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DOCUMENT TYPE: Software User Manual TITLE: GRID - Agile

1. L L 7 L L L TTT OTT AGILE Team 7 7 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 INPUT PARAMETERS Input index file name LOG _test_5 0 index Output file name map exp map dimension deg 30 00 map resolution deg 0 30 map centroid G long deg 263 55 map centroid G lat deg 2 79 TMIN s 111844735 000000 TMAX Is 112103935 000000 MIN ENERGY MeV 100 0 MAX ENERGY MeV 50000 0 maximum off axis angle deg 50 00 minimum off axis angle deg 0 00 radius of earth albedo deg 90 00 Orbital Phase Code 2 Pointing direction tolerance deg 0 50 Roll angle tolerance deg 360 00 Earth direction tolerance deg 5 00 raeffFileName home ADC scientific_analysis data AG GRID_G0017_SFMG_10023 sar gz SPECTRAL INDEX 2 10 map bin step 2 projection ARC time step 160 AG exPMADEERN ee ee ee ee ee ee starting image read OK Upper bound greater than the last channel treated as infinity AG exXDMADEEN ees ee ee ke ee addfile starting TIME gt 111844735 000000 amp amp TIME lt 112103935 000000 amp amp LIVETIME 0 amp amp LOG STATUS 0 amp amp MODE 2 amp amp PHASE NE 1 amp amp ROW 1 ROW ROW 160 160 AG exXDMADEEN ees ee ee eke ee addfile exiting STATUS 0 AG _exXpMAapgeN coccccnnonnncnnonnnncnnninnnss exiting dept ff Y AU AE AE AE AU Y AE AE AE AE AE Y AU AU AE AE AE AU Y AE AE AE AL AE AE AE AE AE AE AU AA
2. RDI3 GRID Correction and Standard Analysis User Manual AGILE IFC OP 010 26 1 2006 1 3 Contacts The reference person at TASF Milano for this document is Andrew Chen chen iasf milano inaf it 02 23699343 The packages described in this Document have been developed at IASF MI by A Giuliani A Pellizzoni A Chen A Trois S Vercellone and T Contessi and by A Bulgarelli at IASF BO as AGILE Team software manager S Mereghetti acts as the IASF MI software working group coordinator The software has been tested and debugged with the support of the AGILE Data Center Team at ASDC See also RD 1 for a detailed description of the developer list 2 Basic concepts 2 1 Introduction AGILE is an ASI Italian Space Agency Small Scientific Mission dedicated to high energy astrophysics which was successfully launched on April 23 2007 The AGILE instrument is composed of three main detectors a Tungsten Silicon Tracker designed to detect and image AGILE Team 3 3 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 photons in the 30 MeV 50 GeV energy band an X ray imager called Super AGILE operating in the 18 60 keV energy band and a Mini Calorimeter that detects gamma rays and charged particle energy deposits between 300 keV and 100 MeV The instrument is surrounded by an anti coincidence AC system The main purpose of the Silicon Tracker is to provide a compact imager for gamma ray pho tons of energy above 30 MeV The Tracker con
3. AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 CRVAL2 2 787 CTYPE1 GLON ARC CTYPE2 GLAT ARC CRPIX1 50 5 CRPIX2 50 5 CDELT1 0 3 CDELT2 0 3 CUNIT1 deg CUNIT2 deg RADESYS FKS EQUINOX 2000 LONPOLE 180 TSTART 111844735 OBT first event time TSTOP 112103935 OBT last event time TIMESYS TT TIMEUNIT s DATE OBS 2007 07 18T12 00 00 start date and time of the observation TT DATE END 2007 07 21T12 00 00 end date and time of the observation TT TIMEZERO 0 TT MJDREFI 53005 MJDREFF 0 000754444444444444 MINENG 100 MAXENG 50000 TELESCOP AGILE INSTRUME GRID PIXCENT T BUNIT FOV 50 Maximum off axis angle deg FOVMIN 0 Minimum off axis angle deg ALBEDO 90 Earth zenith angle deg PHASECOD 2 Orbital phase code FILTERCO 5 Event filter code END 5 The Intensity Map Generator Task Intensity maps are generated by the procedure AG intmapgen the executable can be found in ADC scientific_analysis bin AG_intmapgen reads an exposure map produced by AG_expmapgen and a counts map produced by AG_ctsmapgen and outputs a FITS image file in the same format as the exposure map in which each pixel contains the intensity in that pixel The image is a square array in the ARC projection The two input maps should have been produced using the same set of parameters The intensity map
4. Set this value to 2 0 for upper limits at the same level that AG srctest fixed writes in output The loccl parameter is the deltaTS for the position confidence contours Set this parameter to 5 9914659 corrisponding to a confidence level of 95 for contours at the same confidence level as the output of AG srcloc A future revision of the software will replace this parameter with the confidence level expressed as a probability i e 0 95 instead of 5 9914659 Ipoint and bpoint specifies the AGILE pointing for each observation block See the ASDC web site for the list of observation blocks The srclist parameter is the name of a text file whose format is similar but not identical to the format of the input of AG srclist Here is a sample srclist for AG_multi2 Example of source list file AGILE Team 33 33 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Field Name Instrument AGILE GRID flux 1ii bii index fix minTS label 0 00E 06 263 65 2 95 2 1 2 2 0 21 0 00E 06 260 35 0 35 2 1 2 2 0 22 0 00E 06 270 55 0 36 2 1 2 2 0 23 0 00E 06 268 46 4 14 2 1 2 2 0 24 0 00E 06 267 56 4 74 2 1 2 2 0 25 0 00E 06 261 53 11 65 2 1 2 2 0 31 The lines beginning with are comments and are ignored Each of the remaining lines is an input source The columns are as follows 1 flux photons cm s If fix 0 this flux is fixed otherwise a new optimum is found 2 1 deg Galactic latitude 3 b deg Galactic longitude Note th
5. AE AE AE AM AM AE AE AE AL AE AE AE AE AE AE AE AE AE AE AE AU AM AE AE AA AE AE AE AI HUUR HIE IE IE HE HIE IE IE HEHE IE HEI II HIE IE IE IE HIE IE HEI HIE HE HEI HIE IE IE IE II HIE IE HEHE HIE IE HEI IE IE T HUH IE HIE IE IE HIE IE HEHE HEHE IE HEI HIE HIE IE II HIE IE EIE HIE HE HEI HIE IE IE IE IE HE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE II TE TT TT TE TT IT II NI TE TT NI TE IT MI TE II TE TE IT TE TE TE TE TE TE TT TE TE NI TE IT NI TE NT To TT DI NI II MI NI II MI TE II TT TE NI TT TE IT TT TT AGILE Team 8 8 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Exposure Map sample header SIMPLE T file does conform to FITS standard BITPIX 64 number of bits per data pixel NAXIS 2 number of data axes NAXIS1 100 length of data axis 1 NAXIS2 100 length of data axis 2 EXTEND T FITS dataset may contain extensions COMMENT FITS Flexible Image Transport System format is defined in Astronomy COMMENT and Astrophysics volume 376 page 359 bibcode 2001A8A 376 359H CRVAL1 263 55 CRVAL2 2 787 CTYPE1 GLON ARC CTYPE2 GLAT ARC CRPIX1 50 5 CRPIX2 50 5 CDELT1 0 3 CDELT2 0 3 CUNIT1 deg CUNIT2 deg RADESYS FK5 EQUINOX 2000 LONPOLE 180 TSTART 111844735 OBT first event time TSTOP 112103935 OBT last event time TIMESYS TT TIMEUNIT s DATE OBS 2007 07 18T12 00 00 start date and
6. HEI HIE HIE IE IE IE HIE IE EIE HIE IE HEI HIE HE IE IE EIE HIE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE II TE NI TT TE TT IT N NI TE TT NI TT IT MI TE II TE TE IT TE TE TE TE TE TE TT TE TE NI TE IT NI TT IT TE TT DI NI II MI NI II MI TE II TE TE TT TT TE IT TT TT 7 JE jp jf jf tf pf Jf Jf AI HHHHHH AG multid v 1 2 15 03 2011 A C T C A T HAHHHHHF dept ft tf tp AE AE AE pp pp AE AE AE AE AE dd AE AE AE AI HULE HIE IE IE HE HIE IE IE HEHE IE HEI HIE HIE IE IE IE HIE IE HEI HEHE HE HEI HIE IE IE IE HE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE TE TE NI TT TE TT IT II NI TE TT NI TT IT MI TE II TE TE IT TE TE TE TE TE TE TT TE TE NT TE IT NI TT IT TE TT DI NI II MI NI II MI TE II TT TE N TT TE IT TT TT JH AE AE AE AU AE AE AE pp AE AE AE AE AE AE AE AE AU AE AE AE AU AE AE AE AE HALE AE AE AE AE AE AE AE AU AE AE AE AU AM AE AE AE AL AE AE AE AE AE AE AE AE AE AE AE AM AM AE AE AE AE AE AE AE AI HUUR IE HIE IE IE HE HIE IE HEI HEHE IE HEI HIE HIE IE II HIE IE HEI HIE HE HEI HIE IE II IE HIE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE TT TE NI TT TE TT IT II NI TE TT NI TT IT NI TE II TE TE IT TE TE TE TE TE TE TT TE TE NI TE IE NI TT IT To TT DI NI II MI NI II MI TE II TT TE NI TT TE IT TT TT INPUT PARAMETERS Map file name list txt SAR file name AG_GRID_G0017_SFMG_10023 sar gz EDP file name AG_GRID_G0017_SFMG_10023 edp gz PSD file name AG_GRID_G0017_SFMG 10023 psd
7. are written in C and use the ROOT CERN and CFITSIO NASA libraries All the tools can be run from the command line The Science Tools use the Parameter Interface Library PIL developed by the ISDC for parameter input allowing a variety of input methods 1 the user can start the tool which then asks for the values of some parameters interactively on the console 2 the user can input all or some of the parameter values on the command line in the same order as the provided parameter file 3 the user can input all or some of the parameter values on the command line in any order writing parameter names explicitly as pname value In all methods the user can accept the defaults stored in each task parameter file if the task was already run defaults are the last values used for parameter values not explicitly provided by adding mode h on the command line Some task input parameters are text files of index type reporting in each row an input file name followed by the minimum and maximum times contained in the file and the file type The parameter when specified on the command line must be preceeded by a See examples in the task sections AGILE Science Tools use the calibration files in ADC scientific analysis data The corresponding parameter in each task parameter file is set to a deafult value suitable for a standard analysis of events of type G in a full energy band 100 50000 MeV To perform a different analysis th
8. gamma ray sources to fit to the list of maps above Refer to the srclist section for details string outfile The name of the main text output file the title of the HTML output and the prefix of the other output file names number ulcl Sources for which a flux optimization is requested will have a flux upper limit calculated in addition to a best fit flux and error where possible This parameter specifies the confidence level for the flux upper limits 1 for 1 sigma 2 for two sigma etc number loccl This parameter specifies the confidence limit of the source location contour for sources for which a source location optimization is requested It is expressed as a difference in test statistic dis tributed according to chi squared with two degrees of freedom e g 1 38629 50 2 29575 68 4 60517 90 5 99147 95 9 21034 99 7 4 The Map List The map list is a text file listing containing at least one line of text Each line of text describes one set of maps and it is possible to include empty lines or comment lines The comment lines begin with an exclamation mark Each set of maps is described by a line containing space separated values in the following order lt cts file gt lt exp file gt lt gas file gt lt off axis angle gt lt galCoeff gt lt isoCoeff gt The file names may contain absolute or relative path information However because the values in each line are separated from one another by a space they
9. is not used in the scientific analysis it is useful solely as a visualization tool AGILE Team 13 13 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Figure 3 shows the image produced by DS9 for an intensity map generated by AG_intmapgen with Galactic coordinate axes displayed 0 00022 0 00044 0 00066 0 00088 9 00110 0 00131 0 00153 0 00175 0 00197 Figure 3 DS9 image of an intensity map produced by AG_intmapgen with the listed parameter file AGILE Team 14 14 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 inputs AG_intmapgen par expfile s ql map exp Enter exposure file name outfile s gql map int Enter output file name ctsfile s ql map counts Enter counts map file name You can type the command AG_intmapgen at the command line and insert the requested parameters or insert the parameters as arguments of the procedure Here we provide an example of command line home adc GO_test_dataset gt AG intmapgen expfile map exp outfile map int ctsfile map counts outputs Screen output HHHHHHHAR HEHEHE H HH III IR III R III IR RR R RR III III RR R RR RR RR RR RR RR HHHHHHHHHH AG intmapgen cpp v 0 19 12 05 A C A T HERA HR RIIIIR RR RR RR RR RR RI RR RI III RR RR RIG RR RR RR RR RR RR RR RR RR HR RIIIIR RR RR R RR RR RR RR RI III RR RR IR RR IR RR RR RR RR RR RR IR INPUT PARAMETERS Enter exposure file name map exp Enter output file name map int Enter counts map file name map counts AG int
10. line and insert the parameters or insert the parameters as arguments of the procedure Here we provide an example of command line home adc GO_test_dataset gt AG ctsmapgen evtfile 0Evt index outfile map counts mdim 30 AGILE Team 10 10 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 mres 0 3 la 263 55 ba 2 787 tmin 111844735 tmax 112103935 emin 100 emax 50000 fovrad 5 fovradmin 0 albrad 90 lonpole 180 phasecode 2 filtercode 5 projection ARC outputs Figure 2 DS9 image of a counts map produced by AG_ctsmapgen Screen output GEE GEE GEE EE EE EE EE EE Ee EE EE EE EE EE EE EE EE Ee Ee EE EE EE GE GE GE GE GE EE GEE SE GEE EE EE HHHHHHHHHH AG ctsmapgen cpp v 0 19 12 05 A C A T HHHHHHH WIR AAA IE RE IE WIE RR AAA IE WETE TE IE TERMIETE TE TE TTT TEI TE AAA AAA WERE TE TE TER IE WETE TEE INPUT PARAMETERS Input index file name OB1000_Velatest EVT index Output file name map counts AGILE Team 11 11 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 map dimension deg 30 00 map resolution deg 0 30 map centroid G long deg 263 55 map centroid G lat deg 2 79 TMIN s 111844735 000000 TMAX s 112103935 000000 MIN ENERGY MeV 100 0 MAX ENERGY MeV 50000 0 maximum off axis angle deg 50 00 minimum off axis angle deg 0 00 radius of earth albedo deg 90 00 Orbital Phase Code 2 Filter code 5 AG cCtSMADEEN esse ee ee ee starting AG cCtSM
11. may not themselves contain a space The cts exp and gas files are produced from experimental data by the procedures AG_ctsmapgen AG_expmapgen and AG_gasmapgen2 They contain the photon counts the instrument exposure and the Galactic diffuse emission model respectively collected in a given period of time falling in a given energy interval and detected with a given angle of incidence among other selection criteria see the appropriate sections about map generation for further details The selection criteria affect the shape of the point spread function of the instrument calcu lated by AG multi4 using the calibration files Most of the parameters energy phase code etc are already contained in the FITS headers of the input files however the off axis angle must be specified explicitly In general a separate set of maps should be generated for each range of off axis angles In this case the off axis angle specified for each set of maps should AGILE Team 22 22 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 be the mean value in the range in degrees For example a value of 20 degrees would be an appropriate choice for a set of maps generated for off axis angles between 10 and 30 degrees The galCoeff and isoCoeff are the coefficients for the Galactic and isotropic diffuse emission components respectively The values may be fixed during the fitting process or some or all of them may be optimized by allowing them to vary Positive valu
12. 59H CRVAL1 263 CRVAL2 2 6 CTYPE1 GLON ARC CTYPE2 GLAT ARC CRPIX1 67 1666666666667 CRPIX2 67 1666666666667 CDELT1 0 3 CDELT2 0 3 CUNIT1 deg CUNIT2 deg RADESYS FK5 EQUINOX 2000 LONPOLE 180 TSTART 111748135 OBT first event time TSTOP 112363135 OBTllast event time TIMESYS TT TIMEUNIT s MJDREFI 53005 MJDREFF 0 002354444444444444 TIMEZERO 0 TT DATE OBS 2007 07 13T12 00 00 start date and time of the observation TT DATE END 2007 07 24T12 00 00 end date and time of the observation TT MINENG 100 MAXENG 50000 TELESCOP AGILE INSTRUME GRID PIXCENT T YTOL 0 5 Pointing direction tolerance deg ROLTOL 360 Roll angle tolerance deg AGILE Team 19 19 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 EARTOL 5 Pointing direction tolerance deg STEP 2 Interpolation step size TIMESTEP 16 Log file step size BUNIT cm 2 s sr 1 FOV 60 Radius of field of view deg FOVMIN 0 Minimum off axis angle deg ALBEDO 80 Earth zenith angle deg PHASECOD 18 Orbital phase code INDEX 2 1 SC Z LII 287 305239941523 SC Z Bll 0 237547573935354 SC LONPL 0 EXTNAME GAS DH_CONF_ G0017 GRID DHSim configuration ID STAN CON SFMG GRID Standard an configuration ID FILE ID 10023 File Identification Number Issue END 7
13. 77 19 2379 2 45517e 07 1 4117e 07 24 2 32719 268 24 4 19059 35 8519 17 489 2 64166e 07 1 28864e 07 25 0 874173 267 56 4 74 17 098 20 5399 1 26528e 07 1 51999e 07 31 3 79917 261 676 11 809 40 8257 14 0467 3 15587e 07 1 08583e 07 w w w w The lines beginning with are comments in order to help the reader Gascoeff and Isocoeff are set to the last values to emerge from the analysis which may not be the most useful values Check the screen output to see the values that emerge depending on the source and region of interest being analyzed Note that errors both symmetric and asymmetric are now provided Each source has its significance position counts counts error flux and flux errors listed For convenience only the symmetric errors are printed in the main output file but each source with fix gt 1 also has its own output file the name of which is the output prefix followed by _ followed by the name of the source as listed in the srclist input file For example if the output prefix is vela res and the name of the source is VELA the source output file would be named vela res_ VELA If fix 2 for this source and its significance is above both minTS and AGILE Team 36 36 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 locdl Oo additional output files are written a file with suffix con containing the confidence contour in ds9 format a file with suffix ellipse con that is the fit with
14. ADEEN ee ee ee ee ee ee adding events files AG cCtSMADEEN ee ee es ee ee ee addfile exiting STATUS 0 1389 creating Counts Map sees esse se ee ee writing Counts Map esse sesse ss se ee se ee writing header sesse sesse ee ee Se ee AG cCtSMADEEN ese ee ee ee exiting va mb la bs ss ls sb ls ds ls bs nl ba a WAL dy dy HY A Ae de He AL i p sas Let He te He te He A AL Th TP TP TP TP ATP TP ATP TP TN Task AG ctsmapgen en Es exiting Th Tt T Tr Tt TP TP TP T dept ff tf df AE AE AE pp pp AE AE AE AE AE AE AE AE AE AE dd AE AE AI HUUR III HIE IE IE HE HIE IE HEI HEHE IE HEI HIE HIE IE IE IE HIE IE HEI HIE HE HEI HIE IE II II HE TEE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE TT TE NT TT TE TT IT II NI TE TT NI TT IT NI TE II TE TE IT TE TE TE TT TE TE TT TE TE NI TE IE NI TE IT TE TT DI NI II N NI II MI TE II TE TE NI TT TE IT TT TT Counts Map sample header SIMPLE T file does conform to FITS standard BITPIX 16 number of bits per data pixel NAXIS 2 number of data axes NAXIS1 100 length of data axis 1 NAXIS2 100 length of data axis 2 EXTEND T FITS dataset may contain extensions COMMENT FITS Flexible Image Transport System format is defined in Astronomy COMMENT and Astrophysics volume 376 page 359 bibcode 2001A amp A 376 359H BZERO 32768 offset data range to that of unsigned short BSCALE CRVAL1 1 default scaling factor 263 55 AGILE Team 12 12
15. AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 DOCUMENT TYPE Software User Manual PREPARED BY CHECKED BY TITLE GRID SCIENTIFIC ANALYSIS USER MANUAL DOC REF AGILE IFC OP 09 N of PAGES ISSUE Build 21 DATE 16 November 2011 A CHEN A BULGARELLI T CONTESSI A GIULIANI S MEREGHETTI A PELLIZZONI A TROIS S VERCELLONE P SANTOLAMAZZA C PITTORI APPROVED BY SOFTWARE MANAGER SUBSYSTEM LEADER PRINCIPAL INVESTIGATOR A BULGARELLI S MEREGHETTI M TAVANI AGILE Team AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Contents 1 Introduction 1 1 Scope and Contents of this Document o 1 2 Reference Documents HS Go AA ROETE NE NS GLO OT EL 2 Basic concepts Dels Ntro ducto ia ke ER De ME Re es ie a fale hes ed el 2 2 Event classification and standard data format 130 AGILE bei fee Tools da Se Me oS eB oi NY EER RY dec ac nah ee at 3 The Exposure Map Generator Task 4 The Counts Map Generator Task 5 The Intensity Map Generator Task 6 The Diffuse Map Generator Task 7 Source Detection and Location ley ATEO UCA A A A A 4 TX Seti FAR AS WA Mo eee 6 ME ed A IA e e 7 3 The AG multi4 Command Line 4 rs o ld es is a ed TA Tre Map bits ls Ms neis le ER Ek OB amen d a A des ce AA o Tie oOUCE ASE 4 4 ds we Qe Bos tied a ee i sy EE n 7 6 Galbration Pil s oie ins de Bon rd a a art dns 2 TE Amelysis para
16. L 0 5 Pointing direction tolerance deg ROLTOL 360 Roll angle tolerance deg EARTOL 5 Pointing direction tolerance deg STEP 2 Interpolation step size TIMESTEP 16 Log file step size BUNIT cm 2 s sr 1 FOV 60 Radius of field of view deg FOVMIN 0 Minimum off axis angle deg ALBEDO 80 Earth zenith angle PHASECOD 18 Orbital phase code INDEX 2 1 SC Z LII 287 305239941523 SC Z BII 0 237547573935354 SC LONPL 0 END AGILE Team 16 Build 21 deg 16 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 6 The Diffuse Map Generator Task Diffuse emission maps are generated by the procedure AG_gasmapgen2 the executable can be found in ADC scientific_analysis bin AG_gasmapgen2 reads an exposure map produced by AG_expmapgen and the master diffuse emission map and outputs a FITS image file in the same format as the exposure map in which each pixel contains the diffuse emission in that pixel The image is a square array in the ARC projection Figure 4 shows the image produced by DS9 for a diffuse emission map generated by AG_gasmapgen2 with Galactic coordinate axes displayed 5E 05 0 0001 0 00015 0 0002 0 00025 0 0003 Figure 4 DS9 image of the diffuse emission map produced by AG_gasmapgen2 with the listed parameter file The input calibration files should have the extension SFMG_I0023 disp conv sky gz These maps contain models of the diffuse emission c
17. Source Detection and Location 7 1 Introduction This section describes how to use AG_multi4 the latest version of the source detection and location task using the maximum likelihood method This version comes after version 2 version 3 was not released and is very similar in many respects 7 2 Getting started AG_multi4 is a command line application running under Linux 32 or 64 bits or Mac OS X The aim of this application is to find the best values for the flux the position and or the spectral index of a list of gamma ray sources in order to explain a set of experimental data The user will provide a list of maps containing maps of photons detected by the AGILE satellite during one or a series of observations together with maps of the instrument exposure during those observations and the corresponding Galactic diffuse emission models The user will also provide a list of sources that may explain the photons detected giving a guess for the flux position and spectral index of those sources AG multi4 will find the best values for the sources to fit the data using the method of maximum likelihood estimating the improved likelihood due to the presence of each source in the list The application also calculates the test statistic and significance for each source The user has a variety of options to influence the process as explained in the following 73 The AG_multi4 Command Line The command line is internally managed by the parameter interfac
18. T NT TE II TE TE IT TE TE TE TE TE TE TT TE TE NT TE IE NI TT IT To TT II NI TP N NI II MI TE II TT TE NI TT TE IT TT TT INPUT PARAMETERS Enter exposure file name VELA exp gz Enter output file name VELA gas gz Enter diffuse model file name 100_50000 0 5 SFMG_10023 disp conv sky gz Enter high res diffuse model file name 100_50000 0 1 SFMG_10023 disp conv sky gz AG gasmapEend sesse ees se ee starting AG gasmapEend ees ees se ee exiting AGILE Team 18 18 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 TOTANA Ly Le A A A AL AL A A A He He AL A ETES ek AL AL AL LL LL AL AL HL mM m Ti TT tT Tt TT Tt Tt TT Th TT Tt TT HHH HHH TT TT TT tT TT TT FH TTT TT HH HEH HER HH ETE UAL de He 4 sys Yet He Ae Ae de TL HY m m Tt Tt HHH Tt HA Task AG gasmapgen raii ie exiting FA Tt MU EN IR HHH HHH WAL dy dy HY A A Ae A Ah A HL Ue te de HE Ae de de HL Y TINA m m Tt Tt Ti if Tt Ti Tt Tt HH TH HH Tt TT Tt HH Tt HHH al Tt HH Tt TT TT TT HH Tt Tt HH Tt H Tt Tt Wt Tt HHH HH Diffuse Map Sample header SIMPLE T file does conform to FITS standard BITPIX 64 number of bits per data pixel NAXIS 2 number of data axes NAXIS1 134 length of data axis 1 NAXIS2 134 length of data axis 2 EXTEND T FITS dataset may contain extensions COMMENT FITS Flexible Image Transport System format is defined in Astronomy COMMENT and Astrophysics volume 376 page 359 bibcode 2001A amp A 376 3
19. ame ranal r gl 10 Enter radius of analysis region galmode i gl 1 0 3 Enter diffuse emission mode isomode i gl 1 0 3 Enter isotropic emission mode srclist s ql src_list txt Enter sources list outfile s ql my2src out Enter output file name ulc1 r q1 2 0 Enter upper limit confidence level locc1 r q1 5 99 Enter source location contour confidence level You can type the command AG multid at the command line and insert the requested pa rameters or insert the parameters as arguments of the procedure Here we provide an example of command line home adc GO_test_dataset gt AG multi4 maplist list txt sarfilesAG GRID GOO017 SFMG 10023 sai edpfilesAG GRID GOO017 SFMG 10023 edp gz psdfile AG_GRID_G0017_SFMG_10023 psd gz ranal 10 galmode 1 isomode 1 srclist src_list txt outfile mysrc out ulcl 2 0 loccl 5 99 AG multi4 prints most of its messages to the standard output Looking at the screen output one can follow each step of the fitting process Most messages are sent to the standard output while the error and warning messages will go to the standard error Some errors are fatal and the application will stop in this case Most fatal errors are about an inconsistent set of input values Screen output dept AE AE Y AE AE AE AU AE AE AE AE AE AE Y AU Y DS Y AE AE AU AE AE AE AE AE AE AE AE AE AE AE AU AM AE AE AE AM AM AE AE AE AL AE AE AE AE AE Y AE AE AE AE AE AM AM AE AE AE AE AE AE AE AI HULE HIE IE IE HIE IE IE HEHE IE
20. an ellipse of the confidence contour level of the previous point in ds9 format a ds9 region file with the ellipse of the previous point Use this file only for display purpose Example of additional output file for each source Label Fix index UL conf level srcloc conf level sqrt TS L B Counts Err Err Err UL Flux Err Err Err UL 21 2 2 1 2 5 99147 40 6372 263 523 2 90138 1183 54 48 5613 49 0616 48 063 1282 66 9 0413e 06 3 70971e 07 3 74793e 07 3 67164e 07 9 79849e 06 As before the lines beginning with are comments to aid the reader The first line gives the name of the source followed by some input parameters fixflag spectral index upper limit confidence level source location confidence level The second line is the sqrt TS The third line give the galactic coordinate of the source The fourth line gives the counts with errors and the fifth line gives the flux with errors Note that in every case the symmetric and asymmetric errors and the upper limits are provided AGILE Team 37 37
21. at this parameter suffers from the bug noted in section Known Issue 4 spectral index spectral index of the source used to calculate the PSF 5 fix 0 leave fixed both the flux and position of the source 1 optimize the flux of the source while leaving the position fixed 2 optimize both the flux and the position of the source Note that the initial TS of the source must be above both min T S and loccl in order for the position to be optimized 6 minTS if the YES of the source is initially below this value and fix gt 1 its flux will be set to zero during the analysis of the other sources 7 label A unique string without spaces It will be used as part of an output filename Note that minTS is expressed as sqrt TS as is the case for outputs on the screen and in output files outputs You can type the command AG_multi2 at the command line and insert the requested pa rameters or insert the parameters as arguments of the procedure home adc GO_test_dataset gt AG_multi2 Enter exposure file name VELA exp gz Enter counts file name VELA cts gz Enter diffuse map file name VELA gas gz Exposure Correction file name ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 expcorr gz Enter source list vela multi Enter output file name vela res Enter minimum energy 100 AGILE Team 34 34 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Enter maximum energy 50000 Enter radius o
22. bove the significance threshold With a pre defined list of sources AG_multi4 tries to mimic this process internally instead of immediately fitting all sources on the list simultaneously it performs the following steps 1 Add the fix 0 sources immediately 2 Set the fluxes of the fix gt 1 sources to 0 3 Fixing the position optimize the flux of the source with the highest initial flux guess 4 If fix 2 and the significance is high enough optimize the position 5 If the significance is not high enough set the flux to zero for subsequent sources otherwise set it to the optimized flux level but leave it free to vary 6 Follow steps 3 5 for the remaining sources in order For each source fix the flux of sources outside the corresponding region of interest during the analysis 7 Repeat steps 3 6 this time calculating upper limits and contours Calculate errors and upper limits even for sources with fix gt 1 whose fluxes have been set to zero 8 Write output files In the Galactic plane it is almost always advisable to use a predefined list of nearby sources 8 3 Example 3 Light curve To find the light curve of a source over a given time period first perform an analysis over the whole time interval letting the diffuse coefficients isotropic for high latitude sources both Galactic and isotropic for low latitude sources and if desired the position vary Then perform the analysis for each time bin fixing both the diffuse coefficien
23. ded into two sections input and output The input section contains three subsections the command line options the map list and the source list contents The command line options are listed in two tables one with the names of the PSD SAR and EDP files the other with the rest of the command line The maplist subsection also contains two tables The first lists the mapfile contents and the second contains AGILE Team 28 28 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 the data from the map files themselves The last table of the input section contains the source list contents The output section is also divided into three subsections The first is a table showing the Galactic and isotropic coefficients and their errors Also in this table some cells may be grouped together when the values are all the same The second is a table showing the fit results for the sources and their errors One of the listed values is the contour equivalent radius explained in the next section The last table shows the source flux per energy channel and it is present only when different energy channels are considered This table has one row for each source and one column for each energy channel 7 11 Ellipse fit to source location contour If AG_multi4 was able to find a source contour an ellipse is fit to the contour The source contour is a list of points which defines a polygon by connecting each point sequentially The value of Radius found in the HTML o
24. e library PIL devel oped by the INTEGRAL Science Data Center ISDC Each command line option is de AGILE Team 20 20 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 scribed by a par file AG_multi4 par in this case a sample of which comes with the dis tribution The environment variable PFILES should be defined in your account pointing to the directory where the file AG_multi4 par resides The user may specify the option val ues on the command line in two ways One is to specify the option name and its value in any order the other is to give just the option values in the order they appear in the par file For example AG_multi4 optioni valuel option2 value2 option3 value3 or AG_multi4 valuel value value3 Otherwise if any of the command line options are miss ing AG_multi4 will prompt the user to either confirm the previously used value or to provide a new one The values used in the current session will be stored and used in the next session This behaviour depends on the par file that comes with the distribution which the user may change Refer to the PIL library online documentation for all the details This is the list of the program options required in the order they are expected Each option can be a number or a string string maplist name of a text file containing the list of the maps An explanation of this file and its syntax is given below string sarfile One of three calibration files required This file con
25. e user can change the parameter explicitly providing it on the command line The input and output files are in FITS format FITS files can be read and modified by standard tools such as fv and the output maps generated by the tools can be displayed with the ds9 tool 3 The Exposure Map Generator Task Exposure maps are generated by the procedure AG expmapgen the executable can be found in ADC scientific analysis bin AG expmapgen reads the auxiliary LOG files listed in the GRID LOG index integrates the exposure between tmin and tmax and outputs a FITS image file Each row of the index file is a GRIDLOG file followed by the minimum and maximum times contained in the GRID LOG file The index file may list multiple GRID LOG files Sample GRID LOG index file agstd_GridLog log 0 000000 32400 000000 LOG AGILE Team 5 5 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 150 200 250 300 350 Figure 1 DS9 image of an exposure map produced by AG_expmapgen The image is a two dimensional array in either the ARC or AIT projection The projection size and resolution and center and rotation of the map in Galactic coordinates tmin tmax emin emax andspectral index are specified in the AG_expmapgen par parameter file along with various integration parameters fovrad fovradmin albrad y tol roll tol earth tol phasecode and spatial and temporal interpolation step sizes step timestep The interpolation p
26. er roll tolerance degrees keepmono b hl no Keep monochromatic exposure maps yes or no phasecode i h1 2 Orbital phase code projection s ql ARC Enter projection ARC or AIT step r ql 4 Enter step size timestep r ql 160 Enter LOG file step size You can type the command AG expmapgen at the command line and insert the requested parameters or insert the parameters as arguments of the procedure Here we provide an example of command line home adc GO test dataset AG expmapgen logfile 0LOG test 5 0 index outfile map exp raeffFileNames ADC scientific analysis data AG GRID GOO017 SFMG 10023 sar gz mdim 30 mres 0 3 la 263 55 ba 2 787 lonpole 180 tmin 111844735 tmax 112103935 emin 100 emax 50000 index 2 1 fovrad 50 fovradmin 0 albrad 90 y_tol 0 5 roll_tol 360 0 earth_tol 5 0 keepmono NO phasecode 2 projection ARC step 2 timestep 160 outputs Screen output UH jf tf tf J Jf tr u HAAT HYT TT TT TE TE TE TT TE TE TT TT TE HHHHH AG expmapgen cpp V2 2 31 07 2009 A C A T A B T C ER AAN LY TTT L LHL HI PITT Mm TT top tp df df LE H HH HHHH TTP TP TP TP TP TPT 7 LL T LLH HYT dd HE LL TTT pope pp dp pf AE AE pp pp df AE AE AU 3 AA AE AE Y AM AU AE AE MH AE AU AE dy MH AE AM AE AE MH AL AE AE AE AM AA 1 T JH AE AE AU AE AU AE AE AM E yp HAHA TT TT TE TT TE TP TT TE TT TPT H AE MH fy MH AE AE AM AA HI HAI HI TT TT TE TE TT TE TE TE TT
27. es are considered fixed while negative values are free to vary starting from their absolute values These coefficients are affected by the galMode and isoMode you have given in the command line according to the following table mode 0 all the coefficients are fixed to their initial absolute values mode 1 all the positive coefficients are fixed while the negative ones are variable normal behaviour mode 2 all the coefficients are variable regardless of their sign mode 3 all the coefficients are variable but their relative proportion is fixed according to their initial values For example if two maps have 1 and 2 as initial values of isoCoeff and isoMode 3 the final coefficient may have final values of 3 and 6 maintaining a fixed ratio of 1 2 7 5 The Source List The source list is a text file listing at least one source Each line of text describes one source and it is possible to include empty lines or comment lines The comment lines begin with an exclamation mark Each source is described by a line containing space separated values in the following order lt flux gt lt 1 gt lt b gt lt spectral index gt lt fixFlag gt lt minSqrt TS gt lt name gt location limitation Because the values in each line are separated from one another by a space they may not themselves contain a space The first 4 values flux in cm s galactic longitude and latitude in degrees and spectral index of each source represen
28. f analysis region 10 Enter diffuse emission coefficient 999 Enter isotropic coefficient 999 Enter upper limit confidence level 2 0 Enter source location contour confidence level 5 9914659 Galactic longitude of instrument pointing direction 999 Galactic latitude of instrument pointing direction 999 Screen output HERRIE RIES IRIS RR RRERO HE FERRORO HORROR HERRERO RI RR RR RR HORARIA RR HR HR RR RR HHHHHHHHHH AG multi2 cpp B18 22 04 2009 A C T C A T HHH HERRIE RR R RR R IRIS RR R HR RE HI R HR RR RI RR RR RHR RR HR HR HR RR RR HERRIE RIES IRIS R HR RR RI RE HI R HR RE RI RR RR RR RR RR HR HR HR RR RR INPUT PARAMETERS Exposure file name VELA exp gz counts file name VELA cts gz diffuse map file name VELA cts gz SAR file name ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 sar gz EDP file name ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 edp gz PSD file name ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 psd gz Exposure Correction file name ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 expcorr gz minimum energy 100 maximum energy 50000 Radius of analysis 10 Diffuse emission coefficient 999 Isotropic coefficient 999 Upper limit confidence level 2 Location contour confidence level 5 99147 Pointing direction 999 999 source list vela multi Output file name prefix vela res Galactic longitude of instrument pointing directi
29. ganized as lists of photons from the start of the mission until the last released data The list of photons is provided in the event files EVT The events provided within the event files are G S L Normally the AGILE team use the G class for the analysis Only for gamma ray bursts and pulsar timing analysis are the G S and L classes used To know where AGILE is pointed at a given time and when the spacecraft operates nominally the auxiliary LOG files are provided The scientific tools take the events and LOG files as basic input for the analysis The event and LOG files are in FITS format FITS files consist of a series of units each containing a header and data Each header contains a list of keywords and their values which describe the format of the data The first unit is the primary unit and may or may not contain data The subsequent units are called extensions The version number of the AGILE data processing is the value of the keyword OBSW_VER in the FITS header of the EVT files e g OBSW_VER 3_18_17_16 OB SW version PipeOB_B SCI_B STD_B COR means the version of the ADC pipe is 3 the version of scientific analysis integrated into the AGILE Team 4 4 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 ADC pipeline is 18 and the version of the standard analysis that has produced the data is 17 The last number is the version of correction software 2 3 AGILE Science Tools The AGILE Science Tools
30. gz Exposure Correction file name expcorr fits gz Radius of analysis 10 Galactic parameter mode 1 from file Isotropic parameter mode 1 from file Sources list src_list txt Output file name prefix my2src out AGILE Team 25 25 AGILE GRID SCIENTIFIC ANALYSIS User Manual 7 3EGJ0859 4257 f 2 8e 07 free 8 3EGJ0859 4257_x 2 fixed 9 3EGJ0859 4257_1 264 64 fixed 10 3EGJ0859 4257_b 2 02 fixed Begin first loop Considering source 1 VelaPSR Source 1 VelaPSR Flux free position and index fixed Fitting of source 1 Flux free FCN 1850 56 FROM IMProve STATUS RESET 8 CALLS 119 TOTAL EDM 1 70305e 11 STRATEGY 1 ERROR MATRIX UNCERTAINTY 50 0 per cent EXT PARAMETER APPROXIMATE STEP FIRST NO NAME VALUE ERROR SIZE DERIVATIVE 1 Galactic 4 45914e 01 2 08769e 01 2 08769e 03 2 91695e 05 2 Isotropic 1 99151e 00 4 55797e 01 4 55797e 03 2 30105e 05 3 VelaPSR f 8 06342e 00 1 11869e 00 1 11869e 02 1 10773e 08 4 VelaPSR x 1 70000e 00 fixed 5 VelaPSR 1 2 63550e 02 fixed 6 VelaPSR b 2 79000e 00 fixed 7 3EGJ0859 4257 f 0 00000e 00 fixed 8 3EGJ0859 4257 x 2 00000e 00 fixed 9 3EGJ0859 4257 1 2 64640e 02 fixed 10 3EGJ0859 4257_b 2 02000e 00 fixed Fitting done in 120 iteration Result 4000 omissis Fitting done in 666 iteration Result 4000 0 440086 1 97711 8 14638 1 7 263 545 3 03356 1 35525e 12 2 264 64 2 02 SrcCount 2 m_galParCount 1 m_isoParCount 1 Source 1 0111 Source 2 0011 m_binCo
31. ibing the most relevant results for all the sources and a set of source specific files containing more detailed data about that source One of the two main files is in HTML format and it includes both the input and output data grouped in tables Having a look at this file the user should guickly understand the outcome of the fitting process and its main results The next section describes the HTML output in more detail The second of the two main files contains the same data printed in the HTML file but in text format making it is easy to pass it as input to another application for further processing This file is divided in two sections The first contains one line for each diffuse component and the second one line for each source The first line of each section begins with an exclamation mark a comment line for many applications labeling the values printed beneath In each line the values are separated by a space This is an example of text output in which three sets of maps and one source are used The diffuse components coefficients are allowed to vary freely for each set of maps The symmetric positive and negative errors are provided The flux and position of the source are allowed to vary while the spectral index is fixed The name significance of the source detection position source counts with error source flux with error and spectral index with error are provided In this case because the source spectral index is fixed its error
32. iffusefile 100_50000 0 5 SFMG_10023 disp conv sky gz hiresdiffusefile 100_50000 0 1 SFMG_I0023 disp conv sky gz outputs Screen output dept ff ty dp AE AE AE pp pp AE AE AE AE AE AE AU AE AE AE AE AU AE AE AE AE AE AE AE AE AE AE AE AU AU AE AE AE AU AM AE AE AE E AE AE AE AE AE AE AE AE AE AE AE AM AM AE AE AA AE AE AE AI HUUR IE IE HE HIE IE IE HEHE IE HEI HIE HEI IE II HIE IE HEI HIE HE HEI HIE HE IE II HE IE HE HIE IE HEI IE IE T TIETE TE TP TP TE TP TE TIETE II TIETE III TE IE II TE II TIETE IE III TE IE TIETE II TIETE III TE IE III II TEI TE IE IT II TE IE TR WAL dy de HY A Ae de He AL a Le te Ae He Ae LL ALH Th TP TP TP TP ATP TP TP TP TN AG_gasmapgen2 cpp v 2 10 10 10 J A C A T TN HAEHAA AE AE AE AE AE AE AE A dd AE AE AE AI HUUR III HIE IE IE HEI IE IE HEHE IE HEI II HIE IE IE IT HIE IE EIE HIE HE HEI HIE IE IE II HE IE HE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE TE TE NI TT TE TT IT II NI TE TT MI TT IT NT TE II TE TE IT TE TE TE TT TE TE TT TE TE NI TE IE NI TE IT TE TT DI NI II MI NI TT MI TE II TT TE NI TT TE IT TT TT dept AE AE AU AE AE AE pp AE AE AE AE AE AE AE AE AE AE AE AE AU AM AE AE AE AE AE AE AE AE AE AE AU AE AE AE AE AM AM AE AE AE AL AE AE AE AE AE AE AE AE AE AE AE AM AM AE AE AE AE AE AE AE AI HUUR IE IE HIE IE HEI HEHE IE HEI HIE HEI IE II HIE IE HEI HIE HE HEI HIE IE IE IE HE IE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE IT FE NT TT TE TT IT N NI TE TT NI TT I
33. is set to zero DiffName Coeff Err Err Err Galactic_1 1 0497 0 0293663 0 0293867 0 0293513 Galactic_2 0 903874 0 0309914 0 0310404 0 0309524 Galactic_3 0 445709 0 0403257 0 040476 0 0401969 Isotropic_1 6 19155 0 17882 0 17929 0 178379 Isotropic_2 1 61033 0 0750936 0 0754122 0 0747974 Isotropic_3 0 599942 0 0449255 0 0452161 0 0446586 SrcName sqrt TS L B Counts Err Flux Err Index Err 1AGL JO835 4509 149 957 263 574 2 84422 71782 858 393 6 05223e 06 7 23747e 08 1 66 O AGILE Team 27 27 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 For each source an additional text file is generated and when possible additional files describing the source contour The text file contains some comment like lines first character is an exclamation mark labeling the values printed beneath This is an example of text output consistent with the example given above Label Fix index UL conf level srcloc conf level sqrt TS L_peak B_peak L B r a b phi Counts Err Err Err UL Flux Err Err Err UL Exp Index Err 1AGL_J0835 4509 3 1 66 2 5 99147 149 957 263 574 2 84422 263 574 2 84126 0 0127191 0 0101623 0 0160235 35 4372 71782 858 393 861 055 855 729 1727 97 6 05223e 06 7 23747e 08 7 25991e 08 7 21501e 08 1 45692e 07 1 18604e 10 1 66 0 The values L_peak and B_peak are set to the initial values if the source location is fixed If it is allowed to vary then they are set
34. mapEen re ia ia starting AGAIN EMAPEN rot a e exiting HHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHH HHHHHHHHH Task AG_intmapgen exiting HHHHHHHHHHHHHHHH HHHHHHHHA HEHEHE III RI IR III III IR RR RR RI III RR RR RR RR RR RR RR AGILE Team 15 15 AGILE GRID SCIENTIFIC ANALYSIS User Manual Intensity Map sample header SIMPLE T file does conform to FITS standard BITPIX 64 number of bits per data pixel NAXIS 2 number of data axes NAXIS1 134 length of data axis 1 NAXIS2 134 length of data axis 2 EXTEND T FITS dataset may contain extensions COMMENT FITS Flexible Image Transport System format is defined in Astronomy COMMENT and Astrophysics volume 376 page 359 bibcode 2001A8A 376 359H CRVAL1 263 CRVAL2 2 6 CTYPE1 GLON ARC CTYPE2 GLAT ARC CRPIX1 67 1666666666667 CRPIX2 67 1666666666667 CDELT1 0 3 CDELT2 0 3 CUNIT1 deg CUNIT2 deg RADESYS FK5 EQUINOX 2000 LONPOLE 180 TSTART 111748135 OBT first event time TSTOP 112363135 OBTllast event time TIMESYS TT TIMEUNIT s MJDREFI 53005 MJDREFF 0 002354444444444444 TIMEZERO 0 TT DATE OBS 2007 07 13T12 00 00 start date and time of the observation TT DATE END 2007 07 24T12 00 00 end date and time of the observation TT MINENG 100 MAXENG 50000 TELESCOP AGILE INSTRUME GRID PIXCENT T YTO
35. meters iaa he Ose a RR A Rg 7 8 Task execution TO SOUT Ue Ae EA As ds DR EA ER ae a ee dl ss TAO HUMO bo ae a RAN a OE ORR OU 7 11 Ellipse fit to source location contour ar a ek a EP OR 8 Analysis procedure 8 1 Example 1 Isolated extragalactic point source o o 8 2 Example 2 Point source in the presence of other point sources 8 3 Example 3 Light curve N PER A e SURE WEER DS 8 4 Example 4 Spectra ER RD EA RE LE DR Rg DA N EE ore a So 8 5 Example 5 Dependence on off axis angle o o 9 Obsolete Likelihood Analysis Procedures 10 13 17 32 9 1 The Source Detection and Location Task Multiple Source Location Detection 32 AGILE Team 2 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 1 Introduction 1 1 Scope and Contents of this Document This document provides a user manual for the following packages 1 Scientific Analysis Counts Map Generator 2 Scientific Analysis Exposure Map Generator 3 Scientific Analysis Intensity Map Generator 4 Scientific Analysis Diffuse Map Generator 5 Scientific Analysis Likelihood Analysis Multiple Source Location Detection which pertain to the AGILE GRID Scientific Analysis subsystems described in RD 1 1 2 Reference Documents RDI1 Scientific Ground Segment Software Requirements and Architecture AGILE IFC SA 001 Issue 2 0 RDI2 GRID Standard Analysis User Manual and Test Procedures AGILE IFC OP 008 16 5 2005
36. ne starting from the position where the position may be a known counterpart or a peak in the counts or TS map Set the flux to any positive value spectral index to 2 0 Make sure to insert a label Note that for sources far from the Galactic plane it is inadvisable to allow both the Galactic and isotropic coefficients to be left free to vary because the two components are degenerate One can fix the Galactic coefficient to 0 7 and let the isotropic coefficient vary AGILE Team 29 29 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 Figure 5 DS9 image of a smoothed counts map of Vela with the ellipse fit to the 95 confidence contour level Unless the source has been previously identified due to correlated variability at other wave lengths e g a pulsar with known ephemeris or a variable AGN it is advisable to let the AGILE Team 30 30 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 source position vary to check whether the candidate counterpart lies within the 95 confidence contour 8 2 Example 2 Point source in the presence of other point sources For sources along the galactic plane or near other sources the situation is a little more compli cated In principle one should use an iterative process Find and optimize the most significant source by itself Then find the next most significant source in the region and write a list with the first source and this additional source Continue until no new sources are a
37. on Galactic latitude of instrument pointing direction image read OK Source creation Parameters O 263 65 2 95 2 1 2 2 21 O 260 35 0 35 2 1 2 2 22 O 270 55 0 36 2 1 2 2 23 O 268 46 4 14 2 1 2 2 24 AGILE Team 35 286 419 1 896 35 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 O 267 56 4 74 2 1 2 2 25 O 261 53 11 65 2 1 2 2 31 Diff Component 0 fixflag 1 param 0 released max set to 100 param 0 set to 1 Diff Component 1 fixflag 1 param 1 released max set to 100 param 1 set to 1 HHEHHHHHHHHEEHHHEHEHHAEHHHHHHEE HI RT RR RR IR RE HI R RARO RI RR RR RR HR IR HR HHHHHHHHH Task Multi exiting H HHHHHHHHHEHHHE HERRIE RR SIR RI RR RI RE HI RR RI RR RI RR RR RR RR RR HR HR HR RR RR Output File AG multi 2 writes its output to a text file whose name is specified by the outfile parame ter in the parameter file Example Gascoeff Coeff Err Err Err 0 742128 0 065269 0 0654482 0 0651016 Isocoeff Coeff Err Err Err 5 17523 0 779803 0 786474 0 773244 21 sqrt TS L B Counts Err Flux Err 22 sqrt TS L B Counts Err Flux Err 23 sqrt TS L B Counts Err Flux Err 24 sqrt TS L B Counts Err Flux Err 25 sqrt TS L B Counts Err Flux Err 31 sqrt TS L B Counts Err Flux Err 21 40 6372 263 523 2 90138 1183 54 48 5613 9 0413e 06 3 70971e 07 22 1 40721 260 35 0 35 22 7524 17 4484 1 79216e 07 1 37437e 07 23 1 92633 270 55 0 36 33 45
38. onvolved with the energy dependent point spread function and combined into predefined observed energy ranges according to the appropriate energy dispersion function for G events using the FM background filter AGILE Team 17 17 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 The diffuse emission map should be selected based on the energy range of the analysis If the analysis is performed between 100 MeV and 50 GeV select the file 100_50000 0 5 SFMG_10023 disp conv sky gz for the diffusefile parameter and 100_50000 0 1 SFMG_10023 disp conv sky gz for the hiresdiffusefile parameter The first number in the file name is the minimum energy and the second number is the maximum energy Note that 0 1 degrees is the bin size of the diffuse emission map at low latitudes while 0 5 degrees is the bin size of the diffuse emission map at high latitudes inputs AG_gasmapgen2 par expfile s ql map exp Enter exposure file name outfile s ql map gas Enter output file name diffusefile s ql 100_50000 0 5 5FMG_10023 disp conv sky gz Enter diffuse model file name hiresdiffusefile s ql 100_50000 0 1 SFMG_I0023 disp conv sky gz Enter high res diffuse model file name You can type the command AG_gasmapgen2 at the command line and insert the requested parameters or insert the parameters as arguments of the procedure Here we provide an example of command line home adc GO_test_dataset gt AG gasmapgen expfile map exp outfile map gas d
39. orrfile s ql ADC scientific_analysis data expcorr fits gz Enter Exposure Correction file name Emin r q1 100 0 Enter minimum energy Emax r q1 50000 Enter maximum energy ranal r q1 10 0 Enter radius of analysis region gascoeff r ql 999 Enter diffuse emission coefficient isocoeff r ql 999 Enter isotropic coefficient srclist s ql Vela_multi det Enter source list outfile s ql Velamulti res Enter output file name ulc1 r q1 2 0 Enter upper limit confidence level locc1 r q1 5 9914659 Enter source location contour confidence level lpoint r 1 999 Enter galactic longitude of instrument pointing direction 999 for undefined bpoint r 1 999 Enter galactic latitude of instrument pointing direction 999 for undefined The first six parameters should be familiar The expcorrfile parameter specify a file that contains the correction of the flux based on the off axis angle Note that gascoeff and or isocoeff may be set to a fixed value or set to 999 to find the optimum non negative value srclist is a new input parameter while the remaining three are new output parameters The outfile parameter is a string which is both the name of an output file and the prefix for other output files The ulcl parameter is the confidence level for flux upper limits These upper limits are cal culated for all sources with fix gt 1 no matter what their significance level Like minTS it is ex pressed as sqrt TS
40. rocedure is a linear interpolation method in which only one bin each N is calculated where N is the step size parameter A spatial interpolation width of 2 is sufficient for a good approximation of the exposure map implying step 4 for a bin size of 0 5 or step 8 for a bin size of 0 25 Figure 1 shows the image produced by DS9 for an exposure map generated by AG_expmapgen with Galactic coordinate axes displayed AGILE Team 6 6 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 inputs AG_expmapgen par logfile s ql Log index Enter grid log index file name outfile s gql map exp Enter output file name raeffFileName s hl AG_GRID_GO017_SFMG_I0023 sar gz Enter effective area file name mdim r ql 120 5 Size of Map degrees mres r ql 0 5 Bin size degrees la r q1 101 45 Longitude of map center Galactic ba r ql 0 81 Latitude of map center Galactic lonpole r h1 180 Rotation of map degrees tmin r gl 0 Enter initial time sec tmax r q1 32400 Enter final time sec emin r q1 100 Enter minimum energy emax r q1 50000 Enter maximum energy index r ql 2 1 Enter spectral index fovrad r ql 50 Enter max off axis angle degrees fovradmin r ql 0 Enter min off axis angle degrees albrad r h1 90 Enter radius of earth albedo degrees y tol r hl 0 5 Enter boresight movement tolerance degrees roll_tol r hl 360 Enter roll tolerance degrees earth_tol r hl 5 0 Ent
41. seen above during the fitting process some values are fixed and others are variable depending on the values of the flags The execution time strongly depends on the number of the variable parameters It is not possible to predict how long the fitting process will last or how it depends on the number of parameters but the dependence is not linear If all the diffuse coefficients are variable and all the fix flags are set to 7 for M maps and S sources the number of variable parameters will be 2M 4S In the case of many maps and many sources this may lead to a very long execution time The fitting process takes place in two steps according to the method of Maximum Likeli hood During each step all the sources are considered one by one and several fitting attempts are performed by invoking the function TH1D Fit provided by the ROOT library developed by CERN The user will see on the screen the output printed by that function and will find the related documentation on the CERN web site AGILE Team 24 24 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 inputs AG multi4 par maplist s ql list txt Enter maps file name sarfile s hl AG_GRID_G0017_SFMG_10023 sar gz Enter SAR file name edpfile s hl AG GRID GOO17 SFMG 10023 edp gz Enter EDP file name psdfile s hl AG GRID GOO017 SFMG 10023 psd gz Enter PSD file name expcorrfile s hl ADC scientific analysis data expcorr fits gz Enter Exposure Correction file n
42. sk AG_multi4 for the scientific analysis The task AG multi has been provided only for backward compatibility 9 1 The Source Detection and Location Task Multiple Source Lo cation Detection This task is performed by the procedure AG multi 2 found in ADC scientific_analysis bin AG multi reads an exposure map produced by AG_expmapgen a counts map produced by AG ctsmapgen and a diffuse emission map produced by AG_gasmapgen2 spectral index and energy range as well as a text file containing a source list listed in the parameter file It calculates the test statistic significance counts and flux of each of the point sources starting from a given positions in the presence of simultaneously optimized fluxes of all nearby sources in the list and outputs the results to text files The main purpose is to optmize both the flux and position of the sources given as input inputs AG_multi2 par expfile s ql VELA exp gz Enter exposure file name ctsfile s ql VELA cts gz Enter counts file name gasfile s ql VELA gas gz Enter diffuse map file name sarfile s 1 ADC scientific_analysis data AG_GRID_G0017_SFMG_10023 sar gz Enter SAR file name edpfile s 1 ADC scientific_analysis data AG_GRID_G0017_SFMG_I0023 edp gz Enter EDP file name AGILE Team 32 32 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 psdfile s 1 S ADC scientific_analysis data AG_GRID G0017_SFMG_10023 psd gz Enter PSD file name expc
43. t the initial estimates of the values for that source According to the fix flag some or all of those values will be optimized by being allowed to vary The flux estimates are relevant in the fitting process as the sources are considered one by one starting with the one with the brightest initial flux value regardless of the order they are given in the source file The fix flag is a bit mask each bit indicating whether the corresponding value is to be allowed to vary 1 indicates the flux 2 the position and 4 the spectral index The user may combine these values but the flux will always be allowed to vary if at least one of the other values are Examples fixFlag 0 everything is fixed This is for known sources which must be included in order to search for other nearby sources fixFlag 3 flux and position variable index fixed fixFlag 5 flux and index variable position fixed fixFlag 7 flux position and index variable and also fixFlag 2 only the position is variable but AG multi4 will let the flux vary too so this is 2 AGILE Team 23 23 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 equivalent to 3 minSqrt TS is the minimum acceptable value for the square root of TS if the optimized significance of a source lies below this value the source is considered undetected and will be ignored set to flux 0 when considering the other sources After the name of the source which should not contain a space an optional
44. tains the effective area of AGILE GRID for a given filter and event type as a function of energy and direction in instrument coordinates string edpfile One of three calibration files required This file for a given filter and event type contains the energy dispersion function the observed energy distribution for measurements of photons of a given true energy as a function of direction in instrument coordinates string psdfile One of three calibration files required This file for a given filter and event type contains the point spread dispersion function the distribution of observed offsets from the true photon direction as a function of energy and direction in instrument coordinates string expcorrfile An optional file containing corrections to the effective area as a function of off axis angle Pro vided with the distribution it should not be changed by the user number ranal The analysis radius in degrees When considering a given source only the photons falling inside the radius will be considered and the flux location and spectral index of sources outside of the analysis region will be fixed number galMode number isoMode These two numbers wich range from 0 to 3 tell AG multi4 how to handle the Galactic and AGILE Team 21 21 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 isotropic diffuse components Refer to the maplist section for details string srclist The name of a text file containing the list of the
45. td_Grid EVT 0 000000 32397 000000 EVT The image is a two dimensional array in the ARC or AIT projection The projection size and resolution the center and rotation of the map in Galactic coordinates tmin tmax emin and emax are specified in the AG_ctsmapgen par parameter file along with various integration parameters fovrad fovradmin albrad phasecode and a filter code filtercode fil tercode 5 correspond to events classified as gamma G Figure 2 shows the image produced by DS9 for the counts map generated above with Galactic coordinate axes displayed inputs AG_ctsmapgen par evtfile s dl Evt index Enter event file index file name outfile s dl map counts Enter output file name mdim r ql 120 5 Size of Map degrees mres r ql 0 5 Bin size degrees la r q1 101 45 Longitude of map center Galactic ba r ql 0 81 Latitude of map center Galactic tmin r gl 0 Enter initial time sec tmax r q1 32400 Enter final time sec emin r q1 100 Enter min energy emax r q1 50000 Enter max energy fovrad r q1 50 00 Enter max off axis angle degrees fovradmin r q1 0 00 Enter min off axis angle degrees albrad r h1 90 00 Enter radius of earth albedo degrees lonpole r h1 180 Rotation of map degrees phasecode i h1 2 Orbital phase code filtercode i hl 5 Event filter code projection s ql ARC Enter projection ARC or AIT You can type the command AG_ctsmapgen at the command
46. time of the observation TT DATE END 2007 07 21T12 00 00 end date and time of the observation TT TIMEZERO 0 TT MJDREFI 53005 MJDREFF 0 000754444444444444 MINENG 100 MAXENG 50000 TELESCOP AGILE INSTRUME GRID PIXCENT T YTOL 0 5 Pointing direction tolerance deg ROLTOL 360 Roll angle tolerance deg EARTOL 5 Pointing direction tolerance deg STEP 2 Map interpolation step size TIMESTEP 160 Log file step size BUNIT cm 2 s sr FOV 50 Radius of field of view deg FOVMIN 0 Minimum off axis angle deg ALBEDO 90 Earth zenith angle deg PHASECOD 2 Orbital phase code INDEX 2 1 SC Z LII 289 698417511038 SC Z BII 0 718600555009459 SC LONPL 0 END All header keywords are standard FITS keywords except for SC Z LII SC Z BII and AGILE Team 9 9 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 SC LONPL which indicate the pointing direction and rotation of the spacecraft 4 The Counts Map Generator Task Counts maps are generated by the procedure AG ctsmapgen the executable can be found in ADC scientific analysis bin AG ctsmapgen reads the event files listed in the event file index bins the counts between tmin and tmax and outputs a FITS image file Each row of the index file is an event file followed by the minimum and maximum times contained in the event file The index file may list multiple event files Sample GRID EVT index file ags
47. to the position for which the TS is maximized If a confidence contour was found the parameters on the following line describe the best fit ellipse of the contour described in detail below The counts and fluxes are provided as well as their symmetric positive and negative errors if the flux is allowed to vary For convenience the exposure of the source used to calculate the source counts from the flux is also provided Finally the spectral index and its error if applicable are provided If source location was requested for a given source and a source location contour was found then three additional files are generated for that source These files are written using galactic coordinates in degrees and can be loaded by applications such as ds9 and overlaid on the maps provided as input to AG multi4 to visualize the source location contours One of the three files with extension con contains the source contour as found by the ROOT functions expressed as a list of galactic coordinates one point per line where the last line is a repetition of the first It may depict any shape The other two files describe the ellipse that best fits the contour One has extension ellipse con and represents the ellipse as a contour in a format analogous to that of the con file The other has extension reg and describes same ellipse by its axes and orientation See the section about the ellipse for more details 7 10 HTML output The HTML output file is divi
48. ts and the position to the values found over the longer integration This will allow the short time interval analyses to proceed even with low statistics AGILE Team 31 31 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 8 4 Example 4 Spectra A similar procedure can be used for spectral analysis Perform an analysis over the entire energy range to determine the Galactic coefficient if the source is low latitude and the position Then fix those values and perform a simultaneous analysis of multiple maps one for each energy band keeping the position and Galactic coefficient fixed to the values found over the whole energy range Note that because the isotropic component depends on the instrumental cosmic ray background the coefficients of the isotropic component in each energy band must be allowed to vary and cannot be determined through an analysis over the entire energy range 8 5 Example 5 Dependence on off axis angle For strong sources a more accurate determination of flux and possibly spectra may be obtained by producing separate counts and exposure maps using thin rings of off axis angle where fovradmin fovrad take on the values of 0 10 10 20 20 30 50 60 and are then analyzed simultaneously Here again the isotropic coefficients must be allowed to vary independently as they are a strong and unpredictable function of off axis angle 9 Obsolete Likelihood Analysis Procedures We strongly suggest to use only the ta
49. unt 3484 Source 1 with 10 21 3 8 08533 41 7 5 263 545 6 3 03356 7 1 35525e 12 82 9 264 64 10 2 02 likeWith 966 498 likeWithoutVar 1201 46 Source 1 without fixed 11 21 30 AGILE Team 26 Build 21 26 AGILE GRID SCIENTIFIC ANALYSIS User Manual Build 21 41 7 5 263 545 6 3 03356 7 1 85525e 12 8 2 9 264 64 10 2 02 likeWithoutFixed 996 14 TS 21 6775 0 TSf 7 69958 0 HAH AE AM MH AE AM MA 2 AM AA AE 2 E 2 ge AE MH AE AE AE MM AE MM dd LY LEAL AE AE EE ALE AM ALA AM MAMA A AAA AE AE MH AL Le Hy HIE III IE III II HE HIE HE HE HIE HEI EIE HE HEI IE HE HE HIE HEI HIE HEI III HIE EIE HIE HE IE IE T TIETE IT TIETE TT TP TP TIETE TE II TIETE III TE IE II TEI TE II T Wed dy dy HY Ae Ae de de AL TE Ue te Ye He Ae Ye de He Ye Ye A Ye A A A A A AL H Th TP TP TP TP TP TP ATP TP Task AG_Multi4 exiting Th TP TP TP TP TP TP TP TP TP TP TP TP TP TP TP TP TR WAL Ay de A A Ae A A HE MM Ak AL AL A ke AL AL HEHE A AE HE kk A AL HE ke ke A AL HE MM LL Uk AL AL EE HE MM HEHE LL AA AA AL HE LL MM LL HL HUUR IE IE HE HIE IE HEI HEHE IE HEI HIE HIE IE II HIE IE HEI HIE HE HEI HIE IE II EIE HE IE HEHE HIE HE HEI IE IE T TT TT TE TE TE TE TE TE TT TP TE TT TE NT TT TE TT IT N NI TE TT NI TT IT NI TE II TE TE IT TE TE TE TE TE TE TT TE TE NI TE TE NI TT IT TE TT DI NI II MI NI TP MI TE II TT TE TT TT TE IT TT TT 7 9 Output At the end of the fitting process AG multi4 generates two main files descr
50. utput is the radius in degrees of a circle with the same area as the polygon AG_multi4 determines the ellipse which best fits the contour This ellipse will have the same area as the polygon and the distance between each contour point and the intersection between the ellipse and the line connecting that point to the centre will be minimized The ellipse is completely described by three parameters the two axes and the rotation in degrees of the first axis around the centre as expected by the ds9 application If the ellipse is a circle its axes will both be equal to the Radius found in the HTML output The ellipse is described by two files that are readable by ds9 one is a reg file which contains the centre the axes and the rotation of the ellipse while the other describes the same ellipse as a list of points in galactic coordinates thus using the same syntax of a contour file and has extension ellipse con This is an example of ellipse reg file galactic ellipse 263 579 2 8398 0 0167177 0 0205552 22 3895 Figure 5 shows a smoothed counts map of Vela with the ellipse fit to the 95 confidence contour level The image was generated by DS9 superimposing an output file of type ellipse con generated by AG_multi4 8 Analysis procedure 8 1 Example 1 Isolated extragalactic point source For sources far from the galactic plane and isolated sources analysis is relatively straightfor ward In AG_multi4 one can use a source list with one li
51. value for the location limitation in degrees may be provided If this value is present and not zero the longitude and latitude of the source will not be allowed to vary by more than this value from its initial position 7 6 Calibration Files The parameters sarfile edpfile and psdfile provide the names of the three calibration files These files are described in detail in other documents and are provided with the distribution They are FITS files whose common prefix specifies the filter and event type used and whose suffixes are sar gz edp gz and psd gz respectively Ordinarily they should not be changed by the user The parameter expcorrfile provides a correction factor as a function of off axis angle for older calibration files It should not be changed by the user 7 7 Analysis parameters The parameters ulcl and loccl will typically have the values 2 0 2 sigma upper limits and 5 99147 95 confidence contour respectively but may be changed by the user for use in for example light curves e g ulcl 1 or cases in which the 95 contour cannot be calculated e g loccl 2 29575 The parameter ranal should be the smallest value consistent with 1 the angular extent of the point spread function in the given energy range and 2 the distance to nearby strong sources In most cases no more than 10 degrees will be required and in many cases it is possible to use a smaller value such as 5 degrees 7 8 Task execution As we have
52. verts the gamma rays in heavy Z material layers 245 um of Tungsten 0 07 Xo into an electron positron pair of Minimum Ionizing Particles MIP corresponding to a most probable value of 110 keV in the detector and records the electron positron tracks through a combination of Silicon microstrip detectors and associated readout A GRID event is a collection of all the electron positron interactions in the microstrip detector called clusters with additional information from energy deposits in the MCAL bars and the configuration of the AC plastic scintillators if present A complete representation of the event topology allows the reconstruction of the incoming direction and energy of the gamma ray 2 2 Event classification and standard data format A set of different on board triggers enables the discrimination of background events mainly cosmic rays in the AGILE Low Earth Orbit from gamma ray events These data are sent to Earth where the AGILE Data Center ADC hosted at the ASI Science Data Center ASDC processes these GRID events with an additional on ground filter and provides a classification of each event P events classified as a charged particle and rejected G events classified as gamma ray photons This is the most useful class for the analysis S events classified as single track this is a special class of events with no separation between the electron and positron tracks L event not classified The AGILE data are or

DOCUMENT TYPE: Software User Manual TITLE: GRID - Agile

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