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High mass X-ray binaries and recent star formation in the host galaxy

High mass X-ray binaries and recent star formation in the host galaxy. P.Shtykovskiy , M.Gilfanov. IKI, Moscow; MPA, Garching. Grimm, Gilfanov & Sunyaev , 2003. High mass X-ray binaries and recent star formation. Observations:. HMXB XLF HMXB XLF.

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High mass X-ray binaries and recent star formation in the host galaxy

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  1. High mass X-ray binaries and recent star formation in the host galaxy P.Shtykovskiy, M.Gilfanov IKI, Moscow; MPA, Garching

  2. Grimm, Gilfanov & Sunyaev, 2003 High mass X-ray binaries andrecent star formation Observations: HMXB XLF HMXB XLF Scaled to one SFR

  3. NHMXB=Σ NHMXBi=Σ Miη(ti) M1 ,t1 , NHMXB1 M - Mass t - Age NHMXB – number of HMXBs of the stellar population M2 ,t2,NHMXB2 M3 ,t3,NHMXB3

  4. Evolution ofHMXBs population SNII rate First B.H. Last N.S.

  5. Evolution ofHMXBs population: observational constraints Small Magellanic Cloud in the IR(100µm)+ HMXBs (XMM, Shtykovskiy & Gilfanov 2005) Observed HMXBs: X inverse problem for

  6. Star formation history in the Small Magellanic Cloud 10 Myr MS Supergiants 40 Myr CMD of the SMC (MCPS catalogue, Zaritsky et al., 2002) + Padua isochrones (Girardi et al., 2002)

  7. Super giants MS + Sg Model stellar populations: • Metallicity • Extinction, distance • IMF, binary fraction, binary mass ratio • An adequacy of stellar evolution models • Completeness • Photometric errors • Foreground stars Model stellar population

  8. Star formation history in the SMC SMC in the IR(100µm)+ HMXB (XMM)

  9. Evolution of HMXBs population: observational constraints • Maximum abundance of HMXBs 20-50 Myr after the SF event • Paucity of young HMXBs NHMXB(t)

  10. Evolution of HMXBs population: observational constraints • Maximum abundance of HMXBs 20-50 Myr after the SF event • Paucity of young HMXBs Black hole XRB

  11. Evolution of HMXBs population: observational constraints • Maximum abundance of HMXBs 20-50 Myr after the SF event • Paucity of young HMXBs Popov et al. (1998)(Z=0.02, log(Lmin)=33)

  12. Evolution of HMXBs population: observational constraints Bright HMXBs (expected) Bright HMXBs: young Weak HMXBs: older on average SMC: Log(Lmin)=34 Distant galaxies: Log(Lmin)=38-39

  13. Spiral structure and HMXBs • BrightHII regions • Current star formation • HMXB • -Star formation10-50 Myr ago Density wave М 51 HST image Stars and gas

  14. HMXBs in M51 M51 in Hα+ ChandraHMXB (Terashima et al., 2004) Bright HII regions HMXB Distance to the closest spiral arm

  15. HMXBs in the Galaxy Young objects HMXB peaks shifted 40 Myr Lutovinov et al. (2005) - Shift in the HMXB density has been observed with INTEGRAL

  16. Conclusions • Simple linear relation N(HMXB)=A*SFR may break down in some cases. • Maximum number of HMXBs is reached after 20-50 Myr after the star formation burst. • Spiral structure in the HMXBs distribution may be shifted relative to the spiral structure in the distribution of young objects.

  17. HMXBs in Magellanic Clouds XMM-Newton ASCA XLF of HMXBs in the Small Magellanic Cloud

  18. HMXBs in Magellanic Clouds • Standart SFR indicators: • FIR • Hα • UV X-ray luminosity - Independent SFR indicator

  19. X-ray binaries • HMXB Mopt >5-10 M☼t~5-100 Myr N ~SFR • LMXB Mopt~ M☼t~ few Gyr N~Stellar mass

  20. HMXBin the LMC LMC in Нα Supergiant shell LMC4: Numerous HMXBs, Weak SF, t~10-30 Myr 30 Dor: No HMXBs, Intensive SF, t<10 Myr LMC4 30 Dor HMXB (Liu, 2005)

  21. Magellanic Clouds SMC (IRAS, 100 µm) • High SFR/M*NHMXB>NLMXB • D=50-60 kpc Sensitivity(XMM) LXmin~1033erg/s • Low metallicity LMC (IRAS, 100 µm) 30 pointings XMM-Newton

  22. Outline: • HMXBs and recent star formation history in Magellanic Clouds • HMXBs and the spiral structure of the host galaxy

  23. High mass X-ray binaries and the spiral structure of the host galaxy

  24. Spiral structure • BrightHII regions • - Current SF • HMXB • -Star formation10-50 Myr ago 0 Myr Age gradient 40 Myr corotation 40 Myr Young objects d Black hole systems – on spiral arms Neutron star low luminosity systems - shifted d = Расстояние до ближайшей ветви

  25. HMXBs in Galaxy Peaks in density are shifted Young objects 40 Myr objects Lutovinov et al. (2005) - peaks inHMXB density observed by INTEGRAL are shifted

  26. HMXBs in the M51 M51 in Hα+ ChandraHMXB(Terashima et al.., 2004) • Nature of X-ray souces: • HMXB~SFR • LMXB~ Stellar mass • AGNUniform distribution

  27. HMXBs in the M51 • Evolution of HMXBs population HMXBs shift - AGE • Galactic dynamics Corotation radius etc.

  28. Спиральная структура в распределении HMXB • Яркие области HII • текущее звездообразование • HMXB • -звездообразование 10-50 млн. • лет назад Волна плотности М 51 HST image 0 млн. лет Вращение звезд возраст 40 млн. лет Внутри радиуса коротации: Ω(волна плотности)<Ω(звезд)

  29. Grimm, Gilfanov & Sunyaev, 2003 HMXBs as a star formation indicator X-ray luminosity functions SFR~0.15-7 M☼/yr

  30. Grimm, Gilfanov & Sunyaev, 2003 HMXBs as a star formation indicator X-ray luminosity functions, scaled to one SFR HMXBs – SFR indicator

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