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Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 1
XMM-NewtonXMM-Newton
ESACESAC
Status of XMM-NewtonStatus of XMM-Newtoncross-calibration with SAS-6.1cross-calibration with SAS-6.1
B.AltieriB.Altieriwith inputs/support from whole cross-calibration team with inputs/support from whole cross-calibration team
(XMM SOC, Leicester, MPE(XMM SOC, Leicester, MPE))
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 2
XMM-NewtonXMM-Newton
ESACESACTalk outlineTalk outline
• Response stability at low energies : Response stability at low energies : • SNR (extended)SNR (extended)• AGN view (trend analysis)AGN view (trend analysis)
• Low-energy problem: effect of the new pn Low-energy problem: effect of the new pn redistribution in SAS-6.1redistribution in SAS-6.1
• Spectral fitting examples on various type of Spectral fitting examples on various type of sourcessources
• Chandra/Newton cross-calibrationChandra/Newton cross-calibration• Other cross-calibration problems:Other cross-calibration problems:
MOS low-energy overestimated redistributionMOS low-energy overestimated redistribution EPIC high-energy discrepancyEPIC high-energy discrepancy Fudging RGS low-energy (<0.5 keV) effective area Fudging RGS low-energy (<0.5 keV) effective area
proposal proposal • ConclusionsConclusions
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 3
XMM-NewtonXMM-Newton
ESACESACEPIC-pn flux stability: N132DEPIC-pn flux stability: N132D
EPIC-pn is stable
M.P. Esquej
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 4
XMM-NewtonXMM-Newton
ESACESACEPIC-pn Flux stability: RXJ1856EPIC-pn Flux stability: RXJ1856
F. Haberl
• Confirmed by the Isolated Neutron star:
EPIC-pn is extremely stable
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 5
XMM-NewtonXMM-Newton
ESACESACMOS flux stability: N132DMOS flux stability: N132D
Rev771: • flux decrease in 0.5-1 keV• Redistributed below 0.4 keV
Rev 828 :• Less clear, especially MOS2, while at the same distance relative to low-E on-axis patch.
Some changes at low energies (0.5-1keV) at ~5% level.
• spatial dependent• time dependent
Rev 771Rev 771 Rev 828Rev 828
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 6
XMM-NewtonXMM-Newton
ESACESACMOS flux stability: N132D (2)MOS flux stability: N132D (2)
Why MOS’s see more flux Why MOS’s see more flux deficit in 0.5-1 keV band in deficit in 0.5-1 keV band in rev.771 than rev.828 ? rev.771 than rev.828 ?
While it is relatively at the While it is relatively at the same distance from the on-same distance from the on-axis patch.axis patch.
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 7
XMM-NewtonXMM-Newton
ESACESACEPIC flux stability: N132DEPIC flux stability: N132D
N132D 0.4-0.8 keV band:
• EPIC-pn: pn flux is stable pn-LW lower fluxes than pn-SW due to pile-up
• MOSs : MOS1 lower than MOS2 by 5% Both MOSs have decreased by 6% since launch
MOS2 lower than pn by 10% at launch up to 15% by rev.~800 MOS1 lower than pn by 15% at launch up to 20% by rev.~800 But MOS/pn normalisation TBD because of possible small pile-up for MOSs.
M.P. Esquej
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 8
XMM-NewtonXMM-Newton
ESACESACMOS flux stability: 1ES0102MOS flux stability: 1ES0102
1ES0102 0.4-0.8 keV band:
• MOS cameras seems stable in flux since launch but ..
for off-axis positions• also consistent with a 5% decrease.
• 10% lower flux observed on-axis where a spatially dependent degraded redistribution has developed (‘patch’)
A.M.R. Read
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 9
XMM-NewtonXMM-Newton
ESACESACMOS on-axis low-E patch (1)MOS on-axis low-E patch (1)
A.M.R. Read
When the SNR is centered close to on-axis position one observes :
• a deficit in 0.35-0.7 keV• an excess below 0.3 keV
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 10
XMM-NewtonXMM-Newton
ESACESACMOS on-axis low-E patch (2)MOS on-axis low-E patch (2)
MOS low-E patch elongated along the MOS low-E patch elongated along the line joining the 2 bore-sights.line joining the 2 bore-sights.
A.M.R. Read
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 11
XMM-NewtonXMM-Newton
ESACESACEPIC Low-energy flux stability :EPIC Low-energy flux stability :The SNR storyThe SNR story
EPIC-pn stable below 2 keV and particularly in the 0.4-0.8 keV band
MOSs were possibly ~10% below EPIC-pn at launch in 0.4-0.8 keV with MOS1 5% lower than MOS2
MOSs seem to have lost 5%+ since launch, in the 0.4-1 keV band
possibly redistributed to lower energies (< 0.4 keV) where a low-energy patch is observed on-axis.
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 12
XMM-NewtonXMM-Newton
ESACESAC
Sample of AGNs mostly in SW/Medium analysed in 15-40 arcsec annulus used, hence excluding the “MOS patch.”
Low-energy problem :
• Either MOSs & RGSs loose flux relative to pn at the same rate : 8% in 800 revs (I) because of :
• MOS on-axis redistribution ?• RGS ??• contamination of MOSs and RGSs, cooler CCDs than pn.
• or pn is gaining flux at the same rate (II) : • filters degradation discarded from SNRs• redistribution ?
Flux stability: The AGN viewFlux stability: The AGN view
S. Sembay
(I)
(II)
cooling
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 13
XMM-NewtonXMM-Newton
ESACESACRGS flux stability: 1ES0102RGS flux stability: 1ES0102
red: 0.33-0.7 keV, green: 0.7-0.972 keV, blue: 0.972-1.74 keV
A.Pollock
M. Smith
• At other energies > 0.7 keV, it seems stable contamination ?contamination ?
• RGS flux in 0.4-0.8 keV band consistent with a 5-8% decrease but :
• very little flux below 0.55 keV• background subtraction not easy for extended source, ~20% of the flux• not confirmed by Zeta Puppis Nitrogen line flux monitoring (preliminary result, full analysis underway, by A. Pollock)
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 14
XMM-NewtonXMM-Newton
ESACESAC
Somewhat contradictory results :Somewhat contradictory results :– EPIC-pn seems stableEPIC-pn seems stable– MOS response is changingMOS response is changing
– loosing flux in 0.4-1 keV- redistributed below 0.4 keV– In the on-axis area (‘patch’) only ?
– RGS constant ? Study of RGS stability crucialRGS constant ? Study of RGS stability crucial
MOS: Contamination or redistibution only ?MOS: Contamination or redistibution only ? Exact amount of variations ?Exact amount of variations ? Why RGS and MOS relative calibration is Why RGS and MOS relative calibration is
unchanged ?unchanged ?– RGS and MOS CCDs are coolerRGS and MOS CCDs are cooler– mirror contamintion ?mirror contamintion ?
Interim cross-cal. resultsInterim cross-cal. results
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 15
XMM-NewtonXMM-Newton
ESACESACSAS-6.1 : effect of new pn RMF (1)SAS-6.1 : effect of new pn RMF (1)
H1426+428, rev278, single MOS/OM power-law model
SAS 6.0 SAS 6.1
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 16
XMM-NewtonXMM-Newton
ESACESACH1426: new pn rmf residualsH1426: new pn rmf residuals
Strange residuals shape below 0.6 keV but could be due to a CTI/gain problem at low energies hence residuals around the O-edge.
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 17
XMM-NewtonXMM-Newton
ESACESACSAS-6.1 : effect of new SAS-6.1 : effect of new pnpn RMF (2) RMF (2)
SAS-6.0
PKS 2155-504, rev 545
SAS-6.1
• Same 0.5 keV non-physical dip of pn residuals • combined fit is possibly the “truth” ?
M.Kirsch M.Kirsch
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 18
XMM-NewtonXMM-Newton
ESACESACSAS-6.1 : effect of new pn RMF (3)SAS-6.1 : effect of new pn RMF (3)
• Another case of Another case of “0.5 keV dip” on a “0.5 keV dip” on a continuum spectrum continuum spectrum
• black : MOS1black : MOS1• Red: pn SAS-6.0Red: pn SAS-6.0• Green: pn SAS-6.1Green: pn SAS-6.1
R. Saxton
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 19
XMM-NewtonXMM-Newton
ESACESACH1426 second revisitH1426 second revisit
Although the increasing Although the increasing pn/MOS discrepancy could pn/MOS discrepancy could be attributed to MOS …be attributed to MOS …
MOS seem to have the MOS seem to have the right spectral slope at low right spectral slope at low energies even in late revsenergies even in late revs
Assuming a single power-Assuming a single power-law from UV to soft X-raylaw from UV to soft X-ray
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 20
XMM-NewtonXMM-Newton
ESACESAC
R. Saxton
Early mission : no excess ?Early mission : no excess ?
• MS0737.9+7441 MS0737.9+7441 (BL Lac)(BL Lac)• rev.63rev.63 (Cal/PV) (Cal/PV)
• Best fit MOSs Best fit MOSs model: wabs *powermodel: wabs *power
• very nice very nice agreement overallagreement overall
• No excess of pn wrt No excess of pn wrt to MOS at low to MOS at low energies energies (pn/MOS=0.95 ! )(pn/MOS=0.95 ! )
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 21
XMM-NewtonXMM-Newton
ESACESACVery soft sourcesVery soft sources
RXJ 1856
• pn exhibits a strong excess attributed to pile-up from photons below detection threshold.• MOS agree well with Chandra (nH, kT)
• EPIC-pn cannot be EPIC-pn cannot be used on very soft used on very soft sourcessources
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 22
XMM-NewtonXMM-Newton
ESACESACExtremely soft sourcesExtremely soft sources
GD153, White Dwarf, kT=25eV, maximum below detection threshold
• OM-MOSs can be fitted with a WD SED model• EPIC-pn displays an excess by a factor 2 in the range 0.2-0.3 keV.
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 23
XMM-NewtonXMM-Newton
ESACESACBright (extended) galaxy clusterBright (extended) galaxy cluster
• Good combined fit overall
• 0.5-1 keV : ~ 10% pn excess (or MOS deficit)
• above 3keV : >10% MOS excess
• pn residuals at Fe-K (CTI or gain)
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 24
XMM-NewtonXMM-Newton
ESACESACHot Compact high-z clusterHot Compact high-z cluster
• Rather good combined fit (but lower statistics)
• 0.5-1 keV : about 15% pn excess(or MOS deficit)
MOS1: kT=15 keVMOS2: kT=12 keVpn : kT=10 keV
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 25
XMM-NewtonXMM-Newton
ESACESACMOS vs EPIC-pnMOS vs EPIC-pn
Why MOSs -the apparently varing Why MOSs -the apparently varing instrument- is making good or better fits instrument- is making good or better fits than EPIC-pn -the constant instrument - on than EPIC-pn -the constant instrument - on various types of objects/spectras at any various types of objects/spectras at any epoch ?epoch ?
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 26
XMM-NewtonXMM-Newton
ESACESACNewton/Chandra cross-cal.: PKS2155Newton/Chandra cross-cal.: PKS2155
Rev 362 Rev 545
• LETG agrees very well with MOSs• pn low-energy excess higher in rev.545
Model: wabs*bknpowerBest fit: MOSs
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 27
XMM-NewtonXMM-Newton
ESACESACNewton/Chandra cross-cal.: 3C273 (1)Newton/Chandra cross-cal.: 3C273 (1)
Rev.277
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 28
XMM-NewtonXMM-Newton
ESACESAC
Rev.655
EPIC-pn excess also higher with time
MOS/LETG agreement excellent.
Newton/Chandra cross-cal.: 3C273 (2)Newton/Chandra cross-cal.: 3C273 (2)
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 29
XMM-NewtonXMM-Newton
ESACESACNewton/Chandra cross-cal.Newton/Chandra cross-cal.
MOSs agree very well with Chandra (LETG, MOSs agree very well with Chandra (LETG, HETG & HRC)HETG & HRC)
RGSs too low in 0.3-0.5 keVRGSs too low in 0.3-0.5 keV
EPIC-pn too high at E < 1 keV wrt too all EPIC-pn too high at E < 1 keV wrt too all other instruments.other instruments.
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 30
XMM-NewtonXMM-Newton
ESACESACZeta Puppis wide cross-correlationZeta Puppis wide cross-correlation
Assuming zeta Assuming zeta Puppis is a stable Puppis is a stable source…source…
All measurement All measurement agree except pn agree except pn SAS-6.0SAS-6.0
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 31
XMM-NewtonXMM-Newton
ESACESACRGS low-E effective areaRGS low-E effective area
• Effective area correction of up to 20% below 0.5 keV suggested by a statistical analysis of BL Lacs (Pollock)
• It is unavoidable to be fudged.
•The exact function will be based on upcoming Crab observation (special set-up)
• This will bring MOSs and RGSs in very good agreement on the whole RGS energy range
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 32
XMM-NewtonXMM-Newton
ESACESACMOS low-E redistributionMOS low-E redistribution
Still too much redistribution at low energies ?
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 33
XMM-NewtonXMM-Newton
ESACESACEPIC high-E discrepancyEPIC high-E discrepancy
•MOSs return higher fluxes than pn above 3 keV
• F5-10 keV (MOS) higher than F5-10 keV(pn) by 10-15%
• MOS1 > MOS2 > pn
MOS (MOS1) finds always
•Harder spectra (AGNs)•Hotter temperature (galaxy clusters)
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 34
XMM-NewtonXMM-Newton
ESACESACLow-energy statusLow-energy status
A MOS/RGS deficit wrt EPIC-pn is developing with time at low A MOS/RGS deficit wrt EPIC-pn is developing with time at low energies (<1keV) increasing by up to 10% apparently due to energies (<1keV) increasing by up to 10% apparently due to a loss of flux from MOS/RGSa loss of flux from MOS/RGS Was there a deficit a launch ?Was there a deficit a launch ? Did the trend accelerate after cooling ?Did the trend accelerate after cooling ? Is it due to the MOS on-axis degraded response Is it due to the MOS on-axis degraded response
(“patch”)?(“patch”)? If due to contamination why at same rate for MOSs & If due to contamination why at same rate for MOSs &
RGSs ?RGSs ?
Why Chandra agree better with MOSs at any epoch ?Why Chandra agree better with MOSs at any epoch ?
On very soft sources pn shows a strong excessesOn very soft sources pn shows a strong excesses EPIC pn cannot be used for very soft sourcesEPIC pn cannot be used for very soft sources To what extent bright & soft (To what extent bright & soft ( >1.7) AGNs are affected ? >1.7) AGNs are affected ?
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 35
XMM-NewtonXMM-Newton
ESACESACXMM-Newton cross-cal. : To doXMM-Newton cross-cal. : To do
Document current status with SAS-6.1Document current status with SAS-6.1 Extend the statistical analysis on AGNsExtend the statistical analysis on AGNs
– Investigate possible flux/mode and spatial Investigate possible flux/mode and spatial dependence and spatial of MOS/pn relative dependence and spatial of MOS/pn relative calibration.calibration.
– EPIC-pn redistribution EPIC-pn redistribution NRCOs:NRCOs:
– Hz43 : comparison with early rev.89 obs. (June 2005)Hz43 : comparison with early rev.89 obs. (June 2005)– H1426+428 simultaneously with FUSE (June 2005 )H1426+428 simultaneously with FUSE (June 2005 )
Fudge RGS effective area below 0.55 keVFudge RGS effective area below 0.55 keV Need for a change of boresight for MOSs ?Need for a change of boresight for MOSs ?
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 36
XMM-NewtonXMM-Newton
ESACESAC
The End
Bruno Altieri Bruno Altieri EPIC Calibration meeting, Feb. 1-3, 2005 EPIC Calibration meeting, Feb. 1-3, 2005
European Space Astronomy Centre
Page 37
XMM-NewtonXMM-Newton
ESACESACH1426+428, rev852, pn fitH1426+428, rev852, pn fit