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Last modified: 5 April 2010
Where are the PDFs?

LETG/ACIS-S Grating ARFs

CIAO 4.2 Science Threads



Overview

Last Update: 5 Apr 2010 - updated for CALDB 4.2.1: calibration update - the LETG grating efficiency has been upgraded to vN0006.

Synopsis:

fullgarf is a script that creates a grating ARF for a particular order and grating of an observation. While the mkgarf tool will create a grating ARF for an individual chip given an aspect histogram, this script creates ARFS for each chip, creating aspect histograms as necessary. The script then combines the individual ARFS into one for the full array.

Purpose:

To create grating ARFs for an LETG/ACIS-S observation.

Read this thread if:

you are working with an LETG/ACIS-S observation and intend to model and fit the spectra.

Calibration Updates:

Related Links:




Contents



About the Chandra Grating Data Archive and Catalog

The Chandra Grating Data Archive and Catalog (TGCat) is a browsable interface to analysis-quality spectral products (binned spectra and corresponding response files). TGCat makes it easy to find observations of a particular object, type of object, or type of observation, to quickly assess the quality and potential usefulness of the spectra with pre-computed graphics or custom-generated plots of binned and combined counts or fluxe spectra. Spectra, responses, event files, and summary products may be downloaded as a package.

TGCat runs standard CIAO tools, but also includes customized extractions for non-standard cases to refine the zeroth order position or to use regions appropriate for extended sources. Non-standard extractions details are provided in "verification and validation" comments for users.

Most public grating observations are available and new ones are added soon after they are released. See the list of of observations not included for exceptions. Many of the observations currently in this list will be included when we add enhanced processing for more difficult cases (multiple sources, very extended sources).

Please consider using the spectrum and responses (PHA, ARF, and RMF files) from TGCat in your analysis.



Get Started

Sample ObsID used: 1198 (LETG/ACIS-S, 3C 273)

File types needed: evt2; pha2; asol1; bpix1; msk1; pbk0

If you created a new bad pixel file by running the New ACIS Bad Pixel File: Identify ACIS Hot Pixels and Cosmic Ray Afterglows thread or the Customizing an ACIS Bad Pixel File thread, use that file in this analysis. Otherwise, use the bpix1.fits file from the Archive. Make sure that you have set up ardlib to use the same bad pixel file.

It is assumed that you have created a gRMF for your observation by running the Create Grating RMFs for ACIS-S Observations thread, which is called rmf.fits.

Download the script

This thread uses the fullgarf script; for information about the script, consult the help file ("ahelp fullgarf"). The script is part of the CIAO Scripts distribution. The CIAO scripts package should be the following version or newer:

unix% cat $ASCDS_CONTRIB/VERSION.CIAO_scripts
01 Jun 2009

Please check that you have at least this version of the scripts package installed before continuing. If you do not have the scripts installed or need to update to a newer version, refer to the Scripts page.


Using the mask file

To make sure that the gARF file is correct, set the maskfile parameter to the observation-specific msk1.fits file. If you are working with continuous-clocking (CC) mode data, be sure to read the ACIS Pipeline-Processed Mask Files caveat as well.



Determine the Orders of the Observation

An ARF needs to be calculated for each order in the observation. We can use Prism to examine the pha2 file and determine how many orders there are:

unix% prism acisf01198N002_pha2.fits &

The tg_m column indicates the order of the observation (+/- 1, +/- 2, +/- 3) and the tg_part column indicates the grating (1 = HEG, 2 = MEG, 3 = LEG). The six rows (all +/- orders for LEG) for the LETG observation are shown in Figure 1.



Run fullgarf

It is necessary to run fullgarf for each order that will be modeled, up to six times (once for each row in the PHA file).

For row 2, LEG, order = -2:

unix% punlearn fullgarf
unix% pset fullgarf phafile=acisf01198N002_pha2.fits
unix% pset fullgarf pharow=2
unix% pset fullgarf evtfile=acisf01198N002_evt2.fits
unix% pset fullgarf asol=@pcad_asol1.lis
unix% pset fullgarf engrid="grid(rmf.fits[cols ENERG_LO,ENERG_HI])"
unix% pset fullgarf dtffile=")evtfile"
unix% pset fullgarf badpix=acis_1198_new_bpix1.fits
unix% pset fullgarf maskfile=acisf01198_000N002_msk1.fits
unix% pset fullgarf pbkfile=acisf063833861N002_pbk0.fits
unix% pset fullgarf dafile=CALDB
unix% pset fullgarf rootname=acisf01198

In many cases, there will be more than one aspect solution file (pcad_asol1.fits) for an observation. All the files must be input to the asol parameter, either as a list or a stack. Here we use:

unix% cat pcad_asol1.lis
pcadf063832996N002_asol1.fits

Now run the tool:

unix% fullgarf
Will use /home/username/cxcds_param4/fullgarf.par for the parameter file.
   
/home/username/cxcds_param4/fullgarf.par contains 15 parameters . . . 
   
Input PHA file (Type I or II) (acisf01198N002_pha2.fits): 
Row in Type II PHA file (ignored if Type I) (0:99) (2): 
Event file  (acisf01198N002_evt2.fits): 
Aspect offsets file (@pcad_asol1.lis): 
Energy grid spec (grid(rmf.fits[cols ENERG_LO,ENERG_HI])): 
Dead time correction factor; ACIS->evt file; HRC -> dtf file (')evtfile'): 
Bad pixel file; (filename|NONE|CALDB) (acis_1198_new_bpix1.fits): 
Output rootname (acisf01198): 
NONE, or the name of the parameter block file (acisf063833861N002_pbk0.fits): 
NONE, or name of ACIS window mask file (acisf01198_000N002_msk1.fits):    
Getting the pha file type . . .

Grating arm is LEG, order=-2  
Source location is X=4162.240234375, Y=4084.679931640625
  
Detector is ACIS 
Will run asphist for ccd_id= 4 5 6 7 
  
   
asphist infile=@pcad_asol1.lis outfile=acisf01198_ah4.fits 
evtfile=acisf01198N002_evt2.fits[ccd_id=4] dtffile=acisf01198N002_evt2.fits
   
asphist infile=@pcad_asol1.lis outfile=acisf01198_ah5.fits 
evtfile=acisf01198N002_evt2.fits[ccd_id=5] dtffile=acisf01198N002_evt2.fits
   
asphist infile=@pcad_asol1.lis outfile=acisf01198_ah6.fits 
evtfile=acisf01198N002_evt2.fits[ccd_id=6] dtffile=acisf01198N002_evt2.fits
   
asphist infile=@pcad_asol1.lis outfile=acisf01198_ah7.fits 
evtfile=acisf01198N002_evt2.fits[ccd_id=7] dtffile=acisf01198N002_evt2.fits
   
Finished creating aspect histograms for ccd_id= 4 5 6 7 
Will run mkgarf for the same ccd_id list 
   
mkgarf detsubsys=ACIS-S0 order=-2 grating_arm=LEG outfile=acisf01198_S0_LEG_-2.fits asphistfile=acisf01198_ah
4.fits[ASPHIST] engrid=grid(rmf.fits[cols ENERG_LO,ENERG_HI]) osipfile=CALDB dafile=CALDB pbkfile=acisf063833861N002_pbk0.fits 
pbkfile=acisf063833861N002_pbk0.fits maskfile=acisf01198_000N002_msk1.fits mode=hl verb=0
  
mkgarf detsubsys=ACIS-S1 order=-2 grating_arm=LEG outfile=acisf01198_S1_LEG_-2.fits asphistfile=acisf01198_ah
5.fits[ASPHIST] engrid=grid(rmf.fits[cols ENERG_LO,ENERG_HI]) osipfile=CALDB dafile=CALDB pbkfile=acisf063833861N002_pbk0.fits 
pbkfile=acisf063833861N002_pbk0.fits maskfile=acisf01198_000N002_msk1.fits mode=hl verb=0
   
mkgarf detsubsys=ACIS-S2 order=-2 grating_arm=LEG outfile=acisf01198_S2_LEG_-2.fits asphistfile=acisf01198_ah
6.fits[ASPHIST] engrid=grid(rmf.fits[cols ENERG_LO,ENERG_HI]) osipfile=CALDB dafile=CALDB pbkfile=acisf063833861N002_pbk0.fits 
pbkfile=acisf063833861N002_pbk0.fits maskfile=acisf01198_000N002_msk1.fits mode=hl verb=0 
   
mkgarf detsubsys=ACIS-S3 order=-2 grating_arm=LEG outfile=acisf01198_S3_LEG_-2.fits asphistfile=acisf01198_ah
7.fits[ASPHIST] engrid=grid(rmf.fits[cols ENERG_LO,ENERG_HI]) osipfile=CALDB dafile=CALDB pbkfile=acisf063833861N002_pbk0.fits 
pbkfile=acisf063833861N002_pbk0.fits maskfile=acisf01198_000N002_msk1.fits mode=hl verb=0 
   
Finished creating grating arfs for ccd_id= 4 5 6 7 
   
dmarfadd @thisfile.istemporary acisf01198LEG_-2_garf.fits
  
fullgarf finished. 

You may also see an aspect-related error from mkgarf; it is explained in this FAQ and may be ignored. The content of the parameter file may be checked using plist fullgarf.

The script is run in a similar way for the remaining rows.



Fitting

At this point, you should have the spectra, gARFs, and gRMFs necessary for fitting the data. The Fitting Grating Data thread shows how to load the data and responses, define a model, and fit the spectra.

In order to use Gaussian statistics to fit a model to a dataset, it is often necessary to "group" the data - i.e. combine channels until you have enough counts. Before fitting the data in Sherpa, read the Grouping a Grating Spectrum thread for more information.




Parameters for /home/username/cxcds_param/fullgarf.par


       phafile = acisf01198N002_pha2.fits Input PHA file (Type I or II)
        pharow = 2                Row in Type II PHA file (ignored if Type I)
       evtfile = acisf01198N002_evt2.fits Event file 
          asol = @pcad_asol1.lis  Aspect offsets file
        engrid = grid(rmf.fits[cols ENERG_LO,ENERG_HI]) Energy grid spec
       dtffile = )evtfile -> acisf01198N002_evt2.fits Dead time correction factor; ACIS->evt file; HRC -> dtf file
        badpix = acis_1198_new_bpix1.fits Bad pixel file; (filename|NONE|CALDB)
      rootname = acisf01198       Output rootname
      maskfile = acisf01198_000N002_msk1.fits NONE, or name of ACIS window mask file
      pbkfile  = acisf063833861N002_pbk0.fits NONE, or the name of the parameter block file
       (dafile = CALDB)            NONE, CALDB, or name of ACIS dead-area calibration file
     (osipfile = CALDB)           NONE or Name of fits file with order sorting info
      (clobber = no)              Clobber existing output files? This is passed to ALL child processes.
      (verbose = 0)               Control the level of diagnostic output. 0=>least.
         (mode = hl)              Mode flags.  Set to 'ql' to enable querying, 'hl' to suppress.
    

History

23 Dec 2004 updated for CIAO 3.2: canned gRMFs are no longer available in the CALDB
06 Dec 2005 updated for CIAO 3.3: the fullgarf script has been updated to version 3.3.1 for the new asphist tool syntax; corresponding changes to screen output
01 Dec 2006 reviewed for CIAO 3.4: no changes
26 Feb 2007 fullgarf v4.0.1: Four new parameters have been added, all of which are used by the mkgarf tool: pbkfile, dafile, osipfile, and maskfile; see "ahelp fullgarf" for details on each new parameter. Added ACIS dead area correction section
23 Jan 2008 updated for CIAO 4.0: fullgarf v4.1.1 (parameter updates for applying ACIS dead area correction, which is turned on by default); ACIS QE contamination link moved to "Related Links" section; removed outdated calibration updates
30 May 2008 fullgarf v4.1.3 (Unix head and tail commands replaced by pget and dmkeypar); thread images are inline
12 Feb 2009 updated for CIAO 4.1: "ARDLIB warning ... Assuming the first "interesting" extension." no longer printed; input data must have a CTI_APP keyword
19 Feb 2009 added Fitting section
06 May 2009 check the version of the CIAO scripts package instead of the individual script
01 Jun 2009 fullgarf updated in 01 Jun 2009 scripts package: If bad pixel file is not supplied, use the one from the CALDB. Previously, the script would set the bad pixel file to "NONE" in this case.
16 Jun 2009 added About the Chandra Grating Data Archive and Catalog section
12 Jan 2010 updated for CIAO 4.2: calibration update - the ACIS QE contamination model has been upgraded to vN0005.
05 Apr 2010 updated for CALDB 4.2.1: calibration update - the LETG grating efficiency has been upgraded to vN0006.

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Where are the PDFs?
Last modified: 5 April 2010