A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)

Abstract

We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (γ-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.

Binary pulsars in magnetic field versus spin period diagram

“…The majority of the MSPs are distributed around the spin-up line withṀ = 10 16 g/s. It seems likely that most MSPs may be born at the positions near the spin-up line withṀ = 10 17 g/s, which is the generally observed accretion rate for the X-ray NSs in the Low-Mass X-ray Binaries (Bradt & McClintock 1983;Hasinger & van der Klis 1989;van der Klis 2000;Liu, van Paradijs & van den Heuvel 2007). This fact was also pointed out a decade ago by Lundgren et al (1996) and Hansen and Phinney (1998).…”

“…(1) The observations of X-ray NSs in binary systems show thatṀ = 10 17 g/s is a conventionally detected mass accretion rate (van der Klis 2000; Liu, van Paradijs & van den Heuvel 2007). In the B-P diagram, most BPSRs are distributed around the spin-up line forṀ = 10 16 g/s, which means that most BPSRs should be born at the positions near the spin-up line (Ṁ = 10 17 g/s), from where the PSRs experience the spin-down time of ∼ 10 8−9 yr after the onset of the radio PSR emissions.…”

Intermittent dipping in a low-mass X-ray binary

“…Note the disproportionate reduction in the intensity below ≈ 6 keV for the dip spectra, most notable for the dip 2 interval (green). Liu et al 2007), we might expect at most one additional intermittent dipper to be detectable.…”

“…Since then, the list of known dippers has grown to include EXO 0748−676, 4U 1254−69 (XB 1254, MXB 1659−298, 4U 1746−371, 4U 1323−62, XTE J1710−281, GRS 1747−312, and possibly also XTE J1759−220 and 1A 1744−361, (e.g. Liu et al 2007). The most recent discovery of dipping behaviour is in the 24.27-d binary and burst source, GX 13+1 (Iaria et al 2014).…”

Spin period evolution of a recycled pulsar in an accreting binary

“…First, with a small amount of mass transferred, the NS is spun up from the death valley with a long period and strong field, e.g. the NS in HMXBs (B ∼ 10 12 G, P ∼ 10 s) like Her X-1 (P = 1.24 s, B = 3 × 10 12 G, see van der Meer et al 2007;Liu et al 2007). With the long-lived accretion phase, the binary accepts sufficient mass from its companion and the NS yields a substantial field decay, as in the case of MSPs (Bhattacharya & van den Heuvel 1991), e.g., the fastest known pulsar PSR J1748-2446 (B ∼ 10 8 G, P = 1.4 ms, see Hessels et al 2006).…”