High-mass X-ray binaries as a star formation rate indicator in distant galaxies

Grimm, H.-J.; Gilfanov, M.; Sunyaev, R.

doi:10.1046/j.1365-8711.2003.06224.x

Cited by 655 publications

(1,082 citation statements)

References 83 publications

(171 reference statements)

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“…Grimm et al, 2002). The X-ray luminosity of normal star forming galaxies, dominated by HMXBs and by the hot ionized inter-stellar gas, correlates well with the star formation rate (Grimm et al, 2003;Ranalli et al, 2003;Lehmer et al, 2010;Mineo et al, 2012a,b;Lutovinov et al, 2013b). The discovery by INTEGRAL of many new HMXBs close to the tangent directions to the inner galactic arms also allowed to understand better their distribution in the Milky Way and their relation with star forming regions Bodaghee et al, 2012c;.…”

Section: Introductionmentioning

confidence: 84%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: Introductionmentioning

confidence: 84%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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“…In the studies summarized by Grimm et al (2003), M 51 has about half the star formation rate per unit galaxy mass as the LMC. So, using this assumption we expect half as many bright field stars in M 51 as in the LMC per unit mass, which results (using the mass ratios above) in ∼47 bright field stars.…”

Section: Contamination Of the Sample By Starsmentioning

confidence: 99%

The star cluster population of M 51

Gieles¹,

Bastian²,

Lamers³

2005

A&A

197

277

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Abstract. We use archival Hubble Space Telescope observations of broad-band images from the ultraviolet (F255W-filter) through the near infrared (NICMOS F160W-filter) to study the star cluster population of the interacting spiral galaxy M 51. We obtain age, mass, extinction, and effective radius estimates for 1152 star clusters in a region of ∼7.3 × 8.1 kpc centered on the nucleus and extending into the outer spiral arms. In this paper we present the data set and exploit it to determine the age distribution and relationships among the fundamental parameters (i.e. age, mass, effective radius). We show the critical dependence of the age distribution on the sample selection, and confirm that using a constant mass cut-off, above which the sample is complete for the entire age range of interest, is essential. In particular, in this sample we are complete only for masses above 5 × 10 4 M for the last 1 Gyr. Using this dataset we find: i) that the cluster formation rate seems to have had a large increase ∼50−70 Myr ago, which is coincident with the suggested second passage of its companion, NGC 5195; ii) a large number of extremely young (<10 Myr) star clusters, which we interpret as a population of unbound clusters of which a large majority will disrupt within the next ∼10 Myr; and iii) that the distribution of cluster sizes can be well approximated by a power-law with exponent, −η = −2.2 ± 0.2, which is very similar to that of Galactic globular clusters, indicating that cluster disruption is largely independent of cluster radius. In addition, we have used this dataset to search for correlations among the derived parameters. In particular, we do not find any strong trends between the age and mass, mass and effective radius, nor between the galactocentric distance and effective radius. There is, however, a strong correlation between the age of a cluster and its extinction, with younger clusters being more heavily reddened than older clusters.

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“…Some of these stars will be HMXB secondaries: Indeed several studies of late-type galaxies have established strong correlations between galaxy-wide X-ray luminosity and total SFR (e.g., Bauer et al 2002;Grimm et al 2003;Ranalli et al 2003;Gilfanov et al 2004a;Persic et al 2004;Hornschemeier et al 2005;Persic & Rephaeli 2007;Lehmer et al 2008Lehmer et al , 2010Mineo et al 2012). On the other hand, in quiescent (morphologically elliptical/S0) galaxies, longer-lived (1 Gyr) low-mass stars trace the total stellar mass accumulated over a galaxy's lifetime.…”

Section: Introductionmentioning

confidence: 99%

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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High-mass X-ray binaries as a star formation rate indicator in distant galaxies

Cited by 655 publications

References 83 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

The star cluster population of M 51

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

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