xmm-newton monitoring of 3c 273
DESCRIPTION
XMM-Newton Monitoring of 3C 273. OrbitExposure (s) 09463,000 09527,000 095 30,000 09658,000 27743,000 370 5,000 373 4,900 472 4,900 554 4,500 563 8,500 655 58,000 735 8,500 - PowerPoint PPT PresentationTRANSCRIPT
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
XMM-Newton Monitoring of 3C 273
Orbit Exposure (s)094 63,000
095 27,000
095 30,000
096 58,000
277 43,000
370 5,000
373 4,900
472 4,900
554 4,500
563 8,500
655 58,000
735 8,500
835 20,000
835 18,000
Page, K, Turner, M.J.L., Done, C., O’Brien, P.T.,
Reeves, J.N., Sembay, S., Stuhlinger, M., 2004,
MNRAS, 349, 57
Forthcoming Cross-Cal observations:
~July 2005 XMM/Swift/Integral
~Dec 2005 XMM/Astro-E
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Major changes to low energy calibration for EPIC cameras planned.
(See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting)
MOS: For the next SAS release rmfgen will be modified to generate
rmfs for the MOS detectors which are epoch AND spatially dependant.
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Relative fluxes from sample of AGN (EPIC: 15-40 arcsec extraction radius)
Major changes to low energy calibration for EPIC cameras planned.
(See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting)
MOS: For the next SAS release rmfgen will be modified to generate
rmfs for the MOS detectors which are epoch AND spatially dependant.
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Zeta Puppis:
Early O-type Supergiant
Distance 429 pc, mv=2.25
Major changes to low energy calibration for EPIC cameras planned.
(See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting)
MOS: For the next SAS release rmfgen will be modified to generate
rmfs for the MOS detectors which are epoch AND spatially dependant.
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Major changes to low energy calibration for EPIC cameras planned.
(See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting)
PN: Shows no significant evolution of the rmf or arf with time but a
change in the absolute rmf is being implemented to improve low energy calibration.
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Cross-calibration with (test) MOS rmf and SAS6.1.0 PN rmf:
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Courvoisier et al. 2003 A&A 411, L343
January 2003
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Courvoisier et al. 2003 A&A 411, L343
January 2003
After Renormalisation
to PN Data consistent
with…
Γ ~ 1.74 above 3 keV
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Marshall et al. 2001, ApJ, 549, L167
Merlin HST Chandra
13” from core
20” from core
The observed JET in 3C 273
LX (jet) ~ 3x1043 ergs s-1
c.f.
LX (core) > 1046 ergs s-1
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Description: kTB ~100 eV and kTBB~ 250 eV
Page et al. 2004 MNRAS, 349, 57
Fe EW ~ 0-50 eV
Ginga/ASCA/SAX/XMM
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Grandi, P. and Palumbo, G.G.C., 2004, Science, 306, 998
Analysed 6(9) BeppoSAX observations between 1997 and 2001
“Untangling the Jet and Accretion-Disk Emission”
BeppoSAX 1997 BeppoSAX 2001
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
FSEY = 1.74 + (FBB x 1.64) FJET ~ 1.5 x FSEY
Spectral Fit with wabs * (zbb + pexrav + zpo) model
Γ = 1.8
i = 18o
RC = 0.8
“Seyfert” “Jet”
“Seyfert”
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Predicted “Seyfert” and “Jet” high energy fluxes: EPIC
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Predicted “Seyfert” and “Jet” high energy fluxes: EPIC + SAX
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Predicted “Seyfert” and “Jet” high energy fluxes: EPIC
MCG -6-30-15
Vaughan and Edelson, 2001,
ApJ, 548, 694
ΓSEY Softer ?
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
PN < 22 eV
MOS < 43 eV
PN = 36±19 eV
MOS = 57±23 eV
PN < 32 eV
MOS < 65 eV
Measuring the Iron Line emission
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Power law fit:
χ2 = 1579/1397 dof
With Broad Line:
χ2 = 1510/1394 dof
EFE=6.44±0.11 keV
σ = 0.42±0.09 keV
EQW=36.4±19 eV
F=3.8(1.6)x10-5 phts/cm2/s
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
EFE=6.44 keV (fixed)
σ = 0.42 keV (fixed)
EQW=57±23 eV
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Power law fit:
χ2 = 1036/1060 dof
EFE=6.44 keV
σ = 0.42 keV
EQW < 22 eV
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
EFE=6.44±0.11 keV
σ = 0.42±0.09 keV
EQW=36.4±19 eV
F=3.8x10-5 phts/cm2/s
XMMEPICMOS
Steve Sembay ([email protected])Ringberg 10/04/05
Summary
Major advances in the EPIC low energy cross-calibration soon to be implemented
suggest a more robust determination of the spectral shape/model of the soft
excess in 3C 273 can be made.
The EPIC view of the hard X-ray data suggest that the nonthermal component
is dominant over the “accretion” component, probably more so than suggested by
the recent published analysis of BeppoSAX results.