X-ray sources Marat Gilfanov MPA, Garching X-ray sources X-ray - - PowerPoint PPT Presentation

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X-ray sources Marat Gilfanov MPA, Garching X-ray sources X-ray - - PowerPoint PPT Presentation

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X-ray sources Marat Gilfanov MPA, Garching X-ray sources X-ray binaries accreting neutron stars and black holes accreting white dwarfs with stable hydrogen fusion on the surface (super- and ultra-soft X-ray sources) various faint

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X-ray sources

Marat Gilfanov MPA, Garching

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Marat Gilfanov Heidelberg, 16/7/2014

X-ray binaries – accreting neutron stars and black holes accreting white dwarfs with stable hydrogen fusion on the surface (super- and ultra-soft X-ray sources) various faint sources – CVs, active binaries, stars hot ISM

X-ray sources

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Limitation

X-ray observations are limited to E>0.5 keV due to absorption by ISM in the Milky Way and in the target galaxy. The effect is more severe in star-forming galaxies and for sources with soft spectra (kT<0.2-0.3 keV).

Marat Gilfanov Heidelberg, 16/7/2014

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X-ray binaries

accretion onto a black hole or a neutron star in a binary stellar system accretion disk (Shakura-Sunyaev theory), outflows, jets

Marat Gilfanov Heidelberg, 16/7/2014

LX = η ˙ M c 2 η ~ 0.1− 0.2 ˙ M ~ 10−10 −10−6 MSun /yr L ~ 1036 −1040 erg/s

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formation of stars t=0 a typical HMXB t~10-100 Myrs Δt~0.1-1 Myr a typical LMXB t~1-10 Gyrs Δt~0.1-1 Gyr Cyg X-1 Sco X-1

mass accretion rate

binary evolution calculations

High- and low-mass X-ray binaries

time from star-formation, Gyrs

Marat Gilfanov Heidelberg, 16/7/2014

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formation of stars t=0 a typical HMXB t~10-100 Myrs Δt~0.1-1 Myr a typical LMXB t~1-10 Gyrs Δt~0.1-1 Gyr Cyg X-1 Sco X-1

mass accretion rate

binary evolution calculations

High- and low-mass X-ray binaries

time from star-formation, Gyrs

scale with star formation scale with stellar mass

Marat Gilfanov

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Time dependence – sketch

Marat Gilfanov Heidelberg, 16/7/2014

HMXB LMXB LX , NX log(time) SF event

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Time dependence – observations

Marat Gilfanov Heidelberg, 16/7/2014

SNe rate

HMXB response to SF event

time after SF event, Myrs

Shtykovsky & MG 2005, 2007

5 10 15 20 0.5 1 1.5 2 fXLF Age (Gyr)

720 821 1052 1380 1404 3115 3379 3585 3923 4125 4278 4365 4374 4382 4472 4552 4636 4649 4697 5866

Zhang, MG, Bogdan, 2012

LMXB specific frequency vs age

stellar age, Gyrs

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Time dependence – observations

Marat Gilfanov Heidelberg, 16/7/2014

SNe rate

HMXB response to SF event

time after SF event, Myrs

Shtykovsky & MG 2005, 2007

5 10 15 20 0.5 1 1.5 2 fXLF Age (Gyr)

720 821 1052 1380 1404 3115 3379 3585 3923 4125 4278 4365 4374 4382 4472 4552 4636 4649 4697 5866

Zhang, MG, Bogdan, 2012

LMXB specific frequency vs age

stellar age, Gyrs luminous sources

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Time dependence – theory

  • theory wrong?
  • observations

wrong? (galaxy dating)

Marat Gilfanov Heidelberg, 16/7/2014 Fragos et al., 2014

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Scaling relations for X-ray binaries

HMXBs LMXBs

star-formation rate, M/yr stellar mass, M

Grimm, MG, Sunyaev, 2003 MG, Grimm, Sunyaev, 2004 Mineo, MG, Sunyaev, 2012

Luminosity, erg/s

MG, 2004 Zhang, MG, Bogdan, 2011

Marat Gilfanov Heidelberg, 16/7/2014

0.5-8 keV

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Scaling relations for X-ray binaries

HMXBs LMXBs

star-formation rate, M/yr stellar mass, M

Grimm, MG, Sunyaev, 2003 MG, Grimm, Sunyaev, 2004 Mineo, MG, Sunyaev, 2012

Luminosity, erg/s

MG, 2004 Zhang, MG, Bogdan, 2011

Marat Gilfanov Heidelberg, 16/7/2014

LX = α × SFR + β × M*

0.5-8 keV

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for every 1 M/yr of formation rate of new stars: ~7 bright HMXBs ~2.5⋄1039 erg/s total luminosity

  • n the time scale of <100 Myrs

for every 1010 M of (old) stellar mass: ~10 bright LMXBs ~1039 erg/s total luminosity

  • n the time scale of ~1-10 Gyrs

Marat Gilfanov

Scaling relations for X-ray binaries

Heidelberg, 16/7/2014

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Total luminosity of star-forming galaxies

~2/3 due to HMXBs rms~0.4 dex calibrated to z~1 no significant evolution to z~2-3 (constrained by CXB brightness)

Marat Gilfanov Heidelberg, 16/7/2014

LX = 4⋅ 1039 × SFR erg/s

nearby galaxies ULIRGs CDF galaxies

LX ~ 3.5⋅ 1039 erg/s × SFR

Luminosity, erg/s star-formation rate, M/yr

Mineo, MG, Lehmer et al., 2014

0.5-8 keV

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X-ray luminosity functions

different XLFs of LMXBs and HMXBs (different accretion regimes) total luminosity is determined by:

  • HMXB – brightest

sources, log(LX)~40

  • LMXBs – sources with

log(LX)~38

Marat Gilfanov Heidelberg, 16/7/2014 MG, 2004 Mineo, MG, Sunyaev, 2011

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Ultra-luminous X-ray sources (ULX)

  • ff-nuclear sources with

luminosity log(LX)>39.5 dominate total luminosity of star-forming galaxies their nature still debated

  • super-Eddington accretion onto

stellar mass BH

  • intermediate mass BH

Marat Gilfanov Heidelberg, 16/7/2014

Eddington limit of 10 M object

MG, 2004 Mineo, MG, Sunyaev, 2011

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Spectra (HMXBs)

Marat Gilfanov Heidelberg, 16/7/2014

pulsars BH ULX

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Unresolved emission

Heidelberg, 16/7/2014

10-7 10-6 10-5 10-4 10-3 1 10 E2 x FE / K-band Energy, keV

Massive ellipticals Normal ellipticals Late-type galaxies

Average spectra of unresolved emission in galaxies of different types hot ISM sub-keV kT faint XRBs, CVs, stars, ISM(?)

Bogdan & MG, 2011

Marat Gilfanov

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Hot ISM in star-forming galaxies

apparent luminosity ~1/4-1/3 of HMXBs scatter is real kT~0.25 keV NH>1021 cm-2 (intrinsic) bolometric and absorption corrections are large and not very

  • reliable. However:

Marat Gilfanov Heidelberg, 16/7/2014

LX, 1038 erg/s star-formation rate, M/yr

L0.5−2keV

gas

~ 6⋅ 1038 erg/s × SFR

Mineo, MG, Sunyaev, 2012

Lbol

gas ~ 1.5⋅ 1040 erg/s × SFR

0.5-2 keV

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Faint objects

Marat Gilfanov Heidelberg, 16/7/2014

1037 1038 1039 0.1 1 10 L2-10keV, erg/s SFR, Msun/yr

Spiral Irregular

1036 1037 1038 1039 1040 1041 109 1010 1011 1012 L2-10keV, erg/s LK, LK sun

Early-type Early-type in Virgo cluster

star-forming galaxies elliptical galaxies

star-formation rate, M/yr stellar mass, M Luminosity, erg/s young stellar objects young stars ~5% of HMXBs accreting white dwarfs active binaries ~3% of LMXBs

Bogdan & MG, 2011

0.5-10 keV

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Marat Gilfanov Heidelberg, 16/7/2014

Faint objects XLF (elliptical galaxies)

Sazonov, Revnivtsev, MG et al., 2006

Number of sources Contribution to the luminosity

~3%

0.5-10 keV

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Accreting nuclear burning WDs Population synthesis calculations

Energy of hydrogen fusion ~10-30x times exceeds energy of accretion

Marat Gilfanov Heidelberg, 16/7/2014

soft X-ray luminoisty

Chen et al., 2014a,b

log(time from starburst)

data: Bogdan & MG, 2011, 2012 1.0 1.5 2.0 2.5 3.0

log(λ/ ˚ A)

16 17 18 19 20 21 22 23 24 25

logFλ(erg cm−2 sec−1 cm−1)

typical spectrum

WD atmosphere (Rauch & Werner 2010) black body

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Accreting nuclear burning WDs Population synthesis calculations

Energy of hydrogen fusion ~10-30x times exceeds energy of accretion

Marat Gilfanov Heidelberg, 16/7/2014

7.5 8.0 8.5 9.0 9.5 10.0

log(t/yr)

28.0 28.5 29.0 29.5 30.0 30.5 31.0 31.5 32.0

log(LHe/M⋆)(erg/s/M)

SP only a025 BP only a050 BP only a025 combined a050 combined

soft X-ray luminoisty HeII ionizing luminoisty (E>4Ry)

Chen et al., 2014a,b

log(time from starburst) log(time from starburst)

data: Bogdan & MG, 2011, 2012

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0.1 0.2 0.3 0.4 0.5 0.1 1 10 He II 4686/H Age [Gyr]

Theory vs. observations: problem at young ages

Either theory is wrong or galaxy dating is wrong (cf pop.synth.of LMXBs)

Marat Gilfanov Heidelberg, 16/7/2014

too much soft X-ray emission too strong HeII λ4686 line from ISM due to ionizing effect off WDs

Chen et al., 2014a,b Johansson et al., 2014

log(time from starburst) log(time from starburst)

WDs pAGB stars SDSS stacking

data: Bogdan & MG, 2011, 2012

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Spectrum of a passive galaxy

Marat Gilfanov MG & Sunyaev, 2014, in prep. Chen et al., 2014a,b

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Spectrum of a passive galaxy

Marat Gilfanov MG & Sunyaev, 2014, in prep. Chen et al., 2014a,b

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Thank you!