Catalogue of high-mass X-ray binaries in the Galaxy (4th edition)

By Q. Z. Liu, J. Paradijs, Edward P. J. van den Heuvel. 2006

297 citations recorded by the source corpus.

We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. 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 114 high-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 (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-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 high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/fbb02ed1ec6aaba97fa92ca714297a295fbcffb9

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Citations in the corpus

Gamma-ray binaries and related systems (2013, background): “5 The only radio sources amongst the 117 HMXBs of Liu et al. (2006) are LS 5039, LS I +61◦303, γ Cas, IGR J17091-3624, V4641 Sgr, SS 433, Cyg X-1, Cyg X-3 and CI Cam (likely a nova).”
BlackCAT: A catalogue of stellar-mass black holes in X-ray transients (2015, methodology): “This census is the most updated available and, compared to previous catalogues (e.g. Gottwald et al. 1991; Chen et al. 1997; Remillard & McClintock 2006; Ritter & Kolb 2003; Liu et al. 2006, 2007), represents a substantial improvement in both statistics and observational parameters.”
A CATALOG OF X-RAY POINT SOURCES FROM TWO MEGASECONDS OF CHANDRA OBSERVATIONS OF THE GALACTIC CENTER (2008, background): “Around 300 such X-ray binaries are known in the Galaxy, about half of which contain low-mass donors that overfill their Roche lobe, and half of which contain high-mass (OB and Wolf–Rayet) stars that donate mass through a stellar wind (Liu et al. 2006, 2007).”
FERMI LARGE AREA TELESCOPE FIRST SOURCE CATALOG (2010, unknown): “— 1 Collaboration internal; 2 Manchester et al. (2005); 3 Liu et al. (2006); 4 Liu et al. (2007); 5 Green (2009); 6 Máız-Apellániz et al. (2004); 7 van der Hucht (2001); 8 Clark et al. (2005); 9 Dias et al. (2002); 10Harris (1996); 11Schmidt et al. (1993); 12 Thompson et al. (2007); 13 Massaro et…”
WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, background): “— [1] Kreidberg et al. (2012), [2] Ozel et al. (2010), [3] Cantrell et al. (2010), [4] Liu et al. (2007), [5] van Paradijs & Verbunt (1984), [6] Marti et al. (2010), [7] McClintock & Remillard (2006), [8] Orosz et al. (2014), [9] Cowley (1992), [10] Orosz et al. (2009), [11] Barret et al. (1996a),…”
MISSING BLACK HOLES UNVEIL THE SUPERNOVA EXPLOSION MECHANISM (2011, background): “Our Universe is littered with black holes, ranging from ones roughly the mass of our Sun to behemoths many million times more massive.”
Formation of Double Neutron Star Systems (2017, background): “These sources thus represent ∼43% of the total number of high-energy binary systems, i.e. adding all known LMXBs and HMXBs reported in Liu et al. (2007), Coleiro & Chaty (2013), Bird et al. (2016) and Fortin et al. (2017), respectively.”
FERMI LARGE AREA TELESCOPE FIRST SOURCE CATALOG (2010, unknown): “— 1 Collaboration internal; 2 Manchester et al. (2005); 3 Liu et al. (2006); 4 Liu et al. (2007); 5 Green (2009); 6 Máız-Apellániz et al. (2004); 7 van der Hucht (2001); 8 Clark et al. (2005); 9 Dias et al. (2002); 10Harris (1996); 11Schmidt et al. (1993); 12 Thompson et al. (2007); 13 Massaro et…”