fitting pn and mos data with the iachec models for e0102 ... · the iachec model for e0102 is the...
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CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Fitting pn and MOS data with the IACHEC Models for E0102 and N132D
1
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
IACHEC Thermal SNR Working Group One of the “Standard candle” working groups. Many thanks to the WG members:
XMM-Newton RGS Andy Pollock(Sheffield), Martin Stuhlinger (ESAC) XMM-Newton MOS Steve Sembay (Leicester) XMM-Newton pn Frank Haberl (MPE) Chandra ACIS Paul Plucinsky (SAO) Chandra HETG Dan Dewey (MIT) Suzaku XIS Eric Miller (MIT) Swift XRT Andrew Beardmore (Leicester) Models Adam Foster (SAO) ASTROSAT Sunil Chandra (TIFR)
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The IACHEC model for E0102 is the result of years of work by the members of this group.
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: X-ray brightest in the LMC 1.7X2.3 arcmin, 25x33.5 pc t ~ 3,000 yr (Morse et al. 1996) LX(0.3-10.0 kev) = 1.0x1038 ergs s-1
no compact object “O-rich” core-collapse SNR
E0102: X-ray brightest in the SMC 0.77X0.77 arcmin, 13X13 pc t ~ 2,000 yr (Finklestein et al. 2006) LX(0.3-10.0 kev) = 2.5x1037 ergs s-1
no compact object “O-rich” core-collapse SNR
ACIS 0.35-8.0 keV ACIS 0.35-8.0 keV
3
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: X-ray brightest in the LMC 1.7X2.3 arcmin, 25x33.5 pc t ~ 3,000 yr (Morse et al. 1996) LX(0.3-10.0 kev) = 1.0x1038 ergs s-1
no compact object “O-rich” core-collapse SNR
E0102: X-ray brightest in the SMC 0.77X0.77 arcmin, 13X13 pc t ~ 2,000 yr (Finkelstein et al. 2001) LX(0.3-10.0 kev) = 2.5x1037 ergs s-1
no compact object “O-rich” core-collapse SNR
ACIS 0.35-8.0 keVRed (0.3-0.5 keV), Green (0.5-0.75 keV), Blue (0.75 – 7.0 keV)
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CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: X-ray brightest in the LMC 1.7X2.3 arcmin, 25x33.5 pc t ~ 3,000 yr (Morse et al. 1996) LX(0.3-10.0 kev) = 1.0x1038 ergs s-1
no compact object “O-rich” core-collapse SNR
E0102: X-ray brightest in the SMC 0.77X0.77 arcmin, 13X13 pc t ~ 2,000 yr (Finkelstein et al. 2001) LX(0.3-10.0 kev) = 2.5x1037 ergs s-1
no compact object “O-rich” core-collapse SNR
Red (0.3-0.5 keV), Green (0.5-0.75 keV), Blue (0.75 – 7.0 keV)
Red (0.3-0.75 keV), Green (0.8-1.1 keV), Blue (1.1 – 2.0 keV)
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CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 20176
The IACHEC E0102 Paper is Published !Many thanks to Andy B., Adam, Frank, Eric, Andy P. and Steve for their patience
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
10 15 20 25
10!4
10!3
0.01
0.1
Coun
ts s!
1 cm!2
A!1
Wavelength (A)
OV
II F
OV
II R
OV
III
Ne
IX F
Ne
IX R
Ne
X
RGS Spectra of E0102
E0102
7
Pollock (Sheffield)
Strong well-separated lines in the 0.5-1.0 keV
bandpass make this target attractive for
calibration of CCD instruments
Just a reminder why we use
E0102
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 20178
Comparison of E0102 Line Normalizations for MOS, pn, ACIS, XIS and XRT
Norm OVII OVIII NeIX NeXMOS and
pn disagree by 5-15% depending on the line,
this is apparently
larger than the
discrepancy suggested by other analyses.
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Time Dependence of ACIS S3 on axis in subarray mode
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IACHEC value
average of data
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Time Dependence of pn in small window mode
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the pn in small window mode on-axis is remarkably
stable
2005 2010 2015
0.9
0.95
11.
05
Line
Rat
io
Year
EPIC pn Small Window ModeSAS 14.0
Ne XNe IXO VIIIO VII
Haberl (MPE)
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Time Dependence of MOS in large window mode
11
2000 2002 2004 2006 2008 2010 2012 2014
0.90
0.95
1.00
1.05
1.10
ratio
inst
r/IAC
HEC MOS1
2000 2002 2004 2006 2008 2010 2012 2014Year
0.90
0.95
1.00
1.05
1.10
MOS2
Norm OVII OVIII NeIX NeX
Sembay (Leicester)
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Time Dependence of Suzaku XIS
12
Miller (MIT)
Norm OVII OVIII NeIX NeX
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
Time Dependence of Swift XRT in WT Mode
13
Beardmore (Leicester) Norm OVII OVIII NeIX NeX
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201714
- Martin S., Andy P., & Matteo G. worked on an empirical model with Gaussians for the lines similar to what was done for E0102
- 121 Gaussians for the lines identified in RGS data and pn/MOS data - two component absorption, Galactic and LMC - two “no-line” APEC model for the continuum, one with kT=0.175 keV and
the other with 1.14 keV - power-law component for the background - global normalization that modifies the entire model - 403 parameters in the model UGH !!!
N132D IACHEC Model Description
Fitting Methodology- Only 4 free parameters, all others frozen - fit in the 0.3 - 10.0 keV bandpass - Line energies and widths are not allowed to vary - Only the normalization of the Si XIII, S XV, and Ar AVII line are allowed to
vary - the global normalization is allowed to cary - pn spectral fits used the “gainfit” model in XSPEC - detector background is now modeled, not subtracted, Gaetz (SAO) models
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201715
N132D ACTION ITEMS FROM 2017 IACHEC
- Andy P. will modify the line widths of some line and change the normalizations of some of the weak lines, we expect the CCD instruments will be insensitive to these changes
- Adam and Paul will process pn and MOS data with SAS16 and analyze those spectra [Done, results presented today]
- Develop a non-linear gain correction for the pn data and apply the correction to the events and do NOT use “gain fit” in XSPEC
- the WG will explore allowing the continuum normalization and shape to vary - the WG will experiment wit different energy ranges over which to fit
N132D IACHEC Model v2.10 Released before the 2017 IACHEC Meeting Significant changes from v2.9 to v2.10: • use APEC v3.0.8 • use “nlapec” model in XSPEC • remove power-law component that was there as a crude background model
Objectives of Model Development Short term: use model to compare effective areas in the 1.5 - 3.5 keV bandpass Long term: develop a standard model for the community to use
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201716
“Stringent” Data Selection for MOS
“Stringent” Data Selection for pn • only use PrimeSmallWindow mode to minimize pileup • spectral extraction region is completely enclosed by the Small Window area • only use Thin or Medium filter • low background • no cal source included • no obvious problems with fit to the IACHEC model • 14 of 47 data sets conform with selection criteria
• only use PrimePartialW3 mode to minimize pileup • spectral extraction region is completely enclosed by the Window area • only use Thin or Medium filter • low background • no cal source included • “inner” part of the patch area can NOT intersect spectral extraction region • “outer” part of the patch area can NOT exceed 50% of the spectral
extraction region • 17 of 43 data sets conform with selection criteria
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: sample images for data selection
17
included
excluded
excluded
included
inner and outer patch
pn
pn
MOS1
MOS2
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: sample pn fits for one observation. Fits in 4 energy ranges are evaluated
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0.3-10.0 keV
10−3
0.01
0.1
1
10
100
norm
aliz
ed c
ount
s s−1
keV
−1
2000−0523,PrSmWin,Exp=9954.7,Pile=N,Back=6.9e6,Con=0.993,RPchi=0.89,Cstat=2072.9N132D,v2.10,SAS16,pn,0125100201_pnS001,Medium,DETX=70.3,DETY=332.8,DOF=1937.0
1 100.5 2 50.6
0.8
1
1.2
1.4
ratio
Energy (keV)plucinsk 20−Apr−2017 12:43
0
50
100
norm
aliz
ed c
ount
s s−1
keV
−1
2000−0523,PrSmWin,Exp=9954.7,Pile=N,Back=6.9e6,Con=0.993,RPchi=1.48,Cstat=351.1N132D,v2.10,SAS16,pn,0125100201_pnS001,Medium,DETX=70.3,DETY=332.8,DOF=237.0
0.4 0.6 0.8 1 1.2 1.4
−5
0
5
norm
aliz
ed c
ount
s s−1
keV
−1
Energy (keV)plucinsk 20−Apr−2017 12:43
0.1
1
10
norm
aliz
ed c
ount
s s−1
keV
−1
2000−0523,PrSmWin,Exp=9954.7,Pile=N,Back=6.9e6,Con=0.993,RPchi=1.40,Cstat=471.5N132D,v2.10,SAS16,pn,0125100201_pnS001,Medium,DETX=70.3,DETY=332.8,DOF=395.0
1.5 2 2.5 3 3.5
0.5
1
1.5
ratio
Energy (keV)plucinsk 20−Apr−2017 12:43
10−3
0.01
2×10−3
5×10−3
0.02
0.05
norm
aliz
ed c
ount
s s−1
keV
−1
2000−0523,PrSmWin,Exp=9954.7,Pile=N,Back=6.9e6,Con=0.993,RPchi=0.52,Cstat=517.2N132D,v2.10,SAS16,pn,0125100201_pnS001,Medium,DETX=70.3,DETY=332.8,DOF=494.0
5.5 6 6.5 7 7.5 80
0.5
1
1.5
2
2.5
ratio
Energy (keV)plucinsk 20−Apr−2017 12:43
0.3-1.5 keV
1.5-3.0 keV 5.5-8.0 keV
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 14 selected data sets
19
pn 0.3-10.0 keV
10−3
0.01
0.1
1
10
100
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.990,RPchi=1.25,Cstat=36979.3,DOF=27170.0N132D,v2.10,SAS16,pn,simultaneously fit 14 selected data sets
1 100.5 2 50.6
0.8
1
1.2
1.4
ratio
Energy (keV)plucinsk 22−Apr−2017 18:12
instrument background
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 14 selected data sets
20
pn 0.3-1.5 keV
0
50
100
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.990,RPchi=2.23,Cstat=7515.5,DOF=3370.0N132D,v2.10,SAS16,pn,simultaneously fit 14 selected data sets
0.4 0.6 0.8 1 1.2 1.4
−5
0
5
norm
aliz
ed c
ount
s s−1
keV
−1
Energy (keV)plucinsk 22−Apr−2017 18:13
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 14 selected data sets
21
pn 1.5-3.5 keV
0.1
1
10
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.990,RPchi=1.80,Cstat=9308.6,DOF=5582.0N132D,v2.10,SAS16,pn,simultaneously fit 14 selected data sets
1.5 2 2.5 3 3.5
0.5
1
1.5
ratio
Energy (keV)plucinsk 22−Apr−2017 18:13
Si XIII
S XV
Ar XVII
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 14 selected data sets
22
pn 5.5-8.0 keV
10−3
0.01
2×10−3
5×10−3
0.02
0.05
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.990,RPchi=0.81,Cstat=8305.1,DOF=6968.0N132D,v2.10,SAS16,pn,simultaneously fit 14 selected data sets
5.5 6 6.5 7 7.5 80
0.5
1
1.5
2
2.5
ratio
Energy (keV)plucinsk 22−Apr−2017 18:14
Linear gain adjustment is driven by low energy data. This makes the fit worse at the Fe-K line. Need a non-linear gain adjustment instrument background
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201723
Issues with MOS processing and analysis • for latest reprocessing with SAS16 we used: FLAG==0 and pattern==0 in the evselect extendedsource=yes in arfgen • Sembay recommends FLAG==#XMMEA_EM
How to process the data in the future ?? Sembay suggests two approaches with a suitably large extraction region:
1. use extendedsource=no and FLAG==#XMMEA_EM and accept inaccuracy in bad pixel correction
2. use extendedsource=yes and FLAG==#XMMEA_EM and correct results of the encircled energy fraction
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201724
Encircled Energy Fraction for N132D Sembay (Leicester)
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 17 selected data sets
25
MOS1 0.3-10.0 keV
10−3
0.01
0.1
1
10
100
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.990,RPchi=1.25,Cstat=36979.3,DOF=27170.0N132D,v2.10,SAS16,pn,simultaneously fit 14 selected data sets
1 100.5 2 50.6
0.8
1
1.2
1.4
ratio
Energy (keV)plucinsk 22−Apr−2017 18:12
No gain adjustment to the MOS1 data
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 17 selected data sets
26
MOS1 0.3-1.5 keV
0
10
20
30
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.991,RPchi=2.53,Cstat=10453.5,DOF=4059.0N132D,v2.10,SAS16,MOS1,simultaneously fit 14 selected data sets
0.4 0.6 0.8 1 1.2 1.4−2
−1
0
1
2
norm
aliz
ed c
ount
s s−1
keV
−1
Energy (keV)plucinsk 24−Apr−2017 14:47
No gain adjustment to the MOS1 data
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 17 selected data sets
27
MOS1 1.5-3.5 keV
Si XIII
S XV
Ar XVII
0.1
1
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.991,RPchi=1.49,Cstat=8422.8,DOF=6762.0N132D,v2.10,SAS16,MOS1,simultaneously fit 14 selected data sets
1.5 2 2.5 3 3.5
0.6
0.8
1
1.2
1.4
ratio
Energy (keV)plucinsk 24−Apr−2017 14:48
No gain adjustment to the MOS1 data
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D:simultaneous fit to 14 selected data sets
28
MOS1 5.5-8.0 keV
No gain adjustment to the MOS1 data
10−4
10−3
0.01
norm
aliz
ed c
ount
s s−1
keV
−1
PrSmWin,Thin or Med,Con=0.991,RPchi=0.24,Cstat=6707.4,DOF=8462.0N132D,v2.10,SAS16,MOS1,simultaneously fit 14 selected data sets
5.5 6 6.5 7 7.5 80
0.5
1
1.5
2
2.5
ratio
Energy (keV)plucinsk 24−Apr−2017 14:49
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201729
MOS2 Results No MOS2 results from SAS16 processing. The normalizations we are getting for the MOS2 spectra processed with SAS16 with the parameters as we set them are 10-25% different from MOS1.
MOS1 MOS2
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: Comparison of Fitted Norms for S XIII, S XV, & Ar XVII
30
Norm Si XIII S XV Ar XVII
2017
Shown at the IACHEC, based on single observations for pn and MOS1/MOS2
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 2017
N132D: Comparison of Fitted Norms for S XIII, S XV, & Ar XVII
31
Norm Si XIII S XV Ar XVII 2017
Norm Si XIII S XV Ar XVII
Use pn and MOS1 simultaneous fits
CXCChandra X-ray Observatory
Paul Plucinsky EPIC Cal/Ops 201732
N132D Future Work
- Resolve MOS processing issues and create data sets to use for this analysis - Experiment with allowing the continuum shape and normalization to vary - Decide on the bandpass for the fits and which parameters are free