acis_extract, srclist_filename, obsname, obsdata_filename, /EXTRACT_SPECTRA, ENERGY_RANGE=[energy
, /REUSE_NEIGHBORHOOD, /USE_MKRMF, EMAP_ENERGY=energy
acis_extract, srclist_filename, obsname, /EXTRACT_SPECTRA, /PLOT
idl tee extract_spectra_1875.log
acis_extract, 'all.srclist', '1875', '../obs1875/spectral.evt', /EXTRACT_SPECTRA, ENERGY_RANGE=[0.5,8], EMAP_FILENAME='../obs1875/obs.emap', ASPECT_FN='../obs1875/obs.asol', ASPHIST_DIR='../obs1875/asphist', ARDLIB_FILENAME='../obs1875/ardlib.par', PBKFILE='../obs1875/obs.pbkfile', MSKFILE='../obs1875/obs.mskfile, WARNING_REGION_FILENAME='warning.reg'
acis_extract, 'all.srclist', '1875', /EXTRACT_SPECTRA, /PLOT
- The optional ENERGY_RANGE parameter defines the band over which statistics are computed; default is [0.5,8.0]. An energy filter is NOT applied to the spectra.
- The optional parameter ASPECT_FN is recommended so that various CIAO tools (e.g. dmcoords, mkacisrmf, mkwarf) can be supplied with an aspect file.
- The ASPHIST_DIR should be the path to a directory that contains appropriate
aspect histogram files for each active CCD with names ccd0.asphist, ccd1.asphist,... Each CCD must have its own aspect histogram file because the tool asphist considers a CCD's GTI table when computing the aspect histogram. If omitted the directory ./asphist/ is assumed.
Methods of constructing are aspect histograms are discussed in the CIAO documentation. If you use the CIAO script merge_all to construct SINGLE ObsId exposure maps you can rename the aspect histograms files it produces, e.g. merged_asp_0.fits ccd0.asphist. If you use the AE tool ae_make_emap (§7.14) to construct exposure maps then an aspect histogram directory named asphist with the correct file names is produced.
AE confirms that the exposure times represented in the aspect histograms supplied are similar to the EXPOSUR* keywords in the event data as a potential aide in catching mistakes in aspect histogram construction.
- The required ARDLIB_FILENAME should be the path to an ardlib.par parameter file that has been correctly configured for this observation. To avoid mistakes we STRONGLY recommend that you store a correctly configured ardlib.par in the area where you reduced the observation, rather than in the default parameter directory referenced in your shell's PFILES environment variable.
- The optional PBKFILE parameter enables the ``Dead Area calibration'' available in the mkarf/mkwarf tools. See the ahelp documentation in CIAO or the appropriate CIAO thread.
- The optional MSKFILE parameter should be the path to the observation's ``mask file'', which is used by mkarf and mkwarf.
- See §E.2 for a description of the WARNING_REGION_FILENAME, NEIGHBORHOOD_SIZE, and REUSE_NEIGHBORHOOD parameters.
- Supply /USE_MKRMF to build RMFs using the CIAO tool mkrmf instead of the tool mkacisrmf.
The CXC recommends
the mkrmf tool only for data taken at -110 C on certain CCDs.
- The keyword parameter EMAP_ENERGY must be supplied for diffuse sources (§7.1.2); it should specify the mono-energy (in keV) that was used to build the exposure map (§7.14.3).
You can look up this energy in the headers of the ``instrument maps'' produced by CIAO, for example
dmlist asphist/ccd0.instmap head | egrep "ENERG_LO|ENERG_HI"
- The optional keyword parameter WMAP_ENERGY_RANGE can be supplied for diffuse sources (§7.1.2) to specify the energy range (in keV) over which a ``weight map'' (needed by mkwarf) is constructed ; the default range is 0.5-2 keV.
For each source the following files are produced:
- All data products from the EXTRACT_EVENTS stage (§E.2) are also produced by EXTRACT_SPECTRA.
- the spectrum of the source
- the RMF at the source position for the CCD containing the majority of the band-limited events in source.evt
- the ARF at the source position for CCD i
- the multi-CCD, PSF fraction reduced ARF at the source position
- a FITS file containing keyword information about this observation of the source
Several interactive plots show characteristics of the source extraction; see our AE recipes (§7.1) for descriptions of each.
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Up: E. Obsolete Stages
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Penn State Department of Astronomy