x-ray sourcesqnq/slides/maratgilfanov.pdf · ~2.5⋄1039 erg/s total luminosity on the time scale...
TRANSCRIPT
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).
Marat Gilfanov Heidelberg, 16/7/2014
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 / 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
Marat Gilfanov Heidelberg, 16/7/2014
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
Marat Gilfanov Heidelberg, 16/7/2014
HMXB LMXB
LX , NX
log(time) SF event
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
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
Marat Gilfanov Heidelberg, 16/7/2014
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)
Marat Gilfanov Heidelberg, 16/7/2014
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
Marat Gilfanov Heidelberg, 16/7/2014
0.5-8 keV
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
Marat Gilfanov Heidelberg, 16/7/2014
€
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)
Marat Gilfanov Heidelberg, 16/7/2014
€
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
Marat Gilfanov Heidelberg, 16/7/2014
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
Marat Gilfanov Heidelberg, 16/7/2014
Eddington limit of 10 M" object
MG, 2004 Mineo, MG, Sunyaev, 2011
Spectra (HMXBs)
Marat Gilfanov Heidelberg, 16/7/2014
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:
Marat Gilfanov Heidelberg, 16/7/2014
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
Marat Gilfanov Heidelberg, 16/7/2014
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
star-formation rate, M"/yr stellar mass, M"
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
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
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
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
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 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)
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
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!