1994
DOI: 10.1086/187404
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ROSAT observations of the black hole candidate V404 Cygni in quiescence

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Cited by 44 publications
(51 citation statements)
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“…LIGHT CURVES X-ray and optical light curves are shown in Figure 1. Dramatic X-ray variability is clearly present with a dynamic range of greater than a factor of 20, comparable to that seen by Wagner et al (1994) on longer timescales. The lowest count rates seen in three dips (D 1 -D 3 ) correspond to a luminosity of Շ10 32 ergs s Ϫ1 , which is comparable to the X-ray luminosities of other quiescent black holes (Garcia et al 2001).…”
Section: Optical Spectrophotometrysupporting
confidence: 62%
See 1 more Smart Citation
“…LIGHT CURVES X-ray and optical light curves are shown in Figure 1. Dramatic X-ray variability is clearly present with a dynamic range of greater than a factor of 20, comparable to that seen by Wagner et al (1994) on longer timescales. The lowest count rates seen in three dips (D 1 -D 3 ) correspond to a luminosity of Շ10 32 ergs s Ϫ1 , which is comparable to the X-ray luminosities of other quiescent black holes (Garcia et al 2001).…”
Section: Optical Spectrophotometrysupporting
confidence: 62%
“…Of the stellar mass black hole population, the most accessible quiescent object is V404 Cyg. V404 Cyg is known to vary in X-rays (Wagner et al 1994;Kong et al 2002), optical (Wagner et al 1992;Casares et al 1993;Pavlenko et al 1996;Hynes et al 2002;Zurita et al 2003;Shahbaz et al 2003), IR (Sanwal et al 1996), and radio (Hjellming et al 2000), but none of these studies were coordinated. Hynes et al (2002) established that optical emission line variations are correlated with the optical continuum.…”
Section: Introductionmentioning
confidence: 99%
“…Although quiescent black hole binaries are known to be X-ray variable (e.g., Wagner et al 1994;Corbel et al 2006), it is generally assumed that the disk contribution in the IR is minimal and consistent throughout quiescence (e.g., Gelino et al 2001). To the contrary, our observations suggest that the disk may become quite bright during quiescence, even in the IR (see below).…”
Section: Discussionmentioning
confidence: 54%
“…The results also further confirm that during quiescence, significant X‐ray variability can be seen. Such variability in quiescence is also found in several black hole transients such as (Wagner et al 1994; Kong et al 2001), (Parmar et al 1997b) and (Asai et al 1998; Menou et al 1999).…”
Section: Discussionmentioning
confidence: 56%