we distinguish up to 4 sub bands each of 4 GHz bandwidth e the lower outer sub band LO from about 12 GHz to 8 GHz frequency shift relative to the local oscillator e the lower inner sub band LI from about 8 GHz to 4 GHz e the upper inner sub band UI from about 4 GHz to 8 GHz and e the upper outer sub band UO from about 8 GHz to 12 GHz If we select LO LI UI UO as EMIR sub band in the line catalog or directly in RECEIVER the localoscillator will be adjusted so that the specified line frequency goes into that EMIR sub band For details see the EMIR user guide For HERA the sideband must be LSB lower sideband NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names One RECEIVER command is needed for each receiver EMIR band or part of HERA After the receiver is set up and a source has been selected the observer should enter CALIBRATE SKY no START to send the receiver parameters to the NCS The telescope operator or receiver engineer will then tune the receiver HORIZONTAL sbi sb2 and VERTICAL sb1 sb2 apply only to EMIR This option informs the system about which EMIR subbands are going to be used for the horizontal and vertical polarization about the EMIR s
96. N OFF instead 5 4 Continuum Observations with Bolometers NOTES This subsection is preliminary Most bolometer observations are done in the bolometer observing pool which has its own special in structions Observers in the bolometer pool should follow these special instructions NOTE 2011 07 14 the MAMBO bolometers are out of operation 5 4 1 Setup of the Bolometer Id demo bolometer pako 0 9 2005 09 07 by Hans Ungerechts RECEIVER CLEAR completely clear receiver setup RECEIVER BOLOMETER MAMBO2 1 55 gainBolometer 1 channel 55 BACKEND DISCONNECT disconnect all backends previously set bolometer does not need spec of a backend To execute this script simply enter demo bolometer The setup command for a bolometer has only 3 parameters a name identifier for each bolometer the bolometer gain a numerical factor and a number to select one specific bolometer channel pixel that will be centered on the selected source for POINTING FOCUS and ONOFF 5 4 2 Switching Mode Always specify a Switching Mode before an Observing Mode Bolometer observation normally use WOBBLER SWITCHING for almost all observations however TIP must be done with TOTAL POWER The corresponding commands are SWTOTAL SWWOBBLER The following examples for doing observations contain the specification of an appropriate Switching Mode as well as the Observing Mode For more details on Switching Modes see Section
97. NTING specify a pointing measurement TIP specify an antenna tipping a k a skydip TRACK specify tracking of a single position e g with SWFRE ONOFF specify on off a k a position switching OTFMAP specify an On The Fly OTF map LISSAJOUS specify an On The Fly map along a Lissajous curve VLBI specify tracking of a single position for VLBI 7 PAKO LANGUAGE INTERNAL HELP 92 start START start an observation i e send it to the queue save SAVE save parameters to file i e a pako script 7 1 1 Language NEWS paKo v1 1 14 2012 14 NEW in 1 1 14 RECEIVER BOLOMETER NIKA Receiver bolometer NIKA SUBSCAN x0ffset yOffset TUNE for NIKA DIY PURPOSE play my Tune for NIKA NEW in 1 1 12 RECEIVER BOLOMETER GISMO Receiver bolometer GISMO LISSAJOUS Observing Mode Lissajous for GISMO i e an On The Fly map along a Lissajous curve UPDATED in 1 1 11 RECEIVER EMIR Receiver EMIR upgrade of E230 and E330 BACKEND FTS Fourier Transform Spectrometer BACKEND BBC Broad Band Continuum Backend SET EMIRcheck limit checking for EMIR SET UserLevel pako v1 1 6 UPDATED in v1 1 6 BACKEND FTS Fourier Transform Spectrometer 7 PAKO LANGUAGE INTERNAL HELP NEW in vi 1 5 BACKEND BBC Broad Band Continuum Backend BACKEND NBC Narrow Band Continuum Backend NEW in v1 1 4 BACKEND FTS Fourier Transform Spectrometer SET EMIRCheck strict relaxed loose pako v1 1 1 NEW in
98. ON position parameters of the options are the offsets for the reference position the total number of subscans and the time per subscan in s After you enter an ON OFF setup manually we recommend to save it optionally to a named file SAVE ONOFF FILE onoff 1 It can then at any later time be reloaded with onoff 1 see HELP SAVE You may want to save the switching mode seperately or with ONOFF into the same file SAVE SWITCHING FILE onoff 2 SAVE ONOFF FILE onoff 2 APPEND Id demo onoff swwobbler pako ONOFF SWWOBBLER EXAMPLE v 1 1 6 2011 07 31 Hans Ungerechts WOBBLER SWITCHING demo rx spectrometers demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP SET ANGLE arcsec select wobbler switching SWWOBBLER 120 0 120 0 wobbler 120 arc sec TPHASE 1 0 1 seconds per phase CALIBRATE il AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start 1 OPTIONAL 4 PAKO S COOK BOOK 42 OFFSETS 20 30 mapping offsets in SYSTEM projection system projection ONOFF SWWOBBLER NSUBSCANS 12 ONOFF for Wobbler switching number of subscans SYMMETRIC z symmetric subscan sequence TSUBSCAN 30 time per subscan
99. ONOFF xOffset is set to w0ffset1 yOffset is set to 0 0 REFERENCE is set to Yes xOffsetR is set to w0ffset2 yOffsetR is set to 0 0 7 PAKO LANGUAGE INTERNAL HELP 174 systemNameRef is set to TRUEHORIZON SYSTEM systemName is set to TRUEHORIZON NOTE in this case the values selected by SWWOBBLER overrule the corresponding values specified directly in the command NOTE To do ONOFF with Wobbler switching and other unconventional values for the parameters listed above simply specify the values using command ONOFF with option SWWOBBLER NO not recommended NOTE If the selected switching mode is SWWOBBLER and if the option SWWOBBLER is no explicitly given it will be assumed to be True Yes If the selected switching mode is not SWWOBBLER and if the option SWWOBBLER is no explicitly given it will be assumed to be False No 7 27 31 OPTIONS SYMMETRIC SYMMETRIC yes no Logical doSymmetric default no For ONOFF select a subscan sequence that is symmetric in time This requires that the number of subscans is a multiple of 4 Example for ONOFF with SYMMETRIC no SYMMETRIC yes 1st subscan OFF OFF 2nd ON ON 3rd OFF ON 4th ON OFF and so on NOTE that this does not in anyway change the positions of the ON source and OFF source subscans 7 27 32 OPTIONS SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHO
100. P RAMP None RAMP Up tRampUp lt lt TBD RAMP Down tRampDown not yet implemented gt gt 7 PAKO LANGUAGE INTERNAL HELP 156 Real tRamp minimal time for ramp RAMP Up tRamp RAMP Up must be used for Lissajous subscans At the start of a Lissajous subscan paKo will insert a ramp along a straight line i e a linear OTF segment increasing the count of segments by 2 This ramp up starts with speed 0 relative to the source and joins smoothly with the start position and velocity of the Lissajous segment The purpose is to avoid a sudden aceleration at the start of the Lissajous segment Command DIY lists this inserted OTF segment as well as the Lisssajous segment The inserted ramp up segment and the Lissajous segment become part of the same subscan Example SUBSCAN 100 200 0 01 0 02 10 20 0 1 0 2 ramp up 9 Lissajous subscan with a ramp up of at least 9 sec 7 19 3 SUBSCAN SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset This is the system in which OTF maps with Wobbler switching an
101. P SPEED 24444 raap castas ORS ees Hee a 128 TAL OOTP MAP SYSTEM gk ss cee eye ec db es one eke e est Geen 128 TUE OTFMAF PEG ege oe hg Pe ek oe Be ee eS ee E Ra 129 7119 OTR MAP TREFEREN E ce Paw ee oe ee ee Be Ree 130 ILIOO TEMA ZIGZAG heed te DRED Eee a ee ES ERS 130 TILITOTFMAP EXAMPLES lt lt rica a e Bee ee SY Be 130 POINTING 2 5 5 4 8 be dG a Se AE oe Ee Ba Pe a eS SSS we ee 132 7 121 POINTING DEFAULTS 24 108 2444 4 89 28445 a a ws 132 112 2 POINTING DOUBLEBEAM 5 5228285444 8 Sb bee EO we 132 7 12 3 POINTING NOTE e pc krek eee ewe BE Ee DHS Be ee hae 133 T124 POINTING TOTP ogs peera Oe a RE RA ee wR BO 133 112 POINTING EXAMPLES p06 corporea dge ea ER eB EE 133 RECEIVER ENE 134 7 131 RECEIVER DEFAULTS 4 24064 oe4 8 44h b 052 84 5454 136 T132 RECEIVER CLEAR 252 ices caged eee die de eee ees 136 113 3 RECEIVER CONNECT occa 54442 iaa be bee eee 136 2134 RECEIVER DEROTATOR soc scene daa ea 0 4 136 7 13 5 RECEIVER DISCONNECT 22 055 lt lt 405 res ense 136 7136 RECEIVER DOPPLER 3 00 lt 53 lt 0 67 4 ee 434 ehh OP os 137 2127 RECEIVER EFFIGIENOY cos ba be ee kee ee ee ee E Re 137 713 8 RECEIVER GAINIMAGE cosas ARA Pee Ree 137 1139 RECEIVER HORIZONTAL coccion a a 137 7 1310 RECEIVER SCALE e scu bo oa eee EERE e eee he ees 138 7 13 11RECEIVER TEMPLOAD 2064424 48a x pee bees oe Ga ds 138 7 13 12 RECEIVER VERTICAL o ce sos ser aiaa aa ee ks 139 TISI RECEIVER WIDIH se ei cora pa Se
102. Phase 22 44 0 25 sec 522s 44 1 0 sec 120 240 1 0 sec 120 240 2 0 sec Note that for OTFMAPs with Wobbler switching special restoration algorithms are needed to recover an image of the source brightness distribution These are available e g in the MOPSIC software If SWWOBBLER and ONOFF are combined in the standard way we effectively take data at 3 positions 1 the source position 2 the source position throw offset in the true angle horizontal syste 3 the source position throw offset in the true angle horizontal syste with throw ABS wOffset2 wO0ffset1 Data from 1 are treated as source signal data from 2 and 3 as off source reference signal Note that in the astronomical coordinates positions 2 and 3 will rotate around the source position 1 Therefore one must normally be sure that the extent of the source is less than throw beamWidth 2 7 23 1 SWWOBBLER DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 23 2 SWWOBBLER TPHASE TPHASE tPhase time per switching PHASE Real tPhase time 7 PAKO LANGUAGE INTERNAL HELP 162 7 24 TIP TIP azimuth Specify an antenna tipping a k a skydip Real azimuth azimuth of tip If azimuth is not specified the current azimuth of the telescope is used NOTE TIP is always and automatically done with switching mode total power and for bolometer observations the time per phase is fixed
103. Pi frequencyY t phiY SIN is the usual sine function Pi is the number Pi xAmplitude yAmplitude xCenter yCenter are in angle units arc sec frequencyX frequencyY are in Hz phiX phiY are in rad Note that the possible frequencies are very low typically 0 01 to 0 15 Hz At the start of a Lissajous subscan paKo will insert a ramp along a straight line i e a linear OTF segment increasing the count of segments by 2 This ramp up starts with speed 0 relative to the source and joins smoothly with the start position and velocity of the Lissajous segment The purpose is to avoid a sudden aceleration at the start of the Lissajous segment Command DIY lists this inserted OTF segment as well as the Lisssajous segment The inserted ramp up segment and the Lissajous segment become part of the same subscan Lissajous curves with large amplitudes or frequencies can reach the antenna s speed and acceleration limits for tracking Lissajous curves can be executed only for elevations less than a maximum which depends on the Lissajous parameters For information this elevation condition is shown by pako Even below the limits during very fast Lissajous curves the tracking errors will be higher several arc sec than during most other observations DO NOT TRY TO OBSERVE LISSAJOUS ABOVE THIS MAXIMUM ELEVATION 7 19 1 SUBSCAN CROFLAG CROFLAG croCode Character croCode R off source Reference 0 On source 7 19 2 SUBSCAN RAM
104. R not yet implemented gt gt TRACK VLBI All Observing Modes are realized by executing a sequence of 1 or more subscans In most cases the antenna moves between or during the subscans The observing modes are mutually exclusive i e at any time the system executes only one of them Several Observing Modes can be combined with different Switching Modes e g OTFMAP with TOTAL POWER WOBBLER SWITCHING for bolometer or FREQUENCY SWITCHING The Switching Mode should normally be specified before the Observing Mode 2 PAKO GUIDE OF THE PERPLEXED 14 2 11 Combinations of Switching and Observing Modes The Switching modes and Observing modes are not fundamentally different from what they were in the old CS However in the NCS we try to be more explicit about this distinction in order to i avoid having several commands that set up e g parameters of the Wobbler ii to support more combinations of Observing Modes and Switching Modes in the future 2 12 Coordinate Systems Map Projections and Position Offsets For a more detailed explanation see Section 6 1 The NCS will support a variety of astronomical coordinate systems and projections as well as descriptive coordinate systems defined by the user Up to now 2012 12 01 only equatorial coordinates J2000 0 are well tested and available for use Map Projections and Offsets In general a map projection describes the relation between 2 spherical coordinates longi
105. REQUENCY tphase 0 20 same for all receivers bands 7 PAKO LANGUAGE INTERNAL HELP 160 setup frequency switching SWFREQUENCY 3 7 receiver E090 fOffset2 will be 3 7 SWFREQUENCY 11 6 receiver E230 f0ffset2 will be 11 6 7 22 SWTOTAL SWIOTAL no parameters Select total power i e neither beam frequency nor wobbler switching Typically used with OTFMAP with off source references or ONOFF position switching 7 22 1 SWTOTAL DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 22 2 SWTOTAL TPHASE TPHASE tPhase time per switching PHASE Real tPhase time 7 23 SWWOBBLER SWWOBBLER wOffset1 wOffset2 Select and set up wobbler switching using the wobbling secondary mirror to switch between 2 positions on the sky This is typically used with the observing modes POINTING FOCUS ONOFF or with the bolometer OTFMAP Real wOffseti ist wobbler offset 1 2 throw Real WOffset2 2nd wobbler offset wOffseti IMPORTANT NOTE Observers must inform the operator if they want to use this feature 7 PAKO LANGUAGE INTERNAL HELP 161 There is a relation between the maximum allowed Wobbler throw and the minimum time per phase for large throws the switching must be slow i e time per phase must be large For timePhase 1 sec or longer any wobbler throw is allowed up to the maximum of 240 Posssible combinations are e g wOffset1 throw time
106. RIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt 7 PAKO LANGUAGE INTERNAL HELP 175 PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0f
107. RTANT NOTES sourceName is limited to 12 characters So far only Equatorial J2000 0 coordinates are well tested lt lt TBD Observations of the Sun and near the Sun are not yet supported gt gt 7 PAKO LANGUAGE INTERNAL HELP 149 NB Don t use amp lt gt in names of sources lines projects PI observer operator etc Don t use in source names IMPORTANT NOTE ON VELOCITY One should not use very large Doppler velocities thousands of kilome ters to achieve red shift corrections of frequencies Instead one should enter the red shifted frequencies in the line catalog or with the RECEIVER command and use Doppler velocity of 0 0 The alternative approach with very large Doppler velocities needs spe cial methods and attention in the data processing which are not im plemented in CLASS because it is better to observe in such a way that minimum modification to the data is done later on J Pety For a full discussion of this question see Gordon et al 1992 A amp A 264 337 in Sect 6 The second form accepts 6 Real arguments to specify the orbital elements of a solar system body Body special keyword exactly like this Real perihelionEpoch Julian Date d Real ascendingNode deg Real argumentOfPerihelion deg Real inclination deg Real perihelionDistance deg Real eccentricity If only sourceName is specified we try to read the other parameters from the s
108. S FTS FTS ONOOTFRWNK clear Default Default Default Receiver E090 Horiz LI Receiver E230 Verti LI Default Receiver Receiver Receiver Receiver Receiver Receiver Receiver Receiver E090 E090 E230 E230 E090 E230 E090 E230 hor ver hor ver ver ver hor hor LI LI LI LI LO LO LO LO 103 of each sideband of each selected EMIR band EMIR NBC connect 1 part to each selected EMIR subband EMIR WILMA connect 1 part to each selected EMIR subband EMIR 4MHz NOTE 4MHz has only 2 parts with EMIR connect 1 part to each of the first 2 EMIR subbands connect 1 part to E090 Ho LI 2nd part to E230 Ve LI EMIR FTS wide bandwidth mode Fine is NOT present connect 1 part to each selected EMIR subband plus 1 part to each of the 4 outer subbands of E090 short syntax still wide EMIR FTS fine resolution because Fine is present 7 PAKO LANGUAGE INTERNAL HELP BACKEND pause backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 1 1 backend BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND say pause 11 EMIR backend BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND pause 11 EMIR backend BACKEND BACKEND BACKEND pause 11 NOTE FTS Fine Default clear FTS 1 Fine Receiver E090 hor FTS 2 Fine Receiver E090 ver FTS 3 Fine Receiver E230
109. S USER S GUIDE say E090 H UO V LO for FTS pause Vit say 1 NOTE E090 E230 H V UI 4 U0 receiver clear REC E090 12C0 1 0 115 271204 UO Hor UI Ver UI REC E230 12C0 2 1 230 537990 UI Horizontal UI Vertical UI line on UO UI on one of IF cables 1 to 4 line UO on one of cables 5 to 8 say NOTE E090 H V UI 4 GHz BW say JE E090 H V UO for FTS say j E230 H V UI 4 GHz BW say a E230 H V UO for FTS pause say 1 NOTE E090 E230 H V LI 4 LO receiver clear RECEIVER E090 HCN 1 0 Hor LI Ver LI RECEIVER E230 13C0 2 1 Horizontal LI Vertical LI say m NOTE E090 H V LI 4 GHz BW say A E090 H V LO for FTS say E230 H V LI 4 GHz BW say yy E230 H V LO for FTS pause say NOTE E090 V UO 7 say I E230 H LI UI V UI receiver clear REC E090 12C0 1 0 115 271204 UO Hor none Ver uo REC E230 12C0 2 1 230 537990 UI Horizontal LI UI line on UO line UO on one of cables 1 to 4 Vertical UI say NOTE E090 V U0 y say E230 H LI UI V UI m say n E230 H LO U0 V UO for FTS pause say 1 NOTE E090 V UI say R E230 H LI UI il receiver clear REC E090 CS 2 1 97 980965 UI Hor none Ver UI REC E230 12C0 2 1 230 537990 UI 5 NCS USER S GUIDE say say say say pause l say receiver clear RECEIVER E090 RECEIVER E230 say say say say pause Hit say receiver
110. SMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection 7 PAKO LANGUAGE INTERNAL HELP 120 OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 10 1 ONOFF DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 10 2 ONOFF NSUBSCANS NSUBSCANS nSubscans Integer nSubscans number of subscans 7 10 3 ONOFF REFERENCE REFERENCE xOffsetR yOffsetR systemNameRef or REFERENCE NO no reference position of off source reference subscans Real
111. START OTFMAP 300 15 300 15 CROLOOP ROR NOTF 4 REFERENCE 500 400 projection demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP to select total power time per phase data sample ambient load cold load sky at offsets 500 0 400 0 system for SKY offset time per calibration subscan a Chance to check start offsets at start and end of f subscans reference OTF refer number of on the fly subscans offsets of off source referen 130 7 PAKO LANGUAGE INTERNAL HELP STEP 0 10 SYSTEM projection 1 TOTF 120 0 1 TREFERENCE 20 0 1 ZIGZAG PAUSE OTFMAP SWTOTAL OK to start c q Comments we assume here that the source already has see demo source CROLOOP ROR means that there will be subscan sequence will be Id demo otfmap swfrequency pako demo rx BACKEND CLEAR BACKEND VESPA 1 0 040 40 BACKEND VESPA 2 0 040 40 BACKEND VESPA 3 0 080 80 230 hor LI BACKEND VESPA 4 0 080 80 230 ver LI 090 ver LI oooo oooo oooo ta 1 SET ANGLE arcsec 1 SWFREQUENCY 3 9 3 9 receiver E090 SWFREQUENCY 11 7 11 7 receiver E230 SWFREQUENCY tphase 0 20 1 CALIBRATE AMBIENT COLD SKY 600 0 0 0 SYSTEM projection TCALIBRATE 5 0 PAUSE CALIBRATE OK to start c q START 131 step shift between OTF subs system for offsets time per on the fly subscan time per off source reference go back
112. T TRACK 40 0 30 0 NSUBSCANS 5 SYSTEM projection TSUBSCAN 60 PAUSE TRACK SWFREQUENCY OK to start c q START Comments 090 hor LI 090 ver LI 230 hor LI 230 ver LI receiver E090 receiver E230 0 20 we assume here that the source already has see demo source TRACK EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo setup of receivers clear previous backends high spectral resolution with VESPA REPLACE WITH YOUR SETUP setup frequency switching for EMIR band E090 for EMIR band E230 same for all receivers bands ambient load cold load sky at offsets 600 0 0 0 system for SKY offsets time per calibration subscan a chance to check start offsets of on position number of subscans system for offset time per subscan a chance to check start been selected The TRACK observing mode simply tracks one position relative to the source It is normally used with FREQUENCY SWITCHING and offsets in SYSTEM projection The basic parameters are the offsets for the position to track parameters of the options are the total number of subscans and the time per subscan in s After you enter a track setup manually we recommend to save it optionally to a named file SAVE TRACK FILE track 1 4 PAKO S COOK BOOK 40 It can then at any later time be reloaded with track 1 see HELP SAVE You may want to save the switching mode seperately or with TRACK into the same file
113. TURN OPTION ON TRUE YES T OTFMAP ZIGZAG YES TURN OPTION ON TRUE YES T OTFMAP ZIGZAG TRUE TURN OPTION ON TRUE YES T OTFMAP ZIGZAG NO TURN OPTION OFF FALSE NO F OTFMAP ZIGZAG FALSE TURN OPTION OFF FALSE NO F Note the default value for some logical options e g ZIGZAG is T for other logical options the default is F 2 PAKO GUIDE OF THE PERPLEXED 20 2 23 Example Scripts and Catalogs Examples of PAKO scripts source and line catalogs are available on the WWW and in each project account 3 PAKO S SIMPLEST RECIPE 21 3 PaKo s simplest recipe This section gives a very short and simple overview of the steps needed to start spectral line observations Details and more explanations are in the following sections also in user s guides for special topics The following simple example is for both polarizations of one sub band LI or UO of one band E090 of the EMIR receiver see the EMIR user s guide for more information e Prepare a source catalog file e g my sou with one line for each source that looks like W30H EQ 2000 02 27 03 8812 61 52 24 572 LSR 45 000 e Prepare a line catalog file e g my lin with one text line for each line frequency like CS 2 1 97 980968 LI 12C0 1 0 115 271204 UO LI and LO refer to sub bands of the EMIR E090 band See the EMIR user s guide for details e Start up PAKO see local information how to do this e Enter some general options and infor
114. URCE SOURCE CALORI catalog lines J2000 select source from another catalog PAUSE SOURCE OCET EQ J2000 02 19 20 71 02 58 36 17 LSR 46 800 command line specification of sour PAUSE SOURCE Mars planet Mars PAUSE SOURCE Moon our Moon PAUSE SOURCE Io Jupiter s satellite Io PAUSE SOURCE Body Pako 2455000 0 22 2 33 3 44 4 55 5 0 66 solar system body orbital element 7 PAKO LANGUAGE INTERNAL HELP 153 PAUSE SOURCE w3oh will match W30H in demo sou 1 NOTES source names must match 1 full source name in catalog or 1 full name of planet or satellite 11 the case is ignored for source name matching RETURN 7 18 START START Start an observation i e translate its specification to XML and submit it to the observing queue Observing jobs are sent to the observing queue only if the observer has SET DOSUBMIT YES in paKo see command SET DOSUBMIT and if the operator has selected the current project to be the current observing queue IMPORTANT NOTE to avoid any possible confusion in each project account at the 30 m telescope only 1 running instance of Pako should have SET DOSUBMIT YES Example SOURCE OTFMAP START will start and OTF map 7 19 SUBSCAN SUBSCAN x0ffset yOffset SUBSCAN xStart ystart xEnd yEnd SUBSCAN xAmplitude yAmplitude frequencyX frequencyY xCenter yCenter phiX phi NB this is a protected command needs privilege Add to user de
115. Ungerechts CATALOG SOURCE demo sou select source catalog SOURCE NGC7027 select source from catalog OFFSETS Clear optional clear previously set offsets PAUSE OTHER WAYS TO SPECIFY A SOURCE SOURCE CALORI catalog lines J2000 select source from another catalog PAUSE SOURCE OCET EQ J2000 02 19 20 71 02 58 36 17 LSR 46 800 command line specification of source PAUSE I SOURCE Mars planet Mars PAUSE SOURCE Moon our Moon PAUSE SOURCE Io Jupiter s satellite Io PAUSE SOURCE Body Pako 2455000 0 22 2 33 3 44 4 55 5 0 66 solar system body orbital elements PAUSE SOURCE w3oh will match W30H in demo sou NOTES source names must match 11 full source name in catalog or 1 full name of planet or satellite I the case is ignored for source name matching RETURN Id demo source pako more SOURCE demos v 1 1 1 2009 05 08 by Hans Ungerechts CATALOG SOURCE demo sou select source catalog SOURCE Mercury PAUSE 5 NCS USER S GUIDE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE SOURCE PAUSE Venus Mars Jupiter Saturn Uranus Neptune Pluto Phobos Dei
116. VESPA 3 0 080 80 0 0 0 E230 hor LI BACKEND VESPA 4 0 080 80 0 0 0 E230 ver LI SET ANGLE arcsec SWFREQUENCY SWFREQUENCY SWFREQUENCY CALIBRATE AMBIENT COLD SKY SYSTEM TCALIBRATE 3 9 11 7 tphase 600 0 0 0 projection 5 0 PAUSE CALIBRATE OK to start c q START OTFMAP 300 300 300 300 CROLOOP 0 NOTF 4 REFERENCE no STEP 0 10 SYSTEM projection TOTF 120 0 ZIGZAG 3 9 receiver E090 11 7 receiver E230 0 20 PAUSE OTFMAP SWFREQUENCY OK to start c q START Comments we assume here that the source already has see demo source OTFMAP SWFREQUENCY EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo setup of receivers clear previous backends high spectral resolution with VESPA REPLACE WITH YOUR SETUP setup frequency switching for EMIR band E090 for EMIR band E230 same for all receivers bands ambient load cold load sky at offsets 600 0 0 0 system for offset time per calibration subscan a chance to check start offsets at start and end of first OTF only OTF subscans number of on the fly subscans no off source reference subscans step shift between OTF subscans system for offset time per on the fly subscan go back and forth a chance to check start been selected 5 NCS USER S GUIDE 76 5 3 10 RASTER Raster Mapping RASTER may be implemented in a future revision of the NCS It is recommended to use O
117. ame of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made 7 PAKO LANGUAGE INTERNAL HELP 164 TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that the
118. an not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names SHOW lists everything previously set with SET SET TOPOLOGY deserves special attention The 30m antenna has azimuth limits of 60 and 460 degrees Azimuth 360 degrees is due North Therefore there is an overlap range approximately toward East Northeast which the antenna can reach at a low azimuth 60 to 100 from the South or at a high azimuth 420 to 460 from the North SET TOPOLOGY LOW selects to use the azimuth range 60 to 420 degrees SET TOPOLOGY HIGH selects to use the azimuth range 100 to 460 degrees About SET TOPOLOGY also see Section 6 2 and Figure 4 in that section DEVICE is a standard command to open a graphics window for plots It is used by PAKO to provide a preview plot for some observing modes SET LEVEL can be used to control the amount of messages written by PAKO in the terminal window SET LEVEL 3 3 is a good choice in most cases because it suppresses many informational I messages but lets all warnings and serious errors through All these commands should normally be executed in the same way each time observations for a project start Therefore it is a good idea to put them in a script SET doSubmit yes is needed to activate submission of observing commands to the NCS observing queue SET doSubmit no default is useful for debugging so that scripts including START ca
119. and forth a chance to check start been selected an l off source reference subscan R before and after each OTF suscan 0 Therefore with NOTF 4 on the fly subscans the complete R OTF 1 R R OTF 2 R R OTF 3 R R OTF 4 R with CROLOOP ROOROOR it would be R OTF 1 OTF 2 R OTF 3 OTF 4 R OTFMAP SWFREQUENCY EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo setup of receivers clear previous backends high spectral resolution with VESPA REPLACE WITH YOUR SETUP setup frequency switching for EMIR band E090 for EMIR band E230 same for all receivers bands ambient load cold load sky at offsets 600 0 0 0 system for offset time per calibration subscan a chance to check start 7 PAKO LANGUAGE INTERNAL HELP 132 OTFMAP 300 300 300 300 offsets at start and end of f CROLOOP 0 only OTF subscans NOTF 4 number of on the fly subscans REFERENCE no no off source reference subsc STEP 0 10 step shift between OTF subs SYSTEM projection system for offset TOTF 120 0 time per on the fly subscan ZIGZAG go back and forth PAUSE OTFMAP SWFREQUENCY OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source 7 12 POINTING POINTING length Specify a pointing measurement with linear OTF subscans in the true angle horizontal syst
120. and included in the XML but it has no practical effect 7 7 FOCUS FOCUS lengthFocus Specify a focus measurement Real lengthFocus length mm of focus scan The sequence of focus subscans is determined by lengthFocus nSubscans otfFocus lengthFocus total length mm of the focus scan nSubscans number of focus subscans lt lt TD otfFocus not yet implemented gt gt focus subscan 1 is at offset 0 0 focus subscan 2 is at offset lengthFocus 2 in case nSubscans 3 focus subscan 3 is at offset lengthFocus 2 in case nSubscans gt 3 focus subscan 3 is at offset lengthFocus 2 focus subscan 4 is at offset lengthFocus 2 focus subscan 5 is at offset lengthFocus 2 focus subscan 6 is at offset 0 0 etc 7 7 1 FOCUS DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 7 2 FOCUS NSUBSCANS NSUBSCANS nSubscans 7 PAKO LANGUAGE INTERNAL HELP Integer nSubscans number of subscans 7 7 3 FOCUS TSUBSCAN TSUBSCAN tSubscan time per subscan Real tSubscan time FOCUS EXAMPLES Id demo focus pako FOCUS EXAMPLE v 1 1 1 2009 05 08 Hans Ungerechts SWBEAM to select beam switching FOCUS 2 0 length mm NSUBSCANS 6 number of subscans TSUBSCAN 12 time per subscan PAUSE FOCUS OK to start c q a chance to check START start Comments We assume here that a pointing measurement has been done immediately before the FOCUS strongly recomm
121. ary along the telescope axis by maximizing the intensity of the radiation focussed into the receiver s It is best done on a strong point source e g on a planet if or when its angular diameter is less than the beam width at the frequency to be observed It is strongly recommended to do a POINTING on the same source before a FOCUS FOCUS is normally used with BEAM SWITCHING or WOBBLER SWITCHING With the bolometer FOCUS is done with WOBBLER SWITCHING A calibration is not needed for FOCUS anyhow it will probably already have been done before the POINTING before the FOCUS After a focus the data processing software displays the results and you can enter a correction for the observed focus offset with the command SET FOCUS focusCorrection Note that this is the total correction i e the previous correction plus the additional offset found with the FOCUS observation The optiomal focus correction for different receiver bands may be slightly different by a few times 0 1 mm and the observer can decide to optimize for one particular band or use a compromise value After you enter a focus setup manually we recommend to save it optionally to a named file SAVE FOCUS FILE focus 1 It can then at any later time be reloaded with focus 1 see HELP SAVE 6 4 4 TIP TIP antenna tipping or skydip observations are done to measure the transmission of the Earth s athmosphere by taking data at several points with the same azimuth
122. bbler Switching 4310 OTF On The Ply Mapping soss eee gon Pha ie Ra RS SE eS 4 4 Continuum Observations with Bolometers 0 00000 eee 10 10 10 10 10 11 11 12 13 13 13 14 14 16 16 16 16 16 18 18 19 19 19 20 21 CONTENTS 5 NCS User s Guide 5 1 Set General Information s es eg eme ra a A e pi 5 2 Specify your Sou ree Catalog and or Source ss e ss Gee ee ee ee Oe EY oH 5 3 Spectral Line Observations with Heterodyne Receivers 00 4 5 3 1 Specify your Lime Catalog coc aon arat aoa doe ao aoa E Se Eos 5 3 2 Setup of the Receivers Frontends a 5 3 3 Setup of the Backends Spectrometers and Continuum 5 3 4 CALIBRATE sdp p aara i e a kae y A D95 POINTING ep piora p a apa aa e E e BR Ee A ate Reged 5 3 6 FOCUS 5 3 7 TRACK Single Position with FREQUENCY SWITCHING 5 3 8 ON OFF 5 3 9 OTF On 5 3 10 RASTER 5 4 Continuum Obse Position Switching and Wobbler ON OFF The Fly Mapping lt lt lt lt ccce paee bi Ge eee Ee ws Raster Mapping c so ed co tarsa s bas dr ira rvations with Bolometers osooso a 5 4 1 Setup of the Bolometer noaoae Bae Swibchinge Mode ss s 2 4 4 me amaaa a A aea Qe a ea al aa a Bda POINTING er 044 AM do dr ds Oe a a BK Se des 5 4 4 FOCUS 54o TIP Antenna Tipping r Skydip h s si asek kema Re e 5 4 6 ON OFF 5 4 7 OTF On 6 NCS Explained
123. bler phases 2nd the difference between ONOFF subscans a and b This form of ONOFF is also called Wobbler Onoff or sometimes simply Wobbler Switching The combination of ONOFF and WOBBLER SWITCHING provides a very high sensitivity in continuum bolometer observations of compact sources and excellent baselines for spectroscopy It has the disadvantage that the emission free off source positions are very close to the source limited by the maximum Wobbler throw Also the Wobbler direction is fixed in the horizontal system relative to the telescope and therefore in the source system the off source positions rotate around the source position For continumm observations usually a short time per Wobbler phase 0 25 s is used with small Wobbler offsets throws for spectroscopy largest possible Wobbler offsets throws up to 120 are preferred but then the time per phase must be longer 1 2 s 5 4 7 OTF On The Fly Mapping with Wobbler Switching Id demo bolometer onoff pako v 0 2 2005 07 14 by Hans Ungerechts RECEIVER BOLOMETER SWWOBBLER 3 3 0 33 0 Wobbler 33 arc sec TPHASE 0 5 0 5 seconds per phase SET ANGLEUNIT arcsec make sure angle unit is arc sec OTFMAP 200 100 200 100 start and end of first on the fly subscan NOTF 60 number of on the fly subscans 5 NCS USER S GUIDE REFERENCE no STEP 0 6 SYSTEM truehorizon TOTF 66 0 ZIGZAG PAUSE OTFMAP O
124. ce 10 000 WILMA 2 2 000 3720 0 265 0 E090 ver UI 100 0 zigzag T WILMA 3 2 000 3720 0 265 0 E230 hor LI 100 0 WILMA 4 2 000 3720 0 265 0 E230 ver LI 100 0 VESPA 1 0 040 40 0 0 0 E090 hor UO 90 0 CO 1 0 VESPA 2 0 040 40 0 0 0 E090 ver UI 90 0 myLine2 VESPA 3 0 040 40 0 0 0 E230 hor LI 90 0 VESPA 4 0 040 40 0 0 0 E230 ver LI 90 0 LILO PAKONOTFMAP paKo v 1 1 1 Refresh _Exit Figure 2 Screen shot of the PAKO Display 2 PAKO GUIDE OF THE PERPLEXED 18 e06 X lt GREG 0 400 200 200 400 400 200 0 200 400 Figure 3 Screen shot of the PAKO preview plot DEVICE IMAGE W LIMITS 500 500 500 500 SET BOX MATCH BOX Similarly you can use other commands from GREG to change the color of the plotting pens or background of the window 2 18 Defaults Most commands have an option DEFAULT which will set all options and parameters to meaningful default values You can combine this option with explicit values for some parameters and options e g enter at the prompt PAKO gt OTFMAP DEF NOTF 12 means default values for OTFMAP but 12 OTF subscans 2 19 Ranges and checks Most parameters are checked to be within 2 ranges 2 PAKO GUIDE OF THE PERPLEXED 19 1 limits of allowed values If you try to enter a value outside that range you get an error message and the value is not accepted e g enter at the prompt PAKO gt POINTING TOTF 4000 E TOTF value 4000 000 outside limits 1 000000
125. ching BEAM SWITCHING is realized through a rotating chopper wheel in the receiver cabin which during each rotatation switching cycle moves 2 reflecting blades into the beam path in front of the 4th mirror for a total of 4 phases direct beam path to the source same as in TOTAL POWER beam path offset by one blade of the chopper wheel direct beam path to the source same as in TOTAL POWER beam path offset by the other blade of the chopper wheel The offset rotation period and blanking times are fixed BEAM SWITCHING is normally only used for POINTING and FOCUS The source signal is calculated as difference between the direct and offset phases NoTES This beam switching chopper wheel should not be confused with a calibration chopper wheel as it is used at some other mm wave observatories Calibration at the 30 M Telescope is done with different hardware 6 3 2 Frequency Switching FREQUENCY SWITCHING switches between 2 different frequencies so that there are 2 phases The source signal is calculated as the difference between these 2 phases FREQUENCY SWITCHING is normally used with TRACK or OTFMAP Notes IMPORTANT FREQUENCY SWITCHING is very powerful and efficient for some projects e g mapping of narrow spectral lines in cold dark clouds outside the plane of the Milky Way However before deciding to use frequency switching one should consider some potential drawbacks The target lines should be narrow en
126. command 11 HERA with FTS wide bandwidth receiver clear RECEIVER HERA1 WIDTH wide RECEIVER HERA2 WIDTH wide backend clear BACKEND FTS 1 BACKEND FTS 2 RECEIVER HERA1 RECEIVER HERA2 HERA narrow bandwidth with FTS fine resolution receiver clear RECEIVER HERA1 WIDTH narrow RECEIVER HERA2 WIDTH narrow 64 5 NCS USER S GUIDE 65 backend clear BACKEND FTS 1 FINE RECEIVER HERA1 BACKEND FTS 2 FINE RECEIVER HERA2 Id demo backend pako more BACKEND demos v 1 1 11 2011 11 24 Hans Ungerechts one example of a complex EMIR setup RECEIVER CLEAR pako RECEIVER pako RECEIVER clear RECEIVER E090 CS 2 1 97 980965 LI horizontal LI vertical LI RECEIVER E230 CO 2 1 230 537994 LI horizontal LI vertical LI I BACKEND CLEAR clear all backend setups EMIR BBC broad band continuum 1 name resolu bandw fShift band polar SB BACKEND BBC 1 8000 8000 0 E090 H LSB BACKEND BBC 2 8000 8000 0 E090 V LSB BACKEND BBC 3 8000 8000 0 E090 H USB BACKEND BBC 4 8000 8000 0 E090 V USB BACKEND BBC 5 8000 8000 0 E230 H LSB BACKEND BBC 6 8000 8000 0 E230 V LSB BACKEND BBC 7 8000 8000 0 E230 H USB BACKEND BBC 8 8000 8000 0 E230 V USB pause BACKEND CLEAR clear all backend setups 11 EMIR VESPA autocorrelator basic mode NOTE VESPA examples give only some possibilities for 1 a complete list see the VESPA documentatio
127. connected to IF cables 5 to 8 BACKEND NBC WILMA FTS DEFAULT will automatically set the maximum number of backend parts for all available subbands BACKEND BBC is completely independant of the sub band selections for the IF cables NOTE bandwidth selection with EMIR The pako command already allows some flexibility that is not yet fully supported by the data handling e g to select only part of the full bandwidth NOTE FTS on HERA With HERA the FTS can be connected to HERA1 and or HERA2 On HERA the FTS provides some extra bandwidth which is not symmetrical to the point where the line the commanded frequency gets centered With HERA width wide the line gets centered at the center of WILMA and 4MHz Relative to this point the FTS in wide mode covers IF offset frequencies from lt 512 to gt 512 In pako the nominal value of the bandwidth is 1024 symmetric around the line With HERA width narrow the line gets centered at the center of VESPA Relative to this point the FTS in fine mode covers IF offset frequencies from lt 256 to gt 360 In pako the nominal value of the bandwidth is 512 symmetric around the line It is also possible to connect FTS in fine mode on HERA width wide or FTS in wide mode on HERA width narrow However in these cases the 7 PAKO LANGUAGE INTERNAL HELP 99 FTS band coverages are very asymmetric to the line See HERA and FTS documentation for the exact details of the IF ranges
128. d how to define descriptive coordinate sytems will be added as they become available for general use NOTES SOURCE does not clear offsets set with OFFSETS 6 2 Azimuth Topology The 30m antenna has azimuth limits of 60 and 460 degrees Azimuth 360 degrees is due North Therefore there is an overlap range approximately toward East Northeast which the antenna can reach at a low azimuth 60 to 100 from the South or at a high azimuth 420 to 460 from the North SET TOPOLOGY LOW selects to use the azimuth range 60 to 420 degrees SET TOPOLOGY HIGH selects to use the azimuth range 100 to 460 degrees Note that SET TOPOLOGY only has an effect for sources with an azimuth in the overlap range when a source is in the azimuth range 100 to 420 degrees SET TOPOLOGY does not matter Compare Figure 4 6 3 Switching Modes In the NCS we distinguish the following 4 Switching Modes TOTAL POWER BEAM SWITCHING WOBBLER SWITCHING FREQUENCY SWITCHING only with heterodyne receivers The corresponding commands are SWTOTAL SWBEAM SWWOBBLER SWFREQUENCY BEAM SWITCHING WOBBLER SWITCHING and FREQUENCY SWITCHING are realized by a system with hardware synchronization signals that allow a precise and fast switching within subscans TOTAL POWER simply means that none of the other 3 switching modes is active The system switches through a regular cycle with several 1 2 or 4 switching phases 6 NCS EXPLAINED 84 TOPO LOW Az 60 420 TOPO
129. d the bolometer are normally done 7 19 4 SUBSCAN TOTF TOTF tOtf time per OTF subscan or segment 7 PAKO LANGUAGE INTERNAL HELP 157 Real tOtf time In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied NOTE this applies to linear and Lissajous OTF subscan segments 7 19 5 SUBSCAN TSUBSCAN TSUBSCAN tSubscan time per subscan Real tSubscan time NOTE this applies to Track subscans 7 19 6 SUBSCAN TUNE TUNE yes no Logical doTune Tune an instrument e g NIKA NOTE this applies to Track subscans If a valid specification of a TRACK subscan is entered without the option TUNE no is implied 7 19 7 SUBSCAN TYPE TYPE Type Specify segment or subscan type one of TRACK LINEAR LISSAJOUS Character Type 7 20 SWBEAM SWBEAM no parameters Select beam switching i e switching between 2 positions on the sky using the rotating beam switch chopper wheel This mode is usually 7 PAKO LANGUAGE INTERNAL HELP 158 only used for POINTING and FOCUS with the heterodyne receivers 7 21 SWFREQUENCY SWFREQUENCY fOffset1 f0ffset2 Select and set up frequency switching FS Real fOffsetl 1st frequency offset MHz Real f0ffset2 2nd frequency offset MHz fOffset2 should be set to be fOffset1 symmetric FS This is done by default if only fOffseti is specified Note tha
130. dLoad which means to leave the value for tempColdLoad unchanged from the previous RECEIVER command NOTE FOR HERA measured values are always used during the execution of the observations This is the same logic as in older versions of paKo NCS 7 13 12 RECEIVER VERTICAL VERTICAL sbi sb2 VERTICAL n one EMIR subbands for Vertical polarization This option applies only to EMIR Character sbi sb2 for EMIR LOILI UI UO This option selects which EMIR subband s of this polarization will be transmitted through IF cables 1 to 4 Note that some backends NBC 4MHz WILMA VESPA can only be connected to IF cables 1 to 4 i e only to the EMIR subbands selected with the RECEIVER command For each EMIR band and polarization at most 2 subbands can be transmitted through IF cables 1 to 4 Which combinations of EMIR bands polarizations and subbands are possibble is determined by the hardware of the EMIR IF switching box See the EMIR documentation for details If no subband is explicitly specified with this option paKo will assume that for this polarization the same single subband SB is requested as specified for the main parameters frequency tuning of the RECEIVER command for this EMIR band VERTICAL n one means that from this polarization no subband will be transported through IF cables 1 to 4 7 13 13 RECEIVER WIDTH WIDTH width 7 PAKO LANGUAGE INTERNAL HELP 140 Select receiver setup for WIDE or NARROW ba
131. ds directly to the syntax of the command E g for each observing mode the display shows the syntax of all options The most recent command as pako interpreted it is usually shown at the bottom of the display window The keywords for commands and options try to be meaningful and if possible self explanatory As usual with SIC minimum match is supported so you can also write compact and cryptic commands e g enter at the prompt PAKO gt OTF B C CROOR NO 12 REF ST 20 20 SY PR TO 30 TR 22 Z 2 5 SET LEVEL for Errors Warnings and Infos PAKO can be very chatty and display many messages in the command line window They are marked with I for info W for warning or E for error E error is reserved for true errors something not accepted by PAKO You can control the number of messages you see with with SET LEVEL e g SET LEVEL 1 1 will enforce that you get all messages SET LEVEL 3 3 will supress most I infos SET LEVEL 5 5 will supress most I infos and W warnings At this time 2012 12 01 PAKO still displays some debug messages which are not flagged I W or E They will be eliminated as soon as possible 2 6 Saving and Restoring For most commands you can save the parameters into a file e g enter at the prompt PAKO gt SAVE POINTING This saves the parameters of observing mode POINTING The format of the
132. during data processing Normally the system will provide reasonable defaults for all these calibration parameters 5 NCS USER S GUIDE 62 At the 30 m Telescope it is generally recommended to use the antenna temperature scale during observations and to do any scaling to other scales lateron during off line data processing See the documentation about calibration for more details 5 3 3 Setup of the Backends Spectrometers and Continuum basic BACKEND EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts Id demo backend pako swTotal 1 one example of a complex EMIR setup default pako RECEIVER pako RECEIVER clear RECEIVER E090 horizontal LI vertical LI RECEIVER E230 CO 2 1 230 537994 LI horizontal LI vertical LI 1 BACKEND 1 BACKEND 1 1 pause backend BACKEND pause backend BACKEND BACKEND CLEAR BBC Default clear NBC Default clear WILMA Default clear 4MHz Default CS 2 1 97 980965 LI select a switching mode compatible with all backends clear all backend setups EMIR BBC connect 1 part to both polarizations of each sideband of each selected EMIR band EMIR NBC connect 1 part to each selected EMIR subband EMIR WILMA connect 1 part to each selected EMIR subband EMIR 4MHz NOTE 4MHz has only 2 parts with EMIR connect 1 part to each of 5 NCS USER S GUIDE pause BACKEND BACKEND pause
133. e Rw RR Ee 172 Te 2G OPTIONS SCALE sx poor rra Re ee a RA A 172 aca OPTIONS SY i ck bee eee ES oR eRe tee SRE Ee He RSs 172 ES OPTIONS SPEED 6c t oe ei bee oa eee bee he oe eR Eee 173 Tolg OPTIONS STEP 22h bs debe sredo aa ee eee bas 173 7 21 00 OPTIONS SWWOBBLER 24 4544 cese eR Raa eee ee we 173 T23L OPTIONS SYMMETRY sor ees Ro eS ERE Ree eM ee BO 174 Co oe OPTIONS SYSTEM 265424547584 nd oo SRR eee eee ates 174 Tas OPTIONS TCALIBRATE y ccp Satane ee kee ee ee A 175 FeO PIONS PUDO sos A ARA PR eR e 175 fo oo OPTIONS TPHASE gt e si s bMS ERED EE ee EE ee EE ERS 176 T 2130 OPTIONS TREFERENCE ces dse streta eee eee eee aS 176 foro OPTIONS TSUBSCAN 22 s eacop d morace geo pee Ree Se Ses 176 ToS OPTIONS TEMPLOAD o ce ee see AAA ew os 176 T239 0OPTIONS VELOCILY y avec Sage ania sade eek ae a A 177 a AQOPTIONS VERTICAL os 0 0 a opaa 178 TrA OPTIONS WIDTH cs su ios ee e E A A 178 Tel A2 OPTIONS ZIGZAG cocos eA ee tne ka a 179 8 Postscript 180 1 PAKO INTRODUCTION AND OVERVIEW 9 1 paKo Introduction and Overview After this introduction follows section 2 a Guide for the Perplexed Here we briefly explain some general features of PAKO as well as differences from the previous control system for the 30 M Telescope In Section 3 we give a very short recipe with the bare minimum to get started with Heterodyne observations Section 4 is PaKo s Cook Book It is meant to evolve into a gentle step by step and com
134. e ambient temperature load Logical doAmbient default true 7 3 3 CALIBRATE COLD COLD yes no Do a calibration subscan on the cold temperature load Logical doCold default true 7 3 4 CALIBRATE GAINIMAGE 7 3 gt NOTE OBSOLETE WITH CHANGE TO EMIR 5 CALIBRATE GRID GRID yes no NOT YET AVAILABLE FOR EMIR Do a calibration subscan on a grid This is a special calibration option for polarization observations Logical doGrid default true IMPORTANT NOTE remember to turn this option off again for normal calibrations e g CALIBRATE GRID NO or CALIBRATE DEFAULT 106 7 PAKO LANGUAGE INTERNAL HELP 107 7 3 6 CALIBRATE SKY SKY xOffsetC yOffsetC or SKY NO do not do sky calibration Do a calibration subscan on sky Real xOffsetC x offset Real yOffsetC y offset NOTES with the usage SKY x0ffsetC yOffsetC both parameters are required but you can replace either parameter with to leave it unchanged The system for the offsets is selected through the option SYSTEM 7 3 7 CALIBRATE SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection of
135. e we Re ba 100 far BACKEND PINE cios SER SS 4S See KKH eS LEER EG 100 fas BACREND MODE i 264 5602 2043844684 siria 100 7 29 BACKEND LINENAME 2 6454 45485588605 adeeb aeaa 101 7 2 10 BACKEND PERGENTAGE 22 4 4428 24460594 See Se O48 101 7 2 11 BACKEND RECEIVER 5 22665 5455445 24 eed eee ed ae ee 102 7 2 12 BACKEND EXAMPLES 020020022 eee 102 Teo CALIBRATE o oien be a ee ee a oe ee A a h i 105 Tal CALIBRATE ORPAULIS cccp Soa metie Bees ee e E R 106 fae CALIBRATE AMBIENT cecs Pau yh ARA a 106 joe CALIBRADO COLD o eet ve a og a e OES ERS 106 7 3 4 CALIBRATE GAINIMAGE 22344544 G44 a eS 106 Las CALIBRATE GRID ss socia pacs a a A Se RS 106 136 CALIBRATE SRY sia a EA AAA os 107 TaT CALIBRATE SYSTEM sierras BE RE A 107 7 3 8 CALIBRATE TCALIBRATE sico co vecinos Be ee ede 108 TA CATALOG os perme deka ed Peewee Pa dw AG et oe ee ee E 108 TAI CATALOG SOURCE 4 466 doa porosa nte ew RED Ree eH ee 109 TAa CATALOG LINE oc aed poe ana t g ea a OR ee RR ee 109 To DISPLAY copla be kA SDE RE Ee ESE BAD Oe Ge EY ES 110 78 DIYLST cocida daa ia A a Ch be ee ee ed 110 TAL DIYLIST CLEAR 2 25s bebe ghd de eee ee Gadde eet eb bx 110 16 2 DYLLI PURPOSE oso serios eR bee oe Ee GA a ERE SSeS 110 Tat MOS a tds be Se oe ee a we Soe a a a A ee ee 111 Til FOCUS DEFAULTS ess carrasco ohne eee ehh at ae 111 fia FOCUS NSUBSCADS s ul So eed due Ree ee ee A 111 fe FOCUS Foes oos vee Pao eh eek ee ee Be ee eS 112 TIA FOCUS EXAMPLES ois
136. ee ai a a aa A 139 AS JARECEIVER EXAMPLES o a p app ia e k de al eR EE a 140 ng a a Be a dr o RE de eS O de Ee A 141 TAL SAVE APRENDO osos tits E A Ow s 142 HILL SAVE PUE lt lt conato rada AA 142 TL3 SAVE EXAMPLES cocos OH EAS OES a a 142 CONTENTS 7 7 15 7 16 7 17 7 18 1 19 7 20 121 22 7 23 24 7 25 UE ae Pen peek a Be ee oe ee we E e Baek he ee Bo ee Re 143 Pele ART DOSUBMIT lt lt iu oe keke Heed eR a oe Bee a ee p 144 TL SET FOCUS i lee Bea ee oe ee oe ee ee ee ew 144 Welt SEL LEVEL c soscrits ra ea ee eA ee Be ee eS 144 PIDA SET POINTING s i p a ee ob Se ele wa awe Se a Ew oS 145 mioo SET 2NDROTATION so scra popa p ol eos PA E ole oo 145 160 SET TOPOLOGY oir eee Gas be a Re ae 145 TIST DET EMIRCHBOR an othe ae he ee eee a ak ee Ee ee Be 146 Tia OBT LIMIT CHEK gen be g p E pa i go ee BOE Oe Be ee ee 146 TISI SET USERLEVEL cos s deoa ee Poe RY A ee RE Es 147 AS 10SET EXAMPLES cx 620000 e OE RRR RE EEG 147 SHOW recce Bw Ste ke Bae RSG Me eee A A HE 148 SOURCE e cecake he Aa OOS Gaede wee Ba e ee GO e pee ee 148 7 17 4 SOURCE CATALOG 2 2448 duod pa ae Ree al 151 17 2 SOURCE CREP cocos sete snada a ka aes eee n sees 151 TiTa SOURCE VELOCITY eso ee eee eh ay Oa eed eee ee ee ee 151 TATA SOURCE EXAMPLES 4 5 242 5 5 8 DE eee ed 152 e bess by a oe EES EE Oe eS oy Oe ee ee 153 A RAN 153 T191 SUESCAN CROPLA e ic Paw RA Ra 155 710 SUBSCAN RAMP o oceta pr a a Oe A es 155 7 19 3 SUBSCAN
137. ee the EMIR documentation for details If no subband is explicitly specified with this option paKo will assume that for this polarization the same single subband SB is requested as specified for the main parameters frequency tuning of the RECEIVER command for this EMIR band HORIZONTAL n one means that from this polarization no subband will be transported through IF cables 1 to 4 7 13 10 RECEIVER SCALE SCALE scale Select the calibration intensity scale Character scale choices ANTENNA BEAM If scale is ANTENNA the scale is antenna temperature If scale is BEAM the scale is main beam temperature 7 13 11 RECEIVER TEMPLOAD TEMPLOAD tempColdLoad tempAmbientLoad TEMPLOAD L OOKUP L OOKUP TEMPLOAD Set effective temperatures for the calibration loads at cold and ambient temperature Real tempColdLoad Real tempAmbientLoad NEW LOGIC FOR SINGLE PIXEL SIS RECEIVERS FROM SUMMER 2007 paKo v1 0 7 If a numerical value is entered for tempColdLoad or tempAmbientLoad that value is used for calibration calculations Instead of specifying a value one may enter the string L OOKUP for 7 PAKO LANGUAGE INTERNAL HELP 139 tempColdLoad and or tempAmbientLoad This is shown in the pakoDisplay by the letter L instead of a number In this case during the execution of the observations the NCS will use measured values for the corresponding load temperature s A can be substituted for tempCol
138. em along azimuth and elevation all centered on the source Real length length angle of each subscan The first subscan is incrementing in azimuth If the number of OTF subscans n0tf is 2 the second subscan is incrementing in elevation If nOtf gt 2 the subscan sequence is incrementing azimuth decrementing azimuth incrementing elevation and if nOtf gt 3 decrementing elevation etc 7 12 1 POINTING DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 12 2 POINTING DOUBLEBEAM DOUBLEBEAM yes no Pointing do a double beam pointing Logical doDoubleBeam 7 PAKO LANGUAGE INTERNAL HELP 133 This is valid only for pointing with Wobbler switching SWWOBBLER This option has an effect only if SET 2nRotation 0 0 7 12 3 POINTING NOTF NOTF nOtf Integer nOtf 7 12 4 POINTING TOTF TOTF tOtf time per OTF subscan or segment Real tOtf number of OTF on the fly subscans In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 125 POINTING EXAMPLES POINTING EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts Id demo pointing pako SOURCE Mars OFFSETS CLEAR demo rx 1 BACKEND CLEAR BACKEND BBC Default SET ANGLEUNIT arcsec 1 SWBEAM POINTING DEFAULT POINTING 120 NOTF 4 TOTF 30 0 clear previo
139. ended see demo pointing and therefore we assume here that source receivers and backends already have been selected and set up If you want the intensity of the Focus data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before 7 8 LISSAJOUS LISSAJOUS xAmplitude yAmplitude CENTER xCenter yCenter FREQUENCY frequencyX frequencyY PHASES phiX phiY TOTF tOtf SYSTEM system Specify an On The Fly OTF map with a Lissajous curve in 1 subscan LISSAJOUS is at this time 2012 04 01 supported in data processing 112 7 PAKO LANGUAGE INTERNAL HELP 113 only for the GISMO bolomter Real xAmplitude amplitude for x offsets Real yAmplitude amplitude for y offsets Real xCenter center x offset Real yCenter center y offset Real frequencyX frequency Hz for x Real frequencyY frequency Hz for y Real phiX phase offset rad for x Real phiY phase offset rad for y Real tOtf time s Character systemName name of system one of PROJECTION TRUEHORIZON During a Lissajous OTF segment the position offsets x and y as a function of time t are xCenter xAmplitude SIN 2 Pi frequencyX t phiX yCenter yAmplitude SIN 2 Pi frequencyY t phiY x y SIN is the usual sine function Pi is the number Pi xAmplitude yAmplitude xCenter yCenter are in angle units larc sec frequencyX frequencyY are in Hz phiX phiY are
140. erver s Don t use amp lt gt Operator Character len 24 Telescope operator s Don t use amp lt gt Pointing Real Real Focus Real Topology Character len 24 2ndRotation Real Pointing corrections larc sec Focus correction mm Topology for the overlapping azimuth range Rotation angle for Secondary and Wobbler EMIRcheck Character strict relaxed loose doSubmit Logical turn submission of jobs to queue on or off NB Don t use amp lt gt in names of sources lines projects PI observer operator etc Don t use in source names In order to include blank characters in a value of type Character the complete value should be included in see example SET Observer be low Only a few of these parameters are shown in the Display Use command SHOW to list nearly all of them 7 PAKO LANGUAGE INTERNAL HELP 144 7 15 1 SET DOSUBMIT SET DOSUBMIT YES NO Logical doSubmit Turn submission of jobs to observing queue on or off compare command START IMPORTANT NOTE to avoid any possible confusion in each project account at the 30 m telescope only 1 running instance of Pako should have SET DOSUBMIT YES 7 15 2 SET FOCUS SET FOCUS focus Real focus focus correction mm Set focus correction in mm 7 15 3 SET LEVEL SET LEVEL minimalForStandardOut minimalForFile Integer minimalForStandardOut in range O to 9 Integer minimalForFile in range 0 to 9
141. ference frame and source radial velocity Character referenceFrame reference system for velocity Real velocity in units km s Choices for referenceFrame LSR barycentric heliocentric lt lt TBD not yet supported gt gt lt lt TBD 3K gt gt lt lt TBD galactocentric gt gt lt lt TBD body gt gt 7 PAKO LANGUAGE INTERNAL HELP 152 lt lt TBD geocentric gt gt lt lt TBD topocentric gt gt lt lt TBD null gt gt IMPORTANT NOTE ON VELOCITY One should not use very large Doppler velocities thousands of kilometers to achieve red shift corrections of frequencies Instead one should enter the red shifted frequencies in the line catalog or with the RECEIVER command and use Doppler velocity of 0 0 The alternative approach with very large Doppler velocities needs special methods and attention in the data processing which are not implemented in CLASS because it is better to observe in such a way that minimum modification to the data is done later on J Pety For a full discussion of this question see Gordon et al 1992 A amp A 264 337 in Sect 6 7 17 4 SOURCE EXAMPLES Id demo source pako basic SOURCE EXAMPLES v 1 1 1 2009 05 08 by Hans Ungerechts CATALOG SOURCE demo sou select source catalog SOURCE NGC7027 select source from catalog OFFSETS Clear optional clear previously set off PAUSE OTHER WAYS TO SPECIFY A SO
142. ffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 9 1 OFFSETS DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 9 2 OFFSETS CLEAR CLEAR yes no Completely clear a list of connected hardware e g receivers backends or parameters of the associated command 7 9 3 OFFSETS SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing 7 PAKO LANGUAGE INTERNAL HELP 118 focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM
143. fined list of subscans and segments for observing mode DIY compare command DIY The subscan command has the 3 main variants above depending on the number of parameters 7 PAKO LANGUAGE INTERNAL HELP 154 2 gt Track subscan with fixed of sets 4 gt Linear OTF segment subscan 8 gt Lissajous OTF segment subscan IMPORTANT SEE NOTE BELOW Option TYPE allows to enforce that the command is interpreted for one the 3 different types independant of the number of parameters Option TUNE allows to specify that a Track subscan will be used to tune an instrument e g NIKA Real xOffset x offset fixed position TRACK subscan Real yOffset offset fixed position TRACK subscan lt Real phiX Real phiY phase offset rad for x Lissajous OTF segment phase offset rad for y Lissajous OTF segment Real xStart x offset start of linear OTF segment Real yStart y offset start of linear OTF segment Real xEnd x offset end of linear OTF segment Real yEnd y offset end of linear OTF segment Real xAmplitude x amplitude Lissajous OTF segment Real yAmplitude y amplitude Lissajous OTF segment Real frequencyX frequency Hz for x Lissajous OTF segment Real frequencyY frequency Hz for y Lissajous OTF segment Real xCenter x center Lissajous OTF segment Real yCenter y center Lissajous OTF segment If an asterisk appears in place of any parameter the value will re
144. fset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 27 33 OPTIONS TCALIBRATE TCALIBRATE tCalibrate Time per CALIBRATE subscan Real tCalibrate time 7 27 34 OPTIONS TOTF TOTF tOtf time per OTF subscan or segment Real tOtf time 7 PAKO LANGUAGE INTERNAL HELP In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 27 35 OPTIONS TPHASE TPHASE tPhase time per switching PHASE Real tPhase time 7 27 36 OPTIONS TREFERENCE TREFERENCE tReference time per off source reference Real tReference time 7 27 37 OPTIONS TSUBSCAN TSUBSCAN tSubscan time per subscan Real tSubscan time 7 27 38 OPTIONS TEMPLOAD TEMPLOAD tempColdLoad tempAmbientLoad TEMPLOAD L OOKUP L OOKUP TEMPLOAD Set effective temperatures for the calibration loads at cold and ambient temperature Real tempColdLoad Real tempAmbientLoad NEW LOGIC FOR SINGLE PIXEL SIS RECEIVERS FROM SUMMER 2007 paKo v1 0 7 If a numerical value is entered for tempColdLoad or tempAmbientLoad that value is used for calibration calculations Instead of specifying a value one may enter the string L OOKUP for tempColdLoad and or tempAmbientLoad This is shown in the pakoDisplay by the
145. fsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used 7 PAKO LANGUAGE INTERNAL HELP 108 IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 3 8 CALIBRATE TCALIBRATE TCALIBRATE tCalibrate Time per CALIBRATE subscan
146. fsets of on position NSUBSCANS 5 number of subscans SYSTEM projection 2 system for offset TSUBSCAN 60 time per subscan PAUSE TRACK SWFREQUENCY OK to start c q START start a chance to check Comments we assume here that the source already has been selected see demo source 7 26 VLBI VLBI Track a single position for VLBI 7 PAKO LANGUAGE INTERNAL HELP 166 This observing mode must not be used for other non VLBI observations Some special behaviours are asscociated with the observing mode VLBI 7 27 The scan has only one subscan on the fixed source position This subscan will be executed for up to 1 hour In practice it is ended when the START command is executed for the next observation e g when a new VLBI scan or a POINTING or FOCUS is started Normally the VLBI field system sends the commands SOURCE VLBI START directly to paKo which is running in a special terminal window The field system sends these commands for the next scan immediately after the VLBI data recording for the current VLBI target source for the currant scan is finished OPTIONS SUMMARY OF OPTIONS FOR PAKO COMMANDS For help on commands say HELP PAKO For details say e g HELP OPTIONS CROLOOP or HELP OP CRO To see if a command has a particular option see the end of the HELP for this command 7 27 1 OPTIONS AIRMASS AIRMASS airmassStart TO airmassEnd BY air
147. he internal help itself which may be more up to date then an old printout of the user s manual NOTES lt lt and lt lt TBD mark items that are foreseen in the NCS but that are not yet available 7 PAKO LANGUAGE INTERNAL HELP 91 7 1 Language SUMMARY OF PAKO COMMANDS v1 1 14 NEW in 1 1 14 RECEIVER BOLOMETER NIKA Receiver bolometer NIKA SUBSCAN xOffset yOffset TUNE for NIKA DIY PURPOSE play my Tune for NIKA Examples how to use HELP for detailed HELP on a command HELP OTFMAP HELP OTFM one subtopic or option HELP OTFMAP NOTF examples HELP OTFMAP EXAMPLES all subtopics and options HELP OTFMAP options in general HELP OPTIONS news about paKo HELP PAKO NEWS NOTE lt lt TBD Oe oe To BE DONE or lt lt wee gt gt flag items that are planned for the NCS but not yet implemented or propely tested Observers should not try to use these features without consulting the NCS team setup SET amp SHOW set general parameters project observer CATALOG select source or line catalogs SOURCE specify a source OFFSETS specify source offsets RECEIVER set up receivers BACKEND set up backends switching modes select 1 SWBEAM select and set up beam switching SWFREQUENCY select and set up frequency switching SWTOTAL select total power no switching SWWOBBLER select and set up wobbler switching observing modes select 1 CALIBRATE specify a calibration FOCUS specify a focus measurement POI
148. her parameter with to leave it unchanged STEP dx dy Step shift or translation between lines in a map Real rn dX shift in x offsets Real dy shift in y offsets SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset 7 PAKO LANGUAGE INTERNAL HELP 127 NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS xOffset yOffset SYSTE
149. his inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 8 5 LISSAJOUS TOTF TOTF t0tf time per OTF subscan or segment Real tOtf time In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 9 OFFSETS OFFSETS xOffset yOffset Specify source offsets Real xOffset x offset Real yOffset y offset 7 PAKO LANGUAGE INTERNAL HELP 116 IMPORTANT NOTE one should be careful with the OFFSETS command which is only used and only needed in a few special situations e g with Wobbler switching ONOFF and to set NASMYTH offsets for focal plane array receivers The function of OFFSETS is explained in the paKo user s manual Section A Guide to the Perplexed and in more detail in the Section NCS Explained Subsection Coordinate Systems Projections and Offsets For many observations all offsets are specified as parameters or options of the command for the observing mode SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON
150. hor UO E090 hor UO Only FTS parts 5 to 8 can be connected to IF cables 5 to 8 BACKEND NBC WILMA FTS DEFAULT will automatically set the maximum number of backend parts for all available subbands BACKEND BBC is completely independant of the sub band selections for the IF cables Bolometer Character bolometerName name of bolometer Choices for bolometerName are GISMO NIKA NOTE 2011 07 14 the MAMBO bolometers are out of operation 7 PAKO LANGUAGE INTERNAL HELP 136 7 13 1 RECEIVER DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 13 2 RECEIVER CLEAR CLEAR yes no Completely clear a list of connected hardware e g receivers backends or parameters of the associated command 7 133 RECEIVER CONNECT CONNECT yes no connect or disconnect the specified hardware e g backend or backend part gt DEPRECATED PROTECTED needs SET userLevel 7 13 4 RECEIVER DEROTATOR DEROTATOR angle system Specify derotator angle for HERA Real angle in units deg Character system Choices for system Nasmyth horizon equatorial frame same as Nasmyth sky same as equatorial NOTES The last 2 are for consistency with old control system and HERA conve This option works only for RECEIVER HERA1 or RECEIVER HERA2 of course it s same angle for HERA1 and HERA2 7 13 5 RECEIVER DISCONNECT DISCONNECT disconnect the specified
151. ime per OTF subscan in s and the time per off source reference subscan s This observing mode is normally used either with 4 PAKO S COOK BOOK 44 i TOTAL POWER with an off source reference for spectral line observations or ii FREQUENCY SWITCHING without off source reference for spectral line observations see below or iii WOBBLER SWITCHING and TRUE ANGLE HORIZON offsets for continuum mapping with the bolometer After you enter an OTF map setup manually we recommend to save it optionally to a named file SAVE OTFMAP FILE otfmap 1 It can then at any later time be reloaded with otfmap 1 see HELP SAVE You may want to save the switching mode seperately or with OTFMAP into the same file SAVE SWITCHING FILE otfmap 2 SAVE OTFMAP FILE otfmap 2 APPEND And finally OTFMAP with FREQUENCY SWITCHING Id demo otfmap swfrequency pako OTFMAP SWFREQUENCY EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo rx demo setup of receivers BACKEND CLEAR clear previous backends BACKEND VESPA 1 0 040 40 090 hor LI high spectral resolution BACKEND VESPA 2 0 040 40 090 ver LI with VESPA BACKEND VESPA 3 0 080 80 230 hor LI BACKEND VESPA 4 0 080 80 230 ver LI REPLACE WITH YOUR SETUP SET ANGLE arcsec oOoooo oooo oooo bota setup frequency switching SWFREQUENCY 3 9 3 9 receiver E090 for EMIR band E090 SWFREQUENCY 11 7 11 7 receiver E230 for EMIR band
152. in rad Note that the possible frequencies are very low typically 0 01 to 0 15 Hz At the start of a Lissajous subscan paKo will insert a ramp along a straight line i e a linear OTF segment increasing the count of segments by 2 This ramp up starts with speed 0 relative to the source and joins smoothly with the start position and velocity of the Lissajous segment The purpose is to avoid a sudden acceleration at the start of the Lissajous segment The inserted ramp up segment and the Lissajous segment become part of the same subscan Lissajous curves with large amplitudes or frequencies can reach the antenna s speed and acceleration limits for tracking Lissajous curves can be executed only for elevations less than a maximum which depends on the Lissajous parameters For information this elevation condition is shown by pako Even below the limits during very fast Lissajous curves the tracking errors will be higher several arc sec than during most other observations DO NOT TRY TO OBSERVE LISSAJOUS ABOVE THIS MAXIMUM ELEVATION 7 8 1 LISSAJOUS CENTER CENTER xCenter yCenter 7 PAKO LANGUAGE INTERNAL HELP 114 position of center Real xCenter center x offset Real yCenter center y offset 7 8 2 LISSAJOUS FREQUENCY FREQUENCY frequencyX frequencyY Real frequencyX frequency Hz for x Real frequencyY frequency Hz for y 7 8 3 LISSAJOUS PHASES PHASES phiX phiY Real phiX phase offset
153. is achieved by using the special option SWWOBBLER of the command ONOFF Subscans are then taken alternating between 2 positions in such a way that a in some subscans one position of the antenna the source is in the first of the two Wobbler phases b in the other subscans the other position of the antenna the source is in the second of the two Wobbler phases During the data processing the source signal is computed as a double difference 1st the difference of the 2 Wobbler phases 2nd the difference between ONOFF subscans a and b This form of ONOFF is also called Wobbler Onoff or sometimes simply Wobbler Switching The combination of ONOFF and WOBBLER SWITCHING provides a very high sensitivity in continuum bolometer observations of compact sources and excellent baselines for spectroscopy It has the disadvantage that the emission free off source positions are very close to the source limited by the maximum Wobbler throw Also the Wobbler direction is fixed in the horizontal system relative to the telescope and therefore in the source system the off source positions rotate around the source position For continumm observations usually a short time per Wobbler phase 0 25 s is used with small Wobbler offsets throws for spectroscopy largest possible Wobbler offsets throws up to 120 are preferred but then the time per phase must be longer 1 2 s 6 4 6 OTFMAP In OTFMAP on the fly observations
154. is the total correction i e the previous correction plus the additional offset found with the POINTING observation After you enter a pointing setup manually we recommend to save it optionally to a named file SAVE POINTING FILE pointing 1 It can then at any later time be reloaded with pointing 1 see HELP SAVE 4 3 7 FOCUS Id demo focus pako FOCUS EXAMPLE v 1 1 1 2009 05 08 Hans Ungerechts SWBEAM to select beam switching FOCUS 2 0 length mm NSUBSCANS 6 number of subscans TSUBSCAN 12 time per subscan PAUSE FOCUS OK to start c q a chance to check START start Comments We assume here that a pointing measurement has been done immediately before the FOCUS strongly recommended see demo pointing and therefore we assume here that source receivers and backends already have been selected and set up If you want the intensity of the Focus data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before FOCUS measurements are done to optimize the position of the subreflector secondary along the tele scope axis by maximizing the intensity of the radiation focussed into the receiver s It is best done on a strong point source e g on a planet if or when its angular diameter is less than the beam width at the frequency to be observed It is strongly recommended to do a POINTING on the same source before a FOCUS FOCUS i
155. it SB explicit SB explicit NOTE E090 H amp V 4 GHz BW say 4 PAKO S COOK BOOK pause say receiver clear RECEIVER E090 RECEIVER E150 say say pause say receiver clear RECEIVER E090 RECEIVER E230 say say pause say receiver clear RECEIVER E150 RECEIVER E330 say say pause LIL RECEIVER HCN 1 0 Hor Ver CS 3 2 H V HCN 1 0 Hor Ver 12C0 2 1 Horizontal Vertical CS 3 2 H V 13C0 3 2 H V clear LI LI LI LI LI LI REC HERA1 12C0 2 1 230 537990 LSB REC HERA2 12C0 2 1 230 537990 LSB pause NOTE E090 LSB Inner LSB Inner LSB Inner LSB Inner NOTE E090 E150 NOTE E090 LSB Inner LSB Inner LSB Inner LSB Inner NOTE E090 E230 NOTE E150 LSB Inner LSB Inner LSB Inner LSB Inner clear all receivers previously set NOTE E150 NOTE E330 E150 bands H V 4 GHz BW H V 4 GHz BW E230 bands H V 4 GHz BW H V 4 GHz BW E330 bands H V 4 GHz BW H V 4 GHz BW 31 Normally we use the RECEIVER command with 2 parameters a receiver name and a line name The line name must be the name of a line in the line catalog selected earlier The frequency and sideband or EMIR sub band are then taken from the line catalog Alternatively the frequency and sideband or sub band can be specified directly as the 3rd and 4th parameter NOTES PAKO S COOK BOOK 32 For the E
156. ized as the planet Mars however W30 does not match W30H Option GREP does a grep search for the partial source name or string in the source catalog This search ignores the case SOURCE Body has a special format that allows to specify directly the orbital elements of a solar system body comet 5 3 Spectral Line Observations with Heterodyne Receivers 5 3 1 Specify your Line Catalog Id demo EMIR lin v 1 1 1 2009 05 06 Hans Ungerechts 1 l this is a special version for EMIR using sub bands LI UI and UO 1 5 NCS USER S GUIDE Line Frequency EMIR sub band E090 CH30H 84 52121 LI 0CS 7 6 85 139108 LI SIO V1 86 243350 LI H13CN 86 342274 I H13C0 86 754330 LI SIO VO 86 846891 LI HCN 1 0 88 6316024 LI HCO 1 0 89 188523 LI HNC 1 0 90 663574 LI HC3N 10 9 90 9789933 LI C348 2 1 96 412982 LI ocs 8 7 97 3012085 LI CS 2 1 97 980968 LI HC3N 11 10 100 076392 LI 34802 102 031906 LI 13C180 1 0 104 711385 LI C180 1 0 109 782182 UI 13C0 1 0 110 201370 UI C170 1 0 112 359277 UI CN F1 1 0 113 490982 UI 12C0 1 0 115 271204 vo E150 HC3N 15 14 136 464400 LI C34S 3 2 144 617147 LI H2C0 146 145 602952 LI CS 3 2 146 969049 LI E230 C180 2 1 219 560319 LI 13C0 2 1 220 398686 LI CH3CN220 220 747263 LI CH3CCH222 222 166970 LI c170 2 1 224 714370 LI H2C0225 225 697772 LI 12C0 2 1 230 537990 LI C34S 5 4 241 01617
157. jection describes the relation between 2 spherical coordinates longitude l and latitude b on the celestial sphere and 2 Cartesian coordinates x and y which in radio astronomy and the NCS we often call position offsets Up to now 2012 12 01 only the radio projection is supported for which t l lsource cos b y b bsource where lsource and bsource are the source coordinates specified with SOURCE Note that this is the same system of offsets as in OBS of the old control system If we want to observe several positions on the sky at or near the source position as specified with SOURCE we often do this by requesting position offsets in the map projection Also the resulting data e g images are usually stored and displayed as a function of x and y For most observations parameters and options of the observing mode are sufficient to specify the position offsets e for TRACK and VLBI x and y are fixed during the complete scan e for ONOFF x and y change from subscan to subscan e for OTFMAP x and y change continuously or on the fly OTF during the OTF subscans The PAKO commands for most Observing Modes expect fixed offsets or start and end offsets for OTFMAP as parameters These can be either in the radio projection specified with the option SYSTEM projection or in the true angle horizon system see below specified with the option SYSTEM trueHorizon Notes For POINTING the OTF off
158. ko ONOFF SWTOTAL EXAMPLE v 1 1 1 2009 05 05 Hans Ungerechts POSITION SWITCHING demo rx spectrometers demo setup of receivers and spectrometers REPLACE WITH YOUR SETUP SET ANGLE arcsec 1 SWTOTAL select total power TPHASE 0 5 time per phase data sample CALIBRATE Se ol AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start ONOFF 40 0 30 0 offsets of on position NSUBSCANS 12 number of subscans REFERENCE 600 0 0 0 projection offsets of off source reference 4 PAKO S COOK BOOK 41 SYSTEM projection system for offsets SYMMETRIC symmetric subscan sequence TSUBSCAN 30 time per subscan PAUSE ONOFF SWTOTAL OK to start c q a chance to check START start Comments we assume here that the source already has been selected see demo source In its first form ONOFF is used with TOTAL POWER Subscans are taken alternating between a position that s considered to be ON source and a reference position that s normally assumed to be OFF source i e free of emission The source signal is then calculated as the difference between ON and OFF The basic parameters are the offsets for the
159. l offset found with the POINTING observation After you enter a pointing setup manually we recommend to save it optionally to a named file SAVE POINTING FILE pointing 1 It can then at any later time be reloaded with pointing 1 see HELP SAVE 5 4 4 FOCUS Id demo bolometer focus pako v 0 2 2005 07 14 by Hans Ungerechts RECEIVER BOLOMETER SWWOBBLER 22 22 TPHASE 0 5 select Wobbler switching FOCUS 1 0 length mm NSUBSCANS 6 number of subscans TSUBSCAN 12 time per subscan PAUSE FOCUS OK to start c q a chance to check START start To execute this script simply enter demo bolometer focus 5 NCS USER S GUIDE 78 FOCUS measurements are done to optimize the position of the subreflector secondary along the tele scope axis by maximizing the intensity of the radiation focussed into the receiver s It is best done on a strong point source e g on a planet if or when its angular diameter is less than the beam width at the frequency to be observed It is strongly recommended to do a POINTING on the same source before a FOCUS FOCUS is normally used with BEAM SWITCHING or WOBBLER SWITCHING With the bolometer FOCUS is done with WOBBLER SWITCHING A calibration is not needed for FOCUS anyhow it will probably already have been done before the POINTING before the FOCUS After a focus the data processing software displays the results and you can enter a correction for the
160. letely clears the backend setup If option CLEAR is present all other parameters and options are ignored NOTE EMIR subbands IF cables and Backends The output signals from EMIR are transmitted to the spectrometers and NBC through 8 IF cables Each IF cable carries one subband of bandwidth 4 GHz LO LI UI or UO NBC 4MHz WILMA and VESPA can only be connected to IF cables 1 to 4 FTS parts 1 to 4 can also be connected to IF cables 1 to 4 The command options RECEIVER HORIZONTAL and RECEIVER VERTICAL allow to select up to 4 EMIR subbands that will be transmitted through IF cables 1 to 4 compare HELP RECEIVER HORIZONTAL and the EMIR user documentation This selection can include Outer subbands In addition for EMIR bands E090 E230 and E330 the IF cables 5 to 8 carry the 4 Outer subbands corresponding to the subbands selected for IF cables 1 to 4 E g if we select for IF 1 to 4 E230 ver UO E090 ver UI E230 hor UI E090 hor UI then the IF cables 5 to 8 will transmit E230 ver UO E090 ver UO E230 hor UO E090 hor UO Only FTS parts 5 to 8 can be connected to IF cables 5 to 8 BACKEND NBC WILMA FTS DEFAULT will automatically set the maximum number of backend parts for all available subbands BACKEND BBC is completely independant of the sub band selections for the IF cables NOTES for some backends the resolution and or bandwidth are fixed and the short syntax can be used The full syntax is supported for a
161. licitly entering the values of resolution and bandwidth 7 27 16 OPTIONS GAINIMAGE GAINIMAGE gainImage dB Specify the gain ratio of image to signal sidebands Real gainImage If dB is added after the value the ratio is assumed to be in dB otherwise a decimal fraction Simple standard values for these gain ratios can be found on the IRAM 30 m web pages Telescope Summary If you need accurate values for the single pixel heterodyne receivers you should measure them with CALIBRATE GAINIMAGE receiverName 169 7 PAKO LANGUAGE INTERNAL HELP 170 7 27 17 OPTIONS GREP GREP Does a grep search for the partial source name or string in the source catalog and lists any matching lines This search ignores the case This is only to help the user search through a source catalog Even if the match is unique the source found is not selected re enter the SOURCE command with the full source name 7 27 18 OPTIONS GRID GRID yes no Do a calibration subscan on a grid in front of the cold temperature load This is a special calibration option for polarization observations Logical doGrid default true IMPORTANT NOTE remember to turn this option off again for normal calibrations e 8 CALIBRATE GRID NO or CALIBRATE DEFAULT 7 27 19 OPTIONS HORIZONTAL HORIZONTAL sb1 sb2 HORIZONTAL n one EMIR subbands for Horizontal polarization This option applies only to EMIR Character sbi sb2 for
162. line catalog NOTE E090 clear previous receivers everything default NOTE E090 using line catalog line f SB from catalog NOTE E090 explicit options n explicit options SBs for Hori polar SBs for Vert polar Doppler correction image gain ratio COLD and AMB load temp forward and beam eff NOTE E090 H V full band se E090 H V LI UI 2 4 GHz BW E090 H V LO U0 for FTS for spectroscopy on full BW enter BACKEND FTS default NOTE E150 H V 1 subband 5 NCS USER S GUIDE receiver clear RECEIVER E150 CS 3 2 Horizontal LI Vertical LI say receiver clear RECEIVER E230 12C0 2 1 Horizontal LI UI Vertical LI UI say receiver clear RECEIVER E330 13C0 3 2 Horizontal LI UI Vertical LI UI say receiver clear RECEIVER E090 HCN 1 0 Hor LI Ver LI RECEIVER E150 CS 3 2 H LI V LI say say say pause say receiver clear RECEIVER E090 HCN 1 0 Hor UI Ver LI RECEIVER E150 CS 3 2 H none V LI say say 58 NOTE E150 H V LI 4 GHz BW NOTE E230 H V full band NOTE E230 H V LI UI 2 4 GHz BW E230 H V LO U0 for FTS NOTE E330 H V full band NOTE E330 H V LI UI 2 4 GHz BW E330 H V LO U0 for FTS NOTE E090 E150 H V LI E090 LO LSB Inner NOTE E090 H V LI 4 GHz BW E150 H V LI 4 GHz BW E090 H V LO for FTS NOTE E090 full BW E150 LI n LSB Inner NOTE E090 H UI V LI 4 GHz BW E150 V LI 4 GHz BW 5 NC
163. ll backends for VESPA always use the full syntax after changing the receiver configuration BACKEND CLEAR is recommended followed by the backend setup for the new receivers without that it is possible that pako will not accept BACKEND commands because of unresolved conflicts between the RECEIVER and BACKEND setups However the backend command will automatically try to disconnect backends that were connected to receiver sub bands that are not connected anymore 7 PAKO LANGUAGE INTERNAL HELP 97 7 2 1 BACKEND BBC BBC Broad Band Continuum Backend BBC works only with the EMIR receiver One part of BBC always covers the full bandwidth of one available sideband of each polarization of each selected EMIR band Band Sidebands Subbands IF Width Polariz BBC parts GHz GHz E090 LSB and USB 4 12 8 H and V 4 E150 LI or UI 4 8 4 H and V 2 E230 LSB and USB 4 12 8 H and V 4 E330 LSB and USB 4 12 8 H and V 4 Shortcut after selecting EMIR bands and subbands BACKEND BBC DEFAULT automatically sets all this appropriately Notes By convention in the paKo commands we refer to the IF range 4 to 8 GHz as subband LI or UI and to the IF range 4 to 12 GHz as sideband LSB or USB For E090 E230 and E330 the lower sideband LSB includes the lower outer LO and lower inner LI sub bands For E150 the lower sideband includes only the lower inner sub band i e in this case lower sideband and lower inner s
164. lt lt TBD topocentric lt lt TBD null Planets names are accepted Mercury Venus Mars Jupiter Saturn Uranus Neptune Pluto Satellites moons names are accepted if Phobos Deimos To Europa Ganymede Callisto Mimas Enceladus Tethys Dione Rhea Titan Hyperion Tapetus Miranda Ariel gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt gt as a special case if sourceName is one of sourceName is one of 150 7 PAKO LANGUAGE INTERNAL HELP 151 Umbriel Titania Oberon Gabriel Moon 7 17 1 SOURCE CATALOG CATALOG catalogName CATALOG Character catalogName Allows to specify that the search for a source should be done in the catalog file catalogName instead of the catalog specified with command CATALOG The default file extension is sou CATALOG Implies that the search will be done in the standard pointing source catalog iram J2000 sou 7 17 2 SOURCE GREP GREP Does a grep search for the partial source name or string in the source catalog and lists any matching lines This search ignores the case This is only to help the user search through a source catalog Even if the match is unique the source found is not selected re enter the SOURCE command with the full source name 7 17 3 SOURCE VELOCITY VELOCITY referenceFrame velocity Specify re
165. main unchanged from the last valid SUBSCAN command NOTES pako will make its best effort to guess the values for unspecified parameters based on the values of its internal variables after the previous valid SUBSCAN command Each time a SUBSCAN is accepted without error message a subscan is added to the list even if the command is only SUBSCAN by itself Be careful that a parameter in the command line can refer to different variables depending on the type of the segment subscan e g the 1st parameter can refer to xOffset xStart or xAmplitude These features should be used with special care e g to experiment with the DIYLIST and SUBSCAN commands It is recommended to collect all SUBSCAN commands in a paKo script and explicitly specify all parameters for each subscan Before START of a DIY subscanlist you can enter DIYLIST to review pako s I DIY messages listing the subscan currently defined this requires SET LEVEL 2 or lower e g PAKO gt set level 2 PAKO gt diy I DIY segments 1 to 3 I DIY 1 track on at 400 0 300 0 arcsec projection 10 0 s I DIY 2 onTheFly 300 0 200 0 to 330 0 220 0 arcsec projection 66 0 s I DIY 3 track on at 440 0 330 0 arcsec projection 10 0 s 7 PAKO LANGUAGE INTERNAL HELP 155 IMPORTANT LISSAJOUS OTF During a Lissajous OTF segment the position offsets x and y as a function of time t are x xCenter xAmplitude SIN 2 Pi frequencyX t phiX y yCenter yAmplitude SIN 2
166. mand by command explanation of how to do observations with the NCS Next is the NCS User s Guide 5 which follows the same outline as the Cook Book but includes more details The examples included here are all in the form of PAKO command language scripts The section NCS Explained 6 contains detailed explanations of some aspects of the NCS Finally the PAKO Language Internal Help is reproduced in section 7 A lot of information is intentionally duplicated in different sections of this manual so that e g the Cook Book and the User s Guide can be read independently It should not be necessary to read all sections in this manual Also much space is taken up by examples so the actual text to read is not very long We recommend that all users who face the NCS for the first time should read the Guide for the Perplexed Beginning observers and those who like to set up their observations one command at a time can then follow the Cook Book section 4 More experienced observers may prefer the User s Guide section 5 especially those who need more advanced options and those who like to prepare scripts with the specifications of their observations recommended All users may want to consult the section 6 NCS explained for general information or look up details in the HELP section 7 which is a complete reference for all commands and options Before starting observations users should als
167. massStep range of airmass for TIP Real airmassStart Real airmassEnd Real airmassStep NOTE 1 elevation ASIN 1 airmass NOTE 2 for slew tips TIP SLEW airmassStep has no effect airmassStart gt airmassEnd is allowed this implies elevation at start lt elevation at end i e TIP from low to high elevation for traditional TIP with SLEW no airmassStart lt airmassEnd i e they go from high to low elevation 7 PAKO LANGUAGE INTERNAL HELP 7 27 2 OPTIONS AMBIENT AMBIENT yes no Do a calibration subscan on the ambient temperature load Logical doAmbient default true 7 27 3 OPTIONS APPEND APPEND yes no Append to existing file do not create a new one Logical doAppend default false 7 27 4 OPTIONS CLEAR CLEAR yes no Completely clear a list of connected hardware e g receivers backends or parameters of the associated command 7 27 5 OPTIONS COLD COLD yes no Do a calibration subscan on the cold temperature load Logical doCold default true 7 27 6 OPTIONS CONNECT CONNECT yes no connect or disconnect the specified hardware e g backend or backend part 7 27 7 OPTIONS CROLOOP CROLOOP croLoop sequence of R off source Reference O On source subscans Character croLoop 167 7 PAKO LANGUAGE INTERNAL HELP 168 Example croLoop ROOR 7 27 8 OPTIONS DEFAULTS DEFAULTS yes no Restore default values fo
168. mation SIC PRIORITY 1 PAKO SET LEVEL 0 0 SET Project 111 22 SET PI Dr Lilo D Doe SET Observer John Doe SET Operator Pako SET Topology low SET doSubmit YES SHOW PAKO commands get precedence to get verbose chatter from pako project ID project number principal investigator topology for azimuth allow submission to Queue show parameters set with set e Specify the line catalog and the receiver setup CATALOG line my lin specify your line catalog RECEIVER CLEAR clear any previous RX setup RECEIVER E090 12C0 1 0 Horizontal Vertical The options Horizontal Vertical mean that both polarizations will be used e Select your target source from your catalog select a backend and do a calibration without sky to send the receiver setup CATALOG SOURCE my sou SOURCE W30H BACKEND CLEAR BACKEND WILMA default BACKEND 4MHz default CALIBRATE SKY NO START select your source catalog source W30H from your catalog clear any previous Backend setup simple spectrometer setup for EMIR simple spectrometer setup for EMIR doesn t need to move to sky position start PAKO S SIMPLEST RECIPE 22 e Let the operator tune the reciver s e Do a full calibration on the source with default parameters CALIBRATE DEFAULT default calibration START start e Look at the results and check with the operator if the receiver noise temperature is OK e Select a strong compact continuum source for pointing and focu
169. meter The basic parameters of this observing mode and its options are the azimuth the range and step in airmass and the time per subscan 5 4 6 ON OFF Wobbler Switching Id demo bolometer onoff pako v 0 2 2005 07 14 by Hans Ungerechts 5 NCS USER S GUIDE 79 RECEIVER BOLOMETER SWWOBBLER 3 3 0 33 0 Wobbler 33 arc sec TPHASE 0 5 0 5 seconds per phase SET ANGLEUNIT arcsec make sure angle unit is arc sec ONOFF SWWOBBLER ONOFF for Wobbler switching NSUBSCANS 16 number of subscans TSUBSCAN 16 time per subscan PAUSE ONOFF OK to start c q a chance to check START start To execute this script simply enter demo bolometer onoff For bolometer observations ONOFF is used with WOBBLER SWITCHING command SWWOBBLER When ONOFF is used with WOBBLER SWITCHING command SWWOBBLER the position offsets must be set to very specific values in TRUE ANGLE HORIZON depending on the parameters of SWWOBBLER This is achieved by using the special option SWWOBBLER of the command ONOFF Subscans are then taken alternating between 2 positions in such a way that a in some subscans one position of the antenna the source is in the first of the two Wobbler phases b in the other subscans the other position of the antenna the source is in the second of the two Wobbler phases During the data processing the source signal is computed as a double difference 1st the difference of the 2 Wob
170. mited to 12 characters 7 4 2 CATALOG LINE Line Catalog The format of a line in the line catalog is same as that of the 2nd 3rd and 4th parameter of the RECEIVER command lineName frequency SB with frequency in unit GHz see HELP RECEIVER Example 12C0 1 0 115 271204 UI for EMIR 12C0 2 1 230 537990 LI for EMIR 7 PAKO LANGUAGE INTERNAL HELP 7 5 7 6 7 6 7 6 12C0 2 1 230 537990 LSB for HERA IMPORTANT NOTE lineName is limited to 12 characters DISPLAY DISPLAY REDO Redo refresh the text in the display window DIYLIST DIYLIST User defined list of subscans and segments for observing mode DIY to define subscans see HELP SUBSCAN NB this is a protected command needs privilege DIYLIST without any parameters or options lists defined subscans and segments in the pako window this requires SET LEVEL 2 or lower in the pakoDisplay shows conditions e g maximum possible elevation plots defined subscans and segments depending on SET plotStyle 1 DIYLIST CLEAR CLEAR yes no Completely clear the used defined list of subscans and segments DIY 2 DIYLIST PURPOSE PURPOSE purpose Set a purpose for a scan i e an intended use of the data The applies in particular to DIYLIST 110 7 PAKO LANGUAGE INTERNAL HELP 111 Character purpose NOTE PURPOSE by itself or DIY clears the purpose NOTE at this time 2012 11 08 this is only for information
171. mos Io Europa Ganymede Callisto Mimas Enceladus Tethys Dione Rhea 52 5 NCS USER S GUIDE 53 SOURCE Titan PAUSE 1 SOURCE Hyperion PAUSE SOURCE Iapetus PAUSE SOURCE Miranda PAUSE SOURCE Ariel PAUSE SOURCE Umbriel PAUSE l SOURCE Titania PAUSE SOURCE Oberon PAUSE l RETURN We use the command SOURCE to select a source for observations Normally it is used after CATALOG SOURCE to select one of the sources from the source catalog Alternatively the parameters of the source can be specified directly on the command line using the same format as in the source catalog Pluto the planets and some of their Satellites are recognized directly by their name NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names For a full explanation of the parameters of the source command see HELP SOURCE Notes IMPORTANT All characters of the source name in the command SOURCE must match those of a source name in the source catalog or a name of a special source like a planet However the case of the source name is ignored for matching For example W30H w3oh W3oh all match W30H in the source catalog Mars Mars and mars all are recogn
172. n name resolu bandw fShift band polar SB E090 Horiz LI E090 Verti LI E230 Horiz LI E230 Verti LI BACKEND VESPA BACKEND VESPA BACKEND VESPA BACKEND VESPA PWN Fe o o IS o AS o o OO OO oooo 5 NCS USER S GUIDE pause backend clear BACKEND VESPA 1 1 250 320 0 0 0 E090 Horiz LI BACKEND VESPA 2 1 250 320 0 0 0 E090 Verti LI BACKEND VESPA 3 1 250 320 0 0 0 E230 Horiz LI BACKEND VESPA 4 1 250 320 0 0 0 E230 Verti LI pause EMIR VESPA autocorrelator basic mode with fShift optional line name backend clear BACKEND VESPA 1 0 040 40 0 120 0 E090 Horiz LI line EOHUO M BACKEND VESPA 2 0 040 40 0 120 0 E090 Horiz LI line EOHUO P BACKEND VESPA 3 0 040 40 0 100 0 E090 Verti LI line myLine3 BACKEND VESPA 4 0 040 40 0 110 0 E090 Verti LI line myLine4 BACKEND VESPA 5 0 040 80 0 150 0 E230 Horiz LI line BACKEND VESPA 6 0 040 80 0 150 0 E230 Horiz LI line apple BACKEND VESPA 7 0 040 80 0 200 0 E230 Verti LI line orange BACKEND VESPA 8 0 040 80 0 200 0 E230 Verti LI line red pause EMIR VESPA autocorrelator ultra high resolution mode backend clear BACKEND VESPA 1 0 0033 20 0 0 0 E090 Horiz LI BACKEND VESPA 2 0 0033 20 0 0 0 E090 Verti LI BACKEND VESPA 3 0 0066 20 0 0 0 E230 Horiz LI BACKEND VESPA 4 0 0066 20 0 0 0 E230 Verti LI pause backend clear 66 The command BACKEND has up to 8 parameters backend name logical part number
173. n ON and OFF 6 4 Observing Modes The NCS supports the following Observing Modes CALIBRATE POINTING FOCUS TIP ONOFF OTFMAP lt lt TBD RASTER not yet implemented gt gt TRACK VLBI All Observing Modes are realized by executing a sequence of 1 or more subscans In most cases the antenna moves between or during the subscans The observing modes are mutually exclusive i e at any time the system executes only one of them Several Observing Modes can be combined with different Switching Modes e g OTFMAP with TOTAL POWER WOBBLER SWITCHING for bolometer or FREQUENCY SWITCHING The Switching Mode should normally be specified before the Observing Mode 6 4 1 CALIBRATE In a standard calibration for heterodyne receivers we observe 3 subscans SAC on a Sky position an Ambient temperature load a k a hot load and a Cold load Calibrations are always and automat ically done in TOTAL POWER A calibration needs to be done for any heterodyne observation in order to get data with a calibrated intensity scale It is normally done before the target observations It must always be done after changing receiver and or backend setups It should also be done when changing sources and often enough to follow any variation of the athmosphere about every 15 minutes After you enter a calibrate setup manually we recommend to save it optionally to a named file SAVE CALIBRATE FILE calibrate 1 I
174. n 6 1 or ask an astronomer whi is familiar with the NCS For the time being it is recommended not to try fancy combinations of offsets which probably have not yet been fully tested and debugged 2 13 Receiver Setup and Calibration Parameters All parameters and options related to the setup of receivers and their calibration are specified with the command RECEIVER This includes ambient and cold load temperatures image sideband ratio forward and main beam efficiencies calibration scale antenna or main beam and the HERA derotator 2 14 Backends Backend setup for all backends is done with the command BACKEND 2 15 Continuous Data Acquisition and Data Streams In the NCS normally the data acquisition is continuous fast independent data streams are generated by the backends as well as other subsystems e g by the atenna mount drive to describe the antenna s movements The data processing software synchronizes the data from different streams based on time stamps in the data Most data streams keep continuously running even between subscans 2 16 Display of Parameters Most parameters set by the observer are displayed by a separate program pakoDisplay in another window see Figure 2 Several instances of this program can run at the same time including on different screens desktops and Linux machines 2 17 Preview Plots Commands for some observing modes e g otfmap automatically generate preview plots see
175. n Maimun Abu Amran Musa Cordoba 1135 Cairo 1204 From the Arabic Dalalat al Hairin translated into Hebrew as Moreh Neb kim 1204 and into Latin as Doctor Perplexorum Dux Dubitantium French translation entitled Guide des gar s Paris 1856 66 Here quoted from the English translation The Guide of the Perplexed London 1889 Index BACKEND 95 CLEAR 99 CONNECT 100 DEFAULTS 99 DISCONNECT 100 FINE 100 LINENAME 101 MODE 100 PERCENTAGE 101 RECEIVER 102 BBC 97 EXAMPLES 102 FTS 97 CALIBRATE 105 AMBIENT 106 COLD 106 DEFAULTS 106 GAINIMAGE 106 GRID 106 SKY 107 SYSTEM 107 TCALIBRATE 108 CATALOG 108 LINE 109 SOURCE 109 DISPLAY 110 DIYLIST 110 CLEAR 110 PURPOSE 110 FOCUS 111 DEFAULTS 111 NSUBSCANS 111 TSUBSCAN 112 EXAMPLES 112 Language 91 HELP 94 NEWS 92 LISSAJOUS 112 CENTER 113 FREQUENCY 114 PHASES 114 SYSTEM 114 TOTF 115 OFFSETS 115 CLEAR 117 DEFAULTS 117 SYSTEM 117 ONOFF 118 DEFAULTS 120 NSUBSCANS 120 REFERENCE 120 SWWOBBLER 120 SYMMETRIC 121 SYSTEM 122 TSUBSCAN 123 EXAMPLES 123 OPTIONS 166 AIRMASS 166 AMBIENT 167 APPEND 167 CLEAR 167 COLD 167 CONNECT 167 CROLOOP 167 DEFAULTS 168 DEROTATOR 168 DISCONNECT 168 DOPPLER 168 DOUBLEBEAM 168 EFFICIENCY 169 FILE 169 FINE 169 GAINIMAGE 169 GREP 170 GRID 170
176. n and taking data a high rate thus performing scans in the strict sense of the word This is a very fast mode for mapping The basic parameters of the command are the position offsets of the start and end of the first OTF subscan the basic parameters of the options are the number of OTF subscans the offsets of an off source reference position the step shift in x and y offsets between subsequent OTF subscans the time per OTF subscan in s and the time per off source reference subscan s This observing mode is normally used either with i TOTAL POWER with an off source reference for spectral line observations or ii FREQUENCY SWITCHING without off source reference for spectral line observations see below or iii WOBBLER SWITCHING and TRUE ANGLE HORIZON offsets for continuum mapping with the bolometer After you enter an OTF map setup manually we recommend to save it optionally to a named file SAVE OTFMAP FILE otfmap 1 It can then at any later time be reloaded with otfmap 1 see HELP SAVE 5 NCS USER S GUIDE 75 You may want to save the switching mode seperately or with OTFMAP into the same file SAVE SWITCHING FILE otfmap 2 SAVE OTFMAP FILE otfmap 2 APPEND And finally the demo for OTFMAP with FREQUENCY SWITCHING Id demo otfmap swfrequency pako demo rx BACKEND CLEAR BACKEND VESPA 1 0 040 40 0 0 0 E090 hor LI BACKEND VESPA 2 0 040 40 0 0 0 E090 ver LI BACKEND
177. n excute without actually trying to submit observations NOTE the operator also has to set the current observation queue to be that of the project account Submission from other projects will not be accepted by the NCS SET POINTING and SET FOCUS are used to set pointing and focus corrections 4 2 Specify your Source Catalog and or Source A source catalog is a special file containing information about sources to be observed in particular their coordinates and radial velocities The source catalog can be prepared with any text editor Here is an example Id demo sou v 1 0 1 2006 01 03 by Hans Ungerechts generated by ASTRO from IRAM CAT pointing sources 0003 380 EQ 2000 00 05 57 1352 38 20 14 869 LSR 0 000 FL 0 000 0 000 0048 097 EQ 2000 00 50 41 3193 09 29 05 122 LSR 0 000 FL 0 000 0 000 4 PAKO S COOK BOOK 0106 013 0112 017 0113 118 0119 041 0133 476 0135 247 0202 149 0212 735 0221 067 W30H 1958 179 K3 50A 2005 403 2007 776 2013 370 2021 317 2023 336 2037 511 2059 034 NGC7027 2113 293 2121 053 2128 123 2131 021 2134 004 2136 141 2145 067 2200 420 2201 315 2210 257 2216 038 2223 052 2230 114 2234 282 2243 123 2251 158 2254 617 2255 282 NGC7538 2318 049 The following sources are Si0 masers and are useable for pointing EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ EQ
178. n parallel to E230 Horiz LI and E230 Verti LI both must be selected in RECEIVER command 11 HERA with FTS wide bandwidth receiver clear RECEIVER HERA1 WIDTH wide RECEIVER HERA2 WIDTH wide backend clear BACKEND FTS 1 RECEIVER HERA1 BACKEND FTS 2 RECEIVER HERA2 HERA narrow bandwidth with FTS fine resolution receiver clear RECEIVER HERA1 WIDTH narrow RECEIVER HERA2 WIDTH narrow backend clear BACKEND FTS 1 FINE RECEIVER HERA1 BACKEND FTS 2 FINE RECEIVER HERA2 CALIBRATE CALIBRATE no parameters Specify a calibration measurement with the heterodyne receivers normally with subscans SAC Sky Ambient temperature load Cold load NOTE CALIBRATE is always and automatically done with switching mode total and the time per phase is adjusted to be in the range 0 1 to 0 5 sec SKY xOffsetC yOffsetC or SKY NO do not do sky calibration Do a calibration subscan on sky Real xOffsetC x offset Real yOffsetC y offset NOTES with the usage SKY x0ffsetC yOffsetC both parameters are required but you can replace either parameter with to leave it unchanged The system for the offsets is selected through the option SYSTEM 105 7 PAKO LANGUAGE INTERNAL HELP 7 3 1 CALIBRATE DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 3 2 CALIBRATE AMBIENT AMBIENT yes no Do a calibration subscan on th
179. ndwidth mode Character width width choices WIDE NARROW NOTE Option WIDTH NARROW changes the local oscillator setup of receivers HERA1 HERA2 in such a way that a line in the center of the receiver bandwidth appears in the center of the bands of VESPA Spectrometers with 1GHz or more bandwidth normally require WIDTH WIDE gt NOTE THIS OPTION DOES NOT APPLY TO EMIR 7 13 14 RECEIVER EXAMPLES Id demo receiver pako basic RECEIVER EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts CATALOG line demo EMIR lin specify line catalog RECEIVER CLEAR clear all receivers previously set say 1 NOTE E090 band receiver clear RECEIVER E090 12C0 1 0 line f SB from catalog Horizontal SB from catalog Vertical SB from catalog f frequency SB sideband subband pause say NOTE E090 band receiver clear REC E090 12C0 1 0 115 271204 UO Horizontal U0 Vertical UO line f SB explicit SB explicit SB explicit say NOTE E090 H amp V 4 GHz BW pause say 1 NOTE E090 E150 bands receiver clear RECEIVER E090 HCN 1 0 Hor LI LSB Inner Ver LI LSB Inner RECEIVER E150 CS 3 2 H LI LSB Inner V LI LSB Inner say 1 NOTE E090 H V 4 GHz BW say ms E150 H V 4 GHz BW pause 7 PAKO LANGUAGE INTERNAL HELP say receiver clear RECEIVER E090 RECEIVER E230 say say pause say HCN 1 0 Hor Ve
180. ned Azimuth Topology 7 15 7 SET EMIRCHECK SET EMIRcheck emirCheck emirCheck Character Choices for emirCheck are strict relaxed loose Make the checking of frequency limits less than strict This allows to command frequencies that are completely outside the designed and tested range of the receiver bands The standard and recommended limit checking corresponds to strict THIS MUST BE USED CAREFULLY AND ONLY IN CONSULTATION WITH STAFF ASTRONOMERS OR ENGINEERS 7 15 8 SET LIMITCHECK SET LIMITCHECK limitCheck limitCheck Character len 24 Choices for limitCheck are strict relaxed loose Make the checking of some limits less than strict 7 PAKO LANGUAGE INTERNAL HELP 147 The standard and recommended limit checking corresponds to strict THIS MUST BE USED CAREFULLY AND ONLY IN CONSULTATION WITH STAFF ASTRONOMERS OR ENGINEERS NB this is a protected command needs privilege 7 15 9 SET USERLEVEL SET USERLEVEL userLevel userLevel Character len 24 Choices for userLevel are beginner normal experienced Sets level of user s experience with paKo and the NCS Some features that require special care are only available if userLevel is set to a higher level 7 15 10 SET EXAMPLES Id demo set pako basic SET EXAMPLES v 1 1 1 2009 05 18 Hans Ungerechts SIC PRIORITY 1 PAKO PAKO commands get precedence over similar GREG commans SET Project 111 22 project ID
181. ntil nOtf OTF subscans have been generated starting with first letter in the croLo op IF THE CROCODE LETTER IS R AND REFERENCE IS TRUE 1 subscan tracking the fixed off source reference position is IF generated THE CROCODE LETTER IS 0 1 linear OTF subscan is generated The start and end positions of the first OTF subscan are parameters xStart yStart xEnd yEnd of the OTFMAP command For the second and all following OTF subscans xStart yStart xEnd yEnd of the previous OTF subscan are incremented by parameters dx and dy of option step If zigzag is true xStart yStart and xEnd yEnd are interchanged Then the next letter code in the croLoop is considered in th e same way If reference is true a croCode ending in R will ensure that an off source reference subscan follows the last OTF subscan CROL OOP croLoop sequence of R off source Reference 125 7 PAKO LANGUAGE INTERNAL HELP 126 O On source subscans Character croLoop Example croLoop ROOR NOTF nOtf Integer nOtf number of OTF on the fly subscans REFERENCE xOffsetR yOffsetR systemNameRef or REFERENCE NO no reference position of off source reference subscans Real xOffsetR x offset Real yOffsetR y offset Character systemNameRef name of system see SYSTEM for choices NOTE with the usage REFERENCE xOffsetR yOffsetR both parameters are requi but you can replace eit
182. o review the up to date notes on the NCS wiki pages at NCS Wiki at https mrt lx1 iram es mainWiki FrontPage 2 PAKO GUIDE OF THE PERPLEXED 10 e0 ssh paKo 140x32 282 I BACKEND no receiver name specified as parameter I BACKEND no 2nd receiver name specified as parameter I BACKEND Continuum total hardware used 0 0 I BACKEND 100kHz total hardware used 0 0 I BACKEND 1MHz total hardware used 0 0 I BACKEND 4MHz total hardware used 100 0 I BACKEND USB total hardware used 0 0 I BACKEND WILMA total hardware requested 100 0 I BACKEND VESPA total hardware used 33 3 I BACKEND 4MHz 1 4 000 4024 0 248 0 E090 horiz UO none 100 0 none I BACKEND 4MHz 2 4 000 4024 0 248 0 E090 verti UI none 100 0 none I BACKEND WILMA 1 2 000 3720 0 265 0 E090 horiz UO none 100 0 none I BACKEND WILMA 2 2 000 3720 0 265 0 E090 verti UI none 100 0 none I BACKEND WILMA 3 2 000 3720 0 265 0 E230 horiz LI none 100 0 none I BACKEND WILMA 4 2 000 3720 0 265 0 E230 verti LI none 100 0 none I BACKEND VESPA 1 0 040 40 0 0 0 E090 horiz UO none 90 0 CO 1 0 I BACKEND VESPA 2 0 040 40 0 0 0 E090 verti UI none 90 0 myLine2 I BACKEND VESPA 3 0 040 40 0 0 0 E230 horiz LI none 90 0 I BACKEND VESPA 4 0 040 40 0 0 0 E230 verti LI none 90 0 LILO PAKO gt show I SHOW paKo Revision v 1 1 1 2009 04 14 T SHOW Level For standard output 0 For file I SHOW Queue doSubmit F I SHOW
183. o the local oscillator e the lower inner sub band LI from about 8 GHz to 4 GHz e the upper inner sub band UI from about 4 GHz to 8 GHz and e the upper outer sub band UO from about 8 GHz to 12 GHz If we select LO LI UI UO as EMIR sub band in the line catalog or directly in RECEIVER the localoscillator will be adjusted so that the specified line frequency goes into that EMIR sub band For details see the EMIR user guide For HERA the sideband must be LSB lower sideband Lines starting with a are comments The standard file extension for line catalogs is 1in NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names 4 3 2 Setup of the Receivers Frontends Id demo receiver pako basic RECEIVER EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts CATALOG line demo EMIR 1lin specify line catalog RECEIVER CLEAR clear all receivers previously set say 1 NOTE E090 band receiver clear RECEIVER E090 12CQ 1 0 line f SB from catalog Horizontal SB from catalog Vertical SB from catalog f frequency SB sideband subband pause say 1 NOTE E090 band receiver clear REC E090 12C0 1 0 115 271204 UO Horizontal U0 Vertical UO line f SB explic
184. ojection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 PAKO LANGUAGE INTERNAL HELP 7 10 7 ONOFF TSUBSCAN TSUBSCAN tSubscan time per subscan Real tSubscan time 7 10 8 ONOFF EXAMPLES Id demo onoff pako ONOFF SWTOTAL EXAMPLE v 1 1 1 2009 05 05 POSITION SWITCHING demo rx spectrometers SET ANGLE arcsec SWTOTAL TPHASE CALIBRATE AMBIENT COLD SKY SYSTEM TCALIBRATE I 0 5 600 0 0 0 projection 5 0 PAUSE CALIBRATE OK to start c q START ONOFF 40 0 30 NSUBSCANS 12 REFERENCE 600 0 O SYSTEM projection SYMMETRIC TSUBSCAN 30 PAUSE ONOFF SWTOTAL OK to START Comments 1 we assume here that the see demo source Id demo onoff swwobbler O projection
185. ough so that line signals from the 2 phases of the switching cycle are well separated The spectral baseline will generally be less flat than in other switching modes Some spectral lines are also emitted in the earth s mesosphere e g the mesopheric lines from 12 CO are rather strong and they will be seen in FREQUENCY SWITCHING spectra taken toward astronomical sources with a low Doppler shift The mesospheric lines will appear at a frequency and velocity that corresponds to the rest frame of the athmosphere i e the observatory Care must be taken that they are not confused with the lines from the astronomical source Information computed by the ASTRO software can help with this decision When observing sources near the plane of the Milky Way line emission from clouds at other velocities than the target source e g other spiral arms can cause confusion In case of doubt consult the special memo on FREQUENCY SWITCHING or ask an experienced FRE QUENCY SWITCHING observer 6 3 3 Wobbler Switching During WOBBLER SWITCHING the wobbling secondary mirror is switched between 2 positions which are offset from the telescope axis by a fixed amount Thus there are 2 phases and the signal is calculated as the difference between these 2 phases As the positions in both phases are offset from the telescope axis in some observing modes e g POINTING FOCUS ONOFF the telescope position needs to be adjusted to compensate this is done a
186. ource catalog specified with CATALOG SOURCE fileName The sourceName in the command must match a source name in the source catalog with all characters no minimum match but the case is ignored for the matching Example SOURCE w3o0h matches W30H in the source catalog but SOURCE w3o does not The option VELOCITY systemVelocity velocity overrides the values in the catalog Epoch can optionally start with a 1 character code J or B to distinguish between J and B epochs equatorial coordinates If this code letter is not present J is implied The coordinates are specified in astronomical sexagesimal format with as field separator i e hh mm ss ss ddd u uu Examples 12 34 56 78 for 12 hours 34 minutes 56 78 seconds 123 45 67 89 for 123 degrees 45 arc minutes 67 89 arc seconds For systemName equatorial and haDec the longitude lambda is 7 PAKO LANGUAGE INTERNAL HELP assumed to be in hours for all other systems it is assumed to be in degrees Latitude beta is always in degrees Choices for systemName equatorial horizontal lt lt TBD not yet supported lt lt TBD galactic lt lt TBD apparentEquatorial lt lt TBD ecliptic lt lt TBD apparentEcliptic lt lt TBD haDec Choices for referenceFrame LSR barycentric heliocentric lt lt TBD not yet supported lt lt TBD 3K lt lt TBD galactocentric lt lt TBD body lt lt TBD geocentric
187. pako The Observer s User Interface to the New Control System at the IRAM 30 Meter Telescope Title paKo Observer s User Interface to the NCS at the 30 M Telescope Identifier MasterURL http www iram es IRAMES documents ncs30mPako File pako Revision NIKA E150 switch box v 1 1 14 Revision Date 2012 12 01 Expiration Date 2013 11 31 Supersedes v1 1 11 Is superseded by Authors Hans Ungerechts Contributors Joaquin Santiago Affiliations IRAM Granada Addresses Avenida Divina Pastora Local 20 18012 Granada Spain Audience observers operators astronomers Publisher IRAM Granada Subject NCS 30m Observer s User Interface paKo Keywords NCS Documentation User Interface Observer Description about this document This is the documentation of the observer s user interface to the New Control System NCS The user IF program is nicknamed PAKO paKo for astronomers K c ontrol of observations Revision v 1 1 12 introduced support for GISMO and the observing mode Lissajous Revision v 1 1 14 supports NIKA SUBSCAN TUNE for NIKA and the modification 2012 10 of the switch box for E150 README Observers who are new to the NCS are encouraged to read sections 1 2 and 4 Note that much of the space in these sections is taken up by examples so the actual text is not very long or hard to read References and Related Documents Short List New Control System for the 30m Telescope
188. pear in the spectra at 1 the velocity of the Local Standard of Rest relative to the observatory 7 PAKO LANGUAGE INTERNAL HELP 159 Care must be taken that mesospheric lines are not confused with the lines from the astronomical source which will appear in the spectrum at the velocity of the source relative to the LSR The ASTRO software can calculate the velocity of the LSR relative to the observatory for any source and time During observations this velocity is also displayed on one of the NCS monitoring windows When observing sources near the plane of the Milky Way line emission from clouds at other velocities than the target source e g other spiral arms can cause confusion In case of any doubt there is a special report on FS that gives more advice 7 21 1 SWFREQUENCY DEFAULTS DEFAULTS yes no Restore default values for all parameters and options 7 21 2 SWFREQUENCY RECEIVER RECEIVER receiverBand Character receiverBand receiver EMIR band Choices for receiverBand are E090 E150 E230 E330 HERA1 HERA2 7 21 3 SWFREQUENCY TPHASE TPHASE tPhase time per switching PHASE Real tPhase time 7 21 4 SWFREQUENCY EXAMPLES SWFREQUENCY EXAMPLES v1 1 2009 05 11 Hans Ungerechts SWFREQUENCY default Defaults SWFREQUENCY 3 8 3 8 for all receiver bands SWFREQUENCY 3 9 3 9 receiver E090 for EMIR band E090 SWFREQUENCY 11 7 11 7 receiver E230 for EMIR band E230 SWF
189. projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 10 ONOFF ONOFF xOffset yOffset Specify on off measurement a k a position switching Real xOffset x offset of on source position Real yOffset y offset of on source position Character sourceName name of on source position NOTE if SWWOBBLER is the selected switching mode the special option SWWOBBLER YES TRUE is implied even without specifying it and the on off parameters appropriate for on off Wobbler switching are set If SWWOBBLER and ONOFF are combined in the standard way we effectively take data at 3 positions 1 the source position 2 the source position throw offset in the true angle horizontal syste 3 the source position throw offset in the
190. r 12C0 2 1 Horizontal Vertical receiver clear RECEIVER E150 RECEIVER E330 say say pause Pitt RECEIVER CS 3 2 H V 13C0 3 2 H V clear LI LI LI LI LI LI NOTE E090 E230 bands LSB Inner LSB Inner LSB Inner LSB Inner NOTE E090 H V 4 GHz BW E230 H V 4 GHz BW 1 NOTE E150 E330 bands LSB Inner LSB Inner LSB Inner LSB Inner NOTE E150 H V 4 GHz BW NOTE E330 H V 4 GHz BW clear all receivers previously set REC HERA1 12C0 2 1 230 537990 LSB REC HERA2 12C0 2 1 230 537990 LSB pause 7 14 SAVE SAVE commandToSave SAVE ALL CORRECTIONS SAVE SET CORRECTIONS SAVE SWITCHING Save parameters and options of a command in the form of a valid pako script Character commandToSave command to save If commandToSave is not specified the last selected observing mode is saved 141 7 PAKO LANGUAGE INTERNAL HELP 142 SAVE ALL saves nearly all current setup parameters as well as the current switching and observing modes to file all pako or to a different file specified with FILE NOTE SAVE ALL and SAVE SET save the pointing and focus corrections only if they are used in the form SAVE ALL C ORRECTIONS SAVE SET C ORRECTIONS Normally SAVE ALL and SAVE SET are meant to generate paKo scripts that can be used to re produce the setup at a later time when one probably wants to use different corrections On the other
191. r EMIR band E090 SWFREQUENCY 11 7 11 7 receiver E230 for EMIR band E230 SWFREQUENCY tphase 0 20 same for all receivers bands CALIBRATE AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start TRACK 40 0 30 0 offsets of on position NSUBSCANS 5 number of subscans SYSTEM projection system for offset TSUBSCAN 60 time per subscan PAUSE TRACK SWFREQUENCY OK to start c q START start 1 a Chance to check Comments we assume here that the source already has been selected see demo source The TRACK observing mode simply tracks one position relative to the source It is normally used with FREQUENCY SWITCHING and offsets in SYSTEM projection The basic parameters are the offsets for the position to track parameters of the options are the total number of subscans and the time per subscan in s After you enter a track setup manually we recommend to save it optionally to a named file SAVE TRACK FILE track 1 It can then at any later time be reloaded with track 1 see HELP SAVE You may want to save the switching mode seperately or with TRACK into the same file SAVE SWITCHING FILE track 2 SAVE TRACK FILE track 2 APPEND Notes IMPORTANT FREQUENCY SWIT
192. r all parameters and options 7 27 9 OPTIONS DEROTATOR DEROTATOR angle system Specify derotator angle for HERA Real angle in units deg Character system Choices for system Nasmyth horizon equatorial frame same as Nasmyth sky same as equatorial NOTES The last 2 are for consistency with old control system and HERA conve This option works only for RECEIVER HERA1 or RECEIVER HERA2 of course it s same angle for HERA1 and HERA2 7 27 10 OPTIONS DISCONNECT DISCONNECT disconnect the specified hardware e g backend or backend part 7 27 11 OPTIONS DOPPLER DOPPLER doppler Character doppler apply doppler correction choices DOPPLER FIXED 7 27 12 OPTIONS DOUBLEBEAM DOUBLEBEAM yes no Pointing do a double beam pointing Logical doDoubleBeam 7 PAKO LANGUAGE INTERNAL HELP This is valid only for pointing with Wobbler switching SWWOBBLER This option has an effect only if SET 2nRotation 0 0 7 27 13 OPTIONS EFFICIENCY EFFICIENCY forwardEfficiency beamEfficiency specify forward and beam efficiencies Real forwardEfficiency Real beamEfficiency 7 27 14 OPTIONS FILE FILE fileName Specify file name Character fileName 7 27 15 OPTIONS FINE FINE for BACKEND FTS select the fine mode with a resolution of 0 049 MHz Note with the option DEFAULT or the short syntax this allows to select the fine resolution without exp
193. r with to leave it unchanged 7 27 26 OPTIONS SCALE SCALE scale Select the calibration intensity scale Character scale choices ANTENNA BEAM If scale is ANTENNA the scale is antenna temperature If scale is BEAM the scale is main beam temperature 7 27 27 OPTIONS SKY SKY xOffsetC yOffsetC or SKY NO do not do sky calibration Do a calibration subscan on sky 7 PAKO LANGUAGE INTERNAL HELP 173 Real xDffsetC x offset Real yOffsetC y offset NOTES with the usage SKY x0ffsetC yOffsetC both parameters are required but you can replace either parameter with to leave it unchanged The system for the offsets is selected through the option SYSTEM 7 27 28 OPTIONS SPEED SPEED speedi speed2 speed of OTF subscans Real speedl speed at start Real speed2 speed at end For OTFMAP speed2 speedi In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 27 29 OPTIONS STEP STEP dx dy Step shift or translation between lines in a map Real sirak shift in x offsets Real dy shift in y offsets 7 27 30 OPTIONS SWWOBBLER SWWOBBLER yes no option of command ONOFF set parameters appropriate for on off Wobbler switching Logical doSwWobbler If switching mode SWWOBBLER has been selected the following parameters of ONOFF are set according to wOffset1 and wOffset2
194. rad for x Real phiY phase offset rad for y 7 8 4 LISSAJOUS SYSTEM SYSTEM systemName Name of system for offsets Character systemName name of system one of PROJECTION TRUEHORIZON NASMYTH lt lt TBD DESCRIPTIVE gt gt lt lt TBD BASIS gt gt lt lt TBD EQUATORIAL gt gt lt lt TBD HADECL gt gt lt lt TBD HORIZONTAL gt gt PROJECTION for now means only the standard simple radio projection offsets in the chosen coordinate system This is normally the astronomical system of offsets in which point by point TRACK ONOFF or on the fly OTFMAP maps are made TRUEHORIZON means the horizontal system with a factor 1 cos elevation applied to the azimuth offset NASMYTH are special offsets to point an off center pixel of a focal plane array receiver bolometer HERA to the commanded astronomical position e g to use an off center pixel for pointing 7 PAKO LANGUAGE INTERNAL HELP 115 focus ONOFF IMPORTANT NOTE projection trueHorizon If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM projection OFFSETS SYSTEM projection is ignored not used If the observing mode LISSAJOUS ONOFF OTFMAP is in SYSTEM trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0ffset yOffset are used during the observations t
195. receiver s and backends Remember to select the appropriate backend before Calibrate normally a continuum backend for POINTING and FOCUS and spectrometer s for TRACK ONOFF and heterodyne OTFMAPs In a standard calibration for heterodyne receivers we observe 3 subscans SAC on a Sky posi tion an Ambient temperature load a k a hot load and a Cold load Calibrations are always and automatically done in TOTAL POWER A calibration needs to be done for any heterodyne observation in order to get data with a calibrated intensity scale It is normally done before the target observations It must always be done after changing receiver and or backend setups It should also be done when changing sources and often enough to follow any variation of the athmosphere about every 15 minutes After you enter a calibrate setup manually we recommend to save it optionally to a named file SAVE CALIBRATE FILE calibrate 1 It can then at any later time be reloaded with calibrate 1 see HELP SAVE 5 3 5 POINTING Id demo pointing pako POINTING EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts SOURCE Mars OFFSETS CLEAR clear previously set offsets demo rx demo setup of EMIR REPLACE WITH YOUR SETUP BACKEND CLEAR clear previous backend setup BACKEND BBC Default connect 1 part to each 5 NCS USER S GUIDE 68 EMIR subband selected 1 SET ANGLEUNIT arcsec make sure
196. s normally used with BEAM SWITCHING or WOBBLER SWITCHING With the bolometer FOCUS is done with WOBBLER SWITCHING A calibration is not needed for FOCUS anyhow it will probably already have been done before the POINTING before the FOCUS After a focus the data processing software displays the results and you can enter a correction for the observed focus offset with the command SET FOCUS focusCorrection Note that this is the total correction i e the previous correction plus the additional offset found with the FOCUS observation The optiomal focus correction for different receiver bands may be slightly different by a few times 0 1 mm and the observer can decide to optimize for one particular band or use a compromise value After you enter a focus setup manually we recommend to save it optionally to a named file SAVE FOCUS FILE focus 1 It can then at any later time be reloaded with focus 1 see HELP SAVE 4 PAKO S COOK BOOK 39 4 3 8 TRACK Single Position with Frequency Switching Id demo track pako demo rx BACKEND CLEAR BACKEND VESPA 1 0 040 40 BACKEND VESPA 2 0 040 40 BACKEND VESPA 3 0 080 80 BACKEND VESPA 4 0 080 80 SET ANGLE arcsec SWFREQUENCY D O O 0 oooo oooo W om m 3 9 3 9 SWFREQUENCY 11 7 11 7 SWFREQUENCY tphase CALIBRATE AMBIENT COLD SKY 600 0 0 0 SYSTEM projection TCALIBRATE 5 0 PAUSE CALIBRATE OK to start c q STAR
197. script in a file named yoda pako enter at the prompt PAKO gt yoda 4 1 Set General Information Id demo set pako basic SET EXAMPLES v 1 1 1 2009 05 18 Hans Ungerechts SIC PRIORITY 1 PAKO SET Project 111 22 SET PI Dr Lilo D Doe SET Observer John Doe SET Operator Pako SET Topology low PAKO commands get precedence over similar GREG commans project ID project number principal investigator topology for azimuth SET Level 3 w suppress informational messages I messages from paKo DEVICE image w for plots SHOW show the values set with set NOTE don t use special characters like lt gt amp accents in the names 11 Id demo set2 pako 4 PAKO S COOK BOOK 25 additional SET EXAMPLES v 1 1 1 2009 05 08 Hans Ungerechts I SET doSubmit YES to allow submission to Queue 1 SET Pointing 1 1 2 2 pointing corrections SET Focus 2 3 focus correction mm 1 SHOW show the values set with set SIC PRIORITY 1 PAKO assures that PAKO commands have priority over similar other commands e g POI will be understood as PAKO POINTING and not as GREG1 POINTS With the SET commands we specify some basic information the project number the principal inves tigator PI the names of the observer and telescope operator NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one c
198. set found with the POINTING observation After you enter a pointing setup manually we recommend to save it optionally to a named file SAVE POINTING FILE pointing 1 It can then at any later time be reloaded with pointing 1 see HELP SAVE 5 3 6 FOCUS Id demo focus pako FOCUS EXAMPLE v 1 1 1 2009 05 08 Hans Ungerechts SWBEAM to select beam switching FOCUS 2 0 length mm NSUBSCANS 6 number of subscans 5 NCS USER S GUIDE 69 TSUBSCAN 12 time per subscan PAUSE FOCUS OK to start c q a chance to check START start Comments We assume here that a pointing measurement has been done immediately before the FOCUS strongly recommended see demo pointing and therefore we assume here that source receivers and backends already have been selected and set up If you want the intensity of the Focus data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before FOCUS measurements are done to optimize the position of the subreflector secondary along the tele scope axis by maximizing the intensity of the radiation focussed into the receiver s It is best done on a strong point source e g on a planet if or when its angular diameter is less than the beam width at the frequency to be observed It is strongly recommended to do a POINTING on the same source before a FOCUS FOCUS is normally used with BEAM SWITCHING or WOBBLER SWITCHING
199. sets are always in system trueHorizon and are specified implicitly though the angular length of the subscans Global Offsets On the other hand the command OFFSETS can be used to specify additional position offsets in other systems These globally defined offsets stay fixed during a complete scan They are only needed in special cases e g the Nasmyth offsets or for ONOFF with wobbler switching see below At this time 2012 12 01 the command OFFSETS supports offsets in the following 3 systems projection Offsets in the radio projection see above trueHorizon true angle horizon offsets in Azimuth and Elevation Aa a Gsource cos e Ae e Esource where a and e are the Azimuth and Elevation of the telescope Gsource and Csource are the Azimuth and Elevation of the source calculated from l and b and the time and other parameters 5 In particular for equatorial coordinates corresponds to Right Ascension and b to Declination 6 For the equations all angles are assumed to be in radian 6 NCS EXPLAINED 82 Nasmyth offsets in the Nasmyth receiver cabin system The purpose of Nasmyth offsets is exclusively to re position the telescope so that an off center element of a multibeam receiver looks at the position where otherwise the center pixel would look E g OFFSETS 33 44 SYSTEM Nasmyth adds offsets 33 and 44 in the Nasmyth system for all observing modes Example 1 Observe a single position with offsets
200. simple spectrometer setup for EMIR default calibration start BACKEND WILMA Default connects one part of the WILMA spectrometer to each EMIR sub band selected with RECEIVER BACKEND 4MHz Default connects one part of the WILMA spectrometer to 2 EMIR sub bands selected with RECEIVER e Select your switching and observing mode e g wobbler switching and on off and start observing SWWOBBLER 120 0 120 0 TPHASE 2 0 wobbler 120 arc sec 2 seconds per phase ONOFF NSUBSCANS 12 SYMMETRIC TSUBSCAN 30 12 subscans symmetric subscan sequence 30 sec per subscans START e Do acalibration at least every 15 minutes or when you change sources or when you change receiver and backend setups e Do a pointing every 2 hours or when you change to a different region of the sky e Do a focus every 6 hours and after sunset and sunrise Before focus do a pointing on the focus source e HAVE FUN NOTES PAKO has built in help for all commands e g HELP SWWOBBLER HELP ONOFF NSUBSCANS Most commands can be abbreviated substantially e g the following 2 are equivalent ON NS 16 SYM TS 22 ONOFF NSUBSCANS 16 SYMMETRIC TSUBSCAN 22 If you find that you enter the same command s very often it is not necessary to type them every time They can be put into command scripts either by editing a file or with PAKO s SAVE command see section 2 t Other spectrometers e g VESPA offer much more flexibility but also
201. specified line frequency goes into that EMIR sub band For details see the EMIR user guide For HERA the sideband must be LSB lower sideband Lines starting with a are comments The standard file extension for line catalogs is 1in NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names Note that this format is like the format that can be used directly with RECEIVER see HELP RECEIVER and also like the line catalog format used at PLATEAU DE BURE and in the old control system of the 30 M Telescope 5 3 2 Setup of the Receivers Frontends Id demo receiver pako basic RECEIVER EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts CATALOG line demo EMIR 1lin specify line catalog 5 NCS USER S GUIDE RECEIVER CLEAR say receiver clear RECEIVER E090 12C0 1 0 Horizontal Vertical pause say receiver clear REC E090 12C0 1 0 115 271204 UO Horizontal UO Vertical UO say pause say receiver clear RECEIVER E090 HCN 1 0 Hor LI Ver LI RECEIVER E150 CS 3 2 H LI V LI say say pause l say receiver clear RECEIVER E090 HCN 1 0 Hor LI Ver LI RECEIVER E230 12C0 2 1 Horizontal LI Vertical LI say say pause say receiver clear RECEIVER E15
202. ssing if possible choose a source that is smaller than your beam SOURCE 2251 158 catalog iram J2000 sou pointing source from catalog SOURCE Uranus OR a small planet e Select the continuum backend for pointing and focus BACKEND CLEAR BACKEND BBC Default BACKEND BBC Default connects one part of the continuuum backend BBC to each polar ization and sideband of each selected EMIR band e Select beam switching mode and do a pointing SWBEAM to select beam switching POINTING default pointing START start e After a pointing the data processing software displays the results and you can enter a correction for the observed pointing offsets with the command Let s say the results are 3 4 and 1 2 arc sec SET POINTING 3 4 1 2 e Do a focus measurement FOCUS 2 0 length mm START start e After a focus the data processing software displays the results and you can enter a new focus correction e g 2 1 mm with the command SET FOCUS 2 1 e Select a pointing source that is near your target source and do another pointing measure ment and enter the resulting correction e Select the target source from your catalog select a backend and do a calibration 3 PAKO S SIMPLEST RECIPE 23 SOURCE W30H BACKEND CLEAR BACKEND WILMA default BACKEND 4MHz default CALIBRATE DEFAULT START source W30H from your catalog clear any previous Backend setup simple spectrometer setup for EMIR
203. t c q START RETURN NOTE clear previously set offsets demo setup of EMIR REPLACE WITH YOUR SETUP clear previous backend setup connect 1 part to each EMIR subband selected make sure angle unit is arc sec to select beam switching reset all options pointing with subscan length 120 4 OTF subscans 30 seconds per OTF subscan a chance to check start if you use NASMYTH offsets for an off center pixel of a mutlibeam receiver don t use OFFSETS CLEAR If you want the intensity of the Pointing data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before the pointing POINTING observations are done to optimize the positioning of the telescope in Azimuth and Elevation This is normally done by continuum observations of a cross scan in azimuth and elevation on a point source or at least a small source near the intended target source It is normally used with BEAM SWITCHING or WOBBLER SWITCHING it is also possible with TOTAL POWER With the bolometer POINTING is done with WOBBLER SWITCHING A calibration is not needed for POINTING if one is only interested in the pointing corrections and not in the source intensity After a pointing the data processing software displays the results and you can enter a correction for the observed pointing offsets with the command SET POINTING azimuthCorrection elevationCorrection 4 PAKO S COOK BOOK 38 Note that this
204. t can then at any later time be reloaded with calibrate 1 see HELP SAVE The special calibration subscans are done by switching the beam optics so that the receivers see a special calibration unit in the receiver cabin 6 4 2 POINTING POINTING observations are done to optimize the positioning of the telescope in Azimuth and Elevation This is normally done by continuum observations of a cross scan in azimuth and elevation on a point source or at least a small source near the intended target source It is normally used with BEAM SWITCHING or WOBBLER SWITCHING it is also possible with TOTAL POWER With the bolometer POINTING is done with WOBBLER SWITCHING A calibration is not needed for POINTING if one is only interested in the pointing corrections and not in the source intensity 6 NCS EXPLAINED 87 After a pointing the data processing software displays the results and you can enter a correction for the observed pointing offsets with the command SET POINTING azimuthCorrection elevationCorrection Note that this is the total correction i e the previous correction plus the additional offset found with the POINTING observation After you enter a pointing setup manually we recommend to save it optionally to a named file SAVE POINTING FILE pointing 1 It can then at any later time be reloaded with pointing 1 see HELP SAVE 6 43 FOCUS FOCUS measurements are done to optimize the position of the subreflector second
205. t then ABS fOffset1 FS amplitude 1 2 FS throw FS with fOffset2 not equal fOffseti is experimental RECEIVER allows to set fOffset1 and fOffset2 for each connected receiver differently Parameters of other options are always the same for all receivers Limits for fOffseti and fOf set2 are 9 to 9 with the 3 mm receivers bands 18 to 18 with the 2 mm receivers bands 27 to 27 with the 1 mm receivers bands IMPORTANT NOTES about use of Frequency Switching FS Frequency Switching FS can be very powerful and efficient for some projects e g mapping of narrow spectral lines in cold dark clouds outside the plane of the Milky Way However before deciding to use frequency switching one should consider some potential drawbacks The target lines should be narrow enough so that line signals from the 2 phases of the switching cycle are well separated The spectral baseline will generally be less flat than in other switching modes Some spectral lines are also emitted in the earth s mesosphere e g the mesopheric lines from 12 CO are rather strong typically several K and they will be seen in FS spectra taken toward astronomical sources with a low Doppler shift The mesospheric lines will appear at a frequency and velocity that correspond to the rest frame of the athmosphere i e to good approximation the observatory If e g you observe using Doppler corrections for the LSR scale the mesospheric lines will ap
206. that backend part If no line name is set for a backend part default the line name from the corresponding RECEIVER band will be used in the CLASS header This is an optional convenience feature to make it easier to identify spectra by appropriate names in particular in cases where several different lines are observed simultaneously with the same receiver band This is only a name or label and has no influence on any frequencies or other control parameters 7 2 10 BACKEND PERCENTAGE PERCENTAGE percentage Real percentage percentage of bandwidth to use This is a special option for the autocorrelators VESPA and WILMA For autocorrelators normally some channels at both ends of the band are blanked because they do not contain usable data and only the central percentage of the theoretical bandwidth is used typically about 90 Reasonable conservative defaults are automatically applied in general 90 but 82 for VESPA with bandwidth 640 This option allows the observer to adjust the percentage for special purposes For WILMA connected to EMIR the useful bandwidth is 3720 MHz and counted as 100 7 PAKO LANGUAGE INTERNAL HELP 102 See VESPA user s guide for details 7 2 11 BACKEND RECEIVER RECEIVER receiverBand polarization subband sideband Character receiverBand receiver band to connect to backend part Character polarization EMIR polarization to connect to backend part Character subband
207. though the angular length of the subscans 1 In particular for equatorial coordinates corresponds to Right Ascension and b to Declination 2 For the equations all angles are assumed to be in radian 2 PAKO GUIDE OF THE PERPLEXED 15 Global Offsets On the other hand the command OFFSETS can be used to specify additional position offsets in other systems These globally defined offsets stay fixed during a complete scan They are only needed in special cases e g the Nasmyth offsets or for ONOFF with wobbler switching see below At this time 2012 12 01 the command OFFSETS supports offsets in the following 3 systems projection Offsets in the radio projection see above trueHorizon true angle horizon offsets in Azimuth and Elevation Aa a source cos e De e Esource where a and e are the Azimuth and Elevation of the telescope source and Csource are the Azimuth and Elevation of the source calculated from l and b and the time and other parameters Nasmyth offsets in the Nasmyth receiver cabin system The purpose of Nasmyth offsets is exclusively to re position the telescope so that an off center element of a multibeam receiver looks at the position where otherwise the center pixel would look E g OFFSETS 33 44 SYSTEM Nasmyth adds offsets 33 and 44 in the Nasmyth system for all observing modes Example 1 Observe a single position with offsets 10 and 20 in system radio projection typically
208. total power time per phase data sample ambient load cold load sky at offsets 500 0 400 0 system for SKY offset time per calibration subscan a chance to check start offsets at start and end of first OTF subscans reference OTF reference number of on the fly subscans offsets of off source reference step shift between OTF subscans system for offsets time per on the fly subscan time per off source reference go back and forth a chance to check START start Comments we assume here that the source already has been selected see demo source 11 CROLOOP ROR means that there will be an L off source reference subscan R L before and after each OTF suscan 0 11 Therefore with NOTF 4 on the fly subscans the complete 1 subscan sequence will be 1 R OTF 1 R R OTF 2 R R OTF 3 R R OTFH4 R 11 with CROLOOP ROOROOR it would be 1 R OTF 1 OTF 2 R OTF 3 OTF 4 R In OTFMAP on the fly observations the antenna moves relative to the source while recording its position and taking data a high rate thus performing scans in the strict sense of the word This is a very fast mode for mapping The basic parameters of the command are the position offsets of the start and end of the first OTF subscan the basic parameters of the options are the number of OTF subscans the offsets of an off source reference position the step shift in x and y offsets between subsequent OTF subscans the t
209. trueHorizon OFFSETS SYSTEM trueHorizon is ignored not used IMPORTANT NOTE OFFSETS SYSTEM Nasmyth If OFFSETS x0ffset yOffset SYSTEM Nasmyth are specified in pako the values x0Offset yOffset are used during the observations this inludes the case that they are explicitly set to 0 0 It is up to the observer to make sure that they are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 11 8 OTFMAP TOTF TOTF tOtf time per OTF subscan or segment Real tOtf time 7 PAKO LANGUAGE INTERNAL HELP In commands like OTFMAP that have options SPEED and TOTF either option SPEED or TOTF can be used the values of the other option are then implied 7 11 9 OTFMAP TREFERENCE TREFERENCE tReference time per off source reference Real tReference time 7 11 10 OTFMAP ZIGZAG ZIGZAG yes no alternate direction between lines in a map Logical doZigzag 7 11 11 OTFMAP EXAMPLES Id demo otfmap pako OTFMAP SWTOTAL EXAMPLE v 1 1 6 2011 07 21 Hans Ungerechts demo rx spectrometers SET ANGLE arcsec SWTOTAL TPHASE 0 5 CALIBRATE AMBIENT COLD SKY 500 0 400 0 SYSTEM projection TCALIBRATE 5 0 PAUSE CALIBRATE OK to start c q
210. tude and latitude b on the celestial sphere and 2 Cartesian coordinates x and y which in radio astronomy and the NCS we often call position offsets Up to now 2012 12 01 only the radio projection is supported for which x l lsource cos b y b bsource where lsource and bsource are the source coordinates specified with SOURCE Note that this is the same system of offsets as in OBS of the old control system If we want to observe several positions on the sky at or near the source position as specified with SOURCE we often do this by requesting position offsets in the map projection Also the resulting data e g images are usually stored and displayed as a function of x and y For most observations parameters and options of the observing mode are sufficient to specify the position offsets e for TRACK and VLBI x and y are fixed during the complete scan e for ONOFF x and y change from subscan to subscan e for OTFMAP x and y change continuously or on the fly OTF during the OTF subscans The PAKO commands for most Observing Modes expect fixed offsets or start and end offsets for OTFMAP as parameters These can be either in the radio projection specified with the option SYSTEM projection or in the true angle horizon system see below specified with the option SYSTEM trueHorizon Notes For POINTING the OTF offsets are always in system trueHorizon and are specified implicitly
211. ub bands see above and the EMIR user guide CLEAR completely clears the receiver setup RECEIVER must be specified before BACKEND After you enter a receiver setup manually we recommend to save it optionally to a named file SAVE RECEIVER FILE receiver 1 It can then at any later time be reloaded with receiver 1 see HELP SAVE 4 3 3 Setup of the Backends Spectrometers and Continuum Id demo backend pako basic BACKEND EXAMPLES v 1 1 11 2011 11 24 Hans Ungerechts swTotal default select a switching mode compatible with all backends one example of a complex EMIR setup pako RECEIVER pako RECEIVER clear RECEIVER E090 CS 2 1 97 980965 LI horizontal LI vertical LI RECEIVER E230 CO 2 1 230 537994 LI horizontal LI vertical LI 4 PAKO S COOK BOOK BACKEND BACKEND backend BACKEND pause backend BACKEND backend BACKEND pause 1 BACKEND BACKEND pause 1 backend BACKEND 1 1 pause backend 1 BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND BACKEND CLEAR BBC clear NBC clear WILMA clear 4MHz 4MHZ 1 4MHZ 2 clear FTS clear FTS FTS FTS FTS FTS FTS FTS FTS oo Non Ae UNBE Default Default Default Default Receiver E090 Horiz LI Receiver E230 Verti LI Default Receiver Receiver Receiver Receiver Receiver Receiver Receiver Receiver E090 E090
212. ubband identical Similar remarks hold for the Uppper sidebands and subbands Compare the EMIR user documentation 7 2 2 BACKEND FTS FTS Fourier Transform Spectrometer The FTS supports two modes wide bandwidth up to 4000 MHz on EMIR 1000 MHz on HERA with a resolution of 0 195 MHz or fine resolution 0 049 MHz with a bandwidth up to 1820 MHz on EMIR 500 MHz on HERA All parts of the FTS must use the same resolution NOTE EMIR subbands IF cables and Backends The output signals from EMIR are transmitted to the spectrometers and 7 PAKO LANGUAGE INTERNAL HELP 98 NBC through 8 IF cables Each IF cable carries one subband of bandwidth 4 GHz LO LI UI or UO NBC 4MHz WILMA and VESPA can only be connected to IF cables 1 to 4 FTS parts 1 to 4 can also be connected to IF cables 1 to 4 The command options RECEIVER HORIZONTAL and RECEIVER VERTICAL allow to select up to 4 EMIR subbands that will be transmitted through IF cables 1 to 4 compare HELP RECEIVER HORIZONTAL and the EMIR user documentation This selection can include Outer subbands In addition for EMIR bands E090 E230 and E330 the IF cables 5 to 8 carry the 4 Outer subbands corresponding to the subbands selected for IF cables 1 to 4 E g if we select for IF 1 to 4 E230 ver UO E090 ver UI E230 hor UI E090 hor UI then the IF cables 5 to 8 will transmit E230 ver UO E090 ver UO E230 hor UO E090 hor UO Only FTS parts 5 to 8 can be
213. usly set offsets demo setup of EMIR REPLACE WITH YOUR SETUP clear previous backend setup connect 1 part to each EMIR subband selected make sure angle unit is arc s to select beam switching reset all options pointing with subscan length 4 OTF subscans 30 seconds per OTF subscan 7 PAKO LANGUAGE INTERNAL HELP 134 PAUSE POINTING OK to start c q a chance to check START start RETURN NOTE if you use NASMYTH offsets for an off center pixel of a mutlibeam receiver don t use OFFSETS CLEAR If you want the intensity of the Pointing data to be calibrated you have to do a Calibrate with the same receivers and continuum backends before the pointing 7 13 RECEIVER RECEIVER receiverBand lineName frequency SB RECEIVER BOLOMETER bolometerName Specify selection and setup for receivers The first form is for heterodyne receivers the second form for bolometers choices for HERA LSB USB choices for EMIR LO LI UI UO Heterodyne Character receiverBand name of receiver band to connect Character 12 lineName name of line don t use lt gt Real frequency GHz Character SB sideband or subband 1 1 Choices for receiverBand are E090 E150 E230 E330 HERA1 HERA2 lineName is limited to 12 characters NB Don t use amp lt gt in names of sources lines projects PI observer operator etc Don t use in source names E090 E150 E230
214. uto matically WOBBLER SWITCHING is normally used with ONOFF or for bolometer continuum mapping with OTFMAP 6 NCS EXPLAINED 86 Note that for OTFMAP with WOBBLER SWITCHING special restoration algorithms are needed to recover an image of the source brightness distribution These are available e g in the MOPSIC software If WOBBLER SWITCHING and ONOFF are combined in the standard way we effectively take data at 3 positions 1 the source position 2 the source position throw offset in the true angle horizontal system 3 the source position throw offset in the true angle horizontal system with throw ABS wOffset2 wOffset1 Data from 1 are treated as source signal data from 2 and 3 as off source reference signal Note that in the astronomical coordinates positions 2 and 3 will rotate around the source position 1 Therefore one must normally be sure that the extent of the source is less than throw beamWidth 2 6 3 4 Total Power TOTAL POWER refers simply to data acquistion without any of the other 3 fast Switching Modes Even in this case the same type of hardware synchronization signals is used to control the regular readout of the backends In this case there is only one switching phase Normally when using TOTAL POWER one or several positions ON the source are observed alter nating with one or several OFF source reference positions and the signal is calculated as the difference betwee
215. ving Modes a aooaa Coordinate Systems Map Projections and Position Offsets Receiver Setup and Calibration Parameters 000002 eee Backends suis Fok Gee aa PR be Ge ee ee Gee a ew ae Continuous Data Acquisition and Data Streams 0 0 00 eee Display of Parameters optan sar a RR eR ee ee Preview Plots coe soep ek a a Sw A A Ge He OH Ee eS Di aa ste Be Ak RR Fe Re Pe RA eR eS Rang s and checks o s fcc ek Ce ee RRR Ge RRE ee EEO Independence of Command Parameters e Option keywords 4426 Joie aa ad Ew ee ES Logical YES NO or ON OFF Options 4 44 c0 5 242548 thee os Example Scripts and Catalogs 6 ee 2 23 3 PaKo s simplest recipe 4 PaKo s Cook Book 4 1 Set General Informati n ss 2 24 4 8 a wa ee Se ee oe 4 2 Specify your Source Catalog and or Source o ooo o 4 3 Spectral Line Observations with Heterodyne Receivers 4 3 1 Specify your Line Catalog 2 e 4 3 2 Setup of the Receivers Frontends 4 3 3 Setup of the Backends Spectrometers and Continuum 4 34 Switching Mode cae 4 64 44 2 be Ee ee a Re oe ee eee 495 CALIBRATE a 24 koe bog hae ke AS A a e a SS 436 POINTING gt re sda 64644 4 45 be bbe Ree a ae Ee eS 43 4 FOCUS csse 8 etna eh aye ace ee eee PRO eG a 4 38 TRACK Single Position with FREQUENCY SWITCHING 4 3 9 ON OFF Position Switching and Wo
216. we distinguish up to 4 sub bands each of 4 GHz bandwidth e the lower outer sub band LO from about 12 GHz to 8 GHz frequency shift relative to the local oscillator e the lower inner sub band LI from about 8 GHz to 4 GHz e the upper inner sub band UI from about 4 GHz to 8 GHz and e the upper outer sub band UO from about 8 GHz to 12 GHz If we select LO LI UI UO as EMIR sub band in the line catalog or directly in RECEIVER the localoscillator will be adjusted so that the specified line frequency goes into that EMIR sub band For details see the EMIR user guide For HERA the sideband must be LSB lower sideband NOTES In source names line names and parameters of type character like Project ID names of PI observer operator one can not use characters that have a special meaning in XML in particular don t use amp lt or gt also don t use or in source names One RECEIVER command is needed for each receiver EMIR band or part of HERA After the receiver is set up and a source has been selected the observer should enter CALIBRATE SKY no START to send the receiver parameters to the NCS The telescope operator or receiver engineer will then tune the receiver HORIZONTAL sbi sb2 and VERTICAL sb1 sb2 apply only to EMIR This option informs the system about which EMIR subbands are going to be used for the horizontal and vertical polarization about the EMIR sub bands see above and
217. with SIC options like VELOCITY double beam pointing only for Bolometer and Wobbler switching with 2ndRotation angle 0 0 To BE DONE or flag items that are planned for the NCS but not yet implemented or properly tested Observers should not try to use these features without consulting the NCS team Examples how to use HELP for detailed HELP on a command HELP OTFMAP HELP OTFM one subtopic examples all subtopics options in ge or option and options neral news about pako help about paKo HELP BACKEND name BACKEND CLE 7 2 BACKEND HELP HELP HELP HELP HELP HELP 7 PAKO LANGUAGE INTERNAL HELP OTFMAP OPTIONS PAKO NEWS PAKO HELP OTFMAP NOTF OTFMAP EXAMPLES nPart resolution bandwidth fShift receiverBand polarization subband sideband AR Alternative short syntax only for the backends shown here BACKEND BBC nPart BACKEND NBC nPart BACKEND 4MHz nPart BACKEND WILMA nPart BACKEND FTS nPart BACKEND FTS nPart FINE REC REC REC REC REC REC receiverBand receiverBand receiverBand receiverBand receiverBand receiverBand Set up backends for heterodyne receivers Character Integer Real Real Real Character Character Character Character name 1 nPart resolution bandwidth Shift 1 1 1 receiverBand polarization subband sideband name of backend logical number of backend part MHz MIR
218. y Wobbler Switching The combination of ONOFF and WOBBLER SWITCHING provides a very high sensitivity in continuum bolometer observations of compact sources and excellent baselines for spectroscopy It has the disadvantage that the emission free off source positions are very close to the source limited by the maximum Wobbler throw Also the Wobbler direction is fixed in the horizontal system relative to the telescope and therefore in the source system the off source positions rotate around the source position For continumm observations usually a short time per Wobbler phase 0 25 s is used with small Wobbler offsets throws for spectroscopy largest possible Wobbler offsets throws up to 120 are preferred but then the time per phase must be longer 1 2 s 4 3 10 OTF On The Fly Mapping Id demo otfmap pako OTFMAP SWIOTAL EXAMPLE v 1 1 6 2011 07 21 Hans Ungerechts and spectrometers demo rx spectrometers demo setup of receivers REPLACE WITH YOUR SETUP 4 PAKO S COOK BOOK SET ANGLE arcsec SWTOTAL TPHASE CALIBRATE AMBIENT COLD SKY SYSTEM TCALIBRATE PAUSE CALIBRATE OK to start c q START 500 0 400 0 projection 5 0 OTFMAP 300 15 300 15 CROLOOP ROR NOTF 4 REFERENCE 500 400 projection STEP 0 10 SYSTEM projection TOTF 120 0 TREFERENCE 20 0 ZIGZAG PAUSE OTFMAP SWTOTAL OK to start c q 43 to select
219. y are correct in pakoDisplay SYS Nasmyth will be highlighted as yellow alert If OFFSETS x0ffset yOffset SYSTEM Nasmyth are not specified cleared for the MAMBO bolometer Nasmyth offsets are used automatically according to the selected bolometer channel pixel 7 25 3 TRACK NSUBSCANS NSUBSCANS nSubscans Integer nSubscans number of subscans 7 25 4 TRACK TSUBSCAN TSUBSCAN tSubscan time per subscan Real tSubscan time 7 25 5 TRACK EXAMPLES Id demo track pako 7 PAKO LANGUAGE INTERNAL HELP 165 TRACK EXAMPLE v 1 1 11 2011 11 25 Hans Ungerechts demo rx demo setup of receivers BACKEND CLEAR clear previous backends BACKEND VESPA 1 0 040 40 0 0 0 E090 hor LI high spectral resolution BACKEND VESPA 2 0 040 40 0 0 0 E090 ver LI with VESPA BACKEND VESPA 3 0 080 80 0 0 0 E230 hor LI BACKEND VESPA 4 0 080 80 0 0 0 E230 ver LI REPLACE WITH YOUR SETUP SET ANGLE arcsec setup frequency switching SWFREQUENCY 3 9 3 9 receiver E090 for EMIR band E090 SWFREQUENCY 11 7 11 7 receiver E230 for EMIR band E230 SWFREQUENCY tphase 0 20 same for all receivers bands CALIBRATE ov AMBIENT ambient load COLD cold load SKY 600 0 0 0 sky at offsets 600 0 0 0 SYSTEM projection system for SKY offsets TCALIBRATE 5 0 time per calibration subscan PAUSE CALIBRATE OK to start c q a chance to check START start TRACK 40 0 30 0 gt of
220. y specified with this option paKo will assume that for this polarization the same single subband SB is requested as specified for the main parameters frequency tuning of the RECEIVER command for this EMIR band VERTICAL n one means that from this polarization no subband will be transported through IF cables 1 to 4 7 27 41 OPTIONS WIDTH WIDTH width Select receiver setup for WIDE or NARROW bandwidth mode Character width width choices WIDE NARROW NOTE Option WIDTH NARROW changes the local oscillator setup of receivers HERA1 and HERA2 in such a way that a line in the center of the receiver bandwidth appears in the center of the bands of the Backends 1MHz with 256 or 512 MHz bandwidth and VESPA Spectrometers with 1GHz bandwidth normally require WIDTH WIDE 7 PAKO LANGUAGE INTERNAL HELP 7 27 42 OPTIONS ZIGZAG ZIGZAG yes no alternate direction between lines in a map Logical doZigzag 179 8 POSTSCRIPT 180 8 Postscript You will certainly not doubt the necessity of studying astronomy and physics if you are desirous of comprehending the relation between the world and Providence as it is in reality and not according to imagination You must however not expect that everything our Sages say respecting astronomical matters should agree with observation Astronomy had in the days of Aristotle not yet developed to the height it has reached at present Moses Maimonides Moses be

paKo. The Observer`s User Interface to the NCS

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