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Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 1
XMM-NewtonXMM-Newton
ESACESAC
Status of XMM-NewtonStatus of XMM-Newtoncross-calibration with SASv6.5cross-calibration with SASv6.5
Martin Stuhlinger Martin Stuhlinger with inputs/support from whole cross-calibration teamwith inputs/support from whole cross-calibration team
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 2
XMM-NewtonXMM-Newton
ESACESACCross-calibration teamCross-calibration team
ESACESAC: (Bruno Altieri), Marcus Kirsch, Leo Metcalfe, : (Bruno Altieri), Marcus Kirsch, Leo Metcalfe, Andy Pollock, Richard Saxton, Michael Smith, Martin Andy Pollock, Richard Saxton, Michael Smith, Martin Stuhlinger, Antonio TalaveraStuhlinger, Antonio Talavera
LeicesterLeicester: Steve Sembay, Andy Read, Darren Baskill: Steve Sembay, Andy Read, Darren Baskill MPEMPE: Frank Haberl, Michael Freyberg, Konrad : Frank Haberl, Michael Freyberg, Konrad
DennerlDennerl SRON: SRON: Jelle Kaastra, Jan Willem den Herder, Cor de Jelle Kaastra, Jan Willem den Herder, Cor de
Vries, Jacco VinkVries, Jacco Vink
… … and many others, including Chandra and Swiftand many others, including Chandra and Swift
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 3
XMM-NewtonXMM-Newton
ESACESACTalk outlineTalk outline
Major changes from SASv6.1 to SASv6.5 (EPIC)Major changes from SASv6.1 to SASv6.5 (EPIC) Low-energy improvement: effect of the new pn Low-energy improvement: effect of the new pn
redistribution (CCFs available since May 2005)redistribution (CCFs available since May 2005) Spectral fitting examples on various sourcesSpectral fitting examples on various sources Chandra/XMM-Newton cross-calibrationChandra/XMM-Newton cross-calibration Swift/XMM-Newton cross-calibrationSwift/XMM-Newton cross-calibration
Conclusions and outstanding issuesConclusions and outstanding issues
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 4
XMM-NewtonXMM-Newton
ESACESACChanges in SASv6.5 (1)Changes in SASv6.5 (1)
New MOS rmf generationNew MOS rmf generation
See talk by Andy ReadSee talk by Andy Read
Time dependentTime dependent 9 time epochs9 time epochs
Spatial dependentSpatial dependent 3 spatial regions3 spatial regions
18 new CCFs with SASv6.5 18 new CCFs with SASv6.5 WARNING!!!WARNING!!! Using SASv6.1, rmfgen could create Using SASv6.1, rmfgen could create responses with strange featuresresponses with strange features
A. Read
MOS patchMOS patch
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 5
XMM-NewtonXMM-Newton
ESACESACChanges in SASv6.5 (2)Changes in SASv6.5 (2)
Improvement of arfgenImprovement of arfgen MOS flux correction for more than one missing MOS flux correction for more than one missing
column in sequencecolumn in sequence
MOS SW: FLAG==0MOS SW: FLAG==0 MOS SW: XMMEA_EMMOS SW: XMMEA_EM
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 6
XMM-NewtonXMM-Newton
ESACESACChanges in SASv6.5 (3)Changes in SASv6.5 (3)
Improvement of embadpixfindImprovement of embadpixfind New column rejection algorithm prevents New column rejection algorithm prevents
erronious identification of bad columnserronious identification of bad columns Emproc now using embadpixfind as wellEmproc now using embadpixfind as well
OldOld NewNew
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 7
XMM-NewtonXMM-Newton
ESACESACpn rmf tuningpn rmf tuning
CCFs public since 14 May 2005CCFs public since 14 May 2005
Old CCFsOld CCFs New CCFsNew CCFs
Systematic S-shaped residuals … changed to flat residualsSystematic S-shaped residuals … changed to flat residuals
B. Altieri
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 8
XMM-NewtonXMM-Newton
ESACESACRXJ1856-3754 (1): pn flux stabilityRXJ1856-3754 (1): pn flux stability
Rev. 0427Rev. 0427 Rev. 0878Rev. 0878 Rev. 0968Rev. 0968 SW modeSW mode Thin filterThin filter
Changes byChanges by
less than 1%less than 1%
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 9
XMM-NewtonXMM-Newton
ESACESACRXJ1856-3754 (2)RXJ1856-3754 (2)
SASv6.1SASv6.1
Rev. 0878Rev. 0878 Thin filter, SWThin filter, SW Great improve-Great improve-
ments in ments in consistency with consistency with SASv6.5SASv6.5
SASv6.5SASv6.5
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 10
XMM-NewtonXMM-Newton
ESACESAC3C273 (1)3C273 (1)
SASv6.1SASv6.1
Rev. 0094Rev. 0094 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 11
XMM-NewtonXMM-Newton
ESACESAC3C273 (2)3C273 (2)
Rev. 0277Rev. 0277 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 12
XMM-NewtonXMM-Newton
ESACESAC3C273 (3)3C273 (3)
Rev. 0563Rev. 0563 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 13
XMM-NewtonXMM-Newton
ESACESAC3C273 (4)3C273 (4)
Rev. 0655Rev. 0655 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 14
XMM-NewtonXMM-Newton
ESACESAC3C273 (5)3C273 (5)
Rev. 0835Rev. 0835 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 15
XMM-NewtonXMM-Newton
ESACESAC3C273 (6)3C273 (6)
Rev. 1023Rev. 1023 Medium filterMedium filter All EPICs in SW All EPICs in SW
modesmodes
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 16
XMM-NewtonXMM-Newton
ESACESAC3C273 (7)3C273 (7)
Spectral summary:Spectral summary:
Good agreement between the EPICs at all epochsGood agreement between the EPICs at all epochs
MOS2 bump ~20% at 0.2-0.4 keVMOS2 bump ~20% at 0.2-0.4 keV
pn bump of ~10% at 0.4-0.5 keVpn bump of ~10% at 0.4-0.5 keV
Above ~5 keV pn is lower than MOS by ~10%Above ~5 keV pn is lower than MOS by ~10%
RGS decreased by ~10-20% at lowest energies during the RGS decreased by ~10-20% at lowest energies during the missionmission
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 17
XMM-NewtonXMM-Newton
ESACESAC3C273 (8): Low-energy flux ratios3C273 (8): Low-energy flux ratios
0.4-0.8 keV0.4-0.8 keV MOS to pn ratios MOS to pn ratios
decrease by less decrease by less than 5% than 5%
RGS ratios RGS ratios decrease by 10-decrease by 10-15%15%
Possible different Possible different changes for RGS1 changes for RGS1 and RGS2?and RGS2?
cooling
SASv6.1SASv6.1
S.Sembay
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 18
XMM-NewtonXMM-Newton
ESACESAC1ES0102-7219 (1)1ES0102-7219 (1)
M. Smith
Rev. 0375Rev. 0375 Thin filterThin filter PN SW, MOS LWPN SW, MOS LW
40 lines plus 40 lines plus absorbed absorbed bremsstrahlungbremsstrahlung
Line energies Line energies fixed to laboratory fixed to laboratory valuesvalues
Line widths Line widths determined by determined by RGSRGS
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 19
XMM-NewtonXMM-Newton
ESACESAC1ES0102-7219 (2)1ES0102-7219 (2)
M. Smith
Rev. 0521Rev. 0521 Thin filterThin filter PN SW, MOS LWPN SW, MOS LW pn response pn response
under-estimates under-estimates redistri-bution, redistri-bution, most evident at most evident at O-linesO-lines
Above 0.6 keV the Above 0.6 keV the ageement is goodageement is good
Backgound Backgound subtraction is subtraction is problematic for pn problematic for pn SW modeSW mode
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 20
XMM-NewtonXMM-Newton
ESACESAC1ES0102-7219 (3)1ES0102-7219 (3)
M. Smith
Rev. 0521Rev. 0521 Thin filterThin filter All EPICs in LW All EPICs in LW
modesmodes
pn LW mode pn LW mode agrees better agrees better than pn SW mode than pn SW mode because because background sub-background sub-traction for pn is traction for pn is less problematicless problematic
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 21
XMM-NewtonXMM-Newton
ESACESAC1ES0102-7219 (4)1ES0102-7219 (4)
M. Smith
Rev. 0888Rev. 0888 Thick filterThick filter PN SW, MOS LWPN SW, MOS LW
Large pn-MOS Large pn-MOS discrepancies discrepancies below 0.5 keVbelow 0.5 keV
Perhaps a filter Perhaps a filter issue (C-edge?) issue (C-edge?) rather then rather then redistributionredistribution
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 22
XMM-NewtonXMM-Newton
ESACESAC1ES0102-7219 (5)1ES0102-7219 (5)
M. Smith
Rev. 0981Rev. 0981 Thin filterThin filter PN SW, MOS LWPN SW, MOS LW
Below 0.5 keV Below 0.5 keV RGS flux has RGS flux has decreaseddecreased
Hence the Hence the combined fits are combined fits are unreliable at low unreliable at low energies.energies.
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 23
XMM-NewtonXMM-Newton
ESACESACPKS0558-504PKS0558-504
M. Kirsch
Rev. 0153Rev. 0153 Thin filterThin filter PN SW, MOS LWPN SW, MOS LW Early epoch, before Early epoch, before
MOS “patch” MOS “patch” Excellent Excellent
agreement agreement between all EPIC between all EPIC instrumentsinstruments
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 24
XMM-NewtonXMM-Newton
ESACESACPKS2155-304PKS2155-304
M. Kirsch
Rev. 0545, med., Rev. 0545, med., SWSW
MOS “patch” MOS “patch” presentpresent
Good agreement at Good agreement at lowest and medium lowest and medium energiesenergies
MOSes lower by MOSes lower by ~15% between ~15% between 0.4-0.8 keV0.4-0.8 keV
pn lower above 5 pn lower above 5 keV keV SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 25
XMM-NewtonXMM-Newton
ESACESACH1426+428H1426+428
Rev. 1012Rev. 1012 Medium filter, SWMedium filter, SW Discrepancies Discrepancies
reduced by ~10%reduced by ~10%
SASv6.1SASv6.1
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 26
XMM-NewtonXMM-Newton
ESACESACXMM-Newton versus Chandra LETGXMM-Newton versus Chandra LETG
M. Smith
PKS2155-304PKS2155-304 XMM rev. 0362XMM rev. 0362
Good Good agreement agreement above 1 keVabove 1 keV
ACIS/LETG has ACIS/LETG has higher higher normalisation normalisation than the EPICs than the EPICs below 1 keVbelow 1 keV
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 27
XMM-NewtonXMM-Newton
ESACESACXMM-Newton versus Chandra HETGXMM-Newton versus Chandra HETG
M. Smith
H1426+428H1426+428 XMM rev. 1015XMM rev. 1015
Very good Very good agreement below 2 agreement below 2 keVkeV
Above 2 keV, ACIS/ Above 2 keV, ACIS/ HEG shows a HEG shows a flatter slope than flatter slope than the EPICs the EPICs
Above 2 keV, MOS Above 2 keV, MOS is closer to ACIS/ is closer to ACIS/ MEG than pnMEG than pn
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 28
XMM-NewtonXMM-Newton
ESACESACXMM-Newton versus Swift XRTXMM-Newton versus Swift XRT
H1426+428H1426+428 XMM rev. 1012XMM rev. 1012
Good agreement Good agreement between ~0.6 keV between ~0.6 keV and ~3.0 keV and ~3.0 keV
XRT measures XRT measures steeper slope at steeper slope at high energies than high energies than the EPICsthe EPICs
Large Large discrepancies discrepancies below ~0.6 keV below ~0.6 keV
Martin Stuhlinger Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 X-Ray Universe 2005, Sep.26-30, 2005
European Space Astronomy Centre
Page 29
XMM-NewtonXMM-Newton
ESACESACConclusionsConclusions
• EPIC low-energy issue about to be solved :EPIC low-energy issue about to be solved :• CCF for EPIC-pn available since 2005 MayCCF for EPIC-pn available since 2005 May• Mechanisms for time- and spatial-dependent MOS Mechanisms for time- and spatial-dependent MOS
redistribution are in SASv6.5, corresponding new EPIC-MOS redistribution are in SASv6.5, corresponding new EPIC-MOS CCFs publishedCCFs published
• RGS :RGS :• Low-energy flux difference ~10% at launchLow-energy flux difference ~10% at launch• Sensitivity at the longest wavelengths has decreased by Sensitivity at the longest wavelengths has decreased by
~10-20% over the mission~10-20% over the mission• Status in SASv6.5: EPIC and RGS are not yet consistent below Status in SASv6.5: EPIC and RGS are not yet consistent below
~0.7 keV ~0.7 keV• Open cross-calibration issues :Open cross-calibration issues :
• Implement best knowledge of RGS into SAS (see previous talk)Implement best knowledge of RGS into SAS (see previous talk)• Which of MOS or pn is right at high energies?Which of MOS or pn is right at high energies?• EPIC rmf’s at low energies: still room for improvementEPIC rmf’s at low energies: still room for improvement
We keep on cross-calibrating happily…We keep on cross-calibrating happily…
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