2000
DOI: 10.1086/308582
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Optical Identification of Faint X‐Ray Sources in the Core of ω Centauri

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Cited by 19 publications
(36 citation statements)
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“…This work was pioneered in NGC 6397 with a search for Hα emitting objects by Cool et al (1993Cool et al ( , 1995, and spectroscopic follow-up confirming the classification as cataclysmic variables by Grindlay et al (1995), Cool et al (1998) and Edmonds et al (1999). Plausible candidate counterparts were also found for two X-ray sources in the core of ω Cen (Carson et al 2000). All of these suggested counterparts were confirmed with the more accurate positions obtained with Chandra.…”
Section: Some Information On the Luminous X-ray Sources In Globularmentioning
confidence: 65%
“…This work was pioneered in NGC 6397 with a search for Hα emitting objects by Cool et al (1993Cool et al ( , 1995, and spectroscopic follow-up confirming the classification as cataclysmic variables by Grindlay et al (1995), Cool et al (1998) and Edmonds et al (1999). Plausible candidate counterparts were also found for two X-ray sources in the core of ω Cen (Carson et al 2000). All of these suggested counterparts were confirmed with the more accurate positions obtained with Chandra.…”
Section: Some Information On the Luminous X-ray Sources In Globularmentioning
confidence: 65%
“…The three core sources are the two proposed CV candidates (Carson et al 2000) and source 24 which was found to be variable within the XMM-Newton observation (see Sect. 5 and Fig.…”
Section: Sources Within the Core And The Half Mass Radiimentioning
confidence: 99%
“…From follow-up observations using the accurate Chandra positions, Cool et al (2002) claimed that there were at least three classes of binaries present in the detected sample. Two of the three ROSAT core sources (ROSAT R9a and R9b) may be CVs (Carson et al 2000). The third ROSAT core source (R20, Verbunt & Johnston 2000) was associated with a main sequence optical counterpart, showing weak Hα emission, suggesting a BY Dra system rather than a CV.…”
Section: Introductionmentioning
confidence: 97%
“…It might be possible to eliminate caveat a) by measuring the NH to other objects in the cluster with high precision. We attempted this using spectra from the two brightest cataclysmic variables in ω Cen (Carson, Cool & Grindlay 2000;Cool et al 2013), extracted from the deep 2012 Chandra observations. However, we found that the measured NH for each spectrum was inconsistent with, and larger than, the value predicted by the extinction to the cluster, and the NH we measured for the qLMXB, and that the two NH values were also inconsistent with each other.…”
mentioning
confidence: 99%