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INTEGRAL Science Data Centre IBIS Analysis User Manual

1. 12 2 ibis gti This script builds Good Time Interval GTI information from housekeeping data information about the satellite stability and data gaps It calls the following executables to obtain the GTIs e gti create e gti attitude e gli data gaps e gti import e gli merge For the definition of GTI see Introduction to the INTEGRAL Data Analysis 1 12 2 1 gti create This program generates all GTIs for one instrument that depend on HK and other parameters and are defined by a limit in a limit table see details in Section B 3 In ISGRI case it creates VETO GTIs during which VETO was switched on and ISGRI MCE7X where X varies from 0 to 7 GTIs during which the Xth module was switched on VETO GTIs are taken into account by gti merge executable see Section 12 2 5 and ISGRI_MCE7X GTIs are taken into account later during BINI BIN S and BIN T levels Table 7 gti create parameters included into the main script Name in the main script Name Type Description executable SCWI1 GTI Limit Table LimitTable string The DOL of the GTI limit table default 12 2 2 gti attitude A GTI is defined for each period of time where the pointing stability is better than the accepted tolerance parameter AttStability This GTI is named ATTITUDE For slews this GTI is always set to be good independently of any input data If the necessary data are not available the GTI is set
2. ISDC IBIS Analysis User Manual Issue 10 1 106 SCW2_ISPE_idx isgrResp SCW2 ISPE isgrarf SCW2 ISPE DataMode SCW2_ISPE_MethodInt SCW2_ISPE_MethodFit SCW2_ISPE_isgrUnifDol SCW2_BIN_cleanTrk SCW2_BIN_LidxNoisy SCW2_BIN_LidxLowThre SCW2_BIN_P_inDead SCW2 BIN P inGTI SCW2_BIN_P_PicsCxt SCW2_BIN_P_HepiLut SCW2 BKG LisgrBkgDol SCW2 BKG divide SCW2 BKG badpix SCW2 BKG flatmodule string string integer integer integer string integer string string string string string string string boolean boolean boolean DOL of the index of ISGRI response matrices default DOL of the ARFs for XSPEC default Data Simulation mode default 0 Method to be applied for the pixel value interpolation default 1 Method to be applied for background and source in tensity fitting default 6 DOL of the ISGRI detector uniformity default Cleaning of cosmic ray induced events possible values 0 No 1 Yes default 0 DOL of the index of noisy maps default index of Low Threshold default DOL of the dead time data structure default DOL of the good time interval data structure default DOL of the PICsIT Context Tables default DOL of the hepi lut default DOL of the isgri bckg model or if you want none or empty if you want DOL automatic from the
3. 64 ii shadow build parameters included into the main script o 65 ip ev shadow build parameters included into the main script ls 65 ip_si_shadow_build parameters included into the main script 66 ii map rebin parameters included into the main script o a 67 ii shadow_ubc parameters included into the main script e 68 ip shadow ubc parameters included into the main script 68 cat extract parameters included into the main script 0002 08 2 eee 69 ii skyimage parameters included into the main script o e 72 sumhist parameters included into the main script 22e 74 ghost_busters parameters included into the main script o 74 ip skyimage parameters included into the main script o e a e 75 ii spectra extract parameters included into the main script o o 75 ip_spectra_extract parameters included into the main script 76 Parameters for the Wc etratt ec iosa ee cy vo Ro ORO gx REESE EEEG TT ip skymosaic parameters included into the main script len 78 NOS BICI PES PATINETES a Oee n A e ee a DRE a eG 78 LIGA PALCO e cee i n A A a e Rn 80 List of IBIS RAW Data Structures lt o seco RR RR s 82 Contest of Photon by Photon Mode Raw Data less 82 Content of PICS SPTI RAW Data S
4. p_shadow_ubc ogibis y a a Figure 28 Overview of the binning background step for Imaging Binning backgroud step for SPE ibis binning i og ibis ii shadow build ss lh 3 pixel status jp dd i evsi aP ip shadow build ev si EFFLIC file 7 bi binid e De BKG IC file ii map rebin rebinned maps ibis background cor dis ii shadow ubc s i og ibis ip shadow ubc og ibis 2 e Figure 29 Overview of the binning background step for Spectra Binning backgroud step for Timing ibis binning E og ibis ii shadow build og Mis E pixel status ip shadow build ev si EFFLIC file BKG IC file gt jimap_rebin gt rebinned maps ibis background cor ii shadow ubc 2 7 7 og ibis ip shadow ubc ogibis i Figure 30 Overview of the binning background step for Lightcurves ISDC IBIS Analysis User Manual Issue 10 1 59 12 1 2 ibis isgr energy Due the charge loss in the CdTe crystal for a given energy deposit events which have interacted at different depths in the crystal get different measured amplitudes PHA The rise time of the signal induced by these events is also different and a clear quasi linear correlation between the charge loss and the rise time variation is observed a deeper interaction induces a larger charge loss giving the longer rise time It is then possible to correct this charge loss effect by taking into acc
5. Generates selects and merges Good Time Intervals GTI to produce a unique GTI that is then used by the software to select good events See Section 12 2 for more details DEAD Dead Time Calculation Calculates the total dead time during which the incoming photons may be lost due to the processing of the previous events Also veto strobe signals generated by BGO Bismuth Germanate shield calibration source and Compton events are taken into account See Section 12 3 for more details BIN_I Event Binning for Imaging Sorts data into energy bins For each energy range the intensity shadowgram and a corresponding efficiency map are created See Section 12 4 for more details BKG I Background Correction Creates rebinned maps for background and absorption of support mask see Section 3 2 1 corrections Corrects for efficiency and subtracts background See Section 12 6 for more details After these steps the high level analysis is performed e The second script ibis obs analysis takes the whole Observation Group previously created as input and performs the following tasks CAT I Catalog Source Selection for Imaging ISDC IBIS Analysis User Manual Issue 10 1 14 Selects from the given catalog a list of sources in the Field of View matching the criteria defined by script parameters and creates an output list with location and expected flux values of the selected sources See Section 12 7 for more details
6. IMA ISGRI and PICsIT staring Image Reconstruction In the case of ISGRI shadowgrams are deconvolved source search is performed in the single images as well as in the mosaic combination of different images and a list of detected sources is created If INTEGRAL was stable during the whole period of interest then at your request all PICsIT shad owgrams are combined into one and then are deconvolved into a single image See Section 12 8 for more details e The third script ibis_scw2_analysis again works Science Window by Science Window and performs the following tasks IMA2 PICsIT Image Reconstruction PICsIT shadowgram deconvolution is done at this step creating a separate image for each science window See Section 12 8 4 for more details Nothing is done at this step for ISGRI BIN S Event Binning for Spectra Creates rebinned maps for background and absorption of support mask see Section 3 2 1 corrections Sorts data into energy bins For each energy range the shadowgram and a corresponding efficiency shadowgram is created See Sections 12 4 12 6 for more details SPE ISGRI spectra extraction For each source of interest one PIF is produced ISGRI spectral extraction is done for all catalog sources with the use of these PIFs See Section 12 9 for more details LCR PICsIT Detector Light Curve Creation and ISGRI source lightcurve extraction At this step PICsIT Detector light curves are built from
7. DOL of the index of input images default DOL of the index of output images default Enter source x coordinate in pixels possible values O 10000 default 0 Enter source y coordinate in pixels possible values 0 10000 default 0 Enter source RA possible values 180 360 default 0 Enter source DEC possible values 90 90 default 0 Position fitting mode posible values 1 freeze position as input 0 position is always left free 1 freeze position as found in first energy band default 0 Gaussian width fitting mode posible values 1 radial width frozen as input 0 radial width left free 1 x and y width left free 2 x and y width fixed as found for first band default 0 HWHM of PSF in arcmin possible values 0 1 20 default 6 Enter source box half size in pixels on which the fit is performed possible values 1 1000 default 20 Should a constant intensity background be considered in the fit default no Enter if the program has to select automatically energies default yes Enter vector of energy bands minimum default 25 30 40 Enter vector of energy bands maximum default 30 40 60 ISDC IBIS Analysis User Manual Issue 10 1 79 chatty integer Enter reporting level 10 includes MINUIT log possible values O 10 default 4 12 12 2 21 light For every PIF found in the Science Window ii light extracts simultaneously a li
8. Note that the numbering starts with 0 but often this extension does not contain real data If no extension is specified explicitly the first one 1 will thus be used by default You will find many more useful information in the ISDC list of Frequently Asked Questions FAQ at http www isdc unige ch integral support faq ISDC IBIS Analysis User Manual Issue 10 1 20 7 A Walk through ISGRI Analysis After setting up the OSA environment as described in the previous section you are ready to analyse the data Please do remember that you are dealing with a coded mask instrument not with a focusing telescope and a CCD It is not possible to deal with one source at a time each source is background for the others the whole field of view and not just the few pixels around your source matters In this Section we guide you through your first IBIS analysis but please read also Section 8 where more details on the main parameters are given You could end up with fake sources that are created by a blind use of parameters More tips and tricks are given in Section 9 for advanced users In the example below we analyze observations of the Galactic Center using data we have downloaded and installed as it is described in Section 6 1 Create the Observation Group with the og_create program see its description in the Toolbox section of 1 cd REP_BASE_PROD og_create idxSwg isgri gc lst ogid isgri gc baseDir instrumen
9. GTI ibis_gti L Good Time Intervals Dead Time Calculation DEAD ibis dead Dead Time Event Binning tor Image BIN I ibis binning Binned Events Background Correction BKG e undies R 9 Rebinned Bckg and Efiiciency Shadowgrams HA Shadowgrams Corrected for Background L ibis background cor cat extract Catalog Source Selection cat merge List of Sources in FOV 1 ii skyimage SGRI ard PICS Maria sumhist L SGRI and PICsIT staring Image Reconstruction ip skyimage Images ibis scw2 analysis pccezcasscccessco tces alcc lencl2escc 22ece2z 4 i PICsIT Image Reconstruction IMA2 ip_skyimage PICsIT Images mii map rebin i Event Binning for Spectra ibis binning L Events Binned BIN S i for spectra extraction 1 i Spectra Extraction SPE ii spectra extract c SGRI spectra I ie esee a Te ip st jc extract Lighteurve of PICsIT i LCR i Spectral Timing Data i eee ii lc_exctract t ISGRI source lighteurves i Summing of the results CLEAN ip_skymosaic t PICsIT mosaic Figure 10 Science Analysis Overview e The first script ibis scw1 analysis performs the following tasks COR Data Correction Tags noisy pixels corrects energy of the photons for rise time and temporal variations of the gain transforms channels to energy See Section 12 1 for more details GTI Good Time Handling
10. JA eno IBIS Analysis User Manual ISDC Lag SS 3 September 2014 10 1 ISDC OSA UM IBIS INTEGRAL Science Data Centre IBIS ANALYSIS USER MANUAL Reference ISDC OSA UM IBIS Issue 10 1 Date i 3 September 2014 INTEGRAL Science Data Centre Chemin d cogia 16 CH 1290 Versoix Switzerland http isdc unige ch Authors and Approvals HE lt ISDC IBIS Analysis User Manual ISD pe ee 3 September 2014 10 1 Prepared by M Chernyakova A Neronov L Pavan amp M Tiirler Agreed by Rd Approved by TGOUEPVolslet 125i sre A Eu Sec RE NUN eee et eno E els ve abd edes ISDC IBIS Analysis User Manual Issue 10 1 i Document Status Sheet lt ISDC IBIS Analysis User Manual S 2 April 2003 1 0 First Release 19 May 2003 1 1 Update of the First Release Section 6 Tables 63 10 12 13 16 52 58 and Figures 10 27 were updated Section 12 9 1 was added 18 July 2003 2 0 Second Release Sections 5 6 8 and the bibliography were updated Sections 12 9 12 12 2 C 8 C 9 2 were added 5 December 2003 3 0 Third Release Sections 6 7 and 8 were updated Sections 9 11 C 9 3 were added 19 July 2004 4 0 Fourth Release Sections 6 7 8 and the bibliography were updated 6 December 2004 4 2 Update of the Fourth Release Sections 6 8 Tables 16 17 and the bibliography were updated 29 June 2005 5 0 Fifth Release Cookbook Part was completely rewritten All oth
11. L 14 4 po o t 8 9L 8 L1 Ly H t yf Dr EN Hu h J FFT p t rit Tt tt i T pR Li fy t 4t 4 7 HH pu e A or 1 4 2000 4000 6000 8000 104 Time s Start Time 12713 23 30 22 185 Stop Time 12714 2 03 42 185 Figure 21 Lightcurve of 4U 1700 377 in the 20 40 keV energy range with 100 sec binning ISDC IBIS Analysis User Manual Issue 10 1 32 8 More on ISGRI relevant parameters In the first part of the Cookbook Section 7 the default values of the parameters were used Now it is time to discuss in more details the usage of the main parameters The full list of parameters along with short explanations is given in Table 63 Appendix D 8 1 How to choose the start and end level for the analysis Intermediate levels Once you have specified startLevel and endLevel all the steps listed in the GENERAL levelList parameters between these two levels both included will be performed For instance in section 7 1 you used startLevel COR endLevel IMA2 GENERAL_levelList COR GTI DEAD BIN_I BKG_I CAT_I IMA IMA2 BIN_S SPE LCR COMP CLEAN The levels from COR to IMA2 included listed in GENERAL_levelList were performed You can choose what to run according to what kind of output you need Basically e If you are interested only in imaging results set startLevel COR endLevel IMA2 with the complete list of GENERAL_levelList given above as done in section 7 1 e If you have alread
12. ISDC IBIS Analysis User Manual Issue 10 1 47 ii light is a stand alone tool and does not update the proper files with its results Even if you have run both the lightcurve tools in whichever order only the standard one called within the script LCR step ii lc extract will have updated the proper files with its results i e the swg_ibis fits file Thus if you run lc pick to collect the lightcurves only the standard ones will be selected If you want to collect the results of ii light then you have to create an index file that points to all the ii light produced lightcurves and then give this file as input to lc pick as shown below cd REP BASE PROD obs setenv run 0051 dal create obj name all lcr fits template ISGR SRC LCR IDX tpl foreach file 0GID scw run lcr fits idx collect index all lcr fits template ISGR SRC LCR IDX tpl element file end lc pick source GRS 1758 258 attach n group all lcr fits4 1 lc GRS1758 iilight lc fits emin 20 emax 40 instrument ISGRI GRS1758 iilight lc fits contains the merged lightcurve of GRS 1758 258 in the 20 40 keV band that of course has to exist in the lcr fits original files To display it you can use the lcurve program of the FTOOLS package as shown in Section 7 3 2 9 11 Timing Analysis without the Deconvolution Read this if you are interested in fast variability studies up to milliseconds In this section we describe a way of doing timing analysis in a
13. It combines the following exe cutables e ibis isgr evts tag e ibis isgr energy e ip ev correction Using the information about the noisy pixels see Section 3 2 3 the script flags all the noisy events Then the script performs the energy correction of all the events for which correction is possible no correction can be done for the spectral timing mode The output Data Structures contain the list of the photon energy in keV see Appendix C 1 12 1 1 ibis isgr evts tag ibis isgr evts tag tags as noisy all photons from a pixel if this pixel had a switch off during the ScW It also looks at the distribution of the time between events in each given pixel If this distribution is abnormal all photons from this pixel are flagged as noisy within this ScW Noisy events are ignored in the subsequent analysis Table 4 ibis isgr evts tag parameters included into the main script Name Name Type Description in the main script executable SCWI ICOR idxSwitch idxSwitch string DOL of the index of pixels switch list default SCW1_ICOR_probShot probShot real Probability of shot time decay default 0 0001 ISDC IBIS Analysis User Manual Issue 10 1 57 Figure 27 ibis science analysis ibis correction ibis_isgr evis_tag Y sow ibis isgr energy sew E energy correction ip ey correction gti create gti attitude gti data gaps gti intport gti
14. ModPixShad integer Minimum rise time default 16 Maximum rise time default 116 Conversion factor channel to energy default 7 1 Minimum number of non illuminated pixels per mod ule possible values 100 500 default 400 Parameters specific to SCW1 pipeline SCWI ISGRLevent select string SCWI1 GTI LimitTable string SCW1_GTL attTolerance_X real SCW1_GTL attTolerance_Z real SCW1_GTL gtiUserP string SCW1_GTI gtiUserl string CFITSIO event selection string default gt DOL of the limit table for GTIs default Accepted attitude stability tolerance of X optical axis to generate a GTI arc min possible values O 10800 default 0 5 Accepted attitude stability tolerance of Z axis to gen erate a GTI arc min possible values O 10800 default 3 0 DOL of the user GTI table for PICsIT default DOL of the user GTI table for ISGRI default ISDC IBIS Analysis User Manual Issue 10 1 99 SCW1_GTI_TimeFormat string SCWI GTLAccuracy string SCW1_GTLSCP string SCW1_GTLSCI string SCW1_GTLPICsIT string SCW1_GTLISGRI string SCW1_GTIBTI Dol string SCW1_GTIBTI_Names string SCW1_ICOR_idxSwitch string SCW1_ICOR_GODOL string SCW1_ICOR supGDOL string SCWI ICOR supODOL string SCW1_ICOR_riseDOL string switDOL string SCW1_ICOR rtcDOL string Time format to be used possible values IJD UTC OBT default IJD U
15. NEW SOURCE New source flag 0 if old 1 if new SOURCE ID ISDC unique source identifier RA_OBJ Source right ascension in degrees DEC_OBJ Source declination in degrees Y_FIN Y axis fine position of the source in pixels Z_FIN Z axis fine position of the source in pixels FIN_YZ_ERR Error of the fine position along the Y and Z axis in pixels RA_FIN Right Ascension of the fine position of the source DEC_FIN Declination of the fine position of the source FIN_RD_ERR Error of the fine position of the source in RA and DEC FLUX Flux values for a given energy band FLUX_ERR Flux errors for a given energy band DETSIG Source detection significance in ISGRI Table 53 Content of ISGR SKY RES IDX Data Structure Column Name Description TFIRST Time of the first data element TLAST Time of the last data element TELAPSE Total elapsed time of the data E_MIN Lower bound of the energy range EMAX Upper bound of the energy range Search for the sources in the FOV is then performed and a list of sources found is created Data Structure ISGR MOSA RES has the same structure as the ISGR SKY RES Table52 The index of lists of sources found in each map can be found in Data Structure ISGR MOSA RES IDX structure analogous to the one described in the Table 53 ISDC IBIS Analysis User Manual Issue 10 1 91 The output catalog containing the sources description is written to the data structure ISGR SRCL RES This Data Structure
16. On board time Dead time for Semi module 0 Dead time for Semi module 1 Dead time for Semi module 2 Dead time for Semi module 3 Dead time for Semi module 4 Dead time for Semi module 5 Dead time for Semi module 6 Dead time for Semi module 7 Dead time for Semi module 8 Dead time for Semi module 9 Dead time for Semi module 10 Dead time for Semi module 11 Dead time for Semi module 12 Dead time for Semi module 13 Dead time for Semi module 14 Dead time for Semi module 15 Table 47 Content of COMP DEAD SCP Data Structures Column Name Description OB_TIME On board time IC DEADTIME 0 IC DEADTIME 1 IC DEADTIME 2 IC DEADTIME 3 IC DEADTIME A4 IC DEADTIME 5 IC_DEADTIME 6 IC_DEADTIME 7 Dead time for module 0 Dead time for module 1 Dead time for module 2 Dead time for module 3 Dead time for module 4 Dead time for module 5 Dead time for module 6 Dead time for module 7 C 4 ibis binning This script prepares IBIS data for scientific analysis Its main function is to split the data into energy bins and time bins For each time and energy ranges detector shadowgram and a corresponding efficiency shadowgram are created Output Data Structures are listed in the Table 48 These Data Structures keep the position of each pixel and the total counts in given energy band during integration time or efficiency correspondingly The boundaries of the energy and time bins can be found in the corresponding index Data S
17. This chapter describes how to set up the the environment and the analysis data and how to analyse data from the two instruments that are part of IBIS ISGRI and PICsIT These two instruments are quite different in energy range ISGRI starts from 15 keV and PICsIT starts from 200 keV and sensitivity and are optimised for different targets This is why we have decided to guide you through the analysis of the crowded Galactic Centre around 4U 1700 377 for ISGRI and of the bright Crab for PICsIT Here we assume that you have already successfully installed the ISDC Off line Scientific Analysis OSA Software the directory in which OSA is installed is later on referred to as the ISDC_ENV directory If not then look at the INTEGRAL Off line Scientific Analysis Installation Guide 5 for detailed help 6 1 Setting up the analysis data In order to set up a proper environment you first have to create an analysis directory e g ibis_data_rep and cd into it mkdir ibis_data_rep cd ibis_data_rep This working directory ibis data rep will be referred to as the REP BASE PROD directory in the following All the data required in your analysis should then be available from this top directory and they should be organized as follows e scw data produced by the instruments e g event tables cut and stored by ScWs e aux auxiliary data provided by the ground segment e g time correlations e cat ISDC reference catalogue OSA C
18. possible values YES NO default NO Parameters for ibis binning and ibis image reconstruction IBIS II ChanNum integer Number of output energy bands for ISGRI possible values 1 10 value 1 is for more than 10 energy bands in this case IBIS II inEnergyValues should be set default 4 ISDC IBIS Analysis User Manual Issue 10 1 97 IBIS_II_E_band_min IBIS_II_E_band_max IBIS_IT_inEnergy Values IBIS_IPS_corrPDH IBIS_IPS_ChanNum IBIS_IPS_E_band_min_s IBIS_IPS_E_band_max_s IBIS_IPS_E_band_min_m IBIS_IPS_E_band_max_m IBIS_IP_ChanNum IBIS_IP_E_band_min_s string string string integer integer string string string string integer string List of lower limits of output energy bands keV for ISGRI default 20 40 60 100 List of upper limits of output energy bands keV for ISGRI default 40 60 100 200 DOL of the energy values when required default Packets threshold for tograms default 0 partially downloaded his Number of Energy bands for PICSIT in standard mode possible values 0 256 You should set it to 1 to build automatically the only binning for which background maps are present It corresponds to the following energy ranges keV 203 252 252 329 329 455 455 655 655 1057 1057 1841 1841 3570 3570 6510 default 1 List of lower energy boundary for PICSIT
19. 001 swg fits scw 0051 005100440010 001 swg fits scw 0051 005100450010 001 swg fits and a file picsit lst containing scw 0039 003900020020 001 swg fits scw 0039 003900020030 001 swg fits scw 0039 003900020040 001 swg fits scw 0039 003900020050 001 swg fits scw 0039 003900020060 001 swg fits The created files contain the list of ScWs you want to analyze These file names isgri_gc Ist and picsit lst will be used later as an argument for the og_create program see Sections 7 10 6 1 1 Downloading data from the archive e To retrieve the required ISGRI analysis data from the archive go to the following URL http www isdc unige ch integral archive You will reach the W3Browse web page which will allow you to build a list of Science Windows SCWs that you will analyse with OSA Type the name of the object 4U 1700 377 in the Object Name Or Coordinates field Do not forget to change Search Radius if you are interested in science windows where your source is in the partially coded field of view Set it to e g 10 degrees instead of the default 5 degrees 300 arcmin Click on More Options button at the top or at the bottom of the web page Deselect the All checkbox at the top of the Catalog table and select the ScW Science Window Data one Press the Specify Additional Parameters button at the bottom of the web page Introduce
20. 5 8100 keV 4x 10 5 1 MeV Absolute timing accuracy 3 0 ISGRI 61 ps PICsIT 0 976 500ms selected from ground 1000 Y as e 100 Vc effect 10 10 100 energy PICs si gle N mm T 1 1 RICsIT multiple 1000 10000 kev Figure 1 IBIS effective area ISDC IBIS Analysis User Manual Issue 10 1 3 Instrument Description 3 1 The Overall Design IBIS is a gamma ray imager operating in the energy range 20 keV to 10 MeV with two simultaneously operating detectors covering the full energy range located behind a Tungsten mask which provides the encoding The coded mask is optimized for high angular resolution As diffraction is negligible at gamma ray wave lengths the angular resolution of a coded mask telescope is limited by the spatial resolution of the detector array The angular resolution of a coded mask telescope d0 is defined by the ratio between the mask element size C 11 2 mm and the mask to detection plane distance H 3133 mm ON ug d arctan 5 12 IBIS is made of a large number of small fully independent pixels The detector features two layers ISGRI and PICsIT the first is made of Cadmium Telluride Cd Te solid state detectors and the second of Caesium Iodide CsI scintillator crystals This configuration ensures a good broad line and continuum sensitivity over the wide spectral range covered by IBIS The double layer discrete element design of IBIS
21. 672 1036 1848 3584 IBIS IPS E band max s picsit e max s string List of higher energy boundary single events default 252 336 448 672 1036 1848 3584 6720 IBIS IPS E band min m picsit e minm string List of lower energy boundary multiple default 336 448 672 1036 1848 3584 6720 9072 IBIS IPS E band max m picsit e max m string List of higher energy boundary multiple default 448 672 1036 1848 3584 6720 9072 13440 SCW1_BIN_P_inDead inDead string DOL of the dead time Data Structure default SCW1_BIN_P_PicsCxt PicsCxt string DOL of the PICsIT Context Tables default SCW1_BIN_P_HepiLut HepiLut string DOL of the hepi look up table lut default IBIS_IPS_corrPDH corrPDH integer Packets threshold for partially downloaded his tograms default 0 IBIS_P_convFact convFact real Conversion factor channel to energy default 7 1 12 5 ii map rebin ii map rebin reads input background and or Off axis correction maps and rebins them into new energy ISDC IBIS Analysis User Manual Issue 10 1 66 bands Background maps are summed with coefficients equal to the part of each input map that participates in the sum Off axis maps are also weighted by a power law spectrum with the default slope 2 and ARF if present After rebinning off axis maps are normalized to 1 Output energy bands are defined from the index of detector shadowgrams ISGR DETE SHD of a given type Tab
22. AA Ew e 75 12 9 3 E A 76 12 10 Timing Analysis 2 2005 be x moe a ee o a 77 UO AER so AE ce AA ee Re eae wy a A he eS 77 T2102 PICANTE ood b Re Bee eee COL R wes mom vor P303 78 12 11 Summing up the Tesulis c i 266 Sake wae a A Rh yd 78 AILI dp SPHNMOSE R uos os torem ok a BOX A Bede AR eS HE SEM eA 78 12 12 Tools not included in the pipeline o e e 0000008 78 I12 12 1 POSH SPREE uuu nxor A A A de E a 78 3v O EEE 80 A Low Level Processing Data Products e 82 Ad Rew Date coronar a PERE Swe a se Oe ee a 82 A 1 1 Photon by photon mode gt se lt a acea a lees 82 AIZ PIOSIT Standard Mode ose wa koa ae ee Rmo ko b Oe a a 82 A Propad DER 2409 bate ae A A de RU AI e oe E e 83 B Instrument Characteristics used in Data Analysis o o 84 A a AI ANN 84 B2 Calibration Corrections o go o RR RR RR e aw we ee 34 84 B21 PORD 29 ba ak ba ee aa ARG a td do Ad es 84 B 2 2 PIO o Aa hoe CR Ee E Res 85 B3 Limit Tables scu A A wd A ete Oe WY on 86 BA Instrument Background o es i c i bad 949 d EP o a ee as 86 Co dence Data Products o 1209 ess PAS a ee he ee ee ed 87 ISDC IBIS Analysis User Manual Issue 10 1 vi CT ibis COPEC da oa kokonce a d 9030E OR xou 2 29 B ea POP i 0x a xd 87 C 2 2015 08 see A me he eR ee a era ee a 87 C8 DIN FEMME Daw REG Eb A A cpm 87 C 4 A A RAN 88 CAL 2 POND OUI eru hk aeree poh ew ef PD ren sitae Ge kay a ANE TR deus ue 89 C 5 CU
23. Data Structure Column Name Description SWID Science Window identifier SOURCE ID ISDC unique source identifier NAME One commonly used name for the source RA_FIN Source right ascension in degrees DEC_FIN Source declination in degrees FIN RD ERR Error of the fine position of the source in RA and DEC Y_FIN Y axis fine position of the source in pixels Z_FIN Z axis fine position of the source in pixels FIN_YZ_ERR Error of the fine position along Y and Z axis in pixels DETSIG Source detection significance in ISGRI E_MIN Lower energy boundaries E MAX Upper energy boundaries FLUX Flux values FLUX ERR Flux errors DEADC Mean deadtime and greyfilter correction factor EXPOSURE Mean exposure time over the detector plane TSTART Start time of the observation IJD ISDC IBIS Analysis User Manual Issue 10 1 92 TSTOP End time of the observation IJD C 7 2 ip skyimage ip skyimage performs deconvolution of the PICsIT shadowgrams with the use of the balanced cross correlation method described in Goldwurm et al 2003 10 see also Section 12 8 The values of the decoding G array are taken from PICS DECO MOD Data Structure The output Data Structure PICS SKY IMA store either a cartesian CAR or a tangential TAN pro jection of the celestial sphere The index of deconvolved images is written to the PICS SKY IMA IDX Data Structure it has the same content as ISGR SKY IMA IDX Table 51 IMATYPE can be
24. IBIS Analysis User Manual Issue 10 1 55 11 Known Limitations Please note that in the time between the releases this list can change For the most updated version see http www isdc unige ch integral osa current issues osa 11 1 ISGRI 1 Systematic uncertainties of 1 should be added to ISGRI counts fluxes 2 In the mosaic build with the option spread 1 the source flux is slightly reduced 10 96 compared to the weighted average of the fluxes measured in the Science Window 3 The maximum number of sources handled by ii spectra extract is 200 but it is strongly recommended to only fit spectra of the sources that are effectively active visible detectable during the Science Window 4 With OSA10 new calibration files have been produced including a correction for the variation of gain across the entire mission as observed in previous OSA versions However on single revolution time scale a drift in counts is still observed For the latest part of the mission spectra extracted at the beginning and end of a same revolution can therefore show an artificial difference in counts The secular drift observed in all bands over the mission life time is known and due to the evolution of gain this effect is accounted for by the set of ARF s available in the IC tree 5 The position of the low energy threshold is increasing with time see Sect 12 4 1 A safe lower limit for the response is 18 keV until revolution 848 Between revo
25. IC tree default Divide by efficiency default no Remove bad pixels default yes flatten modules default no ISDC IBIS Analysis User Manual Issue 10 1 107 SCW2_BKG_I_method_cor SCW2_BKG_I_method_int SCW2_BKG_P_method SCW2 BKG picsSUnifDOL SCW2_BKG picsSBkgDOL SCW2_BKG_picsMUnifDOL SCW2_BKG_picsMBkgDOL string string integer string string string string Method to be applied for background removal possible values O background from IC tree is applied to the whole detector 1 parameter switches to this value automatically when background map is specified not an IC one 2 background is threaded for each module separately When using 1 or 2 brPif and brPifThreshold pa rameters are taken into account default 2 Method to be applied for the pixel value interpolation possible values 0 pixels in dead zones are filled with zeros 1 pixels are filled with mean detector value default 1 Method applied in filling gaps possible values 0 2 default 1 DOL of the PICsIT Detector Uniformity model sin gle default DOL of the PICsIT Detector Background model sin gle default DOL of the PICsIT Detector Uniformity model mul tiple default DOL of the PICsIT Detector Background model mul tiple default Parameters for lightcurve extraction ILCR select ILCR delta t ILCR num
26. Look Analysis or for Off Line Scientific Analysis e Pointing Period during which the spacecraft axis pointing direction remains stable Because of the INTEGRAL dithering strategy the nominal pointing duration is of order of 20 minutes e Slew Period during which the spacecraft is manoeuvered from one stable position to another i e from one pointing to another ISDC IBIS Analysis User Manual Issue 10 1 xiii 1 Introduction The IBIS Analysis User Manual i e this document was edited to help you with the IBIS specific part of the INTEGRAL Data Anaysis A more general overview on the INTEGRAL Data Analysis can be found in the Introduction to the IN TEGRAL Data Analysis 1 For the ISGRI and PICsIT analysis scientific validation reports see 3 and 4 The IBIS Analysis User Manual is divided into two major parts e Description of the Instrument This part based to some extent on the IBIS Observer s Manual of the ISOC AO documentation 2 introduces the INTEGRAL on board Imager IBIS Description of the Data Analysis This part starts with an overview describing the different steps of the analysis Then in the Cookbook Section several examples of analysis and their results and the description of the parameters are given Finally the used algorithms are described A list of the known limitations of the current release is also provided In the Appendix of this document you find the description of the
27. Per usrcat fits chmod w usrcat fits If you want to add a new source not specified in the general reference catalog add a line to usrcat fits with the help of the fv tool and fill in the Source ID NAME RA_OBJ and DEC_OBJ columns As Source_ID you can choose whatever you like provided that this identifier is unique NOTE usrcat fits keeps the same format of the general reference catalog from which it was built i e it has the extension of the type GNRL REFR CAT This is the correct extension to be used as input for the Imaging step In Section 7 2 you have been shown how to build a catalogue for the lightcurve LCR and spectral SPE step In that case the catalogue you obtained specat fits was of the type of ISGR SRCL RES which is the correct format for the LCR and SPE steps The two formats cannot be switched meaning that you cannot use a GNRL REFR CAT type catalog for SPE and LCR or an ISGR SRCL RES one for IMA 9 8 Alternative Spectral Extraction from the Mosaic Read this if you want to extract the average spectrum of a source from a set of mosaic images in different energy bands It is possible to extract the spectrum of a source from a set of mosaic images in several large energy bands In general this method gives results similar to the Science Window average spectrum you obtain from spe_pick see Sections 7 2 and 9 4 2 Once you have the spectrum you will need the corresponding rebinned matrix to be able
28. Raw and Prepared Data and also the description of the Scientific Products Part I Instrument Definition 2 Scientific Performances Summary IBIS is a gamma ray telescope observing celestial objects of all classes ranging from the most compact galactic systems to extragalactic objects with powerful diagnostic capabilities of fine imaging source identification and spectral sensitivity in both continuum and lines It is able to localize weak sources at low energy to better than a few arcminutes accuracy covering the entire energy range from a few tens of keV to several MeV Table 1 gives an overview of the scientific capabilities of IBIS The effective area curves are given on the Figure 1 ISDC IBIS Analysis User Manual Issue 10 1 1 Table 1 Scientific Parameters of IBIS Operating energy range 15 keV 10 MeV Energy resolution FWHM 7 Q 100 keV 9 Q 1 MeV Effective Area ISGRI 960 cm at 50 keV PICsIT 870 cm at 300 keV single events PICsIT 275 cm at 1 MeV multiple events Field of view 8 3 x 8 0 fully coded 19 x 19 partially coded 50 Angular resolution FWHM 12 Point source location accuracy 30 100 keV 90 error radius lt 5 Q1 MeV Continuum sensitivity photons cm s keV 3c detection AE E 2 109 s integration 3 8 x 1077 100 keV 1 2x10 7 Q 1 MeV Narrow line sensitivity photons cm s 30 10 s integration 1 3 x 10
29. Table 44 Index of all IBIS GNRL GTI Data Structures for all categories is written to the IBIS GNRL GTI IDX Table 44 Content of IBIS GNRL GTI Data Structures Column Name Description OBT START On board time of start of the GTI OBT END On board time of end of the GTI C 3 ibis_dead This script calculates the dead times for ISGRI PICsIT and Compton cases The results of the executables are written to Data Structures ISGR DEAD SCP PICS DEAD SCP and COMP DEAD SCP This Data Structures contains the information about the on board time and the dead time for each module see Tables 45 47 Table 45 Content of ISGR DEAD SCP Data Structures Description On board time Dead time for module 0 Column Name OB_TIME IL DEADTIME 0 ISDC IBIS Analysis User Manual Issue 10 1 87 ILDEADTIME_1 ILDEADTIME 2 ILDEADTIME 3 ILDEADTIME 4 ILDEADTIME 5 ILDEADTIME 6 ILDEADTIME 7 Dead time for module 1 Dead time for module 2 Dead time for module 3 Dead time for module 4 Dead time for module 5 Dead time for module 6 Dead time for module 7 Table 46 Content of PICS DEAD SCP Data Structures Column Name Description OB_TIME IP_DEADTIME_0 IP DEADTIME 1 IP DEADTIME 2 IP DEADTIME 3 IP_DEADTIME_4 IP DEADTIME 5 IP DEADTIME 6 IP DEADTIME 7 IP DEADTIME 0 IP_DEADTIME_1 IP_DEADTIME_2 IP_DEADTIME 3 IP DEADTIME 4 IP DEADTIME 5 IP DEADTIME 6 IP DEADTIME 7
30. Ton T where Ton T is given by the GTI and the total observation length ISDC IBIS Analysimbleer3Maimial shksswe bild parameters included into the main 65 script Name in the main script Name executable Type Description IBIS IP E band max m IBIS IP E band min s SCWI BIN P inDead SCWI1 GTI PICSIT SCWI BIN P PicsCxt picsit e max m picsit t bin s inDead gti name PicsCxt string string string string string List of higher energy boundaries for PICsIT multiple events default 600 1000 13500 Time bins for the lightcurves default 1 DOL of the dead time Data Structure default Name of GTI to use default VETO ATTITUDE P_SGLE DATA GAPS P MULE DATA GAPS DOL of the PICsIT Context Tables default gt 12 4 3 ip si shadow build ipsi shadow build takes as an input PICsIT data received in standard mode For each given energy and time range intensity and efficiency shadowgrams are produced Efficiency is defined as Eff 1 D x Ton T Table 14 ip si shadow build parameters included into the main script Name Name Type Description in the main script executable IBIS IPS ChanNum picsit e bin integer Number of Energy bands 1 means to use the default ones default 8 IBIS IPS E band min s picsit e mins string List of lower energy boundary single events default 203 252 336 448
31. a longer of order N computation time than extracting a source alone Care has been taken so that the output structure is compatible with HEASARC tools There are no limits on the size of time bin up to 0 1s and number of energy bands ii light is not the official lightcurve extraction tool and should be used mainly to check relative variability of bright sources within a given Science Window rather than for a long term absolute flux estimate An extended comparison between the official lightcurve extraction tool ii lc extract and ii light can be found in Grinberg et al 2011 15 Table 28 i light parameters Name Type Description inSwg string DOL of the input Observation Group default outSwg string DOL of the output Observation Group default outLC string Dol of the light curves file default context string DOL of the context where we can find low threshold default GTIname string Name of the GTI to be applied default select string Event selection condition default ISDC IBIS Analysis User Manual Issue 10 1 80 pifDOL deadDOL corrDol backDol delta t num e e min e max onlydet idxSwitch idxNoise evttype source selectDol maxessential cleanobt chatter string string string string real integer string string boolean string string integer string integer boolean integ
32. and the time window e g the dead time due to the time of the photon detection is equal to the product of the module count rate and the coding time The dead time due to the veto is equal to the product of the veto count rate and the veto time window etc The resulting dead time is taken as a sum of all the dead times connected with different effects Simple summing of dead times can be done since the estimations show that the coincidence probability between different types of events is low The values of the count rates is taken from the HK Data Structures IBIS DPE HRW and IBIS DPE CNV and the corresponding time windows are either measured instrumental or read into HK or IC all others VETO Compton 12 3 1 ibis isgr deadtime The executable ibis isgr deadtime calculates dead times resulting from count rates in ISGRI modules taking into account the instrument configuration ISGRI dead time is due to the combined effect of e Instrument count rate e Veto count rate from the lateral or lateral bottom according to IC file shielding e Calibration count rate e Compton coincidences if Compton mode is on ISDC IBIS Analysis User Manual Issue 10 1 63 Note that the problem of the VETO swapping on board is corrected almost every time through IC file IBIS VETO MOD VETO also sometimes has a wrong level this will be corrected in the future The 3 cases when it happened are in the IC file GNRL INTL BTI with the BTI TYPE ISGRI VE
33. are ready to extract the spectrum To do this you can either fill the values manually from the picsit_sky res file or extract the fluxes from the brightest pixel around the catalog position with the help of the spextract_pics pl cd REP_BASE_PROD obs picsit_ima perl spextract_pics pl i picsit lst r 83 605 d 21 951 n 8 o crabspe_pics fits m ic ibis rsp pics_srmf_grp_0005 fits a ic ibis rsp pics sarf rsp 0003 fits In this command switches i and o define the input and output files r and d define the RA and DEC of the desired pixel n defines the number of energy ranges m and a define the locations of rmf and arf matrices The result is shown in Figure 26 10 3 PICsIT Timing Analysis It is possible to produce a lightcurve of the PICsIT detector from the spectral timing data To build it it is enough to run the analysis from the COR to DEAD level and then from LCR to LCR of course it is not a problem if you have already done the analysis up to the IMA2 level Do not forget to disable ISGRI and enable PICsIT for the analysis The results are in the following FITS files scw RRRRPPPPSSSF 001 picsit_lcr fits ISDC IBIS Analysis User Manual Issue 10 1 54 data and folded model crabspe_pics f te T T normalized counts sec ke 200 500 1000 channel energy keV Figure 26 PICsIT Crab spectrum extracted from the mosaic These files can be analyzed with standard xronos tools ISDC
34. e ILCR e min ILCR e max string real integer string string Event selection condition default Time bin in seconds possible values 0 1 10000 default 100 Number of energy channels possible values 1 10 default 4 List of low energy boundaries default 20 40 60 100 List of high energy boundaries default 40 60 100 200 Parameters for PICsIT mosaic extraction ISDC IBIS Analysis User Manual Issue 10 1 108 OBS2_detThr OBS2_projSel OBS2_imgSel real string string Detection Threshold in sigmas default 3 0 Selection of projection default STG Selection criteria of images default EVT_TYPE SINGLE amp amp E MIN 252 amp amp E_MAX 336 ISDC IBIS Analysis User Manual Issue 10 1 109 References O o N DD 10 11 12 13 14 15 Introduction to the INTEGRAL Data Analysis http www isdc unige ch integral analysiszzZDocumentation IBIS Observer s Manual http integral esac esa int AO10 AO10_IBIS_ObsMan pdf ISGRI Scientific Validation Report http www isdc unige ch integral analysiszz Documentation PICsIT Analysis Scientific Validation Report http www isdc unige ch integral analysiszzZ Documentation INTEGRAL Off line Scientific Analysis Installation Guide http www isdc unige ch integral download osa doc current osa inst guide pdf Di Cocco G Caroli E Celesti E
35. either IMAGE either VARIANCE or SIGNIFICANCE The list of sources that were found during the analysis are written to the PICS SKY RES C 8 Spectral Analysis C 8 1 i spectra extract ii spectra extract reads the shadowgram for each input energy band and creates a spectrum for background and each source from isgri_srcl_res fits file The result is written to the ISGR EVTS SPE and ISGR EVTS SPE IDX Data Structures Table 56 Content of the ISGR EVTS SPE Data Structure Column Name Description CHANNEL Channel number RATE Countrate in the given channel SYS ERR Systematic error STAT_ERR Statistical error QUALITY Quality flag GROUPING Grouping flag Table 57 Content of the ISGR EVTS SPE IDX Data Struc ture Column Name Description SOURCEID ISDC unique source identifier RA_OBJ Source right ascension in degrees DEC_OBJ Source declination in degrees TFIRST Time of the first data element TLAST Time of the last data element TELAPSE Total elapsed time of the data C 9 Timing Analysis C 9 1 2p st lc extract This program build light curves and related errors starting from spectral timing data of PICsIT The content of the filled Data Structures is given in the Tables 58 59 ISDC IBIS Analysis User Manual Issue 10 1 93 Table 58 Content of the PICS EVTS LCR IDX Data Struc ture Column Name Description SOURCEID ISDC unique source identifier CHANMIN Lowest channel of the
36. energy range CHANMAX Highest channel of the energy range E_MIN Lower bound of the energy range E_MAX Upper bound of the energy range PICSMODE Mode of the PICsIT detector layer Table 59 Content of the PICS EVTS LCR Data Structure Column Name Description TIME Time of measurement for the bin TOT_COUNTS Total counts of the source region BACKV Background counts scaled to the source region BACKE Background count errors ERROR Net count error in the source region RATE Countrate in the given energy band FRACEXP Fraction of integration bin time for exposure correction C 9 2 lc extract For all sources from the isgri srcl res fits file lc extract extracts the ISGRI lightcurves The results are written to the ISGR SRC LCR and ISGR SRC LCR IDX Data Structures ISGR SRC LCR has the same structure as PICS EVTS LCR see Table 59 Table 60 Content of the ISGR SRC LCR IDX Data Structure Column Name Description SOURCEID ISDC unique source identifier RA_OBJ Source right ascension in degrees DEC_OBJ Source declination in degrees CHANMIN Lowest channel of the energy range CHANMAX Highest channel of the energy range E_MIN Lower bound of the energy range EMAX Upper bound of the energy range C 9 3 Timing Analysis without the deconvolution During the run of stand alone programevts extract two data structures GNRL EV TS GTI and GNRL EVTS LST are filled GNRL EVTS LST Table 61 c
37. extension of mosa idx instead of the on time map default 2 OBS1_NegModels NegModels integer 0 or absent for no negative models 1 negative models default 0 OBSI FastOpen FastOpen integer if 1 then no CommonPreparePars default 1 12 8 2 sumhist PICsIT needs long integration times to produce a good image Thus if INTEGRAL was stable during several Science Windows it is recommended to sum up PICsIT shadowgrams before the deconvolution If the ibis science analysis parameter staring is set to yes then sumhist checks that INTEGRAL was stable during all the Science Windows within the given limits and sums all the PICsIT shadowgrams into one Table 20 sumhist parameters included into the main script Name Name Type Description in the main script executable tolerance tol real tolerance for staring default 0 0001 12 8 3 ghost busters We have found that some regions of the mask have glue deposits in the void The shadowgrams of strong sources near those glue deposits are not fully correct and create artifacts in the images mostly ghosts In the new ghost buster processing affected pixels are killed from the shadowgrams for strong sources sourcecat ISDC REF CAT ISGRI FLAG2 5 If you include too many sources by changing the default catalog parameter SCW1 BKG buster src in ibis science analysis in this ghost buster algorithm you will also kill too many signal
38. following analysis TIME_TAG Compton delta time to previous event CS CM DUMMY COUNTER Dummy counter some technical information used to CS CM reconstruct the On Board Time A 1 2 PICsIT Standard Mode In this mode the information is accumulated on board and transmitted to the Earth in a kind of histograms Spectral image histograms are written to the Data Structures PICS SISH RAW and PICS SIMH RAW for single and multiple events correspondingly These Data Structures represent a three dimensional ISDC IBIS Analysis User Manual Issue 10 1 82 table with total counts during integration time The axes of the grid are directed along the following axes AXIS 1 Channel number AXIS 2 Y position AXIS 3 Z position Spectral timing histograms are written to the Data Structure PICS SPTI RAW and contain the infor mation on the number of the events accumulated in the up to 8 energy bins during a given time amount see Table 31 Table 31 Content of PICS SPTI RAW Data Structure Column Name Description CELL 1 1st cell of the spectrum CELL 2 2nd cell of the spectrum CELL 3 3rd cell of the spectrum CELL_4 4th cell of the spectrum CELL_5 5th cell of the spectrum CELL 6 6th cell of the spectrum CELL 7 7th cell of the spectrum CELL 8 8th cell of the spectrum The local on board time and the channels definitions can be found in the PICS SPTI PRW Data Structure A 2 Prepared Data The main ta
39. in standard mode for SINGLE Do not touch this parameter default List of higher energy boundary for PICsIT in standard mode for SINGLE Do not touch this parameter default List of lower energy boundary for PICsIT in standard mode for MULTIPLE Do not touch this parameter default List of higher energy boundary for PICsIT in standard mode for MULTIPLE Do not touch this parameter default Number of Energy bands for PICsIT in photon by photon mode possible values 1 300 Do not touch this parameter default 3 List of lower energy boundary single Do not touch this parameter default keV 175 600 1000 ISDC IBIS Analysis User Manual Issue 10 1 98 IBIS IP E band max s string IBIS IP E band min m string IBIS IP E band max m string IBIS NoisyDetMethod integer List of higher energy boundary single Do not touch this parameter default keV 600 1000 10000 List of lower energy boundary multiple Do not touch this parameter default keV 350 600 1000 List of higher energy boundary multiple Do not touch this parameter default keV 600 1000 13500 Noisy Pixel detection method possible values 0 only normal noisy detection 1 add also spectral noisy detection default 1 These parameters are recommended by the IBIS team better not to change them IBIS min rise integer IBIS max rise integer IBIS P convFact real
40. maps somewhere and make them read only Then launch the analysis for other science windows specifying the following parameters in your ibis science analysis call rebinned corrDol ima your path rebinned corr ima fits rebinned_corrDol_spe your_path rebinned_corr_spe fits rebinned_backDol_ima your_path rebinned_back_ima fits ISDC IBIS Analysis User Manual Issue 10 1 44 rebinned_backDol_spe your_path rebinned_back_spe fits rebinned_unifDol_ima your_path rebinned_unif_ima fits rebinned_unifDol_spe your_path rebinned_unif_spe fits IMPORTANT rebinned maps are created for a given set of energies only so these should remain the same only as long as you are not changing energy ranges in your IMA and SPE analysis If you want to change IMA energy bins or spectral response energy boundaries these maps have to be created again 9 7 Create your own catalog Read this if you are familiar with the sources in your field of view and you want to build your own catalog for the Imaging step As already discussed in Section 8 2 1 during the imaging step IMA it can be very useful to use your own input catalog The easiest way to build it is to modify the general catalog with the help of the fcopy program of FTOOLS For example if you want to create a catalog usrcat fits with only three sources Crab 3C111 and XPer do the following cd REP_BASE_PROD fcopy ISDC REF CAT NAME Crab NAME 3C 111 NAME X
41. non binning way i e starting from the single events This way is suitable for very short time scales up to milliseconds and is less recommended for long time bins for which the binning tools i light and ii lc extract are suitable In the text we will use one of the Science Windows with Crab data you have downloaded to run the PICsIT analysis e g 003900020020 In general the table with the events is very big so if you are interested in only part of the Science Window e g in the case of a burst it is better to define a user good time interval see Section 9 and work within it To select the photons that come from a given source in the field of view you need to have the corresponding PIF PIF is automatically created during the SPE step but can also be created with a standalone tool i pif Create with og create observational group REP BASE PROD obs crab og ibis fits and run analysis from COR to DEAD level prepare the catalog with Crab only and run ti pif cd REP BASE PROD obs crab ibis science analysis ogDOL og_ibis fits startLevel COR endLevel DEAD fcopy infile ISDC REF CAT NAME Crab outfile crab_specat fits ii pif in0G outO0G og ibis fits inCat crab specat fits N num band 1 E band min 20 E band max 1000 N mask REP BASE PROD ic ibis mod isgr mask mod 0003 fits N tungAtt REP BASE PROD ic ibis mod isgr attn mod 0010 fits N aluAtt REP BASE PROD ic ibis mod isgr attn mod 00
42. o e 44 9 7 Create your own catalog lt ps s ce eeud ee eR bY Lew ade aw we ee xs 45 9 8 Alternative Spectral Extraction from the Mosaic 00002 e ee 45 9 9 BAVCON HOA 2 on ak ees oe Mew Ee eee PERE OE Se kee ESe Be 46 910 Altemative Timing Analysis o ss e 44 4 ee eR bed eee ee ee s 46 BHO Filipi s oo boo baba ad Suec 9 4 191 Ea ae a ee 46 9402 Buniildldsght o erse rsr Rer x x Be eb de Y esr A xe od 47 ISDC IBIS Analysis User Manual Issue 10 1 iv 9 10 3 Merge the ii light results from different Science Windows 47 9 11 Timing Analysis without the Deconvolution oo o o 48 9 12 Phase Resolved Analysis coi 2 40 a er RR eds 50 10 PIES daba analysa 12 l2 xc ies cara a Aa a da 51 10 1 PICSIT Image Reconstruction 2 omo mon m RR a o REOR RR dew e 51 10 1 1 Results of PICSIT image analysis lees 53 10 2 PICsIT spectral extraction from the mosaic image len 53 10 3 PICSIT Timing Analysis ee eR Rm RR RR eR BOR AUR s 54 Il Known Limitations a Sos eie e hs d E09 a 94h RR a de DR 9 rev m o dogs 56 LT JSOHE ur ia dede CU ERS Ru ure RUE E ES eed ded 56 LL2 PLAT esci RR eR OR ee oan eS Bec Row qo ees a we des 56 III Data Analysis in Details 57 12 SCENES Analysis ora A Ead rd uk Se dd a 57 12 1 IMECIPECHONA pia he eh rue e Seg hoe PUE Re ER Bee ee he ee 97 12 1 1 ASSIM cia A A AA ee 57 12 1 2 e ne Soon Yes Wek Goh ehh qe die fede A edle i
43. of parameters for source intensity variability VAR_PARS Parameters for source intensity variability COMMENTS Comments SPLFLUX 1 SPI flux in the soft SPI energy band SPLFLUX 2 SPI flux in the hard SPI energy band ISGR_FLUX_1 ISGRI flux in the soft ISGRI energy band ISGR_FLUX_2 ISGRI flux in the hard ISGRI energy band PICS FLUX 1 PICsIT flux in the soft PICsIT energy band PICS FLUX 2 PICsIT flux in the hard PICsIT energy band JEMX FLUX JEMX flux in the soft JEMX energy band JEMX FLUX 2 JEMX flux in the hard JEMX energy band E MIN Lower energy boundaries E MAX Upper energy boundaries FLUX Flux values FLUX ERR Flux errors SEL FLAG Source selection flag FLAG Generic flag C 6 ibis background cor This script combines executables performing the background correction in accordance with the chosen method As the output for each energy range for ISGRI shadowgrams of larger dimensions corrected expanded shad owgram and corresponding variance and efficiency expanded shadowgrams are written to ISGR CEXP SHD The energy range is given in the keywords E MIN E MAX CHAN MIN CHAN MAX and a shadowgram type is given by SHD TYPE keyword For PICsIT Data Structures PICS CEXP SHD and PICS VEXP SHD are filled for the corrected ex panded detector shadowgram and the corrected expanded variance detector shadowgram The energy range is again given in the keywords C 7 Image Analysis C 7 1 ii skyimage ii skyimage deconvol
44. successful analysis you should make new rebinned matrix read only chmod w new rmf fits To tell the software to use this newly created matrix set in your analysis IBIS SI inEnergyValues PATH TO THE FILE new rmf fits 3 otherwise the default 13 channels will be used corresponding to an empty value of IBIS SI inEnergyValues To have the correct name of the response matrix in the header of the spectrum file you should set SCW2 ISPE idx isgrResp rmf fits Warning This parameter is hidden Thus you should either provide the value of this parameter during the script launch ibis science analysis SCW2 ISPE idx isgrResp new rmf fits or press hidden button and set this parameter on the SPE page 9 5 1 Extracting images in more than 10 energy ranges If you want to create images in more than ten energy bands you have to create a rebinned matrix new rmf fits as shown in the text just above Then to create images in the energy ranges defined in the third extension of this file set IBIS II ChanNum 1 IBIS II inEnergyValues PATH TO THE FILE new rmf fits 3 The first parameter instructs the program to use the energy boundaries specified in the second parameter 9 6 Some tricks on saving disk space and CPU time To gain time and space it is possible to create the rebinned correction and background maps rebinned fits only once and then give them as an input for the rest Analyse one science window from COR to SPE copy the
45. types of images INTENSITY and SIG NIFICANCE are produced In case PICSIT_inCorVar 1 a variance map is also produced The list of found sources is in the file picsit_sky_res fits In our example the Crab is the only real source that was found In Figure 25 you see the resulting image in the 252 336 keV energy range The Crab is clearly seen in the center The figure was produced with the help of ds9 cat2ds9 isgri_catalog fits cat reg symbol circle color red ds9 picsit_ima fits 5 region cat reg cmap cool scale linear scale limits 0 7 zoom 8 In the case of observations with dithering pattern staring no the pipeline performs the shadowgram deconvolution in every Science Window and the output files are under scw RRRRPPPPSSSF 001 picsit ima fits scw RRRRPPPPSSSF 001 picsit_sky_res fits and the integration of all these images mosaic is in picsit_ima fits 10 2 PICsIT spectral extraction from the mosaic image It is also possible produce the source spectrum from the mosaic image ISDC IBIS Analysis User Manual Issue 10 1 53 Figure 25 Crab significance image in the 252 336 keV energy band as seen by PICsIT At http www isdc unige ch integral osa scripts you find an example of such a of perl script spextract_pics pl To use it create a list of files you want to use for spectral extraction In the case of staring file picsit 1st will contain a single line picsit_ima fits Now you
46. w 005100570010 001 ISDC IBIS Analysis User Manual Issue 10 1 50 cd REP_BASE_PROD og_create idxSwg phase lst ogid phase baseDir instrument IBIS cd obs phase ibis science analysis SCW1_ISGRI_event_select DELTA_TIME lt 50 Note that in this case you create a dead time about which the software is not aware of Thus you will have to correct the resulted flux by the factor original exposure real exposure In the case above we have selected events with phase less than 50 i e half of the time was rejected and the resulted flux should be multiplied by 2 10 PICsIT data analysis Unfortunately PICsIT sensitivity is not high enough to create a good image for a single Science Window thus you should expect good results only if INTEGRAL is in staring mode and the source is really bright In the example below we use Crab observations done in staring mode Download and install as described in Section 6 1 the following Science Windows whose DOLs are assumed to be written to the file picsit lst scw 0039 003900020020 001 swg fits scw 0039 003900020030 001 swg fits scw 0039 003900020040 001 swg fits scw 0039 003900020050 001 swg fits scw 0039 003900020060 001 swg fits Create the working directory picsit_ima with the og_create program cd ibis_data_rep setenv REP_BASE_PROD PWD og_create idxSwg picsit lst ogid picsit_ima baseDir instrument IBIS cp r obs picsit_ima obs picsit_spe 10 1 PICsIT Image Reconstruct
47. 0 lists Data Structures with the instrument background models Table 40 Instrument Background Model Data Structures Data Structure Description ISGR BACK BKG ISGRI instrument background array ISGR UNIF BKG ISGRI instrument background uniformity array PICS SBAC BKG PICsIT instrument background array for single events PICS SUNI BKG PICsIT instrument background uniformity array for single events PICS MBAC BKG PICsIT instrument background array for multiple events PICS MUNI BKG PICsIT instrument background uniformity array for multiple events COMP SBAC BKG COMPTON instrument background array for single events COMP SUNI BKG COMPTON instrument background uniformity array for single events COMP MBAC BKG COMPTON instrument background array for multiple events COMP MUNI BKG COMPTON instrument background uniformity array for multiple events For each type of Data Structures in Table 40 there is an Index Its content is given in Table 41 Two last columns RISE_MIN and RISE_MAX are present only in ISGR BACK BKG IDX and ISGR UNIF BKG IDX Indexes Table 41 Content of Indexes for Table 40 Data Structures Column Name Description VERSION Version of the instrument characteristic file VSTART Start of validity time in IJD VSTOP End of validity time in IJD E_MIN Lower bound of the energy range E MAX Upper bound of the energy range EXPOSURE Effective exposure time VETO_THR Veto threshold METH_BKG Method u
48. 1 gt 100 NAME XX The number of bright sources which could affect the overall normalization of the detector background count rate can be very large in a crowded field like e g the Galactic Center region considered above In this case the number of detector pixels ingored during the calculation of the background normalization can become very large This can result in a worsening of the quality of background subtraction To avoid this one can try two options First possibility is to leave the bright source catalog empty brSrcDOL so that the entire collective contribution of all the bright sources which is almost the same in all detector modules will be taken into ac count Next one can specify if the normalization of the background is calculated using the entire detector or on module by module basis This can be done by changing the value of parameter SCW1_BKG_I_method_cor between 1 default the entire detector and 2 on module by module basis In addition one can try a combination of these two options both give the empty bright source catalog and force the calculation of the normalization of background using the entire detector 8 2 4 Miscellaneous on Imaging e With the parameter OBS1_ExtenType to find it on the GUI pages press the hidden button and go to the IMA page you can choose whether to keep the Residual and or the true Exposure image in the isgri sky ima fits file With OBS1 ExtenType 0 4 maps will be crea
49. 100430010 001 005100440010 001 005100450010 001 You should then download them pressing the Request data products for selected rows button In the Public Data Distribution Form provide your e mail address and press the Submit Request button You will get per e mail the required script to get your data and the instructions for the settings of the IC files and the reference catalogue Just follow these instructions e To retrieve the required PICsIT analysis data from the archive proceed in the same manner with the following parameters Object Name Or Coordinates Crab Search Radius use default value scw_id 0039 To select only science windows starting with 0039 start_date gt 2003 02 07T06 44 19 and end_date lt 2003 02 07T12 44 05 and save your results in a file called picsit 1st which should contain 003900020020 001 003900020030 001 003900020040 001 003900020050 001 003900020060 001 6 2 Setting the environment Before you run any OSA software you must also set your environment correctly The commands below apply to the csh family of shells i e csh and tcsh and should be adapted for other families of shells In all cases you have to set the REP_BASE_PROD variable to the location where you perform your analysis e g the directory ibis_data_rep Thus type setenv REP BASE PROD PWD Then if not already set by default by your system administr
50. 11 fits N leadAtt REP BASE PROD ic ibis mod isgr attn mod 0012 fits ISDC IBIS Analysis User Manual Issue 10 1 48 Bin time 0 1000E 02 s _ AA 5 E or H 4 T z o a I ERAT PA ll N l a pos 4 can5osdp xx xp X p d 4 E e p B doge ge ge e ono i 0 50 100 150 200 250 Frequency Hz Start Time 12866 15 57 30 185 Stop Time 12866 16 33 53 323 Figure 22 Crab power spectrum Now you are ready to create the lists of photons cd REP_BASE_PROD obs crab evts extract group og ibis fits events crabevts fits instrument IBIS sources crab_specat fits gtiname MERGED_ISGRI pif yes deadc yes attach no barycenter 1 timeformat 0 instmod To increase signal to noise ratio select only events with PIF 1 fcopy crabevts fits 2 PIF_1 1 crab_pif1 fits chmod w crab pifi fits Now you can produce the Crab power spectrum powspec Ser 1 filename options or file of filenames options crab pifi fits Name of the window file for default window Newbin Time or negative rebinning 0 001 Number of Newbins Interval INDEF Number of Intervals Frame INDEF Rebin results gt 1 const rebin 1 geom rebin O none 0 Name of output file default Do you want to plot your results yes Enter PGPLOT device XW hardcopy crab powerspec ps PS ISDC IBIS Analysis User Manual Issue 10 1 49 As a result the crab_powerspec ps plot shown in F
51. 2 ees 89 Content of ISGR SKY IMA IDX Data Structure leen 90 Content of ISGR SKY RES Data Structure ee 91 Content of ISGR SKY RES IDX Data Structure e 91 New information added to the ISGR SRCL RES Data Structure o 92 Content of the ISGR OBS RES Data Structure e 92 Content of the ISGR EVTS SPE Data Structure 93 Content of the ISGR EVTS SPE IDX Data Structure leen 93 Content of the PICS EVTS LCR IDX Data Structure o 94 Content of the PICS EVTS LCR Data Structure 94 Content of the ISGR SRC LCR IDX Data Structure o eren 94 Content of the GNRL EVTS LST Data Structure 94 Content of the GNRL EVTS GTI Data Structure leen 95 ibis science analysis parameters description o e e 96 IBIS Analysis User Manual Issue 10 1 xi Acronyms and Abbreviations AD ADD A D AFEE ASIC BGO CdTe CsI DBB DFEE DOL DPE DS FCFOV FIFO FOV FWHM GPS GTI GUI ISDC IBIS Analysis User Manual Issue 10 1 Architectural Design Architectural Design Document Analog Digital Analog Front End Electronics Application Specific Integrated Circuits Bismuth Germanate Cadmium Telluride Caesium lodide Detector Bias Box Digital Front End Electronics Data Object Locator Data Processing Electronics D
52. AT package e ic Instrument Characteristics IC such as calibration data and instrument responses OSA IC package e idx set of indices used by the software to select appropriate IC data OSA IC package The cat ic and idx directories are part of the OSA software distribution and should be installed following the INTEGRAL Off line Scientific Analysis Installation Guide 5 The actual data along with the auxiliary files scw and aux are sent to the Principal Investigators of the observation Alternatively the public data can be downloaded from the archive see Section 6 1 1 In case the data are already available on your system you can either copy these data to the relevant working directory or better create soft links as shown below Alternatively if you do not have any of the above data on your local system or if you do not have a local archive with the scw and the aux branch available follow the instructions in the next section to download data from the ISDC WWW site ln s directory of ic files installation ic ic ln s directory of ic files installation idx idx ln s directory of cat installation cat cat ln s directory of local archive scw scw ln s directory of local archive aux aux 6 Then just create a file isgri gc lst containing the 5 lines scw 0051 005100410010 001 swg fits scw 0051 005100420010 001 swg fits ISDC IBIS Analysis User Manual Issue 10 1 16 scw 0051 005100430010
53. Analysis User Manual Issue 10 1 72 OBS1_mask OBS1_deco OBS1_DataMode OBS1_SearchMode OBS1_ToSearch OBS1_CleanMode tungAtt aluAtt lead Att OBS1_ScwType OBS1_DoPart2 OBS1_MapAlpha OBS1_MapDelta OBS1_MapSize OBS1_PixSpread OBS1_MinCatSouSnr mask deco DataMode SearchMode ToSearch CleanMode tungAtt aluAtt lead Att ScwType DoPart2 MapAlpha MapDelta MapSize PixSpread MinCatSouSnr string string integer integer integer integer string string string string integer real real real integer real ISDC IBIS Analysis User Manual Issue 10 1 DOL of the MASK pattern fits file default DOL of the projected decoding pattern fits file default Data Simulation mode possible values 0 shadowgrams are treated 1 shadowgrams are simulated default 0 Source search mode possible values O search for all significant excesses 1 search for all catalog sources 2 search for K sources where K ToSearch 3 search for all catalog sources plus K significant excesses where K ToSearch Parameter SearchMode 1 3 concerns only images at a Science Window level In the mosaic image ii skyimage always looks for K ToSearch sources default 3 Number of sources to be looked for default 50 Ghost cleaning possible values 1 source model lobes are subtracted from the decon volved image 1 no subtrac
54. BS1 PixSpread 13 OBS1_SouFit 0 2 SCW1 BKG l isgrBkgDol browse brSrcDOL sisbC REF CATIISGRI FLAG2 5 amp amp ISGR FLUX 1 gt 100 browse Figure 13 Imaging page of the IBIS GUI of SCW1_BKG_I_isgrBkgDol means usage of the default map for a given Science Window We choose the back ground normalization to be calculated from the shadowgrams from which the pixels affected by the photons from all sources previously detected by ISGRI with a catalog flux in the 20 60 keV energy band higher than 100 cts sec 600 mCrabs were removed brSrcD0L ISDC_REF_CAT ISGRI_FLAG2 5 84ISGR_FLUX_1 gt 100 In principle the set of bright sources taken into account for the background subtraction should be chosen individually for each analysed observation see more details in Section 8 2 3 We have found that some regions of the mask have glue deposits in the void The shadowgrams of strong sources near those glue deposits are not fully correct and create artifacts in the images mostly ghosts The ghost_buster script first included in OSA 9 is called by the analysis script to kill affected pixels from the shadowgrams of the strongest sources in the image If you include too many sources in this ghost_buster algorithm you will also kill too many signal pixels so only include very bright source and do this if you see artifacts in very deep mosaics After the creation of all the individual Science Window ScW images the mosaic image will
55. C tables ISGR GAIN MOD and ISGR OFF2 MOD ISDC IBIS Analysis User Manual Issue 10 1 84 Table 34 Content of ISGR GAIN MOD Data Structure Column Name Description PARI Parameter 1 for energy gain correction PAR2 Parameter 2 for energy gain correction Table 35 Content of ISGR OFF2 MOD Data Structure Column Name Description PARI Parameter 1 for energy offset correction PAR2 Parameter 2 for energy offset correction PAR3 Parameter 3 for energy offset correction To perform a rise time correction for each raw ISGRI event the Rise Time correction table is used ISGR RISE MOD Data Structure see details in Table 36 This table is composed of NUM_ENER lines giving for each incident energy the correction factor corr for a given value of the rise time Table 36 Content of ISGR RISE MOD Data Structure Column Name Description ENERGY Energy at which the gain offset relationship is measured CHANNEL Channel at which the gain offset relationship is measured CORR Rise time correction for a given rise time value 0 127 The rise time itself and the gain offset are kept at the ISGR OFFS MOD Data Structure Table 37 Content of ISGR OFFS MOD Data Structure Column Name Description AGAIN Amplitude Gain AOFFSET Amplitude Offset RTGAIN Risetime Gain RTOFFSET Risetime Offset PIXTYPE Pixel type B 2 2 PICsIT Data Structure PICS ENER MOD is created by the PI
56. CU uox a th te ee a hh A qot ate ee Vo ee qu ha a GE 89 C 6 WOUSDGCRGTOUNG 00 yo kon m hem SG por t Ewa ORS E dodo ox Rie dod 90 GT mage Analysis 29x ox Rm o os x Roos a RO RO RR EDS oO 90 Cr VLSBUUROUE a wha bus Rok A RIS Yos eges 90 C 7 2 BDSROUNGOE donde ha hex ae meses eR AAA BOS ee ee d 93 CLR Spectral Analysis coo zo dox mm DA a a eR REEDS OO 93 C 8 1 UE E EI TE mum 93 CO Timing Analysis 2 cosa m ce m Ge ARSE XLA de OUR Aso up ee e a 93 C 9 1 DICIS EE Lino ue mU RE sch e uera A Red dede deus 93 C 9 2 WAC CRORE o e Doux ood wh a EUR e EIS vos ego 94 0 9 3 Timing Analysis without the deconvolution 94 D List of ibis science analysis parameters ene 96 ISDC IBIS Analysis User Manual Issue 10 1 vii List of Figures 10 lh 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 ISDC IBIS effective areg o 1 023 3 3e ca cR kN 4 a A SOR ORC Y EUR ee 2 Cutaway drawing of the IBIS detector assembly together with the lower part of the collimator A See etes oeste m d rr run ED RN OR C RO Rt ee be ea ha 4 IBIS detector assembly in numbers 22 2 4 Spacecraft amp Instrument Coordinate Systems a aooo 5 The IBIS coded mask pattern white open elements back closed elements 6 The cross section of the support panel ee 7 ISGRI and PICsIT division in modules and submodules ln 8 The schematic view of PICsIT la
57. CsIT Automatic Calibration Analysis and contains parameters for gain and offset correction of PICsIT raw events Presently all the gain values are set to 1 and all the offset values are set to 0 This means that OSA makes use only of the equalization performed onboard by using HEPI LUT No other corrections are applied Content of this Data Structure is given in the Table 38 The values given in the Table 38 are normalized to the average values given by the keywords AVGAIN for average gain value in units keV channel and AVOFFSET for average offset value in keV Table 38 Content of PICS ENER MOD Data Structure Column Name Description PICSIT_Y Y location in the PICsIT layer PICSIT_Z Z location in the PICsIT layer GAIN Gain OFFSET Offset ISDC IBIS Analysis User Manual Issue 10 1 85 B 3 Limit Tables Instrument GTIs depending on HK and other parameters are defined by a limit in a limit table IBIS GOOD LIM see details in Table 39 Table 39 Content of IBIS GOOD LIM limit table Column Name Description PAR NAME Parameter name OBT START Start of validity of the limit values OBT_END End of validity of the limit values MIN_VAL Minimum value allowed MAX_VAL Maximum value allowed GTLNAME Name of the group to which the parameter belongs SUB_ASSEMBLY Identifier of the instrument sub assembly CHECK MODE Modes in which the parameters must be checked B 4 Instrument Background Table 4
58. ELT ISGRI IMA ISGRI SPE and LCR PICsIT analysis GENERAL levelList COR GTI DEAD BIN I BKG I CAT I IMA IMA2 BIN S SPE LCR COMP CLEAN Hd Figure 12 Main page of the IBIS GUI Keeping all the default values you will make an analysis starting from the energy correction level startLevel COR until the image reconstruction level endLevel IMA2 7 The default input catalog CAT refCat ISDC_REF_CAT ISGRI_FLAG gt 0 will be used it contains the sources that were detected by ISGRI in the pub lic data prior to the release of the catalog ISGRI data alone will be processed SWITCH disablePICsIT yes through all the available levels shown in GENERAL levelList within COR and IMA2 No additional user defined good time interval will be applied to the data SCW1 GTI gtiUserlI field is empty which also implies that the next parameter SCW1 GTI TimeFormat is not effective The last parameter SCW1 GTI BTI Names specifies types of problems which should lead to exclusion of the science window from the analysis The detailed description of all types is given in the Section 9 3 The default value is the most conservative and includes all possible categories You are ready to set the parameters specific for imaging Press the ISGRI IMA button at the bottom of the GUI Another box shown in Figure 13 appears With the default parameters displayed in the GUI you will create four different images of the sky corre sponding to four energy
59. ICsIT multiple PM PICS MULE RAW PICS MULE PRP PICS MULE COR Compton single CS COMP SGLE RAW COMP SGLE PRP COMP SGLE COR photon Compton multiple CM COMP MULE RAW COMP MULE PRP COMP MULE COR Spectral Imaging PICsIT single PICS SISH RAW Histogram PICsIT multiple PICS SIMH RAW Spectral Timing PICS SPTI RAW PICS SPTI PRP Histogram A 1 1 Photon by photon mode In this mode Data Structures with similar contents are created for all types of events Data Structures with names finished by RAW contain the information about the event itself See Table 30 for details Data Structures with names finished by PRW and SRW contain some technical information about the structure of the telemetry packet and the Local On Board Time LOBT of the events Table 30 Contest of Photon by Photon Mode Raw Data Column Name Description Event Type DELTA_TIME Delta time to previous event I PS PM RISE_TIME Event rise time describes the shape of the registered I CS CM pulse ISGRLPHA Pulse height in the ISGRI layer I CS CM PICSIT_PHA Pulse height in the PICsIT layer PS PM CS CM ISGRLY Y location in the ISGRI layer I CS CM ISGRI_Z Z location in the ISGRI layer I CS CM PICSIT_Y Y location in the PICsIT layer PS PM CS CM PICSIT_Z Z location in the PICsIT layer PS PM CS CM CAL_FLAG Calibration flag 1 when neither of the events are CS CM calibration ones only in this case the event is used in the
60. OL string DOL of the PICsIT Detector Uniformity model sin gle default ISDC IBIS Analysis User Manual Issue 10 1 102 SCWI1 BKG picsSBkgDOL string SCWI1 BKG picsMUnifDOL string SCW1_BKG picsMBkgDOL string DOL of the PICsIT Detector Background model sin gle default gt DOL of the PICsIT Detector Uniformity model mul tiple default DOL of the PICsIT Detector Background model mul tiple default gt Parameters specific to OBSI pipeline yimage parameters li_sk OBS1_DataMode integer rebin_slope real rebin_arfDol string OBS1_SearchMode integer OBS1_ToSearch integer OBS1_CleanMode integer OBS1_ExtenType integer ISDC IBIS Analysis User Manual Issue Data Simulation mode possible values 0 shadowgrams are treated 1 shadowgrams are simulated default 0 Spectral slope to be used default 2 DOL of the ISGRI arf for rebinning default gt Source search mode possible values for the Science Window analysis 1 search for all catalog sources 2 search for K sources where K ToSearch 3 search for all catalog sources plus for K significant excesses where K ToSearch For all the above when the mosaic is created the software looks for K ToSearch sources default 3 Number of sources to be looked for default 50 Ghost cleaning possible values 1 source model lobes are subt
61. RI and is stopped in a single pixel of the PICsIT layer generating one scintillation flash The energy of the incident photon is derived in each crystal bar from the intensity of the flash recorded in the photodiode The energy resolution of PICsIT is a function of the signal to noise of the event which in turn is governed by factors operating conditions and PIN capacity e PICsIT multiple event Several PICsIT detection units in one submodule were excited during one event generating several scintillation flashes The energy of the primary photon is determined from the sum of the energies of all detected events The position of the incoming photon is attributed to the position of the most energetic event ISDC IBIS Analysis User Manual Issue 10 1 10 e Compton single event Photons arriving in either ISGRI or PICsIT produce secondary photon via Compton scattering detected in another layer The position of the incoming photon is attributed to the position of the most energetic event and the energy is determined as the sum of the detected events energies e Compton multiple event One ISGRI detection unit and several PICsIT detection units in one submodule were excited As in previous cases the position of the incoming photon is attributed to the position of the most energetic event and the energy is determined as the sum of the detected events energies In Fig 9 the efficiencies of the various detection techniques is shown evalua
62. SGRI events in the given time Tbin and energy Ebin ranges For every shadowgram a corresponding efficiency shadowgram is created For pixels active during the revolution switch status ON efficiency falls into two components and is null for the others the first factor takes into account the dead time D of the corresponding module MDU the second factor reflects the efficiency energy dependence LT for the lower energy bins due to the low threshold operation limit such that Eff Tbin Ebin y z 1 D Tbin mdu LT Ebin y z It is this value that is given in the shadowgram efficiency maps The low threshold LT correction is performed using the same energy correction of the COR step and an erf function with time dependent width which reproduces the degradation in energy resolution of the instrument The position of the low threshold is evolving with time as can be seen in the Fig 31 with the ISGRI efficiency being lower than 5096 below this energy As an example for revolutions later than Rev 1000 energies below 22 keV should be ignored This executable also applies two different noisy pixel detection techniques The first one is time based it discriminates every pixel for which the scientific SELECT FLAG equals one even only once over all the ISDC IBIS Analysis User Manual Issue 10 1 64 Low Threshold keV N N A TA N O 00 o TL erp h A 200 400 600 800 1000 INTEGRAL re
63. TO LEVEL Table 11 ibis isgr deadtime parameters included into the main script Name Name Type Description in the main script executable SCW1_veto_mod icDOL string DOL of the IC file for VETO model and width of Compton window default 12 3 2 ibis pics deadtime The executable ibis pics deadtime extracts from the housekeeping data the PICSIT intrinsic dead time of and dead time induced by the fortuitous coincidence with VETO and calibration system Contrary to the ISGRI case the dead time is measured by the on board electronics and we have only to decipher it from the telemetry data 12 4 ibis binning The main function of ibis binning is to split the data into energy and time bins The number of the time and energy bins depend on the purpose of the analysis The user can choose if the binning is done for imaging spectral extraction or light curve production Typically just one bin in time and few bins in energy are chosen for the image production one time bin and many energy bins for spectral extraction many time bins and just few energy bins for timing analysis This step is repeated for each Science Window in the observational group The shadowgram is created for each energy interval Script ibis binning combines the following executables e ii shadow bwild e ip ev shadow build e ip si shadow build 12 4 1 ii shadow build The executable ii shadow build creates shadowgrams of I
64. UDE ISGRI DATA GAPS ISDC IBIS Analysis User Manual Issue 10 1 62 SCWI GTLPICSsIT MergedName string GTIs to be merged for PICsIT default VETO ATTITUDE P_SGLE_DATA_GAPS P_MULE_DATA_GAPS SCW1_GTLSCI SC_Names string Names of spacecraft GTIs to be merged for ISGRI default SCW1_GTLSCP SC_Names string Names of spacecraft GTIs to be merged for PICsIT default SCW1_GTLSCP BTI Dol string DOL of a bad Time interval table GNRL INTL BTI default 12 3 ibis dead This script combine two executables calculating the dead time for ISGRI PICsIT and Compton cases e ibis isgr deadtime e ibis pics deadtime The detector efficiency is divided into the real efficiency and the dead time D which is due to the delay following a photon detection during which another event can not be recorded The observed count rate C is connected with the real count rate C as O 0 1 D The presence of the BGO shielding see Section 3 2 5 calibration source and the Compton coding induces an efficiency loss due to good events which by chance fall in their respective time windows For IBIS the term efficiency is reserved for the real physical detection efficiency The effects induced by Veto calibration source and Compton tagging are considered as additional dead times to be added to instrumental dead time Numerically dead time is calculated as the product of the count rate
65. Y Enckplane EN Calibration Sources C DETX cathode JMX2 DETX cathode Calibration Sources Y 9 X pointing Figure 4 d Spacecraft amp Instrument Coordinate Systems Note that the X axis of the spacecraft is defined by the pointing direction ISDC IBIS Analysis User Manual Issue 10 1 5 Figure 5 The IBIS coded mask pattern white open elements back closed elements ISDC IBIS Analysis User Manual Issue 10 1 Figure 6 The cross section of the support panel The Peripheral Frame reinforces the sandwich panel The mechanical interfaces with the INTEGRAL payload module also provide extra Tungsten shielding to the diffuse background through the gap between the mask edges and the payload vertical walls 3 2 2 The Collimator In order to maintain the low energy response of IBIS despite the dithering needed for SPI the collimation baseline consists of a passive lateral shield that limits the solid angle and therefore the cosmic gamma ray background viewed directly by the IBIS detector in the full field of view up to a few hundreds of keV The tube collimation system is implemented with three different devices e The Hopper four inclined walls starting from the detector unit with a direct interface to the IBIS detector mechanical structure The hopper is not physically connected to the payload module structure e The Tube The Tube is formed by four payload module walls shielded with g
66. allows the paths of interacting photons to be tracked in 3D if the event involves detection units of both ISGRI and PICsIT The application of Compton reconstruction algorithms to these types of events between few hundred keV and few MeV allows an increase in signal to noise ratio attainable by rejecting those events unlikely to correspond to source photons inside the field of view The detector aperture is restricted in the hard X ray part of the spectrum by passive shielding covering the distance between mask and detection plane An active BGO scintillator VETO system shields the detector bottom as well as the four sides up to the bottom of ISGRI Figure 2 shows a cut away drawing of the various components of IBIS except the mask and tube Figure 3 shows the distances between the different parts of the detector assembly Figure 4 shows the spacecraft amp instruments coordinate systems 3 2 The Subsystems 3 2 1 The Mask The IBIS Mask Assembly is rectangular with external dimensions of 1180 x 1142 x 114 mm and consists of three main subsystems the Coded Pattern the Support Panel and the Peripheral Frame with the necessary interface provisions The Coded Pattern is a square array of size 1064 x 1064 x 16 mm made up of 95x95 individual square cells of size 11 2x 11 2 mm The mask chosen for IBIS is based on a cyclic replication of MURA Modified Uniformly Redundant Array of order 53 The properties of the MURA patterns are described e
67. any science window with such a problem e ISGRI RISE TIME indicates that on board cut on rise time is too low so we don t have arf and rmf for this case e BELT CROSSING indicates that belts are seen in VETO or ISGRI count rates e SOLAR FLARE indicates periods where a strong solar affected part of the data e VETO PROBLEM contains periods when VETO had a strange behaviour with a count rate much lower or higher than expected If it is lower then less ISGRI events were killed and hence science count rate is higher Thus user can analyze these data but must not rely on the flux dead time can be wrong Also 2 cases of voltage breakdown are added to this category e IBIS BOOT indicates that IBIS has been restarted from OFF state unexpectedly e MISCELLANEOUS For the moment there are cases where we have problems with the time values and all others are related to the drop of PICSIT counters For the most conservative data analysis use the following value of the SCW1 GTI BTI Names parameter SCW1 GTI BTI Names IBIS CONFIGURATION ISGRI RISE TIME BELT CROSSING SOLAR FLARE VETO PROBLEM IBIS_BOOT MISCELLANEOUS ISDC IBIS Analysis User Manual Issue 10 1 40 9 4 Combining results from different observation groups Read this if you have a set of science windows belonging to different runs for which you have already built images spectra or lightcurves and want to combine the results Section 9 4 1 explains how to c
68. ata Structure Fully Coded Field of View First In First Out Field of View Full Width at Half Maximum Galactic Plane Scan Good Time Interval Graphical User Interface HEPI HV IC IJD ISDC ISOC MCE MDU OBT OG PCFOV PEB PIF PMT PLM RMF ScW SWG TBW TM Hardware Event Processor High Voltage Instrument Characteristics Integral Julian Day Integral Science Data Center Integral Science Operations Centre Module Control Electronics Modular Detection Units On Board Time Observation Group Partially Coded Field of View PICsIT Electronic Box Pixel Illuminated Factor Photomultiplier Tube Payload Module Redistribution Matrix Files Science Window Science Window Group To be written Telemetry xil Glossary of Terms e ISDC system the complete ground software system devoted to the processing of the INTEGRAL data and running at the ISDC It includes contributions from the ISDC and from the INTEGRAL instrument teams e Science Window ScW For the operations ISDC defines atomic bits of INTEGRAL operations as either a pointing or a slew and calls them ScWs A set of data produced during a ScW is a basic piece of INTEGRAL data in the ISDC system e Observation Any group of ScW used in the data analysis The observation defined from ISOC in relation with the proposal is only one example of possible ISDC observations Other combinations of Science Windows e of observations are used for example for the Quick
69. ator you should set some environment variables setenv ISDC ENV directory of 08A sw installation setenv ISDC REF CAT REP BASE PROD cat hec gnrl refr cat 0033 fits source ISDC ENV bin isdc init env csh Note that it is important to ensure that the version of the catalog is at least 0031 gnr1 refr cat 0031 fits because it includes new flags that are used by OSA The latter command executes the OSA set up script isdc init env csh which initialises further environment variables relative to ISDC_ENV Ignore all warnings mentioning ROOTSYS Besides these mandatory settings the optional environment variable COMMONLOGFILE can also be useful By default the software logs messages to the screen STDOUT To have these messages in a file i e common log txt and make the output chattier use the command 4If the setenv command fails with a message like setenv command not found or setenv not found then you are probably using the sh family In that case please replace the command setenv my variable my value by the following command sequence my_variable my_value export my variable In the same manner replace the command source a given script csh by the following command a given script sh notice the leading 5For instance the exit status of the program will now appear ISDC IBIS Analysis User Manual Issue 10 1 18 setenv COMMONLOGFILE common_log txt 6 3 Two ways of launching the a
70. ault gt IJD for the public data default 1 Parameters specific to SCW2 pipeline PICSIT_deco SCW2_cat_for_extract SCW2_racolumn SCW2_deccolumn SCW2_catalog SCW 2 PIF filter SCW2 ISGRL event select string string string string string string string DOL of the MASK decoding fits file default gt Catalog for spectral and lightcurve extraction if empty then it is taken from the imaging result of the Science Window default Name of the column where to get Ra default RA FIN Name of the column where to get Dec default DEC FIN Catalog for PICsIT imaging default filter to apply on the source default CFITSIO event selection string default 33 parameter for bui Iding light curves from PICsIT spectral timing data Parameters for spectra extraction IBIS SI ChanNum integer Number of Channels possible values 1 10 1 take from ISGR EBDS MOD structure default 1 ISDC IBIS Analysis User Manual Issue 10 1 105 IBIS_SI_E_band_min IBIS_SI_E_band_max IBIS_SI_inEnergy Values PICSIT_source_name PICSIT_source_RA PICSIT_source_DEC IBIS_SS_inEnergy Values IBIS_SM_inEnergy Values IBIS_SP_ChanNum IBIS_SP_E_band_min_s IBIS SP E band max s IBIS SP E band min m IBIS SP E band max a IBIS SPS ChanNum IBIS SPS E band min s IBIS SPS E band
71. bands IBIS II ChanNum 4 in the ranges 20 40 40 60 60 100 and 100 200 keV You will let the software look for all catalog sources and up to 50 brightest sources in the field of view 0BS1 Searchmode 3 and OBS1 ToSearch 50 with detection significance higher than 6 for new sources 0BS1 MinNewSouSnr 6 Note that the OBS1_ToSearch parameter is set to a high value to be safely used to detect all sources in the final mosaic image even in the crowded field around the Galactic Center cf Table 19 The position of all the catalog sources will be fitted OBS1_SouFit 0 except for sources with ISGRI_FLAG 2 whose position is known with an accuracy better than 3 arcs where the fixed catalog position will be used Resulting images will be cleaned with the available background maps provided by the IBIS team empty value Remember that in order to fully exploit the improvements made in OSA 10 the analysis needs ALWAYS to be performed starting from COR level as new calibration files have been introduced TIMA2 level is for PICsIT analysis only and there is no difference for ISGRI analysis whether endLevel is set to IMA or IMA2 ISDC IBIS Analysis User Manual Issue 10 1 22 ISGRI IMAGING Ok IBis__ChanNum 4 IBIS_I_E_band_min 204060 10000 IBIS ILE band max 40601002000 IBIS Il inEnergy Values NEN browse OBS1_SearchMode 34 OBS1_Tosearch 50 j OBSi Mincatsousnr 54 OBS MinNewseusnr q3 OBS1 DoPart2 13 O
72. be created 0BS1 DoPart2 1 In this mosaic image the photons belonging to a source are spread around the single central peak resulting in better source location OBS1_PixSpread 1 Now that you have checked all these parameters press Ok the Imaging window disappears and you are back to the main GUI page Press Run to launch the analysis script 7 1 1 Results from the Image Step When the analysis is finished you will find that new files have appeared in your working directory In Figure 14 an overview of the files related to the image reconstruction is given The full description of all files produced at different levels is given in Appendix C As it is shown in Figure 14 there are results for each science window as well as for the overall group Science window results include e Images scw 0051004X0010 001 isgri_sky_ima fits where X 1 5 ISDC IBIS Analysis User Manual Issue 10 1 23 REP_BASE_PROD obs isgri gc sew isgri mosa ima fits isgri mosa resfits isgri srcl resfits isgri catalog fits N N nput Catalog A created ast CAT I step 0051004X0010 001 set of mosaic images CN List of sources CUtput Catalog found in the mE A mosaic image isgri sky ima fits isgri sky res fits i A set of images List of sources W f the Figure 14 Overview of the IMA level products for each energy range five images are produced INTENSITY VARIANCE SIGNIFICANCE and RESIDUAL and EXPOSURE T
73. bs ogid where all the new results will be stored If the pipeline has crashed in general it is safer to restart your analysis from scratch removing the obs ogid directory and restarting from the og_create step In any case we give below a set of recipes that can be useful Because of the group concept you cannot just delete the result you do not like and restart the pipeline All results that were produced in the course of the analysis are linked to the group and should be detached before you relaunch the script To do this you can use the og_clean program that will clean an Observation Group up to the level specified with parameter endLevel All data structures with a level equal or prior to endLevel will be kept while the data structure with a later level will be erased For example to run the spectral extraction SPE level you should clean from the group whatever comes after the BIN_S level as this is the level immediately preceeding the spectral one see Fig 12 og clean ogD L og ibis fits endLevel BIN_S If og clean fails it could be due to the fact that the group was corrupted You should try to fix it with dal_clean program dal clean inDOL og_ibis fits checkExt 1 backPtrs 1 checkSum 1 and launch og clean only afterwards Unfortunately the current version of og clean is very slow In some cases if you know exactly which data structure has to be detached it would be much faster to launch dal detach For example i
74. ca 60 12 1 8 TPLEMLCOPPECON 209 be eo nk Roe Rob Rededoe V 99 ee M Jr ve dea 60 IE PR DER a PIC EON GRE BOX RT Ww de d 0 AUS GEOP eed a a 4 ee EC qe E 61 1294 1 JOLCM OLE 24 a A A a A Rs 61 s AAN 61 12 2 97 iit dala quDS v ooo c poe c A 4n m ree Re RC MORI OE RUN e 62 12 2 44 QUAM ono e HAR HS BS S Ux nor EUN E Ae Goa ORO Xo xo 62 12 2 5 MAME y m ebd eon AA ae eoe BEER LEG one ded yo eR 62 12 2 mde uuo vo oo RUE a A o ed an eU E ak ey HL e 63 12 9 Anis ASG GeRHPUEe ous num d Eno Rh dox EORR EL EUR ROUX OR ON ROR e M Ans 63 W232 4DIBLDIGSLEGOHIMHE doux no aa RE REED EG OR en be Rd RS 64 lu COIS l EPI 64 12 41 Osho oWL DU uud ode Ro oye Oo EU ww Rey de edes 64 12 4 2 sper 3shadoS DUQd eec appa ae wounds OE BERR ED AGS wae Rd ds 65 1243 E nuu deed e a ERA DR a TE So 66 120 E loc EM awh hb ar c ewe ee ee a ee we ek eb 66 12 0 GOS bDuckoroumi OF ornata ce hee Dow eae AAA HE SG Koo eee ed 67 ISDC IBIS Analysis User Manual Issue 10 1 v 12 6 1 A SGC OU ME nu eee Pohenr AR SSO xou a a d 67 1290 29 OnshadoU UE lt a E A ale eee UE IE 68 12T E IEEE 69 L271 CURE ciar A AA AA g 69 We ARS anay io a AE E A EO dao a ER we a 69 12 8 dLSMUDROUE 6 Qe e Som re Rede e ee ee des 71 12 8 2 SUNT ru ss ee ee hem Ha FC mo RUE SUE ad SG a eg dps 74 A OPO NN 74 L284 S SEEHAG escocia aaa o a a A a Poo 75 12 9 Spectral Analysis oo 02g cc teehee ad aa PGox SES dos 75 1291 Spectro Cuak nb ce A E RR A
75. ce Window images are noisy and many fake new sources are detected Searching only the sources from a given catalog will avoid having ghost cleaning for fake sources This mode can be very time consuming if the observed field is crowded such as the Galactic Center region e OBS1_SearchMode 2 The software will look for the K brightest sources in the field where K OBS1_ToSearch They can be either known sources more significant than OBS1_MinCatSouSnr or new sources more significant than OBS1_MinNewSouSnr This mode is useful if you are interested in having a first glance at your field if you are interested in bright sources only or if you run your analysis on large data sets In fact in these cases you would not like to spend most of your time collecting information on weak sources that are not detected in a single Science Window The drawback of this method is that these undetected weak sources can produce ghosts in the mosaic image We recommend you to start the analysis with OBS1_SearchMode 2 with a high OBS1 ToSearch value around 50 especially for the Galactic plane or Centre crowded regions see the sources that are detected and prepare your own catalog of detected sources see section 9 7 Then launch again the analysis with OBS1_SearchMode 3 described below and give your catalog 14Note that the run time is proportional to the number of sources detected ISDC IBIS Analysis User Manual Issue 10 1 34 as i
76. ce an energetic photoelectron is ejected by the atom carrying away most of the original photon energy The Compton scattering takes place between the incident gamma ray photon and an electron in the absorbing material The incoming photon is deflected and it transfers a portion of its energy to the electron The energy transferred to the electron can vary from zero to a large fraction of the initial gamma ray energy In the pair production process the gamma ray photon disappears and is replaced by an electron positron pair The positron will annihilate in the absorbing medium and two annihilation photons are normally produced as secondary products of the interaction Depending on the size of the detector and on the energy of the incoming photon a photon scattered in a Compton interaction can escape the detector or undergo a second interaction The pairs of 511 keV photons produced by the annihilation of the positrons resulting from pair creation can also produce other interactions or escape the detector Both ISGRI and PICsIT record the coordinates of each event registered in the corresponding layer to build up an image The anticoincidence VETO is used to reject background events The coded mask produces a shadowgram Photons from the source and the background are distributed across the entire field of view but cross correlation techniques allow the full image to be reconstituted for the fully coded field of view 9x9 at each pointing For the par
77. ched for sources and cleaned of the source side lobes In this iterative process the source peaks are fitted with the bi dimensional Gaussian and finely located Then the source contribution to the image is modeled in detail and subtracted The images are rotated projected and summed after being weighted with the variance and then searched for further contributions More details can be found in 8 9 12 8 1 ii skyimage ii skyimage deconvolves shadowgrams in the given energy bands for each Science Window using the balanced cross correlation method described above The energy bands should be either the same as in the ibis binning ISDC IBIS Analysis User Manual Issue 10 1 71 Figure 32 SPSF for the IBIS ISGRI telescope or the bands created by the merger of those bands The deconvolution is weighted by efficiency Thus the weighting array W contains efficiency for normal pixels and O elsewhere A search for sources is performed in the deconvolved image The list of sources found is created and the images are cleaned from the PSF ghosts In the deconvolved image the pixel value at the source position is the total source flux in cts sec units It is calculated as if the source was in the fully coded field of view FCFOV One should NOT do any integration in the source region to estimate the flux from the image The source flux estimation given in the source list is slightly different as the source flux is given at the fitted source p
78. ched off NOIS_FLAG Noisy flag In PICsIT pixels cannot be recovered that easy A PICsIT pixel will remain off once killed Only if half of the detector or so will be off pixels will be attempted to turn on The history of the disable pixels can be found in Data Structure PICS FALT STA see Table 33 Table 33 Content of PICS FALT STA Data Structure Column Name Description PICSIT_Y Y location in the PICsIT layer PICSIT_Z Z location in the PICsIT layer OBT_DETECT First Time when the pixel can be declared as noisy OBT_FAULT OBT when the pixel is switched off FALT_FLAG FLAG reflecting the changes of the pixel status Possible values are ON OFF and OFF ON B 2 Calibration Corrections B 2 1 ISGRI In OSA10 the following corrections to the pulse height gains and offsets have been applied see Section 12 1 For E lt 50 keV the gain is modeled with a linear function gPH gPHio agx revol 2 04 7 6 1 1074 x revol oPH oPHi 0 5 65 5 The parameters needed to describe the gain for E lt 50 keV are hard coded in OSA ibis isgr energy and ii shadow build For E gt 50 keV the pulse height gain and offset are modeled as a function of the rise time rt and revolution number gPH o rt gPHzo 1t b t x revol oPHax rt oPH j rt c rt x revol d rt x revol The values for the gain and offset as a function of the rise time are delivered as calibration files in two new I
79. ckground features should be less than the statistical uncertainties so that background removal is not expected to change the result by much On longer time scales mosaic image things can be different especially in the case of a Staring observation in which background features can accumulate and become important To have no background subtraction set SCW1_BKG_I_isgrBkgDol If a bright source is present in the IBIS field of view then it can change the relative normalization fac tor for the background maps To avoid this you should provide to the script a list of bright sources in the FOV This can be done with the parameter brSrcDOL By default all sources previously detected by ISGRI ISGRI_FLAG2 5 with catalog flux in the 20 60 keV energy band brighter than 100 count s 600 mCrab ISGR_FLUX_1 gt 100 are taken into account cf 1 You can check if addition of other bright sources e g the ones seen in the mosaic of your observation to the bright source catalog im proves the quality of the background subtraction in your particular observation Apart from the per sitent bright sources it is also recommended to include in the bright source catalog bright transients which are visible in the FOV and which were active during the period of observation Addition of a source XX to the bright source catalog can be done by changing the filtering of the ISDC reference catalog brSrcDOL ISDC_REF_CAT ISGRI_FLAG2 5 amp amp 1ISGR_FLUX_
80. d as one of the K new sources 8 2 2 Parameters related to the mosaic step The OBS1_SearchMode parameter concerns only images at a Science Window level In the mosaic image the software always looks for K 0BS1_ToSearch sources more significant than OBS1 MinCatSouSnr for catalog sources or OBS1_MinNewSouSnr for the new sources regardless the real number of sources in the field of view Thus if you are working with a crowded part of the sky mainly Galactic plane and Centre you should use a high OBS1_ToSearch number at least 50 There are two ways to calculate the source flux in the mosaic given the original Science Window information e OBS1 PixSpread 0 The whole input Science Window pixel count is put into one output mosaic pixel no spread is done This method optimises the flux and signal to noise ratio SNR evaluation but can sometimes give some undesired effects such as double source peaks e OBS1 PixSpread 1 default value The input pixel count is spread between different output map pixels This method is better for the source position estimate but is less accurate than the previous method for source flux estimation SNR in the new spread mosaic will be lower than in the previous case The source flux in this case is reduced with respect to the weighted mean of individual science windows or mosaic obtained with OBS1 PixSpread 0 It is not feasible to give the general estimate of this flux reduction as it depends on
81. d to a given source and energy band In the example below we create a file 4U1700 377_scwlc fits with all the information on 4U 1700 377 in 20 40 keV energy band The structure of this file is explained in Appendix C 7 Table 55 src collect group og_ibis fitst 1 results 4U1700 377 scwlc fits instName ISGRI select NAME 4U 1700 377 amp amp E MIN 20 In Figure 17 the ScW per ScW lightcurve of 4U 1700 377 in the 20 40 keV band is shown A ligthcurve with a finer time binning can be constructed at the LCR level see Sect 7 3 Note that the count rates are already corrected for instrumental effects such as the off axis transparency of the mask supporting structure 7 2 Spectral Extraction It is not possible to extract the spectrum of only the source you are interested in All sources brighter or compatible with the one you are interested in should be taken into account too Thus it is strongly recommended when you deal for the first time with your data to run the analysis until the IMA2 level as described in Section 7 1 check the results and call ibis science analysis once again to run the spectral extraction part The description of the algorithm used for spectral extraction is given is Section 12 9 1 Launch ibis science analysis and on the main GUI page change Start Level to BIN S and End Level to SPE After that press the ISGRI SPE and LCR button On the screen that appears see Figure 18 you can specify Spectral energ
82. dly influence the results of your analysis You can do this with cp r ISDC_ENV pfiles Removing them instead is not a good solution as they will be missed when running og_create see Sect 7 The system knows what to copy from where thanks to the PFILES environment variable that is also used in FTOOLS Each parameter is characterized with a letter that specifies its type i e q query parameters are always asked to the user h hidden parameters are not asked to the user and the indicated value is used 1 learned parameters are updated with the user s value during the use of the program The GUI is a fast and easy way to change the parameters see section 6 3 1 for details e What are groups and indices The ISDC software makes extensive use of groups and indices While it is not necessary to grasp all the details of these concepts a basic understanding is certainly quite useful As implied by their names groups make possible the grouping of data that are logically connected Groups can be seen as a kind of data container not completely unlike standard directories At ISDC we create separate groups for each pointing in which we store the many different data types produced by INTEGRAL and its instruments The user then only has to care about one file the group many tens of files being silently included Several pointings the Science Window Groups can be arbitrarily grouped into bigger gr
83. e secondary lobes coding noise On the other hand the modulated radiation from PC sources can be reconstructed by extending the correlation procedure with a proper normalization to the PCFOV URA masks also minimize the statistical errors of the reconstructed peaks Since V G x D YD the variance associated with each reconstructed sky image pixel is constant in the FCFOV and equal to the total counts recorded by the detector therefore the source signal to noise is simply S Cs N VCs Cp where C s and Cpg are source and background counts These masks also have nearly equal number of trans parent and opaque elements and therefore offer minimum statistical error in condition of high background typical for the y ray domain However the sensitivity also depends on the detector spatial resolution and an imaging efficiency factor must be applied to this maximum S N to account for this effect Discrete cross correlation to compute sky and variance images can be written _ 2 Sij X CurjuDa Vij gt Gesu Du kl kl where Poisson statistics was assumed This standard deconvolution in FCFOV can be extended in the PCFOV by extending the correlation of the decoding array G with the detector array D in a non cyclic form padding G with 0 elements Since only the detector section modulated by the PC source is used to ISDC IBIS Analysis User Manual Issue 10 1 70 reconstruct the signal the statistical error at the source position and
84. e source ghosts only 8 3 Spectral and Timing Analysis 8 3 1 Spectral Energy Binning With the help of the IBIS_SI_inEnergyValues parameter you can specify the desired energy bins Apart from specifying the energy bins you should also rebin the responce matrix see Section 9 5 for the detailed discussion on how to do this The rebinned response matrix should then be linked to the spectrum you produce This can be done by setting the parameter SCW2_ISPE_idx_isgrResp your_rebinned_matrix fits This parameter defines the name of the response matrix that would be added to the header of the spectrum file Warning This parameter is a hidden one Thus you should either provide the value of this parameter during the script launch ibis_science_analysis SCW2_ISPE_idx_isgrResp your_rebinned_matrix fits or press hidden button and set this parameter on the SPE page 8 3 2 Background Subtraction In spectral and timing analysis you can choose with the help of the parameter SCW2 BKG I isgrBkgDol whether you want to subtract the instrumental background or not similarly to the imaging case We recommend you to use the option that gives the best results at the imaging level smoother image no clear patterns etc See 8 2 3 for more information 8 3 3 Input catalog The single Science Window and mosaic imaging results are merged in the file isgri srcl res fits By default a spectrum and a lightcurve will be created for all sources listed i
85. ea is to use SCW1 ISGRI event select parameter to define your CFITSIO criteria for the phase selection Unfortunately it is not possible to apply this criterion directly to the TIME column and you will have to modify the DELTA TIME column of the third ISGR EVTS ALL extension of the isgri events fits This file is usually write protected so in general you will have to copy all the data related to the science window of interest to a new place and change links In the example below we are working with science window 005100570010 and are interested in AT 20 milliseconds 0 02 s time bins with zero phase at T0 1170 36 in IJD The general selection criterion can be written as Ph1 lt modulus T TO x 24 x 3600 AT x 100 AT lt Ph2 Here T and TO are expressed in days AT in seconds and phase period is split into 100 intervals i e the phase written to column DELTA TIME changes from 0 to 99 In our example it will look like cd REP BASE PROD rm r scw mkdir scw mkdir scw 0051 cd scw 0051 cp directory of local archive scw 0051 005100570010 001 ln s directory of local archive scw 0051 rev 001 chmod w 005100570010 001 cd 005100570010 001 chmod w isgri_events fits gz fcalc isgri_events fits gz 3 isgri events 1 fits clname DELTA TIME N expr TIME 1170 36 24 3600 0 02 100 0 02 gzip isgri_events_1 fits mv isgri_events_1 fits gz isgri_events fits gz chmod w isgri_events fits gz cd chmod
86. ed directly with the lightcurve But for it successful work the REF BASE PROD variable should be set and point to the place in which there is an ic directory e g directory of ic files installation ic See more details on barycent tool in the Data Analysis section of 1 9 10 Alternative Timing Analysis Read this if you are interested in extracting lightcurves on smaller time bins i e down to about 0 1 sec than the ones allowed by the standard tool 9 10 1 ii light The standard lightcurve extraction tool ii lc extract called within the general analysis script builds shad owgrams for each requested time and energy bin Thus this program is quite time consuming and it is not recommended to use it with time bin less than about 60 seconds Besides be aware that the higher the number of total bins is the higher is the time and space needed The i light tool not called in the analysis script but available as a stand alone tool uses a different algorithm the lightcurve is extracted not via the shadowgram creation but with the use of the Pixel Illuminated Fraction PIF This allows to extract lightcurves up to a time bin of about 0 1 sec This is not the official ISDC IBIS Analysis User Manual Issue 10 1 46 lightcurve extraction tool and should be used mainly to check relative variability of bright sources within a given Science Window rather than for a long term absolute flux estimate Note that to be able to run zz light yo
87. er Dol of the PIF or of the index of PIF default Dol of the ISGR DEAD SCP default DOL of the isgri off axis corrections default DOL of the background maps default Time bin in seconds possible values 0 1 10000 default 100 Number of energy channels possible values 1 10 default 2 List of low energy boundaries default 15 40 List of high energy boundaries default 40 300 Do only detector light curve default NO DOL of the index of pixels switches list default DOL of the index of noisy pixels default Type of data 0 ISGRI comprised between 0 and 5 default 0 DOL containing column NAME of essential sources default Max number of essential sources between 1 and 300 default 3 Discard equal time photons default NO Verbosity of output 0 min verbosity 5 max verbosity default 2 ISDC IBIS Analysis User Manual Issue 10 1 81 A Low Level Processing Data Products A l Raw Data Table 29 summarizes all Data Structures with the raw events measured by IBIS The description of these Data Structures can be found below Table 29 List of IBIS _ _RAW Data Structures Observing Type of event Raw Prepared Corrected mode Data Structure Data Structure Data Structure Photon ISGRI I ISGR EVTS RAW ISGR EVTS PRP ISGR EVTS COR PICsIT single PS PICS SGLE RAW PICS SGLE PRP PICS SGLE COR by P
88. er and start to produce outputs not triggered by an income photon i e to become noisy If the particular pixel countrate is too high relatively to the module countrate then the on board electronics switch it off In ISGRI case the noisy pixels can recover after being switched off for some time and disabled pixels are periodically reset to check their status In PICsIT case pixels cannot be recovered that easily PICsIT pixel will remain off once killed Only if half of the detector or so will be off an attempt will be made to turn pixels on The current situation is shown on Figure 8 Overall the killed pixels are less than 1 3 2 4 On board Calibration Unit IBIS contains an on board collimated radioactive Na source This allows regular calibration of PICsIT at both the 511 keV line calibration to better than 1 in 4 hours and 1275 keV 1 in 8 hours ISGRI can also use the 511 keV line albeit at lower efficiency Any energy deposits from untagged photons will have an impact of 196 on the overall continuum sensitivity between 100 keV and 2 MeV ISDC IBIS Analysis User Manual Issue 10 1 8 SM1 SM1 SM2 63 m a e poe p t n Z 5 4 c d Y Fi 8 Eres The schematic view of PICsIT layer Each module number is indicated The dotted lines represent the division in semimodules whose number is indicated at the top The black pixels are the killed ones The Y Z coordinates are the IBIS ones bo
89. er parts were updated 10 August 2005 5 01 Minor update of the 5 0 version Section 9 6 was added Sections 9 4 1 9 5 1 and 9 8 were updated Table 43 was updated 15 November 2005 5 1 Update of the Fifth Release Sections 7 1 2 7 2 8 3 9 4 2 9 10 2 12 2 12 9 11 and the bibliography were updated Section 12 9 2 and Table 55 were added 12 January 2007 6 0 Sixth Release Figure 8 sections 5 7 8 1 8 2 3 12 6 11 Appendix D and the bibliography were updated Sections 9 3 9 12 were added 26 September 7 0 Seventh Release Sections 7 8 11 and Appendix D updated 2007 7 February 2008 7 0 Seventh Release Typos correction 10 March 2010 9 0 Ninth Release for OSA 9 0 and ghost_buster description 12 July 2010 9 1 Update in section Timing Analysis without the Deconvo lution 1i_pif parameters 19 July 2010 9 2 Update FOV 12 September 10 0 Tenth Release for OSA 10 0 Fully revised modifications are 2012 in blue 3 September 2014 10 1 Release for OSA 10 1 Update of ARF instances in Table 3 04 SEP 2014 Printed ISDC IBIS Analysis User Manual Issue 10 1 Contents Acronyms and Abbreviations e e Glossary of Terme 8 464 owe x ee a 1 luUprOodacbB ee ea ark ae a Gale e Oe Xue om we I Instrument Definition 2 Scientific Performances Summary 3 lustrument Description ac e r dace ee OSES 3 1 The Overall Design 32 The Sub
90. eristics default 0SA ISDC IBIS Analysis User Manual Issue 10 1 corrDol rebinned_corrDol_ima rebinned corrDol spe rebinned corrDol lc rebinned_backDol_ima rebinned_backDol_spe rebinned_backDol_le GENERAL clobber GENERAL levelList string string string string string string string boolean boolean DOL of the isgri off axis corrections default gt DOL of the rebinned isgri off axis corrections for imag ing default gt DOL of the rebinned isgri off axis corrections for spec trum default gt DOL of the rebinned isgri off axis corrections for lc default gt DOL of the rebinned isgri back corrections for imaging default DOL of the rebinned isgri back corrections for spec trum default gt DOL of the rebinned isgri back corrections for lc default gt Clobber existing output data default YES List of all levels default COR GTI DEAD BIN I BKG I CAT I IMA IMA2 BIN S SPE LCR COMP CLEAN Parameters to define which part of data should be analyzed SWITCH disablelsgri SWITCH disablePICsIT SWITCH disableCompton SWITCH osimData boolean boolean boolean boolean Disable ISGRI analysis possible values YES NO default NO Disable PICSIT analysis possible values YES NO default YES Disable Compton analysis possible values YES NO default YES Data are from simulator
91. et al 2003 A amp A 411 L189 A Goldwurm 1995 Exper Astron 6 9 A Goldwurm et al 2000 AIP 510 703 A Goldwurm et al 2001 Proc of 4th INTEGRAL Workshop ESA SP 459 p 497 Goldwurm A David P Foschini L et al 2003 A amp A 411 L223 S R Gottesman amp E F Fenimore 1989 Applied Optics 28 4344 G K Skinner R M Rideout 1995 Imaging in High Energy Astronomy 177 182 Walter R Favre P Dubath P et al 2003 A amp A 411 L25 Lebrun et al 2012 in preparation Grinberg V et al 2011 AcPol 51b 33 ISDC IBIS Analysis User Manual Issue 10 1 110
92. extraction i e the LCR level you can still run ii light following the instructions below We give an example of the shell script that launches ii_light for all Science Windows of your group OGID from a particular revolution 0051 in example below cd REP BASE PROD obs OGID setenv run 0051 foreach file scw run swg_ibis fits echo file ii_light inSwg file num_e 4 e_min 20 40 60 100 e_max 40 60 100 200 delta_t 10 outLC file h lcr fits ISGR SRC LCR IDX tpl GTIname MERGED_ISGRI context scw run rev 001 idx isgri_context_index fits idxSwitch scw run rev 001 idx isgri_pxlswtch_index fits idxNoise scw run rev 001 idx isgri_prp_noise_index fits backDol rebinned_back_ima fits corrDol rebinned_corr_ima fits pifDOL file h isgri_pif fits source selectDol onlydet no tee out log end As a result of this script you will have in each scw run directory a file lcr fits with 4 lightcurves in 20 40 40 60 60 100 100 200 keV energy bands with 10 seconds binning delta t 10 The sources for which a lightcurve is extracted are the ones for which a PIF was created at the SPE level i e specified in SCWSA cat for extract see Section 7 2 9 10 3 Merge the ii light results from different Science Windows If you want to merge in one file all the lightcurves provided by ii light for a given source you can use the lc_pick tool as shown in Section 9 4 2
93. f you run your analysis till SPE or LCR level and would like to produce a mosaic image afterwards you do not have to clean the group deleting all your results but just have to detach ISGRI SRCL RES data structure note that with the option delete y all files with this data structure will be deleted dal detach og ibis fitsN pattern ISGR SRCL RES delete y 9 2 Make your own Good Time Intervals Read this if you are interested in selecting photons arrived at a particular time period e g in analysis of flares or for phase resolved spectroscopy You should define Good Time Intervals GTIs with the help of the gti user program To create a GTI for IBIS starting on IJD 1322 68 and lasting 1 minute do not forget to convert it into days give the command gti user gti user gti fits begin 1322 68 end length 6 944E 4 group og_ibis fits unit day 151f any executable crashes then it terminates with non zero status The meaning of the status value can be found at http www isdc unige ch integral analysis Errors ISDC IBIS Analysis User Manual Issue 10 1 39 Note that the parameter unit governs simultaneously begin end length and step parameters If unit day then begin and end are considered to be absolute values in IJD If unit sec then begin and end are taken relative to tstart See the full list of gti user parameters in 1 It is also possible to define the GTIs of the fixed length parameter leng
94. files RAW data Then the local on board time is converted into the common on board time OBT and the House Keeping HK parameters into physical units PRP data These steps are done at ISDC and you do not have to redo them In the Appendix A and B you will respectively find the description of the raw and prepared data and also the description of the instrument characteristic files that are used in the Scientific Analysis INTEGRAL data is organized into the so called Science Windows see Introduction to the INTEGRAL Data Analysis 1 for more explanations During the scientific analysis all the Science Windows belonging to the same observation are grouped together to form the Observation Group Figure 10 shows in details the different steps performed by the scientific analysis script ibis_science_analysis This high level script consists of four smaller ones ibis scw1 analysis ibis_obs1_analysis ibis scw2 analysis and ibis obs2 analysis ibis scwl analysis and ibis scw2 analysis work on a Science Window basis while ibis obs1 analysis and ibis obs2 analysis work on the Observation Group basis Each subscript performs the tasks shown in Figure 10 explained in more details in the text below 1 For the time being Compton analysis is not available ISDC IBIS Analysis User Manual Issue 10 1 13 ibis science analysis ibis scw1 analysis i Data Correction i COR ibis_correction E a A Corrected data Good Time Handling
95. g in 11 and 12 Approximately half of the mask cells are opaque to photons in the operational energy range of the IBIS instrument offering a 70 opacity at 1 5 MeV The other 50 of cells are open i e with an off axis transparency of 60 at 20 keV Figure 5 shows the mask pattern The Support Panel includes additional elements to support the code mask pixels providing the necessary stiffness and strength to overcome the launch environment and the in orbit operational temperatures This panel is done from the material known as nomex Its transparency should be taken into account in the data analysis as it absorbs part of the flux Figure 6 shows the cross section of the support panel ISDC IBIS Analysis User Manual Issue 10 1 3 __ Hopper _ CdTe layer SGRI t PICSIT Figure 2 Cutaway drawing of the IBIS detector assembly together with the lower part of the collimator Hopper 3502 ar E L 3400 3198 Lis PLM detectr or bench Not to scale fes 3a Spider 7 MESS S eS 3206 w y m PIT x Figure 3 IBIS detector assembly in numbers ISDC IBIS Analysis User Manual Issue 10 1 Spacecraft amp Instrument Coordinate Systems Z Sun 127 127 SCY 1 4 P amp V 5 1 0 P amp V 1 sz L5 P amp V 6 1 1 PREV 2 Star re tracker L3 P amp V 4 Vill 1047 1025 DET
96. ghtcurve for each source and one light curve for background in all specified energy bands Dead pixel data gaps off axis correction energy low threshold and illumination factors are taken into account The method used is a fit of hyperplane through the cloud of points formed by the number of counts versus PIF fraction for every source In the case of one source this is just a linear regression The intercept gives the background while the slope gives the flux of the source in one fully illuminated pixel Normalization is a number of counts in a perfect detector if source is on axis half of all detector pixels illuminated There are two methods to extract the flux for one source 1 the source flux is extracted considering the source alone 2 the source flux is extracted taking into account that other sources are in the FOV For a faint source in the PCFOV it is important to take into account all bright typically larger than 0 1 Crab sources in the entire FOV whereas to analyse a faint source in the FCFOV it is necessary to consider only bright sources in the PCFOV The sources that need to be considered simultaneously for the lightcurve extraction are the essential sources the DOL to the list is stored in source_selectDol parameter The list however should include the lower possible number of sources defined through the maxessential parameter This is due to the fact that extracting simultaneously the flux of many N sources takes
97. gr rmf grp 0027 fits and has 13 energy bins in its third extension The optimum way to rebin the matrix depends on the source and on what you are interested to study so there is not a general best way to rebin it Nevertheless it is reasonable not to spend time on a fine energy binning where the source is too weak and background contaminated as well as it is better to avoid too narrow energy bins for weak sources extracting a spectrum in wider energy bins from the very beginning is better than extracting it in too fine bins being background contaminated and then rebinning the spectrum afterwards To use rbnrmf you should create an ASCII file with three columns representing minimal and maximal channels and the compression factor In the example below we create the file new bin txt in order to apply ISDC IBIS Analysis User Manual Issue 10 1 43 a compression factor of 16 to channels 10 409 17 7 209 26 keV and ignore all the others This will lead to maximal_channel minimal_channel 1 compression factor number of final bins i e in this example to 25 bins 0 9 1 10 409 16 410 2047 1 To rebin the matrix give the command rbnrmf infile REP BASE PROD ic ibis rsp isgr rmf grp 0025 fits outfile new rmf fits binfile new bin txt As a result of this you now have the rebinned response matrix new rmf fits With the help of fv you can see that the rebinned matrix is saved in the third extension of the file For the
98. h output energy band it creates a model PIF for each source The Pixel Illumination Factor PIF is a number between 0 and 1 which expresses the theoretical degree of illumination of each pixel in the detector plane of coded mask instrument The PIF is calculated on the basis of the position and is normalized to 1 cts pix source fits all source intensities together with a background estimate to the data shadowgrams writes all source estimates to the spectra index Finally i spectra extract writes to the PIF index one mean model per input catalogue source There is a possibility to chose one of several fitting metods The recommended method is iterative imaging like Least Squares fit method 6 In the first step of this method the fit of each source separately in its coded zone is done Next in the second step the calculation of reciprocal source contributions is performed The first step is aimed to decrease the background modelling error influence The second one corresponds to the ghost cleaning Please note that Maximum Likelihood method is not working in standard OSA configuration with isdcmath package In the fitting process the source positions are considered to be exact If the input background map is given then the background map fitting is performed Table 23 i spectra extract parameters included into the main script Name Name Type Description in the main script executable SCW2_ISPE_id
99. has structure similar to input catalog ISGR SRCL CAT Each row of this Data Structure contains the description of a source in the OG FOV If it was present in the input catalog all the input info is copied For each source found during the analysis the new info is added see Table 54 The DETSIG in ISGR SRCL RES is calculated from the results of the mosaic image and the results of the analysis at Science Window level detsig 4 Xdetsig where is for all energy bands and all Science Windows and mosaic image For the FLUX and err_flux of ISGR SRCL RES you have lux fie N Xfluxerr l f fluxerr N where i for all Science Windows and a mosaic image for a given energy band Table 54 New information added to the ISGR SRCL RES Data Structure Column Name Description RA FIN Right Ascension of the fine position of the source DEC FIN Declination of the fine position of the source FIN RD ERR Error of the fine position of the source in RA and DEC SCW NUM number of times that the source was in SCW FOV If SCW NUM C 0 then it is a new source SCW NUM F number of times that the source was found in ScW image OG NUM number of times that the source was found in OG image With the help of stand alone program src_collect it si possible to collect results from different science windows Results are written to the ISGR OBS RES Data Structure see Table 55 Table 55 Content of the ISGR OBS RES
100. he extensions With the help of this index you can easily see which extension contains the spectrum of the source you are interested in To get an average spectrum with a better signal to noise ratio one can sum up spectra of a source from different science windows This can be done with the spe_pick tool In the following example we create a joint spectrum of 4U 1700 377 from all the available science windows included in the og_ibis fits file cd REP_BASE_PROD obs isgri_gc Spe pick group og ibis fits source 4U 1700 377 rootname 4U1700 ISDC IBIS Analysis User Manual Issue 10 1 28 File Edit Tools Help SOURCE ID NAME DETSIG FLAG Select 16A 20A 1E 11 JA Invert Modify Modify Modify Modify J170047 9 414023 4 1469898 01 0 1170356 8 575039 au 1700 377 152391202 o 3170544 5 360502 ox 3492 Ss e masomor o 3170854 6 440602 1 486778E 01 0 1170512 0 361600 ron 317252 3616 1412058601 o Sets REOR ES PTE ES 3172733 2 304807 4U 1722 30 1 152869 01 3173157 4 335005 GX 354 0 2 013769E 01 3173858 3 442700 4U 1735 444 1 133946 01 3174354 7 294443 J 1E 1740 7 2942 1 593859E 01 3174449 0 292106 KS 1741 293 8 074253E 00 HN Goto A Figure 19 List of sources used for the spectral analysis SN As a result two files with spectra of 4U 1700 377 will be created 4U1700 sum pha fits contains the final average spectrum of 4U 1700 377 while 4U1700 single
101. he parameter group equal to index comb 2 fits cd REP BASE PROD obs lc pick source GRS 1758 258 attach n group index comb 2 fits 1 lc GRS1758 1c fits emin 20 emax 40 instrument ISGRI GRS1758 lc fits contains the merged lightcurve of GRS 1758 258 in the 20 40 keV band energy range that of course has to exist in the isgri lcr fits original files cd REP BASE PROD obs spe pick group index comb 2 fits N source GRS 1758 258 rootname GRS1758 instrument ISGRI GRS1758_sum_pha fits the combined spectrum of GRS 1758 258 and GRS1758_single_pha2 fits a file with the four spectra of the initial four Science Windows collected together are created spe pick also cre ates an ARF appropriate for your particular dataset This ARF is written to GRS1758 sum arf fits and GRS1758_single_pha2 fits files The names of the response and ancrfile are inserted in the keyword of the final files so that they are automatically recognised by XSPEC 9 5 Rebinning the Response Matrix Read this if you want to use a spectral binning different from the default one You will also learn how to rebin the response matrix to extract images in more than 10 energy ranges The file REP_BASE_PROD ic ibis rsp isgr_rmf_grp_0025 fits contains the latest full response matrix with 2048 channels With the help of the FTOOLS program rbnrmf you can rebin this matrix according to your needs The default rebinned matrix is REP BASE PROD ic ibis rsp is
102. iations are energy dependent and therefore the user should be careful both with photometric and spectral analysis of sources at large off axis angles 11 2 PICsIT 1 The spectra extraction with the PIF method is not reliable for the moment executable ip spectra extraction The user should extract the spectra from images count rates from intensity maps and errors from sig nificance maps and then convolve them with the RMF ARF ISDC IBIS Analysis User Manual Issue 10 1 56 Part III Data Analysis in Details 12 Science Analysis In the Cookbook you have seen that in order to run the Scientific Analysis you should just launch the main script ibis_science_analysis with a desired set of parameters As discussed in the Overview Section 5 the main script consists of smaller scripts which in turn unify executables with similar tasks for different types of events see Figure 27 In this chapter we describe these small scripts in more detail in order to explain how the main script works and which parameters you have to enter for a proper analysis While describing the executables we describe those parameters which were included into the main script You find in the Appendix the detailed description of the results produced at each step In the Appendix you also find the description of raw and prepared data with which you start the analysis 12 1 ibis correction This script produces corrected Data Structures for all types of the events
103. ible values 0 dead zone pixels will be filled with 0 1 dead zone pixels will be filled with mean detector value 1 no dead zones default 1 IBIS_NoisyDetMethod NoisyPixControl integer 0 gt no Noisy Pixel detection 1 gt use SE LECT_FLAG method default 0 brSrcDOL brPif string DOL of the bright sources catalogue which will be removed from background mean calculation default SCW1_BKG_I_brPifThreshold brPifThreshold real pixels with PIF value higher will be removed from background calculation When 1 bright PIF removal will not be performed possible values 0 1 default 0 0001 ModPixShad ModPixShad integer Minimum number of non illuminated pixels per mod ule possible values 100 500 default 400 12 6 2 ip shadow ubc ip shadow ubc reads raw detector shadowgrams and performs the background correction Also detector dead zones are filled at this step Method to be applied for the pixel value interpolation in dead zones is defined by the parameter method int Expanded intensity and variance shadowgrams are produced as output Table 17 ip shadow ubc parameters included into the main script Name Name Type Description in the main script executable SCWI BKG P picsSUnifDOL picsSUnifDOL string DOL of the PICsIT Detector Uniformity model single SCW1_BKG_P_picsMUnifDOL picsMUnifDOL string DOL of the PICsIT Detector Uniformity model multiple ISDC IBIS Anal
104. ience window individually 17The IBIS data mode can be checked in the archive by selecting IBIS mode column on the page with additional parameters ISDC IBIS Analysis User Manual Issue 10 1 52 The science windows we use in the current example were observed in staring mode so check the staring button SCW1_BKG_P_method defines the way to normalize the background maps to the observed shadowgram before performing the background subtraction 0 means scaling with exposure and 1 means scaling with the average counts value over the whole detector Both generally provide the same results though the second method which serves as default is sometimes a bit better PICSIT_inCorVar defines whether you would like the software to partially correct the variance shadowgram for systematic effects due to the background value 1 or not in order to estimate by yourself the degree of systematics present in the deconvolved maps value 0 PICSIT_outVarian defines whether you would like to have the variance maps in output value 1 or not value 0 Note that the varmosaic tool of HEASOFT needs variance maps to work Return to the main GUI window by clicking on OK Without changing other default parameters you are now ready to run the analysis do so by clicking on Run 10 1 1 Results of PICsIT image analysis In case of a staring the output images are in file picsit_ima fits For each energy range and each type of event single multiple 2
105. igure 22 was produced The 33 millisecond pulsation of the Crab is visible For the details on INTEGRAL absolute timing see Walter et al 2003 13 If your data have many short GTIs e g in the case of telemetry saturation due to a solar flare or when PICsIT is in non standard mode you can obtain spurious results A typical case is finding an 8 sec period in your data due to the fact that the telemetry restart is synchronized with an 8 sec frame When possible compare your results with ii light that is immune to this problem and can reach about 0 1 sec binning 9 12 Phase Resolved Analysis Read this if you want to perform phase resolved analysis There are no special tools in OSA 10 for the phase resolved analysis Below we give some hints on how to apply the existing tools for your needs in different cases In general three cases are possible 1 The time scale you are interested in is bigger than several hours In this case you should just select the Science Windows matching your time selection criteria For this you can use e g the keywords TSTART and TSTOP in the header of swg fits 2 The time scale you are interested in is in the range of seconds to hours In this case the GTI usage is recommended see Section 9 2 Note that if the number of USER GTIs exceed 1000 then the program could become unreasonably slow 3 You are interested in very short milliseconds time scale Currently this case requires lots of manual work The id
106. image binning conditions and is different for each source position The displacement of the center of the mosaic could be enough to change source flux Thus the mosaic created with OBS1 PixSpread 7 1is not suitable for flux estimation It is possible to decide whether you want the mosaic to be created along with the Science Window image reconstruction or if you prefer it to be created later on The mosaic production is controlled by the OBS1_DoPart2 parameter e OBS1 DoPart2 0 The mosaic step is not performed and the imaging part ends after the Science Window based part e OBS1 DoPart2 1 default value The mosaic is done after the Science Window image reconstruction in the same run e OBS1_DoPart2 2 The mosaic is performed for images obtained from different already existing runs see 9 4 1 ISDC IBIS Analysis User Manual Issue 10 1 35 8 2 3 Background Subtraction In the current OSA you have background maps provided by the ISGRI team These maps are created on the base of observations containing only faint sources in their fields of view Background subtraction can be tuned with the help of the SCW1_BKG_I_isgrBkgDol parameter If it is left empty then the background map is taken automatically from the IC files You can in principle provide your own background map which is e g specially calculated for the time period of the analyzed observation As a general guideline for short time scale e g 1 Science Window the ba
107. ime if you specify a list of desired minimum energies with the parameter emin If you have more than one energy range with the same minimal energy then you should use the parameter 1cselect to define the unique energy band otherwise the 1cselect parameter can be omitted 7 3 2 Displaying the Results of the Lightcurve Extraction To easily see the source lightcurve you can open the file 4U1700 377 fits with fv and plot the column RATE with ERROR versus the column TIME whereas to see the background lightcurve you should plot column BACKV with error BACKE versus TIME To display the resulting lightcurve it also convenient to use the curve program from the FTOOLS package lcurve Number of time series for this task 1 ISDC IBIS Analysis User Manual Issue 10 1 31 Ser 1 filename options or file of filenames options filei 4U1700 377 fits 2 Name of the window file for default window Newbin Time or negative rebinning 4 6692607009327 100 Number of Newbins Interval 10 95 take this number from the line above Maximum Newbin No 95 Name of output file default Do you want to plot your results yes Enter PGPLOT device XW PLT gt hardcopy 4U1700 377_1c ps PS PLT gt quit As a result the 4U1700 377_1c ps file was produced and is shown in Figure 21 Note that the count rates are already corrected for instrumental effects such as the off axis transparency of the mask supporting structure Bintime 100 0 s
108. ion To start the analysis go to the working directory REP_BASE_PROD obs picsit_ima and call the ibis_science_analysis script cd obs picsit_ima ibis_science_analysis After a few seconds the main page of the IBIS Graphical User Interface GUI appears as shown in Figure 23 Press Reset button to be sure that you have the default ISDC_ENV parameters For PICsIT there were no major changes since the creation of revision 2 data so you can start directly from the BIN I level startLevel BIN_I The end level for PICsIT image creation should be the default endLevel IMA2 Disable ISGRI analysis by checking SWITCH_disablelsgri button and enable PICsIT by unchecking SWITCH disablePICsIT button PICsIT operates in an energy range 0 175 10 MeV where background subtraction plays a very important role The OSA for PICsIT provides a default set of maps for the background subtraction in certain energy bands selected to optimize the instruments performance By default the software will automatically take subtraction with one set of maps with about 1 7 Ms of integration time The default energy bands are in ISDC IBIS Analysis User Manual Issue 10 1 51 Main Save As Load startLevel cor Reset endLevel maz Bun GENERAL levelList COR GTI DEAD BIN I BKG I CAT I IMA IMA2 BIN S SPELLCR COMP CLEAN Quit Help CAT refCat sisDC_REF_CAT ISGRI_FLAG gt 0 browse hidden SWITCH disablelsgri SWITCH disablePICsIT
109. ip shadow ubc 12 6 1 ii shadow ubc ii shadow ubc reads all raw detector and corresponding efficiency shadowgrams and fills the detector dead zones ii shadow ubc is run in three cases to produce images spectra and lightcurves In the imaging case for each pair of detector efficiency shadowgrams it performs the background correction for the uniform default and non uniform spatial distribution The background normalization is calculated on the base of shadowgrams from which the pixels affected by all sources listed in the brPif catalog more than defined by the brPifThreshold parameter were removed ISDC IBIS Analysis User Manual Issue 10 1 67 As output it produces 3 shadowgrams of larger dimensions corrected expanded shadowgram and corre sponding variance and efficiency shadowgrams Method to be applied for the pixel value interpolation in dead zones is defined by the parameter method int Table 16 ii shadow ubc parameters included into the main script Name Name Type Description in the main script executable ii shadow ubc SCW1_BKG I method cor method cor integer Method to be applied for background removal possible values 0 2 0 no background correction 1 background from IC tree is applied to the whole detector 2 background is treated for each module separately default 2 SCW1_BKG_I_ method int method int integer Method to be applied for the pixel value interpolation poss
110. l per mask element and using a G array convolved with detector the PSF in order to optimize S N for point sources with corresponding normalizations This procedure can be carried out with a fast algorithm by reducing previous formulae to a set of correlations computed by FFT The on axis System Point Spread Function SPSF on the whole FOV for an optimum system and PSF deconvolution is shown in Fig 32 Note the peak and flat level in the central FCFOV the secondary lobes coding noise in the PCFOV and the 8 main ghosts of the source peak in the PCFOV located at distances from the source which are a multiple of the basic pattern Bi The average Point Source Location Error PSLE for an optimum coded aperture system with a defined SPSF depends on the source signal to noise ratio S N as following 1 PSLE R S N The IBIS ISGRI telescope assuming no error in pointing axis reconstruction or other systematic effects can locate a 30 o point like source at better than 1 Absolute error in attitude reconstruction for INTEGRAL is expected to be lt 20 In a standard analysis IBIS events or histograms are binned in detector images which are then corrected for detector and background non uniformity 7 and then processed by an iterative algorithm which decodes cleans and composes sky images For each detector image a sky image and its variance are obtained using the deconvolution procedure and then iteratively sear
111. le 15 imap_rebin parameters included into the main script Name Name Type Description in the main script executable corrDol inpCorrDol string DOL of the isgri off axis corrections default rebinned_corrDol_ima rebCorrDol string DOL of the rebinned isgri off axis corrections for imag ing default rebinned_corrDol_spe rebCorrDol string DOL of the rebinned isgri off axis corrections for spec trum default rebinned corrDol lcr rebCorrDol string DOL of the rebinned isgri off axis corrections for lc default rebinned_backDol_ima rebBkgDol string DOL of the rebinned isgri background corrections for imaging default rebinned_backDol_spe rebBkgDol string DOL of the rebinned isgri background corrections for spectrum default rebinned_backDol_lcr rebBkgDol string DOL of the rebinned isgri background corrections for lc default SCW1_BKG lisgrBkgDol inpBkgDol string DOL of the isgri background model default 12 6 ibis background cor This script combines executables which fill the dead zones of the detectors in accordance with the chosen method creating the extended intensity map Iex Then with the help of the IC background B and uniformity U maps See Section B 4 a corrected intensity map Ieor is produced Iex B Icor U Script bis_background_cor combines the following executables e ii shadow ubc e
112. ls see Figures 28 29 and 30 respectively 58 Overview of the binning background step for Imaging leen 59 Overview of the binning background step for Spectra o e e 59 Overview of the binning background step for Lightcurves o cles 59 ISGRI low threshold position as function of INTEGRAL revolution number 65 IBIS Analysis User Manual Issue 10 1 viii 32 SPSF for the IBIS ISGRI telescope lt 2 2 0 4 5 zt REESE ISDC IBIS Analysis User Manual Issue 10 1 List of Tables 10 tl 12 13 14 15 16 T7 18 19 20 2 22 23 24 25 26 27 28 29 30 31 32 Scientific Parameters of IBIS o co i s 244454 ooo 3 RR RE ees 2 Characteristics of the IBIS Telemetry Formats ees 12 ARF instance number to be USA 30 ibis_isgr_evts_tag parameters included into the main script 000 57 ibis isgr energy parameters included into the main script o o 60 1p_ev_correction parameters included into the main script o 60 gti_create parameters included into the main script o o 61 gti_attitude parameters included into the main script o 0000 eee 61 The gti import parameters included into the main script cler 62 gti merge parameters included into the main script o eee 62 ibis_isgr_deadtime parameters included into the main SCript
113. lt OBS1_CAT_fluxMin fluxMin string Low limit for flux selection in ph cm s default OBS1_CAT fluxMax fluxMax string High limit for flux selection in ph cm s default OBS1_CAT class class string Select the sources by class default OBSI CAT date date string IJD for the public data possible values lt 0 all public 0 all private 20 according to DAY ID date default 1 12 8 Image analysis The IBIS telescope is a device based on a coded aperture imaging system The mask chosen for IBIS is based on a cyclic replication of MURA Modified Uniformly Redundant Array of order 53 expanded to 95 ISDC IBIS Analysis User Manual Issue 10 1 69 pixels The properties of the MURA patterns are described in the papers 11 12 For IBIS the mask is about 1 8 times larger than the detector The most important advantage of such configuration is that for a large fraction of the sky a source projects a complete pattern on the detector the Fully Coded Field Of View FCFOV The part of the sky from which only a fraction of the source radiation directed towards the detector plane is modulated is called Partially Coded Field of View PCFOV The complete field of view of the telescope FOV is therefore composed by the central FCFOV of constant sensitivity and optimum image properties surrounded by the PCFOV of decreasing sensitivity A source outside the FOV simpl
114. lued Lead foils e The additional side shielding on the mask Four strips of 1 mm thick Tungsten provide shielding from the diffuse background in the gaps between the mask edges and the top of the tube walls 3 2 3 Detector The ISGRI CdTe and PICsIT CsI TI detectors are layered with respect to each other with PICsIT below ISGRI with respect to the coded mask and hence the astronomical source e Upper Detector Layer ISGRI ISDC IBIS Analysis User Manual Issue 10 1 7 ISGRI PICsIT composed of CdTe crystals composed of Cs1 crystals 128 32 32 64 16 Figure 7 ISGRI and PICsIT division in modules and submodules Cadmium Telluride Cd Te is a semiconductor operating at ambient temperature 0 20 C is the optimum range With their small area the CdTe detectors are ideally suited to build an image with good spatial resolution The CdTe layer is made of 8 identical Modular Detection Units each having 32x64 pixels see Figure 7 Total sensitive area of the detector is 2621 cm e Lower Detector Layer PICsIT Caesium Iodide is a scintillation crystal The CsI T1 layer is divided into eight rectangular modules of 16x32 detector elements see Figure 7 In each module there are two independent semi module each one with its independent Front End Electronics Total sensitive area of the detector is 2994 cm e Noisy Pixels It is possible that with the time some of the pixels of the detector may become out of ord
115. lutions 848 1090 we recommend to ignore data below 20 keV From revolutions 1090 on we recommend the user to ignore data below 22 keV 6 A problem on board IBIS causes event times to be shifted by 2 seconds under some circumstances this is rare The software tries to correct the data The keyword TIMECORR found in the event files ALL or PRP extensions indicates whether the correction was done If you are doing an accurate timing analysis and your data contains TIMECORR gt 0 please take great care If TIMECORR 1 or 2 the applied correction should be OK If TIMECORR 3 you should better not use these data If TIMECORR 4 contact ISDC 7 The lightcurve extraction ii lc extract is performed by building shadowgrams for each time and energy bin It potentially takes a large amount of CPU time and there is a minimum usable time bin The time bin must be such that the total number of maps in the file isgr corr shad does not exceed 2 GB worth of disk space The product of the number of time bins in a science window and the number of energy bands must be less than about 9942 8 ii pif will crash if the input catalog inCat contains more than 500 sources 9 At large off axis angles the IBIS response is not well known and strongly energy dependent Therefore the user should be careful when analyzing observations performed at large off axis angles above 12 degrees since systematic flux variations might be introduced The systematic flux var
116. ly on the group group og_ibis fits 1 If you have Science Windows belonging to different groups you need an intermediate step Basically you need to create a file an index that points to all the Science Windows you want to co add similarly to the case seen in section 9 4 1 Then this file will be given as input via the group parameter at the place of og ibis fits To create the index make a list of the Science Window groups you want to combine and save it as e g dols txt under REP BASE PROD obs To ensure a proper work of the software give the full path i e your file should look like ISDC IBIS Analysis User Manual Issue 10 1 42 WORKING DIR obs GROUPI1 scw 011901070010 001 swg ibis fits WORKING DIR obs GROUPI1 scw 011901080010 001 swg ibis fits WORKING DIR obs GROUP2 scw 012000360010 001 swg ibis fits WORKING DIR obs GROUP2 scw 012000370010 001 swg ibis fits The first 2 files belong to a run with the og create parameter ogid equal to GROUP while the latter two to a run with ogid equal to GROUP2 WORKING DIR has to be the extensive name of REP BASE PROD WARNING make sure that the lightcurve and spectra result files exist for each Science Window you want to co add isgri_Icr fits and isgri spectrum fits files Then give the command that actually builds the fits file from the ASCII file cd REP BASE PROD obs txt2idx element dols txt index index comb 2 fits Then run lc pick and spe_pick putting t
117. many times you don t want the GUI to pop up each time In such a case set COMMONSCRIPT variable to 1 with setenv COMMONSCRIPT 1 This is automatically done if you use the file created with the help of the Save as button see above To have the GUI back again unset the variable unsetenv COMMONSCRIPT 6 4 Useful to know e How do I get some help with the executables All the available help files are stored under ISDC_ENV help To visualize a help file interactively type tool_name h once your environment is set ie the command which tool name properly returns the path to it e Where are the parameter files and how can I modify them All the available executables for the analysis of INTEGRAL data are under ISDC_ENV bin The corresponding parameter files are stored under ISDC_ENV pfiles par The first time you launch ISDC IBIS Analysis User Manual Issue 10 1 19 a script the system will copy the specific tool par from ISDC_ENV pfiles to a local directory user_name pfiles The parameter file in the local directory is the one used for the analysis and is the one you can modify Tf this parameter file is missing e g you have deleted it the system will just re copy it from ISDC_ENV pfiles as soon as you launch the script again When installing a new version of OSA it is safe to update your local instance of pfiles because some default parameter values may have changed and using the old ones may ba
118. max s IBIS SPS E band min m IBIS SPS E band max m string string string string real real string string integer string string string string integer string string string string List of lower limits of output energy bands default List of upper limits of output energy bands default DOL of the energy values when required default gt Name of the source for extracting PICsIT spectrum default gt RA of the source for extracting PICsIT spectrum default gt DEC of the source for extracting PICsIT spectrum default DOL of the energy values for single events default gt DOL of the energy values for multiple events default Number of Channels possible values 0 300 default 51 List of lower limits of output energy bands single default List of upper limits of output energy bands single default gt List of lower limits of output energy bands multiple default List of upper limits of output energy bands multiple default Number of Channels possible values 1 256 default 1 List of lower limits of output energy bands for SINGLE default gt List of upper limits of output energy bands for SIN GLE default List of lower limits of output energy bands for multiple default gt List of upper limits of output energy bands for multiple default
119. merge ibis dead ibis isgr deadtinte ibis pics dead time T E B gti definition ER COR kw GTI kw HKG Ilevd DEAD kwl ee ee RE dap A d M II OL eS a e generalcatalog tract og ibis E Hed ii skyimage xi rebinne efficiency map DAA level I SC l 3 user catalog gt ip skyimage if staing n0 sew i l or TSGRIcatalog Er i3 rebinned y E sw BIN BKG step for Spectra background wae a i efficiency maps scw ibis spectral analysis E rebinned 1 efficiency maps ip spectra extract i SC I L scw BIN BKG step for Timing round sad efficiency maps e a ibis timing analysis tebinned gt ip st lc extract background md _ ii fe extract ET efficiency maps E ibis clean pa _analysis ibis scwl anal analysis ibis obs1 anal _ analysis ibis scw2 anal analysis ibis obs2 an Composition of the main script ibis science analysis For further descriptions of the BIN BKG steps for the DEAD IMA and BIN S levels see Figures 28 29 and 30 respectively ISDC IBIS Analysis User Manual Issue 10 1 58 Binning backgroud step for IMA ibis binning 3 og ibis ii shadow build vg ite 2 w pixel status ip shadow build ev si 3 EFFLIC file 1 De o 2 BEG IC file ii map rebin rebinned maps ge ibis background cor E og ibis ii shadow ubc 2 Z background modell
120. n this file Spectral lightcurve extraction is time consuming and we recommend you to create an input catalog for spectral and timing extraction as discussed in Section 7 2 The spectrum and lightcurve extraction tools use the source position saved in the RA FIN and DEC FIN columns These are the values computed during the imaging step thus in case you want to use catalog source positions you have to modify them manually In case you prefer ISDC IBIS Analysis User Manual Issue 10 1 37 the catalog positions for all catalog sources you can remove RA_FIN and DEC_FIN columns RA_OBJ and DEC_OBJ are used then with the following commands chmod w specat fits fdelcol infile specat fits 1 colname RA_FIN confirm no proceed yes fdelcol infile specat fits 1 colname DEC FIN confirm no proceed yes chmod w specat fits Important make the file with the catalog read only otherwise it may be corrupted in the course of the analysis ISDC IBIS Analysis User Manual Issue 10 1 38 9 Useful recipes for the ISGRI data analysis In this Section we give a number of recipes that can be useful in the analysis of ISGRI data 9 1 Rerunning the Analysis Read this if you would like to redo part of your analysis e g if your run has crashed or if you want to change some parameters In case you want to re run the analysis with different parameters run og create but this time with a different ogid parameter This will create a new tree under o
121. nalysis 6 3 1 Graphical User Interface GUI When you launch the analysis the Graphical User Interface GUI is launched providing an opportunity to set the values of all desired parameters see Figure 12 On the right side of the panel you see the following buttons e Save as button to create a file storing all parameters as they are currently defined in the GUI as a command line script The file can be executed from the command line to launch the instrument analysis program with the parameters as they were defined in the GUI e Load button to read a previously saved file with Save As that will be used to update all parameters of the GUI with the values defined in the loaded file e Reset button to reset all parameters in the GUI to their default values as they are defined in the parameter file of the instrument analysis program and stored in the ISDC_ENV pfiles directory e Run button to launch the analysis with the parameters currently defined in the GUI e Quit button to quit the program without launching the analysis e Help button to open the help file of the main script in a separate window e hidden button to access the hidden parameters with values defined by the Instrument Team Change them with care 6 3 2 Launching scripts without GUI Instead of using the GUI parameters can be specified on the command line typing name value after the script name If you are running your own scripts that call OSA
122. nergy range Upper bound of the energy range Type of energy band Minimum event rise time channel 0 127 Maximum event rise time channel 0 127 Type of histogram data Shadowgram type ID TE PD PE ID IE PD PE ID IE PD PE ID IE PD PE ID IE PD PE ID IE ID IE ID IE PD PE ID IE PD PE ID IE ID ID PD PE cat extract The catalogue extraction selects the sources in the FOV from the reference catalogue The output Data Structure ISGR SRCL CAT have the same structure as the reference catalogue GNRL REFR CAT see Table 50 Table 50 Content of GNRL REFR CAT Data Structures Column Name Description SOURCE ID DAY ID NAME CLASS RA_OBJ DEC_OBJ ERR RAD SPA MODL ISDC unique source identifier Modified Julian Date of source s first identification One commonly used name for the source source classification code Source right ascension in degrees Source declination in degrees Error radius Model for source spatial extension point disk ellipse square gaussian Bspline etc ISDC IBIS Analysis User Manual Issue 10 1 89 SPA_NPAR Number of parameters for source spatial extension SPA_PARS Parameters for source spatial extension SPE_MODL Model for source spectrum XSPEC syntax SPE_NPAR Number of parameters for source spectrum SPE_PARS Parameters for source spectrum VAR_MODL Model for source intensity variability constant sin burst VAR_NPAR Number
123. new energy calibration can be found at 14 Table 5 ibis_isgr_energy parameters included into the main script Name Name Type Description in the main script executable SCW1ICOR_GODOL GODOL string DOL of the Gain Offset correction table default SCW1_ICOR_riseDOL riseDOL string DOL of the rise time correction table default SCW1_ICOR supGDOL supGDOL string DOL of gain coefficients for 2nd method default SCW1_ICOR supODOL supODOL string DOL of offset coefficients for 2nd method default 12 1 3 ip ev correction The executable ip_ev_correction performs energy correction of the events received by PICsIT in photon by photon mode Single events are corrected for each pixel separately with the use of the pixel dependent gain and offset factors and the pixel independent channel to keV conversion factors avgain and avoffset see Section B 2 for more details energy keV avgain gain PICSIT PHA avoffset offset Multiple events are corrected for gain and offset on board and thus they are simply transferred from channels to keV energy keV avgain PICSIT_PHA Table 6 ip_ev_correction parameters included into the main script ISDC IBIS Analysis User Manual Issue 10 1 60 Name in the main script Name Type Description executable SCW1_PCOR_enerDOL enerDOL string DOL of the energy correction table PICsIT default
124. ng string string string boolean boolean boolean string RT correction level increasing from 0 to 2 If 0 no RT correction 2 RT drift included into corrections 1 de fault value default 1 Probability of shot time decay default 0 0001 DOL of the energy correction table PICsIT default Cleaning of cosmic ray induced events possible values 0 No 1 Yes default 1 DOL of the IC file for VETO model and width of Compton window default DOL of the index of noisy maps default gt index of Low Threshold default DOL of the dead time data structure default DOL of the good time interval data structure default gt DOL of the PICsIT Context Tables default DOL of the hepi lut default Divide by efficiency Do not touch it default no Remove bad pixels Do not touch it default yes flatten modules Do not touch it default no DOL of the ISGRI detector uniformity possible values DOL for a specific model no uniformity correction gt DOL is taken from the IC tree default ISDC IBIS Analysis User Manual Issue 10 1 101 SCW1_BKG LisgrBkgDol string DOL of the ISGRI background model possible values DOL for a specific model no background subtraction gt DOL is taken from the IC tree default SCWI1 BKG I method cor integer Method to be applied fo
125. nput for the analysis CAT_refCat usrcat fits WARNING When using OBS1_SearchMode 2 the position of sources detected in the single science window and associated to catalog sources with ISGRLFLAG 2 is assigned to the pixel centre instead of being fixed to the catalog position as it should This problem is not present with OBS1_SearchMode 1 or 3 since in this case the catalog position is used when no fitting is requested see also Sect 11 e OBS1_SearchMode 3 The software will look for all the catalog sources regardless of their detection level i e not using the OBS1 MinCatSouSnr parameter plus for K significant excesses more significant than OBS1_MinNewSouSnr where K OBS1 ToSearch up to a maximum of K sources All these sources will be saved in the final isgri_sky_res fits file if their detection significance is positive but see also discussion on OBS1_NegModels in Section 8 2 4 This mode is very efficient in cleaning the ghosts of all the sources in the field of view It is of course more time consuming since a model is created and deconvolved for each given source We suggest that you should use this mode either with your own catalog built from the previous run with OBS1_SearchMode 2 see above or if no personalised catalog is available using the ISDC cat alog with only the sources that have been detected by ISGRI ISDC_REF_CAT ISGRI_FLAG gt 0 see above Any bright source out of the catalog new or forgotten will be detecte
126. nsmitted with far higher time resolution but without imaging information Thus their usefulness is limited to observations of very strong sources where the source countrate dominates the background The time resolution and the number of energy channels for this spectral timing data can be commanded from ground The time resolution can take values between 1 and 500 ms the current default is 16 ms and eight energy channels In Table 2 the properties of all the modes are summarized ISDC IBIS Analysis User Manual Issue 10 1 11 Table 2 Characteristics of the IBIS Telemetry Formats Detector Image Timing Spectral Observing Mode Resolution Resolution Resolution pixels channels ISGRI photon by photon 128x128 61 035us 2048 PICsIT Photon by Photon 64x64 64us 1024 Spectral Imaging 64x64 lt 730 min 256 Spectral Timing None 1 500ms 2 8 ISDC IBIS Analysis User Manual Issue 10 1 12 Part II Cookbook 5 Overview In this Section an overview of the analysis of IBIS data is given Each photon detected by IBIS is analyzed with the on board electronics and tagged with the arrival time type ISGRI PICsIT Compton etc energy position etc according to the operation mode i e photon by photon standard calibration etc These data are then sent to ground in telemetry TM packets During Pre Processing the TM packet information is deciphered and rewritten into the set of FITS
127. o know which type of image and which energy band correspond to a given extension you can either check in the header of the isgri sky ima fits file extensions or check the first extension of the file an index summarizing the file content In Figure 15 the column highlighted in green was added by hand to identify the corresponding extensions of the file More details on index concept are in 1 e Detected source list scw 0051004X0010 001 isgr sky res fits where X 1 5 list of the sources detected in each energy range with reconstructed RA DEC flux error and signifi cance Observation group results include e Image isgri mosa ima fits The structure of this file with the mosaic images is similar to the one of isgri sky ima fits but instead of residual maps you have the exposure ones e Detected source list isgri mosa res fits list of the sources detected in the mosaic image in each energy range with reconstructed RA DEC flux error and significance The single science window and mosaic results are merged in the file isgri_srcl_res fits This file contains all the sources from the isgri catalog fits plus all the new sources with the information on their fitted position fluxes and detection level You find more details on the structure of the output files in Section C 7 1 8 Note that systematic errors are not included in the calculation of the detection significance DETSIG The intensity image from which all photons att
128. obs GROUP1 scw 011901080010 001 swg_ibis fits WORKING DIR obs GROUP2 sew 012000360010 001 swg ibis fits WORKING DIR obs GROUP2 sew 012000370010 001 swg ibis fits The first 2 files belong to a run with the og create parameter ogid equal to GROUP1 while the latter two to a run with ogid equal to GROUP2 WORKING DIR has to be the extensive name of REP BASE PROD WARNING make sure that obs scw 001 isgri sky ima fits files exist in all the Science Windows you mention otherwise the merging will not work Then give the command that actually builds the fits file from the ASCII file cp dols txt REP BASE PROD obs GROUP1 cd REP BASE PROD obs GROUP1 txt2idx element dols txt index index comb fits The file index comb fits is created and you can look at it with fv In the first extension you have 4 rows each row has the link to a given swg_ibis fits file What you need to do now it to let the software know that it has to use this particular set of Science Windows for the analysis You do this by pointing og ibis fits to this file This has to be done because no matter what level of the scientific analysis you are performing the software will analyse the Science Windows pointed to by og_ibis fits Replace the first row of og ibis fits with cd REP BASE PROD obs GROUP1 ftedit og ibis fits MEMBER LOCATION 1 index comb fits fdelrow og_ibis fits 1 2 1 N Y rm isgri_catalog fits With the fdelrow command you detach f
129. ombine all the existing images in a final mosaic while Section 9 4 2 shows how to merge different lightcurves and spectra 9 4 1 Creating a mosaic from different observation groups Suppose you want to analyse 5 Science Windows and are not interested in the final mosaic You create the group with og create and then you launch the analysis till the imaging step but without the mosaic step i e from COR till IMA with OBS1 DoPart2 0 see 8 2 2 An image is created per Science Window but you do not have the overall final mosaic If you then change your mind and decide that you want the mosaic all you have to do is move in the working directory REP_BASE_PROD obs xxx and relaunch the ibis_science_analysis command with startLevel IMA endLevel IMA and OBS1_DoPart2 1 This is relatively simple because all the Science Windows belong to the same group so combining the results is trivial But if this is not the case i e if you have run different sets of analysis each one with its own og create command then you need to make some intermediate steps 0 You basically need to create a file that points to all the Science Windows you want to co add We call this file an index To create an index make a list of the Science Window groups you want to combine and save it as e g dols txt To ensure a proper work of the software give the full path i e your file should look like WORKING DIR obs GROUPI1 scw 011901070010 001 swg_ibis fits WORKING DIR
130. ombines all available information for photon by photon events from dif ferent instruments during a given time interval Table 61 Content of the GNRL EVTS LST Data Structure Column Name Description DETY Y location in the detector layer offset from center DETZ Z location in the detector layer offset from center ENERGY Energy deposited by the event EVNT TYPE Type and origin of event bit coded TIME Time of event in INTEGRAL Julian Date units ISDC IBIS Analysis User Manual Issue 10 1 94 TIMEDEL Uncertainty of time stamp DEADC Dead time correction factor BARYTIME_N Barycenter time for source number N PIF_N Pixel Illumination Factor for source number N AREASCAL_N Nominal effective area for source number N GNRL EVTS GTI Table 62 contains good time intervals for selecting events Table 62 Content of the GNRL EVTS GTI Data Structure Column Name Description START IJD of start of the GTI STOP IJD of end of the GTI OBT_START On board time of start of the GTI OBT_END On board time of end of the GTI UTC_START UTC of start of the GTI UTC_END UTC of end of the GTI ISDC IBIS Analysis User Manual Issue 10 1 D List of 2bis_science_analysis parameters Table 63 ibis science analysis parameters description Query pa rameters are marked with bold font Name Type Description General parameters ogDOL string DOL of the Observational Group to be analyzed defa
131. on issue are given in Section 8 2 3 while a set of miscellanea on imaging parameters is given in Section 8 2 4 8 2 1 How to choose the source search method in the Science Window analysis Basically the idea is that you can either let the software look for the excesses in the field or you can tell the software to look for sources from a given catalog This catalog can be either the one provided by ISDC CAT_refCat ISDC_REF_CAT from which you can extract e g only the sources that have been detected by ISGRI ISDC REF CAT ISGRI_FLAG gt 0 or a catalog made on your own see section 9 7 to create a catalog on your own The number of sources that are detected in an image is important because detecting a source means also removing its ghosts from the images see section 7 1 The source search method is defined with the parameters OBS1_SearchMode and OBS1 ToSearch These parameters allow you the following possibilities e OBS1_SearchMode 0 This mode was developed for testing purposes and is not recommended for scientific use e OBS1_SearchMode 1 the software will look for all the sources of the input catalog that are in the field of view regardless of their detection level i e not using the OBS1_MinCatSouSnr parameter If the source gives a positive detection then the relevant results are saved in the isgri_sky_res fits file but see also discussion on OBS1_NegModels in Section 8 2 4 This mode can be useful in case your Scien
132. oordinates of the source for which a spectrum will be extracted Since PICsIT operates in an energy range with a few sources this executable works for one source only For each output energy band it creates a model PIF for the source The Pixel Illumination Factor PIF is a number between 0 and 1 which expresses the theoretical degree of illumination of each pixel in the detector plane of a coded mask instrument The PIF is calculated on the basis of the position and is normalized to 1 cts pix source The present PIF is purely geometrical by taking into account that there is one single source with ideal PIF than the Equation at pag L228 of Goldwurm et al 2003 can be simplified In this case all the pixel counts depending on the PIF values are due to the selected single source That is deviations from the average counts in the observed shadowgrams are due entirely to the source writes the source count rates in the selected energy bands and the PIF Table 24 ip spectra extract parameters included into the main script Name Name Type Description in the main script executable PICSIT source name inName string Name of the source for extracting PICsIT spectrum default gt PICSIT source RA inRA real RA of the source for extracting PICsIT spectrum default gt PICSIT source DEC inDEC real DEC of the source for extracting PICsIT spectrum default ISDC IBIS Analysis User Man
133. osaic image Set it to 2 if you want to produce a mosaic image from different existing runs default 1 Mosaic map center deg default Mosaic map center deg default Mosaic map radius deg default 40 0 0 no flux spread in mosaic default 1 The software detects a catalog source only if its signal to noise ratio is higher than this value default 6 The software detects a catalog source only if its signal to noise ratio is higher than this value default 7 defines whether to fit or not the source position O for fitting source position in ScW fit 1 for fixed source position in ScW fit default 0 Detection Threshold default 3 0 Corrected variance to be used DZNO 12 YES default 1 ISDC IBIS Analysis User Manual Issue 10 1 104 PICSIT_out Varian integer Variance maps in output 0 NO 1 YES default 0 cat_extract parameters see Section 12 7 for more details OBS1_CAT radiusMin OBS1_CAT radiusMax OBS1_CAT fluxDef OBSI1 CAT fluxMin OBS1_CAT_fluxMax OBS1_CAT class OBS1_CAT date string string string string string string real Low limit for the position selection default 0 High limit for the position selection default 20 Column used for flux selection default gt Low limit for flux selection default High limit for flux selection default gt Select the object by class def
134. osaic images in the 20 40 keV energy range In the left image we have shown all catalog sources white boxes and in the right one only the detected ones green boxes The color scale at the bottom gives the significance values Although we used here a square root scaling sqrt that enhances the structure in the low values the background we now have a very clean mosaic image compared to images obtained with OSA versions prior to OSA 9 The issue of spurious new sources detected by the software at the position of the ghosts of true sources is therefore much reduced ISDC IBIS Analysis User Manual Issue 10 1 25 Indeed in a coded mask instrument with a symmetric mask pattern as in the case of IBIS a true point source will cause secondary lobes 8 main ghosts aligned with the detector edges at a distance that is a multiple of the mask basic pattern 10 7 degrees in IBIS ISGRI case cf Figures 5 and 32 The ghosts of sources detected in individual ScW images will be removed from these images and will thus not affect the mosaic image However if a source is too weak to be automatically detected in a single ScW its ghosts are not cleaned they can appear in the mosaic image and even be found by the software as new sources IGR UiSaz9 4d g ie Figure 16 INTENSITY left and SIGNIFICANCE right mosaic images in the 20 40 keV energy band There is an easy way to collect from different ScWs all the information relate
135. osition For each output energy band all images of the same type are combined into one mosaic image A search for the sources in the mosaic image is then performed and a list of sources found is created The current version of software allows you to create the mosaic separately from the main analysis see Section 7 1 for the details The Parameter PixSpread sets whether the source flux is spread or not in the mosaic image No spread mosaic puts the whole input pixel count into one output map pixel It permits better flux and signal to noise ratio approximation as each pixel count and variance is summed without any error On the other hand it can give some undesired effects as double source peaks because of binning In the spread mosaic the input pixel count is spread between some number of output map pixels This method is better for source position recovery but not so good for source flux estimation because of the source peak height reduction Furthermore neighbouring pixels in the individual Science Window images are correlated and correct spread variance calculations should take this into account But as exact calculation of the covariance matrix is too heavy for on line analysis the approximative variance formula is used The ti skyimage parameters are given in the Table 19 Table 19 ii skyimage parameters included into the main script Name Name Type Description in the main script executable ISDC IBIS
136. ount the rise time information of the signal The executable ibis isgr energy performs a rise time correction for each raw ISGRI event using the ISGRI rise time correction table Section B 2 The corrected energy is given in keV ISGRI ENERGY and the corrected rise time ISGRI PI is the row number used in the IC file The correction is done by rescaling the measured spectra in accordance with the observed rise time rt so that the corrected event corresponds to the deposited energy Also the temperature and bias corrections are done at this step The ISGRI spectral gain has been observed to decrease with time In OSA9 the description of the gain drift was based on IREM counters integrated over time to take into account the solar flares However this correction proved to be not stable along the whole mission In OSA10 in order to stabilize the instrument response across the whole mission a refined dependence of the gains offsets correction with the measured temperature of the different MDU has been introduced A similar correction was performed also in OSA versions later than OSA 7 assuming however a constant AT between the different modules which is not a correct assumption along the mission The new OSA10 calibration results in an increased stability of the W and Na line positions along the mission and in a minor dispersion of Crab and background spectra along the entire mission compared to previous OSA versions More details on the
137. oups the Observation Group to select data very efficiently according to the user s needs Indices are a special kind of groups which differ only in the fact that all the the data sets they contain are similar and that the indices know the properties of the data sets they contain Indices are a kind of poor man s database For example an imaging program creates several images of different types flux map significance map in different energy bands These images are stored in an index in which the image type and energy band information is replicated ISDC software is then able to select very efficiently the needed images The user can also make use of the indices just by looking at the index for instance using fv the user can identify immediately the content of each image e Why do I sometimes have to add a 1 after a FITS file name A FITS file can have many extensions and sometimes it is necessary to specify as input to a given pa rameter not the file name alone file fits but the extension too file fits 1 or file fits 2 etc The file name with a specified data structure extension is called a Data Object Locator DOL When you modify the parameter file itself see above or use the GUI the extension will be cor rectly interpreted in the file fits 1 case On the command line though the normal CFITSIO and FTOOLS rules apply i e you have to specify it as one of the following file fitsl 1 file fits 1 file fits 1
138. pectral extraction then the file with PIFs of strong sources is not done so no strong source subtraction is done in spectral extraction If you really want to do step SPE or LCR without having done before the step BKG_I then you have two possibilities lSspecat fits has to be of the ISGR SRCL RES type meaning that it has to be created by the imaging step with OBS1_DoPart2 1 since this file is created at mosaic stage See section 7 2 to learn how to go from the imaging result file isgri_srcl_res fits to your specat fits to avoid software crash ISDC IBIS Analysis User Manual Issue 10 1 33 1 there is no strong source in the FOV In this case everything is OK 2 you have to run at least BKG_I and BIN_I for example with just one energy band to save time 8 2 Imaging Source detection is an important and delicate process as the background and all the sources especially the bright ones in the field of view will have an impact on it Because of this intrinsic complexity of the instrument there are different options as far as source search and background correction are concerned The choice of the best method to use for a given case may require a bit of iteration on your side In the next two paragraphs we describe the parameters involved in the source search along with some practical advices The single Science Window case is treated in Section 8 2 1 while the mosaic image case in Section 8 2 2 Comments on the background subtracti
139. pectrum of 4U 1700 377 saved to file 4U1700_spe ps is shown in Figure 20 In the very same manner you can sum up the spectra for all the sources of the input catalog specified in the SCW2 cat for extract parameter Usage of spe pick for spectra created in different observation groups is explained in Section 9 7 3 Lightcurve Extraction After you have done the spectral extraction you may want to produce a lightcurve for the same sources Stay in the working directory SREP BASE PROD obs isgri gc and call the ibis science analysis script again On the main GUI window see Figure 12 change both Start Level and End Level to LCR and press the ISGRI SPE and LCR button The GUI shown in Figure 18 will appear Note that to extract the lightcurve for a source you need the Pixel Illuminated Fraction PIF map Such a map is created during the spectral step that we have just run This means that at this stage you can extract the lightcurve only of the sources for which a spectrum has been created already So leave SCWS 2 cat for extract to point to your specat fits By default for each source from the input catalog specat fits in our example four lightcurves in 20 40 40 60 60 100 and 100 200 keV energy bands with 100 sec time bins will be created You can change these values in the GUI The lightcurve extraction is performed by building shadowgrams for each time and energy bin Hence this step is quite consuming in processing time and di
140. pha2 fits stores all the original spectra of 4U 1700 377 that were averaged up The corresponding Ancillary Response File ARF which contains the energy dependence of the effective area of the instrument is also produced and written to the 4U1700 sum arf fits and 4U1700 single arf2 fits files Note that the correct ARF is automatically chosen by the program from the list displayed in Table 3 and in case your observation spans more than one epoch several ARFs are averaged up to produce the best ARF for your particular dataset 7 2 2 Displaying the Results of the Spectral Extraction The ISGRI systematics are typically of the order of 1 We add this explicitly to the 4U1700 sum pha fits file with the command below cd REP BASE PROD obs isgri gc fparkey 0 01 4U1700 sum pha fits SYS ERR add yes One can now analyse the average spectrum with XSpec as xspec cpd xw data 4U1700_sum_pha fits setplot energy ign 300 x x model cutoffpl fit plot ldata delchi ISDC IBIS Analysis User Manual Issue 10 1 29 Table 3 ARF instance number to be used Period Revolution interval ARF instance XX isgr_arf_rsp_00XX fits 1 1 63 31 2 64 135 32 3 136 254 33 4 255 370 34 5 371 481 35 6 482 635 36 7 636 750 37 8 751 800 38 9 801 900 39 10 901 1000 40 11 1001 1120 Al 12 1121 1190 42 13 1191 1244 43 14 1245 1298 44 15 1299 45 hardcopy 4U1700 spe ps The resulting total s
141. pixels so only include very bright sources and do this if you see artifacts in very deep mosaics Table 21 ghost busters parameters included into the main script Name Name Type Description in the main script executable SCWI BKG busters mask maskmode string Model of the mask areas to be ignored SCWI1 BGK busters src sourcecat string Input source catalog ISDC IBIS Analysis User Manual Issue 10 1 74 12 8 4 ip skyimage ip skyimage performs deconvolution of the shadowgrams with the use of the balanced cross correlation method described above for more detailed explanations see Goldwurm et al 2003 10 The weighting array W corresponds to the efficiency map The values of the decoding G array are taken from the IC file The ip skyimage parameters included into the main script are given in the Table 22 Table 22 ip skyimage parameters included into the main script Name Name Type Description in the main script executable PICSIT det Thr det Thr real Detection threshold for the automatic source location PICSIT inCorVar inCorVar integer Corrected variance to be used 0O NO 1 YES PICSIT_outVarian outVarian integer Variance maps in output 0O NO 1 YES PICSIT deco maskDeco string DOL of the decoding pattern of PICsIT mask 12 9 Spectral Analysis 12 9 1 i spectra extract ii spectra extract reads the shadowgram for each input energy band For eac
142. r background removal possible values 0 no background correction 1 background from IC tree is applied to the whole detector 2 background is threaded for each module separately When using 1 or 2 brPif and brPifThreshold pa rameters are taken into account default 1 brSrcDOL string DOL of the bright sources catalogue which will be removed from background mean calculation default 18DC REF CAT ISGRI FLAG O amp amp ISGR FLUX 1 100 SCW1_BKG_I brPifThreshold real pixels with PIF value higher will be removed from background calculation When 1 bright PIF removal will not be performed possible values 0 1 default 0 0001 SCW1_BKG_L pif string filename of the pif in every ScW default SCWI BKG I method int integer Method to be applied for the pixel value interpolation possible values O pixels in dead zones are filled with zeros 1 pixels are filled with mean detector value default 1 tungAtt string DOL of the Tungsten attenuation length fits file default gt aluAtt string DOL of the Aluminium attenuation length fits file default gt lead Att string DOL of the Lead attenuation length fits file default gt SCW1 BKG P method integer Method applied in filling gaps possible values 0 model in cts is normalized by the time of obser vation 1 model in cts is normalized by the mean count value default O SCW1_BKG_picsSUnifD
143. racted from the decon volved image 1 no subtraction default 1 Save exposure residual maps possible values absent 0 3 O or absent no action 1 true exposure maps are saved in 4 n extension of isgri_sky_ima fits instead of residual images 2 true exposure maps are saved in the 5 n extension of isgri sky ima fits after the residual images 3 one true exposure map is created for the last energy band and saved in the last extension of is gri sky ima fits default 2 10 1 103 OBS1_NegModels OBS1 FastOpen ISGRI_mask OBS1_deco OBS1_covrMod OBS1_ScwType OBS1_DoPart2 OBS1_MapAlpha OBS1_MapDelta OBS1_MapSize OBS1_PixSpread OBS1_MinCatSouSnr OBS1_MinNewSouSnr OBS1_SouFit PICSIT detThr PICSIT_inCor Var integer integer string string string string integer real real real integer real real integer real integer 0 or absent for no negative models 1 negative models default 0 if 1 then no CommonPreparePars default 1 DOL of the MASK pattern fits file default DOL of the projected decoding pattern fits file default gt DOL of the covariance fits file default Type of Science Window to be treated possible values POINTING SLEW OTHER ANY 2 default POINTING if 1 or absent do mosaic part Set it to 0 if don t want to produce a m
144. res from different periods should be generated The simplest way to do this is to run the standard ScW by ScW spectral extraction for your source even if the source is not detected in individual ScWs and then use the spe_pick command see Section 9 which among others will produce the exposure weighted average ARF for your particular data set 9 9 Barycentrisation Read this if you want to apply barycentrisation to an extracted lightcurve The tool making such a correction is called barycent Note that it re writes the input file so it may be worth to copy the original file first Below we show an example for 4U 1700 377 Science Window number 011800900010 and observation group identification ogid parameter of og create equal to OGID cd REP BASE PROD obs OGID cp cw 011800900010 001 isgri lcr fits isgri lcr 011800900010 bar fits barycent inCOL TIME outCOL TIME outD L isgri lcr 011800900010 bar fits 2 inDOL auxDOL aux adp 0118 001 orbit_historic fits ra0BJ 255 9865 dec0BJ 37 84414 In the example we have applied barycentrisation to the first energy range of 4U 1700 377 that happens to be in the extension number 2 2 Thus the extension you give as outDOL depends on the source and energy range you need to correct The overview of the content of each extension is in the input file isgri lcr fits i e the first extension GROUPING Note that barycent tool does not use group concept and is us
145. ributed to the detected sources were removed 10 The actual exposure map of the field of view in seconds ISDC IBIS Analysis User Manual Issue 10 1 24 File Edit Tools Help EXTENSION _ IMATYPE CHANMIN CHANMAX JAM em il Figure 15 A part of the GROUPING extension table of an isgri_sky_ima fits file 7 1 2 Displaying the Results from the Image Step It is convenient to look at the images with the help of the ds9 program First create a region file from the catalog using the cat2ds9 program In the example below we create the region file found reg with all the sources found in the mosaic image isgri mosa res fits for the first energy band extension 2 and a region file cat reg with all sources that were in the input catalog isgri_catalog fits cd REP_BASE_PROD obs isgri_gc cat2ds9 isgri_mosa_res fits 2 found reg symbol box color green cat2ds9 isgri_catalog fits cat reg symbol box color white To see the resulting images ds9 REP_BASE_PROD obs isgri_gc isgri_mosa_ima fits 2 region REP_BASE_PROD obs isgri_gc cat reg cmap b scale sqrt scale limits 0 60 zoom 2 REP_BASE_PROD obs isgri_gc isgri_mosa_ima fits 4 region REP_BASE_PROD obs isgri_gc found reg cmap b scale sqrt scale limits 0 60 In Figure 16 you see the INTENSITY left REP BASE PROD obs isgri gc isgri mosa ima fits 2 and the SIGNIFICANCE right REP BASE PROD obs isgri gc isgri mosa ima fits 4 m
146. rom the first extension of og ibis fits row number 2 the first row to be deleted number of rows to be deleted 1 you were shown no keyword values N and l Please note that the images that you intend to merge MUST have the same energy boundaries i e all the SCW maps must have been analysed in the same way You cannot merge a 20 40 keV map with a 30 50 keV one ISDC IBIS Analysis User Manual Issue 10 1 41 you agreed to proceed Y This second row contained the catalog that was created in previous run during CAT step and contain only sources that were in the field of view of science windows from GROUP1 To have a common catalog for GROUP1 and GROUP2 it would be necessary to rerun CAT_I step for the group referring to all science windows of interest You may check with fv that actually the first row of og_ibis fits is indeed index_comb fits Before running the mosaic step please be aware that e If you had previously run the mosaic step you will see that og_ibis fits points to the mosaic output af ter you have deleted a reference to isgri_catalog fits rows 2 to 4 of the first extension are isgri_srcl_res fits isgri mosa ima fits and isgri mosa res fits This will interfere with the new mosaic you are about to launch thus you have to detach these former mosaic results from the group and delete or rename them cd REP BASE PROD obs GROUP1 fdelrow og ibis fits 1 2 3 N Y rm isgri_mosa_ima fi
147. saic creates a mosaic image of all the science windows within an Observation Group and performs a source location Table 26 ip_skymosaic parameters included into the main script Name Name Type Description In the main script OBS2_detThr detThr real Detection Threshold in Sigmas default 3 OBS2_projSel projSel string Selection of projection default STG 12 12 Tools not included in the pipeline 12 12 1 mosaic spec mosaic_spec is a tool that extracts a count spectrum at a given sky position from a set of mosaic sky images Intensity could be measured in a specific or in the most significant pixel or derived from a gaussian fit with free or frozen position and width Note that if the significance of the point is less than five then mosaic spec will assign a non zero value to its quality flag Table 27 mosaic_spec parameters Name Type Description DOL inp string DOL of the group containing the input images default DOL out string DOL of the group containing the output images default EXTNAME string EXTNAME of the input images default ISGR MOSA IMA ISDC IBIS Analysis User Manual Issue 10 1 78 DOL_idx DOL spec ximg yimg ra dec posmode widthmode psf size back allEnergies emin emax string string real real real real integer integer real integer boolean boolean string string
148. sed accuracy for OBT to IJD conversion and vice versa possible values any inaccurate accurate default any Names of spacecraft GTIs to be merged for PICsIT default gt Names of spacecraft GTIs to be merged for ISGRI default gt GTIs to be merged for PICsIT default VETO ATTITUDE P SGLE DATA GAPS P MULE DATA GAPS GTIs to be merged for ISGRI default VETO ATTITUDE ISGRI DATA GAPS DOL of a bad time interval table GNRL INTL BTI default IBIS CONFIGURATION IBIS BOOT ISGRI RISE TIME VETO PROBLEM SOLAR FLARE BELT CROSSING Input BTI names to be considered default DOL of the index of pixels switches list default DOL of the gain offset table default gt DOL of gain coefficients for 2nd method default DOL of offset coefficients for 2nd method default DOL of the rise time correction table default switch on time default rise time correction default ISDC IBIS Analysis User Manual Issue 10 1 100 SCW1_RTdriftCor SCW1_ICOR_probShot SCW1_PCOR_enerDOL SCW1_BIN_cleanTrk SCW1_veto_mod SCW1_BIN_LidxNoisy SCWI1 BIN L idxLowThre SCW1_BIN_P_inDead SCW1_BIN_P inGTI SCW1_BIN_P_PicsCxt SCW1_BIN_P_HepiLut SCW1_BKG_divide SCW1_BKG_badpix SCW1_BKG_flatmodule SCWI1 BKG LisgrUnifDol integer real string integer string string string stri
149. sed to produce this background image RISE_MIN Minimum event rise time channel 0 127 RISE MAX Maximum event rise time channel 0 127 ISDC IBIS Analysis User Manual Issue 10 1 86 C Science Data Products C 1 ibis_correction This script converts photons energy into keV with the help of the calibration data Table 42 summarises the output Data Structures Table 42 List of Data Structures produced at COR level Observing mode Type of event Corrected Data Structure Photon ISGRI I ISGR EVTS COR PICsIT single PS PICS SGLE COR by PICsIT multiple PM PICS MULE COR Compton single CS COMP SGLE COR photon Compton multiple CM COMP MULE COR The content of the level COR Data Structures for the photon by photon mode is given in Table 43 The abbreviations for the events types are taken from Table 42 Table 43 Content the level COR Data Structures for the photon by photon mode Column Name Description Event Type ISGRI_PI corrected rise time for ISGRI TICS CM ISGRLENERGY Deposited energy in the ISGRI layer LCS CM PICSIT ENERGY Deposited energy in the PICsIT layer PS PM CS CM SELECT FLAG Selection flag shows whether the event was 1 CS CM noisy 1 or not 0 C 2 ibis gti This script builds Good Time Intervals from housekeeping data information about satellite stability and data gaps The resulted GTIs are written to the IBIS GNRL GTI see details in
150. significance of the ghost peaks are minimized However to ensure a flat image in the absence of sources detector pixels which for a given sky position correspond to opaque mask elements must be balanced before subtraction with the factor b n n where n is the number of pixels corresponding to transparent elements and n_ to opaque ones for that given sky position This can be written e B Sij 9 Gia jp Wri Dri Big Y Gi uWiaDu k kl where the decoding arrays are obtained from the mask M by G M and G 1 M then padded with 0 s outside mask region and where the sum is performed over all detector elements In the FCFOV we obtain the same result as the standard cross correlation To consider effects such as satellite drift corrections see 7 dead areas or other specific conditions a weighting array W is used to weigh properly the detector array before correlating it with the G arrays The balance array is el C x j Wei el G uk ju We The variance which is not constant outside the FCFOV is computed accordingly 2 Vij 5 Dr A 2 Bj y Dii Gi s Wa since the cross terms G G vanish Note however that when the weights Wp refer to the same pixel in D the terms G W must be summed before squaring see 7 The varying effective area can be calculated by a similar formula and used to renormalize after background subtraction to FCFOV count rates All this can be performed for sampling finer than 1 pixe
151. sk of the Science Window Pipeline is to prepare raw data for the following Scientific Analysis It converts the housekeeping parameters into the physical units and makes some corrections and transfor mations of the raw data that are not included in Pre Processing The Summary of all the prepared Data Structures with scientific information can be found in Table 29 All these Data Structures has the only column OB_TIME with the on board time ISDC IBIS Analysis User Manual Issue 10 1 83 B Instrument Characteristics used in Data Analysis B 1 Noisy Pixels It is possible that with time some of the pixels of the detector start to produce an output not triggered by an income photon i e to become noisy If the particular pixel countrate is too high relatively to the module countrate then the on board electronics switch it off In ISGRI the noisy pixels can recover after being switched off for some time and disabled pixels are periodically reset to check their status Data Structure ISGR SWIT STA with the list of noisy pixel switches in the ISGRI detector layer is produced during the pre processing basing on the rise time information and pixels light curves transmitted see Table 32 Table 32 Content of ISGR SWIT STA Data Structure Column Name Description ISGRLY Y location in the ISGRI layer ISGRI_Z Z location in the ISGRI layer OBT_DETECT First time when the pixel can be declared as noisy OBT_SWITCH OBT when the pixel is swit
152. sk space Note that due to CFITSIO limitations the product of number of energy bins by number of time bins in a ScW should be less than 250 Press Ok the window will disappear and you are back to the main GUI page Press Run 11To read a given extension in XSPEC version 12 you have to specify it in curly or squared brackets depending on the spectral type If you want to examine in XSPEC the spectra produced at scw level you can load them as e g data scw isgri spectrum fitsV 3 or as data XXX single pha2 fits 3 12PIF is a number between 0 and 1 which expresses the theoretical degree of illumination of each detector pixel for a given source in the sky ISDC IBIS Analysis User Manual Issue 10 1 30 data and folded model 0 1 Ls normalized counts s keV o o E m 1 RETI 20 50 100 200 Energy keV Figure 20 Total spectrum of 4U 1700 377 fitted with a cut off powerlaw model 7 3 1 Results of the Lightcurve Extraction Lightcurves are produced for each science window scw 0051004X0010 001 isgri_lcr fits X 1 5 To create a merged lightcurve in the 20 40 keV energy range ie to store in one file all the available lightcurves of a given source use lc pick lc pick source 4U 1700 377 attach n group 08_ibis fits 1 1c 4U1700 377 fits emin 20 emax 40 The result is written to 4U1700 377 fits It is possible to create more than one merged lightcurve at a t
153. systems MN 3 2 1 The Mask o Oe es de a 3 2 2 The Colimator ss cu icord itea mo 3 2 3 ipsc no PC a A We ae 3 2 4 On board Calibration Unit 3 2 5 Veto Shield 2 0 25 6 55644 54a 4 n 4 How the Instrument works 4 1 Event Types 20 3 es E c9 E e eed 4 2 IBIS observing modes cres II Cookbook 5 Overview cuca 4606 Peed ck GE UP ws 6 Gething startad oe x a de beke3 d ae 6 1 Setting up the analysis data 6 1 1 Downloading data from the archive 6 2 Setting the environment 6 3 Two ways of launching the analysis 6 3 1 Graphical User Interface GUI 6 3 2 Launching scripts without GUI 6 4 Useful to know ir cs Ek e m eee ee we 7 A Walk through ISGRI Analysis Tal Image Reconstruction gt s o lt a ce ssaa aoan Ti Results from the Image Step MZ Displaying the Results from the Image Step ISDC IBIS Analysis User Manual Issue 10 1 10 10 11 13 13 16 16 17 18 19 19 19 19 21 21 23 25 iii 1 2 Spectral Extraction o s noo bod odo 9 RRR Ee PAS Ee RR ee Eod 26 re Results of the Spectral Extraction o 28 2 2 Displaying the Results of the Spectral Extraction 29 Ta Liphteurve ESMTAGUOn on xx eco oh ek a DOR ee eee a ee dod 30 Tal Results of the Lightcurve Extraction 31 53 2 Displaying the Results of the Ligh
154. t dead zone pixels will be filled with mean de tector value 1 gt no dead zones SCW2 ISPE MethodFit MethodFit integer Method to be applied for background and source in tensity fitting default 6 SCW2_ISPE_isgrUnifDol isgrUnifDol string DOL of the ISGRI detector uniformity default SCW2 BKG LisgrBkgDol isgrBkgDol string DOL of the ISGRI background model default gt tungAtt tungAtt string DOL of the Tungsten attenuation length fits file default aluAtt aluAtt string DOL of the Aluminium attenuation length fits file default leadAtt lead Att string DOL of the Lead attenuation length fits file default rebinned corrDol lc corrDol string DOL of the rebinned ISGRI off axis corrections for lc default 77 SCW2_BKG _I brPifThreshold brPifThreshold real pixels with PIF value higher will be removed from background calculation When 1 bright PIF removal will not be performed possible values 0 1 default 0 1 ModPixShad ModPixShad integer Minimum number of non illuminated pixels per mod ule possible values 100 500 default 400 12 10 2 ip st lc extract This program builds PICsIT detector light curves and related errors starting from spectral timing data of PICsIT No parameters of this executable are included into the parameter file of the main script ibis science analysis 12 11 Summing up the results 12 11 1 ip skymosaic ip_skymo
155. t IBIS As a result of the og create command the directory REP BASE PROD obs isgri gc is created In this directory you find all you need for the analysis its structure is illustrated in Figure 11 REP BASE PROD obs isgri gc SCW og ibis fits swg idx ibis fits 0051004X0010 001 Observation Group Index of swe_ibis fits Science Window Groups Science Window Group Figure 11 Structure of the directory created with og_create 7 1 Image Reconstruction The first thing to do when you are looking for the first time at your data is to create an image in order to know how the portion of sky you are interested in looks like whether your source is detected and what other sources you should take into account to do spectral and lightcurve analysis in a proper way ISDC IBIS Analysis User Manual Issue 10 1 21 To start the analysis move to the working directory SREP_BASE_PROD obs isgri_gc and call the ibis_science_analysis script cd obs isgri_gc ibis_science_analysis After a few seconds the main page of the IBIS Graphical User Interface GUI appears as shown in Figure 152 r Main Save As Load startLevel COR y Reset endLevel Imaz y Run Quit Help CAT_refCat sISDC_REF_CATIISGRI_FLAG gt 0 browse hidden SWITCH_disablelsgri I SWITCH_disablePICsIT M SCW1_GTI_gtiUserl browse SCW1 GTI TimeFormat io SCW1 GTI BTI Names lBI5_CONFIGURATION IBIS_BOOT ISGRI RISE TIME VETO PROBLEM SOLAR_FLARE B
156. t reads the user GTI table and converts it into a table in ISDC format The user GTI can be defined either in units of OBT IJD or UTC The output is always in OBT The user table can define either bad or good time intervals The output time intervals are always good ones See more details in the Introduction to the INTEGRAL Data Analysis 1 Table 9 The gti import parameters included into the main script Name Name Type Description in the main script executable SCWI1 GTI gtiUser InGti string DOL of the user GTI table there is no user GTI default gt SCWI GTI TimeFormat TimeFormat string Time format in which the user GTI is given possible values IJD UTC OBT default UTC SCW1_GTL Accuracy Accuracy string Used accuracy for OBT to IJD conversion and vice versa possible values any inaccurate accurate default any 12 2 5 gti merge This program merges input GTIs to form a new GTI It is an AND operation a time in the resulting GTI is defined to be good if the time is good in every input GTI The names of the GTIs and the instrument to which the GTI belongs have to be defined as program parameters Table 10 gti merge parameters included into the main script Name Name Type Description in the main script executable SCW1 GTLISGRI MergedName string GTIs to be merged for ISGRI default VETO ATTIT
157. tcurve Extraction 31 8 More on ISGRI relevant parameters noaoae 33 8 1 How to choose the start and end level for the analysis Intermediate levels 33 8 2 WSO uos s eor le he a a nok a 40 Xebonank 8 o bonse ox v x Pedes 34 8 21 How to choose the source search method in the Science Window analysis 34 8 2 2 Parameters related to the mosaic step ln 35 8 2 3 Background Subtraction s ce et se d ed er ek Rom om o Pod 36 8 2 4 Miscellaneous on Imaging een 36 8 3 Spectral and Timing Analysis ee 37 8 3 1 Spectral Energy Binning aac ea ee ee nedi ts 37 8 3 2 Background Subtraction ca as 244668 soo ee ee ee x 37 8 3 3 Input Catalog e oce to ee ee eV Sod ea OA DS Ee EM ees 37 9 Useful recipes for the ISGRI data analysis o 39 9 1 Rerunning the Analysis ooo ee ee e Ry RU a 39 9 2 Make your own Good Time Intervals e 39 9 3 Usage of the predefined Bad Time Intervals o 40 9 4 Combining results from different observation groups 41 9 4 1 Creating a mosaic from different observation groups 41 9 4 2 Combining spectra and lightcurves from different observation groups 42 9 5 Rebinning the Response Matrix lt e easa doten eeud aa a ee ee 43 9 5 1 Extracting images in more than 10 energy ranges 44 9 6 Some tricks on saving disk space and CPU time
158. ted by Monte Carlo simulation 1 0001 r T T eod ide Mi mre BIS SGRI 5 SS EEN UT e 0 100 PICsIT singles ee Ree or e f PIGsIT multiple e Nr erUE gt E gt ISGRI PICs T EZ 5 pa a q f E e EA 7 L r d dime Las Peg e ees 1 MEM ZZ L L QA on 110 g r i i f j 0 001 l EY nen Wane A amp i A ee eee 10 100 1000 TOC Energy kev Figure 9 IBIS sensitivities for the various detection techniques 4 2 IBIS observing modes IBIS has several observing modes for engineering and calibration purposes However for scientific use there is only one operating mode Science Mode In Science Mode ISGRI registers and transmits events on a photon by photon basis i e every event is tagged with X Y position on the detector plane event energy from the pulse height and rise time and event time PICsIT in principle can also operate in photon by photon mode However with the higher background compared to ISGRI there would be unacceptable data loss Therefore the standard mode for PICSIT is histogram Images and spectra full spatial resolution 256 energy channels are accumulated for about 30 minutes before transmission to ground There is no time tagging internal to the histogram 1 e spectral imaging has time resolution of 30 minutes In addition coarse spectra without imaging information are accumulated by PICSIT and tra
159. ted per energy range Intensity Variance Significance and Residuals With OBS1 ExtenType 1 true exposure maps will be written instead of residual images at the 4 n th extension of isgri sky ima fits The new default value 2 instead of 0 before OSA 10 will add the true Exposure maps in an additional extension OBS1_ExtenType 3 will add single true Exposure map as the last extension Please note that the change of default value from 0 to 2 affects also the mosaic images as instead of an on time map in the image mosaic file isgri_mosa_ima fits one now gets an effective exposure map which has much lower values because of the half opening of the coded mask and various vignetting effects that are here taken into account e If you are interested in running the analysis in more than 10 energy bands please see Section 9 5 e You can decide if you want to let the software find the best fit position of a source in the vicinity of the one in the catalog default OBS1_SouFit 0 or if you would prefer the catalog position for all sources from the input catalog to be used for the flux determination 0BS1 SouFit 1 If OBS1 SouFit 1 then the position of a new source is always attributed to the pixel center and for catalog sources ISDC IBIS Analysis User Manual Issue 10 1 36 the catalog position is used for SearchMode 1 3 or the pixel center for SearchMode 2 Note that OBS1_SouFit 1 fixes all the source posi
160. th separated by the given step parameter step In the example below 6 GTIs of 0 1 day length beginning at time IJD 1092 5 and separated by 0 2 days are defined gti user gti user gti repeat fits begin 1092 5 end A length 0 1 repeat 5 step 0 2 group mygroup fits Then in the main page of the GUI Fig 12 you should set SCW1 GTI gtiUserI user gti fits and specify the time format that was used in this file in the example above SCW1 GTI TimeFormat IJD More details on gti user are in the Data Analysis section of 1 9 3 Usage of the predefined Bad Time Intervals Read this to know how to make proper selection of the science windows that should be used in your analysis Different things could happen to the instrument during a particular science window To inform the user on any unusual things that he should be aware of the list of time intervals which had some anomalies bad time intervals has been created and is kept in the latest REP_BASE PROD ic ibis lim isgr_gnrl_bti_ fits file In this list you find the following 7 categories e IBIS CONFIGURATION is to flag the change of configuration Its time interval is short just the duration of the switch of parameters Column COMMENTS gives changes on the 4 main parameters given in file instr settings txt by order of importance rise time selection VETO configuration low threshold adjustment COMPTON window It is recommended not to use in your analysis
161. th ranging from 0 to 63 X axis is directed toward the source located above the page The Z axis is pointing positively to the sun 3 2 5 Veto Shield The Veto shield is crucial to the operation of IBIS IBIS uses anticoincidence logic to accept or reject detected events as real photons in the field of view or background particles or photons propagating through or induced in the spacecraft The sides up to the ISGRI bottom level and rear of the stack of detector planes are surrounded by an active Bismuth Germanate BGO veto shield Like the detector array the Veto shield is modular in construction There are 8 lateral shields i e 2 modules per side and 8 bottom modules The high density and mean Z of BGO ensures that a thickness of 20 mm is sufficient to reduce the detector background due to leakage through the shielding of cosmic diffuse gamma ray background and gamma rays produced in the spacecraft to less than the sum of all other background components ISDC IBIS Analysis User Manual Issue 10 1 9 4 How the Instrument works 4 1 Event Types The photon entering the telescope can be detected due to its interaction with the absorbing material of the detector Three major types of interactions play a dominant role photoelectric absorption Compton scattering and pair production In the photoelectric absorption process a photon undergoes an interaction with an absorber atom in which the photon completely disappears In its pla
162. the spectral timing data For all sources from the input ISGRI catalog light curves are extracted See Section 12 10 for more details e The fourth script ibis obs2 analysis again works in the whole Observation Group previously created and performs a single task for PICsIT data CLEAN Last step At this step PICsIT mosaic is created See Section 12 11 for more details Revision 3 rev_3 of the INTEGRAL Archive is completed and is now the default data format The older Revision 2 rev_2 archive is no more populated since revolution 1010 2011 01 20 Rev_3 data have been regenerated starting from INTEGRAL telemetry including a much improved time correlation and the improved data selection and calibrations used in OSA9 The data correction step COR as well as the instrumental GTI and deadtime handling DEAD steps have already been performed using a previous version of OSA at the science window level as was done also for rev_2 data However to fully exploit OSA10 improvements it is mandatory to rerun the analysis from COR step included as new calibration files are available The resulting OSA count rates are corrected for the off axis transparency of the mask supporting structure 2 The Pixel Illumination Factor PIF is a number between 0 and 1 which expresses the theoretical degree of illumination of each detector pixel for a given source in the sky ISDC IBIS Analysis User Manual Issue 10 1 15 6 Getting started
163. tially coded field of view out to 29 x 29 special cleaning techniques must be applied to the data to properly reconstruct the image The actual sky coverage in an observation of course depends on the dither pattern The on board electronics classify registered events according to the activated layer and the number of events detected by a submodule practically simultaneously Events detected by different submodules are treated as independent ones There are five main events type e ISGRI single event Photon is stopped in a single pixel of the ISGRI layer generating an electric pulse In principle the amplitude of the pulse yields the energy of the incident photon However above 50 keV the energy is a function of not just the pulse height but also the pulse rise time so both are used to determine the energy of the incident photon In addition the resulting line profile energy resolution is no longer Gaussian but more similar to a Lorentzian The energy resolution depends on the operating temperature and also on the bias voltage the bias voltage has to be optimized as a trade off between high resolution but more noise high voltage or lower noise but lower resolution low voltage All cases of multiple ISGRI detection units excitation in one module are rejected In case of the excitation of the detection units in different modules such events are treated as independent single events e PICsIT single event Photon passes through ISG
164. tion default 1 DOL of the Tungsten attenuation length fits file default DOL of the Aluminium attenuation length fits file default DOL of the Lead attenuation length fits file default Type of Science Window to be treated possible values POINTING SLEW OTHER ANY 2 default POINTING if 1 or absent do mosaic part Set it to 0 if you don t want to produce a mosaic image default 1 Mosaic map center deg default Mosaic map center deg default Mosaic map radius deg default 40 0 0 no flux spread in mosaic default 1 Software detects the catalog source only if its signal to noise ratio is higher then this value This parameter has no meaning for the Science Window level images if OBS1_SearchMode 1 3 default 6 73 OBS1_MinNewSouSnr MinNewSouSnr real Software detects a new source only if its signal to noise ratio is higher then this value default 7 OBS1_SouFit SouFit integer 0 for fitting source position and 1 for fixed source po sition in ScW fit default 0 OBS1_ExtenType ExtenType integer exposure residual maps possible values 0 or absent Residual Map at 4 n th extension of ima idx 1 Exposure Map only at 4 n th extension of ima idx 2 both Residual and Exposure maps at 4 5 n th ex tension of ima idx 3 one Expo map at the end of ima idx if ExtenType 1 2 3 the Mosaic Exposure Map is at the 4 n th
165. tions only in the individual Science Window analysis In the mosaic all source positions are always fitted regardless of the value of OBS1_SouFit These fitted values are written to RA_FIN and DEC_FIN columns of isgri srcl res fits and are later used in spectral and lightcurve extraction steps as a source position To fix the positions of only several sources set for them ISGRLFLAG 2 in the input catalog For the weak sources with well known positions it is recommended to use the catalog position ISGRI_FLAG 2 whereas for bright sources whose position is determined by the software with an accuracy better than 15 it is recommended to let the software to fit the position of the sources ISGRI_FLAG 1 WARNING When using OBS1_SouFit 1 with OBS1_SearchMode 2 not only the position of new sources but also that of cataloged ones is assigned to the pixel centre instead of be ing fixed to the catalog position It is therefore strongly recommended to avoid this combination of parameters This problem is not present with OBS1_SearchMode 1 or 3 since in this case the catalog position is used when no fitting is requested see also Sect 11 e For 0BS1_SearchMode 1 or 3 where you are forcing a catalog extraction ghosts can be cleaned even from the known sources that happen to have a negative peak This is done using OBS1_NegModels 1 while with 0BS1_NegModels empty or equal to 0 the default the deconvolved images will be cleaned from positiv
166. to analyse it in XSPEC We suggest to build such a matrix before launching OSA as shown in Section 9 5 and then extract images with the use of this matrix as shown in Section 9 5 1 See Sections 7 1 and 8 2 2 to learn how to create mosaic images for a better flux estimate use OBS1_PixSpread 0 Once you have the set of mosaic images in the desired energy bands to extract the spectrum from the mosaics attached to the og_ibis fits file at the position of 4U 1700 377 ra 255 9865 dec 37 84414 use mosaic spec cd REP BASE PROD obs xxx mosaic spec DOL_inp 0g_ibis fits DOL out og ibis fits N EXTNAME ISGR MOSA IMA DOL spec 4U1700 mosa pha fits ISGR PHA1 SPE tpl N ra 255 9865 dec 37 84414 size 4 ISDC IBIS Analysis User Manual Issue 10 1 45 Note that if the significance of the point is less than five then mosaic_spec will assign a non zero value to its quality and the point will be not used by XSPEC If you are interested to see this point do change its quality value to zero manually You find more details on mosaic_spec in Section 12 12 1 Please remember that different ARFs should apply to spectra extracted from the data of different obser vation periods see Table 3 Tf the mosaic from which you have extracted spectra contains the data from more than one observation period none of the pre defined ARFs can be used with the spectra generated with mosaic_spec Instead a special ARF averaged proportionally to the exposu
167. to be the whole Science Window 6 not good for Table 8 gti_attitude parameters included into the main script Name in the main script Name Type executable Description SCW1 GTLattTolerance X AttStability real ISDC IBIS Analysis User Manual Issue 10 1 Accepted attitude stability tolerance of X optical axis to generate a GTI arc min possible values 0 10800 default 0 5 61 SCW1_GTLattTolerance_Z AttStability_Z real possible values 0 10800 default 3 0 12 2 3 gti data gaps This program generates GTIs for ISGRI and PICsIT The GTIs depend on the presence of the science data A time is defined as bad if a science packet of the instrument is missing The expected science packets depend on the actual mode of the instrument This is taken into account while the GTI is being created The program does not distinguish between a pointing a slew and an engineering window The time is also set to be bad if there are scientific data that do not agree with the reported mode of the instrument Time is also defined bad if the telemetry indicates that there was an interruption of the on board processing due to a telemetry saturation In normal operation this case is rather seldom The final GTI is written into the IBIS index group and has the name CISGRI DATA GAPS and PIC SIT_DATA_GAPS for ISGRI and PICsIT correspondingly 12 2 4 gti import The gti impor
168. to include sources that are faint in comparison with the source of interest Moreover it is not recommended to have more than 30 sources in the input catalog as the software might crash otherwise Copy isgri srcl res fits to another file say specat fits as shown below leaving only sources with significance higher than a threshold 7 o in the example below cd REP_BASE_PROD obs isgri_gc fcopy isgri_srcl_res fits ISGR SRCL RES DETSIG gt 7 0 specat fits Note that there should be spaces around gt Note that it is important to make the resulting catalog read only to avoid that it gets corrupted during the analysis chmod w specat fits Part of the resulting specat fits catalog is shown in Figure 19 The same catalog will be used later for the lightcurve extraction In the GUI set the SCW2_cat_for_extract parameter to point to specat fits use the browse button to get the full path and press Ok the window disappears and you are back to the main GUI page There press Run to launch the analysis 7 2 1 Results of the Spectral Extraction Spectral files are produced for each ScW scw 0051004X0010 001 isgri_spectrum fits X 1 5 In these files you find the spectra of the desired sources plus the background spectrum In the header of each data structure the Name and ID of each source are given and the first extension of the file scw 0051004X0010 001 isgri spectrum fits is an index summarising the content of all t
169. tructure e 83 Content of ISGR SWIT STA Data Structure 2 55 ooo sra 84 ISDC IBIS Analysis User Manual Issue 10 1 x 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 97 58 59 60 61 62 63 ISDC Content of PICS FALT STA Date Structure oscense 84 Content of ISGR GAIN MOD Data Structure o 85 Content of ISGR OFF2 MOD Data Structure e 85 Content of ISGR RISE MOD Data Structure e 85 Content of ISGR OFFS MOD Data Structure e 85 Content of PICS ENER MOD Data Structure ees 85 Content of IBIS GOOD LIM limit table ees 86 Instrument Background Model Data Structures 2e 86 Content of Indexes for Table 40 Data Structures 86 List of Data Structures produced at COR level o ens 87 Content the level COR Data Structures for the photon by photon mode 87 Content of IBIS GNRL GTI Data Structures e e 87 Content of ISGR DEAD SCP Data Structures e 87 Content of PICS DEAD SCP Data Structures e 88 Content of COMP DEAD SCP Data Structures een 88 List of Data Structures produced at BIN level o 89 Content of _ _SHD IDX Data Structures o e o e 89 Content of GNRL REFR CAT Data Structures
170. tructures see Table 49 for details the abbreviations used in this table were introduced in Table 48 ISDC IBIS Analysis User Manual Issue 10 1 88 C 4 1 31 shadow build Ti shadow bwild prepares ISGRI data for scientific analysis During the run of this executable Data Structures ISGR DETE SHD for a detector shadowgrams and ISGR EFFI SHD for ISGRI detector efficiency shadowgrams are filled These Data Structures keep the position of each pixel and the total counts in given energy band during integration time or efficiency corre spondingly During PICSIT analysis the same information about the PICSIT detector is written to PICS DETE SHD and PICS EFFI SHD Data Structures C 5 Table 48 List of Data Structures produced at BIN level Instrument Type of shadowgram Output Data Structure ISGRI detector ID ISGR DETE SHD efficiency IE ISGR EFFI SHD PICsIT detector PD PICS DETE SHD efficiency PE PICS EFFI SHD Table 49 Content of F _ _SHD IDX Data Structures Column Name Description Shadowgram Type ISDCLEVL TFIRST TLAST TELAPSE ONTIME CHANMIN CHANMAX E_MIN E_MAX BANDTYPE RISE_MIN RISE_MAX HIS_TYPE SHD_TYPE ISDC level of data processing Time of the first data element Time of the last data element Total elapsed time of the data Sum of good time intervals Lowest channel of the energy range Highest channel of the energy range Lower bound of the e
171. ts rm isgri_mosa_res fits rm isgri_srcl_res fits e If you had previously run the spectral and lightcurve steps you have to detach the ISGRI SRCL RES data structure from all your Science Window groups swg_ibis fits That is to each Science Win dow scw group located in the REP_BASE_PROD obs dir directory you should do the following command cd REP BASE PROD obs dal detach object dir scw scw 001 swg_ibis fits pattern ISGR SRCL RES delete n At this point you are ready to launch the analysis and to create a joint mosaic cd REP BASE PROD obs GROUP1 ibis science analysis ogDOL 0g_ibis fits startLevel CAT I endLevel IMA OBS1_DoPart2 2 See 8 2 2 for a description of the main parameters of the mosaic step The above command is valid in case you have just run the ScW analysis part so that you indeed keep the same energy boundaries Otherwise if your parameter file has changed in between you should add in the above the definition of IBIS_II_ChanNum IBIS II E band min and IBIS II E band max according to the boundaries of the single SCW maps you want to merge 9 4 2 Combining spectra and lightcurves from different observation groups In Sections 7 2 and 7 3 you have seen how to merge lightcurves and spectra from different Science Windows belonging to the same group In that case the file og ibis fits points to all the Science Windows and it is pos sible to launch the collecting merging tools lc pick and spe pick direct
172. u need to have ROOT available 9 10 2 Run ii light To be able to use ii light you have to run the standard analysis until the SPE level startLevel COR endLevel SPE You need to run the IMA level with the same energy ranges in which you are going to extract the lightcurves This is due to the fact that the IMA step will produce correction and background maps rebinned corr ima fits and rebinned back ima fits that are energy dependent and that will be put as input to di light Alternatively you can use i_map_rebin to produce these maps in the desired energy bands You need to run the SPE level because during this level the PIF needed as input to 2i light is created Alternatively you can create PIF with ii pif program as described in Section 9 11 Once you have run the script until the SPE level included you are ready to launch the stand alone lightcurve extraction tool ii light works on the Science Window level only meaning that you have to launch it once per Science Window It does not change the structure of the Science Window group so if you would like to compare the results of oi light and ti lc extract it is worth to run the analysis until SPE use 9i light as shown below then go back to REP BASE PROD obs OGID and relaunch the analysis from LCR to LCR in the standard way The output lightcurve files of the standard software are automatically called isgri lcr fits Alternatively if you have first run the standard lightcurve
173. ual Issue 10 1 76 PICSIT_source inOG PICSIT_source_Shadow PICSIT_source_mask PICSIT_source_outOG PICSIT_source_outPIF PICSIT_source_outSpec inOG inShadow maskG outOG outpif outSpec string string string string string string DOL of the input Observation group default DOL of the input Shadowgrams default DOL of the IBIS mask model default DOL of the output Observation group default DOL of the PIF index default DOL of the output spectra default 12 10 Timing Analysis 12 10 1 4G lc extract ii lc extract performs similar tasks to ii spectra extract dealing with time bins instead of spectra ones Table 25 Parameters for the i lc extract ISDC IBIS Analysis User Manual Issue 10 1 Name Name Type Description in the main script executable ISGRI mask mask string DOL of the MASK pattern fits file default gt SCWS2 cat for extract inCat string DOL of the subset of the source catalogue default gt SCW2 ISPE DataMode DataMode integer Data Simulation mode DataMode 0 gt OG shadowgrams are treated 1 gt shadowgrams are simulated SCW2_ISPE_MethodInt MethodInt integer Method to be applied for the pixel value interpolation This parameter should have the same value as in the ii shadow bwild In the source model procedure MethodInt 0 gt dead zone pixels will be filled with 0 1 g
174. ult og_ibis fits start Level string Analysis level at which the analysis begins The names of the possible analysis levels are given in section 5 Possible values COR COMP Also CLEAN value is possible default COR endLevel string Analysis level at which analysis finishes The names of the possible analysis levels are given in the section 5 possible values COR CLEAN We recommend you to proceed by steps as described in the cookbook default IMA2 staring boolean Enter yes if it was a staring observation It has an in fluence on PICsIT analysis for staring observation all shadowgrams are summed before the deconvolution default no tolerance real tolerance for staring In case of staring yes the check is performed that during the Science Windows within the Observation Group the spacecraft was sta ble within the given tolerance default 0 1 sum spectra boolean Do the summing of spectra default no CAT refCat string DOL of Reference Catalog default 1S9DC REF CAT ISGRI FLAG 0 CAT usrCat string DOL of User Catalog CURRENTLY IG NORED chatter integer Verbosity level possible values O 5 0 errors only 1 warnings 2 normal default 2 IC Group string DOL of Instrument Characteristics master group default REP BASE PROD idx ic ic master file fits IC Alias string Selection alias for Instrument Charact
175. v SCW1 GTI gtiUserl browse SCW1_GTI_TimeFormat o SCW1 GTI BTI Names IBIS_CONFIGURATION IBIS_BOOT ISGRI_RISE_TIME VETO PROBLEM SOLAR_FLARE BELT ISGRI IMA ISGRI SPE and LCR PICsIT analysis Figure 23 Main page of the IBIS GUI FERRE keV for single events 203 252 252 336 336 448 448 672 672 1036 1036 1848 1848 3584 3584 6720 For multiple events 336 448 448 672 672 1036 1036 1848 1848 3584 3584 6720 6720 9072 9072 13440 This works for standard mode mode 41 only To select parameters specific for PICsIT analysis press the PICsIT button The PICsIT GUI page is shown in Figure 24 PICsIT analysis Ok Help staring 7 tolerance 0 1 4 SCW1_BKG_P_method 1 S Picsit_incorvar 14 PICSIT outVarian o PICSIT souce nam PICSIT souce RA 04 PICSIT souce DEC 03 SCW catalog FO browse Figure 24 PICsIT page of the IBIS GUI Depending on the observation mode staring or dithering there are two ways to analyze the PICsIT data The first by using the parameter staring yes can be used only for staring observation where the dif ference between all the pointings is less than the value defined by the tolerance parameter for PICsIT use tolerance 0 1 In this case the corrected shadowgrams are integrated before the deconvolution If staring no then deconvolution will be performed for each sc
176. values in the fields of interest For instance Sort output by scw_id for that check the Sort column Put pointing in the field scw_type to specify that only pointings should be returned and not slews Put gt 2003 03 15T23 00 00 in the field start_date and put lt 2003 03 16T02 30 00 in the field end_date Put public in the field ps to specify that only public ScWs should be returned Put gt 100 in the field good_isgri to select Science Windows with good ISGRI time higher than 100 seconds Press the Start Search button at the bottom of the web page In our case a table with 5 ScWs will be displayed Select the ScWs of interest To follow the example in the Cookbook click on AI for all ScWs Press the Save ScW list for the creation of Observation Groups button at the bottom of that table and save the file with the name isgri_gc 1st This file isgri_gc lst will be used later as input for the og_create program see Section 7 From this file you need the 5 lines below either in the format as given above or simple as 3 It is no more needed to add the extension 1 but the name of the FITS file swg fits is needed unless you use the very basic format without the directory path scw 0039 and without the final as shown below 1 ISDC IBIS Analysis User Manual Issue 10 1 17 005100410010 001 005100420010 001 005
177. ves shadowgrams in the given energy bands The index of deconvolved and cleaned images is written to ISGR SKY IMA IDX Data Structure For each output energy band defined four images are created and attached to this index The content of this Data Structure is given in the Table 51 Table 51 Content of ISGR SKY IMA IDX Data Structure Column Name Description ISDC IBIS Analysis User Manual Issue 10 1 90 IMATYPE Type of image Possible values are IMAGE deconvolved and cleaned sky image VARIANCE variance image SIGNIFICANCE significance map RESIDUAL difference between raw deconvolved only and cleaned image EXPOSURE true exposure map can be cre ated CHANMIN Lowest channel of the energy range CHANMAX Highest channel of the energy range E_MIN Lower bound of the energy range E_MEAN Mean energy of the energy range E_MAX Upper bound of the energy range TFIRST Time of the first data element TLAST Time of the last data element TELAPSE Total elapsed time of the data EXPOSURE Effective exposure time CRVAL1 LONG at the reference value CRVAL2 LAT at the reference value For each deconvolved image the list of found sources is created Data Structure ISGR SKY RES and attached to the ISGR SKY RES IDX Data Structure See content of these Data Structures in Tables 53 52 Table 52 Content of ISGR SKY RES Data Structure Column Name Description
178. volution Figure 31 ISGRI low threshold position as function of INTEGRAL revolution number Science Window events Note this flag was filled by the executable ibis isgr evts flag The second method is spectral based it discriminates pixels by estimating their spectral deviation from the average ISGRI spectrum This spectral method can be switched ON OFF by parameter NoisyDetFlag Table 12 ii shadow build parameters included into the main Script Name Name Type Description in the main script executable IBIS II ChanNum isgri e num integer Number of energy intervals for ISGRI possible values 1 10 default 7 IBIS IL E band min isgri e min string List of lower energy boundaries keV default 15 40 100 200 400 700 1200 IBIS ILE band max isgri e max string List of upper energy boundaries keV default 40 100 200 400 700 1200 2500 IBIS min rise isgri min rise integer Minimum rise time default 16 IBIS max rise isgrimax rise integer Maximum rise time default 116 IBIS_NoisyDetMethod NoisyDetFlag integer Defines the way to deal with noisy pixels possible values O Time based noisy detection 1 Time based Spectral based method default 1 12 4 2 ip_ev_shadow_build ip_ev_shadow_build takes as an input PICSIT data received in photon by photon mode For each given energy and time range intensity and efficiency shadowgrams are produced Efficiency is defined as Eff 1 D x
179. x isgrResp idx isgrResp string DOL of the index of ISGRI response matrices default SCW2_ISPE_DataMode DataMode integer Data Simulation mode possible values O real data 1 simulated data default 0 ISDC IBIS Analysis User Manual Issue 10 1 75 SCW2_ISPE_MethodInt SCW2_ISPE_MethodFit SCW2_ISPE_isgrUnifDol SCW2_ISPE_isgrBkgDol tungAtt aluAtt lead Att rebinned corrDol spe MethodInt MethodFit isgrUnifDol isgrBkgDol tungAtt aluAtt lead Att corrDol string string string string string string integer integer default 1 tensity fitting possible values MethodFit 0 gt CHI2 MethodFit 1 gt Maximum Likelihood MethodFit 2 gt Least Squares MethodFit 6 Squares fit default 6 DOL of the ISGRI detector uniformity default DOL of the ISGRI background model default DOL of the Tungsten attenuation length fits file default DOL default DOL of the Lead attenuation length fits file default 6 22 ec 22 spectrum default Method to be applied for the pixel value interpolation Method to be applied for background and source in gt iterative imaging like Least of the Aluminium attenuation length fits file DOL of the rebinned ISGRI off axis corrections for 12 9 2 ip spectra extract ip_spectra_extract reads the shadowgram for each input energy band and the name and c
180. y a catalog of sources for which to extract the spectra e g specat fits do not have sources brighter than 600 mCrabs in the list see warning at the end of this section and you are not interested in the imaging results anymore you can skip all the imaging related levels and do startLevel COR endLevel SPE GENERAL_levelList COR GTI DEAD BIN_S SPE Remember that if you do not do the imaging part then isgri_srcl_res fits is not created This file is the default one that is used for spectral extraction 7 2 Do not forget to specify the catalog you have built for this purpose setting the SCW2_cat_for_extract equal to specat fits e Likewise if you are interested only in lightcurve results and do not have sources brighter than 600 mCrabs in the list see warning at the end of this section you should create PIFs for all sources of interest with ii pif program see Section 9 11 for an example and afterwards you may use startLevel COR endLevel LCR GENERAL_levelList COR GTI DEAD BIN_S LCR again with SCW2_cat_for_extract equal to specat fits e If you are familiar with the sources of your field i e you have already run the imaging part for instance and you want to extract images spectra and lighturves in one go set SCW2_cat_for_extract equal to specat fits and run your analysis with startLevel COR endLevel LCR and the complete list of levels in GENERAL_levelList Warning If you skip the level BKG_I and do s
181. y binning With the help of the parameter IBIS SI inEnergyValues you can specify the file and its extension de scribing the desired binning of the response matrix By default set with empty line the latest available file ISDC IBIS Analysis User Manual Issue 10 1 26 4U1700 377 scwlc fits FLUX 1 5 FLUX count s 100 80 60 40 20 1170 1170 02 1170 04 1170 06 1170 08 TSTART TSTOP 2 Figure 17 ScW per ScW lightcurve of 4U 1700 377 in the 20 40 keV energy band Tm poU A 40 60 100 200 000 Mme 8 estan 0 PO Figure 18 Page of IBIS GUI for Spectral and Ligtcurve extraction ISDC IBIS Analysis User Manual Issue 10 1 27 with the rebinned response matrix is used See sections 8 3 and 9 5 if you want to define your own spectral binning Background maps With the SCW2_BKG _LisgrBkgDol parameter you can specify the background map to be used in the spectral and timing analysis It is recommended to use the same background map as in the imaging case De fault empty value corresponds to the default map REP BASE PROD ic ibis bkg isgr back bkg 0011 fits Input catalog for Spectral and Lightcurve extraction By default spectrum will be created for all sources listed in the isgri srcl res fits catalog created during the IMA step The position of the source will be taken from RA FIN DEC FIN columns Note however that spectral extraction is time consuming and it is not recommended
182. y contributes to the background level Representing the mask with an array M of 1 open elements and 0 opaque ones the detector array D will be given by the convolution of the sky image S by M plus an unmodulated background array term B D SxM B MURA patterns have the remarkable property that their cyclic autocorrelation gives a delta function The decoding array G is inverse to M where G 2M 1 i e G 1 for M 1 and G 1 for M 0 and thus is correlation inverse With the help of array G we can reconstruct the sky S DxG S BxG where S differs from S only by the B x G term which for a flat array B is a constant level that can be measured and removed To have a sidelobe free response a source must be able to cast a whole basic pattern on the detector fully coded source To make use of all the detector area and to allow more than one source to be fully coded the mask basic pattern is normally taken as the same size and shape of the detector and the total mask made by a cyclic repetition 2 x 2 for rectangular mask of the basic pattern For such optimum systems a FCFOV source will always project a cyclically shifted version of the basic pattern and correlating the detector image with the G decoding array will provide a sidelobe free peak with position invariant shape at the source position A source in the PCFOV will instead cast an incomplete pattern and its contribution cannot be a priori subtracted and will produc
183. yer o rm 4 9 IBIS sensitivities for the various detection techniques o e 000 ee eee 11 Science Analysis Overview ee 14 Structure of the directory created with og create ooo e 21 Mata page of the IBIS QUI soyd gee a pe ek e a ee we eg dogs 22 Imaging page of the IBIS GUI 54 secr eae a opc EE um a EUR ad 23 Overview of the IMA level products e 24 A part of the GROUPING extension table of an isgri_sky_ima fits file 25 INTENSITY left and SIGNIFICANCE right mosaic images in the 20 40 keV energy band 26 ScW per ScW lightcurve of 4U 1700 377 in the 20 40 keV energy band 27 Page of IBIS GUI for Spectral and Ligtcurve extraction a 27 List of sources used for the spectral analysis o eee 29 Total spectrum of 4U 1700 377 fitted with a cut off powerlaw model 31 Lightcurve of 4U 1700 377 in the 20 40 keV energy range with 100 sec binning 32 Crab power Spectre 224 faa e e a RO ee d 49 Main p ge of the IBIS GUL e ie he ee BRE a a EE A 52 PICSEE page Goethe IBIS GUL csaa osa tiea eRe ede ge eee eke woe me woe ee ao 52 Crab significance image in the 252 336 keV energy band as seen by PICSIT 54 PICsIT Crab spectrum extracted from the mosaic 2e 55 Composition of the main script bis_science_analysis For further descriptions of the BIN BKG steps for the DEAD IMA and BIN leve
184. ysis User Manual Issue 10 1 68 SCW1_BKG_P_picsSBkgDOL picsSBkgDOL string DOL of the PICsIT Detector Background model single SCW1_BKG_P_picsMBkgDOL picsMBkgDOL string DOL of the PICsIT Detector Background model multiple SCW1_BKG_P_method method integer Method to use in scaling the background maps possible values 0 model in cts is normalized by the time of observation 1 model in cts is normalized by the mean count value default 0 12 7 Catalogs The catalog extraction selects the sources in the field of view FOV from the references catalog 12 7 1 cat extract The executable cat extract performs the source selection from a reference catalog The reference catalog should have the same structure as GNRL REFR CAT see Table 50 in Appendix C 5 Its DOL is passed in the parameter refCat There is no standard output catalogue for IBIS and the parameter outExt must be filled Table 18 cat_extract parameters included into the main script Name Name Type Description in the main script executable CAT refCat ref cat string DOL of the reference catalogue default value 1SDC REF CAT OBS1_CAT_radiusMin radiusMin string Low limit for the position selection default 0 OBS1_CAT_radiusMax radiusMax string High limit for the position selection default 20 OBS1_CAT fluxDef fluxDef string Column used for flux selection defau

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