The Xray 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 • Advancements with Simbol-X observations
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
XMM-Newton EPIC view of the diffuse emission of the starburst galaxy NGC 253 Simbol-X: Bauer et al. 2007 • ULX sources • undetected AGN? ? ? • Hard X-ray halo? ? ?
XMM-Newton survey of the Local Group W. Pietsch, Z. Misanovic, F. Haberl, galaxy M 33 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
Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B 1: 0. 2 -0. 5 ke. V B 2: 0. 5 -1. 0 ke. V B 3: 1. 0 -2. 0 ke. V B 4: 2. 0 -4. 5 ke. V B 5: 4. 5 - 12 ke. V fg-star AGN SSS SNR XRB
Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B 1: 0. 2 -0. 5 ke. V B 2: 0. 5 -1. 0 ke. V B 3: 1. 0 -2. 0 ke. V B 4: 2. 0 -4. 5 ke. V B 5: 4. 5 - 12 ke. V fg-star AGN SSS SNR XRB
Hardness ratio plots of M 33 sources HRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B 1: 0. 2 -0. 5 ke. V B 2: 0. 5 -1. 0 ke. V B 3: 1. 0 -2. 0 ke. V B 4: 2. 0 -4. 5 ke. V B 5: 4. 5 - 12 ke. V fg-star AGN SSS SNR XRB
X-ray sources in M 33 field: identification and classification Using X-ray hardness ratio criteria, optical correlation with USNO-B 1, catalogues at different wavelengths, SIMBAD, NED • foreground stars • AGN • Galaxies • SSS • SNR • XRB • Hard identified 5 1 21 (+2) classified 30 12 1 5 23 (-2) (Ghavamian et al. 2005, AJ 130, 539) 2 267
M 33 zoom in M 33 X-7 [PMH 2004] 47
Eclipsing X-ray binary M 33 X-7 Einstein + ROSAT observations: 3. 45 d period 0. 31 s pulsation? Peres et al. 1989, Ap. J 336, 140; Dubus et al. 1999, MNRAS 302, 731
Eclipsing X-ray binary M 33 X-7 Pietsch et al. 2004, A&A 413, 879 On state Eclipse On state XMM-Newton EPIC 0. 5 -4. 5 ke. V images Chandra ACIS I
Eclipsing X-ray binary M 33 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 box Haberl & Pietsch 2001 Yellow circle: Chandra error box Insert HST image 10“ x 10“ Pietsch et al. 2006, Ap. J 646, 420
Eclipsing X-ray binary M 33 X-7 Pietsch et al. 2004, A&A 413, 879 XMM-Newton EPIC + Chandra ACIS-I Optical V and B-V light curve re-analysis of DIRECT data by B. Mochejska folded modulo 3. 45 d period Dubus et al. 1999 Improved binary ephemeris
Eclipsing X-ray binary M 33 X-7 Best fitting spectral models: Absorbed bremsstrahlung or disk blackbody First eclipsing black hole (high mass) X-ray binary ?
Ch. ASe. M 33 lightcurve of X-7 Gemini North radial velocity curve: Pietsch et al. 2006, Ap. J 646, 420 > 6. 9 Msun black hole Orosz et al. 2007, ATel 977
Ch. ASe. M 33 light curve of [PMH 2004] 47 2 nd eclipsing HMXB in M 33 Orbital period 1. 73245 d Similar to LMC X-4 or Her X-1 Pietsch et al. 2006, ATel 905
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
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
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
Variable X-ray sources in the M 31 centre
XMM-Newton detection of type I X-ray bursts in M 31 W. Pietsch & F. Haberl 2005, A&A 430, L 45 • 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
X-ray burster [PFH 2005] 253 in the GC [WSB 85] S 5 15 Observation c 4 Jan 7, 2002
X-ray burster [PFH 2005] 253 in the GC [WSB 85] S 5 15 Rise time Maximum duration Decay to backgr. Quiescent luminosity < 10 s < 20 s ~150 s ~5 1036 erg/s Total 50 cts Max. rate 1. 4± 0. 4 ct/s corresponds to 3. 8 1038 erg/s (Eddington limit for H-poor matter)
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>
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, . . . ) Important parameters for nearby galaxy – High. Simbol-X mass XRBs (? eclipses with orb. period, pulsations, optical id, . . . ) investigations: – Bright transients • Big Supersoft sources field. X-ray of view high resolution – Classical SSS as known from Magellanic Clouds – Optical novae • Supernova remnants Unexplored energy band – Thermal remnants !!! Discovery space for the unpredicted !!!<hard> – Plerions (PWN) • Nuclear source • Ultraluminous X-ray sources • Diffuse emission in disk and halo – Foreground stars – Galaxies, galaxy clusters and AGN in background <hard>
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