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CRIRES User Manual

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1. 0S9T T8P9T 6 6891 9 91 O 6Z9T amp OCOT 9LI9T LOT 9FZOT U T PE FE O FPOT TL VOSIT LEPOT STP9L 97891 ZEJT 08391 9 2291 61191 69191 TOZ9T 1 1 S Ge Z989I ZL OTOL root 2891 TOES9T U92291 POZ9T CSTOT ZOTIT SZP9l 9 SGI9T U T GE SE great LL 7SI9T 62091 SSO9T 9691 9 S6ST FP ZLSST O G8GT F9L46T FOTIT TESST 1 T G oe gtt SL 019 TEO9T O TO9T O S6ST LOGSE PZSST OSST CH FG091 8LGT U T G oe ip 69 SOOT T86ST Z96ST Z68ST Z L8GT 86281 l t OOLEL TIO9T Z SLGT 1 1 98 oe 2681 OL 90091 8S E6ST O ZEST SPST 629891 v GLGT TELGI 79961 L96ST SOLST U T 9E 9E rage GL 9OLEl 8991 CTOGT PESGT SISST EPGT GOFPST ZEGT G9ST GEGT 1 T 9 9E SGT 92 0999J SBAT q oqqT L8PST GOPST PEST l OEST 9661 90991 PEST U T 9 9E YZST L9 ETIGI CPST TESST EIVAT PYYSI Z LEGT T SEST 94691 LLSST 8 ZEGT vVT 4e LE LPT 89 Feet SOSST O 6PST O ZPST T OPST 8 ZEST LOSST 26697 VEGGI escer u T e LE Core El 18867 60381 OGIST GITST 6091 GIOST Cor J I6FI EZZ SLEPT V T 4 LE Core VL L EZGI GOST SPIST 6 90ST S FOST 69691 YPG 9ST PSIG Z EGPI U T 1 LE LOTT G9 CO OPIST TZIST 9 GOST 0ST 2 9691 rot FAsbt VITSI SZ6PT 1 1 88 ge Gang 99 9IG TOIST ESOSI IOSI 2 66pT 9Z6PT SO6PT T EST YZISI S 88pT U T 8E ge Gro TL ELST GOSPT orl 2 TAVITI 969PT zort S GGPT GTGT LSP Coop 1 1 8 8E EG
2. EUROPEAN SOUTHERN OBSERVATORY S Organisation Europ ene pour des Recherches Astronomiques dans l H misph re Austral O Europ ische Organisation f r astronomische Forschung in der s dlichen Hemisphare ESO European Southern Observatory Karl Schwarzschild Str 2 D 85748 Garching bei Miinchen Very Large Telescope Paranal Science Operations CRIRES User Manual Doc No VLT MAN ESO 14500 3486 Issue 83 2 Date 19 12 2008 R Siebenmorgen A Smette 19 12 2008 A ayer uus out aa Sh OGL eoa ete Ba ye uet tup ected Date Signature G Marconi ADDPOVOO REENEN Date Signature C Dumas A dur ama erbe e En ae ood ES Date Signature CRIRES User Manual VLT MAN ESO 14500 3486 This page was intentionally left blank CRIRES User Manual VLT MAN ESO 14500 3486 Change Record 111 CRIRES User Manual VLT MAN ESO 14500 3486 iv Issue Rev Date Section Parag Reason Initiation Documents Remarks affected 79 1 29 08 06 all RSI ASM First release issued for P79 Phasel 79 2 08 09 06 all ASM Sec 11 corrected wavelength table 79 3 20 12 06 all RSI ASM comments DMD 79 4 21 12 06 14 15 ASM minor editorial corrections 80 1 05 03 07 0 1 ASM corrected layout figure and description 3 added a web link 6 corrected detector gain added comments on a non linearity correction method minor updates and corrected typos 5 updated limiting mag in noAO 8 added subsection on entran
3. 8L0p nicht PI Cen LLL OFZIP 90TH TOTP 07807 6 820 Goor From rom vV6STP C O0P YT PT Tt 08607 GLL F ETI O 960F Z T60P Goin gint tt rm G CCOP G ZPIP 668 U T pT PI 07807 61 COOP T ZZOP 6 9TOP TL66E Z I66E T ILGE TS96E LEVEE TOLOP S 8T6E 1T PT PI 02007 Got ron C OIOP ont O S86E S 6L6E gon Ion TTEGE LLGOP S 906 U T YT FI ong L OZ VLS6E TLE6E CTE6E OI6E T TO6E VZ88E O OLE Tease l IS6E amp 8E 1 3 pT PI 6 0268 6 0c org DZ6 L 8T6E E LESE V IG8E T 698 ZISE LGESE LL9GE 9OZE U c VT FI 0806 SPL LZ6E O ST6E 0 606 SEGRE 9 699 DELLE Gang Tl CG86 sacee rier Vier GI PF 106E oi S8T6E Grupp 6 668 GPE C OSSE OPISE amp 6086 ECE EOPGE Z 8TSE U Z GT ST Z 768 GOL GOP8E PEESE O 608E T ZISE PLOSE 1684 SV8LE 09946 TSE 6 9PLE 1 T ST ST S 038 9T 9 6 8 E EZSE 69198 TOE O L6LE T6LLE 6 ELLE TELE L IOSE 89ELE U T ST GT OT8 OST TILLE MESLE LSPLE COLE TSTLE O VOLE POOLE 10998 S 88LE ronn V I GT ST G6ELE CST COME SEPLE WLELE oU SETLE PP69 8 889E an ELLE 7 S89 U T GT ST Col 6I 769E FELIE ERIE Gong org ron eo Z q6qg SOLE L G8GE 1 3 8T SI T 9998 S 6T 8089 9 I99 amp OCOE Con gun omg OPO9E G C8SGE Teege L ELGE U C GT ST 998 LVL 69998 LTE9E 2 2298 Age 8098 L Z6SE T 88GE S TLGE Coon gange 1 T 9T 9T Coco OTI CA 0 L TZ9E
4. 49 11 2 4 Science Three templates are offered in P83 The CRIRES spec obs AutoNodOnSlit is the preferred observing template for point like sources It allows staring or nodding observations with a fixed nodding throw along the slit with optional jittering The CRIRES spec obs SpectroAstrometry essentially does the same as CRIRES spec obs AutoNodOnSlit but for each value of a list of slit position angles This template is particularly suitable for applying the spectro astrometry technique Beckers J 1982 Opt Acta 29 361 Bailey J 1998 MNRAS 301 161 and refer ences therein First results using this technique with CRIRES are described in Pontoppidan et al 2008 Note that this template can currently only be used with adaptive optics and if the target is also the slit viewer guide star but the AO star can be different The CRIRES spec obs GenericOffset allows generic offsets suitable for observations of very extended objects The observing templates are described in Sect 14 11 2 5 Calibration Darks flat fields and wavelength calibrations are taken during daytime as part of the calibra tion plan see Sect 12 A Halogen lamp is used for flat fields Fiber fed ThAr spectra or the N20 or CO gas cell in front of the halogen lamp are used for wavelength calibration Observed sky lines which can be identified by HITRAN have the advantage that wavelength calibration is done from the science observations themselves Unfortuna
5. 00 38 Figure 23 Atmospheric transmission from 900 5500nm computed with PCLnWin HITRAN for a Paranal atmosphere precipitable water vapor PWV of 2 5mm at zenith and smoothed to a resolution of A AA 104 Transmission 1000 Transmission d vol 1400 1 0 0 8 0 6 0 4 hi ool oo li 1900 Transmission L 1100 1200 1300 H 39 1400 1500 1600 1700 1800 h I 2000 2100 22 00 Transmission iL i ll 2300 2400 1900 2600 2800 Transmission 3000 3200 3400 3600 3800 4000 Y WU m ID 4200 4400 4600 4800 5000 5200 5400 phi li Figure 24 Water vapor only atmospheric transmission from 900 5500nm computed with RFM HITRAN for a Paranal atmosphere precipitable water vapor PWV of 2 5mm at 100000 zenith at a resolution of A AA 40 from a relatively large number of bad pixels In addition the spatial extent of a spectrum is at most a few pixels in nominal conditions Jittering is obtained by adding a small random offset to the telescope in addition to the nodding offset The recommended maximum size of the jitter offset is a free parameter It must be smaller than half the nodding offset but larger than the
6. G EPPOT S 96P0T OIG0I 99901 Z OLEOT ronnt 1 0 69 6 0 196 GP 867801 Z16801 COIVOTL 09POT SPLPOT P LZSOT 6 T7601 L L690I 66E0T Cogont u 0 68 69 896 Q xeu DI 4 xeu uyaq xeu utum xeuly utum xeuly uug CT O PI y wa g va c d I G oguei USUN yybuajaann ut sabuns josjaads aof int ajqvy 229 SPXId QE st ISU9SALM oouoIl9Jol oY Jo Suruoryisod oy uo Koenooe aq T OBUVI payjou3raun OY 9PISMO JVJ 20911 UL UoAIS s n eA IoquinuoAeA jI S DOSIL c Y 1oJ TOAST T Wey o1our ye AyyIqronpoldad Jo yor Aq poyooye st oguer Tetjods po JousSTAUN 913 JO oprsjno uoreurum 1o3ourered e se pogroods oq os e 3snur 1oquinu Iop1o oY jeu sojeorput V e 103293op 103 oxid uro QT ut 49 uotrsrodsrp ue ur 9y SISI Otto ISP oq WATS OSTE ore 103293op MO ot JO Yowo 103 uio ut posso1dxo ol 1oquinuoA A VINNIPA ur oge19A00 pue oguei e1go ds pogjeusrAun qI uorjeogrjuopr q33u AeA euiojur Q JoquINU IpI 1o15991 9p pig eu Jo ZIG Joxid ye q33uo oAeA oY se paugop SSUT JOS YSUSTOEARM prepuejs OY 10 WU ur PY syYSUSTOARM DOUAIOJOY eG ALL 81 V9 9099 919 999 9 99199 VABI 999 79989 770069 2929 178289 1 1 6 6 Ort V9 LL9L9 19619 97089 SE89 LEP89 79189 99889 66169 9 q929 90689 U T 6E 6E E99FT OL 09699 GO0E69 T6E69 0469 Z 969 O OZOL VOEOL 98904 769 Coen T 6E 6E SLEPT OL 9LI69 10969 66969 0 2669 SPOOL SIVOL 2290 Z
7. L 8T9E G E09 Cor cesse 9 84c6 S IOGE 6 CG0 GErse U T 9T 91 T IIOE Xe KEEN uy SEU ume KEHN ume BUM Umi xeurv ume CT O PIV y wa wa z wa I 39d oe man SIQUNUIADN ut SIDUDA 04 o99ds Lof YG DG 2 qD 299 s oxid QF e SI YISU9SALM ADUSISJOI oY JO SUTUOIYSOA oy uo LIVIN AY Y WU ul passaidza wnnava 240 syzbuajaan M 29081 P9IJ9USTAUN OY PISPMO JVF 911891 Ul uoAIS son peA YYSUSPOARM PMS ISIL Z Y 10 TOAST YT wey o1our ye Ajrpiqronpoadozr jo yoe Aq poyooye st osues Terjoeds pojjousrAun oY JO oprsjno uorjeurumg I Joyouered e se payroods oq os e gsmu 1oquinu Jop1O oY 3er so3eorput V IOJo op 10 Toxid uru QT ut YE uorszodsrp ue ur 91 SISI uump oo ISP oq HOA OSTE are S1032939p MOJ oy JO Yo 10 FLI AOD pue oguei e1joods poyoustaun qJ uoryeogrguopr q3guop o eA euu Q 19quinu I pIO 10 De4ep pie oY JO ZIQ exid ye qa33uo pAeA oY Se pougop s Sumj s prepuejs oY 107 Py suq3S8uo oAeA oouoI9god Sp ALL 78 G6I LG6EG TLLES OGLES ECGES SIPEG 6 Gc6G 6616 62666 Z YIGG OPSIG U c Il IL zo Got epses Ppeges co9ES TOPES Ire SETES PLOEG T 98ZG L ZOSS 6 I4IG U Z TT IT ZOSES G TG Une cS468 G69cS V2vcS f Ivc8 LSIcG VIICG U28IG l OITG c 8208 UV T II ITI v8SzS SIZ e866 Tonga OPETS LATS E POZS SLGTS 6 GLIG 9966 2906 U T TT IT Tepes ge 09616 O ELTS 9919 9 RIS ESETA 9 OIIG EE0TS 02406 VZOES 9926F 1 0 TT IT 9T9IG S EZ
8. ck 89977 Z8vEp U I PZ vC 6c8c 66 64887 TSF OISE VOLEY 9 G4eP opt zt geit greer Gerry 1 1 97 Gz 762 OO 0686 SLAP 9298 TZ8EP L 28 V v80vp vrt 7987 rover Orvcvv u 1 97 GZ 187 SOL E 1877 G6 lthh 9 VVV L169 Iert ott 6809 oeer SIP GvIGP 1 1 G GC Pre 601 88877 reay 6 097 gest esr eier cocer 09767 O SEP oeza U T GZ GZ 1982 nQ xeuly utum xeu un y xeu y uug xeuly uyg aM utu qI O PI y o wa z 3g I wa oguer usun yybuajaann ut sabuna o4222ds aof int ajqvy 229 s xtd QE st YISU9SALM oSu 19J91 o JO Suruorjrsod oy uo LIINI aq asueI pogjousraun OY OPISNO Te 20911 UL UoAIS SOTA IoquinuoAeA jI S DOSIL c Y IOJ TOAST T Wey o1our ye jr rqronpoadoz Jo yoe Aq poyooyye st oSuer Tetjods po33jouStAun 913 JO oprsjno uoryeurum 1o3ourered e se pogroods oq os e 3snur 1oquinu OPIO oY jeu sojeorput V e 103293op 103 foxtd uro T ut 19 uotrsrodsrp ue ur 91 SISI Otto ISP oq UDAL OSTE ore 103293op MO ot JO Yowo 103 uio ut posso1dxo ol JOqUINUSARM VINNIPA ur oge19A00 pue oguei erjoods pogjeusrAun qI uoryeogrjuopr q33u AeA euiojur Q JoquINU JopIQ 1032939p PIE ey Jo ZIG OXId ye q33uo oAeA oY se pougop s3utyjos YISUAIALM prepuejs oY 107 WU ur y Saba 90U919J91 Ae SEL 85 COIT 66LZ S TISZ c STSG G 8CSC Ces oer TOS8Z org Z 06L3 Aug 1 0 91 9 gro VOT 02092 2 6T8Z SETS 99 8 amp Ov
9. lengths of the standard settings Tables 6a and 6b lists the allowed minimum and maximum ranges for a given order For visual inspection of the start and end wavelengths of each de tector unvignetted spectral range detector gaps Fig 2 or the appearance of sky lines the ETC should be used INS GRAT ORDER P2PP Grating order is the grating order For most wavelength settings there is a unique relation between the reference wavelength and the grating order In this case INS GRAT ORDER can be kept as its default value of 0 However for some reference wavelengths in order 39 43 and 21 22 there is no unique relation and the grating order has to be specified by the user Table 6a lists the orders and wavelength ranges for which this parameter must be given 14 1 7 Notes 1 If both SEQ NGS ISTARGET and SEQ NGS ISSVGS are set to T then the target is the AO guide star and the slit viewer guide star Therefore only the target coordinates TEL TARG ALPHA and TEL TARG DELTA must be provided 2 If SEQ NGS ISTARGET is T and SEQ NGS ISSVGS is F then the target is the AO guide star but it is not used for guiding with the slit viewer In this case in ad dition to TEL TARG ALPHA and TEL TARG DELTA TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA should be provided see above for the convention 3 If SEQ NGS ISTARGET is F and SEQ NGS ISSVGS is T then the slit viewer guide star is the AO guide star but not the target
10. ol JOqUINUDARM VINNIPA ur oge19A00 pue oguei e1go ds pogjeustrAun q uorjeogrjuopr q33u AeA euiojur Q JoquINU JopIQ 1o159919p PIE ey Jo ZIG exid 3e YYSuspPAeM oY se peurgop sgur33es YASUSTOARM prepuejs OY 103 WU ur y su38uo oAeA oouoloJoi JG LL 86 GLI U80cc 913 SIZ TL LOC GETZ 9 IvcG VIG 8 8LIZ V OSCC UI ET got PLI VEZ vIGcGG LEZ GELS OSE HHP VZ TLV TH8IZ 69823 u g1 Er T887 TOI STSZZ ETZE 6 9cG OPLZZ S OLcG PVLZZ 90673 8 TOEZ EGzzz 0O 8cec 1 T ET T 82077 Co 9292 92 6 693 Cer ESZE 8 EGZZ O LEZZ S 808Z PTET VEEZ U T ET ET SS6EV 8 03 9266 V908 V IIEGC SEZ oer 0 8EEZ SIPEG THSET L ELTZ MLLEZ V I T Er 8 STEV OTG E POEZ SSIES SSIES 86ZEZ TEEST ESPET 6 8PET S T9EZ LO8ZZ LHREZ U T ET ET 6 OEP EZZ GSPEZ 9 L8EZ COVES LELET ELLET L OGEZ L V6EZ ROK rg VEZ 13 T Er Heer SZZ GTSEZ 998 29982 DIES ESSET GEEZ em ELITE OZEEZ vLEvE U z eT ET SOTZ GGT TLLES 6 S8EZ EBBET 9YL6EZ OOPS TOPS TEIDE Lew YESEZ Torre Veit PI 6 84Iv TOT G 8Z PGES SEGEZ CEOPZ 09077 TOTZ T61 8 6zr sesez ozer U z pT FI Com LLL Speg O GEPZ SLEPZ 9 Sppc HIGH TEI 99E 98LPZ SHOPS O 86YZ YT PT FI 08607 61 TISPE VIPS EPPS SSPG amp SGpc COL VEL 8 S8H G OlPC POST U T pT FI 07807 61 ZC 8986 SERPS gc Come Coos OZZSZ L SESZ 6 9SPZ Tz2ssz 1T pT rt 02007 Got S ISPC I EGPZ 696P Tro
11. 0998 U T ZE ZE 69821 ng Kat DI xeuly umaq xeuly utum xeu umg xeulg uyaq qI O Ply ppd wa z wa I 39d osuet man yybuajaann ut sabuns o4222ds aof int ajqvy 229 SPXId QE st YISU9SALM ADUIIAJOL oY Jo Suruorjrsod oy uo LIINI aq OBUVI payyou3raun oY 9PISMO JVJ ILY UL UoAIS s n eA IoquinuoAeA jI S DOSIL c Y IOJ TOAST T Wey o1our ye jr rqronpoadoz Jo yoe Aq poyooye sr oSuer Tetjods po33jouStAun oY JO oprsjno uorjeurum 1o3ourered e se pogroods oq os e 3snur 1oquinu I9p10 I JEY sojeorput V e 103293op 103 foxtd uro T ut 19 UOTsIOdsIp ue ur 91 SISI Otto ISP oq WOAS OSTE ore SIOJ99J9P MO t JO qoeo 103 uio ut posso1dxo ol 1oquinuoA A VINNIPA ur oge19A00 pue oguei erjoods pojjeusrAun q uorjeogrjuopr q33u AeA euiojur Q JoquINU JopIQ 1o15919p pig oy Jo ZIG Joxid ye u3Suo pAeA oY se pougop sgurj3es qj3uo pAe prepuejs ayy 103 WU ur y SYJBUAPALM DOUOIOJOY PG APL 84 OTI LYLGE 6698 EL6SE O 9T9E Z IZIE COPE 2998 998 FOSSE 6499 1 T 03 0 2323 TPI 99999 98098 909 A4c9e 6 ce9 rou 9 9q9 676 96 S TGGE 6699 U T 0Z 0c GO TIT 689696 GGCI9e VITIE STE VEIE VTL Z 9GIE T ELIE T66SE 9899 I I TZ Ic G6SLz ETT 0096 YvIcOe SAZI 90F98 SPPIE T I998 8990e TEes9e Come Z 8L9E U T TZ TZ OCL EZI efL96 906 T2698 VT SLE S GELE OLE 809 6 998 TELE 1 0 13 Ic 00026 GZ 7s9e LOOLE FSOLE O EZLE 622
12. 28817 LIT SEGIT 1 0 27 Lb ron 98 86167 VLOZT 6 S0cT TOOZ S861T SZ6TT SO6TI 9 78IT Canet FO6TI U 0 Lb Jr 0 VS 06II GG8IT THSIT Cat OLLIT GTLTT S69IT Fort FOSTE T69IT 1 0 87 gt T8TI qq GL8IT Cat LOSTI TSLIT SELTT LL9TT O09911 876977 BZ8IT 99911 u 0 9 8h GL ES 9991 VI9IT 66911 SPOTT O SIT LVIT Y OTI L GETT TOIT SVIT 1 0 67 o ZLSTT Vo Fort aert LOSTT Cent 96PIT GEPIL SPIT 69617 gett O ZPITI U 0 6h Gr Get CG amp ETII ett LOSI STETIT 66711 TCIT L ZZIT 890771 SETT P ZZIT 1 0 08 0S O VETT gq TOITE ert VESTIT T 8ZIT VOZIT OTZIT S6ITI SETIT F SETT Co u 0 0 0S SOETT TUS O0GII gett PITT Z601 LOTT ZOIT 200TT 070601 Cat OOTITL 1 0 19 IG STITT ES III YGTIT STITT 0 90TT SPOTT O 660T 2601 9 760F TETIT 601 U O TS TS 98OTT O S 66601 Cront 0 60T 901 9801 O TOT S6L0T 6 EL0T L v60T v6LOT 1 0 38 Z9 root TS 6960 TGOT 66901 rant S ESOT 8 LLOT E 9L0T 9 OLOT 9T6OT 9L0T u O0 cG Z9 80I 6D F8LOT 98101 Ent 901 6 S90T 9YO90T reegt 9 ES0T O VLOT T 6901 1 0 8 E9 goot O S 9901 LOLOT 6901 Cro0t 8 Z90T G LGOT 0 900 7 0G0T ent T 9901 U O ES ES S 99OT SP 99901 8 ES0T amp CG0T SLPOT SOPOT O TPOT 6601 rout O VSOT 9 6801 1 0 79 FES ot 6D 99901 8 0S0T VETOT TTOT TEDOT 6 LEOT 779601 60801 O TSOT S 980T u O0 TG pS OLOT LV 660I YPEOT E0T S8Z0T T LZOT O ZZOT 97001
13. 5 10 Nod throw along the slit SEQ JITTER WIDTH 0 8 0 Jitter width INS OPTI1 NAME INS WLEN REF INS GRAT ORDER REE GAS N20 GAS CO FREE 958 3 5361 9 NODEFAULT 0 59 0 Gas cell Reference wavelength Grating order Fixed values Parameter Value Label DPR CATG SCIENCE Data product category DPR TECH SPECTRUM NODDING DIRECT Data product technique JITTER OTHER DPR TYPE OBJECT Data product type CRIRES spec obs SpectroAstrometry To be specified Parameter Range Default Label DET1 DIT 0 900 NODEFAULT DIT DET1 NDIT 1 1000 1 NDIT INS DROT POSANG LIST 0 0 360 0 List of position angles INS GRAT ORDER 0 59 0 Grating order INS OPTI1 NAME INS WLEN REF FREE GAS N20 GAS CO FREE 958 3 5361 9 NODEFAULT Gas cell Reference wavelength SEQ JITTER RESET FT T Reset jitter for each DROT posang SEQ JITTER WIDTH 0 8 0 Jitter width SEQ NABCYCLES 0 100 1 Number of nodding cycles SEQ NEXPO 1 100 1 Number of exposures per nodding po SEQ NODTHROW 0 22 5 10 Nod throw along the slit Fixed values Parameter Value Label DPR CATG SCIENCE Data product category DPR TECH SPECTRUM NODDING JITTER Data product technique ASTROMETRY DPR TYPE OBJECT Data product type CRIRES_spec_obs_GenericOffset To be specified Parameter Range Default Label DET1 DIT DET1 NDIT OBJECT DET1 NDIT SKY INS GRAT ORDER INS OPT
14. 5 1 AO guide stars la caes kA ee WER OR UR RR LR S11 The distamos of the AO star 2245 so oo k s bor do x a ru 51 2 The brightness of the AD star 24040424 444964 64 44 a4 51 3 Thecolor or the AO star 6 24 6 64 24 omo dee be RO UR 5 2 Limiting magnitude of slit viewer 6 Detector characteristics DI Dark and palin lt p aso REG Reg Q sisa ORE SER ERE ER ERR ES DE SO ee ae ener ce ee E t Qa S ya d qumi we S ae oe ek e ee eh oT MB o RIN 1x wW GO AN e O Gb NNO 16 16 17 17 18 18 19 19 CRIRES User Manual VLT MAN ESO 14500 3486 OA LIA Chet coca cae SESE DES ee 9x ok ue Rok OS EO Ds Detector I N vies ee ace A aS AA e d 7 Characteristics of the spectrograph FAL Wavelet getting orac d nee Se PARES PERS xo OHS Sh UW D Se EES L4 Wavelength calibration lt a kee de Genes Ghee rre di RR ES eS 7 2 1 Standard means ThAr lamp and N20 and CO gas cells 7 2 2 Radial velocity measurements T23 VIERNES e uu uo addera dd p s e Q w SO Pd RT EAS L PIANOS os ER OE WS S is OSE eRe a EH Sa g 7 4 Spectrograph field of view slit width and seeing T Speekral resolving power lt u fh oe ee Peewee OE ALSO eS 8 System efficiency and throughput 8 1 Transmission of the entrance window B CONV cis u s Q ACE S Sh RE Ge KORR a AAA 8 3 PEL ghosts s seeme a AA A A KSEE BA Stability and reproducibility 44 ie re cars ara a a RU
15. 680 Clm 6 890 EZG0E SLPOE 20808 6201 T PE0 V T ST ST ST80E SCI 6608 S E80 9 6L0 rom O 6GOE c cv0e 4 0 676106 0 860 Z PZ0 U T 8T SI G 140 PCL TIZOE Z68908 S SGOE zeros Lee 9208 SZZOE 98006 S ELOE 6 800 1 1 61 or S6F08 SZI SE90 L TSOS E SPOL S GEOE G IEOE S8TOE 9FTOS 0008 TO90E c I008 U T 6T 61 6 IPOS 9 l 28008 666 Z166Z Cp VELGZ 8966 TPZ 660 L LOOE 9 cr6c 1 0 61 61 Z P86z SEI 000008 99866 6 286 7 88967 87967 T0966 S Sr6c 06683 666c Lv 66 U 0 6T 61 88167 Sr 87768 gosez v 9Z67 Z ITGZ T1067 I68Z7 29887 70488 lite 9486 1T 61 61 8 8I6Z pri 69868 TZ6 LIGZ 0 Z06 1 L68Z 8S I88Z CALSC 470988 losen 01987 U T 61 61 96067 LIL 62167 S9067 06 Close O 888Z GL8Z LIASG 8888 S 8T6Z 90987 1 1 07 0 1687 GIL 9016 6687 L 9680 6 88Z T0887 82987 07987 90588 TTI6Z TEG8Z U T OZ 0 00687 OST 84688 T987 L IPSZ v8Z8Z LHZ8Z SOISZ 89087 EELS LEG8 72612 1 0 07 Oc 0 S 8z TSI 00992 7LEBT L EE8G 0787 99TISc 973087 98626 6848 9 LH8Z 06843 um Oc 0296 XQ KEUN ume iden d ume BURY ume NY ume SN ume qI O Ply y wa wa z wa I wa oe man daqunuannn ut SIDUDA qo4g22ds LOS YG DG AQDI 299 s oxid OE e SI YISU9SALM ADUSISJOI oY JO SUTUOIYSOA oy uo K enooe Y Y WU ul passaiudza wnnava 240 syzbuajaan A 29081 P9IJ9USTAUN OY PISANO 8 911891
16. III Observing with CRIRES at the VLT 9 Introduction 9 1 Atmospheric transmission 2 4 46 48445 Rr eR era ee O2 Background Penoval 232 c nono ko eom bee 4 A BAI Sky emission Spectfum uuo o RP Roe k k Re E 8 225 7 AA uou e e mer X 4 SO h om SP NUR dO X we a E x AA BA NG uuu oe E eec eR RUE XE ee RE ERN p s Eu 93 Fus calibration sad tellurie correction uv o m m x i x oes Dal General procedure uu d ote we Ooh P esed a A RS 9 32 Telluric correction s v sese 0045844 55 ena Pew we XS Roo 0 2 9 Hot stars as fellurie standards 2 22222 kou Rx 9 3 4 Late type stars or G stars as telluric standards Ds DIS uou qus a depA ee es 94 The influence of the Moon 2 2 o o ER GR 10 Observing in Visitor and Service Mode JIM DP UNE uu vox a aede Wu EROR OS EE OR oko dois EE e Cod 102 The Exposure Time Calculator so ss po sens EO X we X ew OX 10 3 Overheads o oco a eS eR Ea wR EEK OR Rw EE ES 11 Preparation of Observation Blocks 11 1 Information fequi nk coe e red ar eine Pew skh Ro dD hip 21 22 24 24 24 24 26 ae 29 29 32 33 33 34 35 35 37 37 37 37 37 37 37 40 40 40 40 41 41 41 42 42 42 45 45 CRIRES User Manual VLT MAN ESO 14500 3486 xi 11 2 Observation Blocks and Templates 4122 254 RR 46 A APO Soya Q Ow e o ode ESS ERS Ae ee hw BS 46 11 2 2 Acquisition sequences with AO 0 0 00002 eee 46 11 2 8 Acquisition sequences without AO 48 IAE E
17. In this case of course TEL T ARG ALPHA and TEL TARG DELTA should be provided On the other hand the user can either enter the coordinates of the AO guide star SEQ NGS ALPHA and SEQ NGS DELTA 60 or the offsets TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA following the convention above 14 2 Observation template This section describes the three observation templates offered in P83 e CRIRES_spec_obs_AutoNodOnslit e CRIRES spec obs GenericOffset e CRIRES spec obs SpectroAstrometry An observation template sets up the instrument if different from the acquisition as well as the detector integration time DIT and number of individual integrations averaged to create an exposure NDIT It defines the number of exposures taken at each nodding position as well as the nodding and if needed jittering offsets The following paragraphs describe only the parameters that are not defined in the previous sections 14 2 1 Detector DETI1 DIT P2PP DIT defines the exposure time of an individual integration in seconds For bright objects saturation of the detector 120 000 e must be avoided On the other hand correction of the non linearity of the detectors incl the odd even effects see Sect 6 4 has so far been achieved to a reasonable accuracy only for a signal dark sky object smaller than about 10 000 ADUs 80 000e7 DIT settings leading to stronger count rate should therefore be avoided The ETC outputs a Max
18. L Z z 2 iaa A ica a ERS a 49 RARE KA aeRO ee UR X En ESS EE EG Se Oe os 49 Ma DIT c 2 lt S a eae ee Bee ee ee AR Q v S Be em Be eB ee 49 11 4 README and finding charts cc cie ooo RR as 50 AE NN oh oe hee gs a S a eH SH RS GRRE s ae ES 51 ILI OO 4 he Sus HE RAE SAS AS ER MERE OR ERD We 51 11 5 2 Seeing and Strehl ratio for adaptive optics observations 51 11 5 3 Seeing for seeing limited observations no adaptive optics 51 1154 Eege a hok w wa u X e de doe Q SE Ee be ee Eee s 51 115 9 AWMI uos Grice ss Sa wee ss S Oo Send Bow Ro QOU A Q 51 iLO Water ENER uud eee e EA ei ees 52 11 7 Offset conventions and definitions 52 IV Reference material 53 12 CRIRES calibration plan 53 13 Data format and reduction 54 Toe Pores 6 u ee yun Se ww s sa b RL EERE SE OEE EYEE EO Ge 54 1329 PGS Qa pog wa qe A AA Box LE Ee eB G 54 14 Template parameters 55 14 1 Acquisition templates 6 4 0 ee ee eR Re eR eRe Oe E 55 14 1 1 Target aud SVGS parameters o 2 ow e 9e wis 3 e XC HERE BO 55 ILLE NOS pares osx dace doe ok P ded eoe eee eA ee ee 57 14 1 3 Parameters related to the slit viewer 58 14 1 4 Telescope guide star parameters o o 58 14 1 5 Derotator parameters s c sce ecs coce E EE xor BORSE s 58 141 6 Spectrograph parameters 1 2 45 a 9 o 59 AA 222349 pede eek owe eb PLES P ere eus wb 59 14 2 a In ample au a red o See Se ee eR She ee Shee con 60 I
19. SISIG RSIS TZSTS LZCIG TCIG lt S S60S T 88OS Com 08cG I96v U O TT IT 6 68IG raz 608 710409 990 9LE0S OSO roue 9667 v96v TZ6TS GZ8y 1 T TT IT 970908 go 00809 87909 sto 2 IZ0S VPTOS T2867 C6L6v 8096F YGALTG 098p U T TT IT 87809 0G Cv66v 996v POMP LECH 0 O660 968v 0 888P Z 8S8p 02909 Z 91 Vc Tl IT S 9F6F 46 SLL6F 6096 9 eV6Y 9 SI6vP 62060 6 8L87 COZSP TOPSY TD90OS 6 88Lv U Z TI IT 96767 Lat L 06h S 88v L OSST 9 T98P S9987 T 9E8D LOES T 609F VOG6P T22L 1 3 31 ZI TILS 6 81 17687 PLSP E6987 O OS8P PPSF rer CSISUV voir 916 091 U c Cl Gl 9698F L OZ TOIS 6 681 VVSLY Coup PLGL CGE LY L eGAV 901 9887 YZE 1 1 21 ZI SELLY 60c 126 0 ALLV LILLY OSL PPr GIZ r VSTZD 077697 TLS Z 0Z9F out GI OTOP te LSLLY gon Lian L Y990v E8997 EVEN LTI root STSALY 8LEG V T Cl GI 7919F LU EZOLP 0089F O FL9F epp rot Or O ETOP 8289 COLLTV Yer U I CT CI C99v T LIcO0V 69 otes Caper Pegar gor racer 8667F Cant Terry Uri ZI 98 8 EVE 99097 9 789 uer C ISGY Error V SIGY GOISh TPP 99997 C Scvv U c Cl ZI 9 E97 YQ SERRA ume Xue Urt XE uy Euh ume icd umi GI Q Py y Pd g jot c wa T oG og USUN daqunuanon ut SIDUDA jo igaads LOS YG DG 2100 299 s oxid OE e SI q3Suo oAeA ADUSISJOI oY Jo Suruoryisod oy uo LVM AY Y uu ul passaidza wnnava 240 syzbuajaan M 29081 po JOUSTAUN
20. TI IT S 9F6F 76 68007 610c S ZZOZ EVEOZ SLEOZ Ou TEGOZ Coon 2261 E TOTS U Z TI IT 9 6Z6v Lat 6E0 890Z 6 8POZ Goen Z 6S0 290 0207 Tom 8 E00 FETIZ 1 3 71 ZI TTS 6 81 BEPOZ S TSOZ Leon 6 T90c ron Gm CG rang 88003 FOZIZ u l I 9698F L OZ 060 Lian ton v660 O ZOTS TITS Ir T SZIZ 090 99812 1 1 21 ZI SEL 60 v80c T EGOZ 29600 T SOIZ LLOIZ SLITS VOZIS TIeIG L T60c Tratt nt GTI OT9LP te VOZIS GOETZ TEETS gt L 9PIZ S LETE TOTG ZLIZ 00607 2022 VT CGl GTI 7919F LU 99cIG SETE leet TOSTZ TESTS SPOTS 82916 16416 960Z SOTZZ U T ZT ZI c99v TPZ 0TOICG TGSLTZ Z 8LIZ O 06TG ECTS L900 60cc EES LGETS 20922 Z ZI Er 98LSv EPG VOLTS TESTS G8IC TLETS 007 T ETZE 6912 DOE OPIS 1 8Sz U c Gl ZI 9 9Sp ng xeul 7 MAMA xeuy utrum xeuyg uyg xeu utu ZP urna GI Q PIY y wa g wa c wa T 39d osuel usrAu dE ut sabuns qo4222ds aof Y D07 algo 2929 sjextd QE Y st YISU9SALM oouol9Jol oY Jo Suruorjrsod oy uo LIINI aq a3uel payyou3raun OY SPISMO JVJ ILY UL UOATS son peA IoquinuoAeA jI S DOSIL c Y 1oJ TOAST T Wey o1our ye AyyIqionpoidad Jo yor Aq poyoorye st oSuer e1320ds po33ouSrAun y Jo opIs yno DOIT Ioyourered e se poytoods oq os e 3snur JoqUINU 19PIO 9Y yey s yeorpur V e 1032939p 103 foxtd uio QT ut 19 uorsJodsrp ue ur 91 SISI uumoo ISP oq WATS OSTE ore 103293op MO
21. Table 2 lists the instrument sensitivities The table is intended as a quick reference only Proposers should refer to the Exposure Time Calculator Sect 10 2 for more precise estimates In particular one should note that the grating blaze function introduces a large sensitivity variation within any given order Table 2 Point source sensitivities determined using a 0 4 slit adaptive optics optical seeing of 0 8 The values listed correspond to a S N of 10 for a 1h on source integration in one spectral dispersion element They are obtained by integrating the profile along the spatial direction Band Sensitivity Magnitude mJy J 11 15 4 H 11 15 1 K E 14 6 L 9 5 11 2 M 26 9 4 Short ward of 1100 nm the spectral range accessible to CRIRES overlaps with the one acces sible to UVES For the observations of specific spectral features in this region it is interesting to compare the efficiency of the two spectrographs Figure 21 shows the S N of two spectra of the J 1 3 star Col obtained nearly simultaneously with CRIRES and UVES on February 7 2007 while the star was at an airmass lt 1 07 with very similar seeing conditions 35 In both cases the slit was constantly aligned along the parallactic angle ELEV mode The first spectrum in red was obtained with UVES with a slit width of 0 3 providing a resolution R 110 000 The other one in blue was obtained with CRIRES using AO and a slit width of 0 2 p
22. a bread board located between the Nasmyth focus and the spectrometer It is about 1 5m wide and a top view of the warm optics overlaid by the optical path is shown in Fig 5 the assembly of the deformable mirror is displayed in Fig 6 3 2 1 The corrective optics The wavefront correction is performed by a 60 electrode bi morph mirror developed by CILAS with a pupil diameter of 60 mm The 60 electrodes are sandwiched between two thin piezoelec tric PZT layers with opposite polarization The outside surface of the PZT layers are grounded and covered with 0 1mm glass layers the mirror side being silver coated Applying a voltage to one electrode produces a constant curvature over its surface The geometry of the electrodes in the 4 central rings 40 electrodes matches that of the lenslet array sub apertures while the 20 remaining electrodes are located outside the pupil and constrain the edge of the pupil to correct 0 curvature aberrations tip tilt astigmatism etc The deformable mirror DM provides a stroke to compensate atmospheric aberrations up to an optical seeing of 1 In order to relax the use of the outer electrodes of the mirror the tip tilt error is slowly offloaded to a tip tilt mount designed and built by LESIA which provides a 240 mechanical stroke i e 3 6 on the sky with a 100 Hz 3dB internal closed loop bandwidth The assembly of the DM and tip tilt mount is shown in Fig 6 3 2 2 The Wavefront Sensor The follow
23. at this stage the CRIRES team can only aim at providing the necessary information to apply such a method for the following DIT values e Short exposures on objects brighter than J H K 8 10 mag or in the L or M bands should use DITs of 1 s 1 5 s 2 s 3 s 5 s 7 s 10 s 15 s 20 s 30 s or 45 s e Long exposures on faint targets must select DITs of 60 s 90 s 120 s 180 s 300 s or 600 s For DIT of 900 s a waiver is required 50 Note however that optimal flat fielding correction in particular for the odd even effect re quires that DIT be at least 2 s 86 4 NDIT is specified by the observer to reach the required SNR as computed with the ETC 11 4 README and finding charts General instructions on the README file and finding charts are given at http www eso org observing p2pp while CRIRES specific requirements can be found at http www eso org observing p2pp CRIRES CRIRES P2PP html Appropriate and detailed finding charts are crucial for the success of observations especially in crowded fields e The field of view of the finding chart should be 50 by 50 in size with a clear indication of field orientation The target should be clearly marked by an arrow If observations are performed with the derotator in SKY mode the slit orientation should be clearly drawn e For high proper motion stars gt 1 year the present day position should be indicated by an arrow pointing from the target in the chart to the
24. c Y IOJ TOAST T Wey o1our ye jr rqronpoadoz Jo yoe Aq poyooye sr oSuer Tetjods po JousSTAUN 913 JO oprsjno uoreurum 1o3ourered e se pogroods oq os e 3snur 1oquinu Iop1o oY jeu sojeorput V e 103293op 103 oxid uio QT UL 19 UOTsIOdsIp ue ur 91 SISI Otto ISP oq WATS OSTE ore 103293op MO ot JO qoo 103 uio ut posso1dxo ol 1oquinuoA A VINNIPA ur oge19A00 pue oguei erjoods poyjoustaun q uorjeogrjuopr q33u AeA euiojur Q JoquINU JopIQ 1o019919p PIE eu Jo ZIG Joxid ye q33uo oAeA oY se paugop sSur33es YSUSTOARM prepuejs OY 103 WU ur PY sq3suo pAeA 95U919J91 3 QLL 87 TGT E EGST L6S8T S I99T POST OLST MLLST LGL8T GLSST IST 06761 ut TT Tages GGT 681 8 E98T FIST 9 CAST PLST gt Cragg T Z68T ELIST GEGGT U Z TT IT Z Oq8q G IZ 8881 2 968T 26981 ont 6 061 V9IGT 6 8T6T 6266T SERI Z 6961 T TT IT T 89cG SIZ 87681 T0061 SZ06T 9 016T 6 CGT6T GIZ6I OTG6T ZEEGT O G91 SPL6T U T TT IT Tepes IEZ 9661 TES6T SSEGT SPPEL TLVGT 29961 S6S6T Lopert 669981 86002 0 TT IT 9 PETS S EZ 86761 S8E6T O TP6T Z OSGT LZS6T SZ96T 9961 2 SL6T ST68T Congo IT 6 6ETS PSZ 9961 SZLET 6261 T S86T 6 L86T 98661 S TOOZ T ETOZ 09261 T1S0 1 T TT IT 9 0909 go 8961 8L6T O TS6T VIG6T Cropt Z900 rang Gong SECT S LS0 U T TT IT 8808 02 00 O ETOZ O 9TOZ E2LZ0 amp Og0c VZPOZ gor v890c LL96T cv60c Z
25. consequence the wavelength configuration table has slightly changed users wishing to use the standard wavelength settings should refer to the reference wavelengths listed in Tables 4a to 4h or 5a to 5h Note that these tables now include two new columns referring to the unvignetted range i e the spectral range over which the illumina tion could be reproduced to better than 196 despite the lack of reproducibility of the intermediate slit mainly and other optical elements Part I The instrument 2 Cold part the spectrometer The CRIRES instrument design is presented by mary is presented in the following subsections C R R E S de rotator telescope E gt gt deformable mirror dichroic window Vacuum 65K focal reducer Se df wavefront slitiviewer sensor DS pupil filter 4 lt lt a pre disperser detector mosaic echelle grating 3 mirror TMA I collimator camera Figure 1 Layout of the CRIRES optical design a sum 2 1 Optics The optical layout of CRIRES is shown in Fig 1 Light enters from the direction of the telescope Nasmyth focus either via the telescope or from the calibration unit after insertion of a calibration mirror in the light path The calibration unit itself consists of an integrating sphere illuminated by a continuum Halo gen lamp for flat fielding and together with a gas cell for wavelength calibration An IR emitter lamp used for technical tests is also
26. have more than about 10 000 ADUs 70 000e 3 this is particularly relevant for observations in the L or M bands b for observations of relatively faint targets in the J H or K bands the choice of long DITs gt 60s should be balanced with the increased noise brought by the detector glow and the advantage that multiple exposures allow a better flat field correction in particular if some jitter is introduced 4 Service mode programmes are executed using Observing Blocks OBs that should last less than 1 hour Except for an associated telluric OB a science OB is the typical unit of observation that should be completely independent of other OBs of the same programme Indeed different OBs of a given programme are usually observed in different nights As a consequence a The amount of time to request has to take into account all overheads in particular the ones associated with preset and acquisition for each OB b Typically each science OB should have one associated telluric OB Some exceptions occur for example when targetting a specific line located away from any telluric absorption features The amount of time to request has to take into account the time to execute all associated telluric OBs In particular one should not assume that one telluric OB will be useful for several science OBs 95 19 2 Phase 2 1 If the slit orientation on the sky is not important for the science objective the ELEV mode is strongly recomm
27. intensity at central pixel per DIT object sky and therefore allows one to check if the chosen DIT is adequate It is important to check that the ETC input parameter requested wavelength does not correspond to a deep absorption line either in the target spectrum or caused by the Earth s atmosphere For faint objects in the J H and K bands long DITs are recommended in order to decrease the contribution of the RON to the overall noise See Sec 11 3 for recommended and offered values DETI NDIT P2PP NDIT determines the number of individual integration averaged into one exposure Therefore DET1 NDIT x DET1 DIT sets the total integration time of one exposure SEQ NEXPO P2PP Number of exposures per nodding position is the number of expo sures in any nodding or offset position Therefore the integration time spend in one nodding position is given by DET1 NDIT x DET1 DIT x SEQ NEXPO 14 2 2 Gas cell INS OPTI1 NAME P2PP Gas cell sets the gas cell to be used The default value FREE should be set for observations without gas cell while GAS_N20 or GAS_CO should be set for observations with the N3O or CO gas cell respectively 1 4 61 14 2 3 CRIRES_spec_obs_AutoNodOnSlit and CRIRES_spec_obs_SpectroAstrometry nodding and jittering SEQ NABCYCLES P2PP Number of nodding cycles sets the number of AB or BA nodding cycles Although the value of 0 is allowed staring it is not recommended because of detector glow and other sys
28. large enough so that the spatial profiles of the target in the two nodding positions do not overlap The nodding positions are located symmetrically at SEQ NODTHROW 2 around the centering location SEQ JITTER WIDTH P2PP Jitter width A jitter is a small offset added to each nod ding offset It helps correcting for bad detector pixels Sect 9 SEQ JITTER WIDTH gives the width of the jitter box the maximum offset from the nodding position is therefore given by half of this value The successive values of the jitter offset in a given template are drawn from a set of 100 numbers determined from a Poisson random number generator Jittering is currently not possible if SEQ NABCYCLES 0 staring mode 14 2 4 CRIRES spec obs GenericOffset only list of offsets The CRIRES spec obs GenericOffset allows the user to define a list of offsets offering more flexibility for sky subtraction in case of extended objects It only makes sense to use this template if INS DROT MODE Derotator mode is set to SKY in the acquisition template SEQ OFFSET COORDS P2PP Offset coordinate type selection determines if the list of offsets given in SEQ OFFSETI LIST and SEQ OFFSET2 LIST are given in SKY or DE TECTOR coordinates 62 SEQ OFFSET1 LIST SEQ OFFSET2 LIST P2PP Lists of offsets in RA or X Lists of offsets in DEC or Y In all cases the list of offsets are in arcseconds If SEQ OFFSET COORDS is set to SKY a positive value in SEQ OFFSETI LIST
29. lenslet array Each lenslet feeds an avalanche photo diode APD that ultimately forwards its signal to the Real Time Computer RTC Sect 3 The flux on an APD is limited to 1 million counts in order not to damage the devices The optimal brightness of the AO star is R 11 mag Brighter stars up to a bright magnitude limit of R 0 2 mag can be dimmed using neutral density filters Depending on the B R color some stars with slightly brighter R magnitude can be used Good correction is still obtained with stars as faint as R 14 mag under average seeing condi 19 tions while moderate image quality improvement is seen with stars as faint as R 16 17 mag under good seeing lt 0 6 conditions Stars fainter than R 17 mag will not result in any improvement 5 1 3 The color of the AO star The color is essential for precise atmospheric refraction compensation The AO system takes into account the differential atmospheric refraction between the wavelength used for the AO and the central wavelength of the spectrograph set up in the calculation of the tip tilt mirror orientation 5 2 Limiting magnitude of slit viewer Target centering in the NIR is optimized by slit viewing The slit viewer SV is sufficiently sensitive that any emitting point source for which one aims to obtain a spectrum should be seen on the SV image In particular in AO mode stars of J 14 or H 14 are easily detected in a 10s exposure a typical time scale for
30. means that the new pointing of the telescope is to the east relative to the previous location similarly a positive value in SEQ OFFSET2 LIST means that the new pointing of the telescope is to the north relative to its previous location During the first exposure the telescope points to the location given by TEL TARG ALPHA TEL TARG DELTA the first value given in SEQ OFFSETI LIST SEQ OFFSET2 LIST In other words in this case the offsets corre spond to telescope offsets Slit viewer detector SEQ OFFSET COORDS SKY SEQ OFFSET1 LIST 0 10 0 17 5 0 7 5 SEQ OFFSET2 LIST 0 08 0 8 0 SEQ OBSTYPE LIST OOS S00 Slit enlarged Figure 25 Illustration showing the apparent locations of a target as seen on the slit viewer detector for the given parameters in the case of SKY coordinate offsets If SEQ OFFSET COORDS is set to DETECTOR the offsets correspond to the apparent motion of the target on the slit viewer detector with X increasing from left to right from E to W if the position angle is 0 deg and Y increasing from bottom to top from S to N if the position angle is 0 deg see Fig 17 In other words in this case a positive offset in both X and Y would bring the target to larger X and larger Y values as seen on the slit viewer If the position angle is 0 this corresponds to a motion of the telescope to the East and South Subsequent offsets are similarly made relative to the last telescope offset SEQ OBSTYPE L
31. objects a sky frame is not required for good guiding and therefore may not be taken In crowded fields the choice of a good slit viewer guide star SVGS is important It must not be too close to another star in particular to a brighter star the latter should be chosen instead No object should contribute significant flux within the area limited by the guiding box whose width is optimally set by the instrument operator The guiding box has a minimum width of 0 4 Note that if the SVGS is also the target and therefore also partially hidden by the slit the width of the guiding box will typically be at least 0 2 wider than the slit width 11 2 2 Acquisition sequences with AO In this section we briefly describe the sequence of events taking place during the execution of the acquisition templates 2NGS is an AO natural guide star contrary to a LGS which is laser guide star using the LGS facility This is not available for CRIRES 47 General case NGS z SVGS Target The most general acquisition for observation with AO takes place when the science target the SV guide star and the AO guide star NGS are all different Its sequence is the following 1 preset the telescope to the NGS possibly recenter it 2 acquire the NGS with MACAO and close the AO loop Offset the telescope to the SVGS interactively re center the SVGS start guiding QO Oo A C2 offset the telescope to the target if the target is b
32. output provided by the ETC 9 2 2 Nodding The purpose of nodding is to correct or remove sky emission detector dark current and glow Fig 13 and some ghosts In a simple application of this technique a spectrum is taken at telescope position A after which the telescope is moved along the direction of the slit to position B and another spectrum is taken By subtracting the A and B images dark and sky subtractions are performed The number of nodding cycles and the nodding throw if smaller than 20 are free observing parameters Because of the extended wings of the PSF a nodding throw greater than 5 is recommended preferably 10 9 2 3 Jittering The purpose of jittering is to correct for bad pixels and decrease systematics due to the detector This is particularly important for CRIRES observations Indeed the detectors suffer Oo T e e 1200 o e x 1800 boils 1600 1700 Sa d M leie 0 8 0 6 0 4 o2 0 0 ll EE gt gt Transmission 1800 1900 2000 2100 2200 25 00 1 0 0 8 0 6 0 4 0 2 0 0 d I x l III 2300 2400 2600 2800 3000 3200 3600 3800 4 o 1 0 0 8 0 6 0 4 0 2 0 0 3400 4000 4200 4400 4600 4800 Wavelength nm 5000 5200 5400
33. parallel to the spectral dispersion for detectors 2 and 3 For detectors 1 and 4 the pattern is instead aligned with the columns i e perpendicular to the spectral dispersion This pattern consists of alternating rows or columns of larger and smaller intensities than the mean value 22 rms 5 8 ARA DN Mec ES a a P oh Vete rms 0 95 Meg Umm rms 0 15 relative signal ADU s 200 400 600 800 1000 pixels detector 1 Figure 14 Flats obtained with the halogen lamp at different DITs for detector 1 Each graph represents 1000 pixels of the image collapsed along the columns A DIT 1s dark exposure has been subtracted from each image From top to bottom a a 3 s flat ff3s normalized to its median value shows a bimodal distribution of intensities reflecting the odd even effect The measured RMS of the normalized flat is 5 8 Panel b shows the ratio between two dark subtracted flats of 11s and 3s respectively The ratio shows an RMS of 0 95 Panel c is similar to b but for flats with DITs of 3 and 7s respectively The RMS of the ratio is 0 36 Panel d shows that the ratio for 2 flats obtained with DITs of 2s and 3s respectively has an RMS of 0 15 The decrease of the scatter in the ratio of flats when DITs tend to be similar demonstrates that the odd even effect depends on the signal level This effect cannot be removed by simple flat fielding and is still visible after nodding Figure 14 gives an e
34. present day position especially if similar bright sources are around e The finding chart has to show the field in the NIR band closest to the observing wave length OBS in J band if 950 nm lt ogs lt 1300 nm in H band if 1300 nm lt ogs lt 2000 nm or for very bright targets in K band if 2000 nm lt ogs lt 5400 nm Note that the ESO infrared digitized sky II actually correspond to the I band and should not be used if other infrared images are available e g 2MASS e In crowded fields a second finding chart should be attached to the corresponding OB with a zoom in on the science target s e Incase of binary or multiple stars the target must be clearly indicated in particular a in case of large proper motion including relative proper motion b in case the finding chart was obtained in a band pass that does not include the observing wavelength e AO SVGS and science target should be clearly marked If the AO star or SVGS are less than 15 from the edge of the finding chart centered on the target another 2 by 2 finding chart should be provided The magnitude of the AO and SV guide stars of the science target and of the standard stars should be explicitly given in the Instrument Comments field of each OB Please check the CRIRES P2PP related information at http www eso org observing p2pp CRIRES CRIRES P2PP html for more details 51 11 5 Constraints 11 5 1 Moon As stated ab
35. product technique JITTER OTHER DPR TYPE STD Data product type 68 CRIRES_spec_cal_LampFlats To be specified Parameter Range Default Label INS WLEN REF INS GRAT ORDER 958 3 5361 9 NODEFAULT 0 59 0 Reference wavelength Grating order Fixed values Parameter Value Label DPR CATG CALIB Data product category DPR TECH SPECTRUM Data product technique DPR TYPE FLAT Data product type CRIRES_spec_cal_Wave To be specified Parameter Range Default Label INS LAMP INS WLEN REF INS GRAT ORDER THAR HALOGEN N20 CELL HALOGEN CO_CELL THAR 958 3 5361 9 NODEFAULT 0 59 0 Wavelength calibration source Reference wavelength Grating order Fixed values Parameter Value Label DPR CATG CALIB Data product category DPR TECH SPECTRUM Data product technique DPR TYPE WAVE LAMP ABSORPTION CELL Data product type CRIRES_spec cal_Darks To be specified Parameter Range Default Label DET1 DIT 0 900 60 DIT DET1 NDIT 1 1000 1 NDIT SEQ NEXPO 1 100 3 Number of exposures Fixed values Parameter Value Label DPR CATG CALIB Data product category DPR TECH IMAGE Data product technique DPR TYPE DARK Data product type 69 15 CRIRES standard wavelength settings 15 1 Wavelength ranges 70 71 qq TIIT LOL Z60Z1 Y EOZT OZOZT T96TT SVETI
36. require short DITs to avoid saturation in particular heavily saturated spectra lead to detector remanence that affects subsequent observations On the other hand faint targets in the J H or even K bands may require DITs up to 900s to decrease the readout noise contribution Long DITs are strongly affected by the detector glows which can be corrected by nodding Sect 9 2 All other detector settings such as bias voltages operating temperature etc are automatically set by the system Currently the only read out mode used is Fowler Sampling Fowler amp Gatley 1990 ApJ 353 L33 the detector is first reset then each pixel is non destructively read NDSAMPLES 2 times at the start of the exposure then again NDSAMPLES 2 at the end of the exposure of exposure time DIT The slope of the relation provides the intensity of the given pixel The value of NDSAMPLES is 2 for DITs strictly smaller than 10 s 4 for DITs at least equal to 10 s but strictly smaller than 20 s etc up to a maximum of 128 6 1 Dark and gain In Fig 12 dark current and conversion gain of detector 2 are shown The dark current is estimated from the slope of the signal in ADU or e as a function of integration time s for the linear region Dark current gain read out noise saturation of the four detectors 1 2 3 and 4 as well as the operating temperature are given in Table 1 Note that the raw gain values cf Fig 11 have been corrected by a factor of 0 9
37. stars 11 2 1 Acquisition The objective of the acquisition template is to preset the telescope and to center the target in the slit Point sources shall preferably be observed in ELEV mode where the slit is constantly aligned with the parallactic angle in other words along the atmospheric refraction direction For specific needs to align the slit on the sky at some position angle the SKY mode shall be used CRIRES offers two types of acquisitions 1 The target itself or a star angularly close to it closer than 30 can be used to determine the shape of the wave front and therefore can be used to drive the adaptive optics system 2 No adaptive optics is possible or requested because there is only an extended or a faint science target without a bright compact object in the field Two acquisition templates allow to distinguish between the acquisition modes AO CRIRES_spec_acq_NGS No AO CRIRES_spec_acq_noA0 AO correction is always performed on an NGS In both acquisition methods a sky frame can be taken in an offset field The slit viewer detector control system subtracts this sky from each new image used for guiding in order to enhance the contrast in the SV image It is crucial for faint targets Two acquisition images are usually delivered to the user in the final data package the sky frame as well as the final centering of the target in the slit at the end of the execution of the acquisition template However for bright
38. t Jo qoo 103 D uio UL posso1dxo ol JOqUINUSARM WINNA ur oge19A00 pue oguei e1go ds poyjoustaun Q uorjeogrjuopr u3Suo oAwA euiojur Q JoquINU JopIQ 1o15919p pig ol Jo ZIG Joxid ye u3Suo oAeA oY se pougop SSUI JoS qjguo pAe prepuejs ayy 103 WU ur y SYJBUAPALM DOUOIOJOY YG APL 88 16 Free wavelength settings Table 6a Available ranges of the reference wavelength Aref for the free settings Values should be rounded to the closest 0 1 nm A besides an order number indicates that some reference wavelengths in that order are common to an adjacent order see Table 7 in which case the order number must also be specified as a template parameter O min max ref ref 99 9583 961 0 58 974 8 977 6 57 99139 994 8 56 1009 6 1012 5 55 1028 0 1030 9 54 1047 0 1050 0 53 1066 8 1069 8 52 1087 3 1090 4 51 1108 6 1111 8 50 11308 1134 0 49 1153 9 1157 2 48 1177 9 1181 3 47 1203 0 1206 4 46 1229 1 1232 6 45 1256 4 1260 0 44 1285 0 1288 7 43 1299 8 1333 5 42 1330 8 1365 2 41 1363 3 1398 5 40 1397 3 1433 5 39 1433 2 1470 2 38 1470 9 1508 9 37 1510 7 1549 7 36 1552 6 1592 7 35 1597 0 1638 2 89 Table 6b Available ranges of the reference wavelength Aref for the free settings Values should be rounded to the closest 0 1 nm A besides an order number indicates that some reference wavelengths in that order are common to an adjacent order see Table 7 in which case the order number must also be specified as t
39. to take into account the interpixel capacitance see Finger et al 2006 SPIE 6276 62760F 21 Dork Current CRIRES Mosoic 2 PTF of CRIRES science detector 2 goin 7 664 0 082 e ADU Signol e Voroionce ADU 2 dork current 3 174E 001 3 5E 003 e s o de A A etre see b 0 5 0x10 1 0x10 1 5x10 2 0x10 2 5x10 0 1000 Integrotion time s 2000 3000 4000 5000 Signal ADU Figure 12 Dark current left and conversion gain right of detector 2 6 2 Glow The detectors show glow over areas close to the amplifiers as clearly visible in Fig 13 It is stable and can be subtracted by an exposure obtained with the same DIT Therefore in order to best remove it as well as other detector systematics it is recommended that observations in any given wavelength setting should include at least one nodding cycle Note however that areas affected by the glow suffers from increased Poisson noise 6000 Figure 13 Example of the detector glow on a dark exposure The detector glow in red is emerging from the bottom corners of each detector 6 3 Fringes No detector fringes are detected in the wavelength range useful for science observations Fringes are only visible beyond 5um outside the atmospheric window 6 4 Odd even effect Images obtained with the science detectors show a pattern aligned with the reading direction In other words the pattern is aligned with the rows of the detectors
40. use the N2O during the observations themselves that is to have the gas cell on the light path of the astronomical object First results from science verification or commissioning data or regular science observations indicate that a radial velocity accuracy of the order of 20 to 30 m s can be reached A monitoring programme has started to determine the long term behavior It is important to note that the atmosphere itself contains N20 Therefore it is difficult to disentangle the origin of N2O lines originating in the gas cell from the ones originating in the atmosphere at least in the L or M band In the K band N20 lines originating from the atmosphere are weaker but still present Similarly the CO gas cell can also be used for observations Its use is particularly recommended in the K band order 24 26 The CRIRES team is actively working on alternative solutions for wavelength calibration such as an accurate instrument model or the use of additional gas cells In particular it is currently testing an OCS gas cell in laboratory 7 2 2 Radial velocity measurements Huelamo et al 2008 A amp A 489 9 and Seifahrt amp Kaeufl 2008 A amp A 491 929 have demonstrated that accurate radial velocity measurements to better than 35 ms 1 even possibly to 10 ms 1 are feasible with CRIRES The Seifahrt amp Kaeufl 2008 study covered data over only 4h 30m while the Huelamo et al 2008 study extends over slightly less than 7 days Al
41. wavelength calibration for each order 1 Sky lines A possible output of the ETC is the emission sky spectrum for the requested reference wavelength Its examination should provide enough information as to decide if the required wavelength accuracy can be achieved 2 ThAr lamp For wavelengths below 2300 nm the Thorium Argon lamp provides enough lines for a good wavelength calibration Since April 2008 the ThAr spectra are obtained by means of a set of fibers This method allows to avoid strong scattered light sometimes mimicking real lines and making the identification difficult The several spectra obtained also provides a way to determine the distortion of the spectrograph 3 M20 gas cell For wavelength longer than 3500 nm N20 is a strict National Institute of Standards and Technology NIST wavelength standard For shorter wavelengths the available line list originates from the HITRAN database itself based on Toth et al see http cfa www harvard edu hitran Unfortunately N20 has no lines below 1650 nm and only weak lines between 1650 2100 nm Their distribution over the detectors for a given wavelength setting can be seen by using the ETC A line list can be accessed from the Tools section in the CRIRES web page 4 CO gas cell A CO gas cell is now available since April 2008 The line list is also available at the NIST web site and will soon be available at the Tools section of the CRIRES web page It is also possible to
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50. ALOGEN N20 useful ranges 4136 7 4145 9 4161 9 4177 9 4234 3 4368 8 4411 7 4528 6 12 HALOGEN N30 useful range 4484 0 4702 4 11 HALOGEN N20 useful range 5250 0 5395 6 94 Part V Tips for successful observations 19 Checklist In this section we provide a number of recommendations in order to increase the chances that a program is executed successfully 19 1 Phase 1 Before submitting an ESO proposal involving CRIRES the following points should be taken into account 1 Tables 4a 4h and 5a 5h provide the current best estimate of the unvignetted spectral ranges for each standard setting i e the one for which illumination should be repro ducible to the 1 level If the interesting spectral features are affected by detector glow or vignetting in a standard setting a free wavelength setting may be chosen to optimize their location on the detectors See also 8 7 1 2 The expected S N for each object should be given in the time justification it must be stated if it corresponds to the S N per pixel or per resolution element For extended objects it is important to state if it corresponds to the S N per pixel in the spatial direction or over the whole expected extension along the spatial direction 3 Overheads can only be reasonably estimated if the DIT has been appropriately chosen Although long DITs allow to reduce overheads it is important to note that a the total object plus sky spectrum should not
51. I1 NAME INS WLEN REF SEQ NEXPO SEQ NOFF SEQ OBSTYPE LIST SEQ OFFSET COORDS 0 900 NODEFAULT 1 100 1 1 100 1 0 59 0 FREE GAS N20 GAS CO FREE 958 3 5361 9 NODEFAULT 1 100 1 1 100 NODEFAULT O S NODEFAULT SKY DETECTOR SKY DIT NDIT for the OBJECT positions NDIT for the SKY positions Grating order Gas cell Reference wavelength Number of exposures on each position Number of offset positions List of observation types O or S Offset coordinate type selection SEQ OFFSET1 LIST NODEFAULT List of offsets in RA or X SEQ OFFSET2 LIST NODEFAULT List of offsets in DEC or Y Fixed values Parameter Value Label DPR CATG SCIENCE Data product category DPR TECH SPECTRUM Data product technique DPR TYPE OBJECT or SKY Data product type 67 CRIRES_spec_cal_AutoNodOnSlit To be specified Parameter Range Default Label DET1 DIT 0 900 VODEFAULT DIT DET1 NDIT 1 1000 1 NDIT SEQ NEXPO 1 100 1 Number of exposures per nodding po SEQ NABCYCLES 0 100 1 Nube of nodding cycles SEQ NODTHROW 0 22 5 10 Nod throw along the slit SEQ JITTER WIDTH 0 8 0 Jitter width INS OPTI1 NAME INS WLEN REF INS GRAT ORDER REE GAS N20 GAS CO FREE 958 3 5361 9 NODEFAULT 0 59 0 Gas cell Reference wavelength Grating order Fixed values Parameter Value Label DPR CATG CALIB Data product category DPR TECH SPECTRUM NODDING DIRECT Data
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53. IST P2PP List of observation types O or S is a list that determines if the exposure taken once the corresponding offset has been completed is an OBJECT O or a SKY S measurement Therefore the total integration time of one exposure in an OB JECT location is DET1 NDIT OBJECT x DET1 DIT Similarly the total integration time of one exposure in SKY location is DET1 NDIT SKY x DETI DIT Note that SEQ NEXPO exposures can be obtained at each location 63 Slit viewer detector SEQ OFFSET COORDS DETECTOR SEQ OFFSETL LIST 0 0 0 08 00 8 0 0 SEQ OFFSET2 LIST 0 0 10 0 0 17 5 0 0 7 5 SEQ OBSTYPE LIST OOSS00 Slit enlarged T Figure 26 Illustration showing the apparent locations of a target as seen on the slit viewer detector for the given parameters in the case of DETECTOR coordinate offsets Although the derotator mode must be set to SKY the position angle is irrelevant since all the motions are made in detector coordinates SEQ NOFF P2PP Number of offset positions gives the total number of telescope po sitions that the telescope will have during the execution of the template Minimum value is 1 If this value is larger than the number of values listed in SEQ OFFSETI LIST or SEQ OFFSET 2 LIST then the list is started again For example if SEQ NOFF 5 SEQ OFFSETI LIST 0 0 0 and SEQ OFFSET2 LIST 70 10 10 SEQ OFFSET COORDS DETECTOR the list of offsets will be 0 0 0 0 0 along t
54. L 760L GEP69 2 L80L U T 6E 6E Gert C9 6669 17669 10069 S T669 66669 8 ZE0L EZPOL 99404 9 1v69 Z TSOL 1 1 07 OF Gert 9 97769 T1169 6269 nm S6TOL ron 9 90L 44604 0969 TIL0L u 1 0 OF 9 6ZFI 89 97104 S LOTZ 6911 991 EZ9TZ V66TZ S OTZL I 096L 00TZ O 9TZL VT Ov OF out 69 29604 T6CIL 8 8 TZ MPLIL 6V8TZ SEL SEEZL 8 ELGL IL G 8EZL U T 0P OF 282681 0 9 49604 99 YSI ron TSITA 8 80 L L 8TZL Che i VSTIZ GIEL Vum TV 998681 T9 6TIIL 6YVIL VESTAL Cost S TOLL 987 C9822 STLEL LYSlL 6 9vcL um Th 8 v6ET 99 TIGEL VS86L 0622 VTIEEL YTVEL G6LEL OT6EL TITEL 846L 69682 VTI Iv Tv vL9ET L9 Z2 LO L 69182 TEGEL Igel OSOL OTT oeh 00 4 v8TDL U T Tp Th o E9 T 69 TOLGL 00 L 680 2 TITEL TOSEL VP8El SV6EL TITEL L 68cL O 1 1 77 GV oner 0 9 992 O 6TEL Y LZEL T T9EL 269 Z S0PL TSTDL Teer vV60EL PEs our ZV 9 T9ET 99 ESEL TEIL SELL OIGL VOZSA L6SGL CTAGL L 619L ULGVAL 898292 U T GV 8 vE T G9 667fL 9 98vL TS6PL 0 ESL SEPSL 8 89 8969 FLEIM V6LVL Y 6692 U T Zb ZV o8 OEET SCAS S ELDL CCSVL VGIGL OSZGL S0992 9OLSL 909 SEL 98292 YI ED Er GEI 88 TG9FL Ve6vL vcOGL V9ESL VAAL GISGL G T6SL 9669 6 E8VDL 1669 U T eV EV Got 9 909 moi TIS9L 8889 76694 6 624 ETSLL 9 E6LL SVEWL 6842 YI ED ev gout vV9 SLE9L 099 0349 T ETZL SECLL 9YV9LL L OLLL 8
55. L PT CL IESTL air TVI TLIVI c GOYT Girl Coppi GTI cat OPSI U T 8E 88 6 OLFT XQ xeu ume NEU up EN ume iin 4 ume Xen Umm qI O Pv v wa wa z 3g T o mei man SIQUNUIADN ut SIDUDA qo4g22ds LOS YG DG 2100 299 s oxid OE ez SI q3Suo oAeA ADUSISJOI oY JO SUTUOIYSOA oy uo LIVIN Y Y WU ul passaiudza wnnava 240 syzbuajaan A 29081 po JOUSTAUN oY PISPMO 8 911891 ut uoAIS son peA YYSUPOARM PMS ISL c Y 10 TOAST YT wey o1our ye jrpiqronpoadoz jo yor Aq poyooye st osues erjoods pojjousrAun oY JO oprsjno uorjeurumg I Joyowered e se payroods oq os e 84 1oquinu Jop1O oY 3er so3eorput V 103293op 103 Toxid uru QT ut YE uorszodsrp ue ur o SISH uump oo ISP oq UOA ose ore S1032939p MOJ oy JO Yo 10 oseIoAOD pue oguei e1joods poyoustaun q uoryeogrguopr q3Suop o eA euirojur Q Joquinu I pIO 1035939p PIE ou Jo ZIQ exid ye qjSuo o eA oY se peugop sSurjjes prepuejs oY 10 Py sqySuopenem DOUSIOJOY OP ALL 74 G6 LTE VIZ 660ZZ Uz V26IG Cette HELIS TRI V6LIG 1 1 97 9 emt 96 09568 990 OPOZE SETS VIGIS TISIZ T 8LIZ EL9TS VIZ ELIG U T 9Z 9 T66TZ VOL SPLIG 9YV91Z SIO TISTE C SvIC Ditz SEIS amp 2878 E 69TZ 6 671Z 1 T1 9 9 S9STZ GOL 891 TRGIZ VSSTE OPIS YTPTE VOETE GLEIC GSTs 8 Z9TE T EZIZ U T 97 9 0 0STZ C6 6678 DOTS PSI L8TIC TOTIZ 90TZ VEOTZ zoue gott 6 860 VII LZ VETS 6 07618 6PTIZ GI
56. LI Detector a NW SE Cu SE AAA Bed eR e Sos x E EDA wg 60 o EI cog yng iy it AR E A E ee AA 60 14 2 3 CRIRES_spec_obs_AutoNodOnSlit and CRIRES spec obs SpectroAstrometry nodding and Jittering o so s sor cr rara Ee A 61 14 2 4 CRIRES_spec_obs_GenericOffset only list of offsets 61 14 2 5 CRIRES spec obs SpectroAstrometry only list of derotator angles jit HOP PES ce aree ee GR Q aS es See Amex p ecb ee Rufe Be a 63 CRIRES User Manual VLT MAN ESO 14500 3486 143 Calibration templates uo ei ek or ea SES eee ee we CS a ge ES 14 3 1 Standard star or telluric observations 226 eee be rr Mi PIC cur Za EE Se OE ee ee ee EA 14 3 3 Wavelength calibration 2 cuo om RR ERRARE A a xs a A eA HA RO ESSE FEES ROS 14 30 Template Seige nk wee X EROR E A KE EGER RR OE s 15 CRIRES standard wavelength settings 15 1 Wavelength ranges o o E ROS RO RO eA Ewe Ee He EE 152 EEN Tans u uy 2 RE Ee OR ie ORE RC OE E eon 16 Free wavelength settings 17 Reference wavelengths common to different orders 18 Calibration source for wavelength calibration V Tips for successful observations 19 Checklist ID PROS oras A oA Sy LAS Weed hm ESE Nes Rene EES E e 192 Phase coo Boe Ree x 3 Lo we ee oc x Poe eee be 4238 o4 xii 64 64 64 64 64 65 70 70 79 88 90 91 CRIRES User Manual VLT MAN ESO 14500 3486 1 1 Introduction The cryogenic high resolution IR echelle spectrograph CRIRES is the in
57. OY oprsjno 9j 911891 Ul uoAIS SoNTeA YISUSPOARM PMS ISIL Z Y 10 TAA YT wey o1our ye AYrrrqtonpoid jo yor Aq poyooye st osues erjoods pojjousrAun oY JO oprsjno uoneurumr Joyouered e se payroods oq ose SNU 1oquinu Jop1O oY 3er so3eorput V IOJo op 103 Toxid uru OT ut YE uorszodsrp ue ur 91 SISI uump oo ISP oq HOA ose are S1032939p MOJ oy JO Yo 10 FLI AOO pue aSuer e1joods poyoustaun q uoryeogrguopr YSusParm euu Q 19quinu I pIO 4iojo j p pie eqj JO ZIQ exid ye YYSusToAeM oy se pouyep s Sumnj s prepueys ayy 103 Py syySUSTOARM DOUSIOJOY Up AQL 15 2 Wavenumber ranges 79 80 qq 08868 6928 66929 V80 8 vetes SO9E8 Tezes T9749 ezeze 9989 VO LV Ly Y90cI 98 79768 eQ 926 9 cee8 Sevres Leses 542608 LIS 894728 qO u O Ly Ly ont Vo LL6E8 GEPS CGSVv8 Vesrs CO6V8 Caro Oq 06668 692 gesss 1 0 87 Sk TSIT qq ITG6l seers 9698 66028 G ICGS SEIS 0468 676698 SETE 6 99 u O Sy st GC LLIT gq 2 99 E0198 VICOS 81998 0 L98 Doug T6728 hus T909 TEL8 1 0 67 6 Z LSTI ve 99658 greng EGIS 99898 29698 OZ 09918 E7088 v Oe08 99828 U 0 6h Gr 6 8STI ES 9 9998 169 V6GE88 099 PPE88 T2068 27268 61848 6068 1 0 08 OS Per gq 29 STI ZZQ 999 E9188 90S CTY 68 L 0868 099 oo u 0 0G OS get TS 66668 T7968 V 468 Cep 27 06 61406 T6806 GEI6 99q69 9806 1 0 TS TS STIIT ZS 69768 O8868
58. S OSTIZ S OTIZ VOOTZ S4607 74808 TOSTE T E60 UI 4 LITE Out 237608 VV8OZ L IS0c GTLOZ 9 890 Gin gro L S7O 88803 TTSOZ 1 T 23 Je 99 0 TOT 68808 Cam 980 Z 890 eco S TSOZ rar SLEDS cS0c gr n 16 10106 8 8 TE908 ro TZGOZ TEPOZ YOVOZ rem E8ZOZ Fame v c0c ren 1 1 87 8 92707 68 908 T6VOZ Um S LEOZ eem rem zm game CEST S 8TOZ U T SG 87 T O L6 f 6r0g O 0TOZ V LO0Z S L66T Iropt Trap VIS6T L OLGF PTOZ 092461 1 T 8 8 P7007 86 96108 O0 v00c V I00c v IGGT 99861 SSL6T Coiet hoer 6 L007 6 IL6T U T 8 Z 8 V9661 G8 02661 28961 VT86T ier Cer TI96T W886T 976T E8861 FSET 1 1 63 6 0261 98 69867 v 8L6T T 9L6T 796T SPIT oer 6 Z86T BEET 629861 0 6P61 U T 6Z 6 LTLET 6 8676F LOVET amp SE 6T 98Z6T 09261 O09161 ETGT emt V HV6T O 0T6T 1 1 63 6 PET V6 Pr GPEGT EZEGT LZZET 0 0Z6T GGOGT OLOGT 679687 S 8 6T O09061 U T 6 6 Gig C8 99661 GLIGT E STGT 6 906T SPOGT 2 S68T T EG8T 6 888T 6 IZ6T v 6881 1 1 08 OF TTIGT 8 90861 GZIGT E 0T6T L TOGT 66ST rot 87881 L8T LOT6T rot U T OE 0E 0 906T 0 6 7887 09281 leist POST LITIST Uer E 6v8T Cosi POLST Y OPST 1 T 08 Of 6 898T T6 F6L8T vOLST 0 898T 9 8081 gent OVST C EPST FEET 8 EL8T L OPST U T 08 OF 98T 008 698T LGGST 9 S8T V SPST GEVST reet ZEST 38387 8 698T 98781 Vum TE S 6GV8T TS 8 8887 60981 grat C OPST C 8EST oct O LZST 08181 G YSST MES
59. S WLEN REF and possibly INS GRAT ORDER INS LAMP P2PP Wavelength calibration source determines the source used for the wavelength calibration The values allowed are THAR for the Thorium Argon lamp HALO GEN N20_CELL for the Halogen the N20 gas cell and HALOGEN CO_CELL for the Halogen the CO gas cell See Sect 18 14 3 4 Darks Darks are obtained during daytime calibration by the VLT observatory There is no need to execute dark exposures during the night The parameters required by this template are DIT NDIT and NEXPO 14 3 5 Template signatures CRIRES spec acq NGS To be specified Parameter Range Default Label SEQ NGS ISTARGET SEQ NGS ALPHA SEQ NGS DELTA SEQ NGS COLOR SEQ NGS FWHM SEQ NGS SNR SEQ NGS USELASTSKY SEQ NGS SKYALPHA SEQ NGS SKYDELTA SEQ NGS ISSVGS SEQ SV USELASTSKY TEL SKY OFFSETALPHA TEL SKY OFFSETDELTA TEL AG GUIDESTAR TEL GS1 ALPHA TEL GS1 DELTA TEL TARG OFFSETALPHA TEL TARG OFFSETDELTA INS DROT MODE INS DROT POSANG INS SLIT WID INS WLEN REF INS GRAT ORDER TF T 0 0 1 5 0 0 10 0 0 0 0 10000 0 1000 TF P 30 30 4 0 30 30 4 0 T F T TF T 120 120 30 0 120 120 30 0 NONE SETUPFILE CATALOGUE CATALOGUE 0 0 0 0 22 5 22 5 0 0 22 5 22 5 0 0 SKY ELEV NODEFAULT 0 0 360 0 0 0 0 05 3 0 0 2 958 3 5361 9 NODEFAULT 0 59 0 Target AO Guide Star RA of AO guide s
60. SC G vGSC ao L EL8Z 862 T0882 U 0 9T ot Leo GLI 29992 87186 LOL8Z LT6SZ SG68Z erter T9T6Z L ZEGZ 9ZG8 Z PIEGZ 1 1 91 OT LOVE LLL WLO8Z 8 I88Z L G88Z 6 006 T S06 T IZ6Z S Sc6c org 9T198c 6 Sv6z U T 9T OT Corp SEL SET6Z S76 v Sc c LOPEZ umme O LG6Z 80967 oe ron P0867 VIII LT L LOVE OFT 60367 MET L SEGZ T SP6Z 9 196c groer User ra ZZIGZ T 886Z U T LT LT T66EE CST FL6Z 9 LEZ cT66c Com T 600 rom F8Sc0 mme 06967 9908 1 0 LT LT EGEEE VST 93867 09667 26667 mr O 8TOE Com LEOS Com 92266 SGS0 U 0 LT T 8 988 GOL LL60 LZGOE S 980 LZLOE TLLOE 6 60 8860 779776 V SE0E 8STISG IT LT LT CCIE LOT 6 970 Coon 990E G CS0 T L80E O VOTE Conte OLSTE TSVOS 6 GcT amp U T LT LI 9 qz Tel 67808 02608 FOOTE EEITE OOITE MOTE YDETE T6PTE 2 6206 9YTSTE 1 T ST 8I L 8IZE CET Z608 LTOT amp SOTE SIZIE GPZIE SSETE O EPTE 8LGTE GL80E BESTE 4 T 8T gt 9YOTZ rr S6PIE PEINTE TLOTE TESIS 98STE G TOZGE VIOE TEZZE TLPTE C ccce 1 0 81 gt OOSTE orl 6 L8TE TELTE 09218 TTGTE VS6TE VII T9TZe gaer COGIE GTEze U O ST gt TIPTE 9 GL LIITE PETE LEZE 8S ESTE S8STE SOLE VISTE T DOEE Y LIZE 6 967 1 T 8T gt Cam SGI 29228 SUE SPE EVITE OGIE TL8TE WZGTE ISe GLEE 29088 U T 8T gt Um PUL SOGE SIZE TELTE mer S GSCE EPOSSE TOES score SEGE FETES 1T 6T or q 6F08 SZI 697 CITE GO
61. SEQ SV USELASTSKY F By default sky exposures are taken 30 in RA and DEC from the science target position In crowded fields however one has a high chance that the sky exposures is contaminated by some other source s Therefore these parameters offer freedom to specify RA and DEC offset positions These offsets are usually executed early in the procedure at the time of the acquisition of the NGS The convention for these RA DEC offsets are TEL SKY OFFSETALPHA agxy a NGS TEL SKY OFFSETDELTA sky 6 NGS 14 1 4 Telescope guide star parameters Sometimes the telescope operator may have difficulties to find an appropriate telescope guide star which is also used to set up the M1 active optics This often happens in the Orion nebula in other nebulae that appear as saturated in the Digital Sky Survey or in extended dark nebulae In these cases it is useful to provide a telescope guide star TEL AG GUIDESTAR P2PP Telescope guide star selection if set to CATALOGUE the Telescope Control System semi automatically searches for a telescope guide star If the user wishes to provide the coordinates of the telescope guide star then TEL AG GUIDESTAR should be set to SETUPFILE TEL GS1 ALPHA TEL GS1 DELTA P2PP RA DEC of telescope guide star are only relevant if TEL AG GUIDESTAR SETUPFILE These parameters correspond to the J2000 coordinates epoch of the observations of the telescope guide star Otherwise
62. SZE PPEZE 867 6ZIEE TLIEE Sess amp IOCE OZEES 4 T 6T 6T GI QE leier OGEEE TEPEE Gar TEISE L 6LEE L v8EE sore S TCEE ropp 1 0 61 er Z v86 3 SEL E EEEE 8VEE WZSEE Pees Ges L68 Lv6EE Give Teese Camp U 0 6T er 8826 STI 89666 YGIVE SLIVE OSETE G6EVE L 8SvE CTIE 8 88 rop nr 1 T 6T GI 88I6Z GPL T907 TEE SLEVE CGGPPE OTSPE TOPE O GLYE 9964 TOTHE 0 88hg U T 6T GI 96067 TT VLE 9YODDE PYE gor 979E 6218 Ewe 58676 voz ve goe 1 1 03 0 2687 GIL GEE T6PPE 6ZSve GLOVE gur OLE OTGYE anc org omg U T OZ Oc 00687 OSI 2667 SHIGE OGISE 9YSESE Ce L LGGE STIGE 67866 8 TOGE og 1 0 03 02 ees Let 88098 gro 0 6cGE Gvge v OGGE T8998 tAGE Teese IIe Cool u 0 0c 0 02787 19 Kat uug xeuly utu xeuly utu xeulg umg xeu uyaq OT O PI y wa wa z wa I 39d osuet man yybuajaann ut sabuns o4222ds aof int ajqvy 229 SPXId QE st YISU9SALM ADUIIAJOL oY Jo Suruorjrsod oy uo LIINI aq OBUVI payyou3raun OY OPISNO JVJ 20911 UL UoAIS s n eA IoquinuoAeA jI S DOSIL c Y 10 TOAST T Wey o1our ye jr rqronpoadoz Jo yor Aq poyooyye st osuel Tetjods po33ouStAun 913 Jo oprsjno uoreurum Joyourered e se poyloeds oq os e 3snur 1oquinu Jop1O oY FEY sojeorput V e 103293op 103 foxtd uio QT ut 49 uotrsrodsrp ue ur 91 SISI Otto ISP oq UDAL OSTE ore 103293op MO t JO qoeo 103 uio ut posso1dxo
63. Spectral imaging using a 31 long slit e Adaptive Optics to maximize the signal to noise ratio SNR and spatial resolution Functionally the instrument can be divided into four units 1 The fore optics unit provides field de rotation cold pupil and field stops curvature sensing adaptive optics and slit viewing 2 The prism pre disperser isolates one echelle order and minimizes the total amount of background entering the high resolution unit 3 The high resolution unit comprises the collimator the echelle which is tilt tuned for wavelength selection the camera and the science detectors 4 The calibration unit outside the cryogenic environment contains the light sources for wavelength calibration and detector flat fielding 1 1 Science drivers Thanks to CRIRES new phenomena and objects are now available for spectroscopic studies Some highlights are e Extra solar planets CRIRES User Manual VLT MAN ESO 14500 3486 2 1 2 radial velocities spectroscopy of CO CH Solar system Giant planets Titan Hi CH4 CH3 NH3 HCN Terrestrial planets CO HCL HDO H20 Mars imaging spectroscopy of CO depletion at 40km resolution Jo volcanic activity SO Pluto Charon Triton CO CH search Comets H20 abundance temperatures velocities Stars stellar evolution and nucleosynthesis CNO abundance stellar mass stellar radii stellar winds and mass loss atmosp
64. T U T TE TE 9PP8T L8 0291 V STST TSTST TPOST L TOST Z6LT geit 6 6LLT 99191 07821 U T T TE 98081 8 8 48787 OOT8T 920981 986 1 T 96 T 99891 6 8 1 JI TEIST VISI U T TE TE T EOST LL 89081 LLOLT 2 q621 8 48LT 988 1 TLALI SPLLT Soir OTOST 914241 1 1 28 ZE LTOLT 82 9009 Eet 60621 638 1 LOSAT E ZLLT 8691 T I9LT 8 9641 29941 U t ze 69811 XQ ED ume dan d ume BURY ume NY ume SN ume qI O Ply y wa wa z wa I wa oe man daqunuannn ut SIDUDA qo4g22ds LOS YG DG AQDI 299 s oxid OE e SI YISU9SALM ADUSISJOI oY JO SUTUOIYSOA oy uo K enooe Y Y WU ul passaidza wnnava 240 syzbuajaan AA 9BULI P9IJ9USTAUN OY PISANO 8 911891 Ul uoAIS son peA YYSUSPOARM PMS 29821 c Y 10 TAA YT wey o1our ye jrpiqronpoadozr jo yoe Aq poyoye st oguel erjoods pojjousrAun oY JO oprsjno uoneurumr Joyowered e se payroods oq ose SNU 1oquinu Jop1O oY 3er so3eorput V 1032093op 103 Toxid uru QT ut YE Worssodstp ue ur a SISI uump oo ISP oq OAI OSTE 91e S1032939p MOJ oy JO Yo 10 FLI AOD pue oguei e1joods poyoustaun qJ uoryeogrguopr YYSusPaem eui jur Q Joquinu I pIO 10399I9P pie eqj JO ZIQ exid ye u39uo oA A oy se pouyep s3uryjos prepueys ayy 10 Py sYYSUSTOARM DOUSIOJOY PP qe 75 OFT FLELE L E8LZ 66222 S89LZ SIOZ YOPLZ ZZ LISLE 0 E6L3 8 EELZ 1 1 03 0 LSA CTI 688 8 OGLZ STILLS YIGST YTLE SLELE EELS GLILE U
65. T 9 9E LEST O L 14169 VLZ9 VISTO 6609 S LTE9 9 LPE9 IGEI T 8889 6 COCO 7999 U T 9 oe reegt SL 0969 T689 E S0V9 SLEVY COVVO 9 6LV9 ong 6 Y369 9 88E9 96790 1 T 9 8 oe SLAST 9L L869 V9lV9 LVI ierg Z99P9 00S9 OTSA soten 8 LOV9 S 9IS9 U T 9E 9E groot 29 90 TED9 L 8EP9 T L9V9 O GLP9 S0S9 Z VTS9 679799 omg ron 1 1 18 LE erger 8 9 07819 8VV9 S SSV9 T S8V9 TEGVI O vcGO O EES9 6999 TLEV9 V cvco U T LE LE GGVGI 4 E489 TSLS9 889 6 ST99 T SZ99 0 0999 8 6999 90L9 ronn G9L99 1 T LE LE TSTST VL 06999 TVES9 87099 T 9E99 v SY99 S O899 870699 349 6 9889 0 L699 U T LE LE LOTST 9 97499 09099 6199 6199 E 0S99 F899 0699 reg L699 70029 1 T 8E 8 68081 99 17659 TZZ99 00899 00999 0 8999 26699 6029 9 87 L9 TII99 Z9U9 wu T S amp 8 6 POST TL 608L9 22919 1929 60649 9099 6 6 99 0889 6 899 GrPLO v9889 T 8 8E Coirt GL FOLI Sc19 G18 9 ST89 0Gc89 T I989 61489 676069 oun 92289 U T 8 88 60171 Q xeuly utum xeu uug Kat uyaq xvur utu xeuly utu OT O PI y o wa c wa I wa om m in yybuajaann ut sabuns josjaads aof int ajqvy 2929 SPXId QE st ISU9SALM oSu 9J91 o Jo Suruoryisod oy uo Koenooe aq a3uel payyou3raun oY OPISNO Te 20911 UL UOATS s n eA IoquinuoAeA jI S DOSIL c Y 10 POAT T Wey o1our ye AyIqionpoldad Jo yoe Aq poyooye st oSuer Tetj
66. T WID INS WLEN REF INS GRAT ORDER TF T 120 120 30 0 120 120 30 0 NONE SETUPFILE CATALOGUE CATALOGUE 0 0 0 0 40 40 0 0 40 40 0 0 SKY ELEV NODEFAULT 0 0 360 0 0 0 0 05 3 0 0 2 958 3 5361 9 NODEFAULT 0 59 0 Use the last sky measurement for the SV RA offset to sky DEC offset to sky Telescope guide star selection RA of telescope guide star DEC of telescope guide star RA offset between target and SV guidestar DEC offset between target and SV guidestar Derotator Mode Position angle Entrance slit width Reference wavelength Grating order TEL TARG ALPHA TEL TARG DELTA TEL TARG EQUINOX TEL TARG EPOCH NODEFAULT NODEFAULT 2000 3000 2000 2000 3000 2000 Right Ascension Declination Equinox Epoch TEL TARG PMA 10 10 0 Proper Motion RA TEL TARG PMD 10 10 0 Proper Motion DEC TEL TARG ADDVELALPHA 15 15 0 0 Diff RA TEL TARG ADDVELDELTA 15 15 0 0 Diff DEC Fixed values Parameter Value Label DPR CATG ACQUISITION Data product category DPR TECH IMAGE Data product technique DPR TYPE OBJECT Data product type 66 CRIRES_spec obs_AutoNodOnSlit To be specified Parameter Range Default Label DET1 DIT 0 900 VODEFAULT DIT DET1 NDIT 1 1000 1 NDIT SEQ NEXPO 1 100 1 Number of exposures per nodding po SEQ NABCYCLES 0 100 1 Nube of nodding cycles SEQ NODTHROW 0 22
67. V values USD will flag OBs requiring low PWV so that the night time astronomers observe them in appropriate conditions ESO considers the possibility to add a constraint on the water vapor in the P2PP constraint set for future periods For more detailed information see the online help provided on the ETC page 10 3 Overheads Estimated overheads are listed in Table 3 Actual values for the change of wavelength setting itself vary considerably between 46 to 105 s depending on the orientation of the prism and or grating before the requested change However to the average value of 65 s for the wavelength setting change additional overheads are added in order to insure that the intermediate slit does not vignette the spectrum cf 8 4 44 Table 3 Telescope and instrument overheads The overhead for change of derotator position angle applies to the CRIRES_spec_obs_SpectroAstrometry template Action Time s Telescope Preset 360 CRIRES Acquisition without AO 180 CRIRES Acquisition with AO 300 CRIRES Read out DIT in s 2 3 0 9 NDIT 0 1 NDIT DIT CRIRES Nodding cycle 24 CRIRES Change of wavelength setting 210 CRIRES Attached wavelength calibration 150 CRIRES Attached lamp flat 120 CRIRES Change of derotator position angle 60 45 11 Preparation of Observation Blocks This sections provides some guidelines on how to prepare CRIRES observation blocks A CRIRES Tutorial with a more detailed description has been p
68. Y se paugop SSUT JoS qj3uo pAe prepuejs ayy 103 WU ur y su3Suo pA A oouoI9JoW qG ALL 82 G8 6999 0 9898 TEGAS GIZLG E67L8 vV6GLS 0 9929 G 66LG Con 09448 VT C amp ZE Zelt 98 4999 6029 VOTZS Z 6EL8 TAPAS LLLS vOSAG Tase TEGIS l v64G U T ZE ZE Soit GL ETILE TILE STVLS 89LS og OSG COTSG T 6888 Y YCLG LOTS W T Ee E8 VLELT 9L OLELE VIGLG 09929 OPSLG TT6LG LISS C OCSG G GG8F 6 6EL8 og U T EE EE ELT C8 9899 TV988 9 1 88 10069 8806S L686 S 8V6S 07869 GHS8S gong rie e 6 869T 8 8999 T888 68888 98TGS 04268 vV8S6S E L96S 20009 TL8S 8PL6S U T EE EE 8 E69T GL 19889 86069 9168 S ZP6S E 0S6S 0 8L6S 7986S Tomm 0 8688 9668 ur PE V9891 VL 0068 op 9668 6969 6996S 7466S S009 zong PTGS Z ETO9 U T PE PE got 008 Z ET09 9YTVO9 2609 F6L09 91809 96119 98219 276979 TZEOD Com 1 T pe PE 0 6p9T U8 90809 46509 92909 62609 S 90T9 gem C SPIO 0 8879 L OSO9 vS8TO U T pe ve rot TL 78909 8 809 6 0609 2 LIT9 Z 9319 8 ESTO C COTO 8619 im eum Vue GE Coen ZL 6EL09 6609 69019 YETI tor E TLTO L 6LT9 70I189 8809 omg U T SE GE great LL 70619 6IZ9 VLZZI 98879 22929 96679 6089 976769 V OICO 9TE9 1 T 8 GE gt SL 18069 6 LEZ9 T9VZ9 Lal 19829 S 6TED T 6ZE9 871969 0 63Z9 6 SEE9 U T GE GE O02691 69 TEG9 VLS79 6929 G c6c9 VOOED 6 6zE9 ESEGI 6989 L Gvco V SvEo 1
69. Y 6 v3LG U T 0Z 0 Graz TIL F6LLE TROLS SGOT SEGLT YOSLE 08 c TGELZ GLE V9 Bele VI IG T6 Geo ETI FELLE VIDS VSGLZ SOPLS 9 VIELE 62222 TSILE GILL L 8TLZ U T TG TE rot ETI L TGL amp MGOLZ E9OLZ LE69Z T0697 0 LL9 TEL9Z 6992 S8TLZ T9997 1 0 13 TG 00027 STI amp TILG TZOLT 8 869 09897 SZ89 og E9997 Creos Tout rie U 0 TG TG rr VEL 107998 O01992 rn LEI 6 6coc YSTI TTI L969 seg orl 1 T TG 1 Gord GEL 69998 engen Z ST9Z v Ic9c O L09Z 8 ZO9 67892 t amp OG9c 09683 U T T1G TG TZEN LOL 68898 STPIZ Ion S Scoc L ST9Z T VTIZ 6 OT9G 68646 VISA 63097 Vue ZZ CTE SOL 69 98 og TEEIZ TZZ9Z 0 6T9c rimm O VO9 7698 SHIT 19692 U T ZG ZE 9279 SIL 08698 S 988 SESSE ETLGZ 6 L98 8887 tee 98898 CvOGG VV 1 0 77 TE CLLEGE GIL 60698 6L8 T9LGZ 6 98 GO9GZ gieler gue 69887 Yugo U O cc cc og SZI 88 68 Cer ege SETSZ TOTSZ G 96vc WE6VE 99178 O LEGZ LOVE 1 1 3 Ee Co GCI PEGE GS OGIST GOSZ TZOST v SSvc VISTZ BOLTS 0 678 LLP U T 7e Ze WISE SOL froe Gomez aert 01877 oer rr OLS cS0Gc CcOvc 1 1 83 erer GOL 67098 V6VT VIGHZ TOSTE TLLPZ G G9vc TZ9VE G6r7e tose LGGvc U T EG S e8vC SIL 985 86 Cie GTEPZ 9922 OITZ Helps E66ss egre 89077 1 1 83 EE GLEE GIL cre a CGE L O amp vc GHZ SIPS S 8OVE S VOVE 97658 LOW v 66gc U T 23 EE gr EOT 89078 LOGE mr PVEEZ TOSET v69EZ 998
70. adequate for bright AO stars R lt 10 For fainter targets it should be set to F In this case the following parameters SEQ NGS SKYALPHA and SEQ NGS SKYDELTA should be determined with care if observations take place in crowded fields SEQ NGS SKYALPHA and SEQ NGS SKYDELTA P2PP WFS Alpha Delta sky offset arcsec gives the offsets of the location relative to the NGS where MACAO measures the sky If SEQ NGS SKYALPHA gt 0 the sky is measured to the East of the NGS If SEQ NGS SKYDELTA gt 0 the sky is measured to the North of the NGS Default values are usually fine except in crowded fields 58 SEQ NGS ISSVGS P2PP SV Guide Star AO Guide Star is a flag If set to T de fault the natural guide star NGS used for the adaptive optics is also the slit viewer guide star SVGS If this flag is F then the user needs to provide the offsets TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA However see also the note 3 below 14 1 7 for a special case 14 1 3 Parameters related to the slit viewer SEQ SV USELASTSKY P2PP Use the last sky measurement for the SV Generally one can use the last sky measurement and therefore leaves SEQ SV USELASTSKY T untouched from its default value However if one observes a faint target a new sky should be obtained for the slit viewer In this case set SEQ SV USELASTSKY F TEL SKY OFFSETALPHA TEL SKY OFFSETDELTA P2PP RA DEC offset to sky are only relevant if
71. amp GIOI S VEOT L OZOT 1 0 88 GG 6 0 0T gr Foot 8 TEOT SOOT VAZOT T PZOT O 6TOT 970 amp GIOI S TEOT SLTOT u O GG qq sent LY Ament T9TOT G DIOT TOTOT 8 800T SLOOT 7 00T TL66 9101 9YZ00T 1 0 98 99 S ZTOT LY OLIOT ETOT OCIOT GLOOT SOOT 8 0001 amp 666 1766 ETOT 2666 u 0 90G 99 96001 9P 62001 V866 C406 F266 T7166 F986 796 L6LE v 866 Cap 1 0 29 18 8766 YD 00001 9966 v66 C686 C886 86 9796 99L6 S666 ccs6 u 029 29 6T66 GV 86 Ip 666 826 0716 3696 8796 Nep TT86 2896 1 0 88 82 926 97 8086 Tag TL46 6 Up 996 6796 8696 c816 96 U 0 8E 82 8726 VP 8 896 G796 06 L866 9786 L296 7196 7976 796 8TS6 1 0 68 6 top Sy 6996 8196 9096 0996 rop 6676 996 98676 9196 org u 0 6G 69 896 Xe SEE ume das d ume ER umy KEHIN umiy BURY ume CT O PIV y aeg g wa c gd I jot oguei USUN SIQUNUIADN ut sabuna qo4g22ds Lof YG DG IQD 299 s oxid Qe e SI q3Suo oAeA oouoioJo1 oY Jo Suruomrsod oy uo Koenooe Y Y wu ul passaidza wnnava 240 sujbuo oanAM I9BULI po JOUSTAUN OY oprs3no 8 911891 Ul uoAIS son peA qu33uo oA M PMS ISIL Z Y 10 TAA YT wey o1our ye Ajrpiqronpoadozr jo yoe Aq popope st osues erjoods pojjousrAun oY Jo oprsjno uorjeurumg I 1o03ourered e se pogroods oq ose SNU 1oquinu Jop1O oY 3er so3eorput V 103293op 103 Toxid uru OT ut YE uorszodsrp pat o SISH uump oo 3se oq HOA OSTE are S
72. are saturated and do not scale linearly with airmass Therefore it is necessary to observe a telluric standard as close as possible in airmass and with the same instrument setup as that used for the science target Furthermore the strength of some telluric lines varies with time so it is also necessary to observe the standard soon after or soon before the science target Thereafter the spectrum of the science target is directly divided by the one of the telluric standard Ideally the spectrum of the telluric standard should be known so that features belonging to it can be removed step 2 above However this is usually not the case so one has to use standards in which the spectrum is approximately known At present no high precision IR atlas of standard stars with bona fide spectra exists The CRIRES Team will compile such a list of spectro photometric standard stars and once it is available will put it on the CRIRES home page http www eso org instruments crires 9 3 3 Hot stars as telluric standards Usually either hot stars or solar analogs should be used as telluric standards Spectra of stars hotter than B4 are well fitted by a black body with the exception of a few lines for example neutral hydrogen Brackett lines So by knowing its spectral type the continuum of a star 41 can be fitted by a Planck function with the appropriate temperature On the other hand the spectra of stars cooler than A0 show molecular features So
73. at http www eso org sci observing phase2 P2PP P2PPTool html Information for the preparation of Service mode observations with CRIRES are available at http www eso org sci observing phase2 SMGuidelines html CRIRES Visiting astronomers do not need to submit Observation Blocks in advance of their observa tions However they should prepare them before arriving at the observatory or at the latest at the observatory the nights before their observing run They will find further instructions on the Paranal Science Operations web page and the Paranal Observatory home page http www eso org paranal http www eso org paranal sciops Reference frames static calibration frames information regarding the CRIRES pipeline and quality control can be found at http www eso org observing dfo quality http www eso org observing dfo quality index_crires html 1 4 Contact Information In case of specific questions related to Service Mode observations and proposal preparation please contact the ESO User Support Department usd help eso org For Visitor Mode observations please contact the Paranal Science Operations Team For general information use paranal eso org For specific questions regarding the use of CRIRES use crires eso org 1 5 News Since the release of User Manual v83 1 The announced major change to the instrument control and observing software was successfully implemented in November 2008 although still incom
74. both parameters should be kept to default 0 14 1 5 Derotator parameters INS DROT MODE P2PP label Derotator Mode determines the derotator mode SKY or ELEV In ELEV mode the slit is constantly aligned with the parallactic angle in order to reduce slit loss introduced by differential refraction This is particularly important if slit viewer 59 guiding has to be made in one band e g in K and the observations in another one e g M However in ELEV mode guiding with a SVGS different from target is not implemented The use of the CRIRES_spec_obs_SpectroAstrometry and CRIRES_spec_obs_GenericOffset templates is only possible if the derotator mode is set to SKY INS DROT POSANG P2PP label Position angle determines the position angle PA of the slit if INS DROT MODE SKY The values must be set such that INS DROT POSANG PA 14 1 6 Spectrograph parameters INS SLIT WID P2PP Entrance slit width determines the slit width in Recommended value is 0 2 0 4 with AO Without AO the optimal S N is obtained with a slit width equal to the seeing however a value larger than 0 4 is not recommended as a large fraction of the spectral range can be affected by vignetting or lack of reproducibility see 8 4 A value of 0 2 gives the highest resolution INS WLEN REF P2PP Reference wavelength is the reference wavelength This wave length corresponds to pixel 512 of detector 3 Tables 4a to 4f provide the reference wave
75. ce window transmission updated sensitivities 10 updated overheads 11 added 3 recommended DIT values updated text 12 updated 80 2 12 03 07 0 8 1 10 3 corrected typos 1 2 14 2 added paragraph on gas cell and generic offsets template 80 3 20 03 07 15 corrected J band wavelength ranges 80 4 26 03 07 15 corrected missing entries in Table 4 80 5 07 05 07 1 corrected description 21 05 07 14 2 new observation template 05 06 07 7 2 added link to N2O line list 1st results on RV accuracy 09 06 07 0 1 7 4 corrected slit length and slit viewer f o v 09 06 07 14 1 1 corrected typo in RA offset 09 06 07 12 daytime wavecal only for lt 2400 nm 19 06 07 1 4 6 4 contact information odd even 19 06 07 8 4 add important note on intermediate slit 20 06 07 17 18 new section 17 update 18 20 06 07 11 1 14 1 added comments on ext objects moving targets 20 06 07 9 3 added comments on std stars 20 06 07 14 2 added gas cell P2PP parameter description 81 1 31 08 07 8 4 updated 31 08 07 8 2 Added Fig 21 comparison UVES vs CRIRES 31 08 07 10 3 Table 3 overheads updated 31 08 07 15 Slightly changed captions 01 09 07 6 4 Added links to method and reference frames 01 09 07 9 1 Added link to ETC 01 09 07 11 2 1 Added para choice of a SVGS in crowded field 01 09 07 8 2 Added para on slit loss due to diff refraction 01 09 07 11 4 Added requirement for fe 02 09 07 5 7 5 Figures added AO performance resolving pow
76. ch that the targets stay in the slit area at all nodding jittering positions This is especially important when an extended object or multiple targets are in the slit Telluric standards should be chosen close in right ascension and airmass to the target To avoid any confusion in the assignment of a telluric to a science target it is recommended to name the telluric OB according to the science OB i e CAL_ lt science OB name gt Finding charts should be created from infrared images e g 2MASS and should clearly indicate the location of the target AO star and SVGS The necessary information on the target AO and SV stars should be given in the Instrument Comments field of each OB More detailed information on Phase 2 requirements can be found in 811 and at http www eso org sci observing phase2 P2PP P2PPTool html
77. corresponding to a resolution of 94 300 This value is therefore a lower limit to the spectral resolving power of CRIRES CO v 1 0 4 7 um FWHM 3 18 km s Optical depth GC r ETT AAA AAA dba aca a a a a aca PARA 20 10 0 10 20 L km s Figure 18 Optical depth profile obtained from the combination of 5 CO lines seen in ab sorption toward the young star DG CrA Courtesy Klaus Pontoppidan A slit width narrower than 0 2 is possible in particular in the case of observations of very bright targets However there is no guarantee that the requrested slit width can be achieved for slit narrower than 0 2 due to the limitations of the slit mechanism Also there is no guarantee that the spectral resolution can be larger than 100 000 33 8 System efficiency and throughput The overall efficiency of CRIRES has been measured on spectrophotometric standard stars The flux F of such a star expressed in Jy is converted to the flux N in photons s pixel by C Aral N E y E e AA 3 7 where E hc A is the photon energy Ara the telescope collecting area The dispersion AA is output by the ETC Efficiency of CRIRES versus slit width Efficiency of CRIRES meosured with HIP102497 0 20 0 20 0 15 a Efficiency o 3 Efficiency e photon 3 0 05 0 05 gt 2 15 2 16 2 17 2 18 1 Wavelength micron Slit width oresec Figure 19 Overall system efficiency also called th
78. ctly determines the quality of the formed image One of the main parameters characterizing this image quality is the Strehl ratio SR which corresponds to the amount of light contained in the diffraction limited core relative to the total flux Observed object Plane wavetront Sei Atmospheric turbulence mo Corrugated wavefront Y Uncorrected image Deformable mirror Tip tilt mirror X Real Time Computer Wavefront sensor Y AO corrected mage Beam splitter Corrected wavefront e y Camera high resolution image Figure 4 Principle of Adaptive Optics Note that in practice and contrary to this schematic design CRIRES has no dedicated Tip Tilt mirror but performs low and high order correc tions with a single deformable mirror mounted on a tip tilt stage see Figures 5 6 An AO system is a servo loop system working in closed loop The DM flattens the incoming WE and the WFS measures the residual WF error A commonly used WFS is the Shack Hartmann WFS used for example in NACO However CRIRES as well as the other ESO MACAO systems relies on a curvature WFS it is designed to measure the WF curvature as opposed to the WF slope This is achieved by comparing the irradiance distributions of two planes placed behind and in front of the focal plane In practice a variable curvature mirror membrane is placed in the telescope focus By vibrating inside 11 a
79. d spectral dispersion Since the release of User Manual v82 1 e version 1 7 0 of the CRIRES pipeline is available http www eso org projects dfs dfs shared web vlt vlt instrument pipelines html e a CO gas cell is available e an intervention took place in April 2008 it consisted in 1 replacing the carriage by a faster translation table 2 moving the ThAr lamp mounted on the carriage to a location close to the baffle where it feeds a set of fibers through a neutral density filter The end of these fibers are fixed on a connector located on the carriage In this way a lot of scattered light is eliminated and spectrograph distortion can be estimated for each ThAr spectrum 3 installation of an AO fiber for AO calibrations until then performed using a pin hole 4 an encoder has been installed to control the intermediate slit therefore increasing its reproducibility 5 the location of sensors and the values of control loop parameters have been modified to increase the thermal stability of the instrument a reproducibility of less than 2 pixels has been achieved once the instrument is stable in temperature e unfortunately a detaching Sheldal tape initially used to decrease possible scattered light started to vignette the entrance slit limiting the field first to 12 then 8 after a VLTI run during which the cryo coolers were switched off to limit the amount of vibrations felt by the VLTI As a consequence a new interventi
80. e array 133 542 mm 4946 pixel gap of 7 15 mm 0 5 mm for mounting adds up to 7 65 mm 283 pixel 1024 pixel 27 um 27 648 mm 0 5 mm for mounting me IMEEM ALADDIN III ALADDIN II Assy 411731 ALIRD04 low dark current 4x10 e s ALADDIN III ALADDIN III Slit Assy 411730 Assy 415477 Figure 2 Layout of the mosaic of four Aladdin science detectors numbered Z 1 to 4 from left to right The detectors are not science grade arrays and show bad cosmetics Only the half bottom part of each detector is used as indicated by the thick black rectangle The mosaic used for science observations therefore consists of 4 x 1024 x 512 pixels 2 3 Detectors The spectrograph focal plane provides a useful optical field of 135 x 21mm which is well covered by a 4x1 mosaic of four Raytheon 1024x1024 pixel InSb Aladdin III detectors with a pixel size of 27m The spacing between 2 successive detectors corresponds to approximately 280 pixels and is slightly different from one gap to the other Fig 2 shows their relative orientation In particular it should be noted that only the bottom half of the mosaic is used and that the reading out is executed parallel to the mosaic for detectors 2 and 3 and perpendicular to it for detectors 1 and 4 A fifth Aladdin III detector is used in the slit viewer The arrays are read out using standard ESO IRACE contro
81. ec trograph Lab results are confirmed by on sky measurements and demonstrate some gain in J more than to 40 for an optical seeing of 0 6 and a strong factor 2 increase of the frac tion of the energy available for the spectrometer in the K and M band respectively Fig 10 J band 0 2 slitwidth K band 0 2 slitwidth T T T T I 1 T T T T I x V 10 guide star V 10 guide star nor WEI E E 0 9 V 13 V 16 0 9 ost L ouo e in E i T i 1 i L i fraction of energy available for the spectrograph m 0 1 L 1 L L L L L 4 1 1 0 2 0 3 0 4 0 5 0 6 0 7 0 8 0 9 1 1 1 12 02 0 3 04 0 5 0 6 0 7 0 8 0 9 1 1 1 1 2 seeing seeing Figure 10 The fraction of energy available for the spectrograph in a 0 2 slit as a function of optical seeing is shown for the J left and K right band for AO stars of V 10 12 16 mag and without AO correction For reference please consult the Exposure Time Calculator ETC Fig 11 illustrates the increased throughput made possible thanks to the use of the adaptive optics The graphs shows the spatial profile summed over a few columns at 2170nm of the spectrum of a mpre 5 3 in open and closed loop The DIMM seeing was 0 67 and 0 72 respectively and the coherence time was 3 ms In both cases the exposure time was 2 min The gain in integrated flux is 1 63 In other words the same flux level is reached in clos
82. ed loop in 61 of the time needed in open loop 5 1 AO guide stars CRIRES wavefront sensing is done in the R band The performance of the adaptive optics system depends on the distance to the science target and on the brightness of the selected guide star 18 10 Comparison qpentogp closed loop 40 45 50 55 En 65 70 75 80 pixel 0 1 arcsecipixel Figure 11 Improved throughput thanks to the use of the MACAO Flux measured along the slit measured in open loop blue solid line and in closed loop black dashed line in the K band 5 1 1 The distance of the AO star Although the field selector allows the selection of the AO star within 30 from the nominal position of the science target the AO star should be as close as possible to the scientific target usually closer than 10 ideally it is the science target itself Depending on the atmospheric conditions in particular on the isoplanatic angle 09 mild improvement on the amount of encircled energy can still be obtained if a bright R lt 11 AO star is used 20 30 from the scientific target It is important to recall that the isoplanatic angle decreases with zenith distance z as 0o sec z 5 and increases with wavelength as 04 c A9 5 On the other hand the Strehl ratio decreases with the angular distance to the AO star d as SR exp 0 09 5 1 2 The brightness of the AO star The intra and extra focal pupil of the AO star is imaged on a
83. ed with the same DITs as the science telluric or spectro photometric standard star observations as well as for any flat fields or wavelength calibrations Note that the frequency may change to weekly if darks are found to be stable enough e daily flat fields obtained with the same wavelength setting as the science and telluric or spectro photometric standard star observations e daily wavelength calibration obtained with the same wavelength setting as the science and telluric or spectro photometric standard star observations for reference wavelengths shorter than 2400 nm Currently the reproducibility of the wavelength setting between night time observations and day time calibrations is 3 pixels e daily bad pixel maps derived from darks and flat fields Note that the frequency may change to weekly or monthly these quantities are found to be stable enough e approximately monthly linearity e yearly or after instrument warm up distortion map and photon transfer function e typically once per night CRIRES is used radial velocity standard Flats and wavelength calibration are only obtained with a slit width of 0 2 and DIT gt 2 s 54 13 Data format and reduction 13 1 Format The SV image and the spectra recorded on the four science detectors are saved in extended FITS files Each of the 4 extensions for the science images have format of 1024 x 512 pixels see Fig 2 13 2 Pipeline A first version of the CRIRES pipe
84. eing limited observations no adaptive optics For NoAO observations only the seeing at the wavelength of observations is relevant The user should therefore specify the FWHM for the respective bands of the science observations The constraints set and definitions are the same as for all other seeing limited VLT instruments The input field for the Strehl ratio should remain unchanged i e N A The classification of each observation will be based either a on the measured spatial profile of the spectrum if the object is a point source or b on FWHM of a star seen on the Slit Viewer if there are more stars available or c on the seeing measured on the guide probe otherwise using the Roddier formula to convert it to the seeing at the observed wavelength 11 5 4 Transparency Thin clouds THN usually do not hamper CRIRES observations for bright objects Clear CLR conditions are justified for observations requiring stable Strehl ratios for example to study the close environment of the target as clouds could otherwise adversely affect the adaptive optics For the same reason CLR conditions should be requested for AO observations using AO stars fainter than R 14 11 5 5 Airmass In addition to the influence of airmass on the quality of the adaptive optics correction men tioned above observations in SKY mode can be strongly affected by differential refraction 52 effects Some guide lines are given in 88 2 11 6 Water vapor Obs
85. emplate parameter O min max ref ref 34 1644 0 1686 4 33 1693 8 1737 4 32 1746 8 1791 7 31 1803 1 1849 5 30 1863 3 1911 1 29 1927 5 1977 0 28 1996 4 2047 6 27 2070 4 2123 4 26 2150 0 2205 0 25 2236 1 2293 2 24 2329 3 2388 7 23 2430 6 2492 5 22 2512 4 2634 2 21 2632 1 2759 5 20 2763 9 2897 3 19 2909 6 3049 5 18 3071 5 3218 7 17 3252 6 3407 7 16 3456 3 3620 2 15 3646 3 3901 4 14 3908 0 4178 9 13 4210 3 4498 7 12 4563 6 4871 1 11 4929 6 5362 1 90 17 Reference wavelengths common to different orders Table 7 Ranges of reference wavelengths that are common to 2 successive orders for wave length in these ranges inclusive it is mandatory to specify the grating order as a template parameter This is valid for both standard and free wavelength settings Common ranges Orders min Amax 1330 8 1333 5 42 43 1363 2 1365 3 41 42 1397 3 1398 5 40 41 1433 2 1433 5 39 40 2632 1 2634 2 21 22 91 18 Calibration source for wavelength calibration The table given below lists the recommended calibration source required by the wavelength calibration template attached immediately before or after a science template Such a template is required if a wavelength calibration more accurate than 3 pixels is needed otherwise the internal model of the instrument is sufficient If the entry is sky emission lines or sky absorption lines then neither the ThAr lamp nor the Halogen N20 o
86. ence and standard star OBs must start with an acquisition template Two acquisition templates are available e CRIRES_spec_acq_NGS e CRIRES spec acq NoAO CRIRES_spec_acq NGS acquires the AO star with MACAO which allows the user to make the following science or standard star observations with the adaptive optics system On the other hand observations following the CRIRES_spec_acq_NoAO acquisition template will not be done with the adaptive optics system The acquisition templates contain the parameters required for the pointing and tracking of the telescope centering of the target in the slit setting of the derotator mode which includes the orientation of the slit on the sky CRIRES_spec_acq_NGS also includes parameters used to acquire the natural guide star NGS and close the loop of the Adaptive Optics system Note that currently the observing template CRIRES_spec_obs_SpectroAstrometry can only be used if the acquisition template is CRIRES_spec_acq_NGS with the additional restriction that the target is the SVGS 14 1 1 Target and SVGS parameters TEL TARG ALPHA TEL TARG DELTA TEL TARG EQUINOX P2PP RA DEC Equinox are the coordinates of the science target and the equinox for which these coordinates correspond to In case of multiple objects in the slit or of extended objects these coordinates correspond to the telescope pointing during the observations TEL TARG PMA TEL TARG PMD P2PP Proper Motion Alpha Delta are proper mot
87. ended This avoids slit losses due to atmospheric refraction In the choice of wavelength settings the interesting science features should avoid the vignetted and detector glow areas the latter point is particularly critical for DITs longer than 60s The wavelength coverage of the chosen wavelength settings can be compared with the output spectra of the CRIRES ETC The position of the science features can be compared with Fig 13 and the unvignetted range in Tables 4a 4h or 5a 5h If the interesting spectral features are affected by detector glow or vignetting in a standard setting a free wavelength setting may be chosen to optimize their location on the detectors See also 7 1 The selection of the DIT value does not only depend on the brightness of the target but also on the brightness of the infrared sky The longer the wavelength the brighter the sky the shorter the DIT to avoid saturation of the sky This should be carefully checked with the help of the ETC In case the target is not the SV guide star or the pointing position is located between two or more targets in the slit special care has to be taken to correctly define the offsets See 14 1 1 for definitions and conventions It is worth noting that the default telescope pointing is not centered on the 31 slit see Fig 17 The distance to the North and South edge are 12 and 19 respectively Therefore the nodding throw and jitter width should be chosen carefully su
88. er 02 09 07 11 5 Add a para on airmass CRIRES User Manual VLT MAN ESO 14500 3486 v 81 2 82 1 82 2 83 1 83 2 19 11 07 20 11 07 21 11 07 21 11 07 22 11 07 18 12 07 18 12 07 27 12 07 27 12 07 27 12 07 27 12 07 27 12 07 27 12 07 28 12 07 20 01 08 20 01 08 03 03 08 03 03 08 03 03 08 03 03 08 03 03 08 03 03 08 19 06 08 19 06 08 19 06 08 23 06 08 23 06 08 23 06 08 23 06 08 25 06 08 25 06 08 25 06 08 25 06 08 29 08 08 29 08 08 29 08 08 29 08 08 29 08 08 19 12 08 19 12 08 19 12 08 19 12 08 19 12 08 19 12 08 11 24 14 2 142 5 14 1 2 15 10 1 14 2 4 Table 1 Ta Tables 4a 5h 87 5 8 4 9 1 9 2 1 59 2 3 10 2 11 1 1 2 1 SILZA 101481 141 5 SILAS 5 1 SO 52 55 1 2 YA 819 87 1 88 4 811 7 811 6 814 1 6 818 810 2 Table 3 89 1 Fig 24 87 2 514 2 1455 1 5 SL 1125 812 814 1 6 87 1 811 4 Tab 8a 81 5 819 1 SEA 87 4 S7 2 2 87 5 86 5 14 1 2 88 2 813 11 19 2 Added SpectroAstrometry template Change default value of SEQ NGS USELASTSKY to T New section NEWS Added specific comments for SM telluric OBs Expanded description of generic offsets template Dark current values corrected Changed comment regarding gas cells Wavelength settings updated typos corrected typos corrected typos corrected clarified updated AO star bright mag limit updated updated available gas cells added section updated
89. ervations in the NIR can be severely affected by the presence of water vapor in the atmo sphere large amount of water vapor can significantly decrease the sky transmission and in particular in the L and M bands increase the sky emission background The ETC offers the possibility to select sky spectra calculated with a set of representative amounts of water vapor in the atmosphere Service mode users with the help of USD can then indicate in the README file which observations can be adversely affected by large amount of water vapor ESO considers the possibility to add a constraint on the water vapor in the P2PP constraint set for future periods 11 7 Offset conventions and definitions CRIRES follows the standard astronomical offset conventions and definitions Position angles PAs are measured from 0 to 360 degrees North corresponds to a PA of 0 degree East to a PA of 90 degrees All offsets are given in arc seconds Proper motions must be given in per year For solar system objects additional tracking velocities are given in arcsec per second For a position angle of 0 in SKY mode the reconstructed slit viewer image shows North up and East left 53 Part IV Reference material 12 CRIRES calibration plan The calibration plan defines the default calibrations obtained and archived for the user by the Paranal Science Operations The CRIRES science calibration plan includes the following measurements e daily darks obtain
90. ested as this manual is being released it has largely improved This element is not shown in Figure 1 It is located between the collimator the concave mirror located after the prism and the small flat mirror located before the TMA 37 Part III Observing with CRIRES at the VLT 9 Introduction 9 1 Atmospheric transmission The transmission of the Earth s atmosphere in the J H K L and M bands is shown in Fig 23 The amount of telluric absorption varies non linearly with zenith distance and precipitable water vapor In order to facilitate the identification of sky regions affected by water vapor absorption lines Fig 24 shows the atmospheric transmission spectrum only including water vapor absorption lines The transmission spectrum of the sky for a particular setting is an optional output provided by the ETC This tool allows one to select spectra based on different amount of precipitable water vapor 9 2 Background removal 9 2 1 Sky emission spectrum The sky background emission can be divided in two regimes depending on the wavelength Below 2200 nm the sky emission is dominated by OH lines formed at an altitude of 80 km Detailed sky spectra with OH line identifications are available on http www eso org instruments isaac tools Beyond 2200 nm the thermal background dominates with contributions from both atmo spheric and telescope emission The sky emission spectrum for a particular setting is an optional
91. f the fibers is reproducible to the level of accuracy required for reaching a precision better than 100 m s 3 for a discussion on spectral resolution see Bouchy F Pepe F amp Queloz D 2001 id One should note that in the case of CRIRES the choice of resolution is intimately related to the choice of slit width in the case that the PSF FWHM is larger than the slit width If it is smaller the resolution actually depends on the FWHM of the PSF and on the centering error caused by the secondary guiding algorithm 4 the location of the star photocenter on a slit not uniformly illuminated is a crucial aspect A mean precision of 10 ms requires a mean error on the centering of the target of 0 015 slit viewer detector pixel from one observation to the next This precision must be reached in spite of various seeing and transparency conditions In the case of AO observations this precision must also be reached despite variations on the quality of the AO corrections which depends on atmospheric turbulence airmass There is no guarantee that the algorithm used for the secondary guiding on the slit viewer can reach such a level of accuracy on a constant basis with so many variable parameters Two solutions can be adopted e observations in NoAO mode with the narrowest slit in bad seeing conditions FWHM at the observing wavelength larger than at least 4 5 times the slit width In this case the slit illumination is likely to be
92. ference wavelength that corresponds to the wavelength at the middle of detector 3 In a few cases see 7 this reference wavelength is not sufficient and an additional number the grating order is needed Set ups are done by using the instrument model to position the spectrum with an absolute accuracy to better than 30 pixels and a reproducibility 3 pixels Typically about 200 CRIRES settings are sufficient to cover the entire infrared spectrum in the range of 950 lt A lt 5400nm Standard wavelength settings are detailed in Sect 15 Wavelength can also be set using free wavelength settings allowed ranges for the reference wavelength are listed in Tab 6a However as the characterization of the instrument improves the CRIRES team realized that the current set of standard wavelength settings does not guar antee a full coverage without some risk of vignetting by the intermediate slit or contamination by adjacent orders Tables 4a 4h Tables 5a 5h therefore now provide under the columns Unvignetted range the wavelength wavenumber ranges for which reproducibility of the illumination is estimated to be better than 1 for a 0 2 slit Wavelength outside of these ranges but still covered by a detector are subject either to sometimes severe vignetting by the intermediate slit or contamination from adjacent orders The wavelength range for which the reproducibility of the illumination is better than 1 is smaller for a wider slit Becau
93. fferent jitter value If the number of nodding cycles is small it is probably better to set this parameter to T For a large number of nodding cycles any residual detector systematic effects may be further decreased by setting the parameter to F 14 3 Calibration templates 14 3 1 Standard star or telluric observations The calibration template CRIRES_spec_cal_ AutoNodOnSlit is used to measure a telluric or spectro photometric standard star Sect 9 Its functionality is similar to the observing template CRIRES spec obs AutoNodOnSlit described above The files produced here will be automatically recognized by the pipeline as standard star observations 14 3 2 Flat field Flat fields can be obtained with the template CRIRES spec cal LampFlats However there is no a priori necessity to obtain flat fields during the night Only INS WLEN REF and INS GRAT ORDER must be defined in this template 14 3 3 Wavelength calibration High precision absolute wavelength calibration can be either obtained with sky emission lines or through the use of an arc lamp spectrum see Sect 7 1 currently the reproducibility of the wavelength setting between night time observations and day time calibrations is 3 pix els If required for your science experiment than insert the CRIRES spec cal Wave template either before or after any new wavelength setting in order to perform a wavelength calibration The parameters required by this template are INS LAMP IN
94. frared 0 95um 5 4um high resolution spectrograph located at the Nasmyth A focus of UT1 Antu It provides long slit 31 spectroscopy with a spatial sampling of 0 086 Spatial resolution and signal to noise ratio can be maximized by the optional use of a MACAO adaptive optics system equipped with an optical R band wavefront sensor The main optical elements consist of a prism acting as a pre disperser and a 31 6 lines mm echelle grating Total spectral coverage per individual wavelength setting is 70 thanks to an array of four Aladdin III detectors Acquisition and guiding are performed by means of a slit viewer equipped with an additional Aladdin III detector and a series of 5 filters J H K and two neutral density H filters CRIRES has been designed to exploit the enormously enhanced sensitivity provided by a spectroscopic instrument with a large detector array at an 8m telescope The quantitative and qualitative improvements of observational capabilities affect all scientific applications aiming at fainter objects with higher spatial extended sources spectral and temporal resolutions Indeed CRIRES provides e High resolution spectroscopy in the 1 5 um range at the VLT This instrument employs the largest available grating for a spectral resolving power of up to 2 100 000 for 2 pixel Nyquist sampling with a 0 2 slit e Spectral coverage maximized through four 1024 x 512 pixel InSb detector arrays in the focal plane e
95. gives a practical example of the associated error The use of gas cells not part of the observatory standard set which currently only includes N20 and CO gas cells is limited to runs executed in visitor mode as their use would interfere with regular service mode observations 28 Figure 15 The N gt O and CO gas cells mounted on the carriage Mechanical lay out Figure 15 shows the way the present ESO s gas cells are mounted on the carriage Figure 16 describes their mechanical lay out In principle the cells are held in place by a bar pressed down with a knurled nut Any mechanical design which is compatible with the overall design space and this very generic fixation method is acceptable The minimum optical clear diameter should be 22mm to have sufficient field for acquisition and nodding The optical quality of the entrance windows has to be sufficient to allow for diffraction limited imaging Low order aberrations e g spherical aberration or astigmatism are acceptable as the MACAO adaptive optics system would correct for them The windows have to be transmitting and of good quality for both the AO reference wavelength 600 1000nm as well as for the spectral region of interest to be covered by CRIRES One of the windows is very close to the telescope focus so it is important that at least one of the two windows is scratch free and clean If relevant the preferred orientation of the gas cell needs to be indicated The gas cell will ope
96. guiding In NoAO mode J 16 5 H 16 0 or Ks 15 4 stars are barely detected 3c in a similar 10s integration under 0 9 seeing when located away from the slit For guiding on target in NoAO mode the limiting magnitude is much brighter as only a small fraction of the light is reflected by the slit jaws to the slit viewer detector Under 0 9 seeing and a slit of 0 4 reasonable guiding was possible with stars of J 14 1 H 13 8 Ks 13 3 20 Table 1 Summary of detector parameters Detector Parameter 1 2 3 4 Dark current e s 0 053 0 32 0 37 0 34 Gain e ADU 6 97 6 89 6 92 7 27 Quantum efficiency Le fol 0 92 0 97 0 83 0 73 Read out noise e RMS 9 9 9 7 9 6 10 Saturation level e7 120000 120000 120000 120000 Operating Temperature K 27 5 27 5 27 5 27 5 6 Detector characteristics The focal plane of CRIRES is equipped with four 1024 x 1024 pixel InSb Aladdin III 27 y pixel detector arrays However only the bottom half of each detector is actually illuminated by the slit so that the useful mosaic actually consists of 4 x 1024 x 512 pixels Fig 2 The observer needs to specify only two detector parameters the detector integration time DIT and the number of individual exposures NDIT to be averaged in a single exposure whose total integration time is therefore NDITx DIT Both parameters should be adjusted with help of the ETC Sect 10 2 Bright objects or observations in the L or M bands
97. he X direction 0 10 10 0 10 along the Y direction 14 2 5 CRIRES spec obs SpectroAstrometry only list of derotator angles jitter reset The CRIRES spec obs SpectroAstrometry template is allows one to apply the spectro astrometry technique without having to re acquire the target for each position angle It only makes sense to use this template if INS DROT MODE Derotator mode is set to SKY in the acquisition template Currently this template is only implemented in AO mode INS DROT POSANG LIST P2PP List of position angles is the list of position angles the CRIRES spec obs SpectroAstrometry template allows one to repeat the same sequence of observations as the ones done for the CRIRES spec obs AutoNodOnSlit template but for each value of the list of slit position angles given by this parameter Best results are obtained by giving a list of pairs of position angles differing by 180 degrees SEQ JITTER RESET P2PP Reset jitter for each DROT posang Only relevant if SEQ JITTER WIDTH Jitter width is larger than 0 If this parameter is set to T the list of 64 jitter positions calculated by the observation software is repeated identically in detector coor dinates for each value of the slit position angle In other words the location of the different spectra for each nodding position will be identically repeated for each position angle If set to F each nodding position in the execution of the whole template will be given a di
98. he membrane mirror vibrates the pupil image is projected on both sides of the lenslet array plane The normalized difference between the intra and extra pupil flux collected by each sub aperture is proportional to the local wavefront curvature which provides the wavefront error The fibers drive the signal from the fiber feed module to the APD cabinet mounted on the instrument The APD counts are recorded by the APD counter module synchronously with the membrane signal The front end assembly of the fiber bundle is shown in Fig 8 3 2 3 Control loop The oscillating membrane produces a signal modulated proportional to the local wavefront curvature This signal collected by APDs is sent to the real time computer RTC The RTC computes this modulation and retrieves the voltages to be applied to the mirror and tip tilt mount to optimally compensate for the local curvature measured For this a precise calibration of the system is required which includes synchronization of the membrane mirror determination of the membrane curvature pupil alignment and interaction matrices 14 mM SBM1 pupil image 14 mm diameter SBM4 Lenslet array SBM3 SBM2 membrane mirror 45 00 MM zy wavefront sensor box ESO 0l Aug 01 Figure 7 The optical path of the wavefront sensor box Figure 8 Fro
99. heric structure and oscillations magnetic field structure Star formation and ISM accretion and outflows ISM chemistry and cloud structures H H2O CH4 Extragalactic astronomy AGN velocity structure of the broad and narrow line region Fell H gt lines in low extinction regions H recombination fine structure lines Structure and scope of the User Manual The CRIRES user manual is structured as follows Part 1 provides a technical description of CRIRES and its adaptive optics system AO Part II details the instrument performance Part III describes the commonly used observing techniques in the infrared summarizes the CRIRES observing modes and provides guidelines for Phase 2 preparation Reference material is given in Part IV It includes a description of the calibration plan the data format the template reference guide and the defined wavelength settings Finally Part 19 provides a number of recommendations written to increase the chances that a program is executed successfully CRIRES User Manual VLT MAN ESO 14500 3486 3 1 3 More information on CRIRES All CRIRES related manuals are available on the CRIRES instrument web pages together with the most updated information on the instrument http www eso org instruments crires Both Service and Visitor mode Observation Blocks OBs should be prepared with the latest version of the Phase 2 Proposal Preparation tool P2PP available
100. ible sources of fringing e g interference filters were avoided in the spectrograph design The requirement on the grating reproducibility has been set to 0 05 pixel Currently the absolute wavelength reproducibility is achieved by the optical model to 3 pixels The detectors are not science grade arrays they show bad cosmetics and amplifier glow their response to incident light is non linear Information loss caused by bad pixels can be removed by jittering the amplifier glow in any given exposure can be subtracted out by a dark obtained with the same detector integration time DIT see below However amplifier glow as well as other systematic effects are best removed by telescope nodding A method to correct for the non linearity of the detector has been implemented in the pipeline A first light spectrum of the sky is shown in Fig 9 The OH doublet at 1708 6nm is resolved at the resolution of CRIRES In the dispersion direction the FWHM is 2 8 pixels Figure 9 First light spectrum of the sky The OH doublet at 1708 6nm is resolved at the resolution of CRIRES 17 5 AO performance The performance achieved by the MACAO system of CRIRES has been evaluated by lab oratory simulations by comparing two cases i in closed loop with guide stars of various magnitudes and ii in open loop thus without AO corrections The optimization was done over the encircled energy on a 0 2 slit representative of the available energy for the sp
101. ines mm 63 5 blaze angle 100 000 0 2 50 000 0 4 slit 0 95um lt A 5 4um A 70 4096 x 512 pixels using 4 Aladdin III detectors 0 086 J H K 2 H neutral density Aladdin III array gz 36 x 43 0 045 ZnSe prism CRIRES User Manual VLT MAN ESO 14500 3486 vill This page was intentionally left almost blank CRIRES User Manual VLT MAN ESO 14500 3486 Contents 1 Introduction Ll a oes oodd E S Be Be are Be ete Be Ee Be oe w QUN eX 1 2 Structure and scope of the User Manual LS Mor information on CRIRES 2 cocidas ra e X 3 EH E ai MA A E Br E PURUS nue Ne mop Pa mum PEU ee Q I The instrument 2 Cold part the spectrometer S OPNS ee coe a3 eub xu HU Pok e Mou ub VER ub EROR TE eS ee AR 27 Merthan e been e S pasqa a o4 e X ome ow Xon Rm Se oe Re SE oue 2 9 Detects xu do x Eo a Go xe omo OE XX Xe ES X Res dest X Bes dot wR 3 Warm part the adaptive optics system Od TOGO uuo eee a qr See s s RO V moe A s d All Atmosphere turbulence oces ra bed Dee ee AS E Y EE e B LZ Adaptive ONG d me w s k O PRA a RE HEHE SA N 22 Hardware descriphon e s os s ZJ X ac ste s SC she s ew A EE EDD Re OR CN 3 2 1 The Corrective Optics ba bee Roe ook reo a a o RA 3 2 2 The Wavefront Sensor CAS MEE oM oh Q v eee Bee EMEA SS KSEE RE S Quim EH 224 Membrane SUE ss sca oon om Rex Yos mk Ee oe Es RE n II Instrument Performance 4 Overview 5 AO performance
102. ines up to about 2500 nm The ESO Calibration and Instrument Modelling group in Garching together with the US National Institute of Stan dards and Technology have collaborated to increase the number of identified Thorium and Argon lines in the NIR This collaboration to support the wavelength calibration of CRIRES 25 lead to a paper available in the Tools section in the CRIRES web page Users whose science has benefitted from the ThAr calibration should cite Kerber F Nave G amp Sansonetti C J 2008 accepted for publication in ApJ At the time of issuing this Manual the catalogue available at the CRIRES calibration data page at http www eso org observing dfo quality CRIRES pipeline pipe calib html and part of the CRIRES pipeline distribution catalogue only contain lines that were identified be fore this later work Check these web pages for any update An additional high precision method is provided by the use of a N2O gas cell in front of a halo gen lamp as the N20 lines are recognized wavelength standards beyond 3500 nm However they are only present in a limited number of settings The list of N2O lines is also available at http www eso org observing dfo quality CRIRES pipeline pipe_calib html and is also part of the CRIRES pipeline distribution The following guidelines shall be considered in case high precision absolute wavelength cal ibration is required Section 18 details the recommended method to carry out an accurate
103. ing functions are sequentially implemented in the wavefront analyzer e Extraction of the reference star beam field selector 12 e P urku uwa E b i F 15 Nasmyth focus Py O a RL H Dichroic Analysis tool Figure 5 Top view of the warm optics of the MACAO CRIRES system From f 15 Nasmyth focus and after the optical derotator one notices the deformable mirror and tip tilt mount assembly Light enters from the dichroic to the cold and warm part of the instrument For the latter the wavefront sensor and some analysis tools are visible e Projection of the reference star image on the membrane mirror imaging lens e Scan of the intra and extra pupil regions by modulation of the membrane mirror cur vature e Creation of a pupil image centered on the lenslet array e Reduction of the flux to work within the linear range of the APDs by means of neutral density filters e Re imaging of the 60 sub pupils on the 60 fiber cores by the lenslet array unit e Injection of the collected beams onto the 60 APDs The scanning lens of the field selector is mounted on an XYZ table the XY axes enable the star used for AO correction to be selected in the 50 x 50 field of view while the Z stage com pensates for the VLT field curvature The position of the field selector defines the reference for the pointing The imaging lens creates an image of the AO star on the membrane mirror which i
104. ion values in RA and DEC and specified in units of year If they are different from 0 the epoch TEL TARG EPOCH P2PP Epoch at which the coordinates were valid should be given 56 TEL TARG ADDVELALPHA TEL TARG ADDVELDELTA P2PP Diff in RA DEC are additional velocities in a and in units of second For solar system objects the coordinates should be the J2000 ICRF astrometric coordinates In particular the user should not provide the apparent coordinates Note Starting with P2PP 2 12 the differential velocities for moving targets are to be specified directly in the target package and not in the acquisition template as in previous versions i e the fields Telescope Alpha Delta additional tracking velocity should be left blank Please check Section 5 5 3 of the P2PP User Manual for more details TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA P2PP RA DEC offset between target and SV guide star In some cases such as e relatively faint targets observed through a relatively wide slit for which not enough light is reflected from the slit jaws to the slit viewer detector this situation may occur e g for H 14 targets and slit wider than 0 3 in good seeing conditions e diffuse objects on which guiding is difficult or impossible the use of a brighter object in the field of the slit viewer is recommended This object will be used as a reference object for initial centering and as a guide star for secondary guidi
105. line has been released by ESO SDD It uses the ESO CPL library The main observation and calibration templates are supported by an automatic version of the pipeline for quick look analysis at the telescope Raw images are combined spectra extracted and calibrated in wavelength Photometric conversion factors based on standard star observations are provided More information can be found at http ww eso org sci data processing software pipelines and http www eso org observing dfo quality index crires html 59 14 Template parameters All scientific and calibration observations with ESO instruments are prepared as observation blocks OBs and with the phase 2 proposal preparation tool P2PP Observation blocks consist of the target information a small number of user selected tem plates the constraints sets and the scheduling information The input parameters of the templates described below are list of keywords that define the telescope pointing and instru ment configuration One OB contains only one acquisition template and is followed by one or more science or calibration templates User accessible input parameters of CRIRES templates for acquisition science dark flat wavelength calibration and or standard star observation are described in the following sections The pipeline is triggered by DPR keywords which are described in the pipeline user manual There are given here for completeness 14 1 Acquisition templates All sci
106. ll range 52 ThAr full range 51 ThAr full range 50 ThAr full range 49 ThAr full range 48 ThAr full range 47 ThAr full range 46 ThAr full range 45 ThAr full range 44 ThAr full range 43 ThAr full range 42 ThAr full range 41 ThAr full range 40 ThAr full range 39 ThAr full range 38 ThAr no lines in range 1514 1520 3T ThAr no lines in range 1514 1523 36 ThAr no lines in range 1583 1594 35 ThAr no lines in range 1583 1594 34 ThAr no lines in range 1659 1672 33 ThAr no lines in ranges 1659 1672 1698 1701 32 ThAr no lines in ranges 1730 1739 1738 1747 1764 1784 1803 1811 31 ThAr no lines in ranges 1764 1784 1803 1811 1816 1825 30 ThAr no lines in range 1880 1890 92 93 Table 8b Recommended wavelength calibration source Order Source Comment 29 ThAr few lines 28 ThAr few lines 27 ThAr few lines 26 ThAr few lines 25 sky absorption lines full range 24 HALOGEN CO full range 23 sky absorption lines full range 22 HALOGEN N20 useful ranges 2581 0 2640 6 2645 4 2652 7 21 HALOGEN N20 useful range 2651 2 2698 3 20 HALOGEN N20 useful ranges 2742 3 2781 3 2847 8 2917 7 19 HALOGEN N30 useful range 2860 6 3016 7 18 sky emission lines full range 17 sky emission lines full range 16 HALOGEN N30 useful range 3533 8 3629 9 15 HALOGEN N30 useful ranges 3581 6 3629 5 3831 8 3927 0 14 HALOGEN N20 useful ranges 3831 8 4145 9 4161 9 4177 9 13 H
107. llers having 64 channels 4 x 16 for the science arrays and 32 channels for the slit viewer one 3 Warm part the adaptive optics system The adaptive optics system of CRIRES is discussed by Paufiqu et al 2004 SPIE 5490 216 The multi applications curvature adaptive optics system MACAO for CRIRES cor rects a turbulent wavefront and provides diffraction limited images at the focal plane The overall sensitivity is thereby improved by about a factor two for point sources To highlight the advantage of combining MACAO and CRIRES a PSF is shown in Fig 3 in AO open loop uncorrected and closed loop where the PSF is reconstructed from wavefront measurements The non circular PSF in open loop is due to the very short integration time used Figure 3 PSF without left and with right AO correction Images have been taken in the lab using a turbulence generator 3 1 Introduction The following section provides an introduction to the field of adaptive optics and atmospheric turbulence and essentially is taken from the NACO user manual For further reading see for example Adaptive optics in astronomy Rodier 1999 Cambridge University Press or Introduction to adaptive optics Tyson 2000 Bellingham SPIE 3 1 1 Atmospheric turbulence The VLT theoretical diffraction limit is 1 22 A D 0 07 arcsec at 2 2um But the resolution is severely limited by atmospheric turbulence to A ro z 1 arcsec where ro is the Fried para
108. located in the integrating sphere The integrating sphere provides uniform illumination of the entrance slit of the spectrometer and its flux can be adjusted by a moving baffle A carriage can then insert one of the following elements in the light path i a gas cell either for wavelength calibrations when used with the halogen lamp or for accurate radial velocity measurements similar to the way the iodine cell is used in UVES ii a pinhole used for calibration purposes iii an AO fiber for MACAO calibrations iii a set of fibers fed by a Thorium Argon lamp used for wavelength calibration This carriage has also a free position with no optical element Light then goes through a 3 mirror de rotator which can be used to counteract the telescope field rotation for observations with a slit fixed relative to the sky On the other hand for point sources it can also maintain the slit aligned along the parallactic angle to accommodate the differential atmospheric refraction between the R band used by the adaptive optics system and the IR band used for observations and slit viewer guiding Next the adaptive optics AO system concentrates the light on the spectrograph s entrance slit The AO wavefront sensor uses the visible light reflected by the dichroic which serves also as entrance window while the infrared light enters the cryogenic spectrograph Further details of the AO system can be found in Sect 3 of this manual CRIRES can be used
109. me hot stars also have emission lines or are in dusty regions and should therefore be avoided A positive value of the V I color of a star can be used as an indicator of reddening due to the presence of dust on its line of sight Hot stars tend to lie near the galactic plane Correction of telluric features for objects close to the galactic pole may therefore require a different strategy 9 3 4 Late type stars or G stars as telluric standards Unfortunately spectra of hot stars do contain some features usually lines of hydrogen and helium that can be difficult to remove If the region around the hydrogen and helium lines is of interest then a late type star could instead be observed as its spectrum only show weak hydrogen and helium lines Solar analogs for the purpose of removing telluric features are stars with spectral type GOV to G4V These stars have many absorption lines in the IR particularly in the J band These features can be removed by dividing the solar analog spectrum by the solar spectrum at the resolution of the observations In addition to hot stars and solar analogs IR astronomers have used other stellar types as telluric standards For example F dwarfs are commonly used 9 3 5 Catalogs The CRIRES tools web page http www eso org instruments crires tools provides a number of catalogs of stars that can be used as telluric standards 9 4 The influence of the Moon Moonlight does not noticeably increase the backg
110. meter rp is directly linked to the strength of the turbulence and depends on the wavelength as gt For average observing conditions ro is typically 60cm at 2 2 um Temperature inhomogeneities in the atmosphere induce temporal and spatial fluctuations in the air refractive index and therefore cause fluctuations in the optical path This leads to random phase delays that corrugate the wavefront WF The path differences are to a good approximation achromatic Only the phase of the WF is chromatic The coherence time of WEF distortions is related to the average wind speed V in the atmosphere and is typically of the order of rg V 60 ms at 2 2 um for V 10 m s 10 3 1 2 Adaptive Optics A technique to overcome the degrading effects of atmospheric turbulence is real time compen sation of the deformation of the WF by adaptive optics AO Figure 4 The wavefront sensor WFS measures WF distortions which are processed by a real time computer RTC The RTC controls a deformable mirror DM to compensate the WF distor tions The DM is a continuous thin plate mirror mounted on a set of piezoelectric actuators that push and pull on the back of the mirror Because of the significant reduction in the WF distortions by continuous AO correction it is possible to record near diffraction limited images with exposure times that are significantly longer than the turbulence coherence time The residual error from the WF compensation WF error dire
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112. nd outside focus blurred pupil images can be imaged on a detector array in the case of CRIRES a lenslet array feeds avalanche photo diodes APDs The modulation frequency of the membrane corresponds to the temporal sampling frequency of the WFS The difference between the inside and outside pupil image measures the local WF curvature The performance of an AO system is related to the number of lenslets in the lenslet array the number of actuators behind the DM and the rate at which WF errors can be measured processed and corrected the server loop bandwidth The performance of an AO system is also linked to the observing conditions The most important parameters are the seeing the brightness of the reference source used for WFS and the distance between the reference source and the object of interest In case of good conditions and a bright nearby reference source the correction is good and the resulting point spread function PSF is very close to the diffraction limit A good correction in the K band typically corresponds to a SR larger than 30 At shorter wavelengths particularly in the J band or in the case of poor conditions or a faint distant reference source the correction is only partial the Strehl ratio may only be a few percent 3 2 Hardware description The MACAO system for CRIRES is based on a 60 actuator deformable mirror inserted in a so called relay optics These optics and the wavefront sensor optics are mounted on
113. new configuration table updated numbering changed new sub section on water vapor updated updated ETC updated precipitable water vapor incl overhead for derotator motion in spectroastrometry added a fig with water vapor only transmission ThAr fibers CO gas cell and visitor gas cells Updated for the use of CO gas cell Updated Updated for ThAr fiber calibration plan updated added note regarding slit width Added note vacuum wavelength are used Added note regarding multiple stars updated with CO gas cell for order 24 news updated checklist updated update on identification of ThAr lines added not regarding slit width radial velocity measurements added spectral resolution updated linearity added WES last sky measurements updated limitations due to differential refraction removed P2PP links updated L Tacconi Garman and M Hilker provided numerous comments on the various versions of this manual that greatly improved its accuracy and clarity The content of 7 2 2 RV mea surements is based on discussions with H U Kaeufl P Figueroa and Andreas Seifarht CRIRES User Manual VLT MAN ESO 14500 3486 vi Abbreviations and Acronyms AO APD BOB CPL CRIRES DM DMO ESO ETC FC FoV FWHM NGS NIR NIST OB P2PP PSF QC RTC RTD SDD SM SNR SR TIO TTM USD VLT VM WF WES Adaptive optics Avalanche photo diode Broker of observation blocks Common Pipeline Library Cryogenic high resolu
114. ng It is referred to as slit viewer guide star SVGS In this case TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA correspond to the offsets im between the SVGS and the target If a SVGS and 9 SVGS are the coordinates of the slit viewer guide star the sign conventions are as follow TEL TARG ALPHA TEL TARG OFFSETALPHA a SVGS TEL TARG DELTA TEL TARG OFFSETDELTA SVGS In other words TEL TARG OFFSETALPHA and TEL TARG OFFSETDELTA are positive if the SVGS is located to the East and North of the target Example one wishes to observe the target at Q2000 Target 04h53m50 678s d2000 Target 25 25 56 017 To center it in the slit the nearby star at oam VOR 04h53m49 690s s9990 SVGS 25 25 45 078 is used as a reference star as well as the slit viewer guide star Both these objects have negligible proper motions Then TEL TARG OFFSETALPHA Aa Q2990 SVGS Q2000 Target 4 TEL TARG OFFSETDELTA Ad 52999 SVGS ooo0 Target 5 Therefore the relevant P2PP parameters are RA 04 53 50 678 DEC 25 25 56 017 RA offset between target and SV guide star 13 38 DEC offset between target and SV guide star 10 94 Notes 57 1 the use of a SVGS different from target is only possible if the derotator is set to SKY mode 2 the use of the CRIRES_spec_obs_SpectroAstrometry template is only possible if the SVGS is also the target 14 1 2 NGS parameters The following pa
115. nt end assembly of the 60 fiber bundle which guide the light to the sensors 15 3 2 4 Membrane setting The membrane mirror curvature represents an optical gain for the aberrations measurements A way to increase the performance of the system is therefore to increase the curvature of this mirror Increasing the curvature however requires increasing the field of view of the wavefront sensor optics as well This and some other non linear effects can degrade the estimate of the curvature For the same reason extended sources will affect the quality of curvature measurement and lead to a different optimal gain In some extreme cases the system can be unable to close the loop extended 6 planetary nebula with a faint blue white dwarf in the middle or a faint star close to the Moon for example A trade off is needed and an optimal optical gain has to be determined This optimal gain mainly depends on the seeing and marginally on the star magnitude and other factors It is tabulated in the configuration of the software and is transparent for the user 16 Part II Instrument Performance 4 Overview The sensitivity of the instrument from K band up to the L and M bands is limited by the thermal background whereas it is limited by detector performance in J and H In the thermal background observations benefit from the high resolving power of CRIRES as telluric features are better removed compared to spectrographs at lower resolution Poss
116. ods po33jouStAun 913 JO oprsjno uoryeurum 1o3ourered e se pogroods oq os e 3snur 1oquinu OPIO oY jeu sojeorput V e 103293op 103 oxid uro T ut 19 uotrsrodsrp ue ur 91 SISI Otto ISP oq UDAL OSTE ore 103293op MO t JO Yowo 103 uio ut posso1dxo ol JOqUINUSARM VINNIPA ur oge19A00 pue oguei perjoods pogjeusrAun q uorjeogrjuopr YYSuSTPOARM euiojur Q JoquINU JopIQ 1o15919p PIE u JO ZIG Joxid 3e q33uo oAeA oY se pougop sSUT JoS q33uo poAeA prepuejs oY 107 WU ur y su3Suo pA A oouol9Jow 2G ALL 83 96 zro oozsr rezer caSr sOSGP TAS USAGP 20097 rauer v sscgp 1 1 97 9 Ons 96 IZIS CTE TLES TLP S EI SPscr Ciper 07197 gozer TO9P u T 9c 9 T66IZ VOL 18667 S619 8997 9992 T9997 Z 619V OSOP GB TIL 86097 T9697 V I 96 9 S 9GTZ GOL STI9F Geeor T6eg 6799F 76997 rot It OLELY 9 SZ9F 66027 U T 93 97 OCL c6 OFL9Y e69v 06600 6 6L4P QZF LLbLb rot Fr TZ89P Frot 11 28 16 vEZIZ Cp 0999 T9017 VITLE 981 alt It 94920 T6LY 969 914p U T LE 2 LI OOT r9LLf GL16Lh 9809 PSV PES 698p L998F L 669f VV v SL8p 1 1 13 1 99107 VOL 99927 9TIS 6219 TYS 0 6P8p Cri t 6 ISSP 4 806 6 lOSP GO6S8F u T 2G 1 V 0L0C 88 ILF9f 1199 TL87 gresy S006P pezet coser 7 7S67 waesp Soret 1 1 87 8 9v0c 68 96987 cO0SST 6 288p 0 806p OTI6P L867 rt 4 896 8 898P c vG6r U T 8Z SG TZPOZ L6 O S67 TGL6P 9 T96F
117. on took place in June 2008 The tape has been completely removed Comparison with the value measured before the intervention indicates that no increase in the amount of scattered has been observed CRIRES User Manual VLT MAN ESO 14500 3486 5 e the CRIRES spec cal Wave template was modified to make sure that the ThAr fibers are properly centered in the slit temperature effects can slightly modified the MACAO optics located in the light path e the ETC has been modified in various aspects most notably by allowing the choice of sky and transmission spectra for different amount of precipitable of water vapor in the atmosphere Since the release of User Manual v81 1 e a first version of the CRIRES pipeline is available http www eso org projects dfs dfs shared web vlt vlt instrument pipelines html e anew science template is offered to apply the spectro astrometric technique see 11 2 4 e an intervention took place in December 2007 it consisted in 1 replacing the slit viewer detector with a new cosmetically better one this should decrease the number of bad pixels that affect secondary guiding for faint targets 2 replacing the entrance slit jaws the new slit jaws have sharper edges and show a much improved parallelism leading to a more constant resolution along the slit 3 the temperature setting of the instrument has been changed slightly 70 K instead of 65 K to improve the temperature stability of the instrument as a
118. ove 9 4 an FLI of 1 00 is suitable for most observations However telescope guiding and active optics can be compromised for moon distance smaller than 30 deg A smaller FLI value is recommended only in the case of AO observations with an AO star fainter than R 15 mag In this case a value 0 7 and a moon distance larger than 50 deg is generally adequate 11 5 2 Seeing and Strehl ratio for adaptive optics observations For closed loop AO observations the users must specify in the constraint set the desired on axis Strehl ratio i e the ratio of the maximal intensity of the PSF to the maximal intensity expected for the theoretical PSF with no turbulence This is the main parameter regarding atmospheric turbulence It should be set for the K band this value is produced by the ETC In addition all closed loop AO observations should enter also the FWHM of the seeing although this constraint is less relevant The constraint on the seeing refers to the seeing measured by the DIMM or by the guide probe as they are the most relevant for the MACAO system It is used as a guide together with the coherence time in order to estimate the achievable Strehl ratio If the AO star is not the science target it is worth noting that the isoplanatic angle Oe depends on airmass 9 and on the wavelength as A gt On the other hand the Strehl ratio SR decreases with the angular distance to the AO star 0 as SR exp 0 09 11 5 3 Seeing for se
119. owever the following caveats regarding telluric lines have to be taken into account a on the long term a fundamental limitation is the overall motion of clouds giv ing rise to telluric lines The fastest coherent cloud motion is caused by the jet stream which can reach velocities exceeding 55 ms during the Seifahrt amp Kaeufl 2008 study it reached 29 ms 1 it can therefore possibly induce a shift of up cos zenithal distance x cos difference of azimuth between jet stream direction and direction of observation xjet stream speed for lines that are only produced at the jet stream altitude and some possible line shape changes for lines that are par tially produced at this altitude However the largest contribution to most telluric absorption lines except O3 arise in the first scale height of the atmosphere above the telescope b many settings of CRIRES cover spectral ranges that include water vapor lines the column density of water vapor can change on a time scale of a few minutes In addition since water vapor is mainly located at low altitude its column density dependence on airmass can be different from the one of other molecules Presence of weak water vapor lines can subtly change the centroid of other telluric lines with which they are blended 27 c ThAr spectra are now produced using a set of fibers that illuminate the entrance slit Currently ESO cannot guarantee that the photo center of the light coming out o
120. p 3 start guiding Required information regarding the NGS Acquisition with AO requires the following information e The coordinates of the AO guide star at equinox J2000 and at the epoch of the obser vations unless the science target is also the AO Guide Star e The B R color of the star used for AO AO star or NGS This is used to compute the guiding wavelength for the field selector holding the AO guide star which in turn is used to correct for atmospheric refraction effects e The FWHM of the NGS in order to optimize a diaphragm in the AO system This diaphragm is set as a function of the seeing such that it optimizes the amount of light received from the object with respect to the amount of background light from the sky If the NGS is a point source the FWHM is best left to zero then only the seeing will be taken into account Only if your AO guide star is significantly extended with respect to the seeing should this parameter be set to a value different from zero 11 2 3 Acquisition sequences without AO The most general acquisition sequence for observation without AO is the following 1 preset the telescope to the slit viewer guide star SVGS 2 interactively re center the SVGS in the slit 3 start guiding 4 offset to the target Of course if the SVGS and the target are the same object the sequence simplifies to 1 preset the telescope to the target 2 interactively re center the target in the slit 3 start guiding
121. pect proper motions of both the target and the SVGS must be taken into account e For observations without AO guide star the acquisition template allows one to specify an offset between the SVGS and the target that is larger than half the width of the slit viewer up to 40 In this case guiding on the SVGS is therefore actually not possible The SVGS is then only a reference star e Nodding in the case of extended objects larger than 30 may require observa tions of offset fields to obtain sky measurements Their frequency depends on the band more frequent in J H less in K and on the accuracy with which one wants to subtract them Significant sky variations occur on timescales of a few minutes The CRIRES_spec_obs_GenericOffset is recommended in this case e For moving targets ephemeris files must be attached to each OB Slit Viewer guiding can only be done on the target 46 11 2 Observation Blocks and Templates An Observation Block is the smallest scheduling unit It consists of different templates which are described in more details below Science OBs must contain one and only one acquisition template It is followed by a number of science and possibly calibration templates used to obtain wavelength calibration exposures or flat fields Calibration OBs are intended for observations of telluric spectro photometric standard stars They must contain one acquisition template followed by the template used for telluric standard
122. plete at the time of issuing this manual The missing parts will be implemented in February and March 2009 CRIRES User Manual VLT MAN ESO 14500 3486 4 Since the release of User Manual v82 2 e the CRIRES spec cal Wave template was modified to make use of a variable neutral density filter this allows optimal illumination of the ThAr lines while avoiding the risk to introduce remanence by the brightest lines During P82 a major change to the instrument control and observing software will take place Implementation of differential refraction correction is one of the advantages visible to the users allowing to keep the object properly centered while observing at high airmass and with a reference wavelength different from the effective wavelength of the slit viewer filter 8 2 will be updated once appropriate tests are performed In January 2009 an intervention is foreseen At the time of issuing this Manual the following actions are planned a replace the cryo coolers by another model to avoid vibrations affect ing the VLTI currently the cryo coolers are switched off during a VLTI UT run therefore CRIRES cannot be used neither during a VLTI UT run nor a few days after b slightly lower the location of the science detector mosaic which would allow to offer a longer slit length c installation of metrology fibers that would allow to guarantee a better reproducibility of the wavelength settings both in terms of wavelength range an
123. position A is South of the centering position Conversely for nodding position B the image of the target appears at smaller y values on the slit viewer and larger y value on the science detector On the science detector wavelengths increase from left to right 32 7 5 Spectral resolving power A spectral resolution of 96 000 has been measured with a slit width of 0 2 at 2172 nm Simi larly a spectral resolution of 60 000 has been measured with a slit width of 0 3 Currently the relation slit width to spectral resolution R is such that R x slit width in 0 2 100 000 which is valid for slit width between 0 2 and 0 8 However as of December 2008 the entrance slit width reproducibility can show peak to peak variation of up to 20 In par ticular observations made with slit width larger than 0 2 may be affected if they involve change of wavelength settings indeed a change of wavelength setting triggers an algorithm to check that the spectrum in well centered on the intermediate slit see 8 4 this algorithm uses a slit width of 0 2 It is expected that the reproducibility of the entrance slit width will improve after an intervention in January 2009 Figure 18 shows the optical depth profile obtained from the combination of 5 12CO lines seen in absorption toward the young star DG CrA using a 0 2 slit width A Gaussian fit to this profile taking into account the finite pixel width gives a FWHM of 3 18 kms
124. r Halogen CO gas cells provides enough lines for any useful wavelength calibration the wavelength calibration must therefore be made using the science data them selves Obviously the sky emission lines cover the whole slit length while the sky absorption lines are only useful in front of objects showing a continuum The Halogen CO gas cell is a good option for settings in order 24 Note that sky emission lines can also be used red ward of 2500 nm instead of the Halogen N30 gas cell The exposure time calculator ETC also allows one to determine the density of sky emission lines sky absorption lines or of lines from the Halogen lamp N20 gas cell A ThAr line list for the wavelength range covered by CRIRES is part of the static tables available at http www eso org observing dfo quality CRIRES pipeline pipe_ calib html However a new table providing twice as many identified lines should be available shortly see 7 2 1 The CRIRES team is considering various solutions to provide accurate wavelength calibration in the spectral regions not yet covered by the current scheme Updates will be posted in the instrument web page http www eso org instruments crires Potential users should email their respective contacts 1 4 Table 8a Recommended wavelength calibration source Order Source Comment 59 ThAr full range 58 ThAr full range 57 ThAr full range 56 ThAr full range 55 ThAr full range 54 ThAr full range 53 ThAr fu
125. r a requested SNR In addition it helps to visualize the wavelength coverage of each detector For a point source the SNR corresponds to the one obtained by integration over the spatial diffraction profile and is given per spectral pixel and not per resolution element To compute the SNR for a resolution element the right number of pixels needs to be combined typically 2 pixels for the 0 2 slit For an extended source the SNR corresponds to the one obtained by integrating the signal over 1 It also corresponds to a SNR per step in wavelength When the NGS AO mode is selected the ETC also outputs the estimated Strehl ratio in the K band This value is needed in the constraints set of an OB For extended objects only FWHM should be entered Starting with period 82 Phase 2 and ETC v3 2 6 the user can specify the vertical amount of precipitable water vapor PWV in the atmosphere the ETC therefore uses the appropriate emission and transmission spectra for the PWV and airmass chosen This functionality allows one to determine if the SNR will be or not affected by water vapor One should note that the effect of water vapor lines also depend on the temper ature at the time of observation as well as the altitude of the layers where the water vapor is concentrated therefore limiting the accuracy of the SNR determination to a few 10 In period 82 when relevant users are suggested to group wavelength settings in OBs requiring similar PW
126. r proper secondary guiding It is worth to recall that the seeing FWHM e depends on the wavelength following A nm CS 500nm e A 500nm and on the zenith distance z following e z e z 0 sec z 2 30 l L OOO OOLZEL O 90571 DIO LORI Te PAULA tposz win guo enun emo m nr z at neu pp UM eh LESSE BO TRA HUCIO y T SCR 13 2119 Figure 16 Mechanical lay out of a gas cell 31 SCIENCE CHIP 3 19 ap DY ET Figure 17 Illustration of the geometry of the science and slit viewer detectors for a posi tion angle of 0 degree on sky On the science detector North is to the bottom and East to the left while North is to the top and East to the left on the slit viewer detector The centering position of the science target is the center of the slit in r and pixel y 493 along the slit This position corresponds to pixel y 200 on the science mosaic the exact value depends on the detector With the templates CRIRES spec obs AutoNodOnSlit and CRIRES spec obs SpectroAstrometry nodding is done symmetrically along the slit around the centering position For nodding position A the image of the target appears at larger y values on the slit viewer and lower y value on the science detector at half the nod throw from the centering position In other words for a position angle of 0 degree the telescope position at nodding
127. rameters are only required by the template CRIRES_spec_acq_NGS SEQ NGS ISTARGET P2PP Target AO guide star is a flag If set to T default the natural guide star NGS used for the adaptive optics is also the science target of the observations If this flag is set to F then the user needs to provide the NGS coordinates SEQ NGS ALPHA and SEQ NGS DELTA However see also the note 3 below 814 1 7 for a special case SEQ NGS COLOR P2PP AO quide star B R color value gives the B R color of the NGS This parameter is needed for accurate correction of the differential refraction between the wavelength used for the observations and the effective wavelength of the wavefront sensor SEQ NGS FWHM P2PP AO guide star FWHM arcsec gives the FWHM in of the object used as natural guide star For a point source a value of 0 is appropriate SEQ NGS SNR P2PP AO guide star Minimum S N gives the required signal to noise ratio that MACAO needs on the wavefront sensor to be able to close the loop The default value is fine for most cases except for the faintest objects that the MACAO can acquire in which case a smaller value is to be given SEQ NGS USELASTSKY P2PP Use the last sky measurement for the WES is a flag If set to T the MACAO will not repeat the sky measurement for the wavefront sensor The sky measurement is used to determine the signal to noise ratio of the wavefront sensor flux The default value T is
128. rate in an f 15 beam so that fringing in the windows is not a big issue Still if slightly wedged windows are used they have to be aligned such that the net prismatic deflection is close to zero to avoid differential refraction effects Logistics As part of the proposal process all relevant information as to the properties of the visitor gas cell have to be submitted to ESO In addition the fill gas has to be described and if relevant handling and safety procedures have to be clarified The cell s have to be sent to ESO Garching at least 4 weeks prior to the observing run properly packed for oversea shipment by airfreight ESO takes the responsibility of shipping the cells to and from the observatory At this stage only non toxic gases are allowed in gas cells 29 Operations At the beginning of the visitor run ESO will remove one of the two observatory gas cells and mount one of the user s gas cells to the instrument A change of the cells during one observing night is not possible 7 3 Flat fields Dedicated flats are best taken with the Halogen lamp DIT and NDIT are automatically determined by the template In particular DITs are always longer than 2 s for the reason given in 66 4 There is a priori no need to take flat fields at night time as the detector characteristics are sufficiently stable in time and the spectrograph wavelength setting sufficiently accurate However flat fields may be important for very accurate radial veloci
129. repared and it is available at http www eso org sci observing phase2 CRIRES P2PPTutorialCRIRES html 11 1 Information required The following are important considerations for a successful creation of CRIRES observation blocks e CRIRES acquisition templates may involve 3 different stars observed in 3 different wave lengths 1 the adaptive optics guide star usually referred to as NGS for natural guide star which is used to determine the shape of the wave front only the R band magnitude and B R color of this star matters 2 the slit viewer guide star SVGS which is used for fine guiding using the slit viewer in one of 3 bandpasses J H or K This star is also used as a reference star which can be acquired before a blind offset is made to center the target into the slit 3 the target object itself with a relevant wavelength between 940 and 5400 nm To be complete the user can provide coordinates for a 4th star which is the telescope guide star e Target coordinates should be as accurate as possible VLT absolute pointing accuracy is better than 3 RMS e If any of the science target the SVGS and NGS are different objects it is important that their coordinates have been determined in the same coordinate system e In particular if the SVGS is different from the target it is crucial that their separation at the time of observation is known with high accuracy ideally to better than 1 4 of the slit width In this res
130. right enough recenter it Case NGS SVGS Target If the same star is used for slit viewing and for the AO but is different from the target this sequence becomes 1 preset the telescope to the NGS possibly recenter it 2 acquire the NGS with MACAO and close the AO loop 3 start guiding 4 offset the telescope to the target if the target is bright enough recenter it Case Target SVGS 4 NGS If the target is used for guiding using the slit viewer but another star is needed for the AO the sequence becomes 1 preset the telescope to the NGS possibly recenter it 2 acquire the NGS with MACAO and close the AO loop 3 offset the telescope to the target 4 interactively re center the target 5 start guiding Case Target NGS 4 SVGS If instead the target can be used for the AO but is too faint for guiding using the slit viewer so that another star is needed as a SVGS the sequence becomes 1 preset the telescope to the target possibly recenter it 2 acquire the target with MACAO and close the AO loop Offset the telescope to the SV guide star interactively re center the SVGS start guiding Q Oo A WwW offset the telescope back to the target if the target is bright enough recenter it 48 Case Target NGS SVGS If the same star is the target the AO star and the SVGS the sequence simplifies to 1 preset the telescope to the target possibly recenter it 2 acquire the target and close the AO loo
131. roughput The wavelength dependence of the efficiency for a particular wavelength setting is shown for different slit widths on the left The peak efficiency as a function of slit width is shown on the right The overall efficiency or throughput 7 is defined as the ratio of e s pixel as measured on the detector divided by the theoretical expected photon flux photons s pixel arriving above the Earth s atmosphere Eq 3 In Fig 19 the overall efficiency as a function of slit width for order 26 at 2150 nm is shown together with the peak efficiency versus slit width During these observations atmospheric conditions were rather bad seeing of gt 1 6 and coherence time of 2 ms see Sec 3 so that the AO could not work effectively leading to significant slit loss Measurements have been repeated under better conditions and are currently under analysis 8 1 Transmission of the entrance window The transmission of the dichroic window which also serves as entrance window for the spec trograph has been measured in the laboratory in Garching for gt 1000nm It is shown as a function of wavelength in Fig 20 For shorter wavelengths only manufacturer measurements exist they indicate that the blue wavelength cut off transmission smaller than 50 occurs at 950nm 34 100 80 60 40 Transmission 20 0 1000 2000 3000 4000 5000 6000 Wavelength nm Figure 20 Transmission curve of the entrance window 8 2 Sensitivity
132. round in any of the CRIRES modes so there is no need to request dark or gray time for this reason However it is recommended not to observe targets closer than 30 to the moon to avoid problems linked to the telescope guiding or active optics system On the other hand the moon may affect the quality of the adaptive optics correction if the source used for wavefront sensing is fainter than R 15 mag In these cases reducing the lunar illumination constraint to approximately 0 7 and increasing the distance to the Moon to approximately 50 degrees is generally adequate Observers in visitor mode are encouraged to carefully check their target positions with respect to the Moon at the time of their scheduled observations Backup targets are recommended whenever possible and users are encouraged to contact ESO in case of severe conflict i e when the distance to the Moon is closer to 30 Visitors can use the tools that are available at http www eso org observing support html Select the link airmass which is under User Support Tools to help to determine the distance between targets and the moon for given dates 42 10 Observing in Visitor and Service Mode 10 1 Overview For CRIRES there are no deviations from standard VLT operational procedures As for all ESO VLT instruments CRIRES users must prepare their observations with the P2PP tool available at http ww eso org sci observing phase2 P2PP P2PPToo1 html Acquisition
133. roviding a resolution R zz 100 000 For observations of specific lines accessible in one setup CRIRES is clearly more efficient red ward of 970nm UVES CRIRES observations of B Col Feb 07 8 0 0 O T T T T T T T T T T T T T T a UVES zl CRIRES 6000 a 4000 4 2000 ii 4 f Mi D L a wt Au 4 J wP O be 4 1 1 1 l 1 ll LL l l 1 1 iml I 940 960 980 1000 1020 1040 Wavelength nm Figure 21 Comparison of S N per second of integration time obtained during nearly simultaneous observations of 3 Col Courtesy S Uttenthaler 8 3 Optical ghosts Occasionally especially when using the CRIRES Echelle grating in high order a quasi white light ghost is visible on the data It results from a retro reflection from the detector onto the grating which is redirected onto the detector in a different order and with reduced dispersion Ghosts cancel out by nodding as sky emission lines do One example of a ghost visible in a staring image is given in Fig 22 8 4 Stability and reproducibility For wavelength calibration the stability and reproducibility of the different mechanical func tions grating prism slit are important The absolute setting of the prism and grating guarantees that a given standard wavelength setting is accurate to better than 30 pixels even 36 Figure 22 Example of a quasi white light ghos
134. s observations and calibrations are coded via templates Two or more templates make up one observation block OB which then contains all information necessary for the execution of an observing sequence CRIRES and the telescope are setup according to the content of the OB There is one Real Time Display RTD for the slit viewer and one RTD for the spectrometer Daytime calibrations as described in the calibration plan see Sect 12 are executed the following morning by the Observatory staff In particular for service mode observers it is important to properly take into account the amount of time required for telluric corrections The execution time of a science OB is typically 1 hour Therefore at the time of submitting a proposal an observer has to already foresee that the observing time will be split in a number of OBs each of which usually requires an associated OB of a telluric star Service mode observers should submit their OBs before the Phase 2 deadline whose date is announced in the web letters The most important points for successful observations are listed in 8 19 at the end of this manual 10 2 The Exposure Time Calculator The CRIRES exposure time calculator can be found at http www eso org observing etc It returns an estimate of the on source integration time necessary to achieve a given S N asa function of different input parameters e The input magnitude can be specified for a point or an extended source For the lat
135. s mounted on an acoustic cavity A voice coil is mounted to the other end of the cavity and driven at 2 1kHz by the APD counter module to force an oscillation of the focus mode of the membrane mirror The incidence angle of the beam on the membrane mirror depends on the position of the guiding star in the field In order to keep the pupil image obtained when the membrane mirror is flat centered on the lenslet array the membrane mirror is mounted on a 2 axis gimbal mount which is co ordinated with the field selector For each x y positions 13 Figure 6 Assembly of the deformable mirror DM and tip tilt mount TTM left and of the gimbal mount right of the field selector the gimbal mount is moved so that the light is reflected to the same focus A diaphragm in front of the membrane enables the field to be adjusted to the observing condi tions seeing and guiding reference size The assembly of the gimbal mount is shown in Fig 6 The wavefront sensor box consists of 4 mirrors which provide parallel beam to image the pupil on the lenslet array First the beam is collimated by a spherical mirror It is then folded by a flat mirror and injected in the beam expander which adapts its diameter to the lenslet array 14 mm The optical path of the wavefront sensor box is shown in Fig 7 The lenslet array intercepts the beam and divides the flux in 60 sub aperture Each sub pupil is imaged on a fiber with a 100 wm core diameter When t
136. se of the time needed to resolve the vignetting problem described in 81 5 the CRIRES team did not have time to prepare a new configuration table to palliate this deficiency as earlier announced in the previous version of this manual Critical features can therefore fall at a wavelength not covered by any unvignetted range In case of doubt regarding the influence on some spectral features the user should email the appropriate contact listed in 1 4 Vacuum wavelength are used throughout this manual 7 2 Wavelength calibration 7 2 1 Standard means ThAr lamp and N O and CO gas cells Wavelength calibration of CRIRES spectra is difficult Depending on the wavelength and on the required accuracy different methods can be used For an accuracy corresponding to 3 pixels the start and end wavelengths and the derived dispersion assumed to be linear for each detector is sufficient in particular for the standard settings If present in raw data either emission or absorption sky lines can be used in the data reduction to improve the absolute wavelength calibration The CRIRES team has started to obtain data to quantify the absolute accuracy of such a method However the number of sky lines is insufficient to achieve a high precision absolute wavelength calibration for many settings in particular those below 2500 nm The density of lines provided by arc lamps is usually small in the IR However the Thorium Argon lamp can provide a large number of l
137. spatial extent of the minimum feature that one hopes to detect for point sources it should be larger than the width of the spatial profile 9 3 Flux calibration and telluric correction 9 3 1 General procedure Flux calibration and telluric correction are generally carried out in three steps The first step removes telluric absorption features of the extracted wavelength calibrated science spectrum by dividing it by the one of a telluric standard The second step removes the intrinsic spec tral features of the telluric standard that are imprinted onto the science spectrum because of the first step The third step uses a spectro photometric standard to set the absolute flux scale The spectro photometric standard and the telluric standard can be the same star Note that CRIRES as spectrometers in general is not meant to provide high absolute spectro photometric accuracy The Observatory does not offer observations of telluric or spectro photomeric standard stars Observers who wish to correct for telluric features or flux calibrate their spectrum therefore need to supply a standard star OB Observing time needed to execute telluric or spectro photometric standard stars is charged to the observer and must be taken into account in the amount of time requested during Phase 1 9 3 2 Telluric correction The most prominent features in IR spectra are telluric lines created by the Earth s atmosphere Unfortunately many telluric absorption lines
138. t observed with a reference wavelength of 1153 8 nm The ghost is visible in staring frames top left on the second detector Also a diagonal middle and a vertical right detector scratches are also visible possibly after a minor intervention A model of the instrument currently achieves a wavelength calibration of 3 pixels without simultaneous wavelength calibration A measurement of the stability of the instrument has been obtained by measuring the location of an emission line in short exposures spread over a span of 10 minutes A preliminary value is 1 20 pixel Such tests need to be repeated for different wavelength settings A problem has recently been found with the intermediate slit The main function of this ele ment is to avoid contamination of the spectrum by adjacent orders and to limit the background Unfortunately the whole unit appears to have moved and shows a lack of reproducibility af fecting in particular the settings shorter than 42200 nm A software solution to insure that the spectral range seen by the detector is well centered in the intermediate slit has been im plemented early July 2007 An additional software check to insure that the intermediate slit has the correct width is ready to be implemented On the other hand an encoder has been installed in April 2008 and its installation slightly modified in June 2008 Although the error on the reproducibility of the intermediate slit width is not yet available being t
139. tar DEC of AO guide star AO guide star B R color value AO guide star FWHM arcsec AO guide star Minimum S N Use the last sky measurement for the WFS WES Alpha sky offset arcsec WES Delta sky offset arcsec SV Guide Star AO Guide Star Use the last sky measurement for the SV RA offset to sky DEC offset to sky Telescope guide star selection RA of telescope guide star DEC of telescope guide star RA offset between target and SV guidestar DEC offset between target and SV guidestar Derotator Mode Position angle Entrance slit width Reference wavelength Grating order TEL TARG ALPHA TEL TARG DELTA TEL TARG EQUINOX TEL TARG EPOCH NODEFAULT NODEFAULT 2000 3000 2000 2000 3000 2000 Right Ascension Declination Equinox Epoch TEL TARG PMA 10 10 0 Proper Motion RA TEL TARG PMD 10 10 0 Proper Motion DEC TEL TARG ADDVELALPHA 15 15 0 0 Diff RA TEL TARG ADDVELDELTA 15 15 0 0 Diff DEC Fixed values Parameter Value Label DPR CATG ACQUISITION Data product category DPR TECH IMAGE Data product technique DPR TYPE OBJECT Data product type 65 CRIRES_spec_acq_NoAO To be specified Parameter Range Default Label SEQ SV USELASTSKY TEL SKY OFFSETALPHA TEL SKY OFFSETDELTA TEL AG GUIDESTAR TEL GS1 ALPHA TEL GS1 DELTA TEL TARG OFFSETALPHA TEL TARG OFFSETDELTA INS DROT MODE INS DROT POSANG INS SLI
140. tely sufficient sky lines are not necessarily available for all settings sometimes because they are saturated General recommendations on absolute wavelength calibration is given in Sect 7 1 However observers are strongly advised to use the ETC with the output options Sky Emission Spectrum and Sky Absorption Spectrum and to check for themselves if enough unsaturated telluric lines are available for a proper wavelength calibration in the spectral range of interest Dedicated OBs for wavelength calibration shall be attached immediately before or after the science template so that prism and grating are not moved in between Most observers wish to correct for telluric features and therefore need to supply a standard star OB Observing time needed to execute telluric or spectro photometric standard stars is charged to the observer 11 3 DIT setting In principle there is a free choice to select a DIT between the minimum of 1s and the maximum of 900s However it is strongly recommend to choose the one of the DITs listed below A first reason is that the dark which depends on a particular DIT is taken during day time calibration for all settings used during the previous night if a too large set of different and long DITs is used there is a risk that daytime calibrations cannot be performed entirely In addition the method to correct for non linear detector effects including the odd even effect see Sect 6 4 requires a large number of calibrations
141. tematic effects Sect 6 2 If set to a value gt 1 the total integration time of the template in seconds is DET1 NDIT x DET1 DIT x SEQ NEXPO x SEQ NABCYCLES x2 However one should not confuse integration time with the total execution time of one OB caused by the various overheads which need to be added as described in Sec 10 3 Examples If SEQ NABCYCLES 1 the telescope first points to the A position it is located to the South if INS DROT POSANG 0 at a distance equal to SEQ NODTHROW 2 see below and assuming SEQ JITTER WITDH 0 from the centering position After SEQ NEXPO exposures the telescope nods to the B position it moves to the north by SEQ NODTHROW and takes SEQ NEXPO additional exposures Then the telescope moves back to its original position The telescope has then executed one AB nodding cycle If SEQ NABCYCLES 3 the telescope first points to the A position as defined in the previous paragraph and takes SEQ NEXPO exposures It then moves to the B position takes twice SEQ NEXPO additional exposures It then moves back to the A position when it takes twice SEQ NEXPO exposures Then it moves a last time to the B position for a last sequence of SEQ NEXPO exposures before returning to the original position The telescope had therefore executed 3 nodding cycles AB BA AB SEQ NODTHROW P2PP Nod throw along the slit is the nodding throw or telescope offset between two nodding positions Sect 9 It should be
142. ter the input parameter corresponds to the magnitude per square Also input flux can be specified as surface brightness If the single line option is chosen it corresponds either to the total line flux for a point source or to the surface brightness for an extended source e If the observing date is known it may be used together with the target coordinates to compute the radial velocity shift due to orbital and rotational movement of the Earth Alternatively this tool allows the user to select the best time of the year to observe an object so that the targeted feature avoids a specific telluric line e If an AO guide star is used R mag and spectral type must be specified They can be obtained from online catalogs available at Simbad Vizier 43 Requested output can be either exposure time to achieve a given signal to noise ratio SNR or SNR achieved in a given exposure time In both cases the DIT needs to be specified see Sect 11 3 The following items should be remembered ETC outputs the on source integration time Depending on observing technique and accounting for overheads the total execution time will be longer Sect 10 3 It is always useful to ask the ETC to show the SNR as a function of wavelength due to the presence of numerous telluric features a small difference in the requested wavelength may lead to very different SNR for a given total integration time or alternatively very different integration time fo
143. though the long term accuracy of CRIRES radial velocity measurements has not yet been demonstrated there is no a priori reason to expect that a similar accuracy cannot be reached over a time span of months or years Wavelength calibration is of course the critical aspect of all radial velocity measurements a 10 ms precision corresponds to a mean error on the solution of 0 007 science detector pixel Some fundamental parameters regarding radial velocity measurements can be found in Bouchy F Pepe F amp Queloz D 2001 A amp A 374 733 However this paper mainly deals with measurements in the optical regime though and some results are not valid in the CRIRES accessible spectral range Regarding CRIRES observations the following aspects require particular attention 1 num ber of absorption lines of the star within the spectral range of interest 2 number of lines used for wavelength calibration 3 spectral resolution 4 slit illumination and photocenter error 5 flat fielding error There are briefly discussed in the following 1 in general the number of absorption lines should be as high as possible however blend ing or presence of broad lines should be avoided 2 the number of lines used for wavelength calibration should also be as high as possible here also the presence of broad lines should be avoided In the spectral range of CRIRES telluric lines offer a natural choice of wavelength calibration lines H
144. tion infrared echelle spectrograph Deformable mirror Data management and operations division European Southern Observatory Exposure time calculator Finding chart Field of view Full width at half maximum Natural guide stars Near infrared National Institute of Standards and Technology Observation block Phase II proposal preparation Point spread function Quality control Real time computer Real time display Software Development Division Service mode Signal to noise ratio Strehl ratio Telescope and instrument operator Tip tilt mount User support department Very large telescope Visitor mode Wave front Wave front sensor CRIRES User Manual VLT MAN ESO 14500 3486 vil CRIRES Vacuum 65K Overview telescope de rotator S deformable mirror dichroic window focal reducer m wavefront 4r slit viewer sensor L Bupilfilter lt Ee pre disperser detector mosaic echelle grating rror TMA 3mi collimator camera Calibration system Adaptive optics Slit length Slit width Echelle grating Resolving power Wavelength range Free spectral range Detector science array Pixel scale Slit viewer filters Slit viewer detector Slit viewer field of view Slit viewer pixel scale Pre disperser halogen lamp IR emitter ThAr N20 gas cell 60 actuator curvature sensing MACAO system 31 II 0 05 3 0 recommended 0 2 0 4 40 x 20cm 31 6 l
145. ty measurements They may also be important when the interesting lines appear at the blue or red edge of a spectral setting where possible vignetting by the intermediate slit may affect the detector illumination see 8 4 Flat fields that are part of the calibration plan see Sect 12 have a signal to noise ratio per pixel larger than 200 at the peak efficiency of a given setting A systematic atlas of the S N pixel of the flat fields for each standard wavelength setting has started and will be made available at http www eso org observing dfo quality ALL ref_frames ref_ crires html Users requiring flat fields with larger S N should contact ESO through the email addresses listed in 81 4 7 4 Spectrograph field of view slit width and seeing The field of view of the spectrograph is slit width x 31 The appearance of a spectrum on the science detector is illustrated in Figure 17 Note in particular that the default centering position is not at the center of the slit A slit width of 0 4 offers a close to maximal throughput in most AO observations For non AO observations the optimal slit width would in principle be given by the external seeing at the wavelength of observations However it 1s not recommended to use slit width larger than 0 4 as the spectral range for which the illumination is reproducible to better than 1 shrinks considerably see 7 1 In addition for faint targets not enough light is reflected by the slit jaws fo
146. uniform enough that the exact location of the photocenter is not a problem e in case of AO observations it is important that the light path includes one of the offered gas cells so that the reference lines it offers are fixed relative to the spectrograph Note that some problems listed in point 2 above are also valid here a line blending of the gas cell lines with the star absorption lines as the star radial velocity changes with the Earth motion around the Sun or by the presence of planet around the star under study b line blending with telluric lines of varying intensity depending on airmass or varying atmospheric conditions However in any case the use of a gas cell appears as the solution offering the highest radial velocity accuracy 5 the shape of the absorption lines can be changed subtly if the flat fielding was done with a slit width slightly different from the one obtained during the observations It is therefore important to attach a flat field in the corresponding OB 7 2 3 Visitor gas cells For ultra precise radial velocity work users may wish to employ a special gas cell in absorption during their scientific observations similar to the Iodine Cell method employed in the optical For the moment users have to supply their own gas cell s at their own risk In this context one should keep in mind the problem of pressure shift c f Fig 2b in Glenar et al ADV HELIO AND ASTEROSEISMOLOGY I A U SYMP 123 P 481 1988 which
147. ut uoAIS son peA YYSUSPOARM PMS ISL Z Y 10 TAA YT wey o1our ye jrpiqronpoadozr jo yoe Aq poyoye st osues Terjoeds pojjousrAun oY JO oprsjno uorjeurumg I Joyouered e se payroods oq ose SNU 1oquinu Jop1O oY YY so3eorput V 103293op 103 Toxid uru QT ut YE uorszodsrp ue ur o SISI uump oo ISP oq HOA OSTE are S1032939p MOJ oy JO Yo 10 FLI AOD pue oguei e1joods poyoustaun qJ uoryeogrguopr q3Suop o eA euirojur Q 19quinu I9PIO 1035939p PIE ol JO ZIG Joxid ye q33uo pA eA se pougop sSurj3es prepuezs oY 107 PY syYSUSTOARM DOUIOJOY Jp APL TT GLI 4878 T ZISP 92097 6 687 ogrr gott Cor DIP 96897 Taser 1 3 81 T 28677 VLL loggt LOS OLEH Coirtrlrrirt C OGPP COST S OEPY VSS Ler u g1 I T887 TOI SOM try LIP 9268P Teh TS 2998 Prey S8 6vY O9 G6cv 1 1 81 I 82007 61 v 6crp SOIP rot gor C OSEP vor SESED Geer ISH OTS8Z U T ET T G6 v 8 07 E ZSE OZEEP Y OCEP Cor Copcr Ur OLGE L APE U99682 or 1 1 T Er 89I8YV OZ S 6EEP SEGIST L ETED SH C OSCP EI PLSP TYEZ 9 PS P WEGTH U T ET ET 6 OEP EZZ TEIT MIP Q9 O CP VIZ VOZY IF 6 GLIP VISI Igor SIIIP 1 3 T ET Sheer GU OSZ GLH S ICCP SRIF HIF FIP 9 IOTP got l SSCP L ZOTP U C l T SOTZ 6ST 4 903P T6TP TL8IF S OLIP TOOTH T6rIh TYPIP O OCIP 8 spzb 08807 1 3 71 VI 68LTP TOT Eier LISIh YLLI 6 09Tp 98TP 6 8ETP SETH 9 GITP S8EZp
148. without adaptive optics in which case the AO module just acts as relay optics and the spatial resolution is given by the natural seeing The spectrograph itself is housed in a vacuum vessel Following the input window a pupil image is formed at the position of a cold stop which limits thermal background Light then either passes through the slit or is reflected to the slit viewing camera Light passing through the slit enters the prism spectrometer where it is dispersed and then exits through an inter mediate slit sized to limit the wavelength range passing into the high resolution section to a single order The high resolution spectrograph consists of a 40 x 20cm 31 6 lines mm 63 5 blaze echelle grating plus a TMA three mirror anastigmat which acts first as a collimator and then as a camera to image the spectrum on the four Aladdin detectors effectively forming a 4096 x 512 array 2 2 Mechanics CRIRES is stationary at the Nasmyth A focus of VLT UT1 Antu The instrument is mounted in a 3 m diameter 1 m high vessel Including its support structure the total weight of the instrument is 6 2 t spread between 2 t for the warm part or AO system and 4 2 t for the cold part The optics inside the cryo vessel is cooled to 70 K The detectors are stabilized at 25 K within 0 1 K A main design feature of CRIRES is its cryogenic mechanisms which are required for scanning the pre disperser prism and echelle grating light sensitive length of th
149. xample based on a sequence of flats obtained with different DIT settings It shows that this odd even effect depends on the signal level A method to correct for the odd even effect is described in the next paragraph 6 5 Detector linearity All common IR detectors suffer from non linear effects In the case of CRIRES non linearity effects are of the order of 3 at about 4 000 ADUs 32 000e7 and increase with flux The CRIRES team has developed a method that appears to efficiently correct for the non linear behavior of the detector including the odd even effect Results obtained at the date of issue of this manual indicates that a total signal dark sky object smaller than about 10 000 ADUs 70 000e7 can be corrected with good accuracy residuals much smaller than 1 providing both the science and the flat fields are taken with DITs longer than 2 s Data obtained with shorter DITs are affected by the finite reset time of the detector arrays 23 The method is more detailed in the description of the CRIRES pipeline at http www eso org observing dfo quality CRIRES pipeline pipe_gen html and in particular in the section dealing with the science recipes Static calibration files necessary to correct for the non linearity are available at http www eso org observing dfo quality ALL ref_ frames ref_crires html 24 7 Characteristics of the spectrograph 7 1 Wavelength settings Wavelength settings are defined by a re

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