The Ariel V (3A) catalogue of X-ray sources - I. Sources at low galactic latitude ( b  &lt; 10 )

Warwick, R. S.; Marshall, Nigel; Fraser, George W.; Watson, M. G.; Lawrence, A.; Page, C. G.; Pounds, K. A.; Ricketts, M. J.; Sims, M. R.; Smith, A.

doi:10.1093/mnras/197.4.865

Cited by 96 publications

(35 citation statements)

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“…The differentiation between galactic and extragalactic sources was done using SIMBAD database. The overall shape and normalisation of the Log(N)-Log(S) relation of Galactic sources is similar to that obtained by UHURU (Forman et al 1978) and ARIEL V (Warwick et al 1981). The UHURU result (Matilsky et al 1973) is schematically shown in Fig We further selected X-ray binaries from the sample and divided them into low mass (LMXB) and high mass (HMXB) binaries according to the mass of the optical companion, using the mass of the secondary, M 2 , of 2.5 M to separate high and low mass systems.…”

Section: The Log(n)-log(s) Distributionssupporting

confidence: 84%

X-ray Binaries in the Milky Way and Other Galaxies

Grimm

Gilfanov

Sunyaev

2003

Chin. J. Astron. Astrophys.

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Section: The Log(n)-log(s) Distributionssupporting

confidence: 84%

X-ray Binaries in the Milky Way and Other Galaxies

Grimm

Gilfanov

Sunyaev

2003

Chin. J. Astron. Astrophys.

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Section: The Log(n)-log(s) Distributionssupporting

confidence: 80%

The Milky Way in X-rays for an outside observer

Grimm

Gilfanov

Sunyaev

2002

A&A

369

499

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Abstract. We study the Log(N)-Log(S ) and X-ray luminosity function in the 2-10 keV energy band, and the spatial (3-D) distribution of bright, L X ≥ 10 34 −10 35 erg s −1 , X-ray binaries in the Milky Way. In agreement with theoretical expectations and earlier results we found significant differences between the spatial distributions of low (LMXB) and high (HMXB) mass X-ray binaries. The volume density of LMXB sources peaks strongly at the Galactic Bulge whereas HMXBs tend to avoid the inner ∼3−4 kpc of the Galaxy. In addition HMXBs are more concentrated towards the Galactic Plane (scale heights of ≈150 and ≈410 pc for HMXB and LMXB correspondingly) and show clear signatures of the spiral structure in their spatial distribution. The Log(N)-Log(S ) distributions and the X-ray luminosity functions are also noticeably different. LMXB sources have a flatter Log(N)-Log(S ) distribution and luminosity function. The integrated 2-10 keV luminosities of all X-ray binaries in the Galaxy, averaged over 1996-2000, are ∼2−3 × 10 39 (LMXB) and ∼2−3 × 10 38 (HMXB) erg s −1 . Normalised to the stellar mass and the star formation rate, respectively, these correspond to ∼5 × 10 28 erg s −1 M −1 for LMXBs and ∼5 × 10 37 erg s −1 /(M yr −1 ) for HMXBs. Due to the shallow slopes of the luminosity functions the integrated emission of X-ray binaries is dominated by the ∼5-10 most luminous sources which determine the appearance of the Milky Way in the standard X-ray band for an outside observer. In particular variability of individual sources or an outburst of a bright transient source can increase the integrated luminosity of the Milky Way by as much as a factor of ∼2. Although the average LMXB luminosity function shows a break near the Eddington luminosity for a 1.4 M neutron star, at least 12 sources showed episodes of super-Eddington luminosity during ASM observations. We provide the maps of distribution of X-ray binaries in the Milky Way in various projections, which can be compared to images of nearby galaxies taken by CHANDRA and XMM-Newton.

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“…Its persistent X-ray flux has been observed to vary between (0.3-2) x 10 -9 erg cm -2 s -1, with an average value of ~ 8 x 10 -l~ erg cm -2 s -1 (Davidsen et al 1974;Mason et al 1976a;Forman et al 1978;Warwick et al 1981;Wood et al 1984). Its optical counterpart, V1055 Off, is an ~19th magnitude blue star whose optical spectrum is typical for a low-mass X-ray binary (Murdin et al 1974;Davidsen et aL 1974).…”

Section: + 091mentioning

confidence: 99%

“…This bright galactic-bulge source (X-ray flux typically 200-300 #Jy, Forman et al 1978;Warwick et al 1981;Wood et al 1984) has recently been classified as an atoll-type source (Hasinger and Van der Klis 1989). GX 13 + 1 is a radio source (Grindlay and Seaquist 1986), and a (heavily reddened) infrared counterpart has been proposed by Garcia et al (1992) and Naylor et al (1991).…”

Section: -171/gx 13+1mentioning

confidence: 99%