Metallicity dependence of high-mass X-ray binary populations

Douna, V.; Pellizza, L. J.; Mirabel, I. F.; Pedrosa, Susana

doi:10.1051/0004-6361/201525617

Cited by 97 publications

(159 citation statements)

References 54 publications

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“…In Figure 2 the green squares indicate the total X-ray luminosities from HMXBs in the nearby galaxy sample of Douna et al (2015). Each luminosity value represents the total from individually detected HMXBs, i.e.,is equivalent to our L X values.…”

Section: Discussionmentioning

confidence: 99%

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Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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We obtain total galaxy X-ray luminosities, L X , originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of our galaxies, we find that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, we find that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the ±1σ scatter of the Mineo et al. L X -star formation rate (SFR) correlation or have higher L X than predicted by this correlation for their SFR. We discuss how these "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies are consistent with the Boroson et al. L X -stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low-or high-mass XRBs, we use appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L X values. We find that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L X values can be observed due to strong XRB variability.

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Section: Discussionmentioning

confidence: 99%

“…In Figure 2 we plot L X against SFR for late-type galaxies in this sample, together with the M12 best fit and ±1σ scatter, and the comparison samples of Douna et al (2015) and Basu-Zych et al (2013;see Section 6). Four galaxies are within the correlation's scatter, while the remaining 16 (80%) show an "excess" (higher scatter).…”

Section: X Versus Sfrmentioning

confidence: 99%

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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“…number of objects per unit star-formation rate, SFR) of the HMXB XLF, as well as its possible dependence on other galactic properties such as metallicity (e.g. Linden et al 2010;Douna et al 2015), is also important for studying the 'cosmic dawn', when X-ray binaries belonging to the first generations of (massive) stars and their remnants might have (together with other mechanisms, such as supernova cosmic-ray heating, Sazonov & Sunyaev 2015) significantly preheated the Universe (e.g. Venkatesan, Giroux, & Shull 2001;Madau et al 2004;Ricotti & Ostriker 2004;Mirabel et al 2011) before it was reionised by UV radiation from subsequent generations of stars and quasars.…”

Section: Introductionmentioning

confidence: 99%

Bright end of the luminosity function of high-mass X-ray binaries: contributions of hard, soft and supersoft sources

Sazonov¹,

Khabibullin²

2016

Mon. Not. R. Astron. Soc.

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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/d log L X,unabs ≈ 2.0(L X,unabs /10 39 erg s −1 ) −0.6 (M yr −1 ) −1 from L X,unabs = 10 38 to 10 40.5 erg s −1 , where L X,unabs 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 0.25-2 keV to 0.25-8 keV 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 (0.25-2 keV). 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 10 38 and 10 40.5 erg s −1 is ∼ 5×10 39 erg s −1 (M yr −1 ) −1 , which may be relevant for studying the X-ray preheating of the early Universe.

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“…However, our code is versatile enough to change the noise model or introduce a bias or any other signal, as far as it can be mathematically modelled as a frequency-dependent deterministic process. Random processes other than noise require a more elaborated modification of the code, but their implementation is still possible (see, e.g., [17] for such an implementation in a MCMC code).…”

Section: Tablementioning

confidence: 99%

“…It can be applied to models of arbitrary complexity, the only requirement being that the posterior PDF can be computed either analytically or numerically. It works even for non-deterministic (stochastic) models that include random components other than those arising from measurement uncertainties (e.g., [17]). It can deal naturally with parameter bounds and symmetries, and performs a fast sampling of the parameter space, spending more time in high probability regions and avoiding uninteresting, low probability ones.…”

Section: Introductionmentioning

confidence: 99%