M. Gilfanov

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

Based on CHANDRA observations of nearby starburst galaxies and RXTE/ASM, ASCA and MIR-KVANT/TTM studies of high mass X-ray binary (HMXB) populations in the Milky Way and Magellanic Clouds, we propose that the number and/or the collective X-ray luminosity of HMXBs can be used to measure the star formation rate (SFR) of a galaxy. We show that, within the accuracy of the presently available data, a linear relation between HMXB number and the star formation rate exists. The relation between SFR and collective luminosity of HMXBs is non-linear in the low SFR regime,

Low‐mass X‐ray binaries as a stellar mass indicator for the host galaxy

L_X\propto \SFR^{\approx 1.7}

X-ray emission from star-forming galaxies – I. High-mass X-ray binaries

, and becomes linear only for sufficiently high star formation rate, when the total number of HMXB sources becomes sufficiently large. Such behaviour is caused by the fact, that we measure collective luminosity of a population of the discrete sources. Although more subtle SFR dependent effects are likely to exist, the data are broadly consistent with the existence of a universal luminosity function of HMXBs which can be roughly described as a power law with a differential slope of

The Milky Way in X-rays for an outside observer Log(N)-Log(S) and luminosity function of X-ray binaries from RXTE/ASM data

\sim 1.6

On the X‐ray time‐lags in the black hole candidates

, a cutoff at

Soft state of Cygnus X-1: stable disc and unstable corona

L_X \sim few \times 10^{40}

Correlations between X-ray and radio spectral properties of accreting black holes

erg/sec and a normalisation proportional to the star formation rate. We apply our results to (spatially unresolved) starburst galaxies observed by CHANDRA at redshifts up to

An upper limit on the contribution of accreting white dwarfs to the type Ia supernova rate

z\sim 1

Hard X-ray view of the past activity of Sgr A in a natural Compton mirror

in the Hubble Deep Field North and show that the calibration of the collective luminosity of HMXBs as a SFR indicator based on the local sample agrees well with the SFR estimates obtained for these distant galaxies with conventional methods.

Mapping the Gas Temperature Distribution in Extended X-Ray Sources and Spectral Analysis in the Case of Low Statistics: Application to ASCA Observations of Clusters of Galaxies

Using results of Chandra observations of old stellar systems in eleven nearby galaxies of various morphological types and the census of LMXBs in the Milky Way, we study the population of low mass X-ray binaries and their relation to the mass of the host galaxy. We show that the azimuthally averaged spatial distribution of the number of LMXBs and, in the majority of cases, of their collective luminosity closely follows that of the near-infrared light. Considering galaxies as a whole, we find that in a broad mass range, log(M)~9-11.5, the total number of LMXBs and their combined luminosity are proportional to the stellar mass of the host galaxy. Within the accuracy of the light-to-mass conversion, we cannot rule out the possibility of a weak dependence of the X/M ratio on morphological type. However, the effect of such a dependence, if any, does not exceed a factor of ~1.5-2. The luminosity distributions of LMXBs observed in different galaxies are similar to each other and, with the possible exception of NGC1553, are consistent with the average luminosity function derived from all data. The average XLF of LMXBs in nearby galaxies has a complex shape and is significantly different from that of HMXBs. It follows a power law with a differential slope of ~1 at low luminosities, gradually steepens at log(Lx)>37.0-37.5 and has a rather abrupt cut-off at log(Lx)~39.0-39.5. This value of the cut-off luminosity is significantly, by an order of magnitude, lower than found for high mass X-ray binaries.