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OSIRIS Users Manual - WM Keck Observatory

1. T370 0264799 1230117447 001060193 i ES m 1370 0264814 12 30 123487 47 001218018 9 1370 0204791 12 30 11 0013 gt 47 00 19 640 10 1370 0264807 12 30 12 3027 47 0012140 11 1370 028479412 301 1 2107 47 00 33 710 12 1370 0264799 12 30 11 0713 470025170 13 1370 0264803 12 30 12 0793 47 00 33 141137025417 123016240 47 15 1370 0264787 12 30 07 8640 47 01 07 280 18 1370 0284810 12 30 12 3840 47 0056820 255 142 170130264789 12 30 10 5713 47 0038150 246 12 25 3 15 2010 UCLA Infrared Laboratory 4 ete uiu o SESS TOY CALIFORNIA ASSOCIATION FOR RESEARCH IN OSIRIS USER MANUAL V 2 3 4 Observing procedures 41 User Interface Observational Planning GUI The OSIRIS planning GUI OOPGUI is your main interface for making observations It allows users to plan observational sequences on one field with both the spectrograph and imager Observers are able to change the filter scale coadds itime and dither patterns The Dataset and Object fields are used for header information The LGS mode is used to determine whether the laser should be dithered with your dither pattern or if it should remain fixed on axis File Queue Help IMPORTANT The Keb Kc3 Kc4 and 5 filters are designed to only be used with 100 mas scale Users must select both the combination of filter and the 100mas scale Spectrometer Only ly Imagen om
2. 78 A 5 3 Optimum Operating Temperature icd 78 250 Spectrograph Detector Crosstalk P e RE quai ome pne 78 Appendix B a a tel cioe au Oa ae or M Sa cals min 80 Appendix Atmospheric Transmission etae eaa genna te eon 84 Appendix D Atmospheric Dispersion sb pla bn ges 88 Dl Instrumental Chromatic Dispersion n aede rn 90 Appendix E FITS header keywords pete Ee dre e an 93 Appendix History of Instrument Changes Which matrices to use in reductions 102 Appendix G When all else fails Play Cowboy 105 E 3 15 2010 UCLA Infrared Laboratory 5 CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 1 OSIRIS Overview OSIRIS is an integral field spectrograph IFS designed to work with the Keck Adaptive Optics System It uses an array of tiny lenses to sample a rectangular patch of the focal plane and produces spectra at up to 3000 locations simultaneously There is also an internal diffraction limited camera with a 20 field of view Both the camera and spectrograph can operate at wavelengths b
3. Oc RU assum IM M yu E INE 64 3 15 2010 UCLA Infrared Laboratory oSE amp RK Av OU CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 23 9 I4 aa ah cea i a eat ss 65 5 9 15 Remove Hydrogen Lines 66 3 9 16 Rename not Rome upon e up buo bas UR RA 66 5 9 17 Save DataSet Information o UR ee ding 67 5 9 18 Scaled Sky Subtraction tae 67 Subtract PRAMS sns tie UR Re ea liuc ta viden Lu a genda Rp 70 Appendix A Detector Performance pr Y e e Re Trend A a n banana 71 Characterization Data aia ie basi uestri dA 71 A2 Memory Chars ee ia eae dm ea 72 Fixed Pattern Noise and 21 41 4 8 20 2 5 0600 73 A 4 Spectrograph Detector and Detector Controller 75 A 5 Optimization of Detector Operating Temperature sse 77 A 5 1 Temperature Dependence of QE 77 A 5 2 Temperature Dependence of the Reset Anomaly
4. rFr Lt or oro T 1 T T T T Best Lenslet 4500 4000 Median Lenslet 3500 Spectral Resolution T TT LITT TTTT 3000 Worst Lenslet 2500 gt d oa uari p ei 01 01 01 1 2000 2100 2200 2300 2400 Wavelength nm Figure 2 7 The spectral resolution depends on lenslet number and wavelength This graph shows the resolution as a function of wavelength in the 3 order band over the primary 16x64 lenslet positions median resolution at each wavelength the highest resolution region lenslets near 22 50 and the lowest wavelength region lenslets near 38 12 Other bands are simple scalings of this relationship i e the J band is observed in 5 order so the same resolution occurs at 3 5ths of the wavelengths shown in the graph This is for the 0 050 scale although the 0 020 and 0 035 scales are similar 18 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONomMY OSIRIS USER MANUAL V 2 3 25 Lenslet Fill Factor According the test report supplied by the manufacturer there is a 2 3 micron rounding between the nominally square lenslets This results in a fill factor of approximately 95 Additionally the test report supplied by the manufacturer indicates that the transmittance of the lenslet array is between 95 and 97 The peak transmittance is at 1 2 um 26 Concentricity of the Four
5. aes 19 2 1 Optical Error BUdBeb e nope dad ied 20 MD Et Do boc 21 2 05 e idu e uter eme eut ied 22 240 M 23 3 Observing with Adaptive Optles ec ere Giles i ded a bae ba dte dd e a pe Pn e ven 25 4 JODServinp procedures dores u E pope o eae ies 26 4l User secte ea aee etu E uM EE 26 4 2 Field Acquisitions acne ere ess vetus 34 4 3 Spectroscopic Calibratio estre hat teet oae ond t dn xu dd 36 43 1 belluric Standards ner eee eb o tenia d ptis ave 36 4 3 2 Wavelength Calibrations S tas RE peint per Ne dsl dea baie Ius 36 5 Data Reduction Svstellise s usta ettet veiut ean as Ede 39 5 1 Major Changes to the Pipeline for Version 2 2 sss 41 5 1 1 Changes to Pipeline for Version 2 1 42 5 1 2 Changes to Pipeline for Version 2 0 42 5 2 Installing the Pipeline at Your Home Institution essere 43 5 3 ODRFGUI The OSIRIS Data Reduction File GUI seen 45 5 4 Working Directl
6. 0 gt module Name Clean Cosmic Rays Skip 0 gt lt module CalibrationFile irchive osiris calib SPEC rectification s050624 071 infl_Hn3_100 fits Name Extract Spectra Skip 0 gt module Name Assemble Data Cube Skip 0 gt lt module Name Save DataSet Information OutputDir projects osiris DRP larkin gt lt DRF gt 5 5 2 Output Filename Construction When the pipeline saves output files it builds the name from the FITS header In particular the header keyword DATAFILE acts as the filename base Normally this is set to the FITS file name when the original data is written In addition the three letter filter designation e g Kbb or Hn4 and the plate scale in mas 020 035 050 or 100 are appended to this basename If the input file is 5070406 a029001 fits then the output file could be something like s070406_a029001_Kbb_100 fits In the case where the filter is a dark then the scale is irrelevant and no scale is appended In this case a file might be named 5070406 035001 Drk fits a few modules they will modify the DATAFILE keyword so reduced files receive an additional extension The Combine Frames module adds a combo to the DATAFILE keyword so files become 5070406 a029001 combo Kbb 100 fits where the basename is from the first file specified in the DRF reduction script The Divide by Star Spectrum adds tlc to filenames to indicate that they have been corrected for
7. 1 DN baseline variation from channel to channel Shift register glow Figure A 2 Spectrograph Detector Pattern Noise and Shift Register Glow The outlined areas at the top left in the figure correspond to 2 of the 8 readout channels in the upper left quadrant of the Hawaii 2 The figure also shows four areas of glow from the multiplexer and this is attributed to the shift registers The channel to channel baseline variation increases if the temperature is not stable This is shown in Figure A 3 a dark frame taken at 69 K while the device was allowed to warm up CCR off no temperature controller in operation The baseline variation has increased to approximately 9 electrons 3 DN The number of hot pixels and other artifacts increases as the temperature is further increased This is shown in Figure A 4 and Figure A 5 73 3 15 2010 UCLA Infrared Laboratory oSEEK ar OSIRIS USER MANUAL V 2 3 Figure A 4 Spectrograph Channel to Channel Variation at 73 K 74 3 15 2010 UCLA Infrared Laboratory qiiis giis o SEES CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY 4 OSIRIS USER MANUAL V 2 3 Figure A 5 Spectrograph Channel to Channel Variation at 75 K Spectrograph Detector and Detector Controller Characterization data for the spectrograph detector and detector controller as a system are given in Table 9 Note that since the detector is very linear to large well depths and applying a linearity c
8. gt fits FileName s051123_a013001 fits gt fits FileName s051123_a013003 fits gt fits FileName s051123 a014001 fits gt lt dataset gt module CalibrationFile projects osiris DRP Sky_900_datset_Hn3_100_0 fits 54 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 Name Subtract Frame gt module Name Adjust Channel Levels 0 gt module Name Remove Crosstalk Skip 0 gt module Name Glitch Identification Skip 0 gt module Name Clean Cosmic Rays Skip 0 gt lt module CalibrationFilez irchive osiris calib SPEC rectification s050624 071 3 100 fits Name Extract Spectra Skip 0 gt module Name Assemble Data Cube Skip 0 gt module Name Mosaic Frames Combine Methodz AVERAGE Offset Method TEL Skip 0 1 gt lt module gt lt DRF gt Notice one important difference with this reduction compared to others There is no call to Save DataSet Information Instead the 1 flag has been added to the Mosaic Frames call itself This will cause the mosaicked frame to be written to disk and two additional extensions will be attached to the FITS file The output FITS file will contain the image as the 0 extension a noise frame as the 1 extension a bad pixel map as 2 extension map of how many original images were combined at each outp
9. Change in the measured dark current after readout for pixels exposed to 90 or more of the maximum detector charge storage capacity Excess dark current at the level of a 0 01 e sec is detectable many hours after the detector is exposed to light even if not saturated Rockwell measured 12 69 e with output amplifiers Rockwell measured 0 026 e pixel sec for a 14 400 sec exposure after a long period of dark soaking For a 20 minute exposure at a detector temperature of 67 K using CDS This is the average injection of flux or charge generated in a pixel from reading out the device one time Data supplied by manufacturer Ae 3 15 2010 UCLA Infrared Laboratory 4 456 44 lt ATOR CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER 2 Memory Charge memory charge phenomenon was observed during the lenslet scans used to perform spectrograph calibration During the scan the mask stage is used to isolate each lenslet column and a spectrograph exposure with a continuum source is taken for each lenslet column Figure A 1 shows 4 images taken under similar conditions to a lenslet scan The upper left hand panel of the image is a 40 second exposure taken with the H broad band filter with a single lenslet column illuminated to produce a nearly saturated exposure 85 000 electrons In the first dark shown in the upper right hand panel taken after the nearly saturated exposure
10. afterwards This will cause the shift and number frames to be attached to the FITS file as additional extensions Mosaic Frames requires you to specify the method to combine overlapping pixels AVERAGE MEANCLIP or MEDIAN and the method to determine the dither between the frames FILE TEL NGS or LGS Examples lt module Name Mosaic Frames Combine Method AVERAGE Offset Method TEL Skip 0 Save 1 gt lt module gt 64 3 15 2010 UCLA Infrared Laboratory MT CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 5 9 14 Remove Crosstalk Brief Description If a bright spectrum covers most of the rows of one of the 32 detector outputs then the other 31 will show a crosstalk signal from the electronic effect on the detector The level of this crosstalk is approximately 196 of the bright signal Tests revealed that the crosstalk is constant across the row of an affected channel and it is in fact constant for all 32 channels The Remove Crosstalk measures this value and subtracts it from all 32 affected rows It requires that at least one of the rows has an actual average signal more than 50 times the crosstalk value The figure below shows the pre and post crosstalk removal on a bright telluric standard star The module is not necessary on faint sources but is relatively quick and does not harm the data Figure 5 1 On the left is a raw spectrum of a bright star showing vertical stripes
11. the GUI will attempt to locate the appropriate calibration file based on the module and the filter and scale of the input files The calibration file directory can be set using the Set Calibration Directory option in the File menu When a valid calibration file is found the text turns from red to black Input files are added using the Add Files button above the input file list 45 3 15 2010 UCLA Infrared Laboratory ard 45 CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 o3 MM Ei Data Reduction File GUT Ele File Tools Help Input Files Add Files Remove Files Clear List inetihelium data rchive osiris 070517 SPEC raw s070517 a035002 fits inetihelium data rchive osiris 070517 SPEC raw s070517 a035003 fits inetihelium data rchive osiris 070517 SPEC raw s070517 a035004 fits Filter Kbb Scale 0 035 Dataset Name Automatically create dataset name from input files Output Path inetihydrogen datajprojects osiris DRP larkin 070517 LogPath 5 2 70517 2 lt Reduction ARP SPEC B Reduction Templates basicARP drfTemplate xml Available Modules Module Name Skip Find File Resolved Filename Subtract Frame Subtract Frame 1 Specifyafile et helium data rchive
12. the wavelength dependence of this solution He compared four broadband Z J H K summer 2009 observations and found that there is a systematic shift between each of these filters This wavelength dependency is plotted in Figure 4 2 090501 Kbb 50 mas Rel 090501 Kbb 50 mas Abs 60 60 090507 Kn3 35 mas Rel 090507 Kn3 35 mas Abs pix Ang pix Ang 50 0 300 50 1 000 0 300 1 000 0 217 0 667 0 217 0 667 49 0 133 49 0 333 0 133 0 333 0 050 0 000 0 050 0 000 30 30 0 033 0 333 0 033 0 333 20 0 117 20 0 667 0 117 0 667 0 200 1 000 0 200 1 000 10 10 0 10 20 30 40 50 0 10 20 30 40 50 Mean 0 00 sigma 0 03 Mean 0 08 sigma 0 06 0 0 5 10 15 0 5 10 15 Mean 0 04 sigma 0 04 Mean 0 17 sigma 0 11 Figure 4 1 Relative and absolute pixel and angstrom offsets for broadband and narrowband field of views measured using OH lines Tuan Do measured these offsets using Kbb 050 and Kn3 035 reduced cubes from May 2009 These are residual offsets after using the new Assemble Data Cubes v2 3 with the temperature dependence of the grating and the new spatial dependent wavelength solution If additional accuracy is needed for your program then we recommend reducing one of your frames with a dark frame for subtraction This will leave OH lines in the spectrum that can then be fit for their spectral position as a function of lenslet The OH lines then serve as a local spectral reference close to your science wavelengths At the long end
13. 102973 0 116827 0 126736 0 134068 0 139644 45 1 41 0 061534 0 098637 0 122718 0 139228 0 151038 0 159776 0 166422 50 1 56 0 073333 0 117551 0 14625 0 165926 0 18 0 190413 0 198333 55 1 74 0 08788 0 140868 0 17526 0 198839 0 215705 0 228183 0 237675 60 2 00 0 10658 0 170844 0 212554 0 241151 0 261605 0 27674 0 28825 65 2 37 0 13196 0 211528 0 26317 0 298576 0 323902 0 34264 0 356892 70 2 92 0 169063 0 271003 0 337165 0 382526 0 414973 0 43898 0 457239 75 3 86 0 229647 0 368117 0 45799 0 519606 0 56368 0 596289 0 621092 88 3 15 2010 UCLA Infrared Laboratory Zenith Angle 10 15 20 25 30 35 40 45 50 55 60 65 70 75 oS S5 aro 45 ifite RY CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 What is often more important is the amount of image elongation within a particular filter The table below gives this elongation for all of the OSIRIS filters In the spectrograph this results in a motion of the centroid of an object in the parallactic direction as a function of wavelength Airmass 1 004 1 015 1 035 1 064 1 103 1 155 1 221 1 305 1 414 1 556 1 743 2 000 2 366 2 924 3 864 Zbb 0 006 0 012 0 019 0 025 0 032 0 040 Jbb 0 004 0 008 0 013 0 017 0 022 0 027 0 033 0 040 Hbb 0 003 0 005 0 008 0 011 0 014 0 018 0 022 0 026 0 031 0 037 Kbb 0 001 0 003 0 004 0 006 0 008 0 010 0 012 0 014 0 017 0 020 0 024 0 029 0 036 2 2 0 0
14. 1700 roughly the number of spectral channels This will give you the number of DN per spectral channel and compare that to 4 data numbers to get a rough signal to noise for an individual exposure for each lenslet 252 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONomMY OSIRIS USER MANUAL V 2 3 2 10 Imager The imager uses a Hawaii 1 detector from Rockwell Scientific and has a 1024x1024 pixel format The plate scale is 0 020 arcsec per pixel for a total field of view of 20 4 arcsec It is sensitive from 1 to 2 5 microns The minimum exposure time is 2 seconds and times are limited to integer seconds The imager holds virtually an identical set of filters as the spectrograph but due to space within the filter wheels does not have Zn2 Zn4 Zn5 or Jn4 filters see Table 1 The imager field is offset from the spectrograph so that both can be used simultaneously without the need for beam splitters or dichroics There were several motivations for the imager including field acquisition and imaging science But the primary purpose of the imager and the reason for simultaneous viewing is to track changes in the point spread function PSF As with all adaptive optics systems the image quality is continuously changing and is difficult to predict purely from the wavefront sensor data Also for many science cases the spectrograph target cannot be used to measure its own PSF So the imager s goal is to me
15. 5 Optimization of Detector Operating Temperature Certain detector performance parameters exhibit significant temperature dependence The parameters of greatest concern in our application are the temperature dependence of the dark current the temperature dependence of the reset anomaly and the temperature dependence of the device QE To characterize the optimal operating temperature of the detector a series of short and long exposures were taken at 67 and 70 K These included both darks and white light spectra using the Zn3 Jn3 Hn3 and Kn3 filters The white light source was turned on approximately an hour before the tests began to try and eliminate changes in long wavelength heat flux from the white light source as a significant source of error We currently operate the detector heater at a low power level about 0 150 W so approximately 3 hours were required for the detector to transition between 67 K and 70 K Given the long timescales involved the QE measurements may include variations due to changes in the long wavelength heat flux from the white light source A 5 1 Temperature Dependence of QE The results show that between a temperature of 70 K and 67 K the QE of the spectrograph detector drops by 9 in the K band 11 in the H band 15 in the J band and 18 in the Z band These numbers are a factor of roughly 3 higher than more tightly controlled tests performed by Gert Finger of ESO on similar devices Figure A 7 taken from the
16. AO 4 3 2 Wavelength Calibrations The OSIRIS wavelength solution is calculated in vacuum units The IAU standard for conversion from air to vacuum wavelengths is given in Morton 1991 ApJS 77 119 and is reproduced here A Avac TS 131 4182 2 76249 x10 1 0 2 735182 107 I Avac The wavelength solution is extremely stable and the user does not need any additional observations A single global wavelength calibration comes with the pipeline with the routine Assemble Data Cubes Before pipeline version 2 0 the wavelength solution was solely based on arc line positions produced from a set of calibration lamps These don t fill the pupil uniformly so the line centers appear to have a slight wavelength shift usually about 0 1 pixels 0 3 nm in K band or less but in some regions as much as 0 5 pixels To achieve a better wavelength solution Tuan Do was able to use the cross correlation of OH lines in the Kn3 filter and determine an average shift for each lenslet between the arc line positions and sky line locations which should uniformly fill the pupil like an astrophysical object This offset has now been implemented in versions greater than 2 0 of the pipeline and significantly improves the differential line shifts from one lenslet to another During the warmer operating temperatures of OSIRIS between January and August 2009 the wavelength solution had to be adjusted as a function of the grating temperature The
17. FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 5 Data Reduction System Reducing data with OSIRIS is actually quite similar to reducing other infrared images and spectra Since the infrared background is bright and complicated it is very important to have sky frames for subtraction Like images these can sometimes be made by dithering on chip in this case lenslet Each lenslet s spectrum is also basically the same as any other spectrograph s spectrum But there can be over 3000 of them and each has a slightly different path through the optics so each spectrum has slightly different spectral dispersion resolution and PSF quality The most unique aspect of the instrument is that the 3000 spectra all partially overlap on the detector and do so at staggered wavelengths A very custom routine is necessary for uniquely assigning flux from detector pixels back into lenslet spectra We call this the Spectral Extraction process and it is quite similar to Lucy Richardson deconvolution Maps of the point spread function of each lenslet are made at all wavelengths called Rectification Matrices or Extraction Matrices These maps are referenced in the extraction process These matrices appear to be extremely stable lt 0 1 pixels over an indefinite period of time and the user does not need to take new matrices on their own It is important however that you retrieve a set of matrices that match your data There is a di
18. Figure 5 2 Output window after the Scaled Sky Routine is performed Example module Name Scaled Sky Subtraction Min Sky Fraction 0 1 Max Sky Fraction 0 25 Line Halfwidth 4 0 Scale K Continuum YES Show Plots YES CalibrationFile net hydrogen data projects osiris DRP mperrin inputs BPPsc H 32 SKY fits gt 69 3 15 2010 UCLA Infrared Laboratory 44 3 aids CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomMY OSIRIS USER MANUAL V 2 3 5 9 19 Subtract Frame Brief Description Basic routine for subtracting two frames This routine is commonly used as the first module of a standard DRF Usage In addition to Name the CalibrationFile must be specified This will be the full path and name of the file to be subtracted Examples module CalibrationFile projects osiris DRP Sky_Hn3_100_0 fits Name Subtract Frame gt 70 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONomMY OSIRIS USER MANUAL V 2 3 Appendix A Detector Performance Tests were performed at a series of temperatures ranging from 65 K to 75 K In addition to testing basic parameters such as read noise and dark current we found and attempted to diagnose a host of phenomenon seen with the detector Of particular importance is the discovery that clocking the array at intermediate temperatures creates a large number of hot pixels This phenomenon was subsequently verified in discussions with Rockwell S
19. Then the xml file lists all of the raw fits files that are to be combined dataset InputDir net hydrogen data irchive osiris osiris8 051 123 SPEC raw gt lt fits 5051123 a000004 fits gt fits FileNamez s051123 a000005 fits gt fits 5051123 a000006 fits gt fits 5051123 a000007 fits gt fits 5051123 a000007 fits gt fits 5051123 a000008 fits gt fits 5051123 a000009 fits gt fits 5051123 a000010 fits gt fits 5051123 200001 1 fits gt lt dataset gt Now call the big four routines Glitch Identification to find any detector glitches Note that two of the other big four routines Remove Crosstalk and Adjust Channel Levels are not needed because these data typically have no bright stars present and varying channel levels are handled by the special Combine Frames module The Clean Cosmic Rays routine should not be called on individual raw files that have not had another file subtracted because the many hot pixels on the chip will be marked as bad Also since you are typically combining several frames cosmic rays are naturally removed by the Combine Frames module lt module Name Glitch Identification gt Now run the main routine for combining the data frames together It averages all pixels together at a given location lt module Name Combine Frames Skip
20. directions at the quadrant boundary and in both cases runs along the fast direction This and other similar measurements indicate that the ghost is electronic in nature and occurs when an entire row has a strong signal on it If there were crosstalk directly between the pixels that were being simultaneously addressed then the actual spectra in left quadrant which are nearly saturated would create vertical ghosts in the right quadrant Such ghosts are not seen the only ghost in the right quadrant runs horizontally and can be identified with spectra from the upper left quadrant not shown which again run along the fast direction row These near saturated rows occur only in the calibration lenslet scans where essentially all pixels along a given row are exposed to near full charge capacity Additionally the contrast between the spectra and the electronic ghosts is close to 100 1 making their impact minimal 78 3 15 2010 UCLA Infrared Laboratory i gt CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 ana sits oS ERE are Figure A 8 Spectrograph Detector Crosstalk Image 79 3 15 2010 UCLA Infrared Laboratory 4 ets 411 KERKE PE ae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 Appendix B Filter Curves Also see http www2 keck hawaii edu inst osiris technical filters filter index html and Appendix D where the atmospheric spectrum is sho
21. due to electronic crosstalk within the detector On the right is the same spectrum after the Remove Crosstalk module Usage The only command words recognized are Name and Skip Examples module Name Remove Crosstalk Skip 0 gt 65 3 15 2010 UCLA Infrared Laboratory SSES arde CALIFORNIA ASSOCIATION FOR RESEARCH IN AsrRoNouwY OSIRIS USER MANUAL V 2 3 5 9 15 Remove Hydrogen Lines Brief Description Remove Hydrogen Lines takes a 1D spectrum and attempts to remove absorption lines due to hydrogen The primary purpose is to remove hydrogen absorption lines from telluric standard stars Because there are sometimes atmospheric and instrumental features at the same wavelengths we must fit both the line and a local background and subsequently subtract this line fit This tends to leave higher frequency features unaffected For each line a region from 7 less than the wavelength to 7 more than the wavelength is used for the fitting region The lines removed are the following wavelengths in nm Paschen series 10 901 2 Pa9 922 6 Pa8 954 3 Pad 1004 6 1093 5 Pap 1281 4 1874 5 Brackett series Br15 1570 7 Br14 1588 7 Br13 1611 5 Br12 1641 3 11 1681 3 10 1736 9 1818 1 1945 1 Bry 2166 1 Usage The only command words recognized are Name and Skip Examples lt module Name Remove Hydrogen Lines gt 5 9 16 Rename Files Brief Description This module lets you easily change the ou
22. groove density is directly related to the operating temperature of the grating and the coefficient of expansion of aluminum We have modified the module Assemble Data Cubes to use the temperature of the grating from the header of each frame to determine the final wavelength solution for each cube Within the module we reference the wavelength solution to a stable period of OSIRIS during July 01 2006 which had a well measured wavelength solution and uses the coefficient of expansion of Al for a given temperature of the grating during this 36 3 15 2010 UCLA Infrared Laboratory oSESK ar did CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 reference date Tref We use the following formula to find the new wavelength solution Anew using the temperature at the time of each of your raw frames Anew Aref 1 Cai Tret 1 5 Claes In July 2009 Tuan Do took this new wavelength solution and investigated its performance in multiple OSIRIS filters Assemble Data Cubes v2 3 uses this new spatial dependence solution derived by Tuan Do relative calibration in Kn3 was found to be 0 0 0 3 pixels with a max deviation of 0 15 pixels and an absolute calibration of 0 08 0 06 A with a max deviation of 0 6 A Figure 4 1 illustrates the relative and absolute offsets for broadband and narrowband field of views using observed central location of OH emission lines Tuan Do also investigated
23. make a dark frame from many identical darks or an average sky frame from many identical skies The routine treats each of the 32 output channels individually and matches them in level and then combines the frames using an average of the overlapping pixels to produce the final frame It does not match each output channel to another since that is the job of the Adjust Channel Levels module Usage The only command words recognized are Name and Skip Examples module Name Combine Frames Skip 0 gt 5 9 6 Correct Dispersion Brief Description This module corrects for spatial shifts as a function of wavelength by shifting spectral slices to match the true position of the star relative to the first channel shortest wavelength in the cube This should always be run before using Extract Star module This routine calculates the position angle and elevation from headers keywords so no parameters or input files are needed See Appendix D for details on the algorithm Usage The only command words recognized are Name and Skip Examples module Name Correct Dispersion Skip 0 gt 5 9 7 Determine Mosaic Positions 59 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomMY OSIRIS USER MANUAL V 2 3 Brief Description The routine takes sets of individual reduced data cubes and tries to determine the spatial offsets between the cubes It does a cross correlation of the flux to es
24. of K band this does not work since the last OH line is around 2 2 microns It is likely that some of the weak atmospheric 284 3 15 2010 UCLA Infrared Laboratory SSES pb CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 absorption features at the end of K band might provide a suitable reference but we have not tested this process 1 0 0 5 pup TII 0 0 Observed Reference Ang T reel 1 1 E D 2090610 t Connsns 090501 090507 Zbb Jbb Jn3 Hbb Kbb 1 0 Loa aqu du cuta c j a ou cu 3 ica 1 0 1 2 1 4 1 6 1 8 2 0 22 Wavelength microns o 8 o Figure 4 2 Wavelength dependence of the offset of measured OH lines from vacuum wavelength for all four broadband filters measured by Tuan Do The offset is compared to the observed central wavelength of an individual OH emission line compared to the vacuum position Each point was measured for a single line and is the mean observed wavelength value for the central 182 lenslets The black points were measured with broadband data cubes and the blue points were measured using narrowband filters 38 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION
25. relative to the first sky frame by 0 35 west There are multiple dither pattern options to select from Stare no dither Box 4 Box 5 Box 9 Raster Scan Statistical and User Defined The Show Position List button opens another window bottom left image that lists all the frames with their x and y offsets of the dither positions It shows sky frames and the sequence of the observations You may change the order of the frames by selecting one of the frames and using the Up Down Top and Bottom buttons as demonstrated on the bottom right image which now has the last sky frame number 5 being taken at the beginning of the observation sequence e e Dither Positions VIO Dither Positions 2 Xoff Yoff Sky Xoff Yoff Sky 1 0 000 0 250 z 1 5 350 5 250 v 2 0 000 0 500 2 0 000 0 250 1 3 0 000 0 750 B 3 0 000 0 500 E 5 000 5 250 4 0 000 0 750 5 5 350 5 250 v 5 5 000 5 250 Up Down Bott Top Up Down Bott OK OK 27 3 15 2010 UCLA Infrared Laboratory ar dide CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 If you are taking imager frames as well the dither pattern chosen will reflect both the spectrograph and the imager since they are fixed relative to each other bottom left image The imager has several options Disable SPEC only Independent Imager only Maximum Repeats M
26. the OH lines in your science data cube and the OH lines in a sky cube Then one can apply multiplicative scaling factors to the lines in your sky cube in order to minimize the residuals in the final subtracted cube The scaling ratios are applied to the entire sky data cube rather than to an extracted spectrum such that any spatial or wavelength variations in the sky lines across the cube will still be accurately matched and cancelled out in the sky subtraction Interested users should refer to Davies 2007 for a detailed description of the algorithm Not only does this provide superior sky subtraction than the conventional direct subtraction even better it allows a small number of sky frames to be re used to reduce a much larger number of science frames hence improving observation efficiency Davies reports for SINFONI data being able to use a single H band sky frame for over an hour of science data or a single K band sky frame for an entire night Thus far testing with OSIRIS data shows very good results as well We will not definitively answer the question how few skies can you get away with since that will depend on the sky subtraction precision needed for your science goals but it seems that you can take perhaps one sky frame per hour or maybe a bit less and still get good subtractions 67 3 15 2010 UCLA Infrared Laboratory oS ESS PEE CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL Usage V 2 3 Caveat
27. the start of frame was about 20 seconds after the slit mask moved to the dark position the peak signal at the locations of the bright spectra is about 120 electrons In the 274 dark shown in the lower left panel the peak signal is about 25 electrons and in the 3 dark shown in the lower right panel the peak is below 10 electrons In the 4 and 5 darks the persistence was imperceptible Near saturated spectrum where white First dark image after spectrum where corresponds to 85 000 electrons white corresponds to 120 electrons 2100 electrons per second 3 electrons per second ae Window uwa 000000007 KZ Second dark image where white Third dark image where white corresponds corresponds to 120 electrons to 120 electrons 3 electrons per second 3 electrons per second Peak is under 0 25 electrons per second Figure A 1 Spectrograph Persistence 72 3 15 2010 UCLA Infrared Laboratory dn oS ERI rdg CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 Fixed Pattern Noise and Artifacts The Hawaii 2 detector exhibits fixed pattern noise corresponding to the individual multiplexer readout channels This is due to a small channel to channel baseline variation typically 3 electrons or 1 DN when operating at a stable temperature This is shown in Figure A 2 in a dark frame taken at 65 K with the detector temperature controller in operation
28. within the instrument including a cold pupil stop Spectrograph M Collimator optics TMA Adjustable mask 1 Lenslet array Keck II AO focus Fixed grating Re imager collimator R I Camera Pupil plane singlet singlet Re imaged G focal plane Detector Re imaging optics Image sampler Figure 2 1 OSIRIS Spectrograph Optical Configuration Ry 3 15 2010 UCLA Infrared Laboratory I SEES arom CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Fold Mirror Arie poste amp Lenslet Array r CN AO Focus 0 Reimaging Cameras pReimaging Collimators Fold Mirror Spectrograph Camera Mirrors TMA Figure 2 2 Rendering of the real optics within the spectrograph leg of the instrument Note that the lenslet array is the smallest component The reimaging optics are fully refractive to reduce wavefront error while the spectrograph optics are all off axis mirrors to eliminate ghosts Each lenslet in a given row is the source for a spectrum that is nominally separated by 2 pixels vertically from the spectrum of the adjacent lenslet in the same row Each spectrum is also offset or staggered horizontally The stagger results from the slight rotation of the lenslet array relative to the detector The horizontal stagger should be 32 pixels but anamorphism introduced by the TMA in the horizontal direction causes the offset to b
29. 0 gt Finally save the resultant image 52 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 lt module Name Save DataSet Information gt The output filename for the Combine Frames module includes the date of the observations set and file number the name combo the integration time the filter and the plate scale For instance if you were combining multiple sky frames with an integration time of 180 seconds taken in 5 filter and the 0 035 plate scale then the output filename would look something like this 5070823 2011001 combo 180 5 035 fits If you were combining dark frames then the plate scale of the observations does not matter Therefore if the filter is Drk then the scale is not printed in the output filename For instance if the above examples were taken as darks then the output filename would be 5070823 2011001 combo 180 Drk fits Here is the final example DRF for creating a super dark frame lt xml version 1 0 encoding UTF 8 gt lt make_super_dark gt lt DRF LogPath net hydrogen data projects osiris D RP larkin test DRFs OutputDirz net hydrogen data projects osiris DRP larkin test ReductionType CRP SPEC dataset InputDirz net hydrogen data irchive osiris osiris8 051123 SPEC raw fits FileName s051123_a000004 fits gt lt fits 5051123 a000005 fits gt fit
30. 0 019 Kn2 0 000 0 001 0 001 0 002 0 002 0 003 0 003 0 004 0 005 0 006 0 007 0 008 0 010 0 013 0 017 Kn3 0 000 0 001 0 001 0 002 0 002 0 002 0 003 0 004 0 004 0 005 0 006 0 007 0 009 0 012 0 016 Kn4 0 000 0 001 0 001 0 001 0 002 0 002 0 003 0 003 0 004 0 005 0 006 0 007 0 008 0 011 0 015 Airmass and filter combinations with deflections between 0 020 and 0 050 arcsec are shown in tan while those with deflections between 0 050 and 0 100 arcsec are in orange In extreme cases where the elongation is more than 0 100 arcsec the boxes are red 3 15 2010 89 UCLA Infrared Laboratory Kn5 0 000 0 001 0 001 0 001 0 002 0 002 0 003 0 003 0 004 0 004 0 005 0 006 0 008 0 010 0 013 KERKE KE CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 0 1 Instrumental Chromatic Dispersion The adaptive optics bench contains an IR transmissive dichroic that also introduces significant chromatic dispersion parallel to the optical bench We measured this in August 2006 using the white light fiber in the F 15 input to the AO bench Broad band images of the fiber were taken in the Zbb Jbb Hbb and Kbb filters and a source position was measured in both x and y as a function of wavelength using the standard IDL Gaussian fitting routine Figure D 1 shows the motion of the source in both axes relative to its location at 1 0 microns 1000 nm for the old AO dichroic before August
31. 0 electrons 6 When exposed to a constant source flux this is the percentage difference between the linear trend at low flux vs that measured at 80 full well which corresponds to approximately 108 000 electrons 7 Amount of variation in the unexposed portion of a series of short dark frame exposures Values given are for operation at 65 K with the detector temperature controller in operation and maintaining the detector temperature 8 Data supplied by manufacturer No detectable uncorrelated pattern noise was found in any of the test data frames The zero point variation given in Table 9 was taken at a detector temperature of 65 K with the detector temperature controller operating properly Device zero point stability depends on accurate temperature control An anomaly is observed after the detector is reset This takes the form of a time dependent change in the channel output baseline for all multiplexer outputs The time constant of this anomaly is approximately 5 seconds and it is inversely dependent on temperature as shown in the graph of Figure A 6 200 180 160 140 1 second exposure 120 taken 100 e 4 seconds after reset 5 seconds after reset 80 Bias shift electrons 60 40 20 68 69 70 71 72 73 74 75 76 Detector temperature K Figure A 6 Hawaii 2 Reset Anomaly 76 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3
32. 02 0 003 0 005 0 007 0 008 0 010 0 013 0 015 0 018 0 022 0 026 0 031 0 039 Zn3 0 001 0 003 0 004 0 006 0 008 0 010 0 012 0 014 0 017 0 020 0 024 0 029 0 036 Zn4 0 001 0 003 0 004 0 006 0 007 0 009 0 011 0 013 0 015 0 018 0 022 0 027 0 033 Zn5 0 001 0 002 0 004 0 005 0 006 0 008 0 010 0 012 0 014 0 017 0 020 0 024 0 030 Image elongation in arcseconds for each filter Jn1 0 001 0 002 0 004 0 005 0 006 0 008 0 009 0 011 0 013 0 016 0 019 0 023 0 029 0 037 Jn2 0 001 0 002 0 003 0 004 0 006 0 007 0 009 0 010 0 012 0 015 0 018 0 021 0 026 0 034 0 046 Jn3 0 001 0 002 0 003 0 004 0 005 0 007 0 008 0 010 0 012 0 014 0 017 0 020 0 025 0 032 0 043 Jn4 Hn1 Hn2 Hn3 0 001 0 001 0 001 0 001 0 002 0 002 0 001 0 001 0 003 0 002 0 002 0 002 0 004 0 003 0 003 0 003 0 005 0 004 0 004 0 004 0 006 0 005 0 005 0 004 0 007 0 006 0 006 0 005 0 009 0 007 0 007 0 006 0 011 0 009 0 008 0 008 0 013 0 011 0 010 0 009 0 015 0 013 0 012 0 011 0 018 0 015 0 014 0 013 0 023 0 019 0 017 0 016 0 029 0 024 0 022 0 021 0 040 0 033 0 030 0 028 Hn4 0 001 0 001 0 002 0 003 0 003 0 004 0 005 0 006 0 007 0 008 0 010 0 012 0 015 0 019 0 026 Hn5 0 001 0 001 0 002 0 002 0 003 0 004 0 004 0 005 0 006 0 008 0 009 0 011 0 014 0 018 0 024 Kn1 0 000 0 001 0 001 0 002 0 002 0 003 0 004 0 004 0 005 0 006 0 007 0 009 0 011 0 014
33. 2009 A new AO dichroic was installed in August 2009 a new instrumental chromatic dispersion solution was derived from AO fiber data and is included in the v2 3 Correct Dispersion module X axis motion 50 Dispersion compared to 1000 nm mas o 50 Y axis motion 1000 1500 2000 2500 Wavelength nm Figure D 1 Image motion as a function of wavelength for a calibration fiber in the F 15 focus This is the chromatic dispersion from the AO optical bench for the old dichroic before August 2009 90 3 15 2010 UCLA Infrared Laboratory KERE E CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 As Figure D 2 shows the fiber image position moves to the right and down as wavelength increases The x motion is 1 12 times as large as the y motion consistent with an instrumental orientation of 48 3 degrees relative to the optical bench The data approximately follow a square root vs wavelength as would be expected from the traditional inverse cubic form of index vs wavelength So to fit the data we used a 2 order polynomial to the square of the total motion x and y combined with a joint additive offset for 1 00 microns The resulting equations are given by Total Motion mas relative to 1000 nm 20 40 16204 19 662 0 0030422 The model is then projected onto the x and y axes and the residuals are presented in Figure D 2 as a function of wavelength The rms residuals calculated from a
34. 4 5 294 790009 Temperature at sensor 5 CTMP6 292 119995 Temperature at sensor 6 CTMP7 295 690002 Temperature at sensor 7 CTMP8 295 910004 Temperature at sensor 8 95 3 15 2010 UCLA Infrared Laboratory SEC jc orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY ODS Keywords PRESSURE SSIMECH SSISTAT SSINAME SSIRAW SSISWTCH SFWMECH SFWSTAT SFWNAME SFWRAW SFWSWTCH SS2MECH SS2STAT SS2NAME SS2RAW SS2SWTCH SLMMECH SLMSTAT SLMNAME SLMRAW SLMSWTCH IFIMECH IFISTAT IFINAME IFIRAW IFISWTCH IF2MECH IF2STAT IF2NAME IF2RAW IF2SWTCH STRGTMP 3 15 2010 Typical Value 0 001387 Scale Turret 1 OK 0 02 900 1 Spec Filter Wheel OK Hn3 0 387 Scale Turret 2 OK 0 02 900 1 Lenslet Mask Stage OK Narrow 10313 4 Imager Filter Wheel 1 OK Hn2 93 5 Imager Filter Wheel 2 OK Kn2 93 5 67 96 OSIRIS USER MANUAL V 2 3 Description Current pressure read from gauge in mTorr The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechanism in steps Current switch value The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechanism in steps Current switch value The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechan
35. ACIDIC Nau 0njo Keck Il AO chromatic dispersion observed with OSIRIS Nov 2009 60 T T T T T T T T T T T T T 71 Doto Model An L zi Uu 4U N c r NEP uc 4 x ie epr ai 20 15 2 5 _ c L _ 4 J n e 4 s 4 Pd D lt P lt ne ie 4 _ 4 zm An o a _ L Qxis J o T a 5 4 v ar 40 L 4 anion 60 LL 1 1 l 1 1 1 1 1 n 1 1 1 1 1 r 4 4 Ann en an nnn Ann 1000 200 400 1600 800 2000 2200 2400 Wavelength nm Figure D 3 Image motion as a function of wavelength for a calibration fiber in the F 15 focus This is the chromatic dispersion from the AO optical bench for the new dichroic after August 2009 92 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomMY OSIRIS USER MANUAL V 2 3 Appendix E FITS File Information OSIRIS frames are written in an up to ramp output in DN sec Both raw and reduced cubes are in units of DN s unless otherwise modified by the user FITS Extensions The 2nd extension of the raw and reduced fits file and generally referred to by IntAuxFrame in pipeline modules is a byte array indicating the quality of each pixel Originally each bit of the array was assigned a specific meaning like the pixel had a significant l
36. CH IN ASTRONOMY Status GUI OSIRIS USER MANUAL V 2 3 The Status GUI presents the current positions of all the motor mechanisms of OSIRIS spectrograph and imager When the mechanisms are physically moving in the instrument the wheeled images will move on the GUI The integration of a current file in the spectrograph and imager are updated as the exposure is being taken for monitoring File Mechanisms Exposure Help r Spectrometer 37 Object UNDEFINED Comment below scan Itime 60 0 seconds 6276 Reads 8 osiris data osrseng 050621 SPEC raw s050621 c007024 fits Status Exposing Received read 5 8 of coadd 1 1 Coadds 1 imager 0 Status Idling Object Comment time seconds Filename 0 Reads Coadds TotalTime SpecFilter Spec Scale 1 Spec Scale 2 Lenslet Ma OK Imag Filter 1 Imag Filter 2 Scan 51 scan 51 3 15 2010 30 J 05 06 21 08 01 09 UCLA Infrared Laboratory SSES rdg CALIFORNIA ASSOCIATION FOR RESEARCH IN AsTRoNOMY OSIRIS USER Telescope GUI The OSIRIS telescope GUI is used to input and send all commands to the telescope The white box is used for logging which commands where issued The GUI has a set of tabbed headings which bring down different control options e The Cover folder is blank and hides the other folders so observers do not accidentally click and move
37. Cosmic Rays Brief Description Clean Cosmic Rays attempts to identify pixels that have been struck by cosmic rays Cosmic rays generally deposit a large amount of charge within the array in a pattern that is inconsistent with the lenslet PSFs If they are not identified then the spectral extraction will assign the incorrect flux to lenslets Since the distribution will not match the PSFs this will often cause residuals in the extraction which may spread to a larger and larger number of lenslets So a single cosmic ray can affect many lenslets at a variety of wavelengths Identified pixels are marked as bad in the quality frame extension 2 but are not replaced They will be ignored by the Extract Spectra module DO NOT RUN Clean Cosmic Rays on individual raw frames that have not had a matching dark or sky subtracted from them If you do this the many hot pixels on the detector will be marked as bad and you ll get a very large number of bad pixels propagated into later reduction modules 58 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 Usage The only command words recognized are Name and Skip Examples lt module Name Clean Cosmic Rays gt 5 9 5 Combine Frames Brief Description Combine Frames is used to combine multiple frames of the same type scale filter and integration time into a lower noise version The most common applications are to
38. Dir irchive osiris 051 123 SPEC raw gt fits FileNamez s051123 a013001 Hn3 100 fits gt fits FileNamez s051123 a013003 Hn3 100 fits gt fits FileNamez s051123 a014001 Hn3 100 fits gt fits FileNamez s051123 014002 Hn3 100 fits gt fits FileNamez s051123 a014003 Hn3 100 fits gt lt dataset gt lt module Name Mosaic Frames 55 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONoMY OSIRIS USER MANUAL V 2 3 Combine_Method MEANCLIP Offset_Method TEL Save 1 gt lt DRF gt The output will again be the name of the first input file plus mosaic But since the files have been combined together the frame number is removed i e 5051123 a013 mosaic Hn3 100 fits 5 8 On line Pipeline at the Telescope While you are actively taking data it is essential to get real time feedback on where the science target is located and the brightness of your source Since the full pipeline can take several minutes to properly reduce even a single frame we have implemented an abbreviated reduction strategy for real time use The pipeline itself as defined by the idl process and possible modules is actually identical and the same pipeline can be used to reduce in the ARP SPEC mode The primary difference is which modules are left out of the reduction and a few of the parameters used by the modules The only parameter of real significance is the number of iterations used b
39. First light with OSIRIS Observations from June 2005 February 2006 use Rectification Scans taken in June 2005 1 5050623 014 infl Kbb 020 fits with pipeline a global wavelength solution is applied June 2005 New grating is installed November 23 2005 Last night of Commissioning Observations from April 2006 March 2008 use Rectification Scans taken in March 2006 for 0 020 0 035 0 050 lenslet scales in all filters and 0 100 lenslet scale for J and Z broad narrow band modes For H and K broad narrow band modes in 0 100 lenslet scale use Rectification Scans taken in May 2007 102 3 15 2010 UCLA Infrared Laboratory 4 4 D E KERKE PE ae CALIFORNIA ASSOCIATION FOR RESEARCH INAstRoNomY OSIRIS USER a lt lt March 2006 Adjusted lenslet tilt and added new pupils to reduce the background in 0 035 and 0 050 lenslet scales August 2006 Public release of Data Reduction Pipeline May 18 2006 Bad channel on SPEC detector appeared June 27 2006 Fixed bad channel on SPEC detector October 15 2006 Earthquake 6 7 occurred 10 km off shore southwest from Puako This resulted in a broken G10 support of the optical bench which in turn made a thermal short and restricted the dewar cooling December 2006 Fixed broken rear G10 support for the optical bench damaged in earthquake OSIRIS scans were not affected April 2007 Second public release of Data Reduction Pipeline major changes to mo
40. Imager M3 21 6 Imager M4 21 16 Filters min mean max 12 2 5 5 10 Imager Surface Total alignment 50 23 errors ignored Imager design WFE 25 Imager alignment tolerances 30 Spectrograph Total 0 02 scale 35 24 Imager Total design align surface lt 45 The 0 020 scale is very insensitive to alignment issues since there are only two powered optics and these are simple biconvex lenses Tipping or tilting them to first order causes image motion Sufficient tilt to contribute to the wavefront error budget would shift the images off the small lenslet field The same is true of the coarser scales but they are also much more tolerant to wavefront error due to sampling issues So the spectrograph tip tilt and decenter requirements 20 3 15 2010 UCLA Infrared Laboratory ose Barone CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 from the OSIRIS Mechanical Design Note OMDN 01 00 Section 5 must be satisfied in order to achieve the observed image quality The imager has three powered surfaces but these are also spherical which are relatively insensitive to alignment errors To reach the 30 nm of WFE allowed for imager internal alignment the detector would be focused 7 mm from nominal which would be easily seen in our mounting and would shift the plate scale away from our measured value of 0 020 by more than 5 which is not observed in either measurement method This level of alignment error also tends to make
41. KIRMOS PDR report shows the results of the tests performed by Finger for both Hawaii 2 LPE curves and Hawaii 2RG MBE curves devices In those measurements the device used had a lower J band QE than the OSIRIS detector The QE drop over 10 degrees is typically from 5096 to 4096 or a 20 relative change Over our 3 degree test this should have been closer to 6 instead of our measured change of 15 We attribute this difference to the test setup and white light source stability Temperature Dependence of Quantum Efficiency of 2Kx2K arrays Hawaii 2RG Engineering MBE amp Hawaii2 Science By courtesy of Gert Finger ESO ss u 0 80 100 120 140 160 Temperature K Figure A 7 Hawaii 2 Detector Temperature Dependence of QE 77 3 15 2010 UCLA Infrared Laboratory SSES av dia CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 A 5 2 Temperature Dependence of the Reset Anomaly During these same tests the reset anomaly changed shape somewhat but at both temperatures produced a ramp of about 50 DN 150 electrons in the first few hundred pixels Previous tests suggest that the reset anomaly does become better at 75 K see Figure A 6 The dark current measurements were inconclusive for the exposure times used during this test but previous measurements show an increase by a factor of two in dark current from 69 K to 73 K A 5 3 Optimum Operating Temperature The results of the tests to det
42. N ASTRONOMY OSIRIS USER Appendix F History of Instrument Changes Which matrices to use in reductions The most unique step within the OSIRIS pipeline is the extraction of the spectra from the 2 dimensional raw frames This process requires that the PSF of every lenslet as a function of wavelength has been mapped to fairly high precision These PSFs are stable over many months and the calibration is performed by either the instrument team or Keck staff We refer to these scans as Rectification Matrices and they are stored in matrix form for all modes In addition arc lamp calibration scans are taken to perform a global wavelength solution for each lenslet In the event of hardware changes to OSIRIS that significantly alter the optical path or components new scans are taken and will be made available to you The user does not need to take any of this calibration data but does need to obtain the necessary matrices from the Keck repository for their observing modes filter and plate scale In most cases the OSIRIS Support Astronomer will give you the calibration scans for your observations Observations from January May 2005 use Rectification Wavelength Scans and old pipeline version for these reductions taken March 2005 1 for Kbb in 0 020 scale the rectification file is 5050327 c013 infl Kbb 020 fits January 2005 First Calibration Scans Rectification and Wavelength at Keck with the old grating February 22 2005
43. OBLBNAME OBRT OBRTNAME OBSDNAME OBSFX OBSFY OBSFZ OBSFNAME OBSNNAME OBTSNAME OBWCNAME OBWFNAME OBWLNAME OBWPNAME OBWNNAME OBSWSTA OBWF WCDMSTAT WCDTSTAT WSFRRT WSGAIN 3 15 2010 Typical Value 31359 3766 27923 noName 7 43 8 83 0 0 2 4 out noName 60 0136 noName beamSplitter 119 0 0 telescope block home 2 4 noName 2 4 ngs open off 2 472 CLOSED CLOSED WFS 672 2 101 OSIRIS USER MANUAL V 2 3 Description Raw value of FSM ly axis count Raw value of FSM 2x axis count Raw value of FSM 2y axis count Named position control for FSM Image plane x motion for FSM Image plane y motion for FSM Pupil plane x motion for FSM Pupil plane y motion for FSM Named position control for FSS Named position control for ISM Named position control for LBS User value of ROT deg Named position control for ROT Named position control for SOD User value of SFP x axis mm User value of SFP y axis mm User value of SFP z axis mm Named position control for SFP Named position control for SND Named position control for TSS Named position control for WCS Named position control for FCS Named position control for WLS Named position control for WPS Named position control for WND White light power status User value of FCS mm Status of DM loop Status of down tt loop Frame rate for WFS cam Hz Set WFS camera gain UCLA Infrared Laboratory o SESS TRV CALIFORNIA ASSOCIATION FOR RESEARCH I
44. OSIRIS OH Suppressing Infra Red Imaging Spectrograph Not Your Grandma s Spectrograph Entering Deep Water If In Doubt Don t Go Out James Larkin Matthew 2 5 Mike McElwain Marshall Perrin Jason Weiss Shelley Wright UCLA Infrared Laboratory Version 2 3 March 1 2010 oS EEK av dide CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Intentionally Blank DA 3 15 2010 UCLA Infrared Laboratory 1 tiit o SER rdv CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 OSIRIS and CARA members at OSIRIS first light Keck II remote OPS 3z 3 15 2010 UCLA Infrared Laboratory oS ESS AT dide CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Table of Contents LU OSIRDIS OVOLVIGW bang chala 6 2 OSIRIS Capabilities endete vandal ete Geter tak icd uide o de iden d 7 24 Basic Optical sconti t ta nA EI a aska 7 2 2 CIS leh TRY 9 2 3 Piltets and Pields ot VIOW i cierre ea eas eta edd 10 24 Dispersions dnd Resolutions 1 musei s RI state 16 2 5 Pill uot ve stab 19 2 0 Concentricity of the Four Plate Scales ri ett rrr
45. Plate Scales An important consideration is how well aligned are the four spectrograph plate scales If you acquire an object in the center of one scale then you can NOT simply select another scale and remain centered on your object Table 2 4 below gives the relative offset between the field centers of the four scales It is important however to remember that if an object appears centered in the 0 100 scale this represents 5 pixels within the 0 020 scale so a small shift in addition to the table offsets may occur The table assumes that an object has been centered in the 0 020 scale and then calculates by how much it will shift in reduced data cubes if another scale is selected and the object is not moved X offset refers to the short 16 or 48 lenslet axis while the Y offset refers to the long 64 lenslet axis Table 2 4 Relative Offsets between the Four plate Scales Scale Xoffset arcsec Yoffset arcsec 0 020 0 000 0 000 0 035 0 02 0 08 0 050 0 04 0 10 0 100 0 01 0 00 To compensate for these small offsets the Telescope GUI OTGUI can be used to offset an object from the center or specified pixel in one plate scale to the center or specified pixel in another plate scale or even to the imager 9 3 15 2010 UCLA Infrared Laboratory OSIRIS USER MANUAL V 2 3 4 s ite DS E F A orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY 27 Optical Error Budget In
46. Spec which allows the current integration to finish exposing with no effects to the detector and then terminates the rest of the observing sequence The Abort All Immediately should be used ONLY in dire need This will stop the observation sequence in mid integration and resets all the voltages of the detector controller which causes detector thermal problems which may take up to 15 minutes to clear Flushing the detector will become necessary before resuming observations Please see the Telescope GUI OTGUI section for instructions on how to flush the detector 29 3 15 2010 File Engineering Help Dataset Queue Ke Datasets 9 Object BD1 Z AO Mode NGS Spec Filter Hbb a Spec Scale 0 02 lenslet Spec Itime 300 s Spec Coadds 1 858 Object Dither Pattern Raster Scan a Sky Dither Pattern Raster Scan Imager Mode Disabled Spec only Imager Frames None Dither Positions 5 0 00 0 25 0 00 0 00 0 00 0 25 5 00 4 75 Sky 5 35 4 75 Sky Remove Move Up Move Down amp utoLoad DDFs Current Dataset Status Dataset Name Dataset Number Imager Mode Dither Position of Imager Setup of Start Hext Dataset Imager Test Frame Spec Test Frame 1 Automatically Start Next Dataset in Queue osiris 5 6 21 08 25 09 UCLA Infrared Laboratory 414 24 24942 qu WM oS SENS ar ogy CALIFORNIA ASSOCIATION FOR RESEAR
47. Subtract Frame Adjust Channel Levels Remove Crosstalk Glitch Identification Skip Module Clean Cosmic Rays Calibration File Next 7 Extract Spectra Assemble Data Cube Browse Save DataSet Information Save Output 1 Save On Error 07 06 06 10 40 35 32 3 15 2010 UCLA Infrared Laboratory KESK dae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Quicklook2 OSIRIS spectrograph frames are 3D FITS files that require sophisticated image visualization tools The OSIRIS team presents an IDL based software package called Quicklook2 to display and analyze your OSIRIS data cubes Quicklook2 is the OSIRIS image analysis software used at Keck while observing but we also encouraged using Quicklook2 for post observing analysis of 2D 3D FITS This software handles simple image analysis functions such as horizontal and vertical cut plotting surface and contour plotting color stretching photometry analysis image arithmetic and zooms At the same time Quicklook2 is equipped with enhanced image analysis procedures for image rotations wavelength information and line fitting The main image analysis GUI in Quicklook2 is shown below for reference For a complete description of Quicklook2 functionality and operating procedures please see the Quicklook2 Users Manual which is available for download at the url http www astro ucla edu irlab osiris This ma
48. Table 2 5 below we give the estimated RMS wavefront error of each optical element in the spectrograph up to but not including the lenslet array and all elements of the imager These are the elements that affect the Strehl ratios In the case of mirrors the wavefront error is assumed to be twice the surface error For the window lenses and filters the wavefront error is assumed to be equal to n 1 times the sum in quadrature of the two surface errors In all cases the measurements were made over an area equal to or larger than the illuminated region In some cases more than one component was fabricated and the component currently in the instrument is identified in the table Table 2 5 Optical Error Budget Component Design RMS WFE nm Fabricated RMS WFE nm Window 1 n 1 458 4 3 Window 2 4 3 8 will be installed at summit Window 3 4 4 4 in dewar Splitter Mirror Spectrograph 1 13 3 in dewar Splitter Mirror Spectrograph 2 13 13 Splitter Mirror Imager 1 13 8 in dewar Splitter Mirror Imager 2 13 9 Lenslet Fold Mirror 1 13 12 Lenslet Fold Mirror 2 13 14 in dewar Spectrograph Fold Mirror 1 13 6 in dewar Spectrograph Fold Mirror 3 13 8 Spectrograph Fold Mirror 4 13 4 Imager Fold Mirror 1 13 8 Imager Fold Mirror 2 13 3 in dewar F 257 Collimator n 1 474 17 14 F 257 Camera n 1 474 17 9 Imager M1 21 6 Imager M2 21 10
49. Value Description 15 Telescope right ascension 01 00 00 00 h 0 right ascension offset 0 0 arcsec 0 rotator calibration angle 0 00 deg position angle rotator tracking mode 138 623847 rotator physical destination 138 62 deg 0 rotator physical position 0 00 deg 0 rotator user destination 0 00 deg 138 623847 rotator user position 138 62 deg 0 rotator reference angle 0 00 deg 0 secondary mirror focus raw 0 000 mm 0 secondary mirror thetax arcsec 0 secondary mirror thetay arcsec target name 0 target wavelength microns telescope name 0 telescope focus compensated 0 000 mm 0 tube temperature 0 00 degC ACS Keywords Typical Value Description 3 13025 Mirror Temperature I 0 Primary Mirror Focus Mode nm AO Keywords Typical Value Description closed AO deformable mirror loop stat closed AO downlink tip tilt loop stat in position AO control status STBY AO state string closed AO tip tilt offloading mode 415 AO WFC AOA camera median light open AO coma offloading mode closed AO focus offloading mode 2 899 AO WES focus stage FSM coefficient 0 65 Set gain in target CB 0 45 Set TT loop gain mirror Named position control for AFM ngs Named position control for AFS 12072 Raw value of FSM 1x axis count 100 UCLA Infrared Laboratory siiis DS E F A orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY ODS Keywords OBFMIYRA OBFM2XRA OBFM2YRA OBFMNAME OBFMXIM OBFMYIM OBFMXPU OBFMYPU OBFSNAME OBIMNAME
50. a preliminary data cube to appear in the quicklook display package The reduction system also includes a growing set of final reduction steps including correction of telluric absorption and mosaicking of multiple cubes That being said infrared spectroscopy is a fairly complex astrophysical technique and when combined with a laser adaptive optics system and the complexity of over 3000 independent and overlapping spectra OSIRIS is not recommended for the faint of heart In terms of observing planning much of the complication actually comes from the AO nature of the instrument As an imaging spectrograph much of the dithering and exposure settings are quite similar to a traditional infrared camera or spectrograph Since the infrared background is bright and complicated it s important to obtain sky frames for subtraction but in some cases where your object is small you can build a sky by dithering on chip in this case on lenslet but it s identical Similarly telluric standard stars are needed in most cases to remove atmospheric transmission variations as a function of airmass and wavelength Like NIRSPEC or other IR spectrographs we ve found that stars near spectral types AO work well although others sometimes use solar analogs Much of this 1s discussed in detail within this manual but we thought it was important to give you an initial sense of how the instrument works Basically pick a filter and platescale then dither on sour
51. ake the proper dithers when moving in sky coordinates Users may also save their observation planning sequence DDF for later use or for planning before they arrive at the telescope The GUI can be downloaded to your home computer before your run so you can practice laying out your observations It s available at the OSIRIS website http www astro ucla edu irlab osiris 28 3 15 2010 UCLA Infrared Laboratory 4 456 44 lt ATOR CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER bras Execution Client GUI The execution client is the GUI that manages your observing sequences and implements them with the hardware control software Once you have planned your observations in the OOPGUI described above you will Send to QUEUE which sends your planned observations to this GUI Once you are ready to start your observations you click Start Next Dataset which then commands the instrument and telescope You only run this GUI at the telescope and it s easiest to learn at the telescope It only has a few options including removing sequences that you don t want to execute and starting sequences in the queue For convenience it also has the ability of starting spectrometer or imager frames using the current exposure settings If you decide during an observational sequence that you wish to terminate or stop the sequence CAUTION should be taken In most cases users should always use the Abort After Current
52. asure the PSF from off axis stars to at least allow for monitoring of the variation of conditions with time Making use of the PSF stars to predict the PSF at the science target is still a major goal of many adaptive optics groups and is not a fully solved problem The imager and spectrograph are in a fixed orientation compared to each other but they can be dithered on the sky and the pattern can be rotated to arbitrary angles Spectrograph Fields Imager Field Up to 4 8 x6 4 at approximately 20 4 x20 4 45 degrees Horizontal plane of Keck II AO bench and OSIRIS internal optical bench Figure 2 7 Relative locations of the imager and spectrograph focal planes For the imager in most cases you will be background limited So the noise is dominated by the sky background As you can see the background in the K band is significantly elevated over NIRC or NIRSPEC This is primarily due to the increased background from the AO system but it is also due to the optical design of the imager It is based on the SHARC camera and is close to an Offner optical design This leads to excellent image quality with simple optics but the pupil is poorly formed and not directly on an available optical surface So the cold pupil is oversized and allows through additional background Due to this background the H band is definitely the deepest imaging filter But care must be taken for some sources since all of the OSIRIS filters 2997 3 15 2010 UCLA Infrar
53. ating 8 10K warmer than normal operating temperatures This caused noticeable changes in the performance of the OSIRIS pipeline Users with the data sets post January 2009 are recommended to reduce their data using v2 3 pipeline 103 3 15 2010 UCLA Infrared Laboratory oS ERI rdg CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Observations from January September 2009 Users should reduce their data with calibration files that are nearest in time and temperature to their observations from this period They should also ensure that their calibration files were generated with v2 3 calibration reduction pipeline released to Keck January 2010 October 14 2009 OSIRIS was serviced and fixed the thermal contact between the cold head and copper block After cooling down OSIRIS returned to normal operating temperatures Observations from October 2009 to present Users should use the latest calibration files generated by v2 3 of the calibration reduction pipeline 104 3 15 2010 UCLA Infrared Laboratory oSEBI rdg CALIFORNIA ASSOCIATION FOR RESEARCH IN AsrRoNouwY OSIRIS USER MANUAL V 2 3 When all else fails Play Cowboy Cowboy Billiards Rules based on those provided at http www bestbilliard com rules display cfm file cowboy cfm TYPE OF GAME Cowboy combines carom and pocket billiards skill and employs a very unusual set of rules It has been very popular at Palomar Observatory for many decades and
54. aves Waves Zbb 220 0 095 Jbb Not avail Hbb Not avail 0 081 All of the measured values for BW and CWL are based on the 50 power points For the Zbb and Jbb filters the useful ranges are actually set by order overlap and are given in Table 2 1 For the manufacturer s test data slope is determined based on the 80 and 5 relative transmission points The wavefront error wfe in the table peak to valley wavefront error P V wfe in the table and the optical power are given in wavelengths of light waves at 632 8 nm 15 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 24 Dispersions and Resolutions OSIRIS can take up to 3072 spectra simultaneously Due to variations in the incident and diffracted angles with the grating and with spot quality at the detector the spectral resolution has significant variation between lenslets and at different wavelengths The dispersions on the detector are actually fairly constant and have median values given in Table 2 3 Table 2 3 Linear Dispersion Median Dispersion Resampled Dispersion per pixel in raw data in Reduced Cubes Band order Z 6 0 0001410 0 000120 J 5 0 0001692 0 000150 4 0 0002115 0 000200 K GB 0 0002820 0 000250 Over the central 16x64 lenslets
55. aximum Itime and Filter Sets The Maximum Repeats Maximum Itime and Filter Sets are all based on the total integration time of the SPEC frames The Maximum Repeats does the maximum number of imager frames with a user specified imager itime The Maximum Itime calculates the maximum itime the imager can do given a user specified number of repeats The Filter Sets is the most flexible option and allows users to use more than one filter and to directly specify the itime coadds number of repeats for each filter When you select the Filter Sets option and click on the Filter field another window opens bottom right image for the user to interact with each of the values Imager Filter Sets Filter Repeats Coadds Itime Hbb 1 1 40 Kbb 1 1 20 Jbb 1 1 60 Zbb 1 1 80 Add Remove Clear All Estimated time remaining 46 0 seconds OK Altering any of these fields in the GUI does not directly communicate with the instrument or the telescope Once the observation sequence is prepared click the Send to Queue button which adds the Dataset script called a Data Definition File or DDF to a directory queue which the execution client GUI uses to build a list of observations It s important to note that the position angle PA input does not alter the PA of the instrument once the DDF is executed Altering the PA needs to be performed in the Telescope GUI The correct PA is critical to m
56. axis There is no checking of wavelength information in the headers so it is required that the data and stellar spectra have the same length in pixels Note the 1D spectrum is normalized so the median channel has an intensity of 1 0 Usage Name and CalibrationFile keywords must be set in the module call The calibration file must be a 1D FITS file with the same length as the spectral dimension on the dataset being reduced Skip and Save keywords are also obeyed by the module Examples module Name Divide by Star Spectrum CalibrationFile 61 3 15 2010 UCLA Infrared Laboratory ofS SES ar ay CALIFORNIA ASSOCIATION FOR RESEARCH IN AsTRoNowv OSIRIS USER MANUAL V 2 3 DRP larkin 070517 s070517 23037001 1d datset Kbb 035 fits gt 5 9 10 Extract Spectra Brief Description Usage This is the key module that takes 2D raw spectra and extracts them into un blended spectra that can be traced back to particular lenslets It uses a calibration file called an influence matrix sometimes also called a rectification matrix that contains the PSF shape of each lenslet as a function of wavelength There exists a calibration file for each mode of the spectrograph and you must obtain the appropriate ones from the Keck repository before reducing your data The routine goes column by column through the array and uses the measured PSFs to assign the flux from the 2048 pixels into the 1024 lenslets that could potentially place light into tho
57. bute will look like CalibrationFile2 directory SPEC calib calibration file fits The name of the module must be specified using the Name attribute These names are not negotiable and the exact name must be used see Section 5 9 Example Name Remove Crosstalk If you decide to re run a DRF and would like to skip a particular module the easiest way is with the Skip attribute Set it to 1 in order to skip the file and set it back to 0 to execute the file The default is 0 and is not required Skip 1 Other module attributes such as an outputdir are only used by a few modules and are described in Section 5 9 A typical module tag would look like module Name Adjust Channel Levels Skip 0 gt lt module gt 48 3 15 2010 UCLA Infrared Laboratory oS EEK Anday CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Since much of the pipeline processing is driven by header keywords it is sometimes necessary to modify a keyword in a particular file This can be accomplished by the lt update gt tag which is normally placed at the end of the XML file An example might be to change the DATAFILE keyword which is used to build the output file names Here is an example update DataSetNumber 0 HeaderNumber 1 gt lt updateParameter Keyword DATAFILE KeywordValue Andromeda KeywordComment Output Filename KeywordType string gt lt updateParameter gt lt update gt A
58. ce and on sky The pipeline will handle much of the rest For the latest information on OSIRIS please always refer to the website http www astro ucla edu irlab osiris which will have links to the most recent versions of software and documentation It also has links to an OSIRIS wiki page for users 6 3 15 2010 UCLA Infrared Laboratory oS EEK avidi CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER 2 OSIRIS Capabilities 24 Basic Optical Layout A schematic of the OSIRIS IFS optical configuration is shown in Figure 2 1 The IF spectrograph optical configuration consists of three coupled systems a re imager an image sampler and a spectrograph The image sampler is a 2 dimensional array of small lenses or lenslets located at a re imaged focal plane of the Keck II AO system At the focus of each lenslet a much smaller pupil image is formed that contains all of the light from its portion of the field This lenslet array serves to spatially sample the input image The pupil images are well separated and serve to define the entrance aperture of the spectrograph section The dispersion axis of the spectrographic is rotated slightly compared to the lenslet orientations so that the dispersed spectra from each spatial location are interleaved across the spectrograph detector The spatial scale of the instrument is determined by re imaging optics in front of the lenslet array The re imaging optics also provides most of the baffling
59. cientific Clocking the array at intermediate temperatures must not be done since these pixels do not return to normal unless the detector is warmed to ambient temperature It was also found that increasing the voltage increases the dark current Unless otherwise noted for the numbers given below the detector was run with Veset voltage of 0 5 volts at a temperature of 65 K Due to the contribution of readouts to the apparent dark current the dark current was measured using CDS readout no intermediate readouts during the exposure Characterization Data Characterization data for the spectrograph detector a Rockwell Scientific Hawaii 2 part number 73 a specific device identification number is given in Table 8 Table 8 Spectrograph Detector Characterization Parameter Value Units Notes Dark Current 0 035 e pixel sec 6 7 Read Noise 11 e 1 5 Multiplexer Glow 2 e pixel read 8 Charge Storage Capacity gt 90 000 e pixel 5 Memory Charge 120 pixel 2 see 5 2 Dark Current Shift 0 01 e pixel sec 3 Dark Current Decay Time NA seconds 4 Quantum Efficiency J band 85 30 s 7 3 9 H band 81 70 s 7 9 K band 79 30 s 6 7 9 Operability 99 94 9 Notes Using CDS 2 Amount of charge detected in a black frame readout immediately following a readout where 1 or more pixels are exposed to 90 or more of the maximum detector charge storage capacity 3
60. cue ball jump or scratch the incoming player accepts the cue ball in position 106 3 15 2010 UCLA Infrared Laboratory SSES ar diae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 PIDDLES Often a player finds that after several consecutive shots he or she has accumulated a large number of points but does not have a good next shot It would be tempting to make a safety shot that only barely contacts an object ball but does not risk a foul or scratch This is termed a piddle and is one of the worst things a player can contemplate doing Graduate students who are caught piddling against their advisors should generally be removed from graduate school Many professional reputations have been lost through piddling SHORTENED VERSIONS For many players 101 points can take more than an hour even with only two or three players For this reason shortened versions are encouraged The OSIRIS team often plays to 31 points in which the first 25 can be scored by any technique the next 5 only by billiards and the final one by scratching off the one ball Playing to 51 is another common variant first 45 any way then 5 billiards and finally scratching off the one ball 107 3 15 2010 UCLA Infrared Laboratory
61. dules include Remove Crosstalk Extract Spectra Assemble Data Cubes and Mosaic Frames Also we released new versions of the Quicklook2 package and Observing Planning GUI May 2007 New 0 100 lenslet scale scans are taken for all H and K broad and narrow band modes to fix saturation effects from the March 2006 scans In addition the small number of bad array elements in all the rectification files have been fixed and updated to Keck repository June 2007 Version 2 0 and 2 1 public releases of Data Reduction Pipeline Data Reduction GUI OSIRIS manual Quicklook2 package and Quicklook2 User s Manual Observations from March 2008 present For the new Kcb Kc3 Kc4 and Kc5 modes K filters with 100mas new pupil use the new rectification matrices made in March 2008 For the other modes use Rectification Scans taken in March 2006 for 0 02 0 035 0 05 lenslet scales in all filters and 0 1 lenslet scale for J and Z broad narrow band modes For H and K broad narrow band modes in 0 1 lenslet scale use Rectification Scans taken in May 2007 March 6 2008 OSIRIS servicing mission to correct for global and relative focus shifts seen in each of the spatial scales and to install duplicate Kbb Kn3 Kn4 and Kn5 with new 100mas 9m effective pupils this new combo is called Kcb Kc3 Kc4 and Kc5 and require their own rectification matrices January September 2009 OSIRIS had thermal issues during this period and the detector is oper
62. e formula for dry air where the index of refraction is approximately given by n A 1 0 0 000074 x t E oe A T where P is the pressure in millibars T is the temperature in Kelvin and is the wavelength in microns It s based on Allen s Astrophysical Quantities and is an approximation for wavelengths longer than about 400 nm For Mauna Kea I ve assumed a pressure of 620 millibars and a temperature of 273 K The deflection at a particular wavelength is then approximated by the tangent of the zenith angle times the difference in index between space n 1 000 and the telescope AQ nu 1 000 tanla And finally the differential atmospheric refraction is the tangent of the zenith angle times the difference in index between the two wavelengths n n xtan a Table D 1 Displacement in arcsec compared to 1 0 microns Wavelength microns Zenith Angle Airmass 1 2 1 4 71 6 1 8 2 0 2 2 2 4 5 1 00 0 005384 0 00863 0 010736 0 012181 0 013214 0 013979 0 01456 10 1 02 0 01085 0 017392 0 021639 0 02455 0 026632 0 028173 0 029345 15 1 04 0 016488 0 02643 0 032882 0 037306 0 040471 0 042812 0 044593 20 1 06 0 022397 0 035901 0 044666 0 050675 0 054973 0 058154 0 060573 25 1 10 0 028694 0 045995 0 057225 0 064923 0 07043 0 074505 0 077604 30 1 15 0 035527 0 056948 0 070852 0 080384 0 087202 0 092247 0 096084 35 1 22 0 043087 0 069066 0 085928 0 097489 0 105758 0 111876 0 11653 40 1 31 0 051633 0 082766 0
63. e of 2005 then the data required for the global solution does not exist and you will need to use the older routines which are intentionally not described in this manual The data cubes that are created have their indices arranged in Euro3D format which while not intuitive is at least standard The order is A y x Note that in IDL there is a transpose function and the default case when dealing with a 3D array is to swap the first 57 3 15 2010 UCLA Infrared Laboratory oS EEK ar diae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 and last indices So a call like cube transpose cube from within IDL will produce a cube arranged in the more intuitive x y A order Please see Section 4 3 2 for more information regarding the the rms residuals in data cubes with the new wavelength solution for v2 3 WCS World Coordinate System header information is now added after assembling the cube Usage The only command words recognized are Name and Skip Examples module Name Assemble Data Cube Skip 0 gt 5 9 3 Calibrate Wavelength Brief Description DO NOT USE This is an obsolete routine for resampling data onto regular wavelength grid and it will not work with data taken after commissioning period This routine is maintained only for archival data Usage The only command words recognized are Name and Skip Examples module Name Calibrate Wavelength Skip 0 gt 5 9 4 Clean
64. e reduced to 29 pixels This makes better use of the detector real estate in the horizontal direction by allowing longer spectra to fit onto the detector 3 15 2010 UCLA Infrared Laboratory SERAI SEE CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 22 Lenslet Geometry The lenslet array is rotated by 3 6 degrees relative to the dispersion axis of the grating which itself is aligned to rows of the detector This allows the spectra from neighboring lenslets to miss each other on the detector and to be successfully interleaved A side effect of this is that rows and columns of the lenslet move diagonally across the detector at an angle of 3 6 degrees To keep the spectra roughly centered on the array we stagger the lenslets every 16 row tan 3 6 1 16 So in the end 51 columns and 66 rows of lenslets are at least partially illuminated Figure 2 3 shows the geometry of illuminated lenslets We refer to the bottom left lenslet as 1 1 Note that it is not illuminated Figure 2 3 51 columns and 66 rows of lenslets are at least partially illuminated The pattern above shows in white the lenslets that are illuminated in the narrow band mode and in blue for the broad band mode Note that in many narrow band filters not all of the white lenslets are available either due to order overlap or that the spectra fall off the detector See Section 2 3 for exact sizes Also note that 15 lenslets marked in red are lost off the t
65. e simultaneous in the spectral channels It requires a coincidence in a majority of the channels and if this criterion is met the module will flag all 32 channels as bad at that location In most cases this will affect a tiny percentage of the detector pixels The Extract Spectra routine will ignore these flagged pixels but they are not replaced by the Glitch Identification module Usage The only command words recognized are Name and Skip Examples module Name Glitch Identification Skip 0 gt 63 3 15 2010 UCLA Infrared Laboratory ofS SES ar oy CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRonomy OSIRIS USER MANUAL V 2 3 5 9 13 Mosaic Frames Brief Description Usage This module combines together multiple data cubes taken in a dither sequence It can either accept the relative offsets from a file or it can use the header keywords from either the telescope or the AO system and calculate its own offsets The attribute Offset_Method is used to specify the desired offset method FILE TEL NGS or LGS Similarly at overlapping pixels the method for combining pixels together must be specified using the attribute Combine Method which can be AVERAGE MEANCLIP or MEDIAN Please see the discussion on mosaicking frames in Section 5 7 for details on how and when to use the different settings It is generally preferred to use the 17 option in this module as opposed to calling Save Dataset Information
66. ed Laboratory SSES ar diae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 were designed around the blaze functions of the OSIRIS spectrometer These filters are typically wider than traditional infrared filters and photometric corrections will be necessary for objects with extreme colors or that are line dominated Filter curves are given in Appendix C Imager Zero Point and Background Zero Point Background Band mag in DN sec mag sq arcsec J 27 8 mag 16 2 H 28 1 mag 14 6 K 27 6 mag 10 6 24 3 15 2010 UCLA Infrared Laboratory ie oS EES aro CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONoMy OSIRIS USER MANUAL V 2 3 3 Observing with Adaptive Optics Coordination between OSIRIS and the AO system is largely handled automatically but the user needs to be aware of certain limitations Pre observing planning on each science target is needed The relative position of the guide star to the science fields is not completely arbitrary due to the position of the AO system s optical axis with respect to the OSIRIS optical axis and the range of travel of the AO Field Steering Mirrors A planning tool to help determine the ranges of position angles that are possible for a given guide star science object geometry is available at http www2 keck hawaii edu software findChartGW acqTool php uide Star Tool Mozilla Firefox Keck LGS Tool List of targets C Docu
67. erfect answer for extracting a stellar spectrum but given the small fields of view that are typical for OSIRIS a curve of growth analysis is impossible and variable aperture sizes will often introduce hard to model color effects since the halo is getting smaller at longer wavelengths and has less power while the core 3625 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 is increasing in size and power So the goal of the routine is to provide a simple extraction with relatively easy to model color effects It s up to a sophisticated user to understand what this aperture photometry does to their particular PSF If the star is found near the edge of the field less than 4 pixels from the edge then the routine fails This is again just being conservative so a user is warned that there is a potential problem with their star It is then up to the user to model how the loss of one side of the halo will affect the color of the star Usage There are no parameters for this module Only the Name and Skip keywords are needed in the xml file Examples module Name Extract Star gt 5 9 12 Glitch Identification Brief Description Both the imager and spectrograph detectors show occasional bursts of intense noise which we term glitches This will happen simultaneously for all 32 output channels of the spectrograph detector This module tries to find bursts that ar
68. ermine the optimal operating temperature of the spectrograph detector show that moving from 73 K to 69 K halves the dark current produces approximately a 3 relative loss of QE and increases the magnitude of the reset anomaly from 20 DN at the worst pixel to approximately 50 DN Since any reset anomaly is quite stable and must be corrected an anomaly of 50 DN is not significantly worse in terms of performance than 20 DN Likewise a few percent loss of QE in most background environments is more than offset by the decreased dark current Operating temperatures below 70 K are preferred In the lab stable temperatures below 67 K are not achievable and it is likely that at Mauna Kea this won t change by more than a couple of degrees So we are planning on operating at Mauna Kea at temperatures between 66 K and 70 K and we can easily adjust between these two as needed for additional tests Currently the detector is operated at 68 K at Keck but before June 2007 the operating temperature was 69 K 6 Spectrograph Detector Crosstalk In the same near saturated image used in the persistence measurements a faint ghost is present in the images Figure A 8 shows a region at the boundary between the lower left and lower right detector quadrants In the right half of the image the fast clock direction is horizontal while in the left half it is vertical The image shows that although the spectrum runs horizontally in both quadrants the brightest ghost changes
69. etween 1 and 2 4 microns The center of the imaging camera s field is about 20 offset from the center of the spectrograph field and both can be used simultaneously with the same or different filters The spectrograph has plate scales of 0 020 0 035 0 050 and 0 100 arcsec per lenslet The spectral resolution averages 3800 in the three finest plate scales but is closer to 3000 in the 0 100 arcsec plate scale In the broadband mode each spectrum contains a full broad band z J H or K and a total of 16x64 actually 1019 spectra are taken In the narrowband mode a typical spectrum contains 1 4 of a broad band and an individual exposure contains between 16x64 to 48x64 spectra depending on the exact filter selected The imager has a single fixed plate scale of 0 020 arcsec per pixel and suffers from some vignetting in the corners of the array A great deal of thought has gone into trying to make OSIRIS easy to use For the spectrograph the only user selectable items are the plate scale the filter and the exposure time The imager only has a filter and an exposure time setting A great deal of complexity however is allowed in the observing sequences and the slaving of the imager to the spectrograph All setup and control aspects of the instrument are managed by a few GUIs There is also a data reduction system that includes a real time reduction of raw frames into cubes for display and basic analysis In this real time mode it takes about 1 minute for
70. fferent map for each combination of filter and plate scale Due to the unique nature of OSIRIS data and of its calibration steps the OSIRIS team has developed a pipeline designed to reduce all of the calibration data and to reduce scientific data to the level where an astronomer can begin custom analysis The pipeline is an IDL program that accepts commands only from XML files which we will refer to as Data Reduction Files DRFs Historically these files must be created by hand and then placed into the agreed upon queue directory see below Now the DRFGUI generates XML directly and can automatically submit them into the queue directory When you unpack the pipeline one of the directories created will be drs drf_queue Any file placed in this directory with a numeric prefix and an extension of waiting will be interpreted as a pending DRF file for processing The pipeline will attempt to read the file and parse the instructions It will also change the extension to working while it is processing If the reduction completes successfully then the extension will be changed to done If the reduction fails then the extension will be changed to failed If multiple waiting files exist then the pipeline will reduce them according to their numerical prefixes In run_odrp the o stands for OSIRIS There are multiple pipelines in the sense that the pipeline will treat data of different types in different ways There is actually a calibration pi
71. for v2 3 For instance programs used for the OSIRIS Calibration Reduction Pipeline CRP and the parameter file RPBconfig xml were changed to run under v2 3 If users are generating new calibration files on their own they should use the v2 3 mkrecmatrx 000 c file to generate calibration files for 2009 to present day 41 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 5 2 Major Changes to the Pipeline for Version 2 2 All modules in the pipeline are able to reduce the new K band with attached smaller 100mas pupils Kcb Kc3 Kc4 and Kc5 Added new module Scaled Sky Subtraction scales sky frames to the object frame based on the varying intensities of OH sky emission lines Added a new feature to Combined Frames which allows users to specify either a MEDIAN or AVERAGE combine routine e Added a new feature to Assemble Data Cube which now writes out WCS header information into each reduced cube This is also read in with QL2 and displayed see QL2 manual for v2 2 changes e The ODRFGUI has been updated to include all changes for the new modes and all new parameters with the v2 2 pipeline 5 2 1 Changes to the Pipeline for Version 2 1 e The Combine Frames module now uses an average to compute the output file instead of a median We are recommending that users now use the Save 1 option within the Mosaic Frames module to output the final frame i
72. global fit from 1 to 2 4 microns are 2 3 mas and 1 9 mas in the x and y axes respectively However within each filter the x residuals are 1 1 mas Zbb 0 65 mas Jbb 0 58 mas Hbb and 0 55 mas Kbb And the y residuals are 1 1 mas Zbb 0 23 mas Jbb 0 31 mas Hbb and 0 36 mas Kbb Model Residuals T T T T T T T T T T T Residual bation after adel Subtraction mas Wavelength nm Figure D 2 The residuals in the image motion after subtracting the best fit quadratic model The largest residuals occur at 1 1 microns or less 91 3 15 2010 UCLA Infrared Laboratory pape CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER n The combined effects of atmospheric and instrumental dispersions are removed with the pipeline module Correct Dispersion Instrumental dispersion using the old dichroic after August 2009 We followed the same method as for the old dichroic to derive the instrumental dispersion solution for the new AO dichroic Figure D 3 motion of the source in both axes relative to its location at 1 0 microns 1000 nm and the polynomial fit modeled within Correct Dispersion v2 3 The 2 order polynomial to the square of the total motion x and y combined with a joint additive offset for 1 00 microns is described by the following equation Total Motion mas relative to 1000 nm 55 8 4 1516 5 12 382 0 001932 AC chramatic dien sam Ahearvad with
73. has been played by some pretty famous astronomers This version has been popularized by members of the Caltech Infrared Army and James Larkin in particular makes sure each of his graduate students still masters it at well as IDL It is certainly a good way of spending snowy nights at a telescope PLAYERS Any number BALLS USED Object balls 1 3 and 5 plus the cue ball THE RACK No triangle needed the 1 ball is placed on the head spot the 3 ball on the foot spot and the 5 ball on the center spot OBJECT OF THE GAME To score 101 points prior to opponent s Shorter versions can be played typically to 51 or 31 points see below SCORING The first ninety points exactly may be scored by either of two methods First if you sink an object ball 1 3 or 5 then you score the corresponding number of points 1 3 or 5 A second way to score points is to hit two or more object balls with the cue ball This is generally termed a billiards more properly a carom and an example would be to hit the three ball and then the cue ball ricochets into the one ball Only multiple hits by the cue ball count the one hitting the three is not a billiard and each billiard counts for one point Re hitting a ball like one three one on the same stroke does not count for additional points so the maximum number of points that can be scored by billiards in one shot is two no matter how many times you hit each ball If the cue ball hits each of the three balls and sink
74. he number of iterations to perform in Extract Spectra are stored in the RPBconfig xml file within the DRS installation These should generally not be modified In a few cases however like Mosaic Frames and Divide Blackbody arguments are required within the DRF files Usage examples are given below for each module 5 9 1 Adjust Channel Levels Brief Description Measure any dcs bias shifts between the 32 spectrograph outputs and adjust to common level This is one of the big four routines that need to be run prior to extracting the spectra Usage The only command words recognized are Name and Skip Examples module Name Adjust Channel Levels Skip 0 gt 5 9 2 Assemble Data Cube Brief Description Assemble Data Cube is a crucial routine that takes the raw extracted spectra from the Extract Spectra routine and resamples them to a linear wavelength scale It breaks up narrow band spectral data and places each spectrum in its correct x y location in the data cube It uses the global wavelength map stored in osiris wave coeffs fits which 1s located in the pipeline data subdirectory of the pipeline directory If you are lucky enough to have data from late June 2005 to February 2006 which was prior to the correction of the lenslet tilt then the routine is smart enough to use the Julian day within the FITS header and will use the o d wave coeffs fits file instead If you are really lucky and have data from January to Jun
75. he second exposure is complete the online DRP will produce a data cube containing the star The online DRP reduction should take about a minute If the star is in the field but does not appear in the center use the OTGUI to move it to the center position by specifying which pixel the star is currently located on and move it to the field center Make sure the filter and scale are both set to your working scale and wavelength If the star does not appear in the field at all make sure that the AO system is still locked on the star and that you are at the OSPEC pointing origin ask your OA If everything seems right but you don t see the star it may be off the field Try switching to a narrow band filter in the 0 100 scale to get the maximum field of view 4 87 6 4 If the star is faint try increasing the exposure time although 60 seconds should be sufficient to see any TT star If desired you can take a pair of exposures to verify the centering of the TT star However this is not normally needed and it will cost you time for the exposures and reduction This is normally not necessary but one option would be to start the exposures and go on to the next step while you wait for the pipeline to finish 6 Once the TT star is centered ask the OA to Mark Base this is particularly important for the Mosaic Frames module see Section 5 7 This will set the current offset values to zero and make the telescope RA and DEC keywords ma
76. he spectral axis must also be linear in wavelength and specified with the CRVALI CRPIXI and CDELT1 keywords The CUNIT1 keyword must specify that the spectral units are in nanometers nm The blackbody is first normalized so the average channel in the spectrum is 1 0 This module is primarily used for telluric star extraction but may be applied in other scenarios 60 3 15 2010 UCLA Infrared Laboratory SSES arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomMY OSIRIS USER MANUAL V 2 3 For convenience we duplicate the effective temperatures of main sequence stars V that are appropriate for infrared wavelengths These come from Alan Tokunaga s chapter in Allen s Astrophysical Quantities Arthur N Cox editor 2000 It s important to note that these temperatures are significantly different than those derived from optical colors Sp Type TeK Sp Type Sp Type Usage The Name and Skip keywords are accepted Name is required and a temperature argument is also required Temperature must be in Kelvin Examples module Name Divide Blackbody temperature 9480 0 skip 0 gt 5 9 9 Divide by Star Spectrum Brief Description Reads in a calibration file containing a 1D spectrum typically a fully corrected telluric standard and divides it into all spatial positions within a data cube The cube must have the wavelength as the first
77. hen the cue ball or object ball must contact a cushion Failure to do so is a foul At the completion of each shot any pocketed object balls are placed back on their same positions as at the start of the game If the appropriate position is occupied the ball s in question remain off the table until the correct position is vacant after a shot If however the 1 ball would be held out as a player with exactly 100 points is to shoot the balls are all placed as at the start of the game and the player shoots with cue ball in hand behind the head string When a player scores his 90th point the shot must score the number of points exactly needed to reach 90 if the shot producing the 90th point also scores a point s in excess of 90 for the player the shot is a foul The exception to this rule is that points scored by billiards that occur after the 90 point still count and there is no foul Examples Player begins at 85 then on one stroke sinks the 5 ball and after the ball sinks the cue continues to hit the 3 ball This would raise the player s score to 91 If however the player had hit the 3 ball then hit the 5 ball into the pocket this would be a scratch since the player was at 86 points when the 5 was sunk When a player is playing for points 91 through 100 which must all be scored only by billiards it is a foul to pocket an object ball on a shot When a player is playing for his 101st point it is a foul if the cue ball fails to contact the 1 ba
78. ide by side for comparison E din oS EES aro y CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER MANUAL V 2 3 Figure 2 5 Scale drawing of the pupils for each of the four plate scales Note that the 100 mas pupil is significantly oversized to allow the other scales optical path not to be vignetted To lower the thermal background at longer wavelengths there is a smaller 100mas pupil installed just for the Kband filters magenta 12 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 There are a total of 23 filters available within the spectrograph Originally there were 4 broadband filters and 18 narrowband filters but since installation of the duplicate K band filters with smaller 100mas pupils in March 2008 there are now 5 broadband filters and 18 narrowband filters we used an open position for adding one of the duplicate filters The combination of filters and scales results in 88 discreet modes For each of the broadbands the spectra fit completely on the detector in a single exposure for the central 16x64 lenslets But since the grating does not move in OSIRIS the narrow band filters shift on the detector depending on where they fall within the broadband spectrum So for example Kn1 spectra from the central 16x64 spectra fall at the short wavelength end of the location where the Kbb spectra fall which is at the edge of the detector So lens
79. immediately then the DRF can be directly dropped into the queue by using the Drop DRF In Queue button also on the bottom of the GUI or in the File menu The queue directory can be set using the Set Queue Directory option in the File menu 46 3 15 2010 UCLA Infrared Laboratory oS EES atone CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 5 4 Working Directly with Data Reduction XML Files DRFs The Data Reduction Files DRFs that are used to instruct the pipeline are written in XML eXtensible Markup Language While it is eventually envisioned that users will almost exclusively use the ODRFGUI most current users directly edit XML files and use the osirisDropDRF facility described below For a general introduction to XML try http www brics dk amoeller XML xml index html Here we give a basic introduction to the DRF syntax before discussing the actual modules In general an XML document is a simple ASCII file composed of markup tags For OSIRIS DRFs the most common tag is used to specify the operation of a particular module such as module Name Adjust Channel Levels 0 gt In this example the tag is enclosed in a lt and gt to indicate the start and end of the tag Alternatively we could have used a lt and a gt around the tag contents but then the complete tag would require an additional lt module gt to specify the end of the tag This would look like module Name Adjust Chan
80. inearity correction applied or was hit with a cosmic ray But with the up the ramp sampling mode and a strict limit on the well depth to avoid linearity problems most of these proved unnecessary In the end the 1st and 3rd bits are generally set for valid pixels yielding a value of 9 2 1 2 3 when tested in the module Bad pixels are generally marked with a 0 and include those fixed pixels known to be bad plus any for which a valid slope could not be determined generally due to something quite bad like a cosmic ray after the first read These bits are originally produced by the detector servers in the target reduction pipeline as part of the up the ramp fitting process The IDL pipeline DRS then uses the bad pixel map to determine which pixels to use in the spectral extraction process Since multiple raw pixels are used to extract a spectrum and we know the PSF of each lenslet as a function of wavelength we can often extract a spectral pixel even if multiple detector pixels are marked bad If at least half of the flux of the PSF at a given wavelength is contained in valid pixels as determined from a numerical integration of the rectification matrix multiplied by the bad pixel array then an extracted pixel is considered valid and the quality frame of the extracted spectral pixel will be marked with a 9 value as well This generally means relatively few bad pixels occur in extracted spectra 2 FITS header keywords General Keywords ODS Key
81. ion for Mauna Kea at an airmass of 1 0 and a water vapor column of 1 6 mm All of the figures in this section come from the Gemini telescope website www gemini edu Transmission Wavelength Figure C 1 ATRAN model of the atmosphere for Mauna Kea Colored panels show the bandpasses of the OSIRIS broadband filters For detail below are higher resolution transmission curves for 1 0 and 3 0 mm of water vapor overlaid with the narrow band bandpasses 84 3 15 2010 UCLA Infrared Laboratory oS ERI ards CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Transmission Transmission Wavelength um 85 3 15 2010 UCLA Infrared Laboratory i 2 CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Transmission Wavelength um 86 3 15 2010 UCLA Infrared Laboratory oS ERI ards CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Transmission Transmission Wavelength um 87 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Appendix D Atmospheric Dispersion At adaptive optics plate scales differential atmospheric dispersion can not be neglected The table below shows the displacement in arc seconds along the parallactic axis of an object at a desired wavelength compared to its position at 1 0 microns I ve used a simpl
82. ipeline is always waiting for a new raw file to be written so the little oompa loompas can generate a reduced cube for observational viewing and acquisition needs The on line reduction GUI OORGUI allows observers to select the calibration files for the Subtract Frame and Extract Spectra modules In most cases there should be no need to edit the calibration file for the Extract Spectra module since the GUI will automatically select the most recent rectification matrix based on the observed filter and scale The Subtract Frame module can either use a specified FITS file the first file generated from a dataset or the second file generated from a dataset For example if dataset number 32 had two frames where frame 1 was a star and frame 2 was sky then you would select Next Raw Frame If instead dataset number 32 had two frames where frame 1 was sky and frame 2 was the star then you would select Previous Raw Frame If the Skip module is selected for a blue highlighted module then that module will not be used in the pipeline and will be greyed out 1 Remove Crosstalk module in the image below in the GUI Please refer to Section 5 for a detailed description of the Data Reduction Pipeline Y OSIRIS Online Reduction GUI Hep Default DRF File krootirel defaultidata default OORGUI_DRF xml Browse Log Path Construct from filename w Browse Output Directory Construct from filename 7 Browse Modules
83. is will drop a copy of test xml into the queue directory called 1 test waiting You can drop many files into the queue at the same time and they will be executed in alphabetical order Since the number is added at the front of the name it can be used to specify the reduction order Obtaining extraction matrices In addition to the pipeline itself which contains most of the necessary calibration information you must also obtain the extraction matrices for the modes of your data Since there are 88 modes and each matrix is 158 MB in size it is impractical and unnecessary for each user to collect all of them You can contact your SA at Keck and specify which plate scales and filters you used and they can direct you to a web server where the files are available 44 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 5 3 ODRFGUI The OSIRIS Data Reduction File GUI The ODRFGUI serves as the user interface to the data reduction pipeline It provides the ability to create open and modify DRFs and save them to a user specified directory or drop them directly into the DRF queue The README file included in the ODRFGUI release package contains instructions for installing it and setting up default directories The list at the top of the GUI shows the input files for the reduction Below it is an area for specifying the directories for the output files and logs and the reduction
84. ism in steps Current switch value The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechanism in steps Current switch value The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechanism in steps Current switch value The overall name of the mechanism Mechanism status Ok Moving Error Unknown The name of the current position Current position of mechanism in steps Current switch value Desired temperature for channel 1 UCLA Infrared Laboratory oS EES PEE CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 ODS Keywords Typical Value Description SCURTMP 67 079002 Temperature at channel 1 SHTRACT 1 Switch for temperature control for channel 1 0 0ff 1 0n SHTROUT 45 Heater output percentage of channel 1 SHTRRANG 4 Channel 1 heater range 0 Off 1 min power 5 max power ITRGTMP 67 Desired temperature for channel 2 ICURTMP 67 Temperature at channel 2 IHTRACT 1 Switch for temperature control for channel 2 0 0ff 1 0n IHTROUT 15 Heater output percentage of channel 2 DPWSTATI 0 Power status of outlet 1 DPWSTAT2 0 Power status of outlet 2 DPWSTAT3 0 Power status of outlet 3 DPWSTAT4 0 Power status of outlet 4 DPWSTATS 0 Power status of outlet 5 DPWSTAT6 1 Power status of outlet 6 DPWSTAT7 1 Power status of outlet 7 DPWSTATS 1 Power
85. just as easily use the final reduction GUI DRFGUI or the osirisDropDRF command to put a calibration or final xml file into the queue General Suggestions If you see strange artifacts in the reduced cubes especially roughly rectangular groups of lenslets that are offset in intensity from the main group of lenslets then it may be useful to first process files without the Extract Spectra and Assemble Data Cube routines This will produce images that are 2048x2048 pixels in size and are basically cleaned versions of the raw detector signals Look for blocks of pixels jumping up and down by a few data numbers channel offsets or streaks running vertically through the lower left or upper right quadrants crosstalk The basic routines work in most cases but they can be fooled by bright objects on channel boundaries Try skipping Adjust Channel Levels and Remove Crosstalk and see if the raw signals look improved When the 2D data looks smooth then process to completion with Extract Spectra and Assemble Data Cube Also note that Glitch Identification does not replace the pixels in the 2D data Instead it flags the pixels as bad in the quality frame extension 2 of the images and the spectral extraction ignores these pixels 40 3 15 2010 UCLA Infrared Laboratory oSE amp RK PEE CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 531 Major Changes to the Pipeline for Version 2 3 3 15 2010 Assemble Data Cubes
86. keyword that identifies the mode of the AO system so if you use NGS or LGS options you must be certain of the mode for your data Since the RA and DEC header keywords are meant to be a more accurate reflection of the true location TEL is preferred mosaic method in most cases Currently the AO team s conservative estimate of the NGS astrometric accuracy is 40 mas and the LGS astrometric accuracy is 20 mas which will be reflected in the RA and DEC header keywords as well As an additional note the FILE option is not supported within the Data Reduction GUI ODRFGUI The Combine Method determines whether to combine the frames with either a median MEDIAN average AVERAGE or sigma clipping average routine MEANCLIP The MEANCLIP method is generally preferred because it has good statistical properties and handles bad pixels and other deviants But if the observations are meant to tile a large field of view without significant overlap between each frame then the best option is to combine with AVERAGE so frames where a simple DC offset has occurred doesn t bias output values The MEDIAN option should be used with caution and typically only when there are more than 10 strongly overlapping frames Please note that the MEDIAN option does not honor bad pixels marked in the quality frame and it may do strange things if the PSF or morphology change between frames The header information from the first frame is attached to the final mosaic frame In additi
87. lets on one side of the central 16x64 are actually more centered while those on the other side fall off the detector This leads to only the central narrow band filters falling onto the detector for the full 48x64 lenslets Filters are either extreme Kn1 or Kn5 for example have some spectra off the detector and so have more limited fields of view In addition Z and J bandpasses are working at 6 and 5 diffraction orders respectively So the neighboring orders fall fairly close on the detector and order overlap makes the left most and right most lenslets in the narrowbands unusable Order overlap also limits the wavelength coverage of the broad band Z filter The long wavelength half power point of the Zbb filter lands in the 7 order on top of 0 999 microns in the 6 order So typical wavelength extractions limited to wavelengths greater than 0 999 microns Table 2 1 gives the wavelength range of each filter 5096 transmission points are quoted along with the of simultaneous spectra that are obtained in each exposure the approximate geometry of the spectra on the sky and the fields of view for each of the 4 plate scales In most cases if a narrow band filter does not cover 48x64 lenslets then it is also displaced slightly left or right on the sky The planning gui will show the true coverage of each filter compared to the OSPEC pointing origin But all filters include the central 16x64 lenslets Appendix Appendix B gives the fil
88. ll or if the cue ball contacts any other object ball When a player pockets the cue ball on an otherwise legal shot and according to the special requirements given in Scoring for counting the 101st point pocketing the cue ball on such a shot on the 101st point is not a foul Example A player is at 99 points and first hits the three ball then the one ball and the cue ball continues into a called pocket This is legal and the player would win the game The reverse order of one ball into the three ball into a pocket is a scratch A Player loses the game if he fouls in each of three consecutive plays at the table ILLEGALY POCKETED BALLS Any balls sunk in legal or illegal shots are returned to their starting positions before the next stroke as long as that location is clear JUMPED OBJECT BALLS Balls jumped off the table are returned to their start location and the shot is considered a foul SUNK or JUMPED CUE BALL If the cue ball is sunk into a pocket or jumped off the table then this is a foul and the incoming player has cue ball in hand behind the head string PENALTY FOR FOULS There is no deduction for a foul but any points that have been scored on previous shots of that inning are lost and the player s inning ends So during an inning the points scored for each shot should be totaled but kept separate from the previously scored points Only after an inning ends without a foul are the points combined for a new total After fouls other than
89. ments and Seti Browse loadfile _ Submit Star List Selected target eee ee Target name aw 244 025 _ Resolve 1370 0264802 123011 840 47 00 22 95 2000 0 rmag 9 7 sep 0 6 8 035 1230 11 900 ils s ESSERI 61 1370 0264805 123012 238 47 00 13 19 2000 0 rmagz18 1 10 4 S 0 26 DEC dd mm ss 47 00 23 00 _ 47 00638889 deg 62 1370 0264795 123011 213 47 00 24 15 2000 0 rmag 16 4 sep 7 1 8 0 25 Equinox 2000 7 E science Target 1g 83 wk231 7 1256 14 200 56 52 25 00 2000 0 64 2 125614 133 56 52 25 64 2000 0 rmag 9 7 sep 0 8 S 0 35 options 65 1468 0251307 12 56 14 035 56 52 25 25 2000 0 rmag 9 2 sep 1 4 5 0 35 i 66 1468 0251302 12 56 13 913 56 52 23 41 2000 0 rmag 9 4 sep 2 8 S 0 35 12 E 13 44 42 100 55 53 13 00 2000 0 pe 222 EEE 68 1458 0231 000 1344 42 134 55 53 12 38 2000 0 rmag 10 7 sep 0 7 820 35 Load Target _ Add to Update List Download List _Display Visibility Catalog Archive USNOB 10 Zw 244 025 DSS2R Zw 244 025 Sh _ _ _ 8 1 Position angle deg 45 ctiam Spectrograph z M use laser Aa x Guide Star farget 1370 0264811 12 30 12 5800 47 00 27 650202 1 12 16 59 Ier Pa a i 123011900 A 0 4 1370 0264812 47 0020 7604 57 i LM 2 DEC dd mm ss 470023000 A 0 6 1370 0264802 12 30 11 8400 47 00 22 950 1 34
90. ncludes fold Telescope Transmission AO Transmission Telescope Transmission i AO Transmission Cd 21 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 29 Sensitivities OSIRIS object sensitivities are a little more complicated to calculate than with a normal instrument The OSIRIS throughput varies through each band due to the atmospheric transmission blaze function of the grating and filter functions With an imager all of these factors can often be combined into a single zero point for each filter But for a spectrograph there is in essence a different zero point for every spectral channel In addition the 3000 spectra all have slight variations in efficiency primarily due to detector effects and different angles and footprints on the grating There is also the added complexity of adaptive optics imaging and the unpredictable Strehl ratio that you will achieve on your science target Nevertheless OSIRIS offers substantially better capability for true spectral photometry compared to a traditional slit spectrograph due to its integral field nature So in principle the PSF can be fully characterized and in most cases point sources are fully covered by the fields of view For sensitivity calculations each spectrum is spread over more than one detector pixel so the extraction algorithm sweeps up more than one pixel s worth of noise The amount of read noise
91. nd finally we need to close the DRF with a lt DRF gt 5 5 Reducing a Normal Observation In this section we ll walk through a standard xml file that instructs the pipeline to process the data We ll discuss the construction of some of the calibration files in later sections We begin with the header the start of the DRF tag and the dataset definition tag The ReductionType Attribute is set to SPEC so a full spectral extraction with 40 iterations 15 performed lt xml version 1 0 encoding UTF 8 gt lt final reduction of generic data gt lt DRF LogPath projects osiris DRP larkin test DRFs ReductionType ARP_SPEC gt dataset InputDir irchive osiris 051 123 SPEC raw gt fits FileName s051123_a013001 fits gt fits FileName s051123_a013003 fits gt fits FileName s051123_a014001 fits gt fits FileName s051123_a014003 fits gt fits FileName s051123_a015001 fits gt fits FileName s051123_a015003 fits gt lt dataset gt The most unique step within the OSIRIS pipeline is the extraction of the spectra from the 2D raw frames This process requires that the PSF of every lenslet as a function of wavelength has been mapped to fairly high precision These PSFs appear to be stable over many months and the calibration is done either by the instrument team or the Keck OSIRIS Master and the PSF data are stored at Keck in matrix form for all of the modes The user does not need to take thi
92. nel Levels Skip 0 gt lt module gt The module is the element start tag and specifies the type of tag in this case a module call Then Name and Skip specify attributes of the tag It is up to the pipeline to interpret these attributes In many cases tags can be nested and in fact a DRF is really just one lt DRF gt tag with many sub tags Generally white space such as spaces and carriage returns are ignored add a comment to an xml file surround the text in a lt and a gt such as in this example I This is a comment gt Now we ll begin looking at DRF specific XML tags All DRFs must start with a header specifying the flavor of xml to use lt xml versionz 1 0 encoding UTF 8 gt This is then followed by a DRF tag which must include the LogPath attribute and the ReductionType attribute For the LogPath it is usually beneficial to store these files where you store your xml files or in a nearby directory In this document we assume a directory named DRFs Data Reduction Files and place them a directory above where the reduced files will be outputted and stored The ReductionType tag specifies the type of reduction There are three main reduction types ORP SPEC Online Reduction Pipeline performed at the telescope CRP SPEC Calibration Reduction Pipeline ARP SPEC Astronomical Reduction Pipeline 47 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH INA
93. nstead of a separate call to the Save Dataset Information module This change has also been implemented in the DRFGUI Templates e Bug Fix The correct dispersion routine didn t work in all orientations due to a conflict with setting the output image dimensions 5 1 2 Changes to the Pipeline for Version 2 0 e There is now a GUI so hand editing of XML files is no longer needed except for special cases e Added new module Correct Dispersion corrects for atmospheric dispersion and instrumental dispersion and should be performed on all OSIRIS cubes after Assemble Data Cube in the final reduction processes e Added a new module Extract Star extracts 1D spectrum of a stellar object from an OSIRIS cube 42 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH IN OSIRIS USER MANUAL V 2 3 e Added a new module Remove Hydrogen Lines takes a 1D spectrum and attempts to remove absorption lines due to hydrogen The primary purpose is to remove hydrogen absorption lines from telluric standard stars e Added a new module Divide by Blackbody divides a 1D 2D or 3D spectra by a blackbody of given effective temperature e Added a new module Divide by Star Spectrum Divides cube by 1D stellar spectrum This is primarily useful for telluric correction e Fixed wavelength solution to resolve small 0 1 Angstrom shifts between each lenslet wavelength solution e The Mosaic Frames module now upda
94. nt sky subtraction the data can be prone to four common ailments These are small bias variations between the 32 detector output channels electronic crosstalk if one of the outputs has a very large signal electronic noise bursts called glitches and cosmic ray impacts To remedy these data diseases there are the big four modules which prepare the data for spectral extraction The four can be used on all types of data and should be used in the following order module Name Adjust Channel Levels 0 gt module Name Remove Crosstalk Skip 0 gt module Name Glitch Identification Skip 0 gt module Name Clean Cosmic Rays Skip 0 gt Now the frames should be clean enough to have the spectra extracted The Extract Spectra routine requires the appropriate map of the lenslet PSFs and it must have the CalibrationFile attribute set to the appropriate file lt module CalibrationFilez irchive osiris calib SPEC rectification s050624 071 100 fits Name Extract Spectra Skip 0 gt The spectral extraction produces more than 1000 spectra that are each the full width of the detector long 2048 pixels but it has not linearized the wavelength scale or assigned them to the 2 dimensional position of the appropriate lenslet Also typically 3 narrow band spectra will still be packed head to tail in the extracted spectra To cleave linearize and position the spectra into a data cube use the A
95. ntrol status 70 Telescope declination 70 00 00 0 deg 0 Declination offset 0 0 arcsec 0 Dome azimuth 0 00 deg tracking Dome status 28 217039 Telescope elevation 28 22 deg 1950 Telescope equinox 1950 0 Inas left keyword Focal station 0 guide star wavelength microns 61 391723 Telescope hour angle 19 54 25 99 h 0 Porg to instrument angle 0 0 deg no Porg to instrument y flip 54 26 0 Local apparent sidereal time h 53369 02857 Modified julian date of observation 53369 028565 110 406809 Parallactic angle astrometric 110 41 deg Pointing origin name 0 Pointing origin xposition 0 00 mm 0 Pointing origin yposition 0 00 mm Pointing origin name 1 0 Pointing origin xposition 1 0 00 mm 0 Pointing origin yposition 1 0 00 mm Pointing origin name 2 0 Pointing origin xposition 2 0 00 mm 0 Pointing origin yposition 2 0 00 mm Pointing origin name 3 0 Pointing origin xposition 3 0 00 mm 0 Pointing origin yposition 3 0 00 mm 99 UCLA Infrared Laboratory oS ESS AT dide CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL ODS Keywords RA RAOFF ROTCALAN ROTMODE ROTPDEST ROTPPOSN ROTDEST ROTPOSN ROTREFAN SECFOCUS SECTHETX SECTHETY TARGNAME TARGWAVE TELESCOP TELFOCUS TUBETEMP ODS Keywords MIRRTEMP PMFM ODS Keywords AODMSTAT AODTSTAT AOSTAT AOSTST AOTTMODE AOAOAMED AOCOMODE AOFOMODE AOWFCO DMGAIN DTGAIN OBAMNAME OBASNAME OBFMIXRA 3 15 2010 V 2 3 Typical
96. nual also has detailed instructions on installing Quicklook2 onto local machines This software package supports the UNIX Linux Mac OS and Windows operating systems 1050429 2031003 datset Kbb 0 O X File Display Tools Plot X 0 Value 0 424450 DN s XScale 8 0000 YScale 8 0000 Pointing Type nane More 33 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 42 Field Acquisition As an imaging spectrograph it is easier to acquire targets with OSIRIS than with traditional slit spectrometers but the AO system and some details of the instrument can make field acquisition non trivial Most observations require a separate tip tilt TT star for AO correction Since acquisition of science targets is often performed as a blind offset from this star it is imperative that the coordinates of the science target and the TT star are consistent with each other Given the small field of view of the OSIRIS spectrograph small errors in position can leave the science target just off the field Given the faint nature of many science targets it is easy to waste time integrating at the region adjacent to your science target Please pay attention to issues such as mismatches in coordinates between catalogs which can be particularly prevalent between older and newer stellar catalogs such as HD and HST Also proper motions of stars can be significant between your
97. observing date and the observing epoch in a catalog Remember that for OSIRIS being off by just 1 arcsec can make a big difference In general it is very important to use the Keck s AO planning tools before your run to determine the position angles and offsets from your tip tilt stars For large offsets from the star you may need to use different PAs so that both spectrograph and imager frames can be taken without defaulting the AO field steering mirrors FSM However if your science is purely with the spectrograph then in most cases you do NOT need to take acquisition frames with the imager first The procedure below is the most common type of acquisition acquiring a science target directly to the spectrograph Important to the acquisition process is putting targets accurately at the center of the spectrograph field of view which is called the OSPEC pointing origin by the telescope software The OSPEC pointing origin is the center of reduced cubes in the 0 020 scale for all broadband filters and the narrowband filters Zn3 Jn3 Hn3 and Kn3 For the other plate scales and filters the center of the field 1s slightly offset see Section 2 6 and the OTGUI of Section 4 1 During the afternoon your support astronomer will typically use the fiber source in the AO system to refine this pointing reference The acquisition procedure to place a science target on OSPEC is as follows 1 Ask the OA to slew the telescope to the primary TT star of your de
98. ommand in the source directory gmake f local Makefile On a Mac where gmake is the normal and often the only make command issue the following command in the source directory make f local Makefile To setup the environment variables cd down to drs scripts edit the setup osirisDRPSetupEnv file and set the OSIRIS ROOT variable to the base directory where you extracted the tar file Ex setenv OSIRIS ROOT net highz work 1 larkin code drs Now go to your CShrc or other environment setup file and add a line to source setup osirisDRPSetupEnv upon startup Ex source net highz work 1 larkin code drs scripts setup osirisDRPSetupEnv Source your cshrc or equivalent file and run a rehash command Or login again Running the pipeline You can now start a pipeline process Issue the command run odrp Dropping XML files Once an xml file has been created it needs to be placed into the queue This could be done simply by copying the file into the queue with a numeric prefix and a suffix of waiting Ex cp test xml drs drf queue 1 test waiting will put a copy of the test xml file into the queue and the pipeline will immediately begin to parse and execute its instructions As part of the pipeline deployment we have also created a script which accomplishes this task and knows the default queue location see the environment variable DRF QUEUE DIR In the directory with the xml file enter the command osirisDropDrf test xml 1 Th
99. on the RA and DEC for the final mosaicked frame is calculated from the pointing origin and updated in the header RA and DEC keywords The header RA and DEC keywords correspond to the location 0 0 In an individual frame the pointing origin RA and DEC is defined from either the center of the broadband 9 32 or narrowband 25 32 modes It s important if you are interested in the RA and DEC information to note that Mosaic Frames assumes the user has zero ed any offsets before their dithering script to calculate the new RA and DEC header information Please take care when centering your targets and zeroing the offset Marking Base The Mosaic Frames module should be run on frames that are taken during the same AO acquisition with same position angle PA This means if you had to reacquire at anytime during your mosaic observing sequence the keywords for the TEL and AO systems have changed compared to the previous acquisition If this is the case you can still mosaic the frames but you won t be able to rely on the header keywords and instead will need to input a file with the predetermined offsets 1 e centroid on a source see Section 5 9 7 between each of the frames lt xml version 1 0 encoding UTF 8 gt lt final reduction of generic data gt lt DRF LogPath projects osiris DRP larkin test DRFs OutputDir projects osiris DRP larkin test ReductionType ARP_SPEC gt dataset InputDir irchive osiris 051 123 SPEC raw
100. op of the detector and are not available oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 23 Filters and Fields of View OSIRIS provides four spatial scales to choose from 0 020 0 035 0 050 and 100 arcsec per lenslet There are also subtle differences in the spatial scales in terms of the effective pupil size matched to each scale This leads to differences in terms of the sensitivities and backgrounds of the four scales In a little more detail the scales are achieved by swapping in matched pairs of lenses that magnify the images onto the lenslet array As Figure 2 4 shows they all must have the same physical length of 700 mm and there are constraints about the physical size and location of the lens and filter mechanisms In particular the magnification is basically the ratio of the focal length of the camera lens to the collimator lens For the 20 mas scale this requires us to go from an F 15 beam to an F 257 beam or a magnification of 17 1 So its collimator lens has a very short focal length of only 20 mm so its cold pupil is roughly 20 mm behind the lens The collimator for the coarsest scale is closer to 100 mm so its pupil is roughly 200 mm from the input AO focus In the end only each of the three fine scales 20 35 and 50 mas have a cold pupil stop mounted with them while the coarse scale 100 mas has a fixed cold stop permanently mounted in the optical path This has the unfortunate effect tha
101. orrection would be a very time consuming step in the target reduction pipeline prior to writing FITS files we give here the raw non linearity of the device at 50 and 80 If a pixel is above the 80 full well level then the target reduction pipeline ignores its value Notes 1 3 15 2010 Table 9 Spectrograph Detector Controller Characterization Parameter Value Units Notes Noise 69K 8 5 to 11 5 e RMS 1 73K 10 e RMS 1 75K 11 e RMS 1 Crosstalk 100 1 ratio 2 row to row only Readout Time 0 829 seconds 3 Uniformity 10 4 8 Non linearity at 50 2 5 Non linearity at 80 3 6 Zero Point Variation lt 3 e 7 75 Using up the ramp sampling at a readout rate appropriate for the required total readout time Values given based on a difference frame with an assumed gain of 3 e DN UCLA Infrared Laboratory egisti 5 oS EEK Pb CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 2 See A 6 3 Time required to read out the full array using all 32 ports This is as measured with the deliverable clocking code 4 Total uniformity of the detector response at any instrument wavelength and over the full useful dynamic range after flat fielding and other response corrections 5 When exposed to a constant source flux this is the percentage difference between the linear trend at low flux vs that measured at 50 full well which corresponds to approximately 68 00
102. osiris 0 705 17 SPEC r Adjust Channel Levels Adjust Channel Levels _ Not Used USED Remove Crosstalk Remove Crosstalk 1 Not Used USED Glitch Identification litch Identification _ Not Used USED Clean Cosmic Rays lean Cosmic Rays _ Not Used USED Extract Spectra xtract Spectra ost recent valid file net helium datairchive osiris calib SPEC rect Assemble Data Cube Assemble Data Cube _ Not Used USED Correct Dispersion orrect Dispersion ot Used USED Mosaic Frames Frames Not Used USED Extract Star Save DataSet Information NotUsed USED Remove Hydrogen Lines Divide Blackbody Divide by Star Spectrum Save DataSet Information 4 il Argument Value Mosaic Frames combines multiple Combine Method AVERAGE p Offset Method TEL OSIRIS cubes with the same PA using header keywords from TEL default NGS and LGS Combining frames may he performed with either AVERAGE default MEDIAN or MEANCLIP Save DRF As Drop DRF In Queue If the user wishes to skip a module but not remove it from the list the check box in the Skip column can be checked This will include the module in the DRF but with a Skip flag set so the pipeline doesn t execute that module When the DRF is configured as desired the user can save it to disk for later use by clicking on the Save DRF As button on the bottom of the GUI or in the File menu If the user wishes to have the DRP execute the DRF
103. peline a stellar pipeline an online pipeline and a final pipeline But this is somewhat artificial and all pipelines can be executed by the single pipeline process simply by specifying the type of reduction you d like in the first line of the DRF The reason for the distinction is that each pipeline can in principle use different module code attached to the same command For example if you use the Extract Spectra command in your DRF file it will do something different in the online pipeline compared to the final pipeline In this particular case it s just the number of iterations that are performed which ensures the online version is fast The final 39 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 pipeline will complete more iterations which will result in cleaner spectra A configuration file RPBconfig xml is part of the pipeline distribution and specifies which modules are allowed for each pipeline and which pro file to use for a particular command In the case of spectral extraction a single program is called but it forks to different algorithms based on which pipeline was specified In principle when you are taking data and have the pipeline running in the background it can perform any type of reduction The OORGUI is what actually senses new frames and drops DRF files into the queue with the ORP specification During a long exposure you could
104. per spectral channel therefore depends weakly on plate scale and wavelength The best demonstrated read noise per pixel using the up the ramp sampling method is 4 8 electrons this actually also includes a dark current and detector glow component With the new grating installed in June 2005 arclines are more elongated perpendicular to the dispersion axis than at the time of preship This leads to more read noise per spectral channel than with the original grating although several other factors including throughput improved dramatically A typical read noise component for extracted spectra is about 10 electrons in the up the ramp mode In Table 2 7 below we give the zero points for the OSIRIS spectrograph expressed in extracted DN sec In these units the zero points are defined in the standard way Mag 2 5 log flux in DN sec Mag zero point Table 2 7 Spectrograph Zero Points Spectrograph Zero Points Band if flux is in DN sec J 23 5 mag H 24 3 mag K 23 7 mag To convert to electrons assume a detector gain of 0 23 DN per electron To calculate rough sensitivities for a continuum source estimate the flux per lenslet element for your target assuming a reasonable Strehl ratio see the AO page for expected Strehls with the Laser or NGS targets You can then use the zero points to determine the number of data numbers per lenslet that will be generated per second Multiply this by your exposure time and divide by
105. pif Lp PE La pj Vavelength nr For the Hbb filter the extracted wavelengths are limited to the half power points of the filter at 1 473 to 1 803 microns The excluded wavelengths for this filter are shown in the shaded red regions For the Hnarrow filters each is also effective from their half power points given in Table 2 1 The atmosphere may also be a significant limitation in some wavelengths Please see Appendix C for atmospheric transmission 82 3 15 2010 UCLA Infrared Laboratory oS EEK pee CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 Transmissior 1 t a 7 Reed For the Kbb filter the extracted wavelengths are limited to the half power points of the filter at 1 965 to 2 381 microns The excluded wavelengths for this filter are shown in the shaded red regions For the Knarrow filters each is also effective from their half power points given in Table 2 1 The atmosphere may also be a significant limitation in some wavelengths Please see Appendix C for atmospheric transmission 83 3 15 2010 UCLA Infrared Laboratory oS EES rdg CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER a Appendix C Atmospheric Transmission The atmospheric transmission across the 1 2 4 micron region is dominated by deep water bands at roughly 1 13 1 4 and 1 9 microns Figure C 1 shows an ATRAN Lord S D 1992 model for the atmospheric transmiss
106. plots by setting the keyword show plots 0 in the DRF The five rows of plots are as follows 1 In the first row you can see how it selects lenslets in the science data cube that are probably sky i e have low counts 2 The next plot shows the extracted spectra from the sky and object cubes using those same selected lenslets the OH lines are highlighted in different colors 3 The third plot shows the different scaling factors found for each family of OH lines in this case variously about 1 14 4 The next plot shows the subtracted spectra of the science cube minus the raw and scaled sky cubes while 5 the final plot shows the residuals post subtraction for the raw and scaled skies In this case you can tell that the scaling algorithm works well as the red OH residuals before scaling have vanished in the blue plot after scaling These test data happen to be adjacent 900 s Hbb exposures so this shows the kind of improvement possible over even short timescales by compensating for OH variation 68 3 15 2010 UCLA Infrared Laboratory KESK CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Scaled Sky Subtraction for intermed pip Imaga log scala Good Spoxels used for sky Input Spectra OBJ qreen purple SKY eyan blue Ane x m k n 1 65 Wordength micron Sealing Factar E 2 E 1 E EJ H E 8 1 65 Wavelength micron
107. s 5051123 a000006 fits gt fits 5051123 a000007 fits gt fits 5051123 a000007 fits gt fits 5051123 a000008 fits gt fits FileName s051123_a000009 fits gt lt fits FileName s051123_a000010 fits gt fits 5051123 a00001 1 fits gt lt dataset gt module Name Glitch Identification gt lt module Name Combine Frames gt lt module Name Save DataSet Information gt lt DRF gt 5 7 Mosaicking Multiple Science Exposures In order to combine multiple science exposures that are dithered with respect to each other you may use the Mosaic Frames module This module is part of the ARP SPEC reductions There are two parameter values for this routine The Shift_Method parameter specifies how the spatial shifts between frames should be calculated If Shift_Method is set to TEL which is the recommended method then the offsets are calculated from the telescope right ascension and declination coordinates in the header If Shift_Method is set to FILE then a file containing the RA and DEC offsets relative to the first frame in arcsec is required If Shift_Method is set to ipt 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH IN OSIRIS USER MANUAL V 2 3 NGS or LGS then AO offset header information 1s used from either the NGS or the LGS header keywords Note there is no
108. s This code has only been tested on a limited data set and we encourage users to carefully evaluate how well it works for different filters and in different atmospheric conditions In order to use this module you must first make a reduced sky cube that can be scaled then subtracted The overall steps are as follows a make a master dark frame from several raw dark frames b reduce a sky frame into a sky cube using the master dark Save this sky cube to a FITS file c reduce the object frame to a cube using the same master dark and subtract the scaled sky The scaled sky subtraction module should go in DRF right after Correct Disperson and takes as its CalibrationFile argument the name of your sky cube The module then applies the Davies algorithm to scale each OH line family to minimize the residuals and outputs the subtracted cube There are a few options for tweaking the algorithm most of which can safely be left at their defaults These keywords include Min Sky Fraction and Max Sky Fraction which influence how much of the sky is used for determining the ratios and Line Halfwidth which sets how many spectral channels are used for each detected OH line In addition the Scale K Continuum keyword allows the user to choose whether to perform scaling of the continuum at K band to match observations the default is Yes When run this module displays some plots so you can see how well it s working or you can disable the
109. s all three balls then a total of 11 points would be scored which is the maximum for any stroke Points 91 through 100 exactly must and may only be scored by execution of carom shots billiards Point 101 winning point must be scored by scratching the cue ball off of the one ball into a called pocket The one ball must be the only ball hit by the cue ball since any other contact would be a billiard and would result in a foul see below Any multiple contacts with the one ball or bumpers must be called 105 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH IN AsrRoNouwY OSIRIS USER MANUAL V 2 3 OPENING BREAK No break shot as such Beginning with cue ball in hand behind the head string line the starting player must cause the cue ball to contact the 3 ball which will be at the opposite stop first If starting player fails to do so incoming player has the choice of 1 requiring starting player to repeat the opening shot or 2 executing the opening shot himself RULES OF PLAY A legally executed shot conforming to the requirements of Scoring entitles the shooter to continue at the table until he fails to legally execute and score on a shot The series of consecutive shots taken by a single player is termed an inning Innings continue as long as a player scores at least one point on each shot and does not foul On all shots player must cause the cue ball to contact an object ball and t
110. s type of calibration data but does need to obtain the necessary matrices from the Keck repository for their observing modes filter and plate scale The Extract Spectra routine can then use the PSFs to iteratively assign flux at a particular pixel location into its corresponding lenslet and wavelength channel This is the most CPU intensive algorithm and there are two versions one for real time use at the telescope and one for science grade post processing An essential 49 3 15 2010 UCLA Infrared Laboratory CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONomY OSIRIS USER MANUAL V 2 3 element of the spectral extraction is that it assumes that any signal within the data frame is due to photons from the astrophysical source Any detector artifacts or extraneous signals will be incorrectly attributed to lenslets and create artifacts that are hard to track down in the reduced data cubes The first step in the data reduction is always to subtract a high quality dark or sky frame in order to remove detector glow and bias These features are the dominant detector artifacts that would corrupt the spectral extraction process This is extremely important and it is essential that clean sky images are taken as part of the observing sequences Then the first module within most DRFs will be Subtract Frame module CalibrationFile2 projects osiris DRP Sky 900 datset Hn3 100 O fits Name Subtract Frame gt Even with an excelle
111. sTRONomMY OSIRIS USER MANUAL V 2 3 So an example DRF tag might look like DRF LogPath directory DRFs ReductionType ARP SPEC Note that the gt does not end the tag and future tags are really attributes within the DRF tag At the end of the file you must close DRF tag with a lt DRF gt See below for examples After the DRF tag you need to define the data frames that should be processed This is done with the DATASET tag It must include an InputDir attribute and then a series of FITS attributes that list the filenames Optionally you can include a Name attribute and an outputdir tag although name is completely optional and the outputdir is more commonly specified in the specific output modules So an example of the DATASET tag might be dataset InputDirz archive osiris 051123 SPEC raw gt fits FileNamez s051123 a013001 fits gt fits FileNamez s051123 a013003 fits gt fits FileNamez s051123 a014001 fits gt fits FileNamez s051123 a014003 fits gt fits FileNamez s051123 a015001 fits gt fits FileNamez s051123 a015003 fits gt lt dataset gt The typical DRF is then composed of a series of module files specifying the order of the reduction steps as well as any calibration files and parameters that are needed The specific calibration files and parameters for each module are described in Section 5 9 If the frame needs a calibration file 1 e Subtract Dark Frame Extract Spectra the attri
112. se locations This is an over determined problem which is treated as a large sparse matrix inversion The inversion occurs iteratively in a process that is mathematically identical to Lucy Richardson deconvolution The resulting spectra are stored back into a new 2D array in which the now clean spectra lay along a single row with no contamination from neighbors The only routine that can make sense of one of these images is the Assemble Data Cube module that will linearize the wavelength scale and position each spectrum in its correct 2D position The name and skip keywords are accepted as always but a CalibrationFile is also required This will be the full name of the influence matrix for the type of data that you re working on Note there is a unique influence matrix for each filter and scale combination Examples module CalibrationFilez archive SPEC rectification s050624 071 100 fits Name Extract Spectra Skip 0 gt 5 9 11 Extract Star Brief Description Extract Star accepts a cube containing a relatively bright point source It collapses the spectral channels and attempts to find the centroid of the brightest source in the field It then performs aperture photometry about this centroid in each spectral channel and produces a 1D spectrum The tag 147 is added to the filename so Save DataSet Information does not overwrite a cube produced from the same dataset Simple aperture photometry is never the p
113. sired science target 2 During the slew adjust the position angle to the desired value using Rotate tab on the OTGUI See Section 4 1 3 When the rotation is complete locate the TT star on the guider display using a finding chart Ask the OA to acquire the TT reference star to the OSPEC pointing origin by giving the pixel coordinates of the TT star on the guider often this will be obvious and the OA will immediate acquire the star The OA should acquire to the OSPEC pointing origin using the Adjust Pointing button on xguide The TT star should now be centered on OSPEC 34 3 15 2010 UCLA Infrared Laboratory SSES av diae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 4 If you are planning to take science frames in the 0 020 scale in a filter for which OSPEC is the center see above skip to the next step Otherwise you must perform an offset to put the TT star in the center of your working scale and filter On the Offset tab of the OTGUI perform a move from the center of any OSPEC centered filter in 0 020 mode to the center of the scale and filter you plan to use for your science 5 Once you ve moved the star to your particular center location take an on source and off source or sky pair of images Using the OOPGUI define a dataset with a stare exposure with no offset as the object frame and a stare exposure with an offset of 5 arcsec as the sky frame When t
114. ssemble Data Cube module module Name Assemble Data Cube Skip 0 gt This is the last reduction step that we want to perform so we re ready to output the reduced FITS files This is done with the Save DataSet Information module which requires an outputdir attribute The output filenames are built out of the DATAFILE keyword in the FITS files lt module Name Save DataSet Information OutputDir projects osiris DRP larkin gt 50 3 15 2010 UCLA Infrared Laboratory oSESK ard CALIFORNIA ASSOCIATION FOR RESEARCH IN AsrRoNouwY OSIRIS USER MANUAL V 2 3 Finally we close the DRF tag which ends the XML file lt DRF gt For our example the full DRF looks like lt xml version 1 0 encoding UTF 8 gt lt final reduction of generic data gt lt DRF LogPath projects osiris DRP larkin test DRFs ReductionType ARP_SPEC gt dataset InputDir irchive osiris 051 123 SPEC raw gt fits FileNamez s051123 a013001 fits gt fits FileNamez s051123 a013003 fits gt fits FileNamez s051123 a014001 fits gt fits FileNamez s051123 a014003 fits gt fits FileNamez s051123 a015001 fits gt fits FileNamez s051123 a015003 fits gt lt dataset gt module CalibrationFile projects osiris DRP Sky_900_datset_Hn3_100_0 fits Name Subtract Frame gt module Name Adjust Channel Levels Skipz 0 module Name Remove Crosstalk Skip 0 gt module Name Glitch Identification Skip
115. status of outlet 8 DPWNAMEI Unused Name of the device controlled by outlet 1 DPWNAME2 Unused Name of the device controlled by outlet 2 DPWNAME3 Unused Name of the device controlled by outlet 3 DPWNAMEA Unused Name of the device controlled by outlet 4 DPWNAMES Unused Name of the device controlled by outlet 5 DPWNAME6 Imager Electronics Name of the device controlled by outlet 6 DPWNAME7 Spec Electronics Name of the device controlled by outlet 7 DPWNAMES EC Cooling System Name of the device controlled by outlet 8 EPWSTATI 1 Power status of outlet 1 EPWSTAT2 1 Power status of outlet 2 97 3 15 2010 UCLA Infrared Laboratory WM eiiis DS SEC jc orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY ODS Keywords EPWSTAT3 EPWSTAT4 EPWSTATS EPWSTAT6 EPWSTAT7 EPWSTATS EPWNAMEI EPWNAME2 EPWNAME3 EPWNAME4 EPWNAMES5 EPWNAME6 EPWNAME7 EPWNAMES ISSKY OBSERVER TELESCOP SETNUM DATASET OBJECT SFILTER IFILTER SSCALE SFRAMES IFRAMES OBJPTTRN SKYPTTRN IMAGMODE 3 15 2010 Typical Value 1 1 Pressure Gauge Lakeshore 340 Dewar Lakeshore 218 Cabinet Lakeshore 218 Motor Controllers Terminal Server Unused EC Cooling System 1 Nobody 21 test009 Dark at 67 Kelvin Hn3 Hn3 0 02 1 1 Slave 2 Maximum Itime 98 OSIRIS USER MANUAL V 2 3 Description Power status of outlet 3 Power status of outlet 4 Power status of outlet 5 Power status of outlet 6 Power status of outlet 7 Power status of outle
116. t 8 Name of the device controlled by outlet 1 Name of the device controlled by outlet 2 Name of the device controlled by outlet 3 Name of the device controlled by outlet 4 Name of the device controlled by outlet 5 Name of the device controlled by outlet 6 Name of the device controlled by outlet 7 Name of the device controlled by outlet 8 Flag for sky frames 0O not sky 1 sky Observer name s Telescope name Dataset number Dataset name Object name Move spec filter wheel by name Imager filter Spec Scale Number of spec frames in dataset Number of imag frames per spec frame Dither pattern for object frames Dither pattern for sky frames Imager observation mode UCLA Infrared Laboratory WM eiiis DS E F A orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY ODS Keywords UTC AIRMASS AXESTAT AZ CALOCAL CELOCAL CURRINST DATE OBS DCSSTAT DEC DECOFF DOMEPOSN DOMESTAT EL EQUINOX FOCALSTN GUIDWAVE HA INSTANGL INSTFLIP LST MJD OBS PARANG PONAME POXPOS POYPOS PONAMEI POXPOSI POYPOSI PONAME2 POXPOS2 POYPOS2 PONAME3 POXPOS3 POYPOS3 3 15 2010 OSIRIS USER MANUAL V 2 3 DCS Keywords Typical Value Description 41 08 0 Coordinated Universal Time h 0 Air mass 0 00 tracking Axes control status 19 923125 Telescope azimuth 19 92 deg 0 Collimation azimuth local 0 0 arcsec 0 Collimation elevation local 0 0 arcsec AO Current instrument 12 30 2004 Universal date of observation unknown Drive and co
117. t it must be oversized to allow through all of the other beams and allows through considerable excess thermal background In order to lower thermal background at longer wavelengths in March 2008 the OSIRIS team smaller pupil sizes designed smaller 100 mas pupils to be used with duplicate K filters There are four filter holders and four new pupils that were attached individually for each duplicate K filter Kbb Kn3 Kn4 Kn5 The pupil sizes for each of the scales and the new effective 9 meter inscribed pupil for the 100mas scale is illustrated in Figure 2 5 0 020 arcsec scale This is the only scale that has proper sampling across the AO PSFs for wavelengths longer than 1 5 microns So it is optimized for image quality and has a slightly oversized pupil that is circumscribed around the 10 94 m outer edges of the Keck telescope Because of this it has an elevated thermal background K 11 2 mag sq arcsec At wavelengths below 2 microns it is primarily read noise limited so the coarser scales have better raw sensitivity 0 035 amp 0 050 arcsec scales These two scales are optimized for maximum sensitivity at thermal wavelengths K 11 8 mag sq arcsec They both have circular pupils equivalent to a 10 meter telescope so they slightly clip the edges of the Keck primary But since they have coarse sampling the PSF is not significantly affected 0 100 arcsec scale Originally this was only included to help with target acquisition but many users ha
118. tch the sky Then ask the OA to Offset to science target which will place your science target on the OSPEC pointing origin In LGS AO operations the OA will acquire using LGS AO Acq on OSPEC 7 Begin science observations 35 3 15 2010 UCLA Infrared Laboratory oS EEK Pep CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 43 Spectroscopic Calibration 4 3 1 Telluric Standards The atmosphere in the infrared has significant transmission variation both with wavelength and with time In order to properly reduce a spectrum this transmission must be estimated at an elevation and atmospheric condition close to your science target We recommend using an AO star within 0 1 airmasses of your science exposure Stars with magnitudes between 7 and 9 work well and typical exposure times are 20 seconds If you spend roughly an hour on a given target field we often select a telluric star at about the same declination but 30 minutes later in RA from the science target This will place the star at about the average location in the sky that the science exposures were taken The pipeline modules Extract Star Remove Hydrogen Lines and Divide by Blackbody work to produce a 1D spectrum of a star taken for telluric correction To work properly the star must be at least 4 pixels from the field edges and must have no significant spectral features besides hydrogen absorption lines This typically means using stars near spectral type
119. telluric absorption e g 5070406 a029002 tlc Jbb 100 fits When a datacube is passed through the Extract Star module it becomes a ID spectrum and the 14 tag is added eg 5070406 021001 Kbb 100 fits For the Mosaic Frames module the preferred method to output a file is with the Save 1 flag to the module In this case the base will again be the name of the first input file plus mosaic Since the files have been combined together the frame number is removed e g 8051123 a013 mosaic 3 100 fits 51 3 15 2010 UCLA Infrared Laboratory 44 3 ard CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomY OSIRIS USER MANUAL V 2 3 5 6 Reducing Multiple Darks or Skies into a Super File Often you will take many dark or sky frames and would like to combine them into a single frame with significantly better signal to noise This is a standard procedure and is easily handled by the pipeline The procedure is the same for darks or skies and the routines assume that each frame within a set is similar except for noise and fluctuations of sky lines The xml file starts with the standard header information including the output directory logpath and reduction type which can be ARP or CRP lt xml version 1 0 encoding UTF 8 gt lt make_super_dark gt lt DRF LogPathz net hydrogen data projects osiris DRP larkin test DRFs OutputDirz net hydrogen data projects osiris DRP larkin test ReductionType CRP SPEC
120. temperature sensor 1 DTMPLOC2 Primary Plate Location of temperature sensor 2 DTMPLOC3 Secondary Plate Location of temperature sensor 3 DTMPLOC4 Front Splitter Mirror Location of temperature sensor 4 DTMPLOCS5 Scale Turret 2 Location of temperature sensor 5 DTMPLOC6 Lenslet Mask Stage Location of temperature sensor 6 DTMPLOC7 TMA Housing Location of temperature sensor 7 DTMPLOCS8 Cold Shield Location of temperature sensor 8 DTMPI 38 806 Temperature at sensor 1 DTMP2 53 089001 Temperature at sensor 2 DTMP3 43 915001 Temperature at sensor 3 DTMP4 55 848 Temperature at sensor 4 DTMP5 45 626999 Temperature at sensor 5 DTMP6 52 550999 Temperature at sensor 6 DTMP7 51 935001 Temperature at sensor 7 DTMP8 64 728996 Temperature at sensor 8 CTMPLOCI ECCSI Intake Name of the location of temperature sensor 1 CTMPLOC2 ECCS1 Exhaust Name of the location of temperature sensor 2 CTMPLOC3 Top of Cabinet Name of the location of temperature sensor 3 CTMPLOCA Ambient Air Name of the location of temperature sensor 4 CTMPLOCS ECCS2 Intake Name of the location of temperature sensor 5 CTMPLOC6 ECCS2 Exhaust Name of the location of temperature sensor 6 CTMPLOC7 EC2 Mid of Cabinet Name of the location of temperature sensor 7 CTMPLOC8 EC2 Top of Cabinet Name of the location of temperature sensor 8 CTMPI 295 95999 Temperature at sensor 1 CTMP2 294 029999 Temperature at sensor 2 CTMP3 294 95999 Temperature at sensor 3 CTMP4 297 200012 Temperature at Sensor
121. ter transmission curves Take note that the filters named Kcb Kc3 Kc4 and Kc5 in the OSIRIS planning GUI OOPGUI are just duplicate Kbb Kn3 Kn4 and Kn5 filters with the smaller 100mas pupil 13 3 15 2010 UCLA Infrared Laboratory SEE aro CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 Table 2 1 OSIRIS Spectrograph Filters Scales and Fields of View Shortest Longest Number of Number of Approx Wavelength Wavelength B peg Complete Lenslet FOV for FOV for FOV for Filter Extracted nm Extracted nm e Spectra Geometry 0 020 0 035 0 050 Zbb 999 1176 1476 1019 16x64 0 32x1 28 0 56x2 24 0 8 3 2 Jbb 1180 1416 1574 1019 16x64 0 32x1 28 0 56x2 24 0 8 3 2 Hbb 1473 1803 1651 1019 16x64 0 32x1 28 0 56x2 24 0 8x32 Kbb 1965 2381 1665 1019 16x64 0 32x1 28 0 56x2 24 0 8 x 3 2 Zn4 1103 1158 459 2038 32x64 0 64x1 28 1 12x2 24 1 6 x 3 2 Jnl 1174 1232 388 2038 32x64 0 64x1 28 1 12x2 24 1 6 x 3 2 Jn2 1228 1289 408 2678 42x64 0 84x1 28 1 47x2 24 2 1 x 3 2 Jn3 1275 1339 428 3063 48x64 0 96x1 28 1 68x2 24 2 4 x 3 2 Jn4 1323 1389 441 2678 42x64 0 84x1 28 1 47x2 24 2 1 x 3 2 Hnl 1466 1541 376 2292 36x64 0 72x1 28 1 26x2 24 1 8 x 3 2 Hn2 1532 1610 391 2868 45x64 0 90x1 28 1 58x2 24 2 25x3 2 Hn3 1594 1676 411 3063 48x64 0 96x1 28 1 68x2 24 2 4 x 3 2 Hn4 1652 1737 426 2671 42x64 0 84x1 28 1 47x2 24 2 1 x 3 2 1721 1808 436 2038 32x64 0 64x1 28 1 12x2 24 1 6 x 3 2 1955 2055 401 2292 36x64 0 72x1 28 1 26x2 24 1 8
122. tes the RA and DEC header in the output file e The Save Dataset Information module has a new naming convention for output files 1 e 5070404 2017001 datset Kbb 100 fits will now be 5070404 3017001 100 fits without the datset 5 2 Installing the Pipeline at Your Home Institution The system requirements are IDL 6 or later and a gcc compiler on a linux or solaris computer It also works under MAC download Marshall Perrin s MAC installation script install drs py The pipeline also requires roughly 1 GB of memory and will run slowly on a machine with limited RAM To obtain tar file Go to http www astro ucla edu irlab osiris and click on the link for the pipeline To unpack Place tar file in a directory that is part of your path and idl path In our example we ll use net highz work 1 larkin code Then unpack the tar file cd net highz work 1 larkin code cp net highz kroot krootdev osrsdev kroot kss osiris drs tar tar xvf drs tar To compile cd down to drs modules source edit the local Makefile to set the IDL INCLUDE directory to where your local idl source resides You may also need to set the CFITSIOLIBDIR variable to the directory containing the cfitsio binary file The scisoft default will be correct for most people 43 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRoNomMY OSIRIS USER MANUAL V 2 3 On a linux or Solaris system issue the following c
123. the plate scales in each direction different which is not observed 28 Throughputs In this section we summarize the vendor data on individual component efficiency along with the estimate of the grating efficiency as derived from the relative efficiency of the spectrograph and imager For simple elements such as the gold mirror or BaF lenses we use the coating reflectances or transmittances supplied by the coating vendor Notice that the measured efficiencies in the H and K bands are comparable to each other but about 3096 lower than expected We have somewhat arbitrarily assigned the majority of this to the grating In the J band however the efficiency falls dramatically to only 2 796 We do not know the source of this efficiency loss and we believe it is unfair to assign the full extent to OSIRIS We note that NIRC2 appears to have at least a factor of 2 loss of efficiency from the K to the J bands Table 2 6 lists the component efficiencies as presented at the PDR and as built Table 2 6 Predicted and As built Efficiencies Efficiency predicted at PDR H and K bands 97 92 75 92 96 96 92 assumes some dirt 7096 peak 42 avg 96 ED 65 25 80 65 90 TOTAL THROUGHPUT OPTICAL ELEMENT Window old Mirrors ollimator Lens ilters amera Lens enslet Array AR Coated 2 surfaces Collimator 4 mirrors 99 includes first fold rating varies with wavelength amera Optics 4 mirrors 99 i
124. the telescope The GUI will automatically switch to this cover when not in use e The Offset folder allows users to center the spectrograph between different modes filter and scale and offset to the imager It also allows users to offset in RA and DEC in arcsec or detector pixels it will use the current scale of the instrument so check the status GUI e The Rotate folder changes the position angle of OSIRIS The Adaptive Optics folder allows input wait4ao ON or OFF The script wait4ao determines whether you want the observations to wait for the AO loops DM and TT to close before taking an exposure You can either select wait4ao which includes both the DM and TT or wait4dm or wait4tt ON or OFF e The OSIRIS folder allows you to flush the spectrograph and imager detector It takes a number of short integrations to clear the detector This should only be done if persistence is seen in the detector from a bright star or if there are detector artifacts after issuing the command Abort All Immediately OSIRIS Telescope GUI File Help wait4dm Y Instrument Filter From of to pixelat v of Imager v Zh Offset in RA Dec in arcsec en Offset in Spec X Y in arcsec 07 06 06 10 36 40 A 3 15 2010 UCLA Infrared Laboratory pape CALIFORNIA ASSOCIATION FOR RESEARCH INASTRONOMY OSIRIS USER On line Reduction GUI At the telescope the OSIRIS p
125. timate the shifts and does not work without a significant source within the field It is not generally needed since the Mosaic Frames module can normally use the RA and DEC header keywords to do a good job of mosaicking frames But if objects are reacquired during a sequence and the header RA and DEC are slightly inconsistent then this routine can produce a file containing the offsets for the Mosaic Frames module This module is not supported within the Data Reduction GUI Usage The name and skip keywords are accepted and OutputDir must be specified so that the output shifts can be stored Examples module Name Determine Mosaic Positions OutputDir home larkin data Save 0 SaveOnErr 0 Skip 0 gt lt module gt lt module Name Mosaic Frames OutputDir home larkin data CalibrationFile the offset file that has been produced by Determine Mosaic Positions Save 0 SaveOnErr 0 Skip 0 gt lt module gt This way you have to execute the xml file twice In the first run you have to skip the second module to determine the name of the offset file that will be produced by mosaicdpos 000 and in the second run you do not need to determine the offset list again so skip the first module 5 9 8 Divide Blackbody Brief Description Divide Blackbody divides a spectrum by a blackbody spectrum of a specified temperature It works on 1D 2D or 3D data but it assumes the spectral axis is the 1 one Euro3d standard T
126. tput filename of the reduced data to be something other than the default Usage It accepts an OutputFilename argument which should be a string containing the desired name of the output file This file will be written into the regular output data directory Example module Name Rename File OutputFilename myawesomestar_H_900s fits gt 66 3 15 2010 UCLA Infrared Laboratory SSES arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 5 9 17 Save DataSet Information Brief Description The Save Dataset Information routine is the primary method to have the pipeline output reduced data It uses the DATAFILE header keyword in the FITS header to build an output filename Usage It accepts a Name Skip and OutputDir keywords Examples lt module Name Save DataSet Information OutputDir projects osiris DRP larkin gt 5 9 18 Scaled Sky Subtraction Brief Description Marshall Perrin generated this module which implements mostly the OH line suppressing scaled sky subtraction algorithm from Davies 2007 MNRAS The basic idea is that the various OH lines that make up the sky background arise from certain families of vibrational transitions While the intensity of the sky lines can vary unpredictably throughout the night the lines within a given family tend to fluctuate up and down together Thus one can look at the brighter sky lines and determine for each transition family the ratio between
127. type Below this is a dropdown list for selecting one of several predefined reduction templates Under this section are a few tables in resizable windows On the left is a listing of all available modules for the selected reduction type A description of the module is displayed below the list when a module is clicked Double clicking on a module will add it to the active list of currently used modules to the right The modules are ordered in a specific manner based on the backbone requirements modules cannot be reordered Double clicking on a module in the active module list removes it from the list For modules with arguments clicking on a module will show the argument options below the active module list Values for the arguments can be set by typing text directly into the box or selecting from a dropdown if enumerated choices are given To create a DRF first select a reduction template The active module list is then populated with the set of modules as specified by the template Calibration files that have not been specified or found are displayed in red text The Find File column is used to specify how the GUI will find the calibration file If it is Specify a file the user must manually specify the file A file browser is presented when the user clicks on Specify a file from the dropdown in the Find File column or by double clicking in the Resolved Filename field With some Find File methods such as Most recent valid file
128. ut lenslet location as the 3 extension and finally a record of the shifts applied to each image as the 4 extension The shifts in the 4 extension are given in the original data coordinates which is the transpose of what is displayed in the QL2 window x y A Therefore the first column of the array in the 4 extension will represent the y shifts in the QL2 display and the second column will represent the x shifts in the QL2 display If Save DataSet Information is used only the zero first and 274 extensions will be written similar to any dataset Any module calls after Mosaic Frames will contain only the mosaicked frame in the dataset All record of the individual input files are lost The output will be the name of the first input file plus mosaic i e 5051123 2013001 mosaic 100 fits The DRF used for creating the mosaic will be stored in the header so the frames used in the mosaic and their mosaic order are recorded The order of the mosaicked frames is important for deciphering the 3 extension of the FITS file To create a mosaic frame from already reduced OSIRIS cubes users can just call the module Mosaic Frames Here is an example using the MEANCLIP and TEL parameters lt xml version 1 0 encoding UTF 8 gt lt final mosaic of generic data gt lt DRF LogPath projects osiris DRP larkin test DRFs OutputDir projects osiris DRP larkin test ReductionType ARP_SPEC gt dataset Input
129. ve expressed interest in using it for faint targets There are several important caveats with using this scale First as the scales get coarser the geometric pupils formed by the lenslet array grow Since OSIRIS is a pupil spectrograph the final spectral resolution and cross contamination between spectra are directly dependent on the size of the pupils Diffraction helps to keep the 20 35 and 50 mas pupils close to the same size as each other and the spectral resolution of 3800 refers to these scales The 100 mas scale is coarse enough that even with perfect optics it would produce a 2x2 pixel blur on 10 3 15 2010 UCLA Infrared Laboratory I SEES CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 the detector With aberrations and diffraction this becomes 2 5 to 3 pixels and results in a reduced spectral resolution of less than 3400 and additional contamination from neighboring spectra The pupil is oversized and allows through a great deal of excess infrared background K 10 6 mag sq In order to alleviate this excess background at the coarsest scale we have installed duplicate K band filters with their own smaller 100mas pupils 9 m effective nim Camera Lenses Filter Locations NENNEN Collimators AO Focus Figure 2 4 Optical paths of the four sets of reimaging optics In reality the lenses are mounted in turrets in wheel mechanisms but here we show them s
130. was modified to includes a new wavelength solution using the operating temperature of the grating for each frame This version also includes a new spatial dependent wavelength solution derived by Tuan Do There were also fixes for how quality bytes were handled in this module Mosaic was modified for shifting the cubes using accurate NGS and LGS headers Correct Dispersion was updated to have the new instrumental dispersion for the new AO dichroic installed in August 2009 Scaled Sky Subtraction was modified to resolve numerous bug issues involving quality bit handling and good regions used for scaling sky Also removes residuals that were previously left behind in J and H band scaling Some portion of continuum subtraction for K band has been added as well However this new version of Scaled Sky Subtraction has been optimized for scaled subtraction with J and H bands Adjust Channels was modified for OSIRIS data taken during the warm detector period between January August 2009 The Julian date is read from the header of each frame to perform the appropriate channel adjustments Combine Frames was modified to include a new option of an average sigma clipping routine AVGCLIP Extract Star was modified to include new options of either an aperture radius of 7 pixels APER RADIUS7 10 pixels APER RADIUS10 or totally the entire cube into a 1d spectrum TOTAL Users should be aware that other look up files were modified
131. which include the full broad band the median spectral resolution in the 0 050 scale is 3900 and the average resolution is 3600 The difference comes from the fact that the long wavelength end of spectra tend to have fairly constant resolutions just above 4000 while the short wavelengths within each order fall to about 2800 Figure 2 6 shows the spectral resolution achieved at a wavelength of 2 190 microns Notice the bright region near lenslet 38 12 where the FWHM is typically less than 2 pixels leading to a spectral resolution above 4500 Towards the lower right the FWHM begins to increase and the spectral resolution bottoms out around 2800 The graph in Figure 2 7 shows the more complex variation of spectral resolution as a function of position and wavelength 16 3 15 2010 UCLA Infrared Laboratory 4 414 24 24 4 rdg CALIFORNIA ASSOCIATION FOR RESEARCH IN 5 OSIRIS USER Figure 2 6 This is the effective spectral resolution achieved as a function of lenslet position at a wavelength of 2 190 microns It includes the linear dispersion and the measured FWHM of an arcline at this wavelength Notice that spectral resolutions are highest near lenslet 38 12 and are lowest near lenslet 22 50 For numeric values use the graph shown in Figure 2 7 49 3 15 2010 UCLA Infrared Laboratory oSESK ar dide CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 5000 P
132. wn IRIS Filters SPEC Z Broad Nar e e Sa a Transmissior 1 For 266 filter order overlap limits the useful wavelength range to 0 999 to 1 176 microns The excluded wavelengths for this filter are shown in the shaded red regions For the Znarrow filters each is effective from their half power points given in Table 2 1 The atmosphere may also be a significant limitation in some wavelengths Please see Appendix C for atmospheric transmission 80 3 15 2010 UCLA Infrared Laboratory oS EEK pee CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 Es T Transmissior 1 For the Jbb filter order overlap limits the useful wavelength range to 1 18 to 1 416 microns The excluded wavelengths for this filter are shown in the shaded red regions For the Jnarrow filters each is effective from their half power points given in Table 2 1 The atmosphere may also be a significant limitation in some wavelengths Please see Appendix C for atmospheric transmission 81 3 15 2010 UCLA Infrared Laboratory oS EEK avidi CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER no IRIS Filters SPEC H Broad amp Nar Transmissior t 1 LI L l ggg
133. words Typical Value Description COMMENT UNDEFINED Comment for frame COADDS 1 Number of coadded frames ITIME 4199 Integration time between reads NUMREADS 8 Number of reads SAMPMODE 1 Sampling Mode 1 up the ramp 2 pseudo CDS subtract 2 read from last DATAFILE 1041228 2015002 File name for saved data image GAIN 0 3 Detector gain in electrons per ADU OBSTYPE astro Observation type astro star calib RDITIME 599 856995 Integration time between start of 93 3 15 2010 UCLA Infrared Laboratory ofS SES ar ay CALIFORNIA ASSOCIATION FOR RESEARCH IN AsTRoNowv OSIRIS USER MANUAL BADPIX INSTR LINCOEFF NOISEFIL PCIFILE SATURATE TIMFILE 3 15 2010 u osrseng ods test badpix imagbadpix fits imag u osrseng ods test lin imaglin fits u osrseng ods test readnoise imagreadnoise fits u osrseng kroot kss osiris sdsu dsp lod pci lod 20000 u osrseng kroot kss osiris sdsu ds p lod tim hl cold lod 94 V 2 3 successive reads Fits file name containing bad pixel map Spectrometer spec or Imager imag Fits file with linearization coefficients File name containing read noise frame File name containing PCI DSP code Saturation level of detector File name containing timing DSP code UCLA Infrared Laboratory OSIRIS USER MANUAL V 2 3 eiiis DS E F A orgy CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY Instrument Keywords ODS Keywords Typical Value Description DTMPLOCI CCR Head Location of
134. x 3 2 2036 2141 421 2868 45x64 0 90x1 28 1 58x2 24 2 25x3 2 2121 2229 433 3063 48x64 0 96x1 28 1 68x2 24 2 4 x 3 2 2208 2320 449 2671 42x64 0 84x1 28 1 47x2 24 2 1 x 3 2 2292 2408 465 2038 32x64 0 64x1 28 1 12x2 24 1 6 x 3 2 Limited by overlap from other orders The Kcb Kc3 Kc4 and Kc5 filter names are identical to these respective filters 14 3 15 2010 UCLA Infrared Laboratory SSES ar diae CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONOMY OSIRIS USER MANUAL V 2 3 Table 2 2 lists the original filter lists of the spectrograph before the March 2008 servicing which swamped out the Zn2 Zn3 and Zn5 filters for the new duplicate K band filters with smaller 100mas pupils The first four rows of Table 2 2 describe the broad band filters for the spectrograph The table lists the original OSIRIS filter specifications first two columns titled Design Specs the actual central wavelength CWL and bandwidth BW as measured in OSIRIS in the next two columns and the remaining columns to the right list the filter parameters for the actual filters as measured by the filter manufacturer Table 2 2 OSIRIS Spectrograph Filter Parameters Design Specs Measured in OSIRIS Test Data Supplied by Filter Manufacturer Avg Rise Fall Slope RMS wfe P Vwfe Power Filter Name CWL BW nm CWL nm BW nm CWL nm BW nm Slope Waves W
135. y the Extract Spectra module This is the module that performs an iterative separation of flux between the different lenslets In the on line mode the number of iterations is limited to 25 which may leave significant cross contamination of flux between lenslets But empirical tests have shown that 25 iterations are more than sufficient to produce an image of the field and examine the basics of the spectrum At the telescope the user does not generate data reduction files DRFs by hand or with the ODRFGUI although both are possible Instead the OORGUI is run as part of the normal set of GUIS at the telescope It senses when new FITS files are written and generates DRFs appropriate for an ODRP reduction The GUI allows you to make minor changes to the processing like specifying which file to use as the sky but most features are automated including the location of all of the calibration files 56 3 15 2010 UCLA Infrared Laboratory oS EEK arde CALIFORNIA ASSOCIATION FOR RESEARCH INAsTRONomMY OSIRIS USER MANUAL V 2 3 5 9 Module Descriptions Below we include descriptions of the most important modules You may notice other modules in the data reduction directories many of which are for engineering purposes only If something looks interesting to you please feel free to ask Most modules don t accept any arguments but instead simply perform a task on the dataset that is percolating through the pipeline In most cases fixed arguments like t
136. y L SpErtromteteranu mage Dataset Brown Dwarf Study Set 1 Object BD1 Reduction Type target w Coords 2 7 Move Units arcsec w 00 Send to Queue AO Type NGS LGS No Laser Filter 7 Scale 0 02 lenslet 7 Coadds 1 time 300 s per coadd r Spectrometer Settings 3 Object Frames Initial Offset X 00 925 Pattern Raster Scan Frames 0 3 X Stepsize 0 0 Y Stepsize 0 25 m imager Settings Filter Opn Repeats Coadds T time s per repeat Disabled Spec only r Sky Frames Nod Offset X 5 0 m Pattern Raster Scan ww Frames 2 x 1 X Stepsize 0 35 Y Stepsize 0 0 Show Position List UCLA Infrared Laboratory 3 15 2010 oS EEK pee CALIFORNIA ASSOCIATION FOR RESEARCH IN ASTRONOMY OSIRIS USER MANUAL V 2 3 In practice we ve found that the fixed position is optimal The dither pattern is determined within the Object Frames and Sky Frames fields For instance in the above example the observer has set up three exposures on the science target frames 1 2 3 with a raster scan and two additional sky frames The first sky frame frame 4 is offset from the science target by 5 west and 5 north and the second sky frame frame 5 is offset
137. y with Data Reduction XML Files DRFs 47 5 5 Reducing a Normal Observation uu a cec ern bn sede 49 5 5 2 Output Filename Construction ord e d ae De dvd 5 5 6 Reducing Multiple Darks or Skies into a Super 52 5 7 Mosaicking Multiple Science Exposures 53 DD Module Descriptions cud e een ace uci hue Mentes edd cue 57 5021 Adjust Channel Levels deti entered Mos Ire reete eder 57 20 2 Assemble Data ea utt adum usi qo Mois ARI rae ied in iux 57 5 9 3 Calibrate Wdyveletgthi obe te etae dei ront dte ai reciba Rs 58 SRL MEDICINES USATE TEE OTT LETT 58 0 9 5 Combine FTAES s nu ee 59 5 9 6 Cotrect DISpefSIOIE uode pa cete iie Asx Save sine dati AVEVO ESI TR ARR 59 5 9 7 Determine Mosaic Positions S ace c meet pue dist tu dosis 59 25 9 8 Divide Blackbody u ooh E Reni e PH ae eub Oed A D lea 60 5 9 9 Divide by Star Spectrum n OS 61 2 9 10 Extract SDOCIPI uu s rend eq ton etta 62 520 1 EX tel SIT mn a cat ete 62 5 9 12 Glitch Identification ced e eH e its tdt Rb ue ade 63 209 13 Mosale

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