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HMXB, ULX and star formation. Marat Gilfanov Hans-Jakob Grimm & Rashid Sunyaev. Topics. compact sources in young & old stellar systems relation to star formation and stellar mass of the host galaxy X-ray binaries (low & high mass) and ULX. HMXB t~10 6 -10 7 years - PowerPoint PPT Presentation
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HMXB, ULX and star formation
Marat GilfanovHans-Jakob Grimm & Rashid
Sunyaev
Marat Gilfanov Kyoto, 28/10/2003
• compact sources in young & old stellar systems
• relation to star formation and stellar mass of the host galaxy
• X-ray binaries (low & high mass) and ULX
Topics
Marat Gilfanov Kyoto, 28/10/2003
Evolutionary time scales
HMXB
• years• ~ duration of star
formation event
Star formation tracer
LMXB
• years• ~ live time of the
host galaxy
Stellar mass tracer
Marat Gilfanov Kyoto, 28/10/2003
Milky Way galaxy
face-on view
HMXB distribution and spiral arms
Lx~2-3 1039 erg/s
LMXB:HMXB~10:1
M*/SFR~1-2 1011 years
Marat Gilfanov Kyoto, 28/10/2003
Nearby galaxies
• Observed by Chandra
• high SFR galaxies -> HMXB• ellipticals, bulges of spirals -> LMXB
• Milky Way• Magellanic Clouds
Marat Gilfanov Kyoto, 28/10/2003
High mass X-ray binaries
(ULX in young stellar systems)
Marat Gilfanov Kyoto, 28/10/2003
HMXB in nearby galaxiesX-ray luminosity functions:
SFR~0.15-7 Msun/yr
Marat Gilfanov Kyoto, 28/10/2003
HMXB in nearby galaxiesX-ray luminosity functions scaled to the same SFR
SFR~0.15-7 Msun/yr
Marat Gilfanov Kyoto, 28/10/2003
Universal luminosity function of HMXBs
• constant shape, normalization ~ SFR
• cut-off @ few 1040
erg/s• no strong non-linear
effects
6.138
38
LSFR3.3dL
dN
Marat Gilfanov Kyoto, 28/10/2003
HMXB XLF: differential form
Marat Gilfanov Kyoto, 28/10/2003
Universal XLF of HMXBs
Galactic NS, Be binaries …
Eddington limit for a neutron star
ULXCyg X-1
Cyg X-3
V4641 Sgr(peak)
Marat Gilfanov Kyoto, 28/10/2003
ULX and HMXB
• ~featureless power law
• smooth extension of ordinary HMXB population
• a completely different population – unlikely
• high M, high Mdot (low probability) tail of ordinary HMXBs ?
Galactic NS, Be binaries …
Eddington limit f or a neutron star
ULXCyg X-1
Cyg X-3
V4641 Sgr(peak)
Marat Gilfanov Kyoto, 28/10/2003
HMXB & ULX in distant galaxies
• distant galaxies– unresolved -> total Lx only
• Hubble Deep Field North– z~0.2-1.3
– SFR~4-200 Msun/year
• Lx-SFR relation XLF parameters
Marat Gilfanov Kyoto, 28/10/2003
Expected Lx-SFR relation
XLF, number of sources ~ SFR
”
i.e. total Lx ~ SFR
Wrong!
SFRdLLdL
dNLX
Marat Gilfanov Kyoto, 28/10/2003
Expected Lx-SFR relation
Lx – total luminosity of discrete sources – 1,2,3…not 0.5
- does not work
kX,totX, LL
SFRdLLdL
dNLX
non-linear Lx-SFR relation
@low Lx and SFR
Marat Gilfanov Kyoto, 28/10/2003
Expected Lx-SFR relation
number of sources
total Lx
• power law luminosity distribution
• total LX is defined by a few brightest sources
Marat Gilfanov Kyoto, 28/10/2003
Predicted Lx-SFR relation
low SFRLX,brightest increases
with SFR non-linearly
non-linear regime
high SFR LX,brightest =LX,cut-off
linear regime
Marat Gilfanov Kyoto, 28/10/2003
Mode and expectation mean of statistical distribution
probability distributionof total Lx
P(Lx,tot)
mode – mostprobable value
expectation mean
SFRLdLdL
dNLX
Lx-SFR relation
kX,totX, LL
Marat Gilfanov Kyoto, 28/10/2003
Observed Lx-SFR relation
SFRLdLdL
dNLX
Marat Gilfanov Kyoto, 28/10/2003
Lx-SFR: observed vs predicted
Lx~SFR
Lx~SFR1.7
Marat Gilfanov Kyoto, 28/10/2003
Predicted Lx-SFR relation
• Linear part – direct consequence of cut-off in LF
• Large and asymmetric dispersion in the non-linear regime
• XLF parameters
Many astrophysical applications
Marat Gilfanov Kyoto, 28/10/2003
Cut-off in the luminosity function
Marat Gilfanov Kyoto, 28/10/2003
ULX @ large redshift (z~1)
• Not significantly more luminous than in nearby galaxies
Marat Gilfanov Kyoto, 28/10/2003
Intermediate mass black holes ???
Luminosity function Lx-SFR relation
Marat Gilfanov Kyoto, 28/10/2003
Low mass X-ray binaries
(ULX in old stellar systems)
Marat Gilfanov Kyoto, 28/10/2003
LMXB in nearby galaxies
Stellar mass range:109-3x1011 Msun
X-ray luminosity functions:
Marat Gilfanov Kyoto, 28/10/2003
LMXB in nearby galaxies
Stellar mass range:109-3x1011 Msun
X-ray luminosity functions: scaled to the same mass
Marat Gilfanov Kyoto, 28/10/2003
LMXB in nearby galaxies
Stellar mass range:109-3x1011 Msun
X-ray luminosity functions: scaled to the same mass,averaged
Marat Gilfanov Kyoto, 28/10/2003
Universal luminosity function of LMXB
• complex but ~constant shape
• normalization ~ mass
• cut-off @ ~few x1039 erg/s
Marat Gilfanov Kyoto, 28/10/2003
Lx-mass relation
number of sources total X-ray luminosity
Nx~16 src per 1010Msun Lx~9x1038 erg/s per 1010Msun
Marat Gilfanov Kyoto, 28/10/2003
X-ray & NIR growth curves - NGC1316
number of sources total luminosity
Marat Gilfanov Kyoto, 28/10/2003
High and low mass X-ray binaries in the galaxies
(ULX in young & old stellar systems)
Summary
Marat Gilfanov Kyoto, 28/10/2003
HMXB & LMXB luminosity functions
• different slopes of XLF for HMXB and LMXBdifferent accretion regimes
• Ultra luminous X-ray sourcesno true ULX among LMXBs at present
Marat Gilfanov Kyoto, 28/10/2003
M101 – bulge and disk population
Marat Gilfanov Kyoto, 28/10/2003
Conclusions
• HMXB population ~ SFR (upto z~1)~22 src (>1037 erg/s), ~7x1039 erg/s per 1 Msun/yr
• LMXB population ~ stellar mass~16 src (>1037 erg/s), ~9x1038 erg/s per 1010 Msun
• ~universal X-ray luminosity functionsdifferent for LMXB and HMXB
Marat Gilfanov Kyoto, 28/10/2003
Conclusions
• Majority of ULXs - members of the same population as ordinary HMXBs
• ULXs @ z~1 are not significantly brighter
• No true ULXs in old stellar systems (LMXBs)
Marat Gilfanov Kyoto, 28/10/2003
Conclusions (cont’d)
• Statistics of small numbers -> non-linear effectsunrelated to the physics of e.g. star formation
Lx~SFR
Lx~SFR1.7
Many astrophysicalapplications
Marat Gilfanov Kyoto, 28/10/2003
The End