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Making an exposure-corrected mosaic

CIAO 4.16 Science Threads

Overview

Synopsis:

The merge_obs script replaces the merge_all script and lets you easily create an exposure-corrected image of a group of observations. These steps can also be taken manually: the reproject_image tool maps an image in one WCS reference frame to the WCS in another image. If you do not have a reference image available, reproject_image_grid can reproject the image to a user-defined WCS grid instead.

Purpose:

To create an exposure-corrected mosaic image from multiple observations of SN1006.

Related Links:

Last Update: 7 Feb 2022 - Review for CIAO 4.14. No changes.

Get Started

Download the sample data: 3838; 4385; 4386; 4387; 4388; 4389; 4390; 4391; 4392; 4393; 4394

unix% download_chandra_obsid 3838,4385,4386,4387,4388,4389,4390,4391,4392,4393,4394

All of these data are ACIS-I observations of SN1006, a supernova remnant.

In this thread we assume that the observations have been reprocessed by chandra_repro and can be found in obsid/repro/; e.g.

unix% chandra_repro 3838,4385,4386,4387,4388,4389,4390,4391,4392,4393,4394 outdir= verbose=1
...

The verbose parameter is set to 1 to provide some feedback on the reprocessing (the default value of 0 provides no on-screen updates).

Using merge_obs to automate the process

The merge_obs script automates the construction of an exposure-corrected image from a set of observations. It replaces the merge_all script.

To create exposure-corrected images in the broad, soft, medium, and hard bands using a binning of 4, you just need to say the following (and wait a while):

unix% punlearn merge_obs
unix% merge_obs "*/repro/*evt*[ccd_id=0:3]" sn1006/ bin=4 bands=broad,csc
Running merge_obs
Version: 05 November 2021

Verifying 11 observations.
Using CSC ACIS broad science energy band.
Using CSC ACIS soft science energy band.
Using CSC ACIS medium science energy band.
Using CSC ACIS hard science energy band.
Calculating new tangent point.
New tangent point: RA=15h 2m 56.505s Dec=-41d 56' 15.66"

Observations to be reprojected:

   Obsid  Obs Date   Exp    DETNAM     SIM_Z    FP   Sepn   PA  
                    (ks)                (mm)    (K)   (')  (deg)
----------------------------------------------------------------
 1 3838  2003-04-08  20.1 ACIS-01237  -233.587 153.4  14.2   +80
 2 4385  2003-04-08  19.8 ACIS-01237  -233.587 153.4  13.6  +125
 3 4386  2003-04-08  19.8 ACIS-01237  -233.587 153.4  13.9  +172
 4 4387  2003-04-09  19.8 ACIS-01237  -233.587 153.4  14.3  -142
 5 4388  2003-04-09  19.8 ACIS-01237  -233.587 153.4  15.1  -101
 6 4389  2003-04-09  19.8 ACIS-01237  -233.587 153.6  13.7   -56
 7 4390  2003-04-09  19.8 ACIS-01237  -233.587 153.9  13.8    -5
 8 4391  2003-04-10  19.9 ACIS-01237  -233.587 153.4  15.8   +36
 9 4392  2003-04-10  19.6 ACIS-01237  -233.587 153.4   4.6   +54
10 4393  2003-04-11  19.6 ACIS-01237  -233.587 153.4   4.1   -80
11 4394  2003-04-11  19.6 ACIS-01237  -233.587 153.4   4.5  +177

Running tasks in parallel with 4 processors.
Reprojecting 11 event files to a common tangent point.
Merging reprojected events files to sn1006/merged_evt.fits

Calculating the output grid

The merged images will have 1619 by 1579 pixels, a pixel size of 1.968 arcsec,
    and cover x=844.5:7320.5:4, y=928.5:7244.5:4.

Creating the fluxed images for 11 observations in parallel.
Creating 4 aspect histograms for obsid 3838
Creating 4 aspect histograms for obsid 4385
Creating 4 aspect histograms for obsid 4386
Creating 4 aspect histograms for obsid 4387
Creating 4 aspect histograms for obsid 4388
Creating 4 aspect histograms for obsid 4389
Creating 4 aspect histograms for obsid 4390
Creating 4 aspect histograms for obsid 4391
Creating 4 aspect histograms for obsid 4392
Creating 4 aspect histograms for obsid 4393
Creating 4 aspect histograms for obsid 4394
Creating 16 instrument maps for obsid 3838
Creating 16 instrument maps for obsid 4385
Creating 16 instrument maps for obsid 4386
Creating 16 instrument maps for obsid 4387
Creating 16 instrument maps for obsid 4388
Creating 16 instrument maps for obsid 4389
Creating 16 instrument maps for obsid 4390
Creating 16 instrument maps for obsid 4391
Creating 16 instrument maps for obsid 4392
Creating 16 instrument maps for obsid 4393
Creating 16 instrument maps for obsid 4394
Creating 16 exposure maps for obsid 3838
Creating 16 exposure maps for obsid 4385
Creating 16 exposure maps for obsid 4386
Creating 16 exposure maps for obsid 4387
Creating 16 exposure maps for obsid 4388
Creating 16 exposure maps for obsid 4389
Creating 16 exposure maps for obsid 4390
Creating 16 exposure maps for obsid 4391
Creating 16 exposure maps for obsid 4392
Creating 16 exposure maps for obsid 4393
Creating 16 exposure maps for obsid 4394
Combining 4 exposure maps for 4 bands (obsid 3838)
Combining 4 exposure maps for 4 bands (obsid 4385)
Combining 4 exposure maps for 4 bands (obsid 4386)
Combining 4 exposure maps for 4 bands (obsid 4387)
Combining 4 exposure maps for 4 bands (obsid 4388)
Combining 4 exposure maps for 4 bands (obsid 4389)
Combining 4 exposure maps for 4 bands (obsid 4390)
Combining 4 exposure maps for 4 bands (obsid 4391)
Combining 4 exposure maps for 4 bands (obsid 4392)
Combining 4 exposure maps for 4 bands (obsid 4393)
Combining 4 exposure maps for 4 bands (obsid 4394)
Thresholding data for obsid 3838
Thresholding data for obsid 4385
Thresholding data for obsid 4386
Thresholding data for obsid 4387
Thresholding data for obsid 4388
Thresholding data for obsid 4389
Thresholding data for obsid 4390
Thresholding data for obsid 4391
Exposure-correcting 4 images for obsid 3838
Exposure-correcting 4 images for obsid 4385
Exposure-correcting 4 images for obsid 4386
Exposure-correcting 4 images for obsid 4387
Exposure-correcting 4 images for obsid 4388
Exposure-correcting 4 images for obsid 4389
Exposure-correcting 4 images for obsid 4390
Thresholding data for obsid 4392
Thresholding data for obsid 4393
Exposure-correcting 4 images for obsid 4391
Exposure-correcting 4 images for obsid 4392
Thresholding data for obsid 4394
Exposure-correcting 4 images for obsid 4393
Exposure-correcting 4 images for obsid 4394

Combining 11 observations.

The following files were created:

The co-added clipped counts images are:
     sn1006/broad_thresh.img
     sn1006/soft_thresh.img
     sn1006/medium_thresh.img
     sn1006/hard_thresh.img

The co-added clipped exposure maps are:
     sn1006/broad_thresh.expmap
     sn1006/soft_thresh.expmap
     sn1006/medium_thresh.expmap
     sn1006/hard_thresh.expmap

The combined FOVs are:
     sn1006/merged.fov

The co-added exposure-corrected images are:
     sn1006/broad_flux.img
     sn1006/soft_flux.img
     sn1006/medium_flux.img
     sn1006/hard_flux.img

Warning: the merged event file sn1006/merged_evt.fits
   should not be used to create ARF/RMF/exposure maps because
      the RA_NOM keyword varies by 0.6461 (limit is 0.0003)
      the DEC_NOM keyword varies by 0.4584 (limit is 0.0003)

The contents of the parameter file may be checked with plist merge_obs or using dmhistory:

unix% dmhistory sn1006/broad_flux.img merge_obs expand=no
merge_obs infiles="*/repro/*evt*[ccd_id=0:3]" outroot="sn1006/"
   bands="broad,csc" xygrid="" maxsize="INDEF" binsize="4"
   asolfiles="" badpixfiles="" maskfiles="" dtffiles="None"
   refcoord="" units="default" expmapthresh="1.5%"
   background="default" parallel="yes" nproc="INDEF"
   tmpdir="/tmp" cleanup="yes" clobber="no" verbose="1"

The script performs all the tasks needed to create the exposure corrected image (Figure 1), including:

validating each observation (e.g. to check that they are all compatible);
calculating the position for the reprojected data (this can be over-ridden by setting the refcoord parameter);
time sort the observations and display a summary;
automatically find the supporting files for each observation, such as aspect solution, bad-pixel, DTF file for HRC, mask file for ACIS (these files can be explicitly included or ignored if required using the asolfiles, badpixfiles, maskfiles, and dtffiles parameters);
create the output directory if required;
reproject each observation to the new reference position;
merge the reprojected event files (keeping only the common columns);
run fluximage on each reprojected observation;
combine the per-observation images and exposure maps, and use these to create the exposure-corrected image (or images, if multiple bands are given);
and summarize any observational differences that make using the merged event file with CIAO tools and scripts like specextract or mkwarf problematic.

Figure 1: Broad-band exposure-corrected image of SN1006 created by merge_obs

[Thumbnail image: The grid of ACIS-I data has been combined to show the SN1006 remnant.]

[Version: full-size]

[Print media version: The grid of ACIS-I data has been combined to show the SN1006 remnant.]

Figure 1: Broad-band exposure-corrected image of SN1006 created by merge_obs

unix% ds9 sn1006/broad_flux.img -scale log -zoom 0.25 -smooth -cmap b

The exposure-corrected 0.5 to 7 keV image is displayed. It can be compared to the "raw" counts image shown in Figure 2. Since the observations were filtered by [ccd_id=0:3], only the ACIS-I chips were used in the analysis. This avoids issues with combining data from front- and back-illuminated chips, as shown in Figure 8, at the expense of losing data.

Figure 2: Broad-band image and exposure map of SN1006 created by merge_obs

[Thumbnail image: Instrumental effects, such as chip edges, bad columns, and the grid pattern used, can be seen.]

[Version: full-size]

[Print media version: Instrumental effects, such as chip edges, bad columns, and the grid pattern used, can be seen.]

Figure 2: Broad-band image and exposure map of SN1006 created by merge_obs

unix% ds9 -scale log -zoom 0.25 -smooth -cmap b sn1006/broad_thresh.img sn1006/broad_thresh.expmap -scale linear

The image on the left - shown with a logarithmic scale - is the counts image in the 0.5 to 7 keV band. The image on the right - shown with a linear scale - is the exposure map for the data, and was evaluated at 2.3 keV. Both images have been "thresholded" to remove pixels where the exposure map has dropped to a small value (in this case, 1.5 percent of the maximum value per observation).

Since we set bands=broad,csc, we can also create a three-color image of the remnant (see Figure 3).

Figure 3: Three color, exposure-corrected image of SN1006 created by merge_obs

[Thumbnail image: The edge of the remnant is a different color to the central emission.]

[Version: full-size]

[Print media version: The edge of the remnant is a different color to the central emission.]

Figure 3: Three color, exposure-corrected image of SN1006 created by merge_obs

unix% cd sn1006
unix% ds9 -zoom 0.5 -scale log -smooth -rgb -red soft_flux.img -green medium_flux.img -blue hard_flux.img

The soft (red) channel is for the 0.5 to 1.2 keV band, the medium (green) channel is for the 1.2 to 2.0 keV band, and the hard (blue) channel is for the 2.0 to 7.0 keV band. More information can be found at the merge_obs parameter.

Manual reduction

In this section we run fluximage on each observation and then reproject the images to combine them. This is slightly different to the approach used by merge_obs above, which does the reprojection first, on the event files.

reproject_image_grid caveat

Users should be careful with the images created with reproject_image_grid (below). While the tool does preserve total flux, it does not preserve integer pixel values. Partial pixels with integer counts in the input image are mapped into non-integer, real valued pixels in the output image. This can lead to some aliasing effects especially when the input and output bin sizes are nearly the same.

The approach taken by merge_obs, to dmmerge the individual event files is the best way to combine images.

Create an Image and Exposure Maps for Each Observation (fluximage)

To run this thread, we want a source image and a congruent exposure map for each of the observations. We choose to create both by running the fluximage script. The image and exposure maps may also be created by following the Multiple-Chip ACIS Exposure Map thread.

In this example, we filter out the ACIS-S3 chip (ccd_id=7) from the images. Since the back-illuminated chips (ACIS-S1 and S3) have different background than the front-illuminated chips, eliminating S3 will reduce the chip-to-chip variations in the final image. If you choose to filter out a chip from your image, make sure that doing so does not remove important features from the data.

The image is binned by a factor of 4, and the preset "broad" energy band filter (500-7000 eV) is applied:

unix% punlearn fluximage
unix% pset binsize=4
unix% fluximage "3838/repro/*evt*[ccd_id=0:3]" manual/3838
Running fluximage
Version: 04 November 2021

Using event file 3838/repro/acisf03838_repro_evt2.fits[ccd_id=0:3]
Using CSC ACIS broad science energy band.
Aspect solution 3838/repro/pcadf03838_000N001_asol1.fits found.
Bad-pixel file 3838/repro/acisf03838_repro_bpix1.fits found.
Mask file 3838/repro/acisf03838_000N004_msk1.fits found.

The output images will have 740 by 741 pixels, pixel size of 1.968 arcsec,
    and cover x=2552.5:5512.5:4,y=2604.5:5568.5:4.

Running tasks in parallel with 4 processors.
Creating 4 aspect histograms for obsid 3838
Creating 4 instrument maps for obsid 3838
Creating 4 exposure maps for obsid 3838
Combining 4 exposure maps for obsid 3838
Thresholding data for obsid 3838
Exposure-correcting image for obsid 3838

The following files were created:

 The clipped counts image is:
     manual/3838_broad_thresh.img

 The observation FOV is:
     manual/3838.fov

 The clipped exposure map is:
     manual/3838_broad_thresh.expmap

 The exposure-corrected image is:
     manual/3838_broad_flux.img

Repeat the fluximage command for each of the ObsIDs, changing the infile and outroot:

unix% foreach obsid (4385 4386 4387 4388 4389 4390 4391 4392 4393 4394)
foreach? fluximage "${obsid}/repro/*evt*[ccd_id=0:3]" manual/${obsid}
foreach? end
...

A number of output files are created. The images that will be combined are:

unix% ls -1 manual/*_broad_thresh.img
manual/3838_broad_thresh.img
manual/4385_broad_thresh.img
manual/4386_broad_thresh.img
manual/4387_broad_thresh.img
manual/4388_broad_thresh.img
manual/4389_broad_thresh.img
manual/4390_broad_thresh.img
manual/4391_broad_thresh.img
manual/4392_broad_thresh.img
manual/4393_broad_thresh.img
manual/4394_broad_thresh.img

Figure 4 shows the eleven individual images.

Figure 4: Images of each observation

[Thumbnail image: The eleven event files are tiled in ds9.]

[Version: full-size]

[Print media version: The eleven event files are tiled in ds9.]

Figure 4: Images of each observation

unix% ds9 -zoom 0.25 -scale log -cmap b manual/*broad_thresh.img

Reproject the Images to a Common Tangent Point (reproject_image_grid)

reproject_image_grid maps an image - or many images - from the current WCS to a specified grid. This tool is used to reproject all the images of SN1006 to a common frame of reference, creating a mosaic of the object from the individual observations.

The filenames are input to reproject_image_grid as a stack file, images.lis:

unix% cd manual
unix% ls *_broad_thresh.img > images.lis

The parameters are set to create a 1500 square pixel image, centered at (225.7, -41.9). Each sky pixel will correspond to 2"; read the caveat about defining a pixel size in arcseconds before running reproject_image_grid.

unix% punlearn reproject_image_grid 
unix% reproject_image_grid @images.lis sn1006.image 1500 1500 225.7 -41.9 0
Pixel size (): 2"
BTIMDRFT values are different...FAIL...
BTIMNULL values are different...FAIL...
BTIMRATE values are different...FAIL...
omit - DEC_NOM values different more than 0.000300
omit - DEC_PNT values different more than 0.000300
warning: DS_IDENT has different value...Merged...
warning: OBS_ID has different value...Merged...
omit - RA_NOM values different more than 0.000300
omit - RA_PNT values different more than 0.000300

The messages are related to how the tool merges the header information in the input files. The merging_rules ahelp file explains the rules and how they affect the output file header.

Figure 5 shows the output image. The contents of the parameter file may be checked with plist reproject_image_grid or with dmhistory (which does not suffer the problems with converting 2" to 2'):

unix% dmhistory sn1006.image reproject_image_grid expand=no
reproject_image_grid infile="@images.lis" outfile="sn1006.image" 
   xsize="1500" ysize="1500" xcenter="225.7" ycenter="-41.9"
   theta="0" pixelsize="2"" projection="tan" resolution="1" 
   method="sum" coord_sys="world"
   lookupTab="/soft/ciao/data/dmmerge_header_lookup.txt"
   clobber="no" verbose="0"

Figure 5: Input images reprojected to the same WCS

[Thumbnail image: Chip gaps and exposure variations are visible in the combined image.]

[Version: full-size]

[Print media version: Chip gaps and exposure variations are visible in the combined image.]

Figure 5: Input images reprojected to the same WCS

unix% ds9 -scale log -cmap b -zoom 0.25 sn1006.image

Combining the Exposure Maps (reproject_image)

In order to exposure-correct the images, we need to combine the exposure map images into a single file that has the same resolution and WCS as the mosaic image. reproject_image maps an image - or many images - in one WCS reference frame to the WCS in a match image. The tool is used here to reproject the exposure maps to match the mosaic image.

unix% ls -1 *broad_thresh.expmap > expmaps.lis
unix% head -5 expmaps.lis
3838_broad_thresh.expmap
4385_broad_thresh.expmap
4386_broad_thresh.expmap
4387_broad_thresh.expmap
4388_broad_thresh.expmap

It is important to note that the method parameter is set to average; this is because we want the average exposure value for each pixel in the combined image, not the sum of all of them.

unix% punlearn reproject_image
unix% reproject_image @expmaps.lis sn1006.image sn1006.expmap method=average
BTIMDRFT values are different...FAIL...
BTIMNULL values are different...FAIL...
BTIMRATE values are different...FAIL...
omit - DEC_NOM values different more than 0.000300
omit - DEC_PNT values different more than 0.000300
warning: DS_IDENT has different value...Merged...
warning: OBS_ID has different value...Merged...
omit - RA_NOM values different more than 0.000300
omit - RA_PNT values different more than 0.000300

The messages are related to how the tool merges the header information in the input files. The merging_rules ahelp file explains the rules and how they affect the output file header.

The reprojected exposure maps are shown in Figure 6. The contents of the parameter file may be checked with dmhistory:

unix% dmhistory sn1006.expmap reproject_image expand-
reproject_image infile="@expmaps.lis" matchfile="sn1006.image"
   outfile="sn1006.expmap" resolution="1" method="average"
   coord_sys="world"
   lookupTab="/soft/ciao/data/dmmerge_header_lookup.txt"
   clobber="no" verbose="0"

Figure 6: Reprojected exposure maps

[Thumbnail image: Bad columns, bad rows, and chips gaps are visible in the combined exposure map image.]

[Version: full-size]

[Print media version: Bad columns, bad rows, and chips gaps are visible in the combined exposure map image.]

Figure 6: Reprojected exposure maps

unix% ds9 -cmap b -zoom 0.25 sn1006.expmap

Exposure-correct the Image Mosaic (dmimgthresh & dmimgcalc)

The strongly variable exposure near the edge of a dithered field may produce "hot" pixels when divided into an image. While technically proper, these hot pixels can be an eyesore, drawing attention to a noisy, uninteresting portion of the image. The images and exposure maps used above (those containing the label _thresh) have already been "thresholded" to remove these pixels. If you want to do this yourself you can use the dmimgthresh; for example

unix% punlearn dmimgthresh
unix% dmimgthresh sn1006.image sn1006_thresh.image expfile=sn1006.expmap cut=1.5%
unix% dmimgthresh sn1006.expmap sn1006_thresh.expmap cut=1.5%

which sets those pixels in sn1006.image whose corresponding exposure value (from sn1006.expmap) is less than 1.5% the peak value to 0.0 in sn1006_thresh.image. You may want to adjust these values for your own observation.

We use dmimgcalc to divide the image by the exposure map, creating the exposure-corrected image:

unix% punlearn dmimgcalc 
unix% dmimgcalc sn1006.image sn1006.expmap sn1006.flux div
warning: CONTENT has 1 different values.

The exposure-corrected image is shown in Figure 7.

Figure 7: Exposure-corrected image

[Thumbnail image: Exposure-correcting the image removes the chips gaps and the majority of the exposure variations.]

[Version: full-size]

[Print media version: Exposure-correcting the image removes the chips gaps and the majority of the exposure variations.]

Figure 7: Exposure-corrected image

unix% ds9 -zoom 0.25 -scale log -cmap b -smooth sn1006.flux

Improving the Combined Image

There are several additional methods that may be used to improve the quality of the final image.

Background Subtraction

As discussed in the Create an Image of Each Observation section, we filtered out the ACIS-S3 chip to reduce the chip-to-chip exposure variations. Figure 8 compares this fluxed image to the results if the S3 chip is not removed. This is not an option for all observations, e.g. if there is significant data on the back-illuminated chips. If you must include both front- and back-illuminated chips, try using background subtraction to compensate for the different chip exposures.

Figure 8: Comparing exposure-corrected images with and without the S3 chip

[Thumbnail image: The two images are displayed side-by-side in ds9/]

[Version: full-size]

[Print media version: The two images are displayed side-by-side in ds9/]

Figure 8: Comparing exposure-corrected images with and without the S3 chip

The left frame has ACIS-S3 filtered out of the data; the right image includes that chip.

Energy Filtering

This thread uses monochromatic exposure maps created for the full energy range of the data files. To more accurately represent the spectrum of the data you can use narrower energy bands - such as the soft, medium, and hard bands used to create Figure 3 - or use a spectral weights file to weight the exposure map by a source spectrum.

Smoothing

Adaptively smoothing the data with aconvolve will create a nice image for publication; see the ahelp file for examples. Note that care must be taken in the scientific interpretation of the smoothed image as it is highly processed. The An Image of Diffuse Emission thread describes one way of removing point sources before smoothing data.


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


       infiles = */repro/*evt*[ccd_id=0:3] Input events files
       outroot = sn1006/          Root of output files
        (bands = default)         Energy bands, comma-separated list, min:max:center in keV or ultrasoft, soft, medium, hard, broad, wide, CSC
       (xygrid = )                xygrid for output or filename
      (maxsize = INDEF)           Maximum image width or height in pixels
      (binsize = INDEF)           Image binning factor
    (asolfiles = )                Input aspect solutions
  (badpixfiles = )                Input bad pixel files
    (maskfiles = )                Input mask files
     (dtffiles = )                Input dtf files for HRC observations
     (refcoord = )                Reference coordinates or evt2 file
        (units = default)         Units for the exposure map
 (expmapthresh = 1.5%)            Remove low-exposure regions? '2%' excludes pixels where exposure is < 2% of the maximum
   (background = default)         Method for background removal (HRC-I)
     (parallel = yes)             Run processes in parallel?
        (nproc = INDEF)           Number of processors to use
       (tmpdir = ${ASCDS_WORK_PATH} -> /tmp) Directory for temporary files
      (cleanup = yes)             Delete intermediary files?
      (clobber = no)              OK to overwrite existing output file?
      (verbose = 1)               Verbosity level
         (mode = ql)


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


        infile = @images.lis      Input image file name
       outfile = sn1006.image     Output file name
         xsize = 1500             X-Size of output image in image pixels
         ysize = 1500             Y-Size of output image in image pixels
       xcenter = 225.7            X-Center of image in coord_sys
       ycenter = -41.9            Y-Center of image in coord_sys
         theta = 0                Angle between world coord north and output y axis
     pixelsize = 2'               Pixel size
   (projection = tan)             Projection from world to physical
   (resolution = 1)               Number of point per side to evaluate
       (method = sum)             Average value
    (coord_sys = world)           Coordinate system to match images in
    (lookupTab = ${ASCDS_CALIB}/dmmerge_header_lookup.txt -> /soft/ciao/data/dmmerge_header_lookup.txt) lookup table
      (clobber = no)              Clobber existing files
      (verbose = 0)               Tool verbosity
         (mode = ql)


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


        infile = sn1006_image_clean.fits Input file #1
       infile2 = sn1006_expmap.fits Input file #2
       outfile = sn1006_fluxed.fits output file 
     operation = div              arithmetic operation
       (weight = 1)               weight for first image
      (weight2 = 1)               weight for second image
    (lookupTab = ${ASCDS_CALIB}/dmmerge_header_lookup.txt -> /soft/ciao/data/dmmerge_header_lookup.txt) lookup table
      (clobber = no)              delete old output
      (verbose = 0)               output verbosity
         (mode = ql)

History

24 Jan 2012	reviewed for CIAO 4.4: use fluximage to create the images and the exposure maps; renamed "Create an Image of Each Observation" section to Create an Image and Exposure Maps for Each Observation
15 Oct 2012	The thread has been updated to use the new merge_obs script and to account for updates to fluximage in the 15 October 2012 scripts package release.
03 Dec 2012	Review for CIAO 4.5; mkexpmap chatter removed and dmhistory bug now fixed.
03 Dec 2013	Review for CIAO 4.6: the pbkfiles parameter has been removed from the merge_obs script.
22 Dec 2014	Reviewed for CIAO 4.7. Added a caveat about using reproject_image_grid with integer counts images.
07 Feb 2022	Review for CIAO 4.14. No changes.

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Making an exposure-corrected mosaic

Overview

Synopsis:

Purpose:

Contents

Get Started

Using merge_obs to automate the process

Figure 1: Broad-band exposure-corrected image of SN1006 created by merge_obs

Figure 1: Broad-band exposure-corrected image of SN1006 created by merge_obs

Figure 2: Broad-band image and exposure map of SN1006 created by merge_obs

Figure 2: Broad-band image and exposure map of SN1006 created by merge_obs

Figure 3: Three color, exposure-corrected image of SN1006 created by merge_obs

Figure 3: Three color, exposure-corrected image of SN1006 created by merge_obs

Manual reduction

Create an Image and Exposure Maps for Each Observation (fluximage)

Figure 4: Images of each observation

Figure 4: Images of each observation

Reproject the Images to a Common Tangent Point (reproject_image_grid)

Figure 5: Input images reprojected to the same WCS

Figure 5: Input images reprojected to the same WCS

Combining the Exposure Maps (reproject_image)

Figure 6: Reprojected exposure maps

Figure 6: Reprojected exposure maps

Exposure-correct the Image Mosaic (dmimgthresh & dmimgcalc)

Figure 7: Exposure-corrected image

Figure 7: Exposure-corrected image

Improving the Combined Image

Background Subtraction

Figure 8: Comparing exposure-corrected images with and without the S3 chip

Figure 8: Comparing exposure-corrected images with and without the S3 chip

Energy Filtering

Smoothing

History