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VIMOS User's Manual

1. Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 12 27 28 29 312 50 MM Figure 3 VIMOS optical layout one channel only Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 13 AER Folding a FET NR Mirrors v AG TA E Figure 4 VIMOS opto mechanical layout top view Figure 5 Overall VIMOS view CAD view Word Windows 2000 Fichier vimos users manual v I LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 Date 24 Oct 02 page 14 2 3 Imaging Mode The characteristics of the VIMOS imaging mode are summarized in Table 4 and are described in details in Section 4 Table 4 Imaging characteristics amp performances Configuration Filters inserted in the beams Field AxTx8 corresponding CCD area 2048x2350 pix slight vignetting on the corners out to the 8 field Sampling 0 205 arcsec pixel U BVRIz standard set Limiting magnitudes in 1h V 27 7 I 26 6 50 detection for a point source Ag coated UT V 26 5 I 25 4 56 detection in 3 for a galaxy 2 4 Multi slit Spectroscopy Mode The characteristics of the VIMOS Multi slit spectroscopy mode are summarized in Table 5 and are described in details in Section 6 Word Windows 2000 Fichier vimos users manual v1 LAS r f VI
2. Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F He Exposure time Seconds of exposure for Helium Lamp 1 No He lamp Ne Exposure time Seconds of exposure for Helium Lamp 1 No Ne lamp Ar Exposure time Seconds of exposure for Helium Lamp 1 No Ar lamp Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name root name for resulting files Mask shutters cannot be used with the instrument in IFU mode This means that orders superposition will not be cut out from calibration images 9 3 3 4 VIMOS ifu cal photom Template to acquire spectro photometric calibration exposures in IFU mode Table 36 parameters for VIMOS ifu cal photom Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Wheel Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution IFU Shutter Shu
3. At the end the pointing will have been moved along a square of 2 arcseconds side If Number of exposures is larger than the number of offsets in X or in Y the sequence of offset will be restarted Word Windows 2000 Fichier vimos users manual v I Example List of Offset in X 0 1 List of Offset in Y 0 1 Number of exposures 5 CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIRr f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date The following offsets will be applied Exposure N ro X shift Y shift Xtotal Ytotal shift shift 1 0 0 0 0 2 1 1 1 1 3 0 0 1 1 4 1 1 2 2 5 0 0 2 2 Table 23 parameters for VIMOS ifu obs Jitter Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F Readout Mode CCD read out mode fast medium slow Return To Origin Defines whether telescope should go back to the original position at the end of the sequence of exposures Number of exposures Number of exposures to be made Offset Coordinates Offs
4. Table 18 parameters for VIMOS img obs Jiitter Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode Fast Medium Slow Filter Name Photometric filter to be used U B V R Lz Return To Origin Defines wether telescope should go back to the original position ate the end of the sequence of exposures Number of exposures Number of exposures to be made Offset Ccordinates Offset can be given in pixels or in arcsec List of Offset in X List of offsets in X or Dec direction List of Offset in Y List of offsets in Y or RA direction Exposure Name Root name for resulting files 9 2 1 3 VIMOS img obs Autojitter Template to observe a field in Direct Imaging Mode slightly shifting the pointing from one exposure to the next The offset from one exposure to the next are automatically computed in a random manner within a box of side Jitter Box Width Each exposure will be Exposure time seconds long Table 19 parameters for VIMOS img obs Autojiitter Parameter Name Descritpion Exposure time Exposure time for one observation in seconds Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D AS
5. cscssseseceseeecececeeeceesceeececeseeeseceseeesececeeeceeeeseeseeeseeeseeeceseceeeseeeseeeseeesececeeesesececeseceseceseserecenececeseceeeseceseeeseds 31 65 GAHBRATION iset edited ete ie 31 6 6 DATA PROCESSING cccccccecsssssseceeececsesssuececececsesuueseeeceesensuasaececececsesusaeeeeececeesuaeseesceeseseaaueecececeeaaeseseceseaueaaeseeseeesensaaees 32 To INTEGRAL FIELD SPECTROSCOPY eseeesevsvessvevneensnsvsssnsnnvennnnnesensnneessnsvnvsnnnnenssnsnnvessnnnesennnneesensnnnesnnnnsennnnvnsennnnvenee 32 pa A 32 192 PERFORMANCE a iaa 32 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 4 7 3 OBSERVATION PREPARATION aenieei veto evt ce ener etre Co ev ee eere eei or ee SE re ee E oe ER ee s Ee LE LEE EUER Ee Pea e o dgeceeseaveesdaacudenss 32 ye Ee iunieiseUn s PTE 32 TS CALIBRATION PP L E 33 TO DATA PROCESSING rame rnv ERE ER ROLE ie REG reir eee heade Re 33 8 REFERENCE INFORMA TION inci vesedescsscusteesvssssasnscevesesdsedwecoucosvossescunsccsvessccevescesedsseveetenceesocosvesvesseveuescseseteeasdeesvessonsenes 33 elt FETERE 33 82 GRISMS ste SEN 39 83 DETECTORS MEO 39 S4 COH BH hc ea a er SB eee A E 39 8 5 ARC CALIBRATION LINES eerrvrvrerervrerererererererererererevererereverevereverererererevereveveveveverevereverereve
6. at the end of the sequence of exposures Number of exposures Number of exposures to be made Exposure Name Root name for resulting files Word Windows 2000 manual v1 Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 54 9 3 Calibration Templates Calibration Templates are those to be used for routinely performed scientific calibrations like biases darks etc 9 3 1 Imaging Mode 9 3 1 1 VIMOS img cal Dark Template to acquire a series of darks or biases exposures Table 25 parameters for VIMOS img cal Dark Parameter Name Descritpion X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Number of Exposures Number of exposures to be made Exposure Name root name for resulting files List of exposure times esposure time for each of the exposures The List of exposure Times parameter defines the exposure time for each exposure If exposure time is Zero a bias is acquired Example 1 Number of Exposures 6 List of exposure Times 0 0 60 300 900 3600 Will perform first a series of 2 biases exp time 0 and then a series of 4 darks lasting 1 5 15 and 60 minutes each Example 2 Number of Exposures 6 List of exposure Times 0 Will perform a serie of 6 biases exp t
7. Declination Equinox and Epoch Note that the pointing coordinates in the target description will correspond to the center of VIMOS FOV and the four images will correspond to the four quadrants around this point Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page If the preset option is selected the acquisition sequence will move the telescope to the pointing position taking into account any desired additional offset otherwise it is assumed that the telescope is already at the pointing position An image of the field is acquired and the user may offset the telescope interactively via image display and cursor to better suit his her needs second image is acquired for checking The acquisition offsetting sequence can be iterated at user s wish 9 1 2 IFU Mode 9 1 2 1 VIMOS ifu acq Preset This template inserts IFU masks for this operation a rotation of the instrument in a pre determined position is needed moves the telescope to the Target position offests to IFU position acquires guiding star and starts Autoguiding No check image is acquired Note insertion of IFU masks with rotation of instrument is a slow operation which requires about 2 minutes TBV Table 14 parameters for VIMOS ifu acq Preset Parameter Name Description Guiding lambda Wavelength for guiding Alpha Offset Addit
8. Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 39 6 2 Grisms Table 11 Grisms properties Grism LR1 LR2 HRI1 HR2 HR3 6 LowRed LowBlue HigRed HigBlu HigOra Interm Dimensions Cm 17x16x3 17x16x3 17x16x18 17x16x18 17x16x18 17x16x6 Beam Cm 14 14 glass BK7 resin glass index resin index prism angle blaze angle grooves mm central blaze rec dispers A i 171 resol R 2520 2150 580 MR catalogue 3553750 E 3553570 e 3553570 3563630 central range 550 950 630 870 520 760 500 1000 right range 3 5 550 950 570 805 463 703 500 950 left range 3 57 550 950 690 930 577 817 500 1000 Multiplex number of spectra layers coating u MgF2 tilt shadow Max vignetting grating 0 0 1 0 0 0 0 0 1 vignetting camera 0 0 0 0 0 0 0 0 0 order sorting GG475 NO GG435 Thick O S Fil 12mm 12mm Location of O S Feu 8 3 Detectors 8 4 OH lines Word Windows 2000 Fichier vimos users manual v I 10 5x101 6000 7000 8000 8000 10 Wavelength angstroms Figure 29 sky spectrum in CCD counts 1440 sec integration 1 arcsec slit LRRED grism 8 5 Arc Calibration lines CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 24 Oct 02 page 40 6000 7000 8000 000 10 Wavelength angstroms
9. Figure 30 sky spectrum flux calibrated Fv Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 41 e m i 2e T T kl um H Da 1 5 B Bp A u zia a m go AN m 7 S rild sf Cun Es i 89585 p aot magi p o D m m mi no d Qi el amp Goth 0 ang d S o mut ru c em LA nu mu H nn n HH u 1 mo 4 drm 4 2444 A aa 0 5 6000 TOOO 5000 9000 Wavelength Angstrom Figure 31 He Ar arc spectrum with the LRRed grism Hel 5875 6 Ar 7723 8 blend Ar 8012 blend Ar 8110 blend Td c Do q co T Ar 6965 4 Hel 7281 3 Hel 7383 98 6000 6500 7000 7500 8000 Wavelength Angstrom Figure 32 He Ar spectrum with the HROra grism Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 42 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 9 User s Template description 9 1 Acquisition Templates Acquisition Templates allow to point the telescope at the desired position A check image is NOT necessarily acquired in all of them 9 1 1 Imaging Mode 9 1 1 1 VIMOS img acq Preset This template moves the telescope to the Target position acquires guiding star and starts Autoguidi
10. High resolution Low Red or orange Medium Resolution Cabinet 1 Slot Number Position of mask in Cabinet 1 Cabinet 2 Slot Number Position of mask in Cabinet 2 Cabinet 3 Slot Number Position of mask in Cabinet 3 Cabinet 4 Slot Number Position of mask in Cabinet 4 He Exposure time Seconds of exposure for Helium Lamp 1 No He lamp Word Windows 2000 manual v I Fichier vimos users LAS r f 58 Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page Ne Exposure time Seconds of exposure for Helium Lamp 1 No Ne lamp Ar Exposure time Seconds of exposure for Helium Lamp 1 No Ar lamp Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name root name for resulting files ADP File 1 Name of ADP File for Quadrant 1 ADP File 2 Name of ADP File for Quadrant 2 ADP File 3 Name of ADP File for Quadrant 3 ADP File 4 Name of ADP File for Quadrant 4 ADM File 1 Name of ADM File for Quadrant 1 ADM File 2 Name of ADM File for Quadrant 2 ADM File 3 Name of ADM File for Quadrant 3 ADM File 4 Name of ADM File for Quadrant 4 Mask 1 ID Mask ID of Quadrant 1 mask Mask 2 ID Mask ID of Quadrant 2 mask Mask 3 ID Mask ID of Quadrant 3 mask Mask 4 ID Mask ID of Quadrant 4 mask ADF File 1 4 contain the files for building the masks as generated by the vmm
11. instrument control panel Middle detector control panel Right telescope control panel 2 8 Real Time Display The RTD allows to interact with images as they are readout by the detectors electronics The VIMOS RTD is split in 4 panels each displaying one image provided by one channel The RTD provides various tools to display and analyse the images pan zoom cut capabilities cursor readout FWHM measurements statistics on selected regions Word Windows 2000 Fichier vimos users manual v 1 LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 19 El Vimos Real Time Image Display version 2 40 File View Graphics Real time x 228 v a8 j Value sso ra 051929599 dec 41271970 Low TN High rime Auto Set Cut Levels 2 81 gt 1 B1 302 4 B2 FENAE Camera activity i image window Figure 8 VIMOS Real Time Display 2 9 Calibrations VIMOS calibrations are of three kinds flat field calibration imaging MOS and IFS wavelength calibration MOS and IFS and photometric imaging MOS and IFS Flat field and wavelength calibrations can be performed using the VIMOS calibration unit 2 quartz lamps are available for imaging and spectroscopic flats resp and He Ne Ar lamps are available for spectroscopic wavelength calibrations 2 10 Overheads The allocated time on VLT instruments
12. 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page Guiding lambda Wavelength for guiding ADP File 1 Aperture Definition File for quadrant 1 ADP File 2 Aperture Definition File for quadrant 2 ADP File 3 Aperture Definition File for quadrant 3 ADP File 4 Aperture Definition File for quadrant 4 ADM File 1 Name of ADM File for Quadrant 1 ADM File 2 Name of ADM File for Quadrant 2 ADM File 3 Name of ADM File for Quadrant 3 ADM File 4 Name of ADM File for Quadrant 4 Mask 1 ID Mask ID of Quadrant 1 mask Mask 2 ID Mask ID of Quadrant 2 mask Mask 3 ID Mask ID of Quadrant 3 mask Mask 4 ID Mask ID of Quadrant 4 mask Readout Mode CCD read out mode fast medium slow Filter Name Photometric filter to be used U B V R Lz Preset Telescope Move to desired position Y N ADP File 1 4 contain the files for building the masks as generated by the vmmps software cf AD 5 The parameters indicated as shaded are normally NOT to be filled in by the user but by the OHS cf RD 4 and will not appear in P2PP Note the pointing coordinates are NOT taken from the target description but from the adp files themselves Nevertheless target description must be filled with meaningfull Epoch and Equinox at least If the Preset option is selected the telescope is preset to pointing coordinates Autoguide is started in any case An image with the spectroscopic mask is acquired By comparing the position of the Reference Objects as from ADP file
13. 04 01 14 E 102851 000 04 01 12 000194923 024 04 01 12 D 000175857 2152 04 01 12 E 000771553 960 04 01 11 000149377 336 04 01 12 f 000201005 016 04 01 12 A 000252691 144 04 01 11 000305291 TI6 DIE 3 00012665 i Query results select object double click label object scroll Figure 14 vmmps catalog panel Word Windows 2000 Fichier vimos users manual v1 File Edit Options Object Name J a 22 59 38 435 Min Radius 0 0 Max Objects 10000 Select Area Set From Image CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 Equinox 72000 8 00 04 30 75 Max Radius 5 32 23 59 40 26856 23 59 35 14219 23 58 53 TORSO 23 59 42 19541 23 59 34 24805 23 59 26 22070 23 59 51 54785 23 59 42 71184 23 59 33 85254 23 59 25 53223 29 59 41 29595 23 59 31 19385 Search Results 189 00 C4 01 94000 00 C1 15 02001 00 C1 00 C1 00 C1 00 C1 00 C1 00 C1 D0 C1 00 C1 D0 C1 00 01 03 54000 09 42000 13 09000 09 48000 20 13000 20 07000 21 44001 19 84000 27 50001 27 38000 883 526 1037 19 1368 25 54 RAR 57 852 811 1477 45 2064 34 213 086 858 6 1506 65 2114 43 966 512 1100 88 Figure 15 vmmps slit panel LAS r f Issue 1 0 R v 0 0 page 30 Figure 16 Display of slits selected by vmmps SPOC with objects location and spectra extent Word Windows 2000 manu
14. 1 vmlmaDummy 1 fits 1 Graphics Go Data Servers VIMOS MPS LA Equinox Min Max Bitpix Low High bias 6753 34 04 05 1 7 36 1036 0 1197 0 02 27 20 125 J2000 1 17548e 38 60105 9 32 5663 26 n 06 56 Auto Set Cut Levels a Gnas Sa Zi z S z uj DU n image l select object scroll image measure WCS Control gt select region Figure 12 vmmps main panel Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 29 vmmps_cross 1 Input catalog rea bottinidatifastrocati cat VIMOS catalog rea bottini dati vimoscat bd VIMOS image rea bottini dati vimosima fits Output catalog rea bottini dati astrocatl1 vm cat Matching tolerance arcsec Number of parameters to fit Sigma clipping for residuals Number of iterations Output of CROSS program nmatch 373 nstars 373 rms 0 879 arcsec nmatch 373 nstars 373 rms 0 879 arcsec nmatch 373 nstars 373 E vmCatDummy1 cat 1 E File Edit Options VIMOS MPS Figure 13 vmmps cross correlation panel Search Options Object Name J Equinox 2000 a J J Min Radius Ja 0 Max Radius 10 0 Max Objects 10000 Select Area Set From Image Tead S68 04 OL E 216 04 01 15 E 0 0894515 624
15. LAS r f Issue 1 0 R v 0 0 Date 24 Oct 02 page 18 CNRS LABORATOIRE D ASTRONOMIE SPATIALE File Options Commands Tools VIMOS Cag Tyne Tech Expo File Exp Id 98 Exposure Count Down STATE SUBSTATE SCTENCE Focus IMAGE 00 00 00 ONLINE Expo Name New Data Mpe ETERNO ADM flo A Sa oe si peorm r oos fi POSweTine IDLE Phase Finished Requestor MOS HOS E wcs J Seq Naming 16 R 5 W Archive Header unu W Save exposure file ICS omme me ucu sm pcs ome wssm omne vs sm TCS Unknow Unknown Functions calibration Readout Mode Preset Offsets NO TCS Vimos 225 LL 1x1 Low Galn medium IFU devices ain Ron Speed medium LR_blue NX 2048 J Elongator Off ny 4096 Allowed X t ni 4 Shutter off E binning y 1 Exposure type Normal FOMP mode ir eS TU me No Telescope Auto Y bin ee FOCUS mode norepeat w repeat mal Period see Times Li Exposure Time sec Een 18 15 15 15 Te sTo Jen ej sa Comments Action Log Disk Space y Exposure History 02 PROFILE command received OS PROFILE finished 7 i r CLEAR i SETUP START PAUSE RESUME ABORT END CANCEL i Figure 7 VIMOS OS graphical user interface Left
16. does include overheads in addition to the open shutter time Overheads with VIMOS are mainly Instrument configuration time this is the time required to change the configuration of the instrument e g from imaging mode to MOS mode that is to move the respective elements required mask filters grisms IFU The configuration time is at maximum 2 min 2 5 min 3 5 min for filters grisms masks respectively Moving filters and grisms will take 2 5 min maximum moving filters and masks will take 3 5 min maximum Changing from imaging or MOS mode to IFU mode or back takes 3 5 minutes Word Windows 2000 Fichier vimos users manual v I LAS r f VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date CNRS LABORATOIRE D ASTRONOMIE SPATIALE Detector readout this is the time required to readout the 4 detectors to transfer data on disc and to display the images with RTD Telescope set up this is the time required to move point and guide the telescope as well as to lock the active mirror control loop Since VIMOS occupies a large fraction of the telescope FOV the guiding field accessible without vignetting of the VIMOS FOV is restricted The telescope operator observer has to exercise great care in visually selecting a guide star with no or minimum vignetting This procedure can take up to 5 minutes Mask set up on sky this operation is necessary to ensure that the instrument is positioned in such a way t
17. exposures Number of exposures to be made Exposure Name root name for resulting files Note masks related parameters ADP fle ADM files Slot number etc are NEVER defined within the observation template but ONLY in the acquisition or calibration template It is therefore compulsory to define an OB for each mask set 9 2 2 2 VIMOS mos obs Jitter Template to observe a field in Mos Mode slightly shifting the pointing from one exposure to the next along the slit The offset from one exposure to the next is given by the parameter List of Offsets Offset are in arcseconds and are always incremental from the previous position Offsets are to be read as offsets of THE OBJECT ON THE IMAGE i e the Telescope will move in the other direction Each exposure will be Exposure time seconds long Example List of Offset 0 1 2 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page Number of exposures 3 Exposure N ro shift Total shift 1 0 0 1 1 3 2 1 At the end the pointing will have been moved along a the slit of 1 arcseconds around the center If Number of exposures is larger than the number of offsets in X or in Y the sequence of offsets will be restarted Example List of Offset 0 1 Number of exposures 5 The following offsets will be applied Exp
18. help eso org in Garching 7 Word Windows 2000 Fichier vimos users manual v1 CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA 1 0 R v Issue Date 2 VIMOS the Visible Multi Object Spectrograph 2 1 VIMOS observing modes overview Direct Imaging Direct imaging is aimed at providing images suitable for accurate astrometry and photometry The astrometric and photometric catalogs obtained from these images may be used for Multi Object Spectroscopy Table 1 VIMOS Operation Modes VIMOS OPERATION MODES Maintenance Mode Table 2 VIMOS Observing Modes VIMOS OBSERVING MODES Long slit and Multi Object Spectroscopy Long Slit and Multi Object Spectroscopy Slit spectroscopy is aimed at providing spectra of one or a list of objects selected from user 24 Oct 02 0 0 page criteria Multi object spectroscopy of a list of targets is done with the following sequence Direct imaging Calibrations Astrometry and photometry produce source catalogs Mask preparation design of mask with slits layout and size Mask manufacture and installation at focal plane Spectroscopic observations Integral Field Spectroscopy Integral field spectroscopy aims to obtain spectra of a contiguous area of sky Integral field spectroscopy can be done with or without prior knowledge of the photometry of sources in the field With the VIMOS IFU coordinates of objects in the field may be kno
19. into account the priority ranking set by the OPC VIMOS MOS observations require the preliminary acquisition of pre images images of the fields to be observed These pre images are used to identify targets and prepare masks This cannot be done during the same night as the observations pre images are taken either a few weeks ahead of time service mode or the night before at the latest visitor mode 4 Observing with the VLT and VIMOS 4 1 Telescope and instrument focus Two types of focussing operations are involved for VIMOS observations because two focal planes are involved the entrance or slit mask focal plane located at the telescope focal plane and the CCD focal plane located at the output focal plane of VIMOS Observers should not need to worry about focussing as this is taken care of at the telescope and instrument levels by dedicated procedures However they need to be aware of this specificity to understand standard operations The image quality delivered by VIMOS is better than the specification as shown in Figure 9 The focal plane of VIMOS is not strictly flat because of the complex optical elements involved This results in slight focus variations across the field which translate in a slightly variable PSF from center to edge This is shown in Figure 10 22 Word Windows 2000 Fichier vimos users manual v1 LAS r f 1 0 R v 0 0 Issue CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oc
20. nous auge aeuo uev aunt uev ee oue uen ue aus eue eo ve ue ve eoe sun tx 23 5 DIRECT nien Le 24 Dil AAA 24 5 2 PERFORMANCES SSA 24 5 3 OBSERVATION PREPARATION vrerevvrerererererererererevevererererererererererevererevevereverevevevereveveverevevevevereveveveveveveveveveveveveveveveveenvevevere 24 SI MEQUE UDUMRCTKRIM 25 S C ID UMORE M 25 5 60 DATA PROCESSING i cirea enken dri ERE NR ERES 25 6 MUETESLIT SPECTROSCOPY a ereeee ee ec oto e rores eoe E een e eue te Fea npo sere Eve detente TR Une E Ve eno Oe debate Ve ues Vos Vae aee eae tete secte 25 0 1 OVERVIEW 25 6 2 IAN AN 25 6 3 OBSERVATION PREPARATION rrrersrnannrvrnrnereensnnrnnnensseenannrnnnrnssrenenennrsensnesnenennnsnnsnssnnnannrnnnenenennannnnnsensnennanennnsensnensennnnnvenene 25 6 4 MASK DESIGN AND MANUFACTURING suisse enne nhnhnnnn eset eet nna sess sten te tesa ss esses ete te ande sese esee tede dass seen sette nane seen ette tena 26 64 1 Prezimage catalog ta rte bee tede etie ipee eade bnt E aba e oe de E 26 6 4 2 Case I no pre existing external user catalog inner 26 6 4 3 Case 2 cross correlation of pre image catalog with pre existing external user catalog 26 ULT MEUS cA ERREUR 26 6 4 5 Display slit object selection nee 27 6 4 6 Mask manufacturing mask tracker seine 27 OBSERVING SEQUENCE
21. once the subsystems are started from OS panel click on Menu Tools ICS Control Panel then from ICS panel click on menu Tests More information on Devices Simulat StopSim and choose via the radio buttons the devices you want to use in normal mode Currently known problems and fixes 1 Grisms support collision inside the optical box When the instrument is close to a vertical position at around positions 116 or 64 grisms in channels 2 and 4 are colliding with the protruding support of the grism body reference pins This is due to a tilt of the grism body slightly out of the foreseen mechanical limits needed to align the grism dispersion with the CCD columns Waiting for a simple hardware fix please use the following workaround Workaround the most likely situation is that you are setup on a mask the reference objects are in the holes and you are ready to take spectroscopy Make sure that the template is paused after the mask acquisition part before going to the spectroscopy part Check the rotation angle of the instrument if within 30 of 116 or 64 ask the telescope operator to rotate the instrument to 26 Go to OS panel and move the grisms to the needed position Ask the operator to move back to the correct angle to produce a sky position angle of 0 Continue the template for spectroscopy By using the instrument rotation capability you keep the guider adapter locked on the correct sky position and y
22. series each consisting of one bias exp time 0 and two darks 9 3 2 2 VIMOS mos cal Flat Template to acquire a series of Flat field exposures in MOS mode Note that each Flat field must be acquired with the appropriate mask i e that used for the scientific exposure Table 30 parameters for VIMOS mos cal Flat Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Word Windows 2000 Fichier vimos users manual v I CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date 57 Low Red or orange Medium Resolution Calibration Lamp Name Name of the calibration Lamp to be used Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name Root name for resulting files ADP File 1 Name of ADP File for Quadrant 1 ADP File 2 Name of ADP File for Quadrant 2 ADP File 3 Name of ADP File for Quadrant 3 ADP File 4 Name of ADP File for Quadrant 4 ADM File 1 Name of ADM File for Quadrant 1 ADM File 2 Name of ADM File for Quadrant 2 ADM File 3 Name of ADM File for Quadrant 3 ADM File 4 Name of ADM File for Quadrant
23. series of one bias exp time 0 and two darks 9 3 3 2 VIMOS ifu cal Flat Template to acquire a Flat field with halogen lamps in IFU mode Table 34 parameters for VIMOS ifu cal Flat Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 61 Calibration Lamp Name of the calibration Lamp to be used Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name root name for resulting files Mask shutters cannot be used with the instrument in IFU mode This means that orders superposition will not be cut out from calibration images 9 3 3 3 VIMOS ifu cal arc Template to acquire a wavelength calibration image in IFU mode NOTE this template is by no means different from the analogous one for MOS case The sequence of expose pause continue based on lamps exposure times applies here also Table 35 parameters for VIMOS ifu cal arc
24. 000 manual v1 Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 3 3 Phase II proposal preparation P2PP After observers are awarded telescope time either in service or visitor mode they must prepare their Observation blocks with P2PP In visitor mode P2PP can be used on Paranal a couple of days before the run Help will be provided on site by the operation staff Service observers must prepare their OBs according to the information provided in this manual template description section Erreur Source du renvoi introuvable as well as in the P2PP information http www eso org observing p2pp 3 4 Visitor and service modes Visitors should arrive on Paranal 2 days ahead of their observing run so as to prepare their OBs They receive support from the Paranal science operations team Users are requested to read the P2PP and VIMOS Users Manuals before arriving During the night the users do not have direct interaction with the instrument and the telescope The execution of their OBs is undertaken by the Support Astronomer on duty and or the Telescope and Instrument Operator In service mode OBs must be prepared in advance using P2PP A deadline is set by the VLT operations Passed this deadline interaction with P2PP and change of OBs is discouraged OBs are placed in the OB repository they are executed when the observations conditions are met and taking
25. 4 Mask 1 ID Mask ID of Quadrant 1 mask Mask 2 ID Mask ID of Quadrant 2 mask Mask 3 ID Mask ID of Quadrant 3 mask Mask 4 ID Mask ID of Quadrant 4 mask Cabinet 1 Slot Number Position of mask in Cabinet 1 Cabinet 2 Slot Number Position of mask in Cabinet 2 Cabinet 3 Slot Number Position of mask in Cabinet 3 Cabinet 4 Slot Number Position of mask in Cabinet 4 ADF File 1 4 contain the files for building the masks as generated by the vmmps software cf AD 5 The parameters indicated as shaded are normally NOT to be filled in by the user but by the OHS cf RD 4 and will not appear in P2PP Number of exposures images are taken for EACH MASK SHUTTER POSITION as defined in ADP files So the real number of exposures is given by Number of exposures NMaskShu 9 3 2 3 VIMOS mos cal arc Template to acquire exposures with Calibration lamps in MOS mode Note that each calibration lamp exposure must be acquired with the appropriate mask i e that used for the scientific exposure NOTE this template is by no means different from the previous one but for the lamps to be used Table 31 parameters for VIMOS mos cal arc Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red
26. If planning IFU mode from OS rather than templates the telescope rotator needs to be put at 116 for the IFU masks to deploy Check all subsystems ONLINE status see OS panel figure A 2 Verify that focusing is AUTO if MANUAL appear go to the TOOLS ICS control panel the ICS panel opens up select focus AUTO This will adjust the internal camera focus according to temperature From OS panel launch RTD the real time display application in the RTD menu select attach SVIGA servers in menu REALTIME In another window run task Bob the template broker The Bob panel opens up with all the default VIRMOS templates The instrument is ready to use either from OS or from Bob refer to the description of these applications in the respective sessions Shut down procedure 1 Software on instrument workstation If in IFU mode the telescope rotator needs to be put at 116 for the IFU masks to retract In OS Panel click on menu File Quit To the question do you want to shut down OS Click OK This will close the panel and shut down all OS realted processes vmosServer vmosFitsMerger and imps From vmmsStart configure panel select all subsystems and select shutdown this will put the instrument in safe STANDBY mode The report from vmmsStart should be OFF for all subsystems After 5 7 minutes the system status should be indicated as STANDBY and IDLE Go to the RTD menu ki
27. LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 1 VIMOS User s Manual Prepared by O Le F vre and the VIRMOS consortium Signature Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 2 EVOLUTION PAGE mime 7 12 98 Draft table of contents for comments me he ro PP 24 10 00 First release after last Sept 2002 commissioning Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 3 TABLE OF CONTENTS 1 INTRODUCTION p 7 2 VIMOS THE VISIBLE MULTI OBJECT SPECTROGRAPH cssscccssssccecssscccessscccessscccecssccccessscceesssaccesssseeeess 8 2 1 VIMOS OBSERVING MODES OVERVIEW csssesesesesececececseecececeesceeeceeecececeeeeeseceeeceeececececesececeeeceeesecesececeseeeeeseceseeeceeeeeeesecess 8 2 2 VIMOS GENERAL OVERVIEW i teet eee etico PEE Ee D Pte eee oerte tetro eer Miet n tee oa ier ce cinesi Eoo iden 10 2 3 IMAGINGMODEBA Ha fei n 14 2 4 MULEI SEIT SPECTROSCOPY MODE n icis rire ivre eee E er eive ei A GoavdavasoeseasesedsduosGoateavesecsdnesseivuesseocudents 14 2 5 INTEGRAL FIELD SPECTROSCOPY MODE suresini vete ee eo RE ERE E Eb oe Re Eee Pete edu sere Ee Ves edo ein
28. R r f VLT PLA VIRA Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 15 Table 5 Multi slit spectroscopy characteristics amp performances Configuration Grisms inserted in the beams Field Slit selection is in 4x7 x8 The cameras image spectra on the full 2048x4096 pix CCD area Slit length 7 per beam in single layer mode 28 total length 5x7 per beam in 5 spectra layers mode 140 total length Slit sampling 4 88 pixels for one arcsec slit Slit width amp length any length and shape minimum dimension 0 2 arcsec Grisms 75 to 720 gr mm rulings Dispersions 6 3A pix to 0 53A pix Resolutions R 180 to 2520 1 arcsec slit Limiting magnitudes in 1h I 24 1 50 R 200 I 22 7 50 R 2500 Ag coated UT 2 5 Integral Field Spectroscopy Mode The characteristics of the VIMOS integral field spectroscopy mode are summarized in Table 6 and are described in details in Section 7 Table 6 Integral field spectroscopy characteristics amp performances Input fiber selection special masks in place 54x54 arcmin and 27 x27 Sampling 0 675 arcsec microlens and 0 338 arcsec microlens Wavelength 0 37 to 1 um Silica microlens array range Spectral Same as for MOS with 1 equivalent slit resolution 2 6 Detectors and Acquisition System The detectors and associated electronics have been assembled by the ESO detector team The detectors are thinned back s
29. TRONOMIE SPATIALE Date 24 Oct 02 page X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Filter Name Photometric filter to be used U B V R Lz Jiitter box width side of box within which offsetting the pointing Return To Origin Defines wether telescope should go back to the original position ate the end of the sequence of exposures Number of exposures Number of exposures to be made Exposure Name root name for resulting files 9 2 2 MOS Mode All MOS mode Observation templates allow usage of Spectroscopic CCD readout mode ONLY i e only the full 2048x4096 CCDs are read Order Sorting filters are automatically associated to the chosen grism 9 2 2 1 VIMOS mos obs Stare Generic purpose template to observe a field in Spectroscopic Mode If more than one exposure is requested Number of Exposures gt 1 each exposure will be Exposure time seconds long Table 20 Parameters for VIMOS mos obs Stare Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution Readout Mode CCD read out mode fast medium slow Number of
30. al v 1 Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 31 Curved Slit 1 Area of image to be examined File Code Method Max Opt Grism LR Red Nomal Opt Slit Width arcsec 1 0 Edgy Sky Region arcsec 1 8 tes Humber of Masks Input Catalog vmCatDummylQuadlMaskl dat total input objects 1058 reference objects 2 j RE vmCatDummyl cat Slit Width arcsec 1 11 Straighten Align Image Statistics 187 placed reference slits 2 placed compulsory slits 1 Image X 1120 6 placed curved slits 1 pe n5 5 _ _ IEEE O 00 04 50 57 Make ADP Close Equinox 42000 i j y EA z View Fit Clear Del Close m Figure 17 vmmps curved slit panel Figure 18 vmmps SPOC panel Observing sequence The observing sequence as executed by the MOS templates is e Preset the telescope to the selected coordinates e Setup the masks in the focal plane and a filter e Take a through mask image e Launch an automated measurement of the position of reference stars in the reference apertures and compute telescope offset required to center targets in the apertures Take a through mask image to confirm mask to sky alignment e Inse
31. arameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name root name for resulting files 9 2 3 2 VIMOS ifu obs Jitter Template to observe a field in IFU slightly shifting the pointing from one exposure to the next The offset from one exposure to the next is given by the two parameters List of Offset in X and List of Offset in Y Offset can be given either in pixels if Offset Coordinates is set to SKY or in arcseconds if Offset Coordinates is set to DETECTOR NOTE that offset are always incremental from the previous position and are to be read as offsets of THE OBJECT ON THE IMAGE i e the Telescope will move in the other direction Each exposure will be Exposure time seconds long Example Offset Coordinates SKY List of Offset in X 010 20 List of Offset in Y 0 0 1 0 2 Number of exposures 5 Exposure N ro X shift Y shift Xtotal Y total shift shift 1 0 0 0 0 2 1 0 1 0 3 0 1 1 1 4 2 0 1 1 5 0 2 1 1
32. are e Flat fields taken at twighlight LAS r f e Arc lamps spectra taken during the day e Spectrophotometric calibration standards 7 6 Data Processing 8 Reference Information 6 1 Filters VIR r f VLT PLA VIRA Issue 1 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 R v 0 0 The filters currently installed in VIMOS are listed in Table 10 The measured transmission curves for each filter are presented in Figure 19 to Figure 28 Table 10 list of VIMOS filters Filter CW and BW U CWL 370 nm FWHM 50 nm B CWL 430 nm FWHM 97 nm V CWL 546 nm FWHM 89 nm R CWL 648 5 nm FWHM 130 nm I CWL 830 nm FWHM 80 nm Z CWL 950 nm FWHM 160 nm OS1 Box Filter 370 670 nm OS2 Box Filter 550 950 nm GG 435 Glass cut High pass filter GG 475 Glass cut High pass filter Word Windows 2000 manual v1 Fichier vimos users page LAS r f Issue 1 0 R v 0 0 Date 24 Oct 02 page 34 CNRS LABORATOIRE D ASTRONOMIE SPATIALE 0 6 0 4 0 2 Norm T 0 6 0 4 0 2 360 380 400 380 400 360 Wavelength nm Figure 19 U band filter transmission curves Norm T Figure 20 B band filter transmission curves Word Windows 2000 Fichier vimos users manual v I Norm T Norm T 0 4 0 2 Norm T LAS r f Issue 1 0 R v 0 0 Date 24 Oct 02 page 35 CNRS LABORATOIRE D ASTRONOMIE SPATIALE wi nm Wi
33. constsudbcoudsavtnsseseavertantarotssnenniastaarends 55 Table 28 parameters for VIMOS me cal Zero 55 Table 29 parameters for VIMOS mos cal Dark x sccsscssnscsncsvendanessannsncsvendsneancnivaesvnnsvieteauanstedsunssasanenatinenes 56 Table 30 parameters for VIMOS mos cal Putin A 56 Table 31 parameters for VIMOS mos Cal Mis a proc 57 Table 32 parameters for VIMOS mos _cal_photom ss 58 Table 33 parameters for VIMOS il cal Dark een 60 Table 34 parameters for VIMOS ifu cal Flat ses 60 Table 35 parameters for VIMOS A0 Sal APE A piment 61 Table 36 parameters for VIMOS _ifu_cal_photom pi 61 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 1 Introduction VIMOS is the Visible Multi Object Spectrograph of the European Southern Observatory Very Large Telescope telescope unit 3 Melipal This instrument has been build to provide the ESO community with a wide field spectrograph with high throughput and multiplex dedicated to deep surveys VIMOS operates in the 0 37 1 microns domain in 3 main observing modes direct imaging multi slit spectroscopy MOS and integral field spectroscopy IFS The field of view of the 4 channels is 4x7x8 arcmin in imaging and MOS modes with 0 2 arcsec pix and 54x54arcsec in IFS mode with 0 67 arcsec res element Each of the 4 channels has a 2048x4096 pixels EEV CCD wit
34. dithering pattern depends on the mean size of the observed objects the dithering pattern should be larger than the mean size of objects for the method to work efficiently 6 4 Mask design and manufacturing With the object catalog and the instrument configuration requirements the user can enter the mask design and manufacturing process All the processes below are described in detail in the vmmps users manual see http cosmos mi iasf cnr it bianca vimos sw doc vmmps vmmps um html 6 4 1 Pre image catalog The purpose of the pre image is to allow to link the user s catalog coordinates to the VIMOS CCD coordinates and hence to the mask reference frame coordinates via a secure internal VIMOS mask to CCD mapping and transformation matrix A detection of objects is required in the pre image in order to cross correlate this list of objects with the list of objects in the user catalog A transformation matrix from user catalog to VIMOS coordinates is then produced The user can run e g Sextractor to perform this detection the output needs to be a FITS table About 80 detected objects per channel is a good number for a secure mapping An exposure time of 3min in the R band on any field should produce enough objects to have a sufficient S N for 80 of them in each channel 6 4 2 Case 1 no pre existing external user catalog 6 4 3 Case 2 cross correlation of pre image catalog with pre existing external user catalog For each channel
35. e RE isa doad ose 15 2 6 DETECTORS AND ACQUISITION SYSTEM csiccsicsvsssssecccecsssssvcocdeccdesssovvoevedecssvoaseoteossdeavsavsdocseseesesssuosGoadeavedensdnebseadvess ecuseess 15 2 7 OBSERVATION SOFTWARE cc cis 16 2 8 REAL TIME DISPLAY SAA GREG EE RA GE SR RAS ERE RET EE E lee dense ERR nee 18 2 9 CADIBRATIONS iecit RO ERR PEE ace a cis GE 19 210 OVERHEADS Mr 19 2 11 TEMPLATES SUMMARY iris 21 3 REQUESTING OBSERVING TIME AND PREPARING OBSERVATIONS WITH VIMOS e eec 21 3 1 CALL FOR PROPOSAL Sie einen iii 21 3 2 EXPOSURE TIME CALCULATOR ervvvvevevererererererererevererererererererevererererereverevererevevevevereverevevevevevevevevevevevevevevevevevevevevevevevevevern 21 3 3 PHASE II PROPOSAL PREPARATION P2PP cccsccessessceeseesseeseceseeeaecsaecsaecseecaeecaeessesenesaesesseeeeseeeeceaeeeaeceaecaueceesaeenseeass 22 3 4 VISITOR AND SERVICE MODES ccccessesssseceeeceeseueceeececsessuaeeeceeeceesesusaeseeececeeeaaeeeescceseeaaesececsceeeaseseeeeeeeeeeaaeseeseeesenseaes 22 4 OBSERVING WITH THE VLT AND VIMOS cssssccsssscccessssccscssccccesscccessccececsscceesssacceessceccecsceecessaceecssseccsesceeeees 22 4 1 TELESCOPE AND INSTRUMENT FOCUS csesescosseveseoscevceeessevsceescevssessseececscevsceessevseeessuvseeesseveeeessuvsceesseseesssevsedesceneeeesccestes 22 42 AGUIDING AND OSEA 23 4 3 FLEXURES AND TRACKING STABILITY e eierne eset aereo ne iet a an nerder Ue e eunt neve a cue epa
36. e mask There are 4 filter assemblies to exchange up to 10 filters per channel The 4 grism assemblies allow to select and exchange up to 6 grisms per channel Instrument focussing is performed by moving the first elements of the camera it is automated and calibrated with temperature 3 calibration units provide uniform illumination of the Nasmyth screen for flat field and arc lamp calibrations Detectors Each of the 4 channels has its dedicated CCD detector The detectors are back illuminated 2048x4096 pixels 15um pixel EEV CCDs The 4 shutters allow to control the light arriving on the CCDs Integral field unit The integral field unit is a dedicated opto mechanical system aimed at producing spectra of a contiguous area of up to 54x54 arcsec The sky image is projected onto a 80x80 micro lens Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 11 array With a choice of two magnifications 0 33 or 0 67 arcsec micro lens Each 2D micro lens is coupled to an imaging fiber while the output of the fibers is rearranged on a linear set of micro lenses to produce an entrance slit to the spectrograph at the mask focal plane location Each spectrograph quadrant has a set of 4 fiber slits for a total of 6400 fibers A shutter is provided in front of the input micro lens array to allow the exclusive use of the central 1 4 of t
37. e observing sequence as executed by the imaging templates is e Preset the telescope to the selected coordinates e Initiate guiding and active optics control telescope operator e Configure the instrument with the selected filter e Take a sequence of exposures jitter or no jitter 5 5 Calibration The required calibrations are e Flat fields taken at twighlight e Photometric calibration standards distributed in all 4 channels 5 6 Data Processing 6 Multi Slit Spectroscopy 6 1 Overview In Multi sht spectroscopy mode VIMOS is used to take many spectra simultaneously Transmission gratings replicated on prisms Grisms are available to cover the full spectral range with spectral resolutions R 200 to 2500 for a 1 arcsec wide slit The slit sampling at the detector level has been set by design to 4 88 pixels arcsec Depending on the science goals and on the atmospheric seeing it is therefore possible to narrow the slit to 0 5 arcsec still allowing a proper sampling of the slit at 2 44 pixels In this situation the spectral resolution is obviously doubled to allow R 400 5000 The grisms properties are summarized in Table 11 Order separating filters are available to eliminate the overlap between orders 1 the order used for science and order 2 always present on the detector this is done by restricting the wavelength range of a particular grism to less than one octave in wavelength The allowed slit placement in a mask is directly re
38. er vimos users
39. ets can be given in pixels or in arcsec List of Offset in X list of offset in X or Dec direction List of Offset in Y List of offset in Y or RA direction Exposure Name root name for resulting files 9 2 3 3 VIMOS_ifu_obs_Autojitter Template to observe a field in IFU Mode slightly shifting the pointing from one exposure to the next The offset from one exposure to the next are automatically computed in a random manner within a box of side Jitter Box Width Each exposure will be Exposure time seconds long Table 24 parameters for VIMOS ifu obs Autojitter Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Word Windows 2000 manual v I Fichier vimos users LAS r f Issue CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page 53 Low Red or orange Medium Resolution IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F Readout Mode CCD read out mode fast medium slow Jiitter box width side of box within which offsetting the pointing Return To Origin Defines whether telescope should go back to the original position
40. fsetted so that chosen star falls within the expected location of the requested lit Finally Grism is inserted and calibration exposures are acquired shifting from one quadrant to the next operative one if Cal Flag is set to true Word Windows 2000 Fichier vimos users manual v1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 9 3 3 IFU mode 9 3 3 1 VIMOS ifu cal Dark Template to acquire a series of darks or biases exposures Table 33 parameters for VIMOS ifu cal Dark Parameter Name Descritpion X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Number of Exposures Number of exposures to be made Exposure Name root name for resulting files List of exposure times esposure time for each of the exposures The List of exposure Times parameter defines the exposure time for each exposure If exposure time is zero a bias is acquired Example 1 Number of Exposures 6 List of exposure Times 0 0 60 300 900 3600 Will perform first a series of 2 biases exp time 0 and then a series of 4 darks lasting 1 5 15 and 60 minutes each Example 2 Number of Exposures 6 List of exposure Times 0 Will perform a serie of 6 biases exp time 0 Example 3 Number of Exposures 6 List of exposure Times 0 10 20 Will acquire two
41. g so that the calibration star field 1s at the center of quadrant 1 Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 56 If the 4 quadrant flag is set to True images are acquired shifting the pointing so that calibration star field falls in turn on each of the 4 quadrants 9 3 2 MOS mode 9 3 2 1 VIMOS mos cal Dark Template to acquire a serie of darks or biases exposures Table 29 parameters for VIMOS mos cal Dark Parameter Name Descritpion X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Number of Exposures Number of exposures to be made Exposure Name root name for resulting files List of exposure times esposure time for each of the exposures The List of exposure Times parameter defines the exposure time for each exposure If exposure time is Zero a bias is acquired Example 1 Number of Exposures 6 List of exposure Times 0 0 60 300 900 3600 Will perform first a serie of 2 biases exp time 0 and then a serie of 4 darks lasting 1 5 15 and 60 minutes each Example 2 Number of Exposures 6 List of exposure Times 0 Will perform a serie of 6 biases exp time 0 Example 3 Number of Exposures 6 List of exposure Times 0 10 20 Will acquire two
42. h the 4k pixels being used along the dispersion for an increased spectral coverage Spectral resolutions range from 200 to 2500 for a slit one arcsecond wide The MOS mode allows to place 840 slits 10 arcsec long in the low resolution mode 210 slits in high resolution mode Any slit length can be used having an impact on the total number of objects The objet selection is made with the Mask Preparation Software and masks are cut by the Mask Manufacturing Unit with up to 15 masks being available during observations The IFS mode allows contiguous spectroscopy of 6400 resolution elements fed by an array of micro lenses and fibers These unprecedented multiplex gains position VIMOS as the leading instrument of this kind in the world This manual is organized as follows Section 2 presents the general characteristics of the instrument Sections 4 to 7 describe the imaging MOS and IFS observing modes respectively Section Erreur Source du renvoi introuvable provide a description of the observing templates and Section 8 provides some reference information In addition the user is invited to consult the following documents Call for proposals Phase I preparation http www eso org proposals P2PP Phase II proposal preparation general information http www eso org observing p2pp P2PP Phase II proposal preparation VIMOS specific information Questions on VIMOS operations should be aked directly to the ESO User Support Group usg
43. hat all targets are in the slits as planned The procedure is to take a through mask image of the sky and check that reference stars usually 2 per masks are located at the center of the reference apertures or slightly offset the telescope to center them This procedure via a dedicated template requires to configure the instrument in imaging mode with a set of masks in place take a first exposure measure the position of reference stars offset the telescope if necessary take an image to validate On average this procedure takes no more than 5 minutes Night time instrument calibrations Most instrument calibrations can be performed during the day MOS IFU arc and flat field calibration or during twilight imaging flats During the night the acquisition of photometric or spectrophotometric standard stars is required to accurately flux calibrate Examples for overheads computation are given in Table 8 Table 8 Examples of overheads 20 Imaging no Imaging with MOS observation MOS sequence of 5 IFU observation IFU filter change field change new field one exposures with new field observations same field and filter integration telescope offset same field change shift in slit same new grism field same mask Instrument 0 2 min e Initial Grism setup 2 5 min e 0 if already in 2 5 min configuration mask filter IFU mode setup 3 5 min e 3 5min if e Grism setup starting fro
44. he field when the IFU is used in high spectral resolution mode with wide wavelength coverage In this configuration only fiber slit per quadrant is used for a total of 1600 fibers Mask manufacturing machine The mask manufacturing machine MMU is dedicated to cut user defined slits on a thin mask material with a high speed numerically controlled laser based machine The MMU includes the following e Mask sheets these are the support upon which the slits are cut they are in black coated Invar e Mask cabinets contain up to 15 mask sheets There is one mask cabinet per channel The masks cabinets are installed at the VIMOS focal plane for observations and removed for mask loading e Mask loading amp identification a semi automated process is aided by bar code readers e Mask laser machine and XY stage used to cut the slits on the mask sheets The MMU is located in a dedicated room at the Paranal Observatory base camp Instrument software The instrument software allows the operation and control of the instrument including detectors as well as the necessary software support for mask preparation and manufacturing The instrument software contains the following blocs e Observation Preparation Software OPS Mask Preparation Software MPS Observation Software OS Instrument Control Software ICS Detector Control Software DCS Data Reduction Software DRS Word Windows 2000 Fichier vimos users manual v1 LAS r f
45. he one with chosen height of the first Operative Quadrant 1 If the 4 quadrant flag is set to True images are acquired shifting the pointing so that calibration star field falls in turn on each of the 4 quadrants Operator note The mask required for this template is a dedicated mask having long i e 50 pixels slits of different heights from 0 5 to 2 5 arcsec The ADP for this mask is to be manually created but normally should never change When the mask is manufactured pixels are transformed into millimeters using the CCD to Mask Calibration matrix in the ADP itself Such matrix can be well out of date thus the template when Fine Aligment is set to true does NOT rely on ADP pixel position of the slit but searches for the slit around the expected position spanning a box 3 times the slit length in X and 3 times the slit height in Y The procedure is as follows pointing is shifted so that chisen star falls in the proximity of the required slit guiding is started and an image acquired The user is asked to click on the desired calibration star and its actual position is stored and masks are inserted If the Fine Alignment is requested another image is acquired and the required slit is searched for around the expected position If found the telescope pointing is offsetted so that the chosen star falls within the slit another image is acquired and user is asked for an even finer tuning If fine Aligment is set to False the pointing is of
46. ide illuminated EEV CCDs ref with 2048x4096 pixels each 15x15um The FIERA and associated electronics allow various readout modes and windowing Readout speeds from XX to YY Mpixels sec allow to read the 4 detectors in parallel in less than in the most demanding low gain high resolution mode The readout noise properties of each detector is given in Table 7 Table 7 CCDs readout noise Detector Channel Readout mode Readout noise Gaine ADU e QI Imaging Q2 Imaging Q3 Imaging Q4 Imaging QI MOS IFU Word Windows 2000 Fichier vimos users manual v I LAS r f VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date Q2 MOS IFU Q3 MOS IFU Q4 MOS IFU 2 7 Observation Software OS is the high level software controlling the instrument It has its own GUI which allows to access all instrument parmeters Figure 7 shows the VIMOS OS GUI The users only use templates to control the instrument and have therefore no direct interaction with OS However the OS GUI is useful for the visitors as a status display panel displaying all information for instrument detectors and telescope 16 Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 17 Word Windows 2000 Fichier vimos users manual v I
47. ifferential pointing positions around a central position With the large field of view of the VIMOS IFU techniques equivalent to shift and add classically used in imaging can be used with the IFU this is the preferred mode of operation Several short images exposure times such as the exposures are sky background limited are taken at each position of a dithering pattern to reconstruct an image with the total exposure time required This allows to eliminate the sky contribution cosmic rays the CCD fringing particularly in the red cosmetic defects on the detectors and to produce very accurate flat fielding to correct for detector pixel to pixel variations The dithering pattern depends on the mean size of the observed objects the dithering pattern should be larger than the mean size of objects for the method to work efficiently 7 4 Observing sequence The observing sequence as executed by the IFU templates is e Set the instrument to IFU mode if not already in this mode the instrument rotator needs to be setup at 116 6 for the IFU masks to be allowed to deploy by the instrument control software 32 e Preset the telescope to the selected coordinates e Initiate guiding and active optics control telescope operator e Configure the instrument with the selected grism filter e Take a sequence of exposures jitter or no jitter Word Windows 2000 Fichier vimos users manual v I 7 5 Calibration The required calibrations
48. ime 0 Example 3 Number of Exposures 6 List of exposure Times 0 10 20 Will acquire two series each consisting of one bias exp time 0 and two darks 9 3 1 2 VIMOS img cal FlatDome Template to acquire a series of Flat field exposures on the screen in imaging mode Table 26 parameters for VIMOS img cal FlatDome Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Word Windows 2000 Fichier vimos users manual v I CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 Date 24 Oct 02 page 55 Y binning factor Binning factor in Y direction 1 or 2 Calibration Lamp Name Name of the calibration Lamp to be used Readout Mode CCD read out mode fast medium slow Filter Name Photometric filter to be used U B V R Lz Number of exposures Number of exposures to be made Exposure Name root name for resulting files 9 3 1 3 VIMOS img cal FlatSky Template to acquire a serie of Flat field exposures in imaging mode Table 27 parameters for VIMOS img cal FlatSky Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out m
49. ional pointing offset in RA Delta Offset Additional pointing offset in Dec IFU Shutter Shutter for IFU Unit T F IFU Magnificator Magnification for IFU Unit T F On top of these parameters the target description should be filled in at least with Right Ascension Declination Equinox and Epoch Note that the pointing coordinates in the target description will correspond to the center of VIMOS IFU Field of view i e the pointing sequence will automatically offset the telescope to the IFU position which is about 10 arcmin from the VIMOS center If an additional offset in RA and or Dec is given it will also be taken into account 9 1 3 MOS Mode 9 1 3 1 VIMOS mos acq mask This template allows to point the telescope to the desired position and refine pointing with mask alignment on reference objects Table 15 parameters for VIMOS mos acq Mask Parameter Name Description Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Cabinet 1 Slot Number Position of mask in Cabinet 1 Cabinet 2 Slot Number Position of mask in Cabinet 2 Cabinet 3 Slot Number Position of mask in Cabinet 3 Cabinet 4 Slot Number Position of mask in Cabinet 4 Word Windows 2000 Fichier vimos users manual v I LAS r f 45 Issue 1 0 R v 0
50. ith the Nasmyth rotator and guiding with the Nasmyth guiding probe Optics The optical system is the combination of 4 identical optical channels The optical system includes a Focal Plane Adaptation Lens to correct telescope aberrations at the Nasmyth focus and diminish the field curvature to allow the use of flat masks After the new focal plane the optical system is a classical focal reducer type instrument with a collimator making a parallel beam in which dispersing elements are inserted followed by a camera which transforms the input F 15 beam to a F 1 8 beam projected onto 4 large format 2048x4096 pixels EEV CCDs Structure and main mechanical subsystems VIMOS requires a mechanical structure to attach the various opto mechanical components to the Nasmyth adaptor The main property of the structure is minimize image motion in the CCD focal plane due to mechanical flexures under gravity load and temperature variations Direct access to masks grisms filters and shutters is provided The main mechanical subsystems are The mask assembly has the function to enable mask positionning at the focal plane It has provision for the storage of 15 masks per channel A set of 4 mask shutters is installed near the mask focal plane They allow to block part of the beam coming from a selected area of the mask and thus allow arc and flat field spectroscopic calibrations without order overlap when several layers of slits are used on the sam
51. lated to the wavelength range and the spectral resolution used This defines a spectrum length on the detector At low and medium resolutions LRRED LRBLUE MR the full spectrum range is recorded no matter the slit location on the detector At high spectral resolution HIBLUE HIORA HIRED the slit location will define the wavelength range of the spectrum 6 2 Performances Performances in MOS mode are given in Table 5 section 2 4 6 3 Observation preparation The preparation of observations require the following e Central field equatorial coordinates 0 5 for telescope pointing e Pre image image of the field taken with VIMOS e List of equatorial coordinates 0 0 and epoch of reference a catalog of targets should contain at least the equatorial coordinates and any parameter that the user needs to select target within a large catalog e g magnitudes colors sizes Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page e Grisms Filters to be used e Exposure times e Dithering move in slit pattern Moving targets along the slit in a series of exposures is the preferred way to observe in MOS This allows to eliminate the sky contribution cosmic rays the CCD fringing particularly in the red cosmetic defects on the detectors and to produce very accurate flat fielding to correct for detector pixel to pixel variations The
52. ll the RTD application FILE quit it will automatically detach the SVIGA servers Go on BOB kill the application FILE quit 2 Hardware on platform If instrument is used the following night s leave all systems powered up If instrument is to be completely shut down Power OFF FIERAs and associated electronics Power OFF LCUs Word Windows 2000 Fichier vimos users manual v I Additional checks CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date 64 The normal configuration for user vimos is driven by environment variables To check current values of environment variables relevant for the usage of vimos s w and instrument from the command line just issue the command vmmcfgShowEnv sh It will display vimos realted environment variables ONLY e g as follows CURRENT ENVIRONMENT VARIABLES ARE LILLLLLLLLLLLLLLLLLLLLLLLLLLLLI f S LOG IG INSTRUMENT LCU LCU LCU CCD1LE CCD2LI CCD1NAME CCD2NAME FCD IT HOS FCD IT HOS LOGFILE DFLOW ROOT INS MAINT VMI LOG TE VMILCU LOG ICS OPMODE ENVNAME MOS ROOT vlt MAR2002 CCS ROOT diska V NTROOT diska V MOS NS YSTEM wu3dhs N diska V MOS diska V MOS NS NS diska V VIMOS Vim
53. m after mask MOS or setup 2 5 min imaging Telescope set 0 Started in Started in parallel 0 5 min 0 up parallel with with instrument instrument configuration total configuration time 5 min total time 5 min added time 3 min Mask reference 0 0 5 min 0 0 0 aperture check Detector readout 45 45 sec 45 sec 5x45 sec 45 45 Total overhead 0 75 min 5 75 min 8 25 min 5 5 min 5 75 min 3 25 min Word Windows 2000 Fichier vimos users manual v I LAS r f VIR r f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date CNRS LABORATOIRE D ASTRONOMIE SPATIALE 2 11 Templates Summary The instrument detector and telescope are controlled by observing blocks OBs which are made up of templates Templates are divided into three categories acquisition observation calibration Usually OBs consist of an acquisition template and one or more observation templates for science frames and one or more calibration templates for calibration frames Only one acquisition template is allowed in an OB and therefore only one preset on sky It is not possible e g to group in the same OB observation templates on the science objects and calibration templates on a standard star Table 9 provide a short summary of the templates offered for the next period The template parameters are extensively described in Appendix X for the Phase II preparation Table 9 Templates summary Action Template to use Ob
54. n the corresponding panel button You may also draw curved slits on selected objects see Figure 17 Then click on SPOC select the parameters of the slits width sky region and select the appropriate grism Select the total number of masks you want to produce at this setting and the SPOC algorithm Max_opt takes into account the size of objects if present in your catalog or Normal_opt standard mode Click on Make ADP to run the automated slit object allocation algorithm As an output you get the number of objects selected and a file with all slit and object information e g file_vmQ1M1 adp for mask I of quadrant 1 Close the SPOC window 6 4 5 Display slit object selection This step is to verify that the slit mask design is OK it is indeed recommended to perform this step Select VIMOS MPS Load ADP catalog load the file e g file vmO1Ml adp A new window is opened with the catalog containing the slits see Figure 15 objects selected are identified by a square on the image To visualize all slits and spectral extent click on Plot Slits see Figure 16 If everything is fine your ADP files are ready to be transferred to the mask manufacturing tool 6 4 6 Mask manufacturing mask tracker TBD 27 Word Windows 2000 Fichier vimos users manual v I CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 Date 24 Oct 02 page 28 Skycat version 2 6
55. nd received OS PROFILE finished i SETUP START PAUSE RESUME ABORT END CANCEL Figure A 1 OS panel At completion of the vmmsStart procedure the instrument status should be ONLINE IDLE upper right as well as the ICS and the 2 DCS environments left and middle Word Windows 2000 Fichier vimos users manual v 1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 69 Word Windows 2000 Fichier vimos users manual v I CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 Date 24 Oct 02 page 70 Startup VIMOS Control SW virmos File Help Configure Rtap DCS1 DCS2 ICS OS Status Thu Jul 13 15 39 19 METDST 2000 DCS LCU1 Disabled DCS LCU2 Disabled ICS LCU1 Disabled ICS LCU2 Disabled OK OK OK OK OK Show log Startup Logfile 1 Log file On Off Loading CDT vmosServer vmosServer started vmosFitsMerger started vmouifControl started Rtap status Desi status Des2 status Ics status Os status START SHUTDOWN Update Status Clear Log STOP Figure A 2 vmmsStart panel Selecting the configure menu upper left allows to select the subsystems to be startup or shutdown Word Windows 2000 manual v I Fichi
56. ng No check image is acquired Table 12 parameters for VIMOS img acq Preset Parameter Name Description Guiding lambda Wavelength for guiding Alpha Offset Additional pointing offset in RA Delta Offset Additional pointing offset in Dec On top of these parameters the target description should be filled in at least with Right Ascension Declination Equinox and Epoch Note that the pointing coordinates in the target description will correspond to the center of VIMOS FOV and the four images will correspond to the four quadrants around this point 9 1 1 2 VIMOS img acq MoveToPixel This template moves the telescope to the Target position acquires guiding star and starts Autoguiding acquires and image and allows interactive pointing refinement Table 13 parameters for VIMOS img acq MoveToPixel Parameter Name Description Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Guiding lambda Wavelength for guiding Alpha Offset Additional pointing offset in RA Delta Offset Additional pointing offset in Dec Readout Mode CCD read out mode fast medium slow Filter Name Photometric filter to be used U B V R Lz Preset Telescope Move to desired position Y N On top of these parameters the target description should be filled in at least with Right Ascension
57. nm Wavelength nm Figure 22 R band filter transmission curves Word Windows 2000 manual v I Fichier vimos users LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 Date 24 Oct 02 page 36 Norm T Norm T Figure 23 I band filter transmission curves 0 6 0 4 VPT Ta Thea fet fag Np Veit Pa Norm T 0 6 0 4 0 2 TT ET I ET GJ hd 800 900 1000 800 900 1000 Wavelength nm Figure 24 z band filter transmission curves Word Windows 2000 Fichier vimos users manual v I LAS r f VIR r f VLT PLA VIRA Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 37 Norm T Norm T 400 500 600 700 400 500 600 700 Wi nm Wi nm Figure 25 OSI filter transmission curves Norm T Norm T 0 500 600 700 800 900 100800 600 700 800 900 1000 Wi nm Wi nm Figure 26 OS2 filter transmission curves Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 38 Norm T Norm T 600 800 1000 600 800 1000 Wi nm Wi nm Figure 27 GG435 filter transmission curves HEH 42 0449242434 35 L 4 1 L 4 500 600 700 600 700 800 800 500 Wavelength nm Figure 28 GG475 filter transmission curves Word Windows 2000 Fichier vimos users manual v1 LAS r f
58. ode fast medium slow Filter Name Photometric filter to be used U B V R Lz Number of exposures Number of exposures to be made List of offest in DEC arcsec DEC to offest between exposures List of Offste in RA arcsec RA to offest between exposures Exposure Name root name for resulting files Exposure level Wished counts in resulting Flat Field The template gets an image and automatically computes the exposure time needed to obtain the requested counts in each image It performs the requested number of exposures eventually offsetting the telescope between one and the other of the wished amount 9 3 1 4 VIMOS img cal Zerop Template to acquire photometric calibration exposures in imaging mode Table 28 parameters for VIMOS img cal ZeroP Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Filter Name Photometric filter to be used U B V R Lz Number of exposures Number of exposures to be made 4 quadrants flag Take image with photometric standard in 1 or 4 quadrants Exposure Name Root name to be given to resulting files The template assumes that telescope has been pointed on the calibration field it will itself take care of shifting the pointin
59. os wvmos wt3tcs lvmicsl wvmccda wvmccdb Vimosa Vimosb TI T2 MOS archeso wu3d lvmicsl lvmics2 wvmccda wvmccdb ROOT SYSTI ROOT SYSTI hs data msg ROOT SROOT SYST n n vltdata tmp vmilogFile MA NT P ST _ TEST NORMAL VLT VCCBOO TT ME VLT VCCTIM EOUT 90 ICS CMDT ME 60 ICS STARTT 30 ICS ONLINE 600 ICS OFFT ICS STANDI ICS STOPTI CS SETUPT ICS STATUS T ET CS SETMOD diska V dis 900 vlt MAR2002 CCS ENANC MOS ka V MOS NSRO NSROOT MA M ARCDATA MARC EM ARCDATA DATA BADDATA NT ENANC E M Sc CS LOGS OT MA NT ENANC E M SC ICS LOGS Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page You may want to check in particular that the following variables have the values as indicated CCDILENV wvmccda CCD2LENV wvmccdb ICS OPMODE NORMAL If ICS OPMODE HW SIM it means that before putting the instrument ONLINE you will have to choose MANUALLY which devices will have to be used in simulation or in normal mode To do this
60. osure to the next The offset from one exposure to the next is given by the two parameters List of Offset in X and List of Offset in Y Offset can be given either in pixels if Offset Coordinates is set to DETECTOR or in arcseconds if Offset Coordinates is set to SKY Offsets are always incremental from the previous position and are to be read as offsets of THE OBJECT ON THE IMAGE i e the Telescope will move in the other direction Each exposure will be Exposure time seconds long Example Offset Coordinates SKY List of Offset in X 0 10 10 List of Offset in Y 0010 1 Number of exposures 5 Exposure N ro X shift Y shift Xtotal Y total shift shift 1 0 0 0 0 2 1 0 1 0 3 0 1 1 1 4 1 0 0 1 Word Windows 2000 Fichier vimos users manual v I CNRS LABORATOIRE D ASTRONOMIE SPATIALE LAS r f VIRr f VLT PLA VIRA 1 0 R v 0 0 24 Oct 02 page Issue Date 1 0 0 At the end the pointing will have been moved along a square of 2 arcseconds side If Number of exposures is larger than the number of offsets in X or in Y the sequence of offsets will be restarted Example List of Offset in X 0 1 List of Offset in Y 01 Number of exposures 5 The following offsets will be applied Exposure N ro X shift Y shift Xtotal Ytotal shift shift 1 0 0 0 0 2 1 1 1 1 3 0 0 1 1 4 1 1 2 2 5 0 0 2 2
61. osure N ro shift Total shift 1 0 0 2 1 1 3 0 1 4 1 2 5 0 2 Table 21 parameters for VIMOS_mos_obs_Jitter Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Grism Name Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution Readout Mode CCD read out mode fast medium slow Return To Origin Defines whether telescope should go back to the original position at the end of the sequence of exposures Number of exposures Number of exposures to be made List of Offsets List of offsets along the slit in arcseconds Exposure Name Root name for resulting files 9 2 3 IFU Mode All IFU mode Observation templates allow usage of Spectroscopic CCD readout mode ONLY i e only the full 2048x4096 CCds are read Order Sorting filters are automatically associated to the chosen grism Word Windows 2000 Fichier vimos users manual v1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 51 9 2 3 1 VIMOS ifu obs Stare Generic purpose template to observe a field in IFU Mode If more than one exposure is requested Numebr of Exposures gt 1 each exposure will be Exposure time seconds long Table 22 parameters for VIMOS mos obs Stare P
62. ou are guaranteed that rotating back keeps the mask sky alignment Fix If collision occurs a pop up window will appear reporting which grism unit has failed check also the log monitor To recover from failure go to and xterm window and type the following series of commands vmiCmd SIMULATE INS GRIS2 for grism unit 2 vmiCmd OFF INS GRIS2 vmiCmd ONLINE INS GRIS2 vmiCmd STOPSIM INS GRIS2 vmiCmd OFF INS GRIS2 vimCmd ONLINE INS GRIS2 this reinitializes only the incriminated unit the first three command clear any software flag in simulation mode while the last three commands send the unit to hardware limits for re initialization 2 Mask 4 is 10 pixels off in Y You may be in a situation for which you find that reference stars for channels 1 2 and 3 are perfectly in their reference holes while the reference stars are barely visible or not visible at all in the reference holes of mask 4 We have seen this a couple of time and plan to check the mask blocker limit switches at the next opportunity Fix go to an xterm and type the following series of commands to reinitialize the unit 4 vmiCmd SIMULATE INS MASKA4 vmiCmd OFF INS MASK4 vmiCmd ONLINE INS MASK4 vmiCmd STOPSIM INS MASK4 vmiCmd OFF INS MASK4 vimCmd ONLINE INS MASK4 65 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 66 Word Windows 2000 Fichier vimos users man
63. ps software cf AD 5 The parameters indicated as shaded ar normally NOT to be filled in by the user but by the OHS cf RD 4 and will normally not appear in the distributed version of VIMOS templates Number of exposures images are taken for EACH MASK SHUTTER POSITION as defined in ADP files So the real number of exposures is given by Number of exposures NMaskShu For each Shutter position and each exposure all requested lamps are switched on Exposure starts and it is pasued when the shortest lamp exposure given has elapsed Lamp is switched off and exposition resumed till next lamp exposure time is elapsed and so on till the end Example Number of Exposures 3 He Exposure time 2 Ne Exposure time 2 Ar Exposure time 10 For each Shutter position as indicated in ADM file 3 exposures will be made using the following sequence switch on He and Ar lamps expose for 2 seconds close chutter switch off He lamp re open shutter and continue for the next 8 seconds 9 3 2 4 VIMOS mos cal photom Template to acquire spectro photometric calibration exposures in MOS mode Table 32 parameters for VIMOS mos cal photom Parameter Name Descritpion Exposure Time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode fast medium slow Word Windows 2000 Fichier vimo
64. re 5 Overall VIMOS view CAD VIEW Dis A r iaa aaa 13 Figure 6 The VIMOS instrument installed on the Nasmyth plateform of UT3 Melipal 14 Figure 7 VIMOS OS graphical user interface Left instrument control panel Middle detector control panel Right telescope control panel 18 Figure 8 VIMOS Real Time Display oiii Ua DU id 19 Figure 9 Image quality FWHM vs distance from the optical center in pixels quadrant 4 The FWHM measures the images of pinholes 300 microns in diameter distributed in a grid at the mask focal plane The specification is shown as a dashed line as FWHM 3 2pix the measured image quality is 2 pixels FWHM over the field 23 Figure 10 PSF variation accross the VIMOS field at the field center and field edges images of 300 microns O 23 Figure 11 flexures measured for channel 2 The circle represents a motion of 1 pixel from MONET CH e PO PU EE RES 24 Figure sd iia 28 Freue 13 vinmps cross c rtelation PL aia dada dd 29 Figure 14 vimmps catalog panel aii 29 Figure 15 vymmps slit panel REE S RR CEN RU RU aa nn 30 Figure 16 Display of slits selected by vmmps SPOC with objects location and spectra extent 30 Figure 17 vmmps curved slit panel ina pis s ER nino de ep UR PN OR a 31 Fel viamps SPUC Pastrana aci 31 Figure 19 U band filter transmission Curves essessssesseeseseereesesreseeseseeseestretssessestasensesres
65. researesrestesesseseeee 34 Figure 20 B band filter transmission curves nement 34 Figure 21 V band filter transmission curves ramadan 35 Figure 22 R band filter transmission curves ios ak er Ur e UD notes 35 Figure 23 I band filter transmission CUEVES Lassen URDU VR NUR UA FACE nU EY ra eH bu rcf 36 Figure 245 band filter FO GE VES ANG 36 Figure 25 OS1 filter transmission CUEVOS aeos esie nier bene SEIS ida ciedad 37 F re 26082 filter mA GUY GR nm non seen nn PRO nana 37 Figure 27 GG435 filter transmission CUE ES rv 38 Figure 28 GG475 filter transmission Curves sion inna eaae entra oa eH uu pras te Eve pee ME eda PM Is Re I Ea PET tend 38 Figure 29 sky spectrum in CCD counts 1440 sec integration 1 arcsec slit LRRED grism 40 Figure 30 sky spectrum flux calibrated Visserie 40 Figure 31 He Ar arc spectrum with the LRRed grism eese eene ee ette enne enne tnnen 41 Figure 32 He Ar spectrum with the ROM POMO ase ooa Rt x URN cannes 41 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 6 LIST OF TABLES Table 1 VIMOS Operation Modes 8 Table 2 VIMOS Observing Modes cisne ini 8 Table 5 VIMOS mechanical and optical characteristics uiuos di osten in Rene binh er Rae iio 9 Table 4 Imaging characteristics amp performances hernie 14 Table 5 Multi slit spectroscopy characteristics amp perfo
66. reverevevevevevnvevevevevevnvevnvnvnvevevevevern 40 9 USER S TEMPLATE DESCRIPTION soveeevesesssvnvnvevessssnnnnvnnenesensnnnnnnnnnennnsnnnennennssensnnnnnnenssennnnnnnnnenenensennnnnnennenesennnnnneee 43 JT ACQUISITION TEMPLATES RET 43 OII dmagmsMode 25201 hore A Qoa ein Deda nn einen en 43 OED AFU MO CR 44 GES MOS Mode deze dde ees i ele eere ey tree nro US enes duka NS Eine ane 44 02 OBSERVATION L EMBLATES ettet tre seere eee derved arvede even seiere 47 924 Amagin Mol Esisi uou ote iade n o vn Qo YS d apen opes yeso Dto Y esi eu o De cg ut 47 022 MOS Mode ier e Deer ds stabs od oerte A debt ed eee de E A ey eee exero drite 49 023 E IDs 50 0 3 CALIBRATION TEMPLATES da tinelli i n 54 93 1 Imaging Mode iie e ete tiere aegis rien ee ikek len da 54 USB MOS MODS E M 56 USE MEN OE HOGG m EH H 60 10 ANNEX A START UP AND SHUT DOWN PROCEDURES eere eerte nenne ete tn naa asses sesta sese see eese sn nass sese seca 63 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 5 LIST OF FIGURES Figure 1 VIMOS feld Of VEN aieo epit b eb vide dia on be P RO UNAM Or P sedan UNE ESER EsTa 9 A 12 Figure 3 VIMOS optical layout ome cali 12 Figure 4 VIMOS opto mechanical layout top view ss 13 Figu
67. rmances 15 Table 6 Integral field spectroscopy characteristics amp performances oocococcnocccnoncconncnonoconnnonanonnnoconccnnncnnnno 15 Table 7 CCDS readout NOISE iia 15 Table 8 Examples of overheads LEG 20 Table 9 Templates ANG 21 Table 10 hist of VIMOS fler nia aia 33 HE GE ES Jen GJERE ETT 39 Table 12 parameters for VIMOS mus 3609 Presta 43 Table 13 parameters for VIMOS img acq MoveToPixel RR 43 Table 14 parameters for VIMOS f aed Prestations 44 Table 15 parameters for VIMOS mos acq Mask renrnrnrnrenrrrnrrrnnrnrrrnrenrrennrrsnnserrrrensrennessnreesrnrersesnnrssnneenn 44 Table 16 parameters for VIMOS mos acq photom ss 46 Table 17 parameters Tor VIMOS img oe E 47 Table 18 parameters for VIMOS img obs Jiitter noconocnnncnnn enne 48 Table 19 parameters for VIMOS img obs Autojiitter m u u umeresisesssmseessrassssaesesasnnssanssnsrsnsnsnsnesasnnesvenersene 48 Table 20 Parameters Tor VIMOS MOS DDS DIE 49 Table 21 parameters for VIMOS mos obs Jitter us 50 Table 22 parameters for VIMOS mos obs Stare misil e 51 Table 23 parameters for VIMOS ifu obs Jitter ss 52 Table 24 parameters for VIMOS ifu obs Autojitter ss 52 Table 25 parameters for VIMOS me cal DA oio eser unanimement 54 Table 26 parameters for VIMOS img cal FADOME sn duces Seat naissent 54 Table 27 parameters for VIMOS me cal PIatSEy uie cvurvsoudsassnssese
68. rs This mode has two functions produce science images and produce the preliminary images needed to register the slit masks to the position of targets on the focal plane of the VLT UT3 The filters available for imaging are U B V R I and z Filters characteristics are given in section 8 1 It is possible to install user filters in each of the 4 filter exchange units However this requires to remove one of the filters already in place The field of view as projected on the sky is shown in Figure 1 5 2 Performances Performances are given in Table 4 section 2 3 5 3 Observation preparation The preparation of observations require the following e List of equatorial coordinates 0 0 and epoch of reference e Filters to be used e Exposure times e Dithering jitter pattern list of differential pointing positions around a central position Standard imaging techniques are using several short images exposure times such as the exposures are sky background limited observed at each position of a dithering pattern to reconstruct an image with the total exposure time required This allows to eliminate cosmetic defects on the detectors as well Word Windows 2000 Fichier vimos users manual v1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 25 as cosmic rays and to produce very accurate flat fielding to correct for detector pixel to pixel variations 5 4 Observing sequence Th
69. rt the proper grism filter e Take series of MOS exposures offsetting targets in between each exposure of the sequence if required 6 5 Calibration The required calibrations are e Flat fields taken at twighlight e Arc lamps spectra taken during the day Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page e Spectrophotometric calibration standards 6 6 Data Processing 7 Integral Field Spectroscopy 7 1 Overview The Integral Field mode of VIMOS is used to obtain spectra of all 6400 resolved spatial elements in a contiguous area 54x54 or 27x27 arcsec This mode is set by using the integral field unit head located on the side of the MOS and imaging field of view and inserting 4 special masks at the entrance focal plane of the spectrograph The spectral resolutions available are derived from the equivalent slit width for the fibers micro lens combination of 0 95 arcsec 7 2 Performances In this mode a penalty is paid in terms of overall optical throughput about 75 that of the MOS mode However integral field spectroscopy does not suffer slit losses or overlapping spectra in crowded regions 7 3 Observation preparation The preparation of observations require the following e List of equatorial coordinates 0 0 and epoch of reference e Grisms filters to be used e Exposure times e Dithering jitter pattern list of d
70. s with the position of the same objects in the newly acquired image an offset is computed and applied to the telescope The procedure is iterated till the difference between the two positions is less than 0 1 arcsec or when user stops it It is recommended to enter a guiding wavelength as near as possible to the central wavelength of the grism to be used for the scientific observation to minimize the effects of the chromatic atmospheric refraction Word Windows 2000 manual v I Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 46 9 1 3 2 VIMOS mos acq photm This template is intended in conjuction with Calibration Template VIMOS mos cal photom It ONLY presets the telescope to the Target position and does NOT start guiding as this task will be done by VIMOS mos cal photom after having offsetted so that target is within calibration slit Table 16 parameters for VIMOS mos acq photom Parameter Name Description Guiding lambda Wavelength for guiding Alpha Offset Additional pointing offset in RA Delta Offset Additional pointing offset in Dec On top of these parameters the target description should be filled in at least with Right Ascension Declination Equinox and Epoch Note that the pointing coordinates in the target description will correspond to the center of VIMOS FOV Word Windows 2000 Fichier vimos users manual
71. s users manual v I LAS r f 59 Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page Grism Wheel Grism to be used Low resolution Blue or Red High resolution Low Red or orange Medium Resolution Number of exposures Number of exposures to be made Exposure Name root name for resulting files 4 Quadrant Flag Flag to point calibrator in the 4 quadrants T F Slit Height Required Slit height in Arcsec Fine Alignment Flag to refine alignment with mask ADP File 1 Name of ADP File for Quadrant 1 ADP File 2 Name of ADP File for Quadrant 2 ADP File 3 Name of ADP File for Quadrant 3 ADP File 4 Name of ADP File for Quadrant 4 ADM File 1 Name of ADM File for Quadrant 1 ADM File 2 Name of ADM File for Quadrant 2 ADM File 3 Name of ADM File for Quadrant 3 ADM File 4 Name of ADM File for Quadrant 4 Mask 1 ID Mask ID of Quadrant 1 mask Mask 2 ID Mask ID of Quadrant 2 mask Mask 3 ID Mask ID of Quadrant 3 mask Mask 4 ID Mask ID of Quadrant 4 mask Cabinet 1 Slot Number Position of mask in Cabinet 1 Cabinet 2 Slot Number Position of mask in Cabinet 2 Cabinet 3 Slot Number Position of mask in Cabinet 3 Cabinet 4 Slot Number Position of mask in Cabinet 4 The template assumes that telescope has been pointed on the calibration field it will itself take care of shifting the pointing so that the calibration star falls on the chosen slit i e t
72. serve a field in direct imaging mode VIMOS img obs Stare Observe a field in direct imaging mode slightly shifting the pointing from one exposure to the next in a user defined pattern VIMOS img obs Jiitter Observe a field in direct imaging mode slightly shifting the pointing from one exposure to the next in a random pattern VIMOS img obs Autojiitter observe a field in multi object spectroscopic mode VIMOS mos obs Stare observe a field in MOS mode slightly shifting the objects along the slit from one exposure to the next VIMOS mos obs Jitter observe a field in IFU mode VIMOS mos obs Stare observe a field in IFU mode slightly shifting the pointing from one exposure to the next in a user defined pattern VIMOS ifu obs Jitter observe a field in IFU mode slightly shifting the pointing from one exposure to the next in a random pattern VIMOS ifu_obs_Autojitter 3 Requesting observing time and preparing observations with VIMOS 3 1 Call for proposals The observers are referred to the VLT call for proposals http www eso org proposals for an up to date status of the observing policies at the VLT offered instruments and modes etc 3 2 Exposure time calculator The exposure time calculator ETC is available at http www eso org It allows to compute exposure times for a variety of sources and instrument observing modes Word Windows 2
73. t 02 page 23 E 4 ete 3E 2 e sonate mamanman on pa 0 500 1000 1500 radius pix Figure 9 Image quality FWHM vs distance from the optical center in pixels quadrant 4 The FWHM measures the images of pinholes 300 microns in diameter distributed in a grid at the mask focal plane The specification is shown as a dashed line as FWHM 3 2pix the measured image quality is 2 pixels FWHM over the field Figure 10 PSF variation accross the VIMOS field at the field center and field edges images of 300 microns holes 4 2 Guiding and offsets Guiding and offsets are executed with the telescope control system The user can offset the telescope from the OS panel either as X Y pixel offsets on the detector or a values in arcseconds 4 3 Flexures and tracking stability Flexures are currently within 1 2 pixels for channels 1 2 3 see Figure 11 and 2 pixels for channel 4 Word Windows 2000 Fichier vimos users manual v1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 24 Q2 DE Bo n fi j CO 22 0 Cw x Our 4 l d 2 0 Xx pix Figure 11 flexures measured for channel 2 The circle represents a motion of 1 pixel from central reference S Direct Imaging 5 1 Overview Direct imaging 1s used to produce wide field images VIMOS is the largest imager on the VLT using broad band filters or specific user filte
74. tter for IFU Unit T F Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 62 IFU Magnificator Magnification for IFU Unit T F Readout Mode CCD read out mode fast medium slow Number of exposures Number of exposures to be made Exposure Name Root name to be given to resulting files The template assumes that telescope has been pointed on the calibration field it will itself take care of shifting the pointing so that the calibration star falls NEXT to IFU center and consequently its spectrum in the first operative quadrant Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 10 Annex A Start up and shut down procedures Start up procedure e e n e e e e Hardware on platform Power on the 2 LCUs Power on the 2 FIERAS and associated electronics Verify that detectors have proper temperature and cooling Software on instrument workstation Open session on VIMOS worstation Login VIMOS password vimos2me Run task vmmsStart Select configure and start all subsystems processes ICS DCS1 and DCS2 OS see figure A 1 OS panel opens up select ONLINE in menu COMMANDS STATUS After 5 7 minutes the system status should be indicated ONLINE and IDLE on upper right of the OS panel
75. ual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 67 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 Date 24 Oct 02 page 68 CNRS LABORATOIRE D ASTRONOMIE SPATIALE VIMOS OS TYPE OPERATOR INS_USER SYSTEM File Options Commands Tools cag Type Tech Expo File Exp Id Exposure Count Down PSTRTEISUEST AT Eee VIMOS EE eum 00 00 00 ONLINE Expo Name new Data lt ExposureTime 1 IDLE A EXPOFILE 0015 A fi EXPOFILE 0015 B f Instrument Mode ADM file TFT a Phase Finished Requestor E WCS 1 Seq Naming 16 Bi s M Archive Header Bo M Save exposure file DCS ONLINE wssm omme vs sm PYS Unknown Unknown de Preset Offsets NO TCS Vimos 225 LL 1x1 Low Gain medium IFU devices Gain Ron Speed medium de d ux 2048 1 Elongator Off 2i NY 4096 Fa n l A Xx 1 rar Cr 7I Allowed 5 binning y 1 Exposure type Normal FOMP mode a oe rens enl No Telescope vif FOCUS mode norepeat w repeat Manual Period any 0 Times 1 Exposure Time sec 1 15 15 15 15 ere story pan ERR emen Comments Action Log w Disk Space y Exposure History OR PROFILE comma
76. v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 9 2 Observation Templates Observation templates define a restricted set of possible instrument configuration Observations carried out using these templates can later on be reduced using VIMOS DRS reduction recipes Observations which could be done using different instrument settings are not supported by DRS recipes and Automatic pipeline 9 2 1 Imaging Mode All imaging mode Observation templates allow usage of PHOTOMETRIC FILTERS ONLY and of Imaging CCD readout mode ONLY i e only the central 2048x2340 pixels are read 9 2 1 1 VIMOS img obs Stare Generic purpose template to observe a field in Direct Imaging Mode If more than one exposure is requested Numebr of Exposures gt 1 each exposure will be Exposure time seconds long Table 17 parameters for VIMOS img obs Stare Parameter Name Descritpion Exposure time Exposure time for one observation in seconds X binning factor Binning factor in X direction 1 or 2 Y binning factor Binning factor in Y direction 1 or 2 Readout Mode CCD read out mode Fast Medium Slow Filter Name Photometric filter to be used U B V R Lz Number of exposures Number of exposures to be made Exposure Name Root name for resulting files 9 2 1 2 VIMOS img obs Jitter Template to observe a field in Direct Imaging Mode slightly shifting the pointing from one exp
77. wn to only a few arcseconds 8 Word Windows 2000 manual v1 Fichier vimos users LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 9 VIMOS Field of View The VIMOS field of view is outlined in Figure 1 Note the relative position of the integral field and the imaging MOS field Figure 1 VIMOS field of view Table 3 VIMOS mechanical and optical characteristics Nasmyth focus VLT UT Opto mechanical 4 beams each a complete focal reducer F 1 88 output layout Wavelength coverage 0 37 to 1 um Throughput imaging 4x7 x8 224 arcmin imaging area 4x2048x4096 15um pixels R Spatial Sampling 0 205 arcsec pixel 10 max per channel U BVRIz filter set 170mm diameter Slit length 28 at high R 140 at low R 180 to 2500 1 arcsec slit 360 5000 0 5 arcsec Better than 2 pixels at 80 encircled energ Any position and shape Multiplex 840 simultaneous slits 10 long at R 200 4000A coverage 210 simultaneous slits 10 long at R 2500 3500A coverage Integral Field Spectro 54x54 arcsec field 6400 fibers with 0 675 sampling Word Windows 2000 Fichier vimos users manual v1 LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page 10 2 2 VIMOS general overview VIMOS is installed on the Nasmyth focus of VLT Unit Telescope no 3 Melipal VIMOS relies on the telescope for focusing de rotation w
78. you have to perform the following steps From the vmmps main panel Figure 12 select VIMOS MPS Load ASCII catalog eg file cat to open the cross correlation panel Figure 13 load your user catalog with your objects in the field produced from another observation Enter the FITS pre image after loading the VIMOS Star Catalog is asked for this is the catalog produced from the pre image After running the cross correlation select Cross good output number are nmatch gt 80 and rms lt 0 1 arcsec It produces a file named file vm cat including all objects from your input catalog with the proper VIMOS coordinates 6 4 4 SPOC From the vmmps main panel Figure 12 select VIMOS MPS Load ASCII catalog Load the file e g file vm cat A new window opens containing the full catalog of targets available in your field a yellow circle appears around each available target You have to select 1 or better 2 reference objects per quadrant which will be used for mask to sky alignment click with the cursor on the image of each reference object stellar is preferred and click ref on the panel a blue diamond appears around the selected object 26 Word Windows 2000 Fichier vimos users manual v I LAS r f Issue 1 0 R v 0 0 CNRS LABORATOIRE D ASTRONOMIE SPATIALE Date 24 Oct 02 page You may then select compulsory target or forbidden some of them clicking on the image of each and then o

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