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X-ray luminosity evolution of XRBs in normal galaxies

X-ray luminosity evolution of XRBs in normal galaxies. Zhaoyu Zuo 2009-03-18. aim. To study how the X-ray properties of late-type field galaxies evolve as a function of optical luminosity , stellar mass , and star formation rate (SFR) with time. Observations.

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X-ray luminosity evolution of XRBs in normal galaxies

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  1. X-ray luminosity evolution of XRBs in normal galaxies Zhaoyu Zuo 2009-03-18

  2. aim • To study how the X-ray properties of late-type field galaxies evolve as a function of optical luminosity, stellar mass, and star formation rate (SFR) with time.

  3. Observations • Integrated X-ray emission from HMXB and LMXB populations in local group traces galaxy star formation rate (SFR) and stellar mass (M), respectively. (Colbert et al. (2004)) • Average X-ray luminosities of normal late-type galaxies increases with redshift out to z~1.4-3 using X-ray stacking method. (Brandt et al. 2001; Hornschemeier et al. 2002;Nandra et al. 2002; Georgakakis et al. 2003; Reddy & Steidel 2004; Laird et al. 2005, 2006; Lehmer et al. 2005) • Hornschemeier et al. (2002) observed a factor of 2-3 increase in LX/LB from z=0 to 1.4 for LB galaxies.

  4. Theoretical works in archive • Ghosh & White (2001) discussed SFR evolution on the Lx evolution profiles of normal galaxies using semi-analytical method. • Sipior et al.(2003) simulated the evolution of X-ray binaries formed in a burst of star formation using population synthesis model. • Bogomazov et al.(2007) calculated luminosity function of binary X-ray sources using the “Scenario Machine”.

  5. Binary evolution wind accretion or Roche lobe overflow “primordial” binary MS+MS HMXB stellar evolution massive star: stellar evolution ~2-40 Myrs 50 Myrs Roche lobe overflow LMXB SN explosion low-mass star: stellar evolution or orbital decay (GWB/MB) BH/NS+MS 1-10 Gyrs

  6. Time dependence of XRB populations low-mass star: stellar evolution or orbital decay (GWB/MB) massive star: stellar evolution LX , NX 50 Myrs 1-10 Gyrs HMXB LMXB 50-100 Myr >1 Gyr log(time) SF event 1)HMXBs trace the immediate star formation rate of a galaxy 2)LMXBs trace its star formation history with a lag of a few Gyr.

  7. Lx-mass relation for LMXBs total X-ray luminosity number of sources Gilfanov M. (2004)

  8. Lx-SFR relation for HMXBs number of sources total X-ray luminosity Nx~SFR Lx~SFR Non-physical effect of statistics of small numbers Ltot=Lk Gilfanov M., Grimm H. and Sunyaev R. (2004)

  9. Total luminosity of XRBs Lx ~ 2•1039SFR 8•1038M* Nx(Lx>1037) ~ 7SFR 10M* [SFR]= M/yr [M*]=1010 M SFR/M: 1) High---dominant X-ray point-source contributions from HMXBs (e.g., late-type star-forming galaxies), 2) Low---point-source emission primarily from LMXBs (e.g., massive early-type galaxies).

  10. Significant positive redshift evolution in log(LX/LB) and log(LX/M) over the redshift range of z~0-1.4 • no significant evolution in Log(LX/SFR) Lehmer et al. 2008

  11. My calculation

  12. Model • X-ray luminosity: • B-band: Single Star Binary (primary & secondary) Accretion disk & irradiation of disk • SFH: Constant & Starburst

  13. Constant SF

  14. Constant SF

  15. Constant SF

  16. Star burst for 10Myr

  17. Star burst for 10Myr

  18. Other parameters • Fraction of binary • IMF • Common Envelope(CE) efficiency parameter • …….

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