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HMXB, ULX and star formation Marat Gilfanov Hans-Jakob Grimm & Rashid Sunyaev

HMXB, ULX and star formation

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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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Page 1: HMXB, ULX and  star formation

HMXB, ULX and star formation

Marat GilfanovHans-Jakob Grimm & Rashid

Sunyaev

Page 2: HMXB, ULX and  star formation

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

Page 3: HMXB, ULX and  star formation

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

Page 4: HMXB, ULX and  star formation

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

Page 5: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Nearby galaxies

• Observed by Chandra

• high SFR galaxies -> HMXB• ellipticals, bulges of spirals -> LMXB

• Milky Way• Magellanic Clouds

Page 6: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

High mass X-ray binaries

(ULX in young stellar systems)

Page 7: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

HMXB in nearby galaxiesX-ray luminosity functions:

SFR~0.15-7 Msun/yr

Page 8: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

HMXB in nearby galaxiesX-ray luminosity functions scaled to the same SFR

SFR~0.15-7 Msun/yr

Page 9: HMXB, ULX and  star formation

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

Page 10: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

HMXB XLF: differential form

Page 11: HMXB, ULX and  star formation

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)

Page 12: HMXB, ULX and  star formation

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)

Page 13: HMXB, ULX and  star formation

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

Page 14: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Expected Lx-SFR relation

XLF, number of sources ~ SFR

i.e. total Lx ~ SFR

Wrong!

SFRdLLdL

dNLX

Page 15: HMXB, ULX and  star formation

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

Page 16: HMXB, ULX and  star formation

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

Page 17: HMXB, ULX and  star formation

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

Page 18: HMXB, ULX and  star formation

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

Page 19: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Observed Lx-SFR relation

SFRLdLdL

dNLX

Page 20: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Lx-SFR: observed vs predicted

Lx~SFR

Lx~SFR1.7

Page 21: HMXB, ULX and  star formation

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

Page 22: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Cut-off in the luminosity function

Page 23: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

ULX @ large redshift (z~1)

• Not significantly more luminous than in nearby galaxies

Page 24: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Intermediate mass black holes ???

Luminosity function Lx-SFR relation

Page 25: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Low mass X-ray binaries

(ULX in old stellar systems)

Page 26: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

LMXB in nearby galaxies

Stellar mass range:109-3x1011 Msun

X-ray luminosity functions:

Page 27: HMXB, ULX and  star formation

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

Page 28: HMXB, ULX and  star formation

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

Page 29: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

Universal luminosity function of LMXB

• complex but ~constant shape

• normalization ~ mass

• cut-off @ ~few x1039 erg/s

Page 30: HMXB, ULX and  star formation

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

Page 31: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

X-ray & NIR growth curves - NGC1316

number of sources total luminosity

Page 32: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

High and low mass X-ray binaries in the galaxies

(ULX in young & old stellar systems)

Summary

Page 33: HMXB, ULX and  star formation

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

Page 34: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

M101 – bulge and disk population

Page 35: HMXB, ULX and  star formation

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

Page 36: HMXB, ULX and  star formation

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)

Page 37: HMXB, ULX and  star formation

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

Page 38: HMXB, ULX and  star formation

Marat Gilfanov Kyoto, 28/10/2003

The End