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

3. Large Magellanic Cloud
LMC was observed many times in 2003 and
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)

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

6. High-mass X-ray Binaries
Universal form
a~1.6 Grimm 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

7. Milky Way

8. 9 years Galactic plane survey with INTEGRAL
Dec 2002 – Jan 2011,
total exposure 132 Msec,
peak sensitivity in 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 many others
Krivonos et al. (2012)

9. Wind-fed binaries with NS
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 , 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

10. Majority of sources
have SG companions

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

12. Luminosity function > 2x1035 erg/s completeness 13 kpc
Cash (1979)

13. 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

14. Simple model for the wind accretion NS
Luminosity of NS
depends on:
Companion mass
Orbital period

15. Mc rises 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

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

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

18. 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

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

20. 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

21. Exclude transient sources criteria
Fp/Fmean > 0.5

22. } 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