Populations of bright compact sources in galaxies

1
Populations of (bright) compact sources in
galaxies

• Marat Gilfanov
• MPA, Garching

2

• Hans-Jakob Grimm (CfA)
• Igor Prokopenko (IKI)
• Pavel Shtykovskiy (IKI/MPA)
• Rashid Sunyaev (MPA/IKI)
• Rasmus Voss (MPA, MPE)
• Akos Bogdan (MPA)

3
Binary evolution
wind accretion or Roche lobe overflow
primordial binary MSMS
HMXB
stellar evolution
massive star stellar evolution
2-40 Myrs
Roche lobe overflow
?50 Myrs
LMXB
SN explosion
low-mass star stellar evolution or orbital decay
BH/NSMS
1-10 Gyrs
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Lx-mass relation for LMXBs
total X-ray luminosity
number of sources
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Lx-SFR relation for HMXBs
number of sources
total X-ray luminosity
NxSFR
LxSFR
Non-physical effect of statistics of small
numbers Ltot?Lk
6
Total luminosity of XRBs

• Lx 21039?SFR ? 81038?M
• Nx(Lxgt1037) 7?SFR ? 10?M
• SFR M?/yr
• M1010 M?

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Luminosity functions
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HMXBs
X-ray luminosity functions
SFR0.15-7 Msun/yr
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HMXBs
X-ray luminosity functions scaled to the same SFR
SFR0.15-7 Msun/yr
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HMXB LMXB luminosity functions

• different shapes - different accretion regimes
• HMXB - wind accretion
• LMXB - Roche-lobe overflow
• true ULXs are associated with star-formation
• no features at LEdd for NS - ???

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HMXB XLF IMF slope

• accretion of radiation pressure driven stellar
  wind

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LMXB XLF
gravitational braking in longer Porb systems
magnetic braking(Sco X-1 etc.)
Evolved companionand/or Gravitational braking
in ultracompact binaries NSWD, Porb10
min short life-time problem
King, Bildsten, Postnov and others
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Faint sources (old populations)
number of sources
contribution to total luminosity
3
Sazonov et al., 2006Revnivtsev et al., 2006
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How abundant are X-ray binaries? Nx(Lxgt1037)
7?SFR ? 10?M
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Abundance of HMXBs
number of HMXBs observed at any given time
duration of HMXB phase
birth rate of compact objects
HMXB fraction
number of HMXB
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Abundance of HMXBs
number of HMXBs observed at any given time
Salpeter IMF
Nx-SFR relation
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Abundance of HMXBs
O,B binaries ?HMXB104-105 yrs X/Be binaries
?HMXB105-106 (?) yrs
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Abundance of LMXBs
Per 1010 Msun Salpeter IMF 7.4?107 BH
NS LMXB-Mstar relation NLMXB(LXgt1035)50 LMXBs
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Time dependence of XRB populations
LX , NX
HMXB
LMXB
has been measured (Pavel Shtykovskys talk)
50-100 Myr gt1 Gyr
log(time)
SF event
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HMXBs and the spiral structure
X-ray sources in M51 (Chandra) distance to
spiral arms
HST image of M51
stars
Beckwith, 2005
(low stat. significance)
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X-ray binaries and CXB
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X-ray binaries and CXB
Cosmic star formation
stellar mass
(from Nagamine et al., 2006)
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X-ray binaries and CXB
2-10 keV HMXB 7-10 LMXB lt1-2

• ltzHMXBgt 1.5
• ltzLMXBgt 0.5

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HMXBs unresolved part of CXB

• HMXB contribution can explain 50 of the
  unresolved part of the CXB (via contribution of
  faint normal galaxies)

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LMXBs primordial and dynamically formed (talk
of Rasmus Voss for details)
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LMXBs in M31
primordial
total
tidal capture in the bulge
GC
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LMXBs in M31
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LMXBs in M31
luminosity functions
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Images 5
Andromeda galaxy (M31)
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The End