Introduction This thread describes how to create EPIC background subtracted, exposure corrected images combining data from the three instruments. A full guide to the use of the ESAS software can be found here.Expected Outcome The final outcome of this thread are adaptively smoothed images in two spectral bands. In the process of creating the images full field of view and outer annulus spectral products (source and model background spectra, RMFs, and ARFs) are produced as well as count, exposure, and background count images.SAS Tasks to be Used
Prerequisites Useful Links
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epchain
epchain withoutoftime=true
emchain
pn-filter
mos-filter
Note that mos-filter indicates which CCDs are operating in an anomalous mode (the one marked by **** in the example below). These CCDs should be excluded in downstream processing.
1S003
Limit>1.5 CCD=2 Hardness=5.100 Uncertainty=0.882
Limit>1.5 CCD=3 Hardness=5.607 Uncertainty=1.150
Limit>2.5 CCD=4 Hardness=3.110 Uncertainty=0.418
Limit>2.5 CCD=5 Hardness=1.526 Uncertainty=0.149 ****
Limit>1.5 CCD=6 Hardness=4.000 Uncertainty=0.716
Limit>1.5 CCD=7 Hardness=5.629 Uncertainty=1.032
2S004
Limit>2.5 CCD=2 Hardness=2.639 Uncertainty=0.365
Limit>1.5 CCD=3 Hardness=4.419 Uncertainty=0.746
Limit>1.5 CCD=4 Hardness=6.875 Uncertainty=1.301
Limit>2.5 CCD=5 Hardness=3.982 Uncertainty=0.590
Limit>1.5 CCD=6 Hardness=4.432 Uncertainty=0.807
Limit>1.5 CCD=7 Hardness=4.600 Uncertainty=0.757
The diagnostic plots created by the filtering tasks should also be examined as
they provide an indication of the quality of the data. These have names like
mos1S003-hist.qdp, mos2S004-hist.qdp, and pnS005-hist.qdp
and cam be plotted using the command, for example, qdp mos1S003-hist.qdp.
Figure 1 shows the light-curve screening for the MOS1 instrument.
Figure 1: MOS1 light curve for the Abell 1795 observation. Notice the residual variation of the nominally good data which indicates the possible existence of residual soft proton contamination.
cheese prefixm='1S003 2S004' prefixp=S005 scale=0.5 rate=1.0 dist=40.0 \
clobber=0 elow=400 ehigh=10000
Figure 2: MOS1 (left) and MOS2 (right) images in the soft (0.2-1.0 keV) band. Note the excess counts in the upper left CCD in the MOS1 image most noticeable in the unexposed (to the sky) upper left corner. Displayed by the command: ds9 *soft* &.
Figure 3: MOS1 (left), MOS2 (middle), and pn (right) cheese masks. Displayed
by the command: ds9 *cheese* &
mos-spectra prefix=1S003 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=400 ehigh=1250 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos-spectra prefix=1S003 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=2000 ehigh=7200 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos-spectra prefix=2S004 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=400 ehigh=1250 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
mos-spectra prefix=2S004 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=2000 ehigh=7200 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
pn-spectra prefix=S005 caldb=/software/XMM/CCF/esas region=pn-reg.txt \
mask=1 elow=400 ehigh=1250 pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
pn-spectra prefix=S005 caldb=/software/XMM/CCF/esas region=pn-reg.txt \
mask=1 elow=2000 ehigh=7200 pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
mos_back prefix=1S003 caldb=/PATH/esascaldb diag=0 elow=400 ehigh=1250 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos_back prefix=1S003 caldb=/PATH/esascaldb diag=0 elow=2000 ehigh=7200 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos_back prefix=2S004 caldb=/PATH/esascaldb diag=0 elow=400 ehigh=1250 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
mos_back prefix=2S004 caldb=/PATH/esascaldb diag=0 elow=2000 ehigh=7200 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
pn_back prefix=S005 caldb=/PATH/esascaldb diag=0 elow=400 ehigh=1250 \
pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
pn_back prefix=S005 caldb=/PATH/esascaldb diag=0 elow=2000 ehigh=7200 \
pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
Figure 4: MOS1 (left) and MOS2 (right) model particle images in the soft (0.4-1.25 keV) band. The different colors for the different CCDs are an indication of the variations in their exposures (caused by CCDs operating in anomalous modes, CCD1 operating in non-full field imaging mode, and the loss of CCD6 of MOS1 to the micrometeorite strike. Displayed by the command: ds9 mos1S003-back-im-det-400-1250.fits mos2S004-back-im-det-400-1250.fits &.
Figure 5: MOS1 source (red) and QPB (green) spectra. Displayed by the command: qdp mos1S003-spec.qdp.
rot-im-det-sky prefix=1S003 mask=0 elow=400 ehigh=1250 mode=1
rot-im-det-sky prefix=1S003 mask=0 elow=2000 ehigh=7200 mode=1
rot-im-det-sky prefix=2S004 mask=0 elow=400 ehigh=1250 mode=1
rot-im-det-sky prefix=2S004 mask=0 elow=2000 ehigh=7200 mode=1
rot-im-det-sky prefix=S005 mask=0 elow=400 ehigh=1250 mode=1
rot-im-det-sky prefix=S005 mask=0 elow=2000 ehigh=7200 mode=1
mv mos1S003-obj.pi mos1S003-obj-full.pi
mv mos1S003.rmf mos1S003-full.rmf
mv mos1S003.arf mos1S003-full.arf
mv mos1S003-back.pi mos1S003-back-full.pi
mv mos1S003-obj-im-sp-det.fits mos1S003-sp-full.fits
mv mos2S004-obj.pi mos2S004-obj-full.pi
mv mos2S004.rmf mos2S004-full.rmf
mv mos2S004.arf mos2S004-full.arf
mv mos2S004-back.pi mos2S004-back-full.pi
mv mos2S004-obj-im-sp-det.fits mos2S004-sp-full.fits
mv pnS005-obj-os.pi pnS005-obj-os-full.pi
mv pnS005-obj.pi pnS005-obj-full.pi
mv pnS005-obj-oot.pi pnS005-obj-oot-full.pi
mv pnS005.rmf pnS005-full.rmf
mv pnS005.arf pnS005-full.arf
mv pnS005-back.pi pnS005-back-full.pi
mv pnS005-obj-im-sp-det.fits pnS005-sp-full.fits
specgroup spectrumset=mos1S003-obj-full.pi mincounts=100
rmfset=mos1S003-full.rmf \
arfset=mos1S003-full.arf backgndset=mos1S003-back-full.pi groupedset=mos1S003-obj-full-grp.pi
specgroup spectrumset=mos2S004-obj-full.pi mincounts=100
rmfset=mos2S004-full.rmf \
arfset=mos2S004-full.arf backgndset=mos2S004-back-full.pi groupedset=mos2S004-obj-full-grp.pi
specgroup spectrumset=pnS005-obj-os-full.pi mincounts=100
rmfset=pnS005-full.rmf \
arfset=pnS005-full.arf backgndset=pnS005-back-full.pi groupedset=pnS005-obj-os-full-grp.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=1 maskfile=mos1S003-sp-full.fits \
specfile=mos1S003-obj-full.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=2 maskfile=mos2S004-sp-full.fits \
specfile=mos2S004-obj-full.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=2 maskfile=pnS005-sp-full.fits \
specfile=pnS005-obj-full.pi
The result of the fitting process is shown if Figure 6.
Figure 6: Best fit of the Abell 1795 data from the full FOV. The green data and model curves are from the pn, the black and red data and model curves are from the MOS1 and MOS2, respectively, and the blue model and curve are from the RASS. The straight line model curves for the MOS and pn are the soft proton contribution.
proton prefix=1S003 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 \
ccd6=0 ccd7=1 elow=400 ehigh=1250 spectrumcontrol=1 pindex=0.972080 pnorm=0.131099
proton prefix=1S003 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 \
ccd6=0 ccd7=1 elow=2000 ehigh=7200 spectrumcontrol=1 pindex=0.972080 pnorm=0.131099
proton prefix=2S004 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=0 ccd3=1 ccd4=1 ccd5=1 \
ccd6=1 ccd7=1 elow=400 ehigh=1250 spectrumcontrol=1 pindex=0.972080 pnorm=0.128477
proton prefix=2S004 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=0 ccd3=1 ccd4=1 ccd5=1 \
ccd6=1 ccd7=1 elow=2000 ehigh=7200 spectrumcontrol=1 pindex=0.972080 pnorm=0.128477
proton prefix=S005 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 \
elow=400 ehigh=1250 spectrumcontrol=1 pindex=1.53003 pnorm=0.361532
proton prefix=S005 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 \
elow=3000 ehigh=7200 spectrumcontrol=1 pindex=1.53003 pnorm=0.361532
rot-im-det-sky prefix=1S003 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=1S003 mask=0 elow=2000 ehigh=7200 mode=2
rot-im-det-sky prefix=2S004 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=2S004 mask=0 elow=2000 ehigh=7200 mode=2
rot-im-det-sky prefix=S005 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=S005 mask=0 elow=2000 ehigh=7200 mode=2
At this point all of the components for all three instruments are ready to create and image. Figure 7 displays the components for MOS1.
Figure 7: MOS1 image components with the count image which also shows the excluded point source regions (upper left), exposure image (upper right), QPB image (lower left), and soft proton image lower right.
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=0 \
nbands=1 elowlist=400 ehighlist=1250 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=0 \
nbands=1 elowlist=2000 ehighlist=7200 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
Figure 8 shows the merged component images.
Figure 7: Merged image components with the count image (upper left), exposure image (upper right), QPB image (lower left), and soft proton image lower right. The negative counts in the count image are an artifact of the pn OOT correction.
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=400 ehigh=1250 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=2000 ehigh=7200 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
mv adapt-400-1250.fits adapt-400-1250-full.fits
mv adapt-2000-7200.fits adapt-2000-7200-full.fits
ds9 adapt-400-1250-full.fits adapt-2000-7200-full.fits &
Figure 9 shows the final adaptively smoothed, background subtracted, and exposure corrected images.
Figure 9: Abell 1795 adaptively smoothed, background subtracted, and exposure corrected images in the 0.4-1.25 keV and 2.0-7.2 keV bands.
regm1-ann.txt: &&((DETX,DETY) IN circle(134,-219,14200))&&!((DETX,DETY) IN circle(134,-219,10600))
regm2-ann.txt: &&((DETX,DETY) IN circle(6,-93,14200))&&!((DETX,DETY) IN circle(6,-93,10600))
regpn-ann.txt: &&((DETX,DETY) IN circle(59,-10,14200))&&!((DETX,DETY) IN circle(59,-10,10600))
Run mos-spectra, pn-spectra, mos_back, and, pn_back to do the spectral extraction and prepare for the background modeling. Use band limits of 0 0 since we aren't interested in recreating the image components.
mos-spectra prefix=1S003 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=0 ehigh=0 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos-spectra prefix=2S004 caldb=/PATH/esascaldb region=reg.txt mask=1 \
elow=0 ehigh=0 ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
pn-spectra prefix=S005 caldb=/software/XMM/CCF/esas region=pn-reg.txt \
mask=1 elow=0 ehigh=0 pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
mos_back prefix=1S003 caldb=/PATH/esascaldb diag=0 elow=0 ehigh=0 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1
mos_back prefix=2S004 caldb=/PATH/esascaldb diag=0 elow=0 ehigh=0 \
ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1
pn_back prefix=S005 caldb=/PATH/esascaldb diag=0 elow=0 ehigh=0 \
pattern=4 quad1=1 quad2=1 quad3=1 quad4=1
mv mos1S003-obj.pi mos1S003-obj-ann.pi
mv mos1S003.rmf mos1S003-ann.rmf
mv mos1S003.arf mos1S003-ann.arf
mv mos1S003-back.pi mos1S003-back-ann.pi
mv mos1S003-obj-im-sp-det.fits mos1S003-sp-ann.fits
mv mos2S004-obj.pi mos2S004-obj-ann.pi
mv mos2S004.rmf mos2S004-ann.rmf
mv mos2S004.arf mos2S004-ann.arf
mv mos2S004-back.pi mos2S004-back-ann.pi
mv mos2S004-obj-im-sp-det.fits mos2S004-sp-ann.fits
mv pnS005-obj-os.pi pnS005-obj-os-ann.pi
mv pnS005-obj.pi pnS005-obj-ann.pi
mv pnS005-obj-oot.pi pnS005-obj-oot-ann.pi
mv pnS005.rmf pnS005-ann.rmf
mv pnS005.arf pnS005-ann.arf
mv pnS005-back.pi pnS005-back-ann.pi
mv pnS005-obj-im-sp-det.fits pnS005-sp-ann.fits
specgroup spectrumset=mos1S003-obj-ann.pi mincounts=100
rmfset=mos1S003-ann.rmf \
arfset=mos1S003-ann.arf backgndset=mos1S003-back-ann.pi groupedset=mos1S003-obj-ann-grp.pi
specgroup spectrumset=mos2S004-obj-ann.pi mincounts=100
rmfset=mos2S004-ann.rmf \
arfset=mos2S004-ann.arf backgndset=mos2S004-back-ann.pi groupedset=mos2S004-obj-ann-grp.pi
specgroup spectrumset=pnS005-obj-os-ann.pi mincounts=100
rmfset=pnS005-ann.rmf \
arfset=pnS005-ann.arf backgndset=pnS005-back-ann.pi groupedset=pnS005-obj-os-ann-grp.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=1 maskfile=mos1S003-sp-ann.fits \
specfile=mos1S003-obj-ann.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=2 maskfile=mos2S004-sp-ann.fits \
specfile=mos2S004-obj-ann.pi
proton_scale caldb=/PATH/esascaldb mode=1 detector=2 maskfile=pnS005-sp-ann.fits \
specfile=pnS005-obj-ann.pi
Fit the spectral data to determine the soft proton contamination parameters (Xspec XCM file). Note that the fitting process is complicated with a strong likelihood of local minima. The Al, Si, and Cu fluorescent background lines in particular should start frozen until a reasonably good fit is achieved and then thawed. After a new, and probably a significantly better fit is achieved they can be frozen again to reduce the number of free parameters and again improve the fit.
The result of the annular fitting process is shown if Figure 10. The cluster emission is now relatively minor allowing for a much improved fit to the various background components.
Figure 10: Best fit of the Abell 1795 data from the outer annulus. The green data and model curves are from the pn, the black and red data and model curves are from the MOS1 and MOS2, respectively, and the blue model and curve are from the RASS. The straight line model curves for the MOS and pn are the soft proton contribution.
sp_partial caldb=/PATH/esascaldb detector=1 fullimage=mos1S003-sp-full.fits \
fullspec=mos1S003-obj-full.pi regionimage=mos1S003-sp-ann.fits \
regionspec=mos1S003-obj-ann.pi rnorm=2.10680E-02
sp_partial caldb=/PATH/esascaldb detector=2 fullimage=mos2S004-sp-full.fits \
fullspec=mos2S004-obj-full.pi regionimage=mos2S004-sp-ann.fits \
regionspec=mos2S004-obj-ann.pi rnorm=2.68596E-02
sp_partial caldb=/PATH/esascaldb detector=3 fullimage=pnS005-sp-full.fits \
fullspec=pnS005-obj-os-full.pi regionimage=pnS005-sp-ann.fits \
regionspec=pnS005-obj-os-ann.pi rnorm=4.96011E-02
proton prefix=1S003 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 \
ccd6=0 ccd7=1 elow=400 ehigh=1250 spectrumcontrol=1 pindex=0.827748 pnorm=7.3188223E-02
proton prefix=1S003 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 \
ccd6=0 ccd7=1 elow=2000 ehigh=7200 spectrumcontrol=1 pindex=0.827748 pnorm=7.3188223E-02
proton prefix=2S004 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=0 ccd3=1 ccd4=1 ccd5=1 \
ccd6=1 ccd7=1 elow=400 ehigh=1250 spectrumcontrol=1 pindex=0.827748 pnorm=8.9574702E-02
proton prefix=2S004 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=0 ccd3=1 ccd4=1 ccd5=1 \
ccd6=1 ccd7=1 elow=2000 ehigh=7200 spectrumcontrol=1 pindex=0.827748 pnorm=8.9574702E-02
proton prefix=S005 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 \
elow=400 ehigh=1250 spectrumcontrol=1 pindex=1.15194 pnorm=0.1667362
proton prefix=S005 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 \
elow=3000 ehigh=7200 spectrumcontrol=1 pindex=1.15194 pnorm=0.1667362
rot-im-det-sky prefix=1S003 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=1S003 mask=0 elow=2000 ehigh=7200 mode=2
rot-im-det-sky prefix=2S004 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=2S004 mask=0 elow=2000 ehigh=7200 mode=2
rot-im-det-sky prefix=S005 mask=0 elow=400 ehigh=1250 mode=2
rot-im-det-sky prefix=S005 mask=0 elow=2000 ehigh=7200 mode=2
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=0 \
nbands=1 elowlist=400 ehighlist=1250 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=0 \
nbands=1 elowlist=2000 ehighlist=7200 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=400 ehigh=1250 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=2000 ehigh=7200 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
mv adapt-400-1250.fits adapt-400-1250-ann.fits
mv adapt-2000-7200.fits adapt-2000-7200-ann.fits
ds9 adapt-400-1250-ann.fits adapt-2000-7200-ann.fits
Figure 11 shows the final adaptively smoothed, background subtracted, and exposure corrected images, this time with the better parametrization of the background components allowed by using the outer annulus. The effect is most clearly shown in the 0.4-1.25 keV band where the background is no longer over-subtracted.
Figure 11: Abell 1795 adaptively smoothed, background subtracted, and exposure corrected images in the 0.4-1.25 keV and 2.0-7.2 keV bands.
swcx prefix=1S003 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=0 ccd6=1 ccd7=1 \
elow=400 ehigh=1250 linelist='1 2' gnormlist='0.0 7.65634E-08' objarf=mos1S003-full.arf \
objspec=mos1S003-obj-full.pi
swcx prefix=2S004 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 ccd5=1 ccd6=1 ccd7=1 \
elow=400 ehigh=1250 linelist='1 2' gnormlist='0.0 7.65634E-08' objarf=mos2S004-full.arf \
objspec=mos2S004-obj-full.pi
swcx prefix=S005 caldb=/software/XMM/CCF/esas ccd1=1 ccd2=1 ccd3=1 ccd4=1 elow=400 ehigh=1250 \
linelist='1 2' gnormlist='0.0 7.65634E-08' objarf=pnS005-full.arf objspec=pnS005-obj-full.pi
rot-im-det-sky prefix=1S003 mask=0 elow=400 ehigh=1250 mode=3
rot-im-det-sky prefix=2S004 mask=0 elow=400 ehigh=1250 mode=3
rot-im-det-sky prefix=S005 mask=0 elow=400 ehigh=1250 mode=3
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=1 \
nbands=1 elowlist=400 ehighlist=1250 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
comb caldb=/software/XMM/CCF/esas withpartcontrol=1 withsoftcontrol=1 withswcxcontrol=1 \
nbands=1 elowlist=2000 ehighlist=7200 mask=1 ndata=3 prefixlist="1S003 2S004 S005"
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=400 ehigh=1250 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
adapt_900 smoothingcounts=50 thresholdmasking=0.02 detector=0 binning=2 elow=2000 ehigh=7200 \
withpartcontrol=yes withsoftcontrol=yes withswcxcontrol=0
mv adapt-400-1250.fits adapt-400-1250-ann-swcx.fits
mv adapt-2000-7200.fits adapt-2000-7200-ann-swcx.fits
ds9 adapt-400-1250-ann-swcx.fits adapt-2000-7200-ann-swcx.fits
Caveats
For information about known issues, refer to the ESAS Warnings and Watchouts pages. |