X-ray emission from star-forming galaxies - III. Calibration of the Lx-SFR relation up to redshift z$\simeq$1.3

2; (2) Max Planck Institute for Astrophysics; 3); (3) University of Durham; 4); 4) ((1) Harvard-Smithsonian Center for Astrophysics; (4) Space Research Institute of Russian Academy of Sciences; (5) The Johns Hopkins University; 6); (6) NASA Goddard Space Flight Centre

arxiv: 1207.2157 · v2 · pith:O3354FPLnew · submitted 2012-07-09 · 🌌 astro-ph.HE · astro-ph.CO

X-ray emission from star-forming galaxies - III. Calibration of the Lx-SFR relation up to redshift zsimeq1.3

S. Mineo (1 , 2 , 3) , M. Gilfanov (2 , 4) , B. D. Lehmer (5 , 6) , G. E. Morrison (7

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8) R. Sunyaev (2 4) ((1) Harvard-Smithsonian Center for Astrophysics (2) Max Planck Institute for Astrophysics (3) University of Durham (4) Space Research Institute of Russian Academy of Sciences (5) The Johns Hopkins University (6) NASA Goddard Space Flight Centre (7) Institute for Astronomy University of Hawaii (8) Canada France Hawaii Telescope)

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classification 🌌 astro-ph.HE astro-ph.CO

keywords galaxiesrelationstar-formingfindformationlx-sfrrateredshift

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We investigate the relation between total X-ray emission from star-forming galaxies and their star formation activity. Using nearby late-type galaxies and ULIRGs from Paper I and star-forming galaxies from Chandra Deep Fields, we construct a sample of 66 galaxies spanning the redshift range z~0-1.3 and the star-formation rate (SFR) range ~0.1-10^3 M_sun/yr. In agreement with previous results, we find that the Lx-SFR relation is consistent with a linear law both at z=0 and for the z=0.1-1.3 CDF galaxies, within the statistical accuracy of ~0.1 in the slope of the Lx-SFR relation. For the total sample, we find a linear scaling relation Lx/SFR~(4.0\pm 0.4)x10^{39}(erg/s)/(Msun/yr), with a scatter of ~0.4 dex. About ~2/3 of the 0.5-8 keV luminosity generated per unit SFR is expected to be due to HMXBs. We find no statistically significant trends in the mean Lx/SFR ratio with the redshift or star formation rate and constrain the amplitude of its variations by <0.1-0.2 dex. These properties make X-ray observations a powerful tool to measure the star formation rate in normal star-forming galaxies that dominate the source counts at faint fluxes.

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