J/ApJ/766/19 XRB population synthesis models in 0<z<20 galaxies (Tremmel+, 2013)
Modeling the redshift evolution of the normal galaxy X-ray luminosity function.
Tremmel M., Fragos T., Lehmer B.D., Tzanavaris P., Belczynski K.,
Kalogera V., Basu-Zych A.R., Farr W.M., Hornschemeier A., Jenkins L.,
Ptak A., Zezas A.
<Astrophys. J., 766, 19 (2013)>
=2013ApJ...766...19T 2013ApJ...766...19T
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:
Emission from X-ray binaries (XRBs) is a major component of the total
X-ray luminosity of normal galaxies, so X-ray studies of high-redshift
galaxies allow us to probe the formation and evolution of XRBs on very
long timescales (∼10Gyr). In this paper, we present results from
large-scale population synthesis models of binary populations in
galaxies from z=0 to ∼20. We use as input into our modeling the
Millennium II Cosmological Simulation 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 (SFH) and
metallicity evolution of each galaxy. We run a grid of 192 models,
varying all the parameters known from previous studies to affect the
evolution of XRBs. We use our models and observationally derived
prescriptions for hot gas emission to create theoretical galaxy X-ray
luminosity functions (XLFs) for several redshift bins. Models with low
common envelope efficiencies, a 50% twins mass ratio distribution, a
steeper initial mass function exponent, and high stellar wind
mass-loss rates best match observational results from Tzanavaris &
Georgantopoulos, though they significantly underproduce bright
early-type and very bright (Lx>1041) late-type galaxies. These
discrepancies are likely caused by uncertainties in hot gas emission
and SFHs, active galactic nucleus contamination, and a lack of
dynamically formed low-mass XRBs. In our highest likelihood models, we
find that hot gas emission dominates the emission for most bright
galaxies. We also find that the evolution of the normal galaxy X-ray
luminosity density out to z=4 is driven largely by XRBs in galaxies
with X-ray luminosities between 1040 and 1041erg/s.
Description:
In this study, we use the data from the most recent Millennium Run II
(MRII; Boylan-Kolchin et al. 2009MNRAS.398.1150B 2009MNRAS.398.1150B). This is an N-body
simulation that follows the evolution of 21603 particles, each of
mass 6.9x106h-1M☉ within a comoving box with sides each of
size 100h-1Mpc. The cosmological model used in the simulation is a
Λ cold dark matter model with Ωm=0.25,
ΩΛ=0.75, Ωb=0.045, and h=H0/100km/s/Mpc=0.73.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 51 192 Parameters and likelihood values for models
referred to in the paper
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See also:
J/ApJ/764/41 : X-ray binary evolution across cosmic time (Fragos+, 2013)
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/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/720/368 : Color-magnitude relations of galaxies in CDFs (Xue+, 2010)
J/ApJ/719/L79 : BH spin-orbit misalignment in Galactic XRBs (Fragos+, 2010)
J/ApJ/716/615 : Binary object coalescence rates (O'Shaughnessy+, 2010)
J/A+A/508/355 : Scaled solar tracks and isochrones (Bertelli+, 2009)
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/MNRAS/360/974 : Proper motions of pulsars (Hobbs+, 2005)
J/ApJ/586/826 : Chandra X-ray observations of NGC 1316 (Kim+, 2003)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Model [1/288] Model number
5- 7 F3.1 --- alpha [0.1/0.5] Common envelope efficiency parameter (3)
9- 12 F4.2 --- IMF [2.35/2.7] Initial mass function exponent
14- 17 F4.2 --- eta [0.25/2] Stellar wind strength parameter η
19- 21 A3 --- CE-HG [Yes/No ] Common envelope during Hertzsprung
gap doner
23- 27 A5 --- q Binary mass ratio distribution (flat or 50-50) (1)
29- 31 F3.1 --- Kick [0/0.1] SN kick given to collapse black holes (2)
33- 35 I3 --- rank [1/192] Rank of model based on the likelihood value
37- 51 F15.9 [-] logLk [-3800/0] Log of ratio likelihood of the model to
that of the highest likelihood model.
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Note (1):
50-50 = half of the binaries originate from a "twin binary" distribution
and half from flat mass ratio distribution.
Note (2): SN kick given to direct collapse black holes is:
0.0 = no SN kick given;
0.1 = small SN kick given.
Note (3): Common envelope efficiency parameter αCE measures how
efficiently orbital energy loss is transformed into thermal energy
that will expel the donor's envelope during the CE phase
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 07-Nov-2014