Exploring X-Ray Emission from Galaxies by Marat Gilfanov
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Marat Gilfanov
XMM Workshop 2010
Hans-Jakob Grimm
Pavel Shtykovskiy (IKI/MPA)
Rashid Sunyaev (MPA/IKI)
Rasmus Voss (MPA, MPE)
Akos Bogdan (MPA)
Igor Prokopenko (IKI)
Stefano Mineo (MPA)
Zhongli Zhang (MPA)
Marat Gilfanov
XMM Workshop 2010
Images:
5
Andromeda galaxy (M31)
Chandra X-ray observatory - resolution 0.5”
~confusion free study of XRB population
in nearby galaxies
Why to study
•
X-ray emission from galaxies, properties of galaxies,
a new stellar mass and SFR proxy
Marat Gilfanov
XMM Workshop 2010
Ranalli et al., 20006
Normal galaxies dominate in number
(but not in total flux)
Why to study
•
X-ray emission from galaxies, properties of galaxies,
a new stellar mass and SFR proxy
•
Formation and evolution of X-ray binaries
luminosity distributions
specific frequency, per M
*
and per SFR
Marat Gilfanov
XMM Workshop 2010
Marat Gilfanov
XMM Workshop 2010
X-ray binaries
High mass companion
Low mass companion
Marat Gilfanov
XMM Workshop 2010
X-ray binaries
High mass companion
Low mass companion
Marat Gilfanov
XMM Workshop 2010
Evolutionary time scales
HMXB
t~
10-50 Myrs
~ duration of star
formation event
Star formation tracer
LMXB
t~
1-10 Gyrs
~ live time of the
host galaxy
Stellar mass tracer
Marat Gilfanov
XMM Workshop 2010
L
x
, M
*
and SFR
LMXB
HMXB
Non-physical
effect of statistics
of small numbers
L
tot
=
L
k
Marat Gilfanov
XMM Workshop 2010
A new M
*
and SFR proxy?
LMXB
HMXB
Non-physical
effect of statistics
of small numbers
L
tot
=
L
k
Marat Gilfanov
XMM Workshop 2010
BUT: scatter and systematics
LMXB
HMXB
Non-physical
effect of statistics
of small numbers
L
tot
=
L
k
A new Lx-SFR study
(with Stefano Mineo)
•
uniform sample
•
no systematic effects
•
no data analysis issues
•
BUT: scatter remains
•
unlikely to be related to
SFR inaccuracy
•
(almost) no physically
meaningful correlations
•
the mean is consistent
with Ranalli et al and
Grimm et al.
Marat Gilfanov
XMM Workshop 2010
Marat Gilfanov
XMM Workshop 2010
Luminosity functions
Marat Gilfanov
XMM Workshop 2010
Luminosity functions
HMXBs and LMXBs:
different
shapes/slopes
different
accretion
regimes:
•
wind accretion
•
Roche-lobe overflow
A new HMXB XLF
•
still a power law with
slope of 1.6, fully
consistent with Grimm
et al.
•
still no feature at the
L
edd
for a neutron star
•
a possible feature at the
L
edd
for a black hole
Marat Gilfanov
XMM Workshop 2010
Marat Gilfanov
XMM Workshop 2010
HMXB XLF & IMF slope
accretion of radiation pressure driven stellar wind
Marat Gilfanov
XMM Workshop 2010
LMXB XLF
Evolved companion
and/or
Gravitational braking in
ultracompact binaries
NS+WD, Porb~10 min
short life-time problem
magnetic braking
(Sco X-1 etc.)
gravitational braking
in longer Porb systems
King, Bildsten,
Postnov and others
Marat Gilfanov
XMM Workshop 2010
Total number and luminosity of
X-ray binaries
L
x
~ 2•10
39
SFR
1•10
39
M
*
N
x
(L
x
>10
37
) ~ 7
SFR
10
M
*
[SFR]=
M
/yr
[M
*
]=10
10
M
Marat Gilfanov
XMM Workshop 2010
How many black holes
and neutron stars
become X-ray sources?
Marat Gilfanov
XMM Workshop 2010
number of HMXBs observed at any given time:
birth rate
of compact
objects
fraction
of comp.
objects
duration of
X-ray active
phase
number
of HMXB
Marat Gilfanov
XMM Workshop 2010
Fraction of compact objects
X-ray active once in their
lifetime
Powered by accretion from:
high-mass companion (HMXB)
low-mass companion (LMXB)
Marat Gilfanov
XMM Workshop 2010
Dynamical formation of
LMXBs in dense stellar
environments
Marat Gilfanov
XMM Workshop 2010
Surface density of X-ray binaries
in Andromeda galaxy
Specific frequencies of LMXBs in the Milky Way
Marat Gilfanov
XMM Workshop 2010
Specific frequencies of LMXBs in the Milky Way
•
2 stars involved
*
2
dependence on the
stellar density
•
formation rate of LMXBs in
the center of Andromeda
galaxy:
100 LMXBs per 1 Gyr
Marat Gilfanov
XMM Workshop 2010
image: Li & Wang
Andromeda galaxy (M31)
Luminosity functions
(with Zhongli Zhang)
Marat Gilfanov
XMM Workshop 2010
M31, M81, Cen A, Maffei 1,
NGC3379, NGC4697,
NGC4278, Milky Way
~200 GC LMXB
CXB subtracted
incompleteness corrected
paucity of faint sources
in GCs
no good explanation so far
(He accretors – Voss et al)
GC sources
field sources
Marat Gilfanov
XMM Workshop 2010
Faint field sources
Sazonov et al., 2006
Revnivtsev et al., 2006
number of sources
contribution to
total luminosity
~3%
Marat Gilfanov
XMM Workshop 2010
Cosmic X-ray background
~80-90% of CXB is resolved into
emission of AGN and QSO
Chandra Deep Field North (2 Msec)
CXB spectrum
Marat Gilfanov
XMM Workshop 2010
X-ray binaries and CXB
Cosmic star formation
stellar mass
(from Nagamine et al., 2006)
Marat Gilfanov
XMM Workshop 2010
X-ray binaries and CXB
HMXB contribution is
dominated by ULXs
2-10 keV:
HMXB ~7-10%
LMXB <1-2%
<z
HMXB
> ~ 1.5
<z
LMXB
> ~ 0.5
Marat Gilfanov
XMM Workshop 2010
Contributions of different HMXB kinds
HMXB spectra
HMXB luminosity function
10% HMXB pulsars + 20% BH +70% “ULX”
Swartz et al., 2004
HMXB
pulsars
Black
holes
“ULX”
Marat Gilfanov
XMM Workshop 2010
HMXBs & unresolved part of CXB
HMXB (ULX) contribution
can explain ~50% of the
unresolved part of the
CXB (via contribution of
faint normal galaxies)
Marat Gilfanov
XMM Workshop 2010
Thank you!
Marat Gilfanov
XMM Workshop 2010
Formation of binaries in close stellar
encounters
•
tidal capture
of a normal star by an NS/BH
•
collision
of NS/BH with a
red giant
•
exchange
reactions
Clark, 1975; Fabian,Pringle & Rees, 1975; Press & Teukolsky, 1977; Hut & Bahcall, 1983; Lee &
Ostriker, 1986; Verbunt 1987; …
Marat Gilfanov
XMM Workshop 2010
Centaurus A
radial distribution of LMXBs
2MASS
Chandra
point sources
In this collection of images and discussions from the XMM Workshop 2010, Marat Gilfanov and collaborators delve into the study of X-ray emissions from galaxies. They investigate the properties of galaxies, stellar mass correlations, and the formation and evolution of X-ray binaries. The presentations shed light on populations of accreting X-ray sources and provide insights into high and low mass companions in X-ray binaries, evolutionary time scales, and star formation tracers.
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Presentation Transcript
Populations of accreting X-ray sources in galaxies Marat Gilfanov MPA, GArching
Hans-Jakob Grimm Pavel Shtykovskiy (IKI/MPA) Rashid Sunyaev (MPA/IKI) Rasmus Voss (MPA, MPE) Akos Bogdan (MPA) Igor Prokopenko (IKI) Stefano Mineo (MPA) Zhongli Zhang (MPA) Marat Gilfanov XMM Workshop 2010
Andromeda galaxy (M31) Chandra X-ray observatory - resolution 0.5 ~confusion free study of XRB population in nearby galaxies Marat Gilfanov XMM Workshop 2010
Why to study X-ray emission from galaxies, properties of galaxies, a new stellar mass and SFR proxy Normal galaxies dominate in number (but not in total flux) Ranalli et al., 20006 Marat Gilfanov XMM Workshop 2010
Why to study X-ray emission from galaxies, properties of galaxies, a new stellar mass and SFR proxy Formation and evolution of X-ray binaries luminosity distributions specific frequency, per M* and per SFR Marat Gilfanov XMM Workshop 2010
X-ray binaries High mass companion Low mass companion Marat Gilfanov XMM Workshop 2010
X-ray binaries High mass companion Low mass companion Marat Gilfanov XMM Workshop 2010
Evolutionary time scales HMXB LMXB 10-50 Myrs 1-10 Gyrs ~ duration of star formation event ~ live time of the host galaxy Star formation tracer Stellar mass tracer Marat Gilfanov XMM Workshop 2010
Lx, M* and SFR HMXB LMXB Marat Gilfanov XMM Workshop 2010
A new M* and SFR proxy? HMXB LMXB Marat Gilfanov XMM Workshop 2010
BUT: scatter and systematics HMXB LMXB Marat Gilfanov XMM Workshop 2010
A new Lx-SFR study (with Stefano Mineo) uniform sample no systematic effects no data analysis issues BUT: scatter remains unlikely to be related to SFR inaccuracy (almost) no physically meaningful correlations the mean is consistent with Ranalli et al and Grimm et al. Marat Gilfanov XMM Workshop 2010
Luminosity functions Marat Gilfanov XMM Workshop 2010
Luminosity functions HMXBs and LMXBs: different shapes/slopes different accretion regimes: wind accretion Roche-lobe overflow Marat Gilfanov XMM Workshop 2010
A new HMXB XLF still a power law with slope of 1.6, fully consistent with Grimm et al. still no feature at the Ledd for a neutron star a possible feature at the Ledd for a black hole Marat Gilfanov XMM Workshop 2010
HMXB XLF & IMF slope accretion of radiation pressure driven stellar wind Marat Gilfanov XMM Workshop 2010
LMXB XLF gravitational braking in longer Porb systems magnetic braking (Sco X-1 etc.) Evolved companion and/or Gravitational braking in ultracompact binaries NS+WD, Porb~10 min short life-time problem King, Bildsten, Postnov and others Marat Gilfanov XMM Workshop 2010
Total number and luminosity of X-ray binaries Lx~ 2 1039 SFR 1 1039 M* Nx(Lx>1037) ~ 7 SFR 10 M* [SFR]= M /yr [M*]=1010 M Marat Gilfanov XMM Workshop 2010
How many black holes and neutron stars become X-ray sources? Marat Gilfanov XMM Workshop 2010
number of HMXBs observed at any given time: fraction of comp. objects duration of X-ray active phase number of HMXB birth rate of compact objects Marat Gilfanov XMM Workshop 2010
Fraction of compact objects X-ray active once in their lifetime Powered by accretion from: high-mass companion (HMXB) low-mass companion (LMXB) Marat Gilfanov XMM Workshop 2010
Dynamical formation of LMXBs in dense stellar environments Marat Gilfanov XMM Workshop 2010
Specific frequencies of LMXBs in the Milky Way specific frequency total mass NLMXB Globular clusters Galaxy ~107 Msun 13 1 per ~106 Msun 5 1010 Msun ~200 1 per ~108 Msun Surface density of X-ray binaries in Andromeda galaxy Marat Gilfanov XMM Workshop 2010
Specific frequencies of LMXBs in the Milky Way specific frequency total mass NLMXB Globular clusters Galaxy ~107 Msun 13 1 per ~106 Msun 5 1010 Msun ~200 1 per ~108 Msun 2 stars involved *2 dependence on the stellar density formation rate of LMXBs in the center of Andromeda galaxy: 100 LMXBs per 1 Gyr Marat Gilfanov XMM Workshop 2010
Andromeda galaxy (M31) image: Li & Wang Marat Gilfanov XMM Workshop 2010
Luminosity functions (with Zhongli Zhang) M31, M81, Cen A, Maffei 1, NGC3379, NGC4697, NGC4278, Milky Way field sources ~200 GC LMXB CXB subtracted incompleteness corrected GC sources paucity of faint sources in GCs no good explanation so far (He accretors Voss et al) Marat Gilfanov XMM Workshop 2010
Faint field sources number of sources contribution to total luminosity ~3% Sazonov et al., 2006 Revnivtsev et al., 2006 Marat Gilfanov XMM Workshop 2010
Cosmic X-ray background CXB spectrum Chandra Deep Field North (2 Msec) ~80-90% of CXB is resolved into emission of AGN and QSO Marat Gilfanov XMM Workshop 2010
X-ray binaries and CXB Cosmic star formation stellar mass (from Nagamine et al., 2006) Marat Gilfanov XMM Workshop 2010
X-ray binaries and CXB 2-10 keV: HMXB ~7-10% LMXB <1-2% <zHMXB> ~ 1.5 <zLMXB> ~ 0.5 HMXB contribution is dominated by ULXs Marat Gilfanov XMM Workshop 2010
Contributions of different HMXB kinds HMXB luminosity function HMXB spectra HMXB pulsars Black holes ULX Swartz et al., 2004 10% HMXB pulsars + 20% BH +70% ULX Marat Gilfanov XMM Workshop 2010
HMXBs & unresolved part of CXB HMXB (ULX) contribution can explain ~50% of the unresolved part of the CXB (via contribution of faint normal galaxies) Marat Gilfanov XMM Workshop 2010
Thank you! Marat Gilfanov XMM Workshop 2010
Formation of binaries in close stellar encounters tidal capture of a normal star by an NS/BH collision of NS/BH with a red giant exchange reactions Clark, 1975; Fabian,Pringle & Rees, 1975; Press & Teukolsky, 1977; Hut & Bahcall, 1983; Lee & Ostriker, 1986; Verbunt 1987; Marat Gilfanov XMM Workshop 2010
Centaurus A radial distribution of LMXBs Chandra point sources 2MASS Marat Gilfanov XMM Workshop 2010
