X-ray sourcesQNQ/Slides/MaratGilfanov.pdf · ~2.5⋄1039 erg/s total luminosity on the time scale of

X-ray sources

Marat Gilfanov MPA, Garching

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

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).


X-ray binaries

!  accretion onto a black hole or a neutron star in a binary stellar system

!  accretion disk (Shakura-Sunyaev theory), outflows, jets


€

LX =η ˙ M c 2

η ~ 0.1− 0.2

˙ M ~ 10−10 −10−6 MSun / yrL ~ 1036 −1040 erg /s

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

mas

s ac

cret

ion

rate

binary evolution calculations

High- and low-mass X-ray binaries

time from star-formation, Gyrs


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

mas

s ac

cret

ion

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

Time dependence – sketch


HMXB LMXB

LX , NX

log(time) SF event

Time dependence – observations


SNe rate

HMXB response to SF event

time after SF event, Myrs

Shtykovsky & MG 2005, 2007

0 5 10 15 200.

51

1.5

2

f XL

F

Age (Gyr)

720

821

1052

13801404 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

Time dependence – observations


SNe rate

HMXB response to SF event

time after SF event, Myrs

Shtykovsky & MG 2005, 2007

0 5 10 15 200.

51

1.5

2

f XL

F

Age (Gyr)

720

821

1052

13801404 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

Time dependence – theory o  theory wrong? o  observations

wrong? (galaxy dating)


Fragos et al., 2014

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

Lum

inos

ity, e

rg/s

MG, 2004 Zhang, MG, Bogdan, 2011


0.5-8 keV

Scaling relations for X-ray binaries HMXBs LMXBs


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

Lum

inos

ity, e

rg/s

MG, 2004 Zhang, MG, Bogdan, 2011


€

LX = α × SFR + β × M*

0.5-8 keV

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

on the time scale of <100 Myrs

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

on the time scale of ~1-10 Gyrs

Marat Gilfanov

Scaling relations for X-ray binaries

Heidelberg, 16/7/2014

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)


€

LX = 4⋅ 1039 ×SFR erg/snearby galaxies ULIRGs CDF galaxies

€

LX ~ 3.5⋅ 1039 erg/s × SFR

Lum

inos

ity, e

rg/s

star-formation rate, M"/yr

Mineo, MG, Lehmer et al., 2014

0.5-8 keV

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


MG, 2004 Mineo, MG, Sunyaev, 2011

Ultra-luminous X-ray sources (ULX)

!  off-nuclear sources with luminosity log(LX)>39.5

!  dominate total luminosity of star-forming galaxies

!  their nature still debated o  super-Eddington accretion onto

stellar mass BH o  intermediate mass BH


Eddington limit of 10 M" object

MG, 2004 Mineo, MG, Sunyaev, 2011

Spectra (HMXBs)


pulsars

BH

ULX

Unresolved emission

Heidelberg, 16/7/2014

10-7

10-6

10-5

10-4

10-3

1 10

E2 x F

E / K

-ban

d

Energy, keV

Massive ellipticalsNormal 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

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:


L X, 1

038 e

rg/s

star-formation rate, M"/yr

€

L0.5−2keVgas ~ 6⋅ 1038 erg/s × SFR

Mineo, MG, Sunyaev, 2012

€

Lbolgas ~ 1.5⋅ 1040 erg/s × SFR

0.5-2 keV

Faint objects


1037

1038

1039

0.1 1 10

L 2-1

0keV

, erg

/s

SFR, Msun/yr

SpiralIrregular

1036

1037

1038

1039

1040

1041

109 1010 1011 1012

L 2-1

0keV

, erg

/s

LK, LK sun

Early-typeEarly-type in Virgo cluster

star-forming galaxies elliptical galaxies


Lum

inos

ity, e

rg/s

young stellar objects young stars

~5% of HMXBs

accreting white dwarfs active binaries

~3% of LMXBs Bogdan & MG, 2011

0.5-10 keV


Faint objects XLF (elliptical galaxies)

Sazonov, Revnivtsev, MG et al., 2006

Number of sources

Contribution to the luminosity

~3%

0.5-10 keV

Accreting nuclear burning WDs Population synthesis calculations

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


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

logF

λ(erg

cm−2sec−

1cm

−1)

typical spectrum

WD atmosphere (Rauch & Werner 2010) black body

Accreting nuclear burning WDs Population synthesis calculations

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


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 onlya025 BP onlya050 BP onlya025 combineda050 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

0

0.1

0.2

0.3

0.4

0.5

0.1 1 10

He

II 46

86/H

`

Age [Gyr]

Theory vs. observations: problem at young ages

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


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

Spectrum of a passive galaxy

Marat Gilfanov

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

Spectrum of a passive galaxy

Marat Gilfanov

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

Thank you!

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X-ray sourcesQNQ/Slides/MaratGilfanov.pdf · ~2.5⋄1039 erg/s total luminosity on the time scale of