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The X-ray source population studies in nearby galaxies

The X-ray source population studies in nearby galaxies. Wolfgang Pietsch Max Planck Institut für extraterrestrische Physik. Outline. 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

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The X-ray source population studies in nearby galaxies

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  1. The X-ray source population studies in nearby galaxies Wolfgang Pietsch Max Planck Institut für extraterrestrische Physik

  2. Outline • 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

  3. Introduction: X-ray sources in nearby galaxy 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

  4. XMM-Newton EPIC view of the diffuse emission of the starburst galaxy NGC 253 Bauer et al. 2007 • Simbol-X: • ULX sources • undetected AGN??? • Hard X-ray halo???

  5. XMM-Newton survey of the Local Group galaxy M 33 W. Pietsch, Z. Misanovic, F. Haberl, D. Hatzidimitriou, M. Ehle, G. Trinchieri 2004, A&A 426, 11 408 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

  6. Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keVB2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV fg-star AGN SSS SNR XRB

  7. Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keVB2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV fg-star AGN SSS SNR XRB

  8. Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keVB2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV fg-star AGN SSS SNR XRB

  9. X-ray sources in M 33 field: identification and classification Using X-ray hardness ratio criteria, optical correlation with USNO-B1, catalogues at different wavelengths, SIMBAD, NED 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

  10. M 33 zoom in M33 X-7 [PMH2004] 47

  11. Eclipsing X-ray binary M33 X-7 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

  12. Eclipsing X-ray binary M33 X-7 Pietsch et al. 2004, A&A 413, 879 On state Eclipse On state XMM-Newton EPIC Chandra ACIS I 0.5-4.5 keV images

  13. Eclipsing X-ray binary M33 X-7 Pietsch et al. 2004 Optical identification Star with V 18.9 mag with 3.45 d variability DIRECT image by B. Mochejska Green circle: ROSAT error boxHaberl & Pietsch 2001 Yellow circle: Chandra error box Insert HST image 10“ x 10“ Pietsch et al. 2006, ApJ 646, 420

  14. Eclipsing X-ray binary M33 X-7 Pietsch et al. 2004, A&A 413, 879 XMM-Newton EPIC + Chandra ACIS-I Optical V and B-V light curvere-analysis of DIRECT data by B. Mochejska folded modulo 3.45d period Dubus et al. 1999 Improved binary ephemeris

  15. Eclipsing X-ray binary M33 X-7 Best fitting spectral models:Absorbed bremsstrahlung or disk blackbody First eclipsing black hole (high mass) X-ray binary ?

  16. Pietsch et al. 2006, ApJ 646, 420 ChASeM33 lightcurve of X-7 Gemini North radial velocity curve: > 6.9 Msun black hole Orosz et al. 2007, ATel 977

  17. ChASeM33 light curve of [PMH2004] 47 2nd eclipsing HMXB in M33 Orbital period 1.73245 d Similar to LMC X-4 or Her X-1 Pietsch et al. 2006, ATel 905

  18. The Andromeda Galaxy M 31 W. 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

  19. M 31 centre • All 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

  20. Time variability of X-ray sources in the M 31 centre field H. Stiele, W. Pietsch et al. 2007, in preparation 1035 1036 1037 1038 erg/s • Determine time variability between M 31 center pointings half a year apart • Check classification of SNRs • Classify new XRB candidate by time variability

  21. Variable X-ray sources in the M 31 centre

  22. XMM-Newton detection of type I X-ray bursts in M 31 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

  23. X-ray burster [PFH2005] 253 in the GC [WSB85] S5 15 Observation c4 Jan 7, 2002

  24. X-ray burster [PFH2005] 253 in the GC [WSB85] S5 15 Rise time < 10 s Total 50 cts Maximum duration < 20 s Max. rate 1.4±0.4ct/s Decay to backgr. ~150 s corresponds to 3.8 1038erg/s Quiescent luminosity ~5 1036erg/s (Eddington limit for H-poor matter)

  25. Simbol-X contributions:X-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>

  26. Simbol-X contributions:X-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 resolutionUnexplored energy band !!! Discovery space for the unpredicted !!!

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