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The 7-year view of the accreting X-ray binaries with INTEGRAL

The 7-year view of the accreting X-ray binaries with INTEGRAL. R.Krivonos, M.Revnivtsev, S.Tsygankov, E.Churazov, R.Sunyaev MPA Garching, Germany; IKI, Moscow, Russia. Galactic Center region, 20 Ms, 17-60 keV. Limiting flux ~0.26 mCrab 3.7e-12 erg/s/cm 2

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The 7-year view of the accreting X-ray binaries with INTEGRAL

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  1. The 7-year view of the accreting X-ray binaries with INTEGRAL R.Krivonos, M.Revnivtsev, S.Tsygankov, E.Churazov, R.Sunyaev MPA Garching, Germany; IKI, Moscow, Russia

  2. Galactic Center region, 20 Ms, 17-60 keV • Limiting flux ~0.26 mCrab 3.7e-12 erg/s/cm2 • Luminosity 4e+34 erg/s at the distance of GC The Milky Way is a unique galaxy where we can detect X-ray objects with the lowest possible luminosities.

  3. Galactic Center region, 20 Ms, 17-60 keV Stellar density field

  4. Low-Massive X-ray Binaries in Bulge Revnivtsev et al., 2008

  5. Low-Massive X-ray Binaries in Bulge Break in dM/dT distribution? Change in Lx – dM/dT relation? Recent: the break is due to different classes of companion stars: Gilfanov 2004 d log N / d log L = -0.96 +/- 0.20 at log(L) < 37 Revnivtsev et al., 2010

  6. Cataclysmic Variables: first approach Galactic ridge X-ray emission with INTEGRAL It is shown that the Ridge is due to point sources at energies <10 keV (Revnivtsev et al. 2006, 2007, 2008, 2009)` What is in hard X-rays?

  7. INTEGRAL view of the GRXE NIR contours Krivonos et al. 2006, 2009

  8. Galactic ridge emission in hard X-rays consists of emission of millions of CVs! INTEGRAL RXTE Shape of cutoff average mass of WDs <Mwd>~0.5-0.6 Msun

  9. Cataclysmic Variables: second approach Cataclysmic Variables • The dominant class of INTEGRAL CV is intermediate polars • Revnivtsev et al., 2008 • INTEGRAL provides one of the largest unbiased sample of luminous intermediate polars existing today (37 in the 7-year survey) • The survey is serendipitous with respect to CVs INTEGRAL

  10. Cataclysmic Variables Scale height of Galactic disk population is 130 (+90-50) kpc

  11. Ridge value in 17-60 keV Luminosity function ofhard X-ray emitting CVs only from INTEGRAL allsky survey! INTEGRAL points Revnivtsev et al. 2008 RXTE points Cumulative emissivity of CVs in 17-60 keV

  12. Revnivtsev et al. 2008

  13. Density of HMXBs In the Galactic plane INTEGRAL survey Simple toy model Lutovinov et al. 2005, 2007

  14. The position of spiral arms(ignored) Shtykovskiy & Gilfanov 2007

  15. Method: Integrate the galactic disk model with a given luminosity function, given survey sensitivity map, and measure the probability to have the observed distribution of sources.

  16. High-Massive X-ray Binaries distribution over the Galactic longitude Norma Crux Carina Sgr Cyg -- measured -- not ID -- predicted

  17. Disk without hole

  18. Disk size r_disk = 2.2 (+0.6-0.4) kpc

  19. Gamma = 1.3 (+0.3-0.2) Voss & Ajello 2010 Probing the LF (single) slope over Log(L) 33-38 -Gamma dN/dL ~L

  20. Maximum Likelihood HMXB Luminosity Function delta Likelihood < 1.0 Log

  21. Unrealistic LF shape: Overprediction at low luminosities Log

  22. Unrealistic LF shape: Underprediction at low luminosities Like “Propeller effect” Log

  23. Absolutely unrealistic LF shape: dN/dL~L^1.5 Log

  24. Concluding remarks (1) • The perfect sky imaging with IBIS/ISGRI is possible: • IKI/RSDChttp://hea.iki.rssi.ru/integral • MPA http://www.mpa-garching.mpg.de/integral • 7-year Galactic Bulge Map • Galactic Plane Survey • Galactic Bulge Monitoring • Catalog of sources with spectra and lightcurves INTEGRAL/IBIS 7-year All-Sky Hard X-Ray Survey. Part I: Image Reconstruction A&A (arXiv:1006.2463) INTEGRAL/IBIS 7-year All-Sky Hard X-Ray Survey. Part II: Catalog of Sources A&A (arXiv:1006.4437)

  25. Concluding remarks (2)LMXB in Bulge • Flat end of luminosity function at Log (L) < 37 • The cumulative angular distribution in the Galactic center region traces the cumulative number of stars (bulge and nuclear stellar disk components) => Break in dM/dT distribution? => Change in Lx – dM/dT relation? => Different classes of companions

  26. Concluding remarks (3)Cataclysmic Variables • The scale height of the Galactic disk 130 (+90-50) kpc • Luminosity Function • Luminosity density is consistent with that measured from unresolved emission (“Rigde”)

  27. Concluding remarks (4)HMXB • Spatial distribution of HMXB allows one to constrain lower and upper limits for luminosity function regardless distance information • Probe of flattening at Log (L) < 34 “Propeller effect”

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