The X-ray source population The X-ray source population studies in nearby galaxies studies in nearby galaxies
Wolfgang PietschMax Planck Institut für extraterrestrische Physik
OutlineOutline
• Introduction to X-ray source population in galaxy fields
• X-ray source population of M 33 field• X-ray source population of the Andromeda
galaxy M 31 field• Advancements with Simbol-X observations
Introduction: X-ray sources in nearby Introduction: X-ray sources in nearby galaxy fieldsgalaxy fields
– Sources within galaxy (all approximately at same distance)• X-ray binaries (XRBs)
– Low mass XRBs (?dips with orbital period, bursts, ...) – High mass XRBs (?eclipses with orb. period, pulsations, optical id,...)– Bright transients
• Supersoft X-ray sources– Classical SSS as known from Magellanic Clouds– Optical novae (dominant class of SSS in M 31)
• Supernova remnants– Thermal remnants– Plerions (PWN)
• Nuclear source • Ultraluminous X-ray sources• Diffuse emission in disk and halo
– Foreground stars– Galaxies, galaxy clusters and AGN in background
XMM-Newton EPIC view of the diffuse emission of XMM-Newton EPIC view of the diffuse emission of the starburst galaxy NGC 253the starburst galaxy NGC 253
Bauer et al. 2007
Simbol-X:
• ULX sources• undetected AGN???• Hard X-ray halo???
408 X–ray sources
X-ray properties
Correlation with catalogues from other wavelength
Optical identification
Identify foreground and background sources
Characterization of X-ray source population of M 33
XMM-Newton survey of the Local GroupXMM-Newton survey of the Local Group galaxy M 33 galaxy M 33 W. Pietsch, Z. Misanovic, F. Haberl,
D. Hatzidimitriou, M. Ehle, G. Trinchieri 2004, A&A 426, 11
Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV
B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV
fg-starAGN
SSSSNRXRB
Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV
B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV
fg-starAGN
SSSSNRXRB
Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV
B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV
fg-starAGN
SSSSNRXRB
X-ray sources in M 33 field: X-ray sources in M 33 field: identification and classificationidentification and classification
identified classified• foreground stars 5 30• AGN 12• Galaxies 1 1
• SSS 5• SNR 21 (+2) 23 (-2)
(Ghavamian et al. 2005, AJ 130, 539)• XRB 2• Hard 267
Using X-ray hardness ratio criteria, optical correlation with USNO-B1, catalogues at different wavelengths, SIMBAD, NED
M 33 zoom in
M33 X-7
[PMH2004] 47
Einstein + ROSAT observations: 3.45 d period 0.31 s pulsation?
Peres et al. 1989, ApJ 336, 140; Dubus et al. 1999, MNRAS 302, 731
Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7
On state Eclipse On state
XMM-Newton EPIC Chandra ACIS I
0.5-4.5 keV images
Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004, A&A 413,
879
Optical identification
Star with V 18.9 mag with 3.45 d variability
DIRECT image by B. Mochejska
Green circle: ROSAT error box Haberl & Pietsch 2001
Yellow circle: Chandra error box
Insert HST image 10“ x 10“
Pietsch et al. 2006, ApJ 646, 420
Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004
XMM-Newton EPIC + Chandra ACIS-I
Optical V and B-V light curve
re-analysis of DIRECT data by
B. Mochejskafolded modulo 3.45d period Dubus et al. 1999
Improved binary ephemeris
Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004, A&A 413, 879
Best fitting spectral models:Absorbed bremsstrahlung or disk blackbody
Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7
First eclipsing black hole (high mass) X-ray binary ?
ChASeM33 lightcurve of X-7ChASeM33 lightcurve of X-7 Pietsch et al. 2006, ApJ 646, 420
Gemini North radial velocity curve: > 6.9 Msun black holeOrosz et al. 2007, ATel 977
ChASeM33 light curve of ChASeM33 light curve of [PMH2004] 47[PMH2004] 47
Pietsch et al. 2006, ATel 905
2nd eclipsingHMXB in M33
Orbital period1.73245 d
Similar to LMC X-4 orHer X-1
The Andromeda The Andromeda Galaxy M 31Galaxy M 31W. Pietsch, M. Freyberg, F. Haberl et.al. 2004, A&A 434, 483
• Similar analysis to M 33 based on archival data
• 856 sources in fields
• Hardness ratio and time variability
• classification and identification
M 31 centreM 31 centreAll EPIC mosaic (~100 ks) • SNRs, SSSs• foreground stars• diffuse emission• Many LMXBs • Galaxtic center sources not fully resolved
Movie of centre area by blinking four observationswith separation of half a year plus one 2.5 year later
H. Stiele, W. Pietsch et al. 2007, in preparation
• Determine time variability between M 31 center pointings half a year apart
• Check classification of SNRs
• Classify new XRB candidate by time variability
Time variability of X-ray sources in the Time variability of X-ray sources in the M 31 centre fieldM 31 centre field
1035 1036 1037 1038 erg/s
Variable X-ray sources in the M 31 centre
W. Pietsch & F. Haberl 2005, A&A 430, L45
• search for X-ray bursts in GC candidates from catalogue paper
• 37 sources in fields
• most GC sources in center field that got longest exposure
• two burst sources detected in X-ray faint GCs, neutron star LMXBs
XMM-Newton detection of type I XMM-Newton detection of type I X-ray bursts in M 31X-ray bursts in M 31
X-ray burster [PFH2005] 253 X-ray burster [PFH2005] 253 in the GC [WSB85] S5 15in the GC [WSB85] S5 15
Observation c4 Jan 7, 2002
X-ray burster [PFH2005] 253 X-ray burster [PFH2005] 253 in the GC [WSB85] S5 15in the GC [WSB85] S5 15
Rise time < 10 s Total 50 ctsMaximum duration < 20 s Max. rate 1.4±0.4ct/s Decay to backgr. ~150 s corresponds to 3.8 1038erg/sQuiescent luminosity ~5 1036erg/s (Eddington limit for H-poor matter)
Simbol-X contributions:Simbol-X contributions: X-ray sources in nearby galaxy fieldsX-ray sources in nearby galaxy fields
– Sources within galaxy (all approximately at same distance)• X-ray binaries (XRBs) <hard>
– Low mass XRBs (?dips with orbital period, bursts, ...) – High mass XRBs (?eclipses with orb. period, pulsations, optical id,...)– Bright transients
• Supersoft X-ray sources– Classical SSS as known from Magellanic Clouds– Optical novae
• Supernova remnants– Thermal remnants– Plerions (PWN) <hard>
• Nuclear source • Ultraluminous X-ray sources• Diffuse emission in disk and halo
– Foreground stars– Galaxies, galaxy clusters and AGN in background <hard>
Simbol-X contributions:Simbol-X contributions: X-ray sources in nearby galaxy fieldsX-ray sources in nearby galaxy fields
– Sources within galaxy (all approximately at same distance)• X-ray binaries (XRBs) <hard>
– Low mass XRBs (?dips with orbital period, bursts, ...) – High mass XRBs (?eclipses with orb. period, pulsations, optical id,...)– Bright transients
• Supersoft X-ray sources– Classical SSS as known from Magellanic Clouds– Optical novae
• Supernova remnants– Thermal remnants– Plerions (PWN) <hard>
• Nuclear source • Ultraluminous X-ray sources• Diffuse emission in disk and halo
– Foreground stars– Galaxies, galaxy clusters and AGN in background <hard>
Important Simbol-X parameters for nearby galaxy investigations:
Big field of view high resolution
Unexplored energy band!!! Discovery space for the unpredicted !!!
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