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Based on a homogeneous set of X‐ray, infrared and ultraviolet observations from  Chandra ,  Spitzer ,  GALEX  and 2MASS archives, we study populations of high‐mass X‐ray binaries (HMXBs) in a sample of 29 nearby star‐forming galaxies and their relation to the star‐formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star‐formation activity in the host galaxy and their collective luminosity and number scale with the SFR: in particular, . However, the scaling relations still bear a rather large dispersion of rms ∼ 0.4 dex, which we believe is of a physical origin.  We present the catalogue of 1055 X‐ray sources detected within the  D 25 ellipse for galaxies of our sample and construct the average X‐ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with a slope of 1.6 in the log ( L  X ) ∼ 35–40 luminosity range with moderately significant evidence for a break or cut‐off at  L  X ∼ 10 40  erg s −1 . As before, we did not find any features at the Eddington limit for a neutron star or a stellar‐mass black hole.  We discuss the implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once in their lifetime experienced an X‐ray active phase powered by accretion from a high‐mass companion and obtain a rather large number,  f  X ∼ 0.2 × (0.1 Myr/τ X ), where τ X  is the lifetime of the X‐ray active phase. This is ∼4 orders of magnitude more frequent than in low‐mass X‐ray binaries (LMXBs). We also derive constraints on the mass distribution of the secondary star in HMXBs.

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