1. comparison of rgs model for 1e0102.2 -7219 to the hetg … · 2009. 1. 22. · chandra x-ray...
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Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20061
1.1. Comparison of RGS Model for Comparison of RGS Model for
1E0102.21E0102.2--72197219 to the HETG datato the HETG data
2.2. BI CCD CTI Correction for ACISBI CCD CTI Correction for ACIS
Paul Plucinsky, Dan Dewey,Paul Plucinsky, Dan Dewey,
& Joseph & Joseph DePasqualeDePasquale
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20062
Gratuitous Pretty Pictures of E0102Gratuitous Pretty Pictures of E0102
S3 Summed Data ~100 S3 Summed Data ~100 ksks RGS Spectrum (Pollock 2006)RGS Spectrum (Pollock 2006)
Objective:Objective: develop a spectral model which can be used by RGS, HETG,
EPIC & ACIS, etc.
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20063
WhatWhat’’s New Since the Iceland 2006 Meeting?s New Since the Iceland 2006 Meeting?
• Pollock’s model based on the RGS data has been used by Dan
Dewy of the HETG team to compare to the HETG data
• Dan adopted the RGS spectral model, including the normalizations
• Dan developed a spatial model for the structure of the remnant
• He created simulated datasets to compare the against the MEG
and HEG data from the Chandra HETG
The overall agreement is encouraging !!!
All of the following work has been done by Dan,
many thanks !!!
• Good agreement on the bright lines, some disagreement on the
weaker lines
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20064
Dewey Spatial and Spectral ModelDewey Spatial and Spectral Model
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20065
MEG minus
1st order
Simulation
Comparison
KS test
OVIII OVIINeIXNeXMgXI
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20066
MEG plus
1st order
Simulation
Comparison
KS test
MgXI NeX NeIX OVIII OVII
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20067
HEG minus
1st order
Simulation
Comparison
KS test
MgXI NeX NeIX
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20068
HEG plus
1st order
Simulation
Comparison
KS test
MgXI NeX NeIX
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 20069
Where Do We Go From Here ?Where Do We Go From Here ?
• Dewey analysis needs to be updated with latest response files for
HRMA/ACIS/HETG
• Line-based analysis needs to be updated with the latest response
files for HRMA/HETG/ACIS
• RGS data need to be re-analyzed with new background model for
RGS
• RGS and HETG teams agree on a model well before the IACHEC
meeting in California
• ACIS, MOS, and pn use the new model to fit the CCD spectra
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200610
2. CTI Correction in CIAO for S3 and S12. CTI Correction in CIAO for S3 and S1
• Penn State CTI corrector available since 2001
• CXC response products for S1 and S3 used a position-dependent
gain correction which recovers the true values of the PHs but does
not improve the spectral resolution
• S3 and S1 data will now be CTI-corrected in the events files
provided to GOs
• All TEN CCDs will be CTI-corrected as of CIAO and CALDB
release in December 2006
• small, but significant improvement in spectral resolution and QE
uniformity
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200611
BI CTI correction: PH BI CTI correction: PH vsvs. Row # . Row #
Current CALDB: no CTI correction Prototype CALDB: CTI correction
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200612
BI CTI correction: PH BI CTI correction: PH vsvs. Row # . Row #
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200613
S3 CTI correction:S3 CTI correction: MnMn--K K at the at the Aimpoint Aimpoint
No CTI
correction:
FWHM~162 eV
With CTI
correction:
FWHM~151 eV
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200614
S3 CTI correction:S3 CTI correction: MnMn--K K at theat the Top Top
No CTI
correction:
FWHM~182 eV
With CTI
correction:
FWHM~157 eV
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200615
Current
CALDB
No CTI
correction:
E0102 on
S3
Red Chi=
1.44
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200616
BI CTI
correction:
E0102 on
S3
Red Chi=
1.10
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200617
BI CTI
correction:
E0102 on
S1
Red Chi=
1.57
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200618
Pollock RGS Pollock RGS vsvs.. Flanagan (2004) HETGFlanagan (2004) HETG Line FluxesLine Fluxes
+9.7%1.872.07Ne X Ly-β
-30.7%12.709.72Ne X Ly-α
+8.8%21.1523.18Ne IX triplet
-15.9%7.786.37O VIII Ly-β
-8.9%40.6537.31O VIII Ly-α
-11.7%27.2324.38OVII Res
+17.3%11.5313.95OVII For
DifferencePollock Flux(10-4 photons cm-2 s-1)
Flanagan Flux(10-4 photons cm-2 s-1)
Line
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200619
O O VIII VIII Ly Ly αααααααα and and Ne Ne X X Ly Ly αααααααα NormalizationNormalization ResultsResults• Data sets fit independently, O and Ne line complexes are free to vary as a group
• SMC NH=5.65x1020 cm-2, Bremsstrahlung kT=0.95 keV
92
279
93
95
DOF
2.511.71
[1.68,1.73]
6.42
[6.35,6.53]
MOS10135720601
[90% CL]
2.691.74
[1.72,1.76]
6.14
[6.09,6.19]
pn0135720801
[90% CL]
1.481.77
[1.69,1.84]
6.92
[6.79,7.36]
ACIS S3
(node 0)
6765
[90% CL]
1.271.80
[1.73,1.88]
6.58
[6.44,6.94]
ACIS S3
(node 1)
3545
[90% CL]
Red χ2
Ne X Ly α Norm
(x 10-3 photons cm-2 s)
O VIII Ly α Norm
(x 10-3 photons cm-2 s)
Instrumen
t
OBSID
• Ne X Ly a normalizations agree within ~6.0% for ACIS, pn, & MOS1
• Early S3 and MOS1 agree within ~2.0% for O VIII Ly αααα normalizations
• Most recent S3 and pn disgree by ~18.0% for O VIII Ly αααα normalizations
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal October 200620
LetLet’’s Agree on a Model !!!!!!!s Agree on a Model !!!!!!!
Purpose: to improve the low-energy response model of ACIS, MOS
and pn CCD instruments
1) RGS and HETG agree on flux of bright lines
2) RGS and HETG compromise on existence of weak lines
3) RGS and HETG agree on widths for the lines
4) Select a continuum model and absorption
5) HETG team must analyze second epoch observations of E0102
6) Fit ACIS, MOS, and pn with the same model