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Cross-calibration of the EPIC MOS and PN cameras on-board XMM-Newton using sources with continuum spectra
G. Griffiths, U. Briel , M. Dadina, P. Ferrando, F. Haberl , J.-W. den Herder, D. Lumb, S. Molendi , R. Saxton, S. Sembay,

Introduction
· · · ·

Comparison of MOS/pn continuum spectra using several sources in various modes All MOS data processed using SAS 5.2 All pn SW data processed by instrument team (latest CTI correction), other modes processed using SAS 5.2 Response files used (public - m<1/2>_v9q19t5r5_all_15.rsp) MOS: m<1/2>_v9q20t5r6_all_15.rsp pn: epn__sY9_.rsp (ver. 6.1)
New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001

XMM EPIC


·

Piled-up sources :

·

core of PSF excluded same region of PSF used for MOS and pn no encircled energy correction made Spectrum split into hard (> 2 keV) and soft band (< 2 keV)

The Hard X-ray band (> 2 keV)
Sources analysed: PKS 2149-306 Mrk 3 3C273 PKS 2155-304

Model used: power-law to 2-10 and 3-10 keV band (except Mrk 3 ­ Gaussians used for Fe K complex )

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Source PKS 2149-306 Mrk 3 3C273 (a) 3C273 (b) PKS 2155-304

Mode M1 M2 PN FF FF LW FF FF FF

Extraction region (arcsec) 0-31 0-40 5-42 5-42 10-42

SW SW SW SW SW SW -- SW SW

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


PKS 2149-306 MOS1 ­ black, MOS2 ­ red, PN ­ green
2-10 keV 3-10 keV

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Mrk 3

MOS1 ­ black, MOS2 ­ red, PN ­ green
2-10 keV 3-10 keV

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Statistical evaluation of EPIC flux calibration using large sample of sources (R. Saxton WA2-10)

Good agreement between the MOS instruments

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


MOS flux is higher than pn at hard energies effect is to make MOS slope flatter by about 0.05

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


3C273
Observation A

MOS1 ­ black, MOS2 ­ red, PN ­ green
2-10 keV 3-10 keV

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


3C273

MOS1 ­ black, MOS2 ­ red, PN ­ green
3-10 keV

Observation B 2-10 keV

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


PKS 2155-304
2-10 keV

MOS2 ­ red, PN ­ green
3-10 keV

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Soft X-ray band (< 2 keV)
PN SW mode data unreliable below 0.7 keV Sources analysed: Coma A1795 A1835 MS1229.2+6430 MS0737.9+7441 PKS 0558-504

Model used:

single temp. thermal model + absorption power-law model + absorption

Comparison of derived NH with Galactic values (NHGal). Look for systematic differences between MOS and pn

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Source Coma A1795 A1835 MS1229.2+6430 MS0737.9+7441 PKS 0558-504

Mode M1 M2 PN FF FF EFF FF FF FF FF FF FF FF FF FF

Extraction region (arcsec) 0-120 120-180 60-120 0-40 0-30 5-40

FF FF FF FF FF FF

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


MOS ­ red, PN green, ---- N
HGal
N (1020
H

A1795

cm -2)

Coma
N (1020
H

A1835

cm -2)

Low energy cut (keV )

Low energy cut (keV )

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


MOS1 ­ black, MOS2 ­ red, PN green, ---- N
HGal
N (1020
H

MS 0737.9+7441

cm -2)

MS 1229.2+6430
N (1020
H

PKS 0558-504

cm -2)

Low energy cut (keV )

Low energy cut (keV )

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001


Summary
Hard X-ray band
· · ·

Generally good agreement between MOS and PN (5% level) Evidence that MOS flux is few % higher than PN at high energies For bright sources when MOS and PN in SW mode we see differences in spectral slope of ~ 0.1-0.15 in 3-10 keV band CTI correction for PN SW is a factor

Soft X-ray band
Good agreement between MOS and PN for Full Frame observations However :· For low NHGal sources N H is typically lower for MOS than for PN by approx. 1x1020 cm-2 · NH for the BL Lacs is considerably higher than NHGal (fitting low energy curvature of spectrum?)

XMM EPIC

New Visions of the X-ray Universe in the XMM-Newton and Chandra era 26-30 November 2001