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. 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 Group galaxy M 33 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

6. Hardness ratio plots of M 33 sources HR i = (B i+1 – B i )/ (B i+1 + B i )B 1 : 0.2-0.5 keV B 2 : 0.5-1.0 keV B 3 : 1.0-2.0 keV B 4 : 2.0-4.5 keV B 5 : 4.5- 12 keV fg-star AGN SSS SNR XRB

7. Hardness ratio plots of M 33 sources HR i = (B i+1 – B i )/ (B i+1 + B i )B 1 : 0.2-0.5 keV B 2 : 0.5-1.0 keV B 3 : 1.0-2.0 keV B 4 : 2.0-4.5 keV B 5 : 4.5- 12 keV fg-star AGN SSS SNR XRB

8. Hardness ratio plots of M 33 sources HR i = (B i+1 – B i )/ (B i+1 + B i )B 1 : 0.2-0.5 keV B 2 : 0.5-1.0 keV B 3 : 1.0-2.0 keV B 4 : 2.0-4.5 keV B 5 : 4.5- 12 keV fg-star AGN SSS SNR XRB

9. X-ray sources in M 33 field: identification and classification identifiedclassified foreground stars530 AGN12 Galaxies1 1 SSS 5 SNR 21 (+2)23 (-2) (Ghavamian et al. 2005, AJ 130, 539) XRB2 Hard 267 Using X-ray hardness ratio criteria, optical correlation with USNO-B1, catalogues at different wavelengths, SIMBAD, NED

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

11. 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-7

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

13. 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-7 Pietsch et al. 2004

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

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

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

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

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 observations with separation of half a year plus one 2.5 year later

20. 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 M 31 centre field 10 35 10 36 10 37 10 38 erg/s

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

22. Summary catalogue HR2-HR1 diagram important to select SSS, thermal SNRs and foreground stars f x /f opt separate SNRs and foreground stars Hard X-ray spectra very important for classification: should separate –XRBs –Active nuclei –Plerions Individual papers on bright sources (Osborne et al, Barnard et al., Trudolyubov et al., Mangano et al.) Time variability studies to identify XRBs Simbol-X

23. 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 X-ray bursts in M 31

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

25. Pietsch, Fliri, Freyberg, Greiner, Haberl, Riffeser, Sala 2005, A&A 442, 879 search for optical nova correlations in XMM- Newton, Chandra and ROSAT catalogs and archival observations 21 X-ray counterparts in M 31 and 2 in M 33 novae dominant class of supersoft X-ray sources in M 31 center determine masses of ejecta and burned mass from lightcurve Optical novae: the major class of supersoft X-ray sources in M 31 10 arcmin

26. X-ray burster [PFH2005] 253 in the GC [WSB85] S5 15 Rise time < 10 s Total 50 cts Maximum duration < 20 s Max. rate1.4±0.4ct/s Decay to backgr. ~150 s corresponds to 3.8 10 38 erg/s Quiescent luminosity ~5 10 36 erg/s (Eddington limit for H-poor matter)

27. Chandra HRC nova detections 2004/5 Pietsch et al. 2007, A&A 465, 375 Nova SSS light curves (<250 d) More than 30% of optical novae show SSS state

28. Simbol-X contributions: 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 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

29. Simbol-X contributions: 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 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 Important Simbol-X parameters for nearby galaxy investigations: Big field of view high resolution Unexplored energy band !!! Discovery space for the unpredicted !!!