High mass Xray binaries and recent star formation
High mass X-ray binaries and recent star formation in the host galaxy P. Shtykovskiy, M. Gilfanov IKI, Moscow; MPA, Garching
High mass X-ray binaries and recent star formation Observations: HMXB XLF Grimm, Gilfanov & Sunyaev, 2003 HMXB XLF Scaled to one SFR
NHMXB=Σ NHMXBi =Σ Mi η(ti) M 1 , t 1 , NHMXB 1 M - Mass t - Age M 2 , t 2, NHMXB 2 M 3 , t 3, NHMXB 3 of the stellar population NHMXB – number of HMXBs
Evolution of HMXBs population SNII rate First B. H. Last N. S.
Evolution of HMXBs population: observational constraints Small Magellanic Cloud in the IR(100µm) + HMXBs (XMM, Shtykovskiy & Gilfanov 2005) Observed HMXBs: X inverse problem for
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)
MS + Sg Super giants Model stellar populations: • Metallicity • Extinction, distance • IMF, binary fraction, binary mass ratio • An adequacy of stellar evolution Model stellar population models • Completeness • Photometric errors • Foreground stars
Star formation history in the SMC in the IR(100µm) + HMXB (XMM)
Evolution of HMXBs population: observational constraints NHMXB(t) • Maximum abundance of HMXBs 20 -50 Myr after the SF event • Paucity of young HMXBs
Evolution of HMXBs population: observational constraints • Maximum abundance of Black hole XRB HMXBs 20 -50 Myr after the SF event • Paucity of young HMXBs
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)
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
Spiral structure and HMXBs М 51 HST image Density wave Stars and gas Bright HII regions -Current star formation HMXB -Star formation 10 -50 Myr ago
HMXBs in M 51 in Hα + Chandra HMXB (Terashima et al. , 2004) Bright HII regions HMXB Distance to the closest spiral arm
HMXBs in the Galaxy Young objects 40 Myr Lutovinov et al. (2005) Shift in the HMXB density has been observed with INTEGRAL HMXB peaks shifted
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.
HMXBs in Magellanic Clouds XMM-Newton XLF of HMXBs in the Small Magellanic Cloud ASCA
HMXBs in Magellanic Clouds Standart SFR indicators: • FIR • Hα • UV X-ray luminosity - Independent SFR indicator
X-ray binaries ● HMXB Mopt >5 -10 M☼ t~5 -100 Myr N ~ SFR ● LMXB Mopt~ M☼ t~ few Gyr N ~Stellar mass
HMXB in the LMC in Нα LMC 4 Supergiant shell LMC 4: Numerous HMXBs, Weak SF, t~10 -30 Myr 30 Dor: No HMXBs, Intensive SF, t<10 Myr 30 Dor HMXB (Liu, 2005)
Magellanic Clouds High SFR/M* NHMXB>NLMXB ● D=50 -60 kpc Sensitivity(XMM) LXmin~1033 erg/s ● Low metallicity ● LMC (IRAS, 100 µm) SMC (IRAS, 100 µm) 30 pointings XMM-Newton
Outline: • HMXBs and recent star formation history in Magellanic Clouds • HMXBs and the spiral structure of the host galaxy
High mass X-ray binaries and the spiral structure of the host galaxy
Spiral structure Bright HII regions - Current SF HMXB -Star formation 10 -50 Myr ago 0 Myr corotation Age gradient 40 Myr Young objects d Black hole systems – on spiral arms Neutron star low luminosity systems - shifted d = Расстояние до ближайшей ветви
HMXBs in Galaxy Young objects 40 Myr objects Lutovinov et al. (2005) peaks in HMXB density observed by INTEGRAL are shifted Peaks in density are shifted
HMXBs in the M 51 in Hα + Chandra HMXB (Terashima et al. . , 2004) Nature of X-ray souces: • HMXB ~ SFR • LMXB ~ Stellar mass • AGN Uniform distribution
HMXBs in the M 51 ü Evolution of HMXBs population HMXBs shift - AGE ü Galactic dynamics Corotation radius etc.
HMXBs as a star formation indicator X-ray luminosity functions SFR~0. 15 -7 M☼/yr Grimm, Gilfanov & Sunyaev, 2003
HMXBs as a star formation indicator X-ray luminosity functions, scaled to one SFR HMXBs – SFR indicator Grimm, Gilfanov & Sunyaev, 2003
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