Discovery of a bright X-ray Nova, GS 2000+25

Tsunemi, H.; Kitamoto, Shunji; Okamura, S.; Roussel-Dupré, D.

doi:10.1086/185383

Cited by 57 publications

(32 citation statements)

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“…(1) ASM (this paper), (2) Sazonov et al (1997), (3) Tanaka (1992), (4) Nakamura et al (1989), (5) Kitamoto et al (1992), (6) Watson et al (1978), (7) Tsunemi et al (1989). c Reference(s) for the distance: (i) van Paradijs & White (1995), (ii) Mirabel & Rodriguez (1994), (iii) Bradshaw et al (1999), (iv) Orosz & Kuulkers (1999), (v) Cowley et al (1979), (vi) Smale (1998), (vii) Penninx (1989), (viii) Wachter & Margon (1996), (ix) Christian & Swank (1997), (x) Ebisuzaki et al (1984), (xi) Predehl et al (2000), (xii) Nishiuchi et al (1999), (xiii) Orosz et al (2000), (xiv) King (1993), (xv) Nakamura et al (1989), (xvi) Greiner et al (1994), (xvii) Orosz et al (1996), (xviii) Barret et al (1996), (xix) Orosz et al (2002), (xx) Martin et al (1995), (xxi) Chevalier & Ilovaisky (1990).…”

Section: Rxte All-sky Monitor Datamentioning

confidence: 95%

The Milky Way in X-rays for an outside observer

Grimm

Gilfanov

Sunyaev

2002

A&A

377

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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Section: Rxte All-sky Monitor Datamentioning

confidence: 95%

The Milky Way in X-rays for an outside observer

Grimm

Gilfanov

Sunyaev

2002

A&A

377

499

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“…(1) ASM (this thesis), (2) Sazonov et al (1997), (3) Tanaka (1992), (4) Nakamura et al (1989), (5) Kitamoto et al (1992), (6) Watson et al (1978), (7) Tsunemi et al (1989). (2000), (xiv) King (1993), (xv) Nakamura et al (1989), (xvi) Greiner et al (1994), (xvii) Orosz et al (1996), (xviii) Barret et al (1996), ( .…”

Section: Luminosity Function Andṁ Distribution Of X-ray Binariesmentioning

confidence: 99%

X-ray Binaries in the Milky Way and Other Galaxies

Grimm

Gilfanov

Sunyaev

2003

Chin. J. Astron. Astrophys.

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“…The SXT GS 2000+25 was discovered when it went into outburst in 1988 (Tsunemi et al 1989). Photometric observations during the outburst suggested that its orbital period was near 8.26 hr (Chevalier & Ilovaisky 1990;Charles et al 1991); and the exponential decay of the outburst light curve and the X-ray spectrum suggested that the compact star in the system might be a black hole.…”

Section: Introductionmentioning

confidence: 99%

The Mass of the Black Hole in GS 2000+25

Ioannou

Robinson

Welsh

et al. 2004

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We measured the I-band orbital light curve of the soft X-ray transient GS 2000+25 in 1992 August, and the Rand I-band light curves between 1998 September and 2000 August. The light curves are dominated by the ellipsoidal variations of the secondary star in the system. The light curves also showed transient distortions that persisted through individual observing runs, but were diluted and nearly absent in the mean light curve. A small, residual distortion in the mean light curve is consistent with extra flux from a bright spot where the stream of material from the secondary star interacts with the accretion disk around the compact star. The light curve does not show eclipses. The best fits to the mean light curve were achieved with a model that included ellipsoidal variations of the secondary star plus a bright spot on the edge of the accretion disk. The flux from the accretion disk is not well constrained but must be less than 32% of the total R-band flux. Combining our data with previously published spectroscopy of GS 2000+25, we find that the mass of the compact star lies in the range 5:5 P M 1 =M P 8:8, and therefore it is a black hole. The derived mass of the secondary star depends sensitively on the mass ratio, which is measured from the rotational broadening of the absorption lines in the secondary's spectrum. We find 0:16 P M 2 =M P 0:47, but we deem this result less secure than the mass for M 1 . The radius and spectral type (K5) of the secondary are not consistent with those of main-sequence stars with masses in this range but are consistent with an evolved star that has been stripped of mass.

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Discovery of a bright X-ray Nova, GS 2000+25

Cited by 57 publications

References 0 publications

The Milky Way in X-rays for an outside observer

The Milky Way in X-rays for an outside observer

X-ray Binaries in the Milky Way and Other Galaxies

The Mass of the Black Hole in GS 2000+25

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