Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 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

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




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




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




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





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





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




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




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%




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




ESACESAC3C273 (1)3C273 (1)

SASv6.1SASv6.1

Rev. 0094Rev. 0094 Medium filterMedium filter All EPICs in SW All EPICs in SW

modesmodes




ESACESAC3C273 (2)3C273 (2)


modesmodes

SASv6.1SASv6.1




ESACESAC3C273 (3)3C273 (3)


modesmodes

SASv6.1SASv6.1




ESACESAC3C273 (4)3C273 (4)


modesmodes

SASv6.1SASv6.1




ESACESAC3C273 (5)3C273 (5)


modesmodes

SASv6.1SASv6.1




ESACESAC3C273 (6)3C273 (6)


modesmodes




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




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




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




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




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




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




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.




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




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




ESACESACH1426+428H1426+428

Rev. 1012Rev. 1012 Medium filter, SWMedium filter, SW Discrepancies Discrepancies

reduced by ~10%reduced by ~10%

SASv6.1SASv6.1




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




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




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




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…

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 1...

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