J/MNRAS/466/1019 Bright HMXBs in THINGS galaxies (Sazonov+, 2017)
Bright end of the luminosity function of high-mass X-ray binaries:
contributions of hard, soft and supersoft sources.
Sazonov, S., Khabibullin, I.
<Mon. Not. R. Astron. Soc. 466, 1019 (2017)>
=2017MNRAS.466.1019S 2017MNRAS.466.1019S (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray
Keywords: stars: massive - galaxies: star formation - early Universe -
X-rays: binaries - X-rays: galaxies
Abstract:
Using a spectral analysis of bright Chandra X-ray sources located in
27 nearby galaxies and maps of star-formation rate (SFR) and ISM
surface densities for these galaxies, we constructed the intrinsic
X-ray luminosity function (XLF) of luminous high-mass X-ray binaries
(HMXBs), taking into account absorption effects and the diversity of
HMXB spectra. The XLF per unit SFR can be described by a power law
dN/dlogL=2.0(L/1039erg/s)(-0.6)(M☉/yr)-1 from L=1038 to
1040.5erg/s, where L is the unabsorbed luminosity at 0.25-8 keV. The
intrinsic number of luminous HMXBs per unit SFR is a factor of ∼2.3
larger than the observed number reported before. The intrinsic XLF is
composed of hard, soft and supersoft sources (defined here as those
with the 0.25-2keV to 0.25-8keV flux ratio of <0.6, 0.6-0.95 and
>0.95, respectively) in ∼2:1:1 proportion. We also constructed the
intrinsic HMXB XLF in the soft X-ray band (0.25-2keV). Here, the
numbers of hard, soft and supersoft sources prove to be nearly equal.
The cumulative present-day 0.25-2 keV emissivity of HMXBs with
luminosities between 1038 and 1040.5erg/s is
∼5x1039erg/s(M☉/yr)-1, which may be relevant for studying
the X-ray preheating of the early Universe.
Description:
"Clean sample" of 200 luminous (Lx>1038erg/s, where Lx is the
unabsorbed 0.25-8 keV luminosity) high-mass X-ray binary (HMXB)
candidates found with Chandra in 27 nearby galaxies, which was used
for the construction of the intrinsic X-ray luminosity function of
luminous HMXBs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 154 200 Clean sample of X-ray sources
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
J/ApJS/224/40 : Catalog of Chandra ACIS point like sources (Wang+, 2016)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- CXOGSG Name of the source as in Wang et al.
(2016, Cat. J/ApJS/224/40)
(JHHMMSS.s+DDMMSS)
18- 25 A8 --- GalName Name of the source's host galaxy
27- 31 F5.3 --- r25 Source's offset from the center of the
galaxy in units of its 25mag/arcsec2
radius
33- 37 I5 --- ObsID ObsId of the Chandra observation used in
X-ray data analysis
39- 43 I5 ct Counts Total number of counts detected from the
source during this observation
45 I1 --- ModelBest [0/2] Best-fitting spectral model (1)
47- 51 F5.1 10+20cm-2 NHLos Total gas column density through the
Galaxy and host galaxy in the direction
of the source
53- 57 F5.1 10+20cm-2 NHFit NH from the X-ray spectral fit
59- 63 F5.1 10+20cm-2 b_NHFit Lower limit for NH from the spectral fit
65- 69 F5.1 10+20cm-2 B_NHFit Upper limit for NH from the spectral fit
71- 76 F6.2 10+31W LxFit Intrinsic (i.e. corrected for absorption)
luminosity in 0.25-8keV energy range
78- 83 F6.2 10+31W b_LxFit Lower limit for intrinsic luminosity in
0.25-8keV energy range
85- 91 F7.2 10+31W B_LxFit Upper limit for intrinsic luminosity in
0.25-8keV energy range
93- 98 F6.2 10+31W LsSFit Intrinsic (i.e. corrected for absorption)
luminosity in 0.25-2keV energy range
100-105 F6.2 10+31W b_LsSFit Lower limit for intrinsic luminosity in
0.25-2keV energy range
107-113 F7.2 10+31W B_LsSFit Upper limit for intrinsic luminosity in
0.25-2keV energy range
115-120 F6.2 10+31W LxFitObs Observed (i.e. uncorrected for absorption)
luminosity in 0.25-8keV energy range
122-126 F5.2 10+31W LsFitObs Observed (i.e. uncorrected for absorption)
luminosity in 0.25-2keV energy range
128-131 F4.2 --- SpPar Main spectral parameter of the best model
(ModelBest) (2)
133-136 F4.2 --- b_SpPar Lower limit for main spectral parameter of
the best model (ModelBest)
138-142 F5.2 --- B_SpPar Upper limit for main spectral parameter of
the best model (ModelBest)
144 I1 --- isHard [0/1] Hard source flag
146 I1 --- isSoft [0/1] Soft source flag
148 I1 --- isSsoft [0/1] Supersoft source flag
150 I1 --- isYSN [0/1] Possible association with a young
supernova remnant
152 I1 --- isSNR [0/1] Possbile association with a
supernova remnant
154 I1 --- isNova [0/1] Possible association with a nova
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Note (1): Best-fitting spectral model as follows:
0 = power law (PL)
1 = black body (BB)
2 = multicolor disk emission (DISKBB)
Note (2): i.e. Gamma for PL, kTbb/keV for BB and kTin/keV for DISKBB.
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Acknowledgements:
Sergey Sazonov , sazonov(at)iki.rssi.ru
Ildar Khabibullin, khabibullin(at)iki.rssi.ru
(End) Sergey Sazonov, Ildar Khabibullin [IKI/Moscow, MPA/Garching] 27-Mar-2017