LETG/HRC-I Grating Spectra
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CIAO 4.17 Science Threads
Overview
Synopsis:
Generate a new PHA2 spectrum file for any LETG/HRCS-I grating observation to ensure that consistent calibration is used throughout the analysis.
Run this thread if:
you are working with an HRC-I/LETG dataset and want to create a new level=2 event file and extract a Type II PHA grating spectrum file.
Related Links:
- About the Instrument: HRC & LETG
- Analysis Guide for Chandra High Resolution Spectroscopy: an in-depth discussion of grating analysis.
Last Update: 5 Dec 2024 - Updated for CIAO 4.17. Restored use of dmcopy opt=all.
Contents
- About the Chandra Grating Data Archive and Catalog
- About the chandra_repro script
- Data Preparation
- Get Started
- Generate a New Level=1.5 Event File
- Generate a New Level=2 Event File
- Extract a Grating Spectrum (tgextract)
- Summary
- Parameter files:
- History
- Images
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.
About the chandra_repro script
The chandra_repro script reprocessing script automates the recommended data processing steps presented in the CIAO analysis threads. The script reads data from the standard data distribution (e.g. primary and secondary directories) and creates a new bad pixel file, a new level=2 event file, and a new level=2 Type II PHA file.
chandra_repro also will now create the appropriate ARF and RMF for each grating order and arm in the spectrum using the mktgresp script. The response files will be stored in a tg/ subdirectory of the outdir parameter.
Refer to "ahelp chandra_repro" for more information.
![[WARNING]](../../imgs/warning.png)
If you have run chandra_repro you do not need to complete the rest of this thread unless you want to understand the individual processing steps, the options avaiable, or need to apply any non-standard calibrations.
Data Preparation
This analysis thread starts with the level 1 event file. Before beginning, users may wish to reprocess the data to create a new event file with the most recent calibration applied. Instructions on how to reprocess your data are available in the HRC Data Preparation Analysis Guide.
Get Started
Download the sample data: 1801 (LETG/HRC-I, PKS2155-304)
unix% download_chandra_obsid 1801 evt1,flt,asol
In this thread, we assume that all relevant files are in the same working directory.
If you are satisfied with the zero-order location, go directly to the HRC Grating RMFs thread.
Generate a New Level=1.5 Event File
1. Get position of zero-order image (tgdetect)
To find the zero-order location, the tool tgdetect is run:
unix% punlearn tgdetect unix% pset tgdetect infile=hrcf01801_000N008_evt1.fits unix% pset tgdetect outfile=hrc_1801_evt1_src1a.fits unix% tgdetect Input L1 event file (hrcf01801_000N008_evt1.fits): Input source position(s) file from previous OBI or NONE (NONE): Output source position(s) file name (hrc_1801_evt1_src1a.fits):
The contents of the parameter file may be checked using plist tgdetect.
tgdetect2 may also be used here; however, for HRC observations it always runs the tgdetect tool.
The source list may be viewed over the event file using ds9:
unix% ds9 hrcf01801_000N008_evt1.fits &
Overlay the source list: Region → Load Regions → hrc_1801_evt1_src1a.fits.
If the zero order of the source is outside of the default search area (e.g. far from the aimpoint), tgdetect will not find it. If this problem affects your data, it will be obvious when the source list is displayed on the event file. In this case, run the Correcting a Misplaced Zero-order Source Position thread to identify the correct source position.
2. Get region mask (tg_create_mask)
The location of the spectrum needs to be found next, via the tool tg_create_mask.
unix% punlearn tg_create_mask unix% pset tg_create_mask infile=hrcf01801_000N008_evt1.fits unix% pset tg_create_mask outfile=hrc_1801_evt1_L1a.fits unix% pset tg_create_mask input_pos_tab=hrc_1801_evt1_src1a.fits unix% tg_create_mask Input event file or stack (hrcf01801_000N008_evt1.fits): Output region file or stack (hrc_1801_evt1_L1a.fits): Input table with zero order positions or stack (hrc_1801_evt1_src1a.fits): Observed grating type (header_value|HETG|HEG|MEG|LETG) (HETG|HEG|MEG|LETG|header_value|HEADER_VALUE) (header_value):
The region file, hrc_1801_evt1_L1a.fits, will be used to mask the event file. The regions may be viewed over the event file using ds9:
unix% ds9 hrcf01801_000N008_evt1.fits &
Overlay the region file: Region → Load Regions → hrc_1801_evt1_L1a.fits. Figure 1 shows the regions on the event file.
The contents of the parameter file may be checked using plist tg_create_mask.
Figure 1: Event file with region file overlaid
![[Thumbnail image: The region mask outlines the photons from the source and the grating arms.]](ds9.png)
[Version: full-size]
Figure 1: Event file with region file overlaid
The regions are loaded from the L1a.fits file, which was made by tg_create_mask.
3. Run tg_resolve_events
The tool tg_resolve_events is now used to assign grating events to spectral orders:
unix% punlearn tg_resolve_events unix% pset tg_resolve_events infile=hrcf01801_000N008_evt1.fits unix% pset tg_resolve_events outfile=hrc_1801_evt1a.fits unix% pset tg_resolve_events regionfile=hrc_1801_evt1_L1a.fits unix% pset tg_resolve_events acaofffile=@pcad_asol1.lis unix% pset tg_resolve_events eventdef=")stdlev1_HRC" unix% pset tg_resolve_events osipfile=none unix% tg_resolve_events Input event file or stack (hrcf01801_000N008_evt1.fits): Input region file or stack (hrc_1801_evt1_L1a.fits): Output event file or stack (hrc_1801_evt1a.fits): Input aspect offset file (@pcad_asol1.lis):
It is important to note several things here:
-
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 acaofffile parameter in chronological order (the time is in the filename, so "ls" lists them in order), either as a comma-separated list or as a stack. Here we use:
unix% cat pcad_asol1.lis pcadf01801_000N001_asol1.fits
-
The unusual syntax of the eventdef parameter; the tool will not access the predefined string if the leading ")" is missing.
The contents of the parameter file may be checked using plist tg_resolve_events.
Generate a New Level=2 Event File
1. Filter on status (dmcopy)
Next we apply the status filter that is specific to HRC-I observations; a value of 0 demands that the bit be flagged as "good", a value of x indicates that either status (0/1) is acceptable:
unix% punlearn dmcopy unix% dmcopy "hrc_1801_evt1a.fits[status=xxxxxx00xxxx0xxx00000000x0000000]" \ hrc_1801_flt1_evt1a.fits unix% dmappend "hrc_1801_evt1a.fits[region][subspace -time]" hrc_1801_flt1_evt1a.fits
2. Apply GTI filter (dmcopy)
Finally, the Good Time Intervals (GTIs) supplied by the pipeline are applied:
unix% punlearn dmcopy
unix% dmcopy \
"hrc_1801_flt1_evt1a.fits[EVENTS][@hrcf01801_000N008_std_flt1.fits]" \
hrc_1801_evt2.fits opt=all
Be sure to include the @ symbol in the filter expression; the command will not be executed properly if it is omitted.
Extract a Grating Spectrum (tgextract)
The CIAO tool tgextract produces a PHA2 spectrum file from the level=2 data file:
unix% punlearn tgextract unix% pset tgextract infile=hrc_1801_evt2.fits unix% pset tgextract outfile=hrc_1801_pha2.fits unix% tgextract Input event file (output event file from L1.5 processing) (hrc_1801_evt2.fits): If typeII, enter full output file name or '.'; if typeI, enter output rootname (hrc_1801_pha2.fits): Input ancillary response file name (none): Input redistribution file name (none): Source ID's to process: 'all', comma list, @file (all): Grating parts to process: HETG, HEG, MEG, LETG, header_value (HETG|HEG|MEG|LETG|header_value) (header_value): Grating diffraction orders to process: 'default', comma list, range list, @file (default): Ouput file type: typeI (single spectrum) or typeII (multiple spectra) (pha_typeI|pha_typeII) (pha_typeII):
The contents of the parameter file may be checked using plist tgextract.
Summary
This thread is now complete; the PHA2 grating spectrum file is named hrc_1801_pha2.fits. You should next:
- read the Computing Average HRC Dead Time Corrections thread to see if you need to recompute the deadtime statistics for your dataset
- create HRC Grating RMFs
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/tgdetect.par
##
## TGDETECT -- Create filter; run celldetect; narrow down detected
## 'zero order' source list; set source id's; match
## sources to previous OBI source list.
##
## Note: if either "infile" or "OBI_srclist_file" are @lists, only
## the first item on the list is read in; this tool only works on
## one set of input files; if more than one file is listed,
## everything but the first are ignored.
##
infile = hrcf01801_000N006_evt1.fits Input L1 event file
OBI_srclist_file = NONE Input source position(s) file from previous OBI or NONE
outfile = hrc_1801_evt1_src1a.fits Output source position(s) file name
#
# output file naming
#
(temproot = ) Path and root file name to be given to temporary files
(keeptemp = no) Keep temporary files?
(keepexit = no) Keep exit status file?
#
#
#
(zo_pos_x = default) Center GZO filter sky X position (default=pixel(ra_nom))
(zo_pos_y = default) Center GZO filter sky Y position (default=pixel(dec_nom))
(zo_sz_filt_x = default) Size of GZO filter in X pixels (ACIS=400; HRC=1800)
(zo_sz_filt_y = default) Size of GZO filter in Y pixels (ACIS=400; HRC=1800)
(snr_thresh = 40) SNR threshold to select the detected sources
#
# celldetect parameters
#
(expstk = none) list of exposure map files
(thresh = )celldetect.thresh -> 3) celldetect source threshold
(ellsigma = 3.0) Size of output source ellipses (in sigmas)
(expratio = 0) cutoff ratio for source cell exposure variation
(findpeaks = yes) find local peaks for celldetect
(celldetect_log = )celldetect.log -> no) make a celldetect log file?
(psftable = )celldetect.psftable -> /soft/ciao/data/psfsize20010416.fits) table of PSF size data, for celldetect
(fixedcell = 15) celldetect fixed cell size to use
(fixedcell_cc_mode = 15) celldetect fixed cell size to use for CC mode ACIS data
(bkgfile = none) background file, for celldetect
(bkgvalue = )celldetect.bkgvalue -> 0) background count/pixel, for celldetect
(bkgerrvalue = )celldetect.bkgerrvalue -> 0) background error, for celldetect
(eband = )celldetect.eband -> 1.4967) energy band, for celldetect
(eenergy = )celldetect.eenergy -> 0.8) encircled energy of PSF, for celldetect
(snrfile = none) celldetect snr output file (for convolution only)
(convolve = )celldetect.convolve -> no) use convolutions for celldetect
(xoffset = INDEF) celldetect offset of x axis from optical axis
(yoffset = INDEF) celldetect offset of y axis from optical axis
(cellfile = none) output cell size image file
(centroid = yes) compute source centroids in celldetection?
#
# tgidselectsrc parameters
#
(snr_ratio_limit = )tgidselectsrc.snr_ratio_limit -> 1) Value of SNR ratio to use as lower limit
(setsrcid = )tgidselectsrc.setsrcid -> yes) Set src ids in output file?
#
# tgmatchsrc parameters
#
(max_separation = )tgmatchsrc.max_separation -> 3) Maximum allowed separation (arcsec) for sources to match
#
#
(clobber = no) OK to overwrite existing output file(s)?
(verbose = 0) Verbosity level (0 = no display)
(mode = ql)
Parameters for /home/username/cxcds_param/tg_create_mask.par
##
## TG_CREATE_MASK -- Calculates the mask regions of the grating arms
## for AXAF flight L1 grating data files. The output is a region
## file(s) in sky coordinates.
##
infile = hrcf01801_000N006_evt1.fits Input event file or stack
outfile = hrc_1801_evt1_L1a.fits Output region file or stack
input_pos_tab = hrc_1801_evt1_src1a.fits Input table with zero order positions or stack
grating_obs = header_value Observed grating type (header_value|HETG|HEG|MEG|LETG)
sA_zero_x = 1 Source A - x position of zero order
sA_zero_y = 1 Source A - y position of zero order
sB_zero_x = 1 Source B - x position of zero order
sB_zero_y = 1 Source B - y position of zero order
sC_zero_x = 1 Source C - x position of zero order
sC_zero_y = 1 Source C - y position of zero order
sD_zero_x = 1 Source D - x position of zero order
sD_zero_y = 1 Source D - y position of zero order
sE_zero_x = 1 Source E - x position of zero order
sE_zero_y = 1 Source E - y position of zero order
sF_zero_x = 1 Source F - x position of zero order
sF_zero_y = 1 Source F - y position of zero order
sG_zero_x = 1 Source G - x position of zero order
sG_zero_y = 1 Source G - y position of zero order
sH_zero_x = 1 Source H - x position of zero order
sH_zero_y = 1 Source H - y position of zero order
sI_zero_x = 1 Source I - x position of zero order
sI_zero_y = 1 Source I - y position of zero order
sJ_zero_x = 1 Source J - x position of zero order
sJ_zero_y = 1 Source J - y position of zero order
(input_psf_tab = CALDB) Calibration file with mirror psf vs off-axis angle
(detector = header_value) Detector type: ACIS | HRC-I | HRC-S | header_value
(radius_factor_zero = 50) A scale factor which multiplies the app. calculation of the one-sigma
(width_factor_hetg = 35) A scale factor which multiplies the one-sigma width of the heg/meg mask
(width_factor_letg = 40) A scale factor which multiplies the one-sigma width of the letg mask
(r_astig_max_hetg = 0.5600000000000001) Max grating r coord (deg, along the dispersion) for HETG astigmatism
(r_astig_max_letg = 1.1) Max grating r coord (deg, along the dispersion) for LETG astigmatism calc
(r_mask_max_hetg = 0.992) Max grating r coord (deg) for HETG mask (to support offset pointing)
(r_mask_max_letg = 2.1) Max grating r coordinate (deg) for LETG mask (to support offset pointing)
# --------------------------------------------------------------------------
# The parameters below are to be set ONLY if the user wants to use their
# own grating mask sizes instead of having the masks automatically generated.
# Only ONE input file, with up to 10 soures, can be processed using the user
# params. @ lists of multiple files can only be done with automated mask
# processing, or by running each file individually with hand set mask sizes.
# To start, you MUST set the following parameters:
#
# > pset tg_create_mask use_user_pars=yes last_source_toread=[letter A -> J]
#
# The parameter last_source_toread should be set to the last source letter
# for which you will enter parameters. If you want to input 2 sources
# (regardless of their source id's), the last_source_toread=B. Sections
# A -> J are for (upto) 10 user specified sources. In each sections,
# each source must have an ID, a zero order center position specified,
# as well as the grating mask width(s). An example with 2 HETG sources,
# with src_id's 6 and 3:
#
# > pset tg_create_mask use_user_pars=yes last_source_toread=B
# > pset tg_create_mask sA_id=6 sA_zero_x=4762.34 sA_zero_y=2344.29
# > pset tg_create_mask sA_zero_rad=35 sA_width_heg=25 sA_width_meg=28
# > pset tg_create_mask sB_id=3 sB_zero_x=4063.54 sB_zero_y=6346.62
# > pset tg_create_mask sB_zero_rad=45 sB_width_heg=50 sB_width_meg=75
# (units are all in sky pixels)
#
# NOTE: for Continuous Clocking data (CC mode), the HETG mask does not
# require the s#_width_heg, since the meg mask will encompase the entire
# data set. HEG event processing in CC mode is done using the next
# tool tg_resolve_events.
# --------------------------------------------------------------------------
(use_user_pars = no) Use the user defined mask parameters below: yes or no?
(last_source_toread = A) Last source name to be read; character A->J.
# --------------------------------------------------------------------------
# Source A parameters
# --------------------------------------------------------------------------
(sA_id = 1) Source A - source id number
(sA_zero_rad = ) Source A - radius of zero order mask
(sA_width_heg = ) Source A - width of heg mask in sky pixels
(sA_width_meg = ) Source A - width of meg mask in sky pixels
(sA_width_leg = ) Source A - width of leg mask in sky pixels
# --------------------------------------------------------------------------
# Source B parameters
# --------------------------------------------------------------------------
..(through Source J)..
(geompar = geom) Parameter file for Pixlib Geometry files
(verbose = 0) Verbose level: 0 - no output, 5 - max verbosity
(clobber = no) Clobber existing outfile?
(mode = ql)
Parameters for /home/username/cxcds_param/tg_resolve_events.par
#--------------------------------------------------------------------------
#
# tg_resolve_events.par: Parameter file for the tg_resolve_events program
#
#--------------------------------------------------------------------------
infile = hrcf01801_000N006_evt1.fits Input event file or stack
outfile = hrc_1801_evt1a.fits Output event file or stack
regionfile = hrc_1801_evt1_L1a.fits Input region file or stack
acaofffile = @pcad_asol1.lis Input aspect offset file
(alignmentfile = )acaofffile -> @pcad_asol1.lis) Input sim offset file
(logfile = stdout) Output log (NONE|<filename>|stdout)
# The osipfile contains position dependent energy limits based on
# the CCD resolution, used for order-sorting.
# A value of "NONE" means that the file will not be used, and
# that the parameters, osort_hi and osort_lo will be used.
(osipfile = none) Lookup table for order resolving (for acis data only)
#sort_hi, osort_lo specify fractional deviations from the integer
#order which will be included in order-sorting via CCD ENERGY values (PHA).
#eg. osort_lo-0.3, osort_hi=0.2 means that photons with real-valued
#orders between 0.7 < order <= 1.2 will be included in first order,
#1.7 < order <= 2.2 will be second order, etc.
(osort_lo = 0.3) Order-sorting lower bound fraction; order > m - osort_lo
(osort_hi = 0.3) Order-sorting high bound fraction; order <= m + osort_hi
(grating_obs = header_value) Observed grating type (header_value|HETG|HEG|MEG|LETG)
(detector = header_value) Detector type: ACIS | HRC-I | HRC-S | header_value
(energy_lo_adj = 1.0) Lower Energy limit factor
(energy_hi_adj = 1.0) Upper Energy limit factor
(time_offset = 0) Offset to add to event time to synch w/ alignment data
(rand_seed = 1) Random seed (for pixlib), 0 = use time dependent seed
(rand_pix_size = 0.0) pixel randomization width (-size..+size), 0.0 = no randomization
(eventdef = )stdlev1_HRC -> {d:time,f:rd,s:chip,l:tdet,f:det,f:sky,s:chip_id,s:pha,s:pi,s:tg_m,f:tg_lam,
f:tg_mlam,s:tg_srcid,s:tg_part,s:tg_smap,x:status}) Output format definition
(stdlev1 = )eventdef -> {d:time,f:rd,s:chip,l:tdet,f:det,f:sky,s:chip_id,s:pha,s:pi,s:tg_m,f:tg_lam,
f:tg_mlam,s:tg_srcid,s:tg_part,s:tg_smap,x:status})
(stdlev1_ACIS = {d:time,i:expno,f:rd,s:chip,s:tdet,f:det,f:sky,s:ccd_id,l:pha,s:pi,f:energy,s:grade,
s:fltgrade,s:node_id,s:tg_m,f:tg_lam,f:tg_mlam,s:tg_srcid,s:tg_part,s:tg_smap,x:status})
ACIS event format definition string
(stdlev1_HRC = {d:time,f:rd,s:chip,l:tdet,f:det,f:sky,s:chip_id,s:pha,s:pi,s:tg_m,f:tg_lam,
f:tg_mlam,s:tg_srcid,s:tg_part,s:tg_smap,x:status}) HRC event format definition string
# --------------------------------------------------------------------------
(geompar = geom) Parameter file for Pixlib Geometry files
(verbose = 0) Verbosity level of detail (0=none, 5=most)
(clobber = no) Clobber outfile if it already exists?
(mode = ql)
Parameters for /home/username/cxcds_param/tgextract.par
##
## TGEXTRACT -- create 1D spectrum(a) table file(s) from the
## L1.5 output event list
##
infile = hrc_1801_evt2.fits Input event file (output event file from L1.5 processing)
outfile = hrc_1801_pha2.fits If typeII, enter full output file name or '.'; if typeI, enter output rootname
#
# tg_srcid_list parameter explanation...
# - "all" will process all the sources id's found in the event list
# - a comma list is a comma separated string list of all the
# sources to process, ie:
# "1,2,5,7"
# - @file is a pointer to an ascii file which contains a comma
# separated list of the id's to process
#
tg_srcid_list = all Source ID's to process: 'all', comma list, @file
tg_part_list = header_value Grating parts to process: HETG, HEG, MEG, LETG, header_value
#
# tg_order_list parameter explanation...
# - "default" is set to process the following:
# if ACIS: 1, 2, 3, -1, -2, -3
# if HRC: -1, 1
# - a comma list is a comma separated string list of the orders
# the user wants to process, ie:
# "-5, -1, 1, 3"
# - a range list sets the min and max of the orders to process;
# all the orders in between, will be processed, ie:
# "-1..5" will do orders from -1 to +5th order
# a range list can be mixed with comma separated list
# - @file is a pointer to an ascii file which contains a comma
# separated list and/or range list of the orders to process
#
tg_order_list = default Grating diffraction orders to process: 'default', comma list, range list, @file
ancrfile = none Input ancillary response file name
respfile = none Input redistribution file name
outfile_type = pha_typeII Ouput file type: typeI (single spectrum) or typeII (multiple spectra)
(inregion_file = none) Input region file.
(backfile = none) Input background file name
(rowid = ) If rowid column is to be filled in, enter name here
(bin_units = angstrom) Bin units (for bin parameters below): angstrom, eV, keV
(min_bin_leg = compute) Minimum dispersion coordinate for LEG, or 'compute'
(max_bin_leg = compute) Maximum dispersion coordinate for LEG, or 'compute'
(bin_size_leg = compute) Bin size for binning LEG spectra, or 'compute'
(num_bins_leg = compute) Number of bins for the output LEG spectra, 'compute'
(min_bin_meg = compute) Minimum dispersion coordinate for MEG, or 'compute'
(max_bin_meg = compute) Maximum dispersion coordinate for MEG, or 'compute'
(bin_size_meg = compute) Bin size for binning MEG spectra, or 'compute'
(num_bins_meg = compute) Number of bins for the output MEG spectra, or 'compute'
(min_bin_heg = compute) Minimum dispersion coordinate for HEG, or 'compute'
(max_bin_heg = compute) Maximum dispersion coordinate for HEG, or 'compute'
(bin_size_heg = compute) Bin size for binning HEG spectra, or 'compute'
(num_bins_heg = compute) Number of bins for the output HEG spectra, 'compute'
(min_tg_d = default) Minimum tg_d range to include in histogram, or use 'default'
(max_tg_d = default) Maximum tg_d range to include in histogram, or use 'default'
(extract_background = yes) Extract the local background spectrum?
(min_upbkg_tg_d = default) Minimum value of tg_d for the background up spectrum.
(max_upbkg_tg_d = default) Maximum value of tg_d for the background up spectrum.
(min_downbkg_tg_d = default) Minimum value of tg_d for the background down spectrum.
(max_downbkg_tg_d = default) Maximum value of tg_d for the background down spectrum.
(geompar = geom) Parameter file for Pixlib Geometry files
(clobber = no) OK to overwrite existing output file(s)?
(verbose = 0) Verbosity level (0 = no display)
(mode = ql)
History
| 16 Dec 2004 | updated for CIAO 3.2: minor changes to parameter files |
| 05 Dec 2005 | updated for CIAO 3.3: output filenames include ObsID; parameter file change (kernel parameter removed from all "tg" tools) |
| 05 Jan 2006 | created Data Preparation section |
| 01 Dec 2006 | updated for CIAO 3.4: change to wording of tgdetect/dmcopy warning |
| 11 Jan 2008 | updated for CIAO 4.0: ds9 now automatically looks for the "[REGION]" or "[SRCLIST]" extension in the region file, so it doesn't have to be specified; filenames and screen output updated for reprocessed data (version N006 event file); check if data have gone through Reprocessing III |
| 21 Jan 2009 | updated for CIAO 4.1: image converted to inline |
| 19 Feb 2009 | added grouping information to the Summary |
| 16 Jun 2009 | added About the Chandra Grating Data Archive and Catalog section |
| 14 Jan 2009 | reviewed for CIAO 4.2: no changes |
| 15 Mar 2010 | added link to the Computing Average HRC Dead Time Corrections thread in the Summary |
| 12 Jan 2011 | reviewed for CIAO 4.3: no changes |
| 25 Feb 2011 | the 25 Feb release of the chandra_repro reprocessing script supports data processing for ACIS and HRC grating data |
| 25 Mar 2011 | added workaround for GTI filtering bug to the Apply GTI filter section |
| 06 Jan 2012 | reviewed for CIAO 4.4: no changes |
| 03 Dec 2012 | Review for CIAO 4.5; updated file versions |
| 24 Apr 2013 | Updated the chandra_repro section to make it clear the it does all the steps in this thread and that responses are now also created. |
| 11 Dec 2013 | Review for CIAO 4.6; added a note about tgdetect2 |
| 22 Dec 2014 | Reviewed for CIAO 4.7; no changes. |
| 02 Dec 2020 | Replace dmcopy opt=all with dmappend to copy the [REGION] block. |
| 08 Feb 2022 | Review for CIAO 4.14. Updated for Repro-5/CALDB4.9.6. |
| 05 Dec 2024 | Updated for CIAO 4.17. Restored use of dmcopy opt=all. |