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1. ramp sav bad flag data of ramps created by save button in check_ramp with option rampcorr 1 ramptbl ccf ramp curve correction table with option rampcorr 1 ramp ps Some postscript files produced during the process of making the ramp curve correction table with option rampcorr 1 Major contents of _part1l sav e VER STRING Version of fts_part1 e FILENAMEO STRING The name of the input TSD file e DATATYPE STRING FIS_SW FIS_LW e PKTIDF BYTE 124 for SED mode 14 for Full resolution mode e RSEXT INT Array 2 Removed reset point pre post e PCH INT plotch 1 e RADEC_A DOUBLE Array 2 ndet_all Equatorial coordinate of each channel calculated from AOCU RADEC_A 0 is RA RADEC_A 1 is DEC in degree See FIS IDUM for attitude determination e RADEC G Same as RADEC_A but calculated from G ADS e VIFBAD INT Array ndata ndrv ndet Flag of the interferogram e RANGE DOUBLE Array 2 Range of data for Fourier transform cm e DC DOUBLE Array ndrv ndet Non interferometric component which is an averaged interferogram over a scan e VIF DOUBLE Array ndata ndrv ndet Interferogram of each scan and channel e VIFPOS ODUBLE Array ndata ndrv Optical path difference in each scan for PCH cm e WN FLOAT Array nwn Wavenumber em 22 AKARI FTS Toolkit Manual e SPEC DOUBLE Array nwn 2 average stdv
2. data and acal means the cal A lamp data dark1 dark2 and dark3 refer to the dark data before the observation between the observation of the internal calibration lamp and the celestial object and after the observation respectively acal_b and acal_a are the cal A lamp data before and after the observation respectively If only selected subsets are required options can be set to omit the unneeded subsets e g setting the nomcal option will omit the mcal data subset Either of input_base obj fits gz or input_base mcal fits gz becomes the input for the fts_partl procedure Version 1 May 13 2008 3 2 fts parti The fts part1 process carries out the Fourier transformation of the time series data TSD to obtain spectral information The processing steps are given below During the processing there will be several GUIs for checking of data flagging and corrections Additional optional parameters used at the startup of fts partl are summarized in section 2 2 Raw data 1 ADU to voltage conversion GB pipeline tool 2 Ramp curve correction GB pipeline tool with correction table opti mized for FTS observations Correct for non linearity of the ramp curve GUI check_ramp_curve_corr e Quality check of the ramp curve correction 3 Differentiation GB pipeline tool Interferogram DC component 4 Separate into individual scans 5 Remove reset anomaly GUI check_res
3. plotch 28 or 29 and plotch 4 or 5 for SW and LW observations respectively with AOT parameters of FIS03 1 plotch 54 or 55 and plotch 23 for SW and LW observations respectively with AOT param eters of FISO3 2 and plotch 32 or 33 or 53 and plotch 7 for SW and LW observations respectively with AOT parameters of FIS03 0 2 2 2 rampcorr The ramp curve correction table is selected by rampcorr option By default the correction table in the toolkit for FTS observations which is recom mended for most data is used This option accepts either an integer 1 2 3 or a string of a ccf filename 1 Make a correction table using the data itself This is required for very bright objects 2 Apply correction table for survey mode data Not recommended test purpose 3 No correction Not recommended test purpose ccf file name string select specific ramp curve correction table See below Processing with rampcorr 1 generates a ramp curve correction table file named ramptbl ccf Once a correction table is made for one ob servation the user can use it every time by specifying the file as ramp corr ramptbl ccf instead of making the correction table again If rampcorr 1 is selected the check ramp monitor window appears Figure 10 All ramp curves far from the centerburst used to make a correction table are plotted in the top left window Unsuitable ramp curve data should be flagg
4. is used to refer to a previously saved ramp flag file and should be used with the rampcorr 1 option set ES rampbfig ramp sav 2 2 4 addname This option adds optional characters to output files The default name of the final IDL save file is filename _partl sav The new characters are inserted in between the filename and _partl sav addname 2 2 5 vifbadf If the users have previously saved flagging file of glitches the users import it for the rm_glitch processing by setting this option vifbadf vifbad sav 18 AKARI FTS Toolkit Manual E chec ramp Neptune_p4_SW_obj fits gz yoy plot ramp curve range gt 3 E 3 E detec mask ramp curve sample number range 40 60 30 minimum sample number channel mask sample number save flag y one channel reset ok 2 all channel Figure 10 Window for the check ramp process The data selected with the sample number range sliders turn green plot ramp curve range maximum mask ramp curve sample number range minimum sample number _0 EE Ll maximum channel mask sample number 2 all channel save flag wv one channel reset ok Figure 11 The ramp curve selected with the ramp curve range sliders turn red Version 1 May 13 2008 19 y eval ramp_cor
5. number 1841 shown by the blue point is selected using the selected data range slider sample number 6 ok range channel J plot scan range selected data range 5 5 1841 1841 mask data save quit CE mm J mimi minimum maximum minimum maximum Figure 5 After selecting the glitch data as in the previous figure click mask data After replot by clicking any of the sliders the removed data point turns pink 10 AKARI FTS Toolkit Manual integration is a minimum The determined ZPD is shown as a white forward scan case or yellow backward scan case line in the lower right panel and the red point in the lower left panel Using the zero path position slider you can select the data point and check the interferogram blue line in the lower right panel the integration of the squared imaginary part blue point in the lower left panel and the spectra itself under the assumption that this point is ZPD upper left panel red represents the real part and blue represents the imaginary part You can select the scan number using the scan slider The upper right panel shows the derived ZPD for each scan At this stage it is necessary to check whether the ZPDs in all the scans have been estimated correctly Though the definition of the ZPD is the opd where the integration of the squared imaginary part is a minimum local minima next to the real ZPD may have sma
6. 3 real imaginary phase 2 forward backward ndet Averaged spectrum e SPECBARA DOUBLE Array ndrv nwn 3 real imaginary phase 2 forward backward ndet Spectrum of each scan ndet Number of channels for WIDE band SW LW 60 45 ndet_all Number of channels for WIDE and NARROW band SW LW 100 75 ndrv Number of scans ndata Number of data per scan For SED mode observations the first half of the data corresponds to the forward scan and the last half to the backward scan For Full resolution mode the first half of the data corresponds to the backward scan and last half corresponds to the forward scan nwn Number of wavenumber elements in the spectrum Version 1 May 13 2008 23 3 FTS tools Two tools are provided to support the FTS data reduction Typing without argument will display the usage Suppose the file name of the final output of fts_part1 as input_base partl sav in the following 3 1 fts_checkrawspec The check_raw_spec window Figure 9 is opened by this command plotch specifies the channel to plot though this can be changed using the GUI FISDR gt fts_checkrawspec filename input_base part1 sav plotch 3 2 fts_partl_output This procedure makes postscript or ascii files from input_base partl sav FISDR gt fts_partl_output input_base partl sav mcal addname string psfile fizmin value fixmazx value wnmin value wnmazx va
7. 6 22d TNP ir a A eaa os tee G 16 22 9 TAMpLDiE onio riin uoa a 17 224 addname lena ro ay aTa a 17 Delo A tenes a ss Re gee R ee a t Ih vaai 17 DO MC aa 4 ck AA ip dc o Rt N 20 BLA PISA it a a Ae te ee 20 2 2 8 siemaclip 22a a ea eek ram a ee Be ES 20 2 29 o PD Ant oto Ske dake A s Sh aod Peo 20 2 3 Contents of the save file 0 20 3 FTS tools 23 3 1 fts_Checkrawspec e o 23 3 2 ftspartl_output ss ssaa dre 0 00 00 022 ee 23 Version 1 May 13 2008 1 About this Document This document explains how to analyze AKARI Fourier Transform Spec trometer FTS data The analysis procedure consists of two main steps The first processing step fts_ partl carries out the Fourier transformation of the interferogram obtained from the time series data TSD to provide the spectral information The second processing step carries out the flux and wavelength calibrations on each channel Since the latter calibration part is still under development only the former part fts_partl is described in this document Calibration part will be released in a later version All procedures are based on the IDL programming language In this document it is assumed that the FIS IDL procedures and IDL itself are already installed and running in your environment More information on the basics of the AKARI data flow FIS analysis tools and strategy for data processing using the FTS can be found in the FIS Instr
8. Version 1 May 13 2008 AKARI FTS Toolkit Manual Version 1 Hidenori Takahashi Yoko Okada Akiko Yasuda Hiroshi Matsuo Mitsunobu Kawada Noriko Murakami and Chris Pearson Gunma Astronomical Observatory Institute of Space and Astronautical Science ISAS JAXA 3National Astronomical Observatory of Japan 4Nagoya University 5Bisei Astronomical Observatory SCCLRC Rutherford Appleton Laboratory University of Lethbridge May 13 2008 Version 1 May 13 2008 Date Revision Comments 5 December 2007 Version 0 9 First Draft Hidenori Takahashi 6 December 2007 Version 0 91 pdated Format Chris Pearson 29 December 2007 Version 0 92 pdated Yoko Okada 7 January 2008 Version 0 93 pdated Chris Pearson 14 January 2008 Version 0 94 pdated Yoko Okada 23 April 2008 Version 0 95 a a SISI pdated Yoko Okada 12 May 2008 Version 1 a Jpdated Yoko Okada ii AKARI FTS Toolkit Manual Contents 1 Data Preparation 2 2 fts_partl 3 2 1 Details of GUI processes o oo 0000004 5 2 1 1 check ramp_curve_corr 200 5 2 1 2 check_reset_bad o o 0008 6 213 THi e lithe ica oka be ee en 7 2 1 4 check drvccb diso as areni ae E ee e 0000000 7 2 15 ehekal CBr its ar eo e ai 10 2 1 66 check raw spec ooa a 13 2 2 options for fis part 2 m sa aiia a ee ee 13 AA plote ei iea e ai Re aw ee ed A 1
9. e range channel and plot scan range sliders can be used to look at all data Click ok when finished 2 1 3 rm glitch The rm_glitch window is shown in Figure 4 Here you should flag all individual data affected by glitches by eyes If sigmaclip option is set c clipping glitch removal has been made before this GUI process and flagged data points are shown as pink points If the clipped data points are not valid break this process and run fts_partl without sigmaclip option Use range channel and plot scan range sliders to check all the data Any elitch near the centerburst will affect largely on the resultant spectra and should be removed For flagging select the data to be masked with the selected data range slider and click mask data Figure 5 Click save to create the flag file Click ok to save flags and move to the next step Flagging glitches for all the channels often takes long time The user can break this procedure with the quit button after clicking save and restart fts partl with the vifbadf option see Section 2 2 2 1 4 check_drv_cb The next step is check _drv_cb Figure 6 In this process the zero path difference ZPD position is identified i e the position of the centerburst from the interferograms of a specific channel set by plotch option This processing step is important to obtain proper spectra The lower right panel of Figure 6 shows the interfer
10. e_corr process The white and blue lines in the upper panel represent the interferograms before and after correction respectively 2 1 2 check_reset_bad This step removes reset anomalies During this step the check_reset_bad window can be viewed as shown in Figure 2 Using this GUI user should examine the data to ensure that the reset periods are properly flagged out Flagged data itself have the value 999 and reach far below the window If the flag is not properly set there will be periodic glitches before or after the reset as shown in Figure 2 Normally the reset anomalies can be flagged using the default parameters If periodic glitches as exemplified in Figure 2 are found check the ramp curve correction Version 1 May 13 2008 first since an improper ramp curve correction can produce such periodic glitches Note that at this stage of the processing the user does not have to care about glitches between the resets i e aperiodic random glitches since these will be dealt with in the next step of the processing Two parameters may be changed to mask any anomalous data related to resets The first is used to select the pre reset data points and the other refers to the post reset data points After tuning the before reset and after reset sliders of the reset anomaly range click do again to set the new parameters e g as shown in Figure 3 The reset parameters are common to all channels and scans Th
11. ed in this step A channel is selected using the channel slider There are two additional sets of sliders ramp curve range and sample number range The former is used to remove a ramp curve and the latter is used to remove data of the same sample number from all ramps Version 1 May 13 2008 17 When you select the all channel button the same data points are simul taneously removed in all channels whereas using the one channel button only the data in the selected channel is removed The first point of the ramp curve i e data with the sample number being 0 should be removed because these data should not be included as the beginning of the ramp curve Se lect the first point with the sample number range slider Figure 10 and click mask sample number The actual removal of a ramp curve follows the same methodology of the removal of bad sample data except ramp curve range is used instead of the sample number range sliders Figure 11 It is not necessary to remove bad ramp curves very finely since most of them will be removed automatically in the following processing Click save flag to save the above processing At any time one may return to the last saved position by clicking the reset button Click save flag and ok to move to the next procedure the derivation of the averaged ramp curve Figure 12 and the production of the ramp curve correction table 2 2 3 rampbflg This option
12. ermine zero path position 0 01000000 0 01000000 J J E minimum maximum L J Figure 8 Window for the check_all_cb processing step This window is similar to that of check_drv_cb except the upper right panel represents every channel rather than every scan Note that there is a trend to incline on each row in the case that a large extended object is detected over several channels Version 1 May 13 2008 15 spectrum of each scan averaged spectrum 100 l 100 wavenumber om 1 wavenumber om 1 Interferogram around center burst Interferogram scan number E 2 5 5 wv oplot both wv both plot wreal forward w imaginary w backward Figure 9 Window of check_raw_spec Upper left panel shows averaged spectrum over scans pink real part light blue imaginary part Upper right panel represents the spectrum of the selected scan 16 AKARI FTS Toolkit Manual 2 2 1 plotch The plotch option is used to select a specific channel for the adjustment of the ZPD of every scan used in check_drv_cb A channel which de tects sufficient photons with high S N is recommended For large extended sources the default channels channel 23 for SW and channel 7 for LW are recommended so it is not necessary to set this option For point or small extended sources a channel in which the sources are detected should be set
13. et_bad e Removal of any data affected by resets 6 Remove glitches GUL rm_glitch e Masking glitches by eye if necessary 7 Subtract DC component 10 11 12 AKARI FTS Toolkit Manual Interpolation of bad data Replace any bad data by the median of other scans Since the first scan in SED mode is affected by an irregular drive pattern at the starting point we ignore the first scan when calculating the median in the SED mode Determine the zero path difference ZPD in a specific channel Since the value of the position sensor is correct only relatively the ZPD must be determined The present toolkit determines the ZPD that minimizes the squared imaginary part integrated over the effective wavenumber GUI check_drv_cb e Check the estimated ZPD for the every scan in a specific channel and tune parameters to reject incorrect estimates Determine the ZPD in all channels It is assumed that the relative deviation of the ZPD between different scans is the same for all channels And the ZPD of all the channels are estimated in this step GUI check_all_cb e Check the estimated ZPD for all channels and tune parameters to reject incorrect estimates Discrete Fourier Transform Apply Discrete Fourier Transform using the output of the position sen sor and the determined ZPD in the previous steps to the interferogram of each and every scan Average the spectra After applying Fourier transforms the average spectr
14. ller values in the case of data with low S N or data affected by strong transient effects There are two check points that can prove useful The first is whether the interferogram is a positive peak or a negative peak at the ZPD see white or yellow lines in the lower right panel of Figure 6 For celestial data taken in the SW band and internal calibration data with LW the interferogram should ex hibit a negative peak at the ZPD For celestial data taken in the LW band and internal calibration data with SW the interferogram should exhibit a positive peak at the ZPD The second check point regards the upper right panel Since the ZPD does not change significantly between scans the upper right panel should appear almost constant except for the first scan If you discover any large discrepancy over 0 002 cm between scans as exemplified in Figure 6 the determined ZPDs in some scans are probably not correct If the determined ZPDs are acceptable click ok to finish this procedure If not tune the ZPD using four sliders at the bottom of the window which cover the range of the opd used to determine the ZPD For example in Figure 6 improper positions of opd gt 0 002 cm are selected as the ZPD in several backward scans see upper right panel Moving the lower right slider maximum for backward scan to 0 002 and clicking do_again produces the window shown in Figure 7 after a short wait Note that the newly determined ZPDs seem to be co
15. lue txtfile trtch integer vector If the user wants to obtain a postscript file to show the raw spectra of all the channels set psfile option Then input_base part1 ps file is created The minimum or maximum values of x and y axis can be specified for all the channels by the options wnmin wnmaz firmin and fizmazx respectively If the user wants to obtain an ascii file of the raw spectra set tztfile option then input_base part1 txt file is created By default the data of all the channels are included Data of specific channels can be extracted by tatch option e g tatch 33 34 35 mcal option should be given when the user processes the data of the internal calibration lamp The addname option can be used to add a word between partl and ps or txt of output files
16. mp_curve_corr The standard FIS pipeline tool Green Box is used to correct for any non linearity of the ramp curves see FIS Instrument Data Users Manual Section 4 1 2 The correction table optimized for FTS observations has been pre pared in the toolkit and used for nominal FTS observations For very bright targets whose brightness exceeds the range of the correction table a correc tion table should be made from the data itself setting rampcorr 1 In this case see Section 2 2 2 for detailed explanations of this option This process opens a window check_ramp_curve_corr as shown in Fig ure 1 which has three panels the lower left panel shows the raw integrated time series data the lower right panel shows the relation of the ramp curve correction white measured red corrected and the upper panel displays the derivative of the raw data and ramp curve corrected data of the selected channel One should check on the upper panel whether the corrected inter ferogram blue is flat except for the centerburst compared to the original 6 AKARI FTS Toolkit Manual data white In general the correction is smaller for the LW band than the SW band The display range can be changed by using the range button When it is acceptable click ok to progress to the next step Tf something is unsatisfactory or wrong you may have to quit and start again using a different option Figure 1 Window for the check ramp curv
17. nary part of the full resolution mode data does not represent this residual correctly since the Fourier transform is applied only for one side of the centerburst This step is primarily for confirmation Figure 9 The upper left and upper right panels show the averaged spectrum and the spectrum of selected scans respectively The plot can be adjusted by using several available buttons Use the quit button to finish fts_partl processing 2 2 options for fts_partl In this section we explain the optional commands which are available to the user in the fts_partl processing step of the toolkit option explanation plotch integer channel for the adjustment of the ZPD of each scan rampcorr 1 2 3 or string select ramp curve correction table rampbflg string use previously saved ramp flag file addname string add optional characters to output files vifbadf string use previously saved glitch flag file mcal required to process internal calibration source data pixflg integer vector flag all data on specific channels sigmaclip flag bad data by o clipping before rm glitch GUI setcbp establish ZPD from driving pattern automatically 14 AKARI FTS Toolkit Manual raw spectrum selected zero path position t Spectrum channel Interferogram apt Po zero path position x voplot both v both 2 plot v real w imaginary w backward Range of relative optical difference to det
18. ogram The x axis is the relative optical path difference hereafter opd Initially the tool applies the Fourier transform assuming that each data point is the ZPD estimates the integration of the squared imaginary part over the wavenumber lower left panel of Figure 6 and determines the ZPD as the position where this 8 AKARI FTS Toolkit Manual plot scan range reset anomaly range 0 J mimi before reset 20 ETT channel 1 jaiz after reset do_again range Figure 2 Window for the check reset bad processing step Note that the data just before reset overshoots above the mean level of the interferogram The value of flagged data is 999 and apparent overshoots the bottom of the window represent 999 9 1 minimum IE gt plot scan range reset anomaly range 9 2 J El before reset ET minimum 20 mimi channel 1 jaz after reset do_again range Figure 3 The overshot data seen in the previous figure are removed using ZE gt the reset anomaly range Version 1 May 13 2008 9 sample number plot scan range selected data range MER 5 MES mim minimum maximum 1841 J ET minimum maximum gt Figure 4 Window for the rm_glitch processing step The glitch at the position corresponding to sample
19. r 40 sample number range replot xscale_on ave_plot_on w xscale_off w ave_plot_off channel Figure 12 Window to check the averaged ramp curve White lines are all the ramps with scaling and the blue line is the assumed average Click ok to continue 20 AKARI FTS Toolkit Manual 2 2 6 meal This option should be used when processing the data of the internal cal ibration light source The temperature of the internal calibration source becomes stable only after several scans thus the data of first 3 scans and last scan is discarded with this option mcal 2 2 7 pixflg This option is used to flag all data on specific channels e g saturated channels in addition to LW 2 3 18 33 42 and SW 1 11 which are already known to be bad channel pixflg 6 7 31 2 2 8 sigmaclip Flag bad data by o clipping before glitch check GUI sigmaclip 2 2 9 setcbp The ZPD is automatically established from the driving pattern with this option This option should be used only for faint sources which do not have a clear centerburst and for which the ZPD can not be determined from the data itself setcbp 2 3 Contents of the save file During the fts_partl processing several save files are created Note that the creation of some files depend on the options employed Version 1 May 13 2008 21 partl sav final output of fts_part1 vifbad sav bad flag data of glitches created in rm_glitch
20. rrect for all the scans This process should be repeated until the ZPDs for all the scans are acceptable 2 1 5 check_all_cb The next step is check all cb Figure 8 and is used to check whether the ZPD is reliable for all the channels The window is similar to the check drv_cb window except for the upper right panel in which the ZPD Version 1 May 13 2008 11 raw spectrum of channel 7 selected zero path position zero path position voplot both v both plot yreal v forward w imaginary backward Range of relative optical difference to determine zero path position forward scan r 0 0200000 0 0200000 Ela J ied minimum maximum Range of relative optical difference to determine zero path position backward scan 0 0200000 0 0200000 EE J ZE minumum maximum L J Figure 6 Window of check_drive_cb in the case of LW channel 7 of a celestial object The red point in the lower left panel shows the selected opd where the integration of the square of the imaginary part is a minimum However this is in the negative peak of interferogram as shown in the lower right panel whereas the interferogram of celestial objects observed in the LW band should be the positive peak at ZPD It can also be found that the relative optical path difference of this scan 3 is not in agreement with that of the majority of other scans in the upper righ
21. t panel 12 AKARI FTS Toolkit Manual clear ok do_again zero path position ar oplot 2 both plot real y imaginary Range of relative optical raw spectrum of channel 7 selected zero path position Integration of squared imaginary part v both v forward difference to determine zero path position forward scan 0 0200000 i 0 0200000 ET minimum I By maximum Range of relative optical difference to determine zero path position backward scan 0 0200000 minumum 0 00229000 IS maximum J L Figure 7 After tuning the slider the ZPDs in all the scans are determined correctly Version 1 May 13 2008 13 for every scan is replaced by that of the channels Figure 8 The procedure of this tool is similar to that of check_drv_cb Since there is no need to select forward or backward scans only two sliders are available instead of four Note that the ZPD of bad channels any channels in which objects are not detected is not trustworthy and may be ignored 2 1 6 check raw_spec After applying Fourier transforms to the interferogram of each and every scan the average spectrum is taken As final products spectra of complex type are obtained The real part corresponds to spectra with physical mean ing and the imaginary part is residual of the phase correction Note that the imagi
22. um is taken GUI check_raw_spec e Check the Fourier transformed spectra for all channels Raw spectra final output of the fts_partl Version 1 May 13 2008 5 To start the process from IDL command line input the following com mand FISDR gt fts_partl input_base obj fits gz plotch integer rampcorr 1 2 3 or string mcal sigmaclip Just type fts_part1 to display the usage Refer to Section 2 2 for a detailed description of the available options The rampcorr option see 2 2 2 is used to select the appropriate ramp curve correction table It is not necessary to specify rampcorr except for very bright objects and in most cases the default correction table is used The plotch option see 2 2 1 is used to select a specific channel used for the adjustment of the ZPD For observations of point or small extended sources it is necessary to set the channel in which the source is detected as plotch For large extended sources it is not necessary to specify plotch and the default channels channel 23 for SW and 7 for LW will be used The mcal option see 2 2 6 should be used when the user process the data of the internal calibration lamp The sigmaclip option see 2 2 8 is for automatic glitch removal We recommend to use this option otherwise the user will have to remove all glitches manually by eye The following sub section describes the details of GUI processes 2 1 Details of GUI processes 2 1 1 check _ra
23. ument Data User Manual IDUM The definition of the FIS channel numbering follow Figures 2 1 6 or 3 2 9 in the FIS IDUM In the following sections processing with many iterative steps will be described 1 Data preparation 2 fts_partl 3 FTS tools Definition of words GB Green Box The standard FIS pipeline tool OPD optical path difference TSD time series data The format of the raw data ZPD zero path difference The position where the optical path difference is zero centerburst Same as ZPD though also used for the whole structure in interferogram around ZPD 2 AKARI FTS Toolkit Manual 1 Data Preparation 3 Suppose the file name of the raw observations data set TSD as input_base fits gz Before running the fts_partl processing step it is required to separate the target observation data from the calibration data etc in the raw data set The task is performed by the following simple IDL command FISDR gt fts mk obj_mcal acal input_base fits gz nooby nomcal noacal nodark Just type fts_mk_obj_mcal_acal to display the usage fts_mk_obj_mcal_acal makes several subsets from the TSD fits file of one pointed observation Output files have extra characters between input_base and fits gz which represent the contents of the subset obj means the celestial object data meal means the internal calibration light source data dark means dark

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