1 Introduction

High-mass X-ray binaries (HMXBs) were among the very first X-ray sources detected and optically identified almost 30 years ago. These systems consist of a compact object, mostly a magnetized neutron star (NS) (X-ray pulsar) or a black hole, orbiting a massive star. The X-ray emission in these sources is due to accretion of matter from the early-type mass-losing star by the compact companion. Conventionally HMXBs can be further divided into two subgroups (van Paradijs 1983): those in which the primary is a Be star (Be/X-ray binary) and those in which the primary is a supergiant (SG/X-ray binary).

The majority of the known high-mass X-ray binaries are Be/X-ray systems. Most Be/X-ray binaries have relatively wide orbits with moderate eccentricity and their compact companions spend most of their time far away from the disc surrounding the Be stars (van den Heuvel & Rappaport 1987; Bhattacharya & van den Heuvel 1991; Apparao 1994). X-ray outbursts will be expected during the time of the neutron star's periastron passage, from a low-velocity and high-density wind around Be stars, and thus collectively termed Be/X-ray transients. Their X-ray spectra are usually hard. The hard X-ray spectrum along with the transience is an important characteristic of the Be/X-ray binaries.

In the second group of HMXB systems the compact star orbits a supergiant early-type star, deep inside the highly supersonic wind. The X-ray luminosity is either powered by pure stellar wind accretion or, in the case of the brighter systems, by Roche-lobe overflow via an accretion disk.

In 1983 the number of known HMXBs was about 30 (van Paradijs 1983). By the time of the previous catalogue the number of X-ray sources associated with massive stars had increased to 69 (van Paradijs 1995). The systematic study of ROSAT X-ray sources in the SMC and the LMC (Kahabka & Pietsch 1996; Haberl et al. 1999, 2000) and systematic programme of optical identifications (Schmidtke et al. 1994; Cowley et al. 1997; Motch et al. 1998; Stevens et al. 1999; Coe & Orosz 2000) increased the number considerably.

In this paper we present a new catalogue, which increases the number of known HMXBs to 130, including 61 newly discovered HMXBs as well as the 69 "old" ones listed in van Paradijs' catalogue.