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Survey of the Milky Way and nearby galaxies in hard X- and gamma- rays

Survey of the Milky Way and nearby galaxies in hard X- and gamma- rays. Lutovinov A. Revnivtsev M., Tsygankov S., Krivonos R., Space Research Institute (Moscow) FINCA, University of Oulu (Finland) University of Berkley (USA). INTEGRAL observatory. Launched 17 Oct 2002 (PROTON)

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Survey of the Milky Way and nearby galaxies in hard X- and gamma- rays

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  1. Survey of the Milky Way and nearby galaxies in hard X- and gamma- rays Lutovinov A. Revnivtsev M., Tsygankov S., Krivonos R., Space Research Institute (Moscow) FINCA, University of Oulu (Finland) University of Berkley (USA)

  2. INTEGRAL observatory Launched 17 Oct 2002 (PROTON) orbit - 72 h perigee~ 9000 km apogee~ 153000 km Gamma-telescope IBIS (20keV-10MeV (200 keV) ,~12´) Spectrometer SPI (15keV-8MeV) (E/dE~500)

  3. Large Magellanic Cloud LMC was observed many times in 2003 and 2009-2012 Main goal – registration of the 44Ti lines due to a radioactive decay Discovery lines at 67.9 and 78.4 keV (Grebenev et al. Nature 2012) Total exposure ~7Msec (4.8 Msec dead-time corrected)

  4. at low fluxes the curve of AGN counts inthe 3C273 region is in good agreement with the same curve averaged over the entire sky 3C273 (14) excess of bright objects, with most of them having low redshifts and being closer than ≈70 Mpc. LMC (4) Krivonos et al. (2007) Inhomogeneous of the Local Universe Lutovinov et al. (2012)

  5. High-mass X-ray Binaries Universal form a~1.6Grimm et al. (2003) Postnov (2003) Shtykovskiy, Gilfanov (2005) LMC, XMM-Newton Lutovinov et al. (2012) LMC, INTEGRAL Indication of a flatness of LFat low luminosities Shtykovskiy, Gilfanov (2007) SMC, XMM-Newton Is the LF of HMXBs really universal? Only study of MW can help to answer

  6. Milky Way

  7. 9 years Galactic plane survey with INTEGRAL Dec 2002 – Jan 2011, total exposure 132 Msec, peak sensitivity in 17-60 keV 2.9x10-12 erg/s/cm2 (0.2 mCrab) Total – 402 sources on the average map, galactic – 252 (108 LMXBs, 75 HMXBs, 36 CVs), Extragalactic – 115 (112 AGNs, 3 GCs) Identification completeness – 91% thanks to efforts of number of groups:Masetti+, Burenin+, Bikmaev+, Nespoli+, Chaty+, Bodaghee+ Rodrigues+, Tomsick+, Landi+, Malizia+, and manyothers Krivonos et al. (2012)

  8. Complete, flux-limited sample of HMXBs |b|<5º Only sources with known distances and spectral class Exclude BH, gamma-loud binaries (Cyg X-1, Cyg X-3, LSI +61 303, etc) Exclude transient sources criteria Fp/Fmean > 0.5 Flux limited 0.7 mCrab (10-11 erg/s/cm2) Final sample includes 37 sources Wind-fed binaries with NS

  9. Majority of sources have SG companions

  10. INTEGRAL view through the whole Galaxy Real sensitivity: 2x1035 erg/s 1035 erg/s Limited flux 0.7 mCrab (10-11 erg/s/cm2) 2x1035 erg/s 1035 erg/s The Galaxy was divided into 5 rings 0-2,2-5,5-8, 8-11 and 11-14 kpc Key tasks: 1) LF and 2) Surface density

  11. Luminosity function > 2x1035erg/s completeness 13 kpc > 2x1034erg/s completeness 4.1 kpc Cash (1979)

  12. Density distribution of the HMXBs vs SFR Systematic Δ=20% Guesten& Mezger 1982; Lyne, Manchester, & Taylor 1985; Chiappini,Matteucci, & Romano 2001 N≈5x10-2 SFR/SFRΘ

  13. Simple model for the wind accretion NS Luminosity ofNS dependson: Companion mass Orbital period

  14. Formation and evolution • Our statistically • complete flux- • limited sample • provides clues – • what determines • the HMXB population • Porb distribution • Mc distribution Mc rises min Mc~7-8MSun

  15. dN/dMc ~Mc-2.35(Salpeter) dN/dlogP = const(Bhattacharia, Ghosh, 2012) Orbital parameters 90% completeness Lutovinov et al. (2013)

  16. SFXT (Supergiant Fast X-ray Transients) t~hours Fm/Fp~104-5 Flux Time, days

  17. SFXT (outbursts mechanisms) Clumpy wind (Walter et al. 2006, Sidoli et al. 2011) Inhibition of the accretion (Grebenev & Sunyaev 2007, Bozzo et al. 2008) Flaring activity due to transition from (stable) radiative cooling to (unstable) Compton cooling

  18. Future surveys, predictions Spectrum XG (Russia+Germany) Launch 2014 Large area 1.18x10-13 erg/s/cm2 ~130 persistent HMXB in MW

  19. Conclusions • INTEGRAL: first complete survey of HMXB in Milky Way and LMC (absorption ignorant) • Inhomogeneous of the Local Universe • Dominance of SG systems among persistent sources! • Curved shape of HMXB LF • Surface density distribution - > SFR • Clues to mechanism of SFXT outbursts

  20. Exclude transient sources criteria Fp/Fmean > 0.5

  21. Vertical distribution of HMXBs h≈85-90 pc Distribution of massive stars WR ~45 pc(Conti & Vacca 1990) OB associations ~30 pc (Bronfman et al. 2000) Open clusters ~50 pc(Joshi 2005) Kinematical age } System velocity of HMXBs (Kaper et al. 1997; Hutoff & Kaper 2002

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