J/ApJ/764/41 X-ray binary evolution across cosmic time (Fragos+, 2013)
X-ray binary evolution across cosmic time.
Fragos T., Lehmer B., Tremmel M., Tzanavaris P., Basu-Zych A.,
Belczynski K., Hornschemeier A., Jenkins L., Kalogera V., Ptak A., Zezas A.
<Astrophys. J., 764, 41 (2013)>
=2013ApJ...764...41F 2013ApJ...764...41F
ADC_Keywords: Models, evolutionary ; Binaries, X-ray
Keywords: binaries: close; galaxies: stellar content; stars: evolution;
X-rays: binaries; X-rays: diffuse background; X-rays: galaxies
Abstract:
High-redshift galaxies permit the study of the formation and evolution
of X-ray binary (XRB) populations on cosmological timescales, probing
a wide range of metallicities and star formation rates (SFRs). In this
paper, we present results from a large-scale population synthesis
study that models the XRB populations from the first galaxies of the
universe until today. We use as input to our modeling the
Millennium II cosmological simulation (Boylan-Kolchin et al.
2009MNRAS.398.1150B 2009MNRAS.398.1150B) and the updated semi-analytic galaxy catalog by
Guo et al. (2011MNRAS.413..101G 2011MNRAS.413..101G) to self-consistently account for the
star formation history and metallicity evolution of the universe. Our
modeling, which is constrained by the observed X-ray properties of
local galaxies, gives predictions about the global scaling of emission
from XRB populations with properties such as SFR and stellar mass, and
the evolution of these relations with redshift. Our simulations show
that the X-ray luminosity density (X-ray luminosity per unit volume)
from XRBs in our universe today is dominated by low-mass XRBs, and it
is only at z≳2.5 that high-mass XRBs become dominant. We also find
that there is a delay of ∼1.1Gyr between the peak of X-ray emissivity
from low-mass XRBs (at z∼2.1) and the peak of SFR density (at z∼3.1).
The peak of the X-ray luminosity from high-mass XRBs (at z∼3.9)
happens ∼0.8Gyr before the peak of the SFR density, which is due to
the metallicity evolution of the universe.
Description:
The main tool we use to perform the Population Synthesis (PS)
simulations is StarTrack (Belczynski et al. 2002ApJ...572..407B 2002ApJ...572..407B,
2008ApJS..174..223B 2008ApJS..174..223B), a state-of-the-art code with special emphasis on
processes leading to the formation and further evolution of compact
objects. In the work presented here we consider the global XRB
population, i.e., XRBs in a general galaxy population of both early-
and late-type galaxies, where the contribution of dynamically formed
LMXBs is much smaller. See section 2.1 and 2.4 for further details.
The Millennium II simulation (Boylan-Kolchin et al.
2009MNRAS.398.1150B 2009MNRAS.398.1150B) is a very large N-body simulation of dark matter
evolution in the concordance ΛCDM cosmology. The simulation
uses ∼1010 particles in a 100Mpc.h-1 box, resulting in a spatial
resolution of 1kpc.h-1 and a mass resolution of
6.89x106M☉.h-1. Sixty-seven full snapshots of the simulation
were stored, with time intervals between them varying from ∼30Myr to
∼300Myr, which were then used to derive merger trees of the
dark-matter halos. See section 2.2 and 2.3 for further explanations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 51 288 A complete list of all Population Synthesis (PS)
models used in this work
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
V/106 : Catalogue of X-ray binaries (Liu+ 2001)
J/MNRAS/420/2190 : ECDFS sources with radio counterparts (Vattakunnel+, 2012)
J/MNRAS/419/2095 : HMXBs in nearby galaxies (Mineo+, 2012)
J/ApJ/749/130 : X-ray binaries in NGC 1291 with Chandra (Luo+, 2012)
J/A+A/533/A33 : LMXBs detected in nearby galaxies (Zhang+, 2011)
J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011)
J/MNRAS/417/2239 : SPIRE (f250um>17.4mJy) GOODS-N galaxies (Symeonidis+, 2011)
J/ApJ/721/1843 : Swift-BAT survey of Galactic sources (Voss+, 2010)
J/ApJ/719/L79 : BH spin-orbit misalignment in Galactic XRBs (Fragos+, 2010)
J/ApJ/689/983 : LMXBs in early-type galaxies. I. Chandra (Humphrey+, 2008)
J/ApJ/681/1163 : Late-type galaxies in Chandra deep fields (Lehmer+, 2008)
J/A+A/469/807 : Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)
J/A+A/455/1165 : Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)
J/MNRAS/360/974 : Proper motions of pulsars (Hobbs+, 2005)
J/A+A/442/1135 : High-mass XRBs in the Magellanic Clouds (Liu+, 2005)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq [1/288] Model identifier
5- 7 F3.1 --- alpha [0.1/0.5] Common envelope efficiency parameter
αCE
9- 13 F5.2 --- IMF Exponent of high-mass IMF power law component (1)
15- 18 F4.2 --- eta [0.2/2] Stellary wind strength parameter η (2)
20- 22 A3 --- CE-HG [Yes No] Common Envelope in Hertzspring Gap (3)
24- 28 A5 --- q Binary mass ratio distribution (4)
30- 32 F3.1 --- kappa [0/0.1] κDC kick distribution mutiplier,
Hobbs et al. 2005 (J/MNRAS/360/974) (5)
34- 36 I3 --- Rank [1/288] Model ranking in our statistical comparison
38- 51 F14.9 --- logL [-255/0] Log of likelihood ratio (6)
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Note (1): Value of IMF slope is either
-2.35: Kroupa (2001MNRAS.322..231K 2001MNRAS.322..231K), or
-2.7 : Kroupa & Weidner (2003ApJ...598.1076K 2003ApJ...598.1076K)
Note (2): With which the "standard" Belczynski et al. (2010ApJ...714.1217B 2010ApJ...714.1217B)
stellar wind prescription is multiplied.
Note (3): Code means:
Yes = all possible outcomes of a CE event with a HG donor are allowed.
No = A CE with a HG donor star will always result to a merger.
Note (4): initial mass ratio (q) distribution:
flat = flat distribution of q in range [0,1]
twin = distribution of a in range [0.9,1]
50-50 = half of the binaries originate from a "twin" distribution
and half from "flat" mass ratio distribution.
Note (5): For black holes formed though a supernova explosion with
negligible ejected mass.
Note (6): Of the observations given a model to our maximum likelihood model:
logL(O|Mi)-logL(O|Mref)
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 23-Oct-2014