<i>Our Earliest Ancestors.</i>Bjorn Kurten , Erik J. Friis

Greiner, Thomas M.

doi:10.1086/418760

Cited by 8 publications

(15 citation statements)

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“…Finally, combined X-ray Ginga and ROSAT observations of GU Mus in outburst yielded an X-ray column density N H = 2.6 × 10 21 cm −2 , assuming a thin disc model for the spectra. This was consistent with the extinction obtained from both IUE (E B−V 0.2−0.3), and HST observations (E B−V = 0.287 ± 0.004, Cheng et al 1992), and is larger than the expected galactic reddening in this direction, suggesting that the GU Mus transient is located behind the galactic disc (Greiner et al 1994). Because the estimate of distance from X-ray observations is highly model dependent, we use here the "optical value" of d = 5.5 kpc as our reference distance.…”

Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)supporting

confidence: 91%

“…Prior to 1991, there were no outbursts detected from this source (Greiner et al 1994). Following the 1991 outburst, the source luminosity showed an exponential decline typical of BH-systems, with a characteristic timescale of 21.9 days.…”

Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)mentioning

confidence: 88%

“…The combined high/soft state ROSAT and Ginga spectrum was fitted by a two component model, consisting of a multitemperature disk blackbody (Mitsuda et al 1984), with a maximal disk temperature of 0.96 keV plus a hard powerlaw component with a photon index of 2.45 (Greiner et al 1994). Subsequent photometric observations of the optical counterpart during April 92 to July 94 revealed a periodicity of ∼10.38 hr in this source (Orosz et al 1996).…”

Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)mentioning

confidence: 99%

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XMM-Newton detection of Nova Muscae 1991 in quiescence

Sutaria

Kolb

Charles

et al. 2002

A&A

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Abstract. The soft X-ray transient GU Mus has been detected by XMM-Newton in the quiescent state. The source is very faint, with a 0.5-10.0 keV unabsorbed flux of 1.1 × 10 −14 ergs cm −2 s −1 . The spectra is well fit by an absorbed powerlaw with a photon index of α = 1.6 ± 0.4, close to the value seen when the source was in the low/hard state in Aug. 1991. From our observed luminosity, it seems unlikely that the quiescent state emission is dominated by coronal X-rays from the secondary. The flux also appears to be in agreement with the ADAF model of BH-transients in quiescence.

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Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)supporting

confidence: 91%

Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)mentioning

confidence: 88%

Section: Earlier Observations Of Sxt Gu Mus (Nova Muscae 1991)mentioning

confidence: 99%

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XMM-Newton detection of Nova Muscae 1991 in quiescence

Sutaria

Kolb

Charles

et al. 2002

A&A

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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). d Assuming a distance of 50 kpc for LMC and 60 kpc for SMC.…”

Section: Rxte All-sky Monitor Datamentioning

confidence: 99%

The Milky Way in X-rays for an outside observer

Grimm

Gilfanov

Sunyaev

2002

A&A

369

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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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“…(2000), (xiv) King (1993), (xv) Nakamura et al (1989), (xvi) Greiner et al (1994), (xvii) Orosz et al (1996), (xviii) Barret et al (1996), ( . Since most of the sources in the ASCA survey are unidentified we followed the criterion suggested by Sugizaki et al (2001) in order to discriminate X-ray binary candidates from other sources: that X-ray binary candidates have either a spectral photon index Γ < 1, or a spectral photon index Γ < 3 and a column density N H < 0.8 · 10 .…”

Section: Luminosity Function Andṁ Distribution Of X-ray Binariesmentioning

confidence: 99%