Running wavdetect
![[CXC Logo]](../../imgs/cxc-logo.gif){kind=logo}
CIAO 4.5 Science Threads
Overview
Synopsis:
wavdetect operates on the input in two stages. First it detects possible source pixels in a dataset by repeatedly correlating it with "Mexican Hat" wavelet functions with different scale sizes. Pixels with sufficiently large positive correlation values are removed from the image as assumed sources, and subsequent correlations are performed at the same scale. The second stage generates a source list from information from the first stage at each wavelet scale. This tool separates closely spaced point sources and finds extended sources so long as wavelet scales are chosen appropriately.
In CIAO 4.5, the tool has been updated to robustly work with upto 127 wavelet scales with scale lengths > 100 pixels. Additional optimizations have also been made to the tools that have shown modest (10-20%) speed improvements.
Purpose:
To illustrate several ways to use the detect tool: wavdetect.
Related Links:
- Analysis Guide: Extended Sources
-
Detect manual: other examples of using this tool are available in the "Running wavdetect" chapter.
Last Update: 3 Dec 2012 - Review for CIAO 4.5
Contents
- Getting Started
- Running wavdetect
- Using wavdetect on non-Chandra data
- Caveats
- Parameter files:
- History
- Images
Getting Started
Download the sample data: 578 (ACIS-S, 3C 295)
unix% download_chandra_obsid 578 evt2,fov,asol,bpix
Due to the heavy computational load, the recommended input image size for wavdetect is 2048x2048 or smaller. Images larger than this will require at least 1Gb of memory.
To run this thread, we want a source image and a congruent exposure map (for the "Running wavdetect with an exposure map" section). We chose to create both by running the fluximage script. The image and exposure map may also be created by following the Single-Chip ACIS Exposure Map thread.
In the following examples, a full resolution image of the ACIS-S3 (ccd_id=7) is used:
unix % dmcopy "acisf00578N003_evt2.fits[ccd_id=7,sky=region(acisf00578_000N003_fov1.fits[ccd_id=7])]" 578_evt2_filtered.fits
unix% fluximage 578_evt2_filtered.fits binsize=1 bands=broad outroot=s3
unix% dmlist s3_0.5-7.0_bin1.img blocks
--------------------------------------------------------------------------------
Dataset: s3_0.5-7.0_bin1.img
--------------------------------------------------------------------------------
Block Name Type Dimensions
--------------------------------------------------------------------------------
Block 1: EVENTS_IMAGE Image Int4(1390x1389)
Block 2: GTI7 Table 2 cols x 1 rows
To view the file, load it into ds9:
unix% ds9 s3_0.5-7.0_bin1.img &
which produces Figure 1.
![[Thumbnail image: The filtered and binned event file is displayed in ds9.]](image.png)
[Version: full-size]
Figure 1: Image of the cluster core
Running wavdetect
Create a PSF Map (Optional)
The PSF map is an observation specific file that provides information on the size of the PSF at each pixel in the image. It is an optional file, but wavdetect cannot compute point-spread-function sizes without it. The tool will still run but the source characteristics will not be reliable.
The simplest mkpsfmap uses the eband and eenergy values from your CIAO 4.3 wavdetect command and the input image:
unix% mkpsfmap <image> outfile=psfmap.fits energy=<eband> ecf=<eenergy>
The examples in this thread used the default eband (1.4967) and eenergy (0.393) values in CIAO 4.3, so the command is:
unix% mkpsfmap s3_0.5-7.0_bin1.img outfile=s3_psfmap.fits energy=1.4967 ecf=0.393
The contents of the parameter file may be checked using plist mkpsfmap.
![[New]](../../imgs/new.gif)
(3 Dec 2012)
In CIAO 4.5, mkpsfmap has been updated to include a
spectrum parameter that
allows the PSF map to be spectrally weighted. Users can use the
same thread to create spectral weights
as used by mkinsmap.
A Simple Example
To run wavdetect with the basic parameters set, it is necessary to specify the input and output filenames only. Note that it is not required to create an ASCII version of the region file; if the regfile parameter is left blank, it will not be used.
unix% punlearn wavdetect unix% pset wavdetect infile=s3_0.5-7.0_bin1.img unix% pset wavdetect psffile=s3_psfmap.fits unix% pset wavdetect outfile=s3_src.fits unix% pset wavdetect scellfile=s3_scell.fits unix% pset wavdetect imagefile=s3_imgfile.fits unix% pset wavdetect defnbkgfile=s3_nbgd.fits unix% pset wavdetect regfile=s3_src.reg unix% wavdetect Input file name (s3_0.5-7.0_bin1.img): Output source list file name (s3_src.fits): Output source cell image file name (s3_scell.fits): Output reconstructed image file name (s3_imgfile.fits): Output normalized background file name (s3_nbgd.fits): wavelet scales (pixels) (2.0 4.0): Image of the size of the PSF (s3_psfmap.fits):
The contents of the parameter file may be checked using plist wavdetect.
There are many outputs from the tool:
-
outfile: the FITS source list; contains same sources as regfile (see below)
-
scellfile: the source cell map shows the image pixels which were used to estimate source properties.
-
imagefile: the reconstructed source image is the combined correlation maxima regions, which correspond to probable sources. It is essentially what the data would look like if there were no background and noise fluctuations.
-
defnbkgfile: the normalized background derived from the data after the identified sources have been taken out.
-
regfile: the ASCII region file; contains same sources as outfile (see above).
Full descriptions of these files are given in the "Wavdetect Input Parameters & Data Products Reference" chapter of the Detect manual.
To display the image with the detections overlaid:
unix% ds9 s3_0.5-7.0_bin1.img &
Load the source list from either file (Region → Load Regions... → s3_src.fits OR s3_src.reg). The detections are shown in Figure 2.
![[Thumbnail image: The detections are overlaid on the event file as green ellipses.]](detections.png)
[Version: full-size]
Figure 2: Simple chip S3 detections
The three core sources are detected as a single region when the default parameter values are used.
Key parameters that you may wish to vary are scales and sigthresh. The scales parameter is a list of radii (in image pixels) of Mexican Hat wavelet functions; a wavelet transform is performed for each scale in the list. Usually a list of 5 scales is chosen, and each succeeding value is a factor of 2 or SQRT(2) larger than the previous one. The primary concern is to match the first scale size to the PSF. The choice of how many scaled wavelets to use depends somewhat on the available computing resources.
The sigthresh parameter is the significance threshold for source detection. Specifying a sigthresh that is proportional to the inverse of the number of pixels in the image allows ~1 false source per field (i.e. the default value of 10-6 corresponds to one spurious source in a 1000x1000 pixel map).
The result of running wavdetect on the same image with scales="1.0 2.0 4.0 8.0 16.0" and sigthresh=4e-06 are shown in Figure 3 (zooming in reveals the core and both hotspots (Figure 4) of this radio galaxy at the center of the cluster). The contents of the parameter file for this run may be checked using plist wavdetect.
![[Thumbnail image: Detections from both runs of wavdetect are shown on the data as different-colored ellipses.]](scales.png)
[Version: full-size]
Figure 3: Chip S3 detections: different scales and sigthresh
The red, dashed-line ellipses are the sources detected in the simple wavdetect run (s3_src.reg); the green ellipses are the sources detected with the different scales and threshold. The data is displayed at zoom=2.
![[Thumbnail image: The center of the image is displayed at zoom=8 in ds9.]](zoom.png)
[Version: full-size]
Figure 4: Galaxy core and hotspots
The three core sources are identified as individual detections when different scales and significance threshold are used (solid green ellipses). The data is displayed at zoom=8.
With an Exposure Map
In regions with substantial exposure variations, wavdetect may inaccurately estimate detection significance. Using an exposure map can suppress false positives (erroneous detections) and can help refine source property estimates. On account of this, the number of sources detected with an exposure map may be different than the number detected without one.
The exposure map was created in the Get Started section by running the fluximage script with the broad energy band definition. The exposure map may also be created by following the Single-Chip ACIS Exposure Map thread.
unix% punlearn wavdetect unix% pset wavdetect infile=s3_0.5-7.0_bin1.img unix% pset wavdetect psffile=s3_psfmap.fits unix% pset wavdetect expfile=s3_2.3_bin1.expmap unix% pset wavdetect outfile=s3_expmap_src.fits unix% pset wavdetect scellfile=s3_expmap_scell.fits unix% pset wavdetect imagefile=s3_expmap_imgfile.fits unix% pset wavdetect defnbkgfile=s3_expmap_nbgd.fits unix% pset wavdetect regfile=s3_expmap_src.reg unix% wavdetect Input file name (s3_0.5-7.0_bin1.img): Output source list file name (s3_expmap_src.fits): Output source cell image file name (s3_expmap_scell.fits): Output reconstructed image file name (s3_expmap_imgfile.fits): Output normalized background file name (s3_expmap_nbgd.fits): wavelet scales (pixels) (2.0 4.0): Image of the size of the PSF (s3_psfmap.fits):
The contents of the parameter file may be checked using plist wavdetect.
To display the image with an overlay of the source detections:
unix% ds9 s3_0.5-7.0_bin1.img &
Load the source list from either file (Region → Load Regions... → s3_expmap_src.fits OR s3_expmap_src.reg). The results are shown in Figure 5.
![[Thumbnail image: The detections are overlaid on the event file as green ellipses.]](expmap.png)
[Version: full-size]
Figure 5: Chip S3 detections: with an exposure map
In this case, the detections with the exposure map are identical to those without an exposure map.
There isn't any significant exposure variation across the field in this example, so the source properties do not change in the exposure map run.
To examine the source properties, use either dmlist with the column names of interest:
unix% dmlist "s3_expmap_src.fits[cols RA,DEC,PSF_SIZE]" data -------------------------------------------------------------------------------- Data for Table Block SRCLIST -------------------------------------------------------------------------------- ROW RA DEC PSF_SIZE 1 212.8557803787 52.1797340123 0.59385025501251 2 212.8873326131 52.1843193871 0.87103253602982 3 212.8844946518 52.1878739682 0.77809387445450 4 212.7390925660 52.1918860441 1.7067636251 5 212.8639748347 52.1921476296 0.55221420526505 6 212.7480906064 52.1982333738 1.3846766949 7 212.8361997158 52.2021140388 0.46548777818680 8 212.8351576868 52.2029015355 0.46795111894608 9 212.8474666652 52.2255254817 0.69639825820923 10 212.8712526183 52.2258589972 0.85530811548233 11 212.8839264690 52.2277353224 1.0685614347 12 212.8067117509 52.2280924054 0.79104131460190 13 212.8235350962 52.2283528447 0.73430377244949 14 212.8309929845 52.2335243759 0.8218926191330 15 212.8361461163 52.2366089548 0.91053777933121 16 212.8784169694 52.2399353274 1.2857367992 17 212.7380193991 52.2106692595 1.7449357510 18 212.8625189593 52.2375438843 1.0705546141 19 212.8710354959 52.2430695082 1.2986866236 20 212.8325603991 52.2630017204 1.9648095369 21 212.8099128214 52.2697586664 2.3703918457 22 212.7876127786 52.2791963481 3.0313541889 23 212.7681057278 52.2985241351 4.7453179359 24 212.7657612269 52.2990549730 4.8101892471 25 212.8526431283 52.3232153828 6.0807018280
or prism:
unix% prism s3_expmap_src.fits &
More information on working with source lists is available in the Using the Output of Detect Tools thread.
Using wavdetect on non-Chandra data
This example shows how to run wavdetect on a non-Chandra dataset. In this case, an XMM pn image, P0551690201PNS001IMAGE_8000.FTZ, is used.
Data from other missions is supported if the user can construct a psfmap file. For example, a psfmap file for an arbitrary instrument with a PSF that does not vary significantly over the field-of-view, can be generated with the dmimgcalc tool:
unix% dmimgcalc P0551690201PNS001IMAGE_8000.FTZ none xmm_psf.fits op="imgout=((img1*0)+9.0)" unix% dmhedit P0551690201PNS001IMAGE_8000.FTZ none add BUNIT "arcsec"
which generates an XMM psfmap with a constant size of 9". This is based on the estimate that at 1.5 keV, XMM 0.393 ecf ranges from 7" on-axis to ~11" at edge of the field-of-view. If the size is wrong, then the wrong scales may be used for the determination of source parameters, and thus the source properties may be wrongly estimated. However, the detection process will be unaffected.
Now, run wavdetect:
unix% punlearn wavdetect unix% pset wavdetect infile=P0551690201PNS001IMAGE_8000.FTZ unix% pset wavdetect psffile=xmm_psf.fits unix% pset wavdetect scales="2 4 8 16 32" unix% pset wavdetect outfile=xmm_src.fits unix% pset wavdetect scellfile=xmm_scell.fits unix% pset wavdetect imagefile=xmm_imgfile.fits unix% pset wavdetect defnbkgfile=xmm_nbgd.fits unix% pset wavdetect regfile=xmm_src.reg unix% wavdetect Input file name (P0551690201PNS001IMAGE_8000.FTZ): Output source list file name (xmm_src.fits): Output source cell image file name (xmm_scell.fits): Output reconstructed image file name (xmm_imgfile.fits): Output normalized background file name (xmm_nbgd.fits): wavelet scales (pixels) (2 4 8 16 32): Image of the size of the PSF (xmm_psf.fits):
The contents of the parameter file may be checked using plist wavdetect.
![[Thumbnail image: The detections are overlaid on the event file as green ellipses.]](xmm.png)
[Version: full-size]
Figure 6: XMM detections
XMM sources detected by wavdetect with an estimated 9" PSF size.
Caveats
Source detection and cosmic-ray afterglows
CIAO users who are trying to detect sources of about 10 counts or less should be aware of potential confusion with cosmic-ray afterglows that have not been removed from the data.
The Cosmic-Ray Afterglows why topic explains the current processing options and the limitations of the available tools used to detect afterglows.
A detection tool, not a flux tool
This tool is designed to be used as a source detection algorithm, and only secondarily as a source flux measurement tool. Flux estimation with wavdetect is generally quite reliable, but there is a small fraction of cases where the algorithm will fail to return useful source parameter estimates. This is inevitable, as there is no perfect source detection algorithm.
In section 3.2.2 of "A Wavelet-Based Algorithm for the Spatial Analysis of Poisson Data" (P. E. Freeman, et al. 2002, ApJS, 138, 185) it says:
"We note two situations where care must be exercised in interpreting results. First, the source cell for an [apparently] extended source may be too small if the smoothing scale is ~ [the PSF scale]."
Parameters for /home/username/cxcds_param/mkpsfmap.par
infile = s3_0.5-7.0_bin1.img Input image file name
outfile = s3_psfmap.fits Output image file name
energy = 1.4967 Energy of PSF to lookup [keV]
ecf = 0.393 ECF of PSF to lookup
(psffile = CALDB) PSF Calibration file
(units = arcsec) Units of output image
(geompar = geom.par) Pixlib geometry file
(clobber = no) Clobber files?
(mode = ql)
Parameters for /home/username/cxcds_param/wavdetect.par
#
# parameter file for wavdetect
#
#
# input
#
infile = s3_0.5-7.0_bin1.img Input file name
#
# output
#
outfile = s3_src.fits Output source list file name
scellfile = s3_scell.fits Output source cell image file name
imagefile = s3_imgfile.fits Output reconstructed image file name
defnbkgfile = s3_nbgd.fits Output normalized background file name
#
# scales
#
scales = 2.0 4.0 wavelet scales (pixels)
#
# end of wtransform parameters
#
########################################################################
########################################################################
#
# wrecon parameters
#
#
# PSF size parameters
#
psffile = s3_psfmap.fits Image of the size of the PSF
(regfile = s3_src.reg) ASCII regions output file
#
# output options
#
(clobber = no) Overwrite existing outputs?
(ellsigma = 3.0) Size of output source ellipses (in sigmas)
(interdir = ${ASCDS_WORK_PATH} -> /tmp) Directory for intermediate outputs
#
#########################################################################
#
# wtransform parameters
#
#
# optional input
#
(bkginput = ) Input background file name
(bkgerrinput = no) Use bkginput[2] for background error
#
# output info
#
(outputinfix = ) Output filename infix
#
# output content options
#
(sigthresh = 1e-06) Threshold significance for output source pixel list
(bkgsigthresh = 0.001) Threshold significance when estimating bkgd only
(falsesrc = -1.0) Allowed number of false sources per image
(sigcalfile = ${ASCDS_CALIB}/wtsimresult.fits -> /soft/ciao/data/wtsimresult.fits) Significance calibration file
#
# exposure info
#
(exptime = 0) Exposure time (if zero, estimate from map itself
(expfile = ) Exposure map file name (blank=none)
(expthresh = 0.1) Minimum relative exposure needed in pixel to analyze it
#
# background
#
(bkgtime = 0) Exposure time for input background file
#
# iteration info
#
(maxiter = 2) Maximum number of source-cleansing iterations
(iterstop = 0.0001) Min frac of pix that must be cleansed to continue
#
# end of wrecon parameters
#
########################################################################
#
# run log verbosity and content
#
(log = no) Make a log file?
(verbose = 0) Log verbosity
#
# mode
#
(mode = ql)
Parameters for /home/username/cxcds_param/wavdetect.par
#
# parameter file for wavdetect
#
#
# input
#
infile = s3_0.5-7.0_bin1.img Input file name
#
# output
#
outfile = s3_src_2.fits Output source list file name
scellfile = s3_scell_2.fits Output source cell image file name
imagefile = s3_imgfile_2.fits Output reconstructed image file name
defnbkgfile = s3_nbgd_2.fits Output normalized background file name
#
# scales
#
scales = 1.0 2.0 4.0 8.0 16.0 wavelet scales (pixels)
#
# end of wtransform parameters
#
########################################################################
########################################################################
#
# wrecon parameters
#
#
# PSF size parameters
#
psffile = s3_psfmap.fits Image of the size of the PSF
(regfile = s3_src_2.reg) ASCII regions output file
#
# output options
#
(clobber = no) Overwrite existing outputs?
(ellsigma = 3) Size of output source ellipses (in sigmas)
(interdir = ${ASCDS_WORK_PATH} -> /tmp) Directory for intermediate outputs
#
#########################################################################
#
# wtransform parameters
#
#
# optional input
#
(bkginput = ) Input background file name
(bkgerrinput = no) Use bkginput[2] for background error
#
# output info
#
(outputinfix = ) Output filename infix
#
# output content options
#
(sigthresh = 4e-06) Threshold significance for output source pixel list
(bkgsigthresh = 0.001) Threshold significance when estimating bkgd only
(falsesrc = -1) Allowed number of false sources per image
(sigcalfile = ${ASCDS_CALIB}/wtsimresult.fits -> /soft/ciao/data/wtsimresult.fits) Significance calibration file
#
# exposure info
#
(exptime = 0) Exposure time (if zero, estimate from map itself
(expfile = ) Exposure map file name (blank=none)
(expthresh = 0.1) Minimum relative exposure needed in pixel to analyze it
#
# background
#
(bkgtime = 0) Exposure time for input background file
#
# iteration info
#
(maxiter = 2) Maximum number of source-cleansing iterations
(iterstop = 0.0001) Min frac of pix that must be cleansed to continue
#
# end of wrecon parameters
#
########################################################################
#
# run log verbosity and content
#
(log = no) Make a log file?
(verbose = 0) Log verbosity
#
# mode
#
(mode = ql)
Parameters for /home/username/cxcds_param/wavdetect.par
#
# parameter file for wavdetect
#
#
# input
#
infile = s3_0.5-7.0_bin1.img Input file name
#
# output
#
outfile = s3_expmap_src.fits Output source list file name
scellfile = s3_expmap_scell.fits Output source cell image file name
imagefile = s3_expmap_imgfile.fits Output reconstructed image file name
defnbkgfile = s3_expmap_nbgd.fits Output normalized background file name
#
# scales
#
scales = 2.0 4.0 wavelet scales (pixels)
#
# end of wtransform parameters
#
########################################################################
########################################################################
#
# wrecon parameters
#
#
# PSF size parameters
#
psffile = s3_psfmap.fits Image of the size of the PSF
(regfile = s3_expmap_src.reg) ASCII regions output file
#
# output options
#
(clobber = no) Overwrite existing outputs?
(ellsigma = 3.0) Size of output source ellipses (in sigmas)
(interdir = ${ASCDS_WORK_PATH} -> /tmp) Directory for intermediate outputs
#
#########################################################################
#
# wtransform parameters
#
#
# optional input
#
(bkginput = ) Input background file name
(bkgerrinput = no) Use bkginput[2] for background error
#
# output info
#
(outputinfix = ) Output filename infix
#
# output content options
#
(sigthresh = 1e-06) Threshold significance for output source pixel list
(bkgsigthresh = 0.001) Threshold significance when estimating bkgd only
(falsesrc = -1.0) Allowed number of false sources per image
(sigcalfile = ${ASCDS_CALIB}/wtsimresult.fits -> /soft/ciao/data/wtsimresult.fits) Significance calibration file
#
# exposure info
#
(exptime = 0) Exposure time (if zero, estimate from map itself
(expfile = s3_2.3_bin1.expmap) Exposure map file name (blank=none)
(expthresh = 0.1) Minimum relative exposure needed in pixel to analyze it
#
# background
#
(bkgtime = 0) Exposure time for input background file
#
# iteration info
#
(maxiter = 2) Maximum number of source-cleansing iterations
(iterstop = 0.0001) Min frac of pix that must be cleansed to continue
#
# end of wrecon parameters
#
########################################################################
#
# run log verbosity and content
#
(log = no) Make a log file?
(verbose = 0) Log verbosity
#
# mode
#
(mode = ql)
Parameters for /home/username/cxcds_param/wavdetect.par
#
# parameter file for wavdetect
#
#
# input
#
infile = P0551690201PNS001IMAGE_8000.FTZ Input file name
#
# output
#
outfile = xmm_src.fits Output source list file name
scellfile = xmm_scell.fits Output source cell image file name
imagefile = xmm_imgfile.fits Output reconstructed image file name
defnbkgfile = xmm_nbgd.fits Output normalized background file name
#
# scales
#
scales = 2 4 8 16 32 wavelet scales (pixels)
#
# end of wtransform parameters
#
########################################################################
########################################################################
#
# wrecon parameters
#
#
# PSF size parameters
#
psffile = xmm_psf.fits Image of the size of the PSF
(regfile = xmm_src.reg) ASCII regions output file
#
# output options
#
(clobber = no) Overwrite existing outputs?
(ellsigma = 3.0) Size of output source ellipses (in sigmas)
(interdir = ${ASCDS_WORK_PATH} -> /tmp) Directory for intermediate outputs
#
#########################################################################
#
# wtransform parameters
#
#
# optional input
#
(bkginput = ) Input background file name
(bkgerrinput = no) Use bkginput[2] for background error
#
# output info
#
(outputinfix = ) Output filename infix
#
# output content options
#
(sigthresh = 1e-06) Threshold significance for output source pixel list
(bkgsigthresh = 0.001) Threshold significance when estimating bkgd only
(falsesrc = -1.0) Allowed number of false sources per image
(sigcalfile = ${ASCDS_CALIB}/wtsimresult.fits -> /soft/ciao/data/wtsimresult.fits) Significance calibration file
#
# exposure info
#
(exptime = 0) Exposure time (if zero, estimate from map itself
(expfile = ) Exposure map file name (blank=none)
(expthresh = 0.1) Minimum relative exposure needed in pixel to analyze it
#
# background
#
(bkgtime = 0) Exposure time for input background file
#
# iteration info
#
(maxiter = 2) Maximum number of source-cleansing iterations
(iterstop = 0.0001) Min frac of pix that must be cleansed to continue
#
# end of wrecon parameters
#
########################################################################
#
# run log verbosity and content
#
(log = no) Make a log file?
(verbose = 0) Log verbosity
#
# mode
#
(mode = ql)
Parameters for /home/username/cxcds_param/wavdetect.par
History
| 03 Jan 2005 | reviewed for CIAO 3.2: no changes |
| 03 Jun 2005 | updated links for CIAO 3.2 version of Detect manual |
| 19 Dec 2005 | updated for CIAO 3.3: updated files in detect data tarfile |
| 01 Dec 2006 | reviewed for CIAO 3.4: no changes |
| 16 Jan 2008 | updated for CIAO 4.0: added information about new wavdetect algorithm; updated parameter file listings to include falsesrc and sigcalfile, removed kernel; ds9 now automatically looks for the "[SRCLIST]" extension in the region file, so it doesn't have to be specified |
| 16 Apr 2008 | added Source Detection and Cosmic-Ray Afterglows caveat |
| 12 Jan 2009 | updated for CIAO 4.1: wavdetect algorithm was improved in this release; images are inline |
| 27 Jan 2010 | reviewed for CIAO 4.2: no changes |
| 15 Dec 2010 | updated for CIAO 4.3: the wavdetect "interdir" parameter uses ${ASCDS_WORK_PATH} instead of the working directory (".") for writing intermediate files |
| 15 Dec 2011 | reviewed for CIAO 4.4: wavdetect takes an observation-specific PSF map file as input instead of using the Chandra PSF table data or the tool's internal parameterization of the ROSAT PSF; minor updates to screen output and images; use fluximage to create the image and exposure map; added an example of non-Chandra data |
| 25 Jul 2012 | updated getting started example for necessary files |
| 03 Dec 2012 | Review for CIAO 4.5 |
