NGC ESO s New General Detector Controller

Size: px

Start display at page:

Download "NGC ESO s New General Detector Controller"

Alexandra Parrish
6 years ago
Views:

1 NGC ESO s New General Detector Controller Dietrich Baade 1 Andrea Balestra 1 Claudio Cumani 1 Siegfried Eschbaumer 1 Gert Finger 1 Christoph Geimer 1 Leander Mehrgan 1 Manfred Meyer 1 Jörg Stegmeier 1 Javier Reyes 1 Mirko Todorovic 1 1 ESO As the replacement for ESO s standard infrared and optical detector controllers, IRACE and FIERA respectively, ESO has developed a new controller the New General detector Controller that will be the default detector controller for all new La Silla Paranal in struments in the QH[WGHFDGH7KHEDVLFVRILWVGHVLJQ DQGIXQFWLRQDOLW\DUHGHVFULEHGDQG:UVW SHUIRUPDQFHH[DPSOHVDUHJLYHQ The invisibility challenge In an era when professional astronomers G@UDKNMF@A@MCNMDCSGDM@JDCDXD@MC OGNSNFQ@OGHBOK@SDR@RRBHDMSHjBCDSDB SNQRL@MXTRDQRNE+@2HKK@/@Q@M@K+2/ HMRSQTLDMSRL@XMNKNMFDQJMNVVG@S happens exactly between the arrival of SGDOGNSNMR@SSGDCDSDBSNQ@MCSGDjQRS inspection of the new observation and SGDQDRGNTKCADMNMDDCSN@RSGHROQNB DRRRGNTKCADETKKXSQ@MRO@QDMSSNSGDL.MSGDNSGDQG@MCSGHRSQ@MRO@QDMBXB@M be achieved only if the corresponding OQNBDRRHRUDQXQNATRS@MCCNDRMNSHL OQHMSRHFM@STQDRNEHSRNVMNMSGDC@S@ 2HMBDSGHRjM@KRSDONE@MXLNCDQMNARDQ U@SHNMHRPTHSDBNLOKDW@MCRGNTKCAD BNLOKDSDCPTHBJKXSGDQD@QDL@MXONSDM SH@KE@HKTQDONHMSR@MCRNSGHRK@QFDKXHM UHRHAKDRSDOQDPTHQDRLTBGB@QD@MCDEENQS The detector may have to be cleaned of trons generated where the photons hit SGDCDSDBSNQ@RGTSSDQL@XG@UDSNAD NODMDCSGDDWONRTQDSHLDLTRSAD@BBT Q@SDKXJDOS@RGTSSDQL@XG@UDSNAD BKNRDC@MC@RDPTDMBDQG@RSNFDMDQ@SD SHLDCDODMCDMSUNKS@FDO@SSDQMRSNCQHUD SGD@BBTLTK@SDCDKDBSQNMRSNSGD@LOKHjDQ NQSN@CCQDRRD@BGOHWDK@LOKHjDQRDPTDM SH@KKX ESDQ@LOKHjB@SHNMSGDBG@QFDR@QD BNMUDQSDCSNUNKS@FDR@MCCHFHSHRDC@MC the resulting number must be important ancillary information must be VQHSSDMSNSGD%(32GD@CDQVHSGNTSVGHBG SGDC@S@AKNBJVNTKCMNSENQL@MHL@FD that can be processed further and scien SHjB@KKXHMSDQOQDSDC 3GDQDPTHQDLDMSRNMSGDOQDBHRHNM re peatability and invisibility of this process are quite tough: the shutter timings must be accurate to 1 millisecond; voltages HMFNEQD@CNTSRHFM@KRQDPTHQDRM@MN RDBNMCQDRNKTSHNM@MCHRCHEEDQDMSENQ@KK detector models; the analogue electronics RGNTKC@SLNRSLHMHL@KKXCDFQ@CDSGD NUDQR@LOKDSGHRRXRSDLMNHRD3GHRK@SSDQ S@RJHRLNQDD@RHKX@OOQDBH@SDCHEHSHRQD@K HRDCSG@SLNRSOQDRDMSC@XCDSDBSNQRFDM erate voltages as tiny as a few microvolts ODQOGNSNDKDBSQNM(MNQCDQSNRODDCTO C@S@SQ@MREDQO@Q@KKDKNTSOTSBG@MMDKR@QD TRDCATSMNMDRGNTKCFDMDQ@SD@MDBGN of its own signal in any of the other chan MDKR S@MXNMDLNLDMSRNESV@QD@MC G@QCV@QDDLADCCDCjQLV@QDLTRSJDDO tight control over all steps and give status QDONQSRSNSGDGHFGDQKDUDKBNMSQNKRNES V@QD(ERNLDSGHMFCNDRFNVQNMFCTDSN the failure of some general utility such as DKDBSQHB@KONVDQNQBNLOTSDQMDSVNQJR the user wants to be given a meaningful DQQNQLDRR@FDVGHBGHR@LTBGKDRRSQHUH@K S@RJSG@MHSjQRS@OOD@QR The present past: FIERA and IRACE KLNRS@KKBTQQDMSHMEQ@QDC+2/HMRSQT ments employ IRACE (InfraRed Array Con SQNK$KDBSQNMHBR,DXDQDS@KSN DWDBTSDSGD@ANUD@MCLNQDS@RJRVGHKD all optical instruments use FIERA (Fast Imager Electronic Readout Assembly;!DKDSHBDS@K3GDX@QDSGD5+3 RS@MC@QCCDSDBSNQBNMSQNKKDQR%NKKNVHMF (1 0BE%HMFDQDS@K@MC "$ 1DHRRSGDXVDQDSGDjQRSRS@MC@QC CDSDBSNQBNMSQNKKDQRCDUDKNODC@S$2. A recent analysis has shown their down SHLDVDHFGSDCQDKH@AHKHSXHMSGDjQRSCDB@CD NENODQ@SHNMNESGD5+3SNG@UDQD@BGDC@ KDUDKNE3GDBNMSQHATSHNMNESGD detector systems to the total observatory CNVMSHLDHRSGTRNMKX@ANTSNMDSDMSG 6GXMNSSGDMTRD(1 "$@MC%($1 forever? The answer is twofold and sim ple: the electronics of both FIERA and IRACE include an increasing number of electronic components that are no longer manufactured and cannot be replaced AXNSGDQO@QSR(M@CCHSHNMRNLDCDSDB SNQR@MCDRODBH@KKXSGNRDENQ@CU@MBDC applications such as adaptive DWBDDCHMFSGDRODBHjB@SHNMR@MCB@O@AHK "$3GDQDENQD RTBBDRRNQR@QDMDDCDC(MSDQDRSHMFKXSGD jqrs$2.hmrsqtldmssnaqhcfdsgdbnm ventional gap at 1 micron between opti B@K@MCHMEQ@QDCHMRSQTLDMSR7RGNNSDQ SNNJCDKHUDQXNESGDK@RS(1 "$@RVDKK@R SGDK@RS%($1 RXRSDLR The present future: NGC ESDQRNLDHMHSH@KCDA@SD@MCRTBBDRRETK SDRSRNE@""#VHSG(1 "$HSADB@LD BKD@QSG@SHSVNTKCOQNA@AKXMNSS@JDSVN separate systems to replace FIERA and IRACE and that the development of a uni jdcv@udkdmfsghmcdodmcdmsbnmsqnkkdq RGNTKCAD@SSDLOSDCJMNVM@RSGD-DV &DMDQ@KCDSDBSNQ"NMSQNKKDQ-&" dedicated NGC team was formed from RS@EE@S$2.RSVNCDSDBSNQCDO@QSLDMSR namely the Infrared Detector (1 "$VDQD@M@KXRDCQDPTHQDLDMSRENQ future detectors and applications were RNKHBHSDCS@JHMFMNSD@KRNNESGDOQ@BSHB@K MDDCRNESGD+2/.ARDQU@SNQX@MCENTQ generations of prototypes were G@UDADDML@CDSNSGD,42$OQNSNSXOD SN*,.22/'$1$@MCRNNM@KRNSN 9(,/.+RNSG@SHSHRSHLDKXSNOQDRDMSSGHR MDVfHMUHRHAKDANWtSNSGD+2/BNLLTMHSX NGC architecture Apart from the critical performance O@Q@LDSDQRNSGDQRSQNMFCDRHFMFN@KRNE SGDEQNMSDMCDKDBSQNMHBRHMBKTCDCLNCT K@QHSXRB@K@AHKHSX@MCBNLO@BSMDRR6GHKD both FIERA and IRACE boxes still host a 20 The Messenger 136 June 2009

%/& SNVGHBGSGDX@QD@CCQDRRDC,NRS connections with other parts of an NGC system are through two types of Transi SHNM!N@QCRVGHBGBNLOKDLDMSD@BG!@RHB@MCBG@MMDK BPTHRHSHNM!N@QC QDRODBSHUDKX Figure 1.

N@QCQHFGS@MCA@BJOK@MDLHCCKD G@MCETKNECHEEDQDMSDKDBSQNMHBAN@QCRSGHR CHUDQRHSXHRLTBGQDCTBDCHM-&"3GD RHLOKDRS-&"RXRSDL%HFTQDpBNMRHRSR NENMDRNB@KKDC!@RHB!

2 %/& connections with other parts of an NGC system are through two types of Transi QDRODBSHUDKX Figure CHUDQRHSXHRLTBGQDCTBDCHM-&"3GD RHLOKDRS-&"RXRSDL%HFTQDpBNMRHRSR handle up to four video input channels otherwise both types of boards can be combined in arbitrary quantities to form Figure PCI board 64-bit / 33 MHz Front-end electronics Front-end can Up to 6 boards be attached to instrument structure for passive HR@7HKHMW5HQSDW/QNp((%HDKC/QNFQ@LL@AKD &@SD QQ@X%/& QTMMHMFjQLV@QDOQN FQ@LLDCHM5'#+5'2("'@QCV@QD #DRBQHOSHNM+@MFT@FDVGDQD5'2("HR SGD@BQNMXLENQ5DQX'HFG2ODDC(MSD FQ@SDC"HQBTHS,TKSHOKDAN@QCR@QDC@HRX BG@HMDCSGQNTFGCHQDBS%/& SN%/& GHFGRODDCRDQH@KKHMJRHDSGDQDHRMN O@Q@KKDKATR"NLL@MCR@QDO@RRDCNM through the chain until they reach the Power supply (Remote) Detector cables "$RXRSDLRED@ STQDC4KSQ@2/ 1"A@RDC+NFHB@K"NMSQNK 4MHSR+"4RB@KKDC2+"4RQTMMHMFSGD KNVKDUDKRNESV@QDQDPTHQDCSNOQDO@QDSGD electronics and the detector for an obser U@SHNMSN@BPTHQDSGDQD@CNTSC@S@@MC OQDOQNBDRRSGDLHMLNQD@CU@MBDCQD@ CNTSRBGDLDR@RRDLAKDSGDLHMSN%(32 C@S@AKNBJRONRRHAKXONRSOQNBDRRSGD K@SSDQ@MCSQ@MREDQSGDQDRTKSHMFHL@FDRSN SGDHMRSQTLDMSVNQJRS@SHNMENQRTARD MNS@AKXVHSG(1 "$SGDQNKDNESGD2+"4R HRHM-&"RXRSDLRMNVS@JDMNUDQAX /"REQNLSGD#DKK/NVDQ$CFDE@LHKX 3GDX@QDJMNVM@R++"4RADB@TRDSGDX DLOKNXSGD+HMTWNODQ@SHMFRXRSDL CDCHB@SDCAHS,'Y/"(HMSDQE@BD B@QCG@MCKDRSGDC@S@HMFDRSHNM4OSN two PCI (Peripheral Computer Intercon MDBSAN@QCRB@MADTRDCODQ++"4 which can therefore support up to two -&"EQNMSDMCRVGDQD@R@OOKHB@SHNMR with very high data rates may require LNQDSG@MNMDA@BJDMCODQEQNMSDMC 3GDjAQDKHMJADSVDDMEQNMSDMCDKDBSQNM HBR@MCA@BJDMC++"4L@XADTOSN JLKNMF SNOKDUDKRXRSDLCH@FQ@LNE SGD-&"HRRGNVMHM%HFTQD ware engineers that the interfaces be as close as possible to the ones for "$@QDUDQXCHEEDQDMSNAUHNTRKX NMKXG@KENESGHRQDPTDRSBNTKCADETKjKKDCHE the interface for NGC were to be homoge MDNTR!DB@TRDSGD-&"G@QCV@QDBNM cept has inherited more from IRACE than EQNL%($1 SGD(1 "$HMSDQE@BDV@R@ M@STQ@KRS@QSHMFONHMS(ME@BS5+3HMEQ@QDC (IR) instrument software developers will not see much of a difference between (1 "$@MC-&" 19 Linux PC Full-duplex fiber ink 2.5 Gb/s %TMBSHNM@KKXSGD-&"BNMSQNKRNESV@QD interactions with the NGC electronics and HRTRDCAX@KK-&"@OOKHB@SHNMR!TSSGD The Messenger 136 June

3 next layer has to pay tribute to the fact that an observation in the optical typically consists of one integration with one read out while in the infrared most observa The optical case seemingly boils down to CDRSQTBSHUDKXATSSGDXODQLHSSGDATHKCTO of the signal with the number of readouts thereby drastically improving the data ing continues in the orthogonal states of a CCD exposure require differ DMSUNKS@FDRSNAD@OOKHDC+@RSATSMNS KD@RSSGDLTBGGHFGDQA@BJFQNTMCRHFM@K HM(1C@S@QDPTHQDRUDQXCHEEDQDMSBNTOKDC NODQ@SHMFRSQ@SDFHDRENQCDSDBSNQHMRSQT LDMS@MCSDKDRBNOD3GDQDENQDHSHRLNQD effective to develop two separate soft V@QDAQ@MBGDR3GDHMEQ@QDCNMDHR@F@HM UDQXRHLHK@QSNSGD(1 "$RNESV@QD!X BNMSQ@RSSGDNOSHB@KO@QSVGHKDSQXHMFSN ADMDjSL@WHL@KKXEQNLSGDDWODQHDMBD VHSG%($1 HR@M@KKMDVCDUDKNOLDMS 3GDQDENQDSGDQDV@REQDDCNLSNSDRS software concepts that had not previ NTRKXOK@XDC@L@INQQNKDHMSGD5+3DMUH QNMLDMS3GD@OOQN@BGBGNRDMHRSGD NMDNE@RS@SDL@BGHMDSNVGHBGSGDU@QH NTRRS@SDRNE@MNOSHB@KCDSDBSNQBNM SQNKKDQVHOHMFHMSDFQ@SHMFQD@CHMFDSB L@OUDQXVDKK(M@CCHSHNMSGDBNCDENQ@ state machine can be very effectively QDRSQTBSTQDCHEMDBDRR@QX3GHRHR@M@RRDS MNSSNADTMCDQDRSHL@SDC3GD-&" OQNIDBSV@RENQSTM@SDSG@S@RS@SDL@BGHMD approach had just been introduced to the 5+3BNMSQNKRNESV@QDSGDRNB@KKDC6NQJ RS@SHNM2NESV@QD%Q@LDVNQJ MCNKE@SN *@QA@M The NGC control software is an integral O@QSNESGD5+3BNMSQNKRNESV@QD@MC@R RTBGO@QSHBHO@SDRHMSGD@MMT@KQDKD@RD RBGDLDENKKNVHMFSGNQNTFGSDRSBXBKDR for which a comprehensive suite of dedi B@SDC@TSNL@SHBSNNKRV@RCDUDKNODC Ancillary functions and peripheral devices 3GDSGQDDETMC@LDMS@KNMCDSDBSNQRSDOR that eventually lead to the formation of an image are charge generation (by the urement of the voltage corresponding to SGD@BBTLTK@SDCBG@QFD3GDX@QD@B complished by the application of a set of SHLDCDODMCDMSUNKS@FDRHMO@QSVHSG@ QDRNKTSHNMNEpMR3GDRDRNB@KKDCQD@C NTSO@SSDQMR@QDDMB@ORTK@SDCHM-&" RODBHjBO@Q@LDSDQjKDR6GHKDENQDW@BS BGDBJHMFENQONRRHAKDBNMkHBSRHRCNMD much more effectively with a graphical DCHSNQ3GDSNNKENQSGDK@SSDQHRSGD)@U@ A@RDC!KTD6@UDO@BJ@FD2HMBD!KTD Wave is not directly embedded into the 5+3NODQ@SHNMHSHRMNSO@QSNESGD-&" BNMSQNKRNESV@QDATSHRCHRSQHATSDCVHSGHS The original signals provided by the detectors themselves are so feeble that SGDXLTRSADOQD@LOKHjDC@RD@QKX as possible so that they do not get mixed VHSGO@Q@RHSHBRHFM@KROHBJTOMNHRD emitted by other devices or the electrical L@HMR(MHMEQ@QDCRXRSDLRBQXNOQNNE "NLOKDLDMS@QX,DS@K.WHCD2DLHBNM CTBSNQ",.2A@RDCOQD@LOKHEDQR are integrated along with the detectors into the cryostat heads while for the NOSHB@KOQD@LOKHjDQR@QDKNB@SDCVHSGHM LNESGDQDRODBSHUDGD@CR2XMBGQNMH sation with external activities such as M2 BGNOOHMFHRRTOONQSDC 2HMBDCDSDBSNQR@QDCDKHB@SDCDUHBDR@MC HMRBHDMBDFQ@CDPT@KHSXUDQXDWODMRHUD the Transition Boards of the Basic Boards B@QQX@RDMRHSHUDQ@OHCQDRONMRDOQNSDB tion circuitry to prevent overvoltage caus HMF@MXC@L@FD+HJDVHRDE@HKTQDRNESGD input power or overheating within the NGC housing lead to automatic preventa SHUDRGTSCNVMRVGHBGB@MADQDONQSDCSN SGD+2/"DMSQ@K K@QL2XRSDL" 2 3GD-&"EQNMSDMCDKDBSQNMHBRHR@BBNL LNC@SDCHM@BTRSNLATHKSGNTRHMF%HF TQDp$@BGAN@QC@MCHSR@RRNBH@SDCSQ@M RHSHNMAN@QC@QDOKTFFDCA@BJSNA@BJHMSN Figure 3. Rear side of an NGC housing with connec SNQRENQONVDQB@AKD@MCBNNKHMFKHPTHCGNRDR3GD KRNUHRHAKD@QDSGD A@BJOK@MD@MCNMANSGRHCDRQ@HKRSNFTHCD@MC GNKCSGDAN@QCRNEVGHBGSGDQDL@XADTOSNRHW 22 The Messenger 136 June 2009

4 SGDBNQDNESGDGNTRHMF Although the heat dissipation per HMNQCDQSNLDDSSGDSHFGS5+3DMUHQNM peratures of equipment installed at the the baseline dimensions implied by these DQMRBHDMSHjBCDSDBSNQRHSHRjKKDCVHSG a number of commercial linear power RTOOKHDR@KSGNTFGSGDHQKNVDQDEjBHDMBX results in roughly doubling the must be different for optical and IR CDSDBSNQR%TQSGDQ@OOKHB@SHNMRODBHjB CHUDQRHjB@SHNMHRTMCDQCHRBTRRHNM %($1 BNMSQNKKDCNOSHB@KCDSDBSNQRXR SDLRHMBKTCD@FDMDQ@KOTQONRDGNTRD JDDOHMFTMHS/4+/.ENQRGTSSDQ@MC temperature control and pressure moni SNQHMF'NVDUDQPTHSD@EDVNEHSRBNLON MDMSR@QDMNKNMFDQ@U@HK@AKD(M-&" the shutter control is implemented on the!@rhb!n@qc3gd,42$oqnidbsg@r CDUDKNODCf3DD/DDtVGHBGHRA@RDCNM SGDBNLLDQBH@K)TLN(L@FNLTKSH channel process controller; as the name indicates it is used to handle TEmpera STQ$@MC/Q$RRTQ$.SGDQNOSHB@KCDSDBSNQ systems may use suitable adaptations but TeePee is not part of the NGC OQNIDBS3GDLTBGGHFGDQCDL@MCRNM temperature control of IR detectors (or TKSQ@RS@AKDHMRSQTLDMSRRTBG@RMDDCDC for exoplanet searches) can be met with BNLLDQBH@K+@JD2GNQDBNMSQNKKDQRVGHBG QD@BG@M@BBTQ@BXNE@EDVLHKKH*DKUHM -&".-&"ENQ@C@OSHUDNOSHBR The NGC described so far is also called 2BHDMSHjB-&"@RHSHRTRDCSNBNMSQNK CDSDBSNQRENQSGDQDBNQCHMFNERBHDMSHjB C@S@ MNSGDQHLONQS@MS@OOKHB@SHNM of digital detectors at modern observato NOSHBR2HMBDSGDjQRSSVN@OOKHB@SHNMR Q@QDKXQDPTHQDEQ@LDQ@SDR@ANUDp'Y@MC the interface to the Telescope Control 2XRSDLHRMNSSNNCDL@MCHMFBNLLDQBH@K detector controllers are more economical SG@M@MXBTRSNLHRDCCDUDKNOLDMS3GHR is not (yet) so for adaptive optics (and HMSDQEDQNLDSQX@OOKHB@SHNMRVGDQDEQ@LD Q@SDRNENQCDQp'YPTHBJKXADBNLD RTOQ@BNLLDQBH@KVGDMBNLAHMDCVHSG the requirement of negligible read and RXRSDLMNHRD An agreement was concluded between ESO and e2v technologies for the custom CDUDKNOLDMSNE@M+5HRHNMROKHSEQ@LD SQ@MREDQ""#VHSGpWpOHWDKR@MC DHFGSBG@MMDKR3GHR""#p#NVMHMF DS@KVHKKADSGDRS@MC@QCCDSDBSNQ ENQSGDENQSGBNLHMF5+3@C@OSHUDNOSHBR.V@UDEQNMSRDMRNQRRTBG@R& + "2(,42$&1 +' 6*(NQ2 7. BNMSQNKKDQ."@L&@BGDS@K3GD analogue part of the OCam electronics is being integrated with a specially cus tomised part of the digital electronics of -&"SNENQL-&". BNMRHCDQ@AKD extra challenge associated with the high data rates is that the sequencer must run at subnanosecond resolution and that the controller must be within centimetres NESGDCDSDBSNQVGDQDSGDBNMRSQ@HMSRNM UNKTLDL@RR@MCGD@SCHRRHO@SHNM@QD UDQXSHFGS ESDQQD@CNTSSGDC@S@HR directly and continuously transmitted via serial Front Panel Data Port (FPDP) to $2.R.QD@KSHLDBNLOTSDQRXRSDL 2/ 13 %DCQHFNDS@K Performance and other qualities NGC prototypes were extensively tested at all phases and with various G@QC@MCRNESV@QDQDKD@RDG@RQDPTHQDC RNLDATFjWDR!TSHMMNB@RDV@R@ RHFMHjB@MSQDCDRHFMMDBDRR@QX(SV@R very gratifying that the combination of two sets of expertise did not partly annihilate one another and cause previously TMJMNVMOQNAKDLR@RG@RADDMSGD DWODQHDMBDVHSGL@MXHMCTRSQXRB@KD BNNODQ@SHNMRNQLDQFDQR O@QSHBTK@QKX welcome early observation was that images read out with NGC do not show SGNRDRTROHBHNTRV@UXO@SSDQMRVGHBG mostly add little to the effective overall MNHRDATS@QDUHRT@KKXPTHSDHQQHS@SHMF Very comprehensive tests were run with SGDjQRSRBHDMBDFQ@CDCDSDBSNQENQ *,.2@'@V@HH1&CDUHBDEQNL3DKD CXMD(L@FHMF2DMRNQR3GDMNHRDGHRSN FQ@LHM%HFTQDpCDLNMRSQ@SDR@QD@C MNHRDNEDQNNSLD@MRPT@QDQLR VGHBGV@R@BGHDUDCVHSGRHLOKDCNTAKD correlated sampling and is the lowest noise ever reported for such a detector BE%HMFDQDS@K#DS@HKDCSDRSR were also performed with the prototype CDSDBSNQRXRSDLENQ,42$VGHBG DLOKNXR@JpWpJ""#CDUHBD EQNLDU SpJOHWR@QD@CMNHRD@R KNV@RDV@R@BGHDUDC4RHMF@KK ENTQONQSRSGDDMSHQD@QQ@XB@MADQD@C VHSGHMpRDBNMCR@MC@S@QD@CMNHRD NED MDWBDKKDMSMNMKHMD@QHSXNE V@RLD@RTQDC While system noise is the most decisive jftqdneldqhsenq@mxcdsdbsnqbnmsqnkkdq there are many more advantages to the NGC system: Signals can be sampled once or several SHLDRHMSGD@M@KNFTD@RVDKK@RCHFHS@K CNL@HM Much higher bias voltages are sup (Silicon becomes increasingly more transparent with wavelengths into the MD@Q(1 Gain and bandwidth of the optical OQD@LOKHjDQ@QDANSGOQNFQ@LL@AKDHM RSDORODQLHSSHMFRDMRHSHUDL@SBGHMF of NGC to various types of CCDs and QD@CNTSLNCDR An NGC system can go online within ITRSRDBNMCRKNMFDQHELNQDBNMjFT Q@SHNMBGDBJR@QDODQENQLDC@MC CDSDBSNQDMFHMDDQR@OOQDBH@SDSG@SHM The Messenger 136 June 2009

5 start after having changed voltages so that test sequences can be executed VHSGGHFGSHLDDEjBHDMBX Noise histogram with single DCS KMOS Science 1 H2RG #184 l6ghkd@%($1 EQNMSDMCVHSGENTQUHCDN BG@MMDKRBNLOQHRDRDKDBSQNMHB BNLONMDMSRNEVGHBG@QDCHEEDQDMS SGDRDMTLADQR@QD@MC QDRODBSHUDKXENQ-&"RNSG@SO@QSROQN BTQDLDMS@MCRSNBJJDDOHMF@QDLTBG RHLOKHjDC.TSKNNJ NGC will be the standard detector con SQNKKDQENQETSTQD+2/HMRSQTLDMSRQD F@QCKDRRNEV@UDKDMFSG%NQSGDDWHRSHMF spare parts to sustain the unrestricted functioning of all systems throughout SGDKHEDSHLDRNESGDHQGNRSHMRSQTLDMSR "$-&"VHKKAD@ KHMDQDOK@BD@AKDTMHS@SSGDNARDQU@SNQX Because of the increasingly specialised demands from both new detectors and projects to be realised on one common OK@SENQLATSVHSG@LHMHLTLMTLADQ NE@BST@KKXTRDCU@QH@MSR%NQHMRS@MBD MDV,'Y@M@KNFTDSNCHFHS@KBNMUDQS ers (ADCs) are being tested for their suitability to replace the current default,'y #"RENQGHFGDQRODDC@OOKHB@ SHNMR RODBH@KGHFGRODDCp,'Y CDUDKNOLDMSHR@KRNTMCDQV@X2NESV@QD ENQRS@MC@QCHRDCKNVKDUDKONRSOQNBDRRHMF NEC@S@DF@UDQ@FHMFNEEQ@LDRNQ AH@RBNQQDBSHNMNMSGD++"4HRTMCDQ CDUDKNOLDMS-&"VHKKBNMSHMTDSNRDQUD as the basis for close collaborations between the Infrared Detector Depart LDMS@MCSGD.OSHB@K#DSDBSNQ3D@L@MC a joint NGC production line has been RDSTO$WSQ@ONK@SHNMEQNLSGDDWODQHDMBD ation NGC will be needed to support the $$+3NODQ@SHNMRCTDSNRS@QSHM By then many detectors may come with SGDHQNVMNMNQMD@QBGHOBNMSQNKKDQR Number of Pixels BHQBTHSR!TSSGDXVHKKMDDC@BNLLNM $$+3TLAQDKK@SNHMSDQE@BDSNSGDNUDQ@KK $$+3BNMSQNKRXRSDL@MCNODQ@SHNMR O@Q@CHFL CCHSHNM@KSDBGMHB@KHMENQL@SHNMHMBKTC ing numerous downloadable documents is available on the NGC home page 1 The section General contains pdf ver sions of a number of detailed presenta tions about various aspects of NGC DMPTHQHDR@MCEDDCA@BJ@SMFBDRNNQF BJMNVKDCFDLDMSR SHNM@MCDWDBTSHNMNEDMCKDRROQNBTQDLDMSKHRSR!KTD6@UDV@RCDUDKNODCAX KDRR@MCQN!NQSNKTRRH,@QJ#NVMHMF@MC1NK@MC1DHRRGDKODCVHSGTRDETK QDPTHQDLDMSR@MCEDDCA@BJ1NK@MC1DHRRHRSGDKD@C engineer for the development of TeePee; he also provided some of the performance measurements Readout Noise (e ) Figure 4.-NHRDGHRSNFQ@LENQRHMFKDCNTAKD BNQQDK@SDCQD@CNTSNE@*pWp*'F"C3DRTARSQ@SD removed λ c ppp L'@V@HH1&@QQ@X*,.2 VHSG""#R+THFH MCNKE@SNF@UDFDMDQNTRKXNEGHR experience with state machines built up with the CDUDKNOLDMSNESGD5+36NQJRS@SHNM2NESV@QD %Q@LDVNQJ62%2DA@RSH@M#DHQHDR@MC$QHB,XKKDQ prepared the CCD test bench of the Optical Detector Team for NGC and executed quite a number of ""#SDRSR3GDC@S@A@RDENQSGDQDKH@AHKHSX@M@KXRHRNE FIERA and IRACE was established by Nicolas '@CC@C References MCNKE@SN+*@QA@M12/($!DKDSHB)6DS@K 22+ #NVMHMF,#DS@K2/($ %DCQHFN$DS@K2/($ %HMFDQ&,DXDQ,,NNQVNNC %, 2/($ %HMFDQ&DS@KHM RSQNOGXRHBR#DSDBSNQ 6NQJRGNO-HBDHMOQDRR &@BG)+DS@KHM2BHDMSHjB#DSDBSNQRENQ RSQNMNLX,DXDQp,DS@K2/($ 1DHRR12/($ +HMJR 1 GSSOVVVDRNNQFOQNIDBSRMFB 24 The Messenger 136 June 2009

Optical Detector Systems

1 / 13 Optical Detector Systems Dietrich Baade & Optical Detector Team (ODT) Instrumentation Division The ODT Themes Support of La Silla Paranal regular counseling and trouble shooting (e.g., NAOS, WFI)