2007
DOI: 10.1051/0004-6361:20077186
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Abstract: Aims. We investigate the nature of the X-ray point source population within the Young Massive Cluster Westerlund 1. Methods. Chandra observations of 18 ks and 42 ks were used to determine the X-ray properties of emitters within Wd 1, while a comprehensive multiwavelength dataset was employed to constrain their nature. Results. We find X-ray emission from a multitude of different stellar sources within Wd 1, including both evolved high mass and low mass pre-MS stars. We attribute the X-ray emission from the hig… Show more

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Cited by 87 publications
(212 citation statements)
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References 91 publications
(137 reference statements)
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“…Taken together they raise the possibility that it could be physically associated with the putative star formation complex, with AX J1841.3−0455 located ∼equidistantly between RSGC2 and 3, and directly within the region identified by Garzón et al (1997) and López-Corredoira et al (1999) as showing a significant overdensity of "field" RSGs. The expected rate of SNe for such a complex would be fully consistent with the relative youth expected of magnetars (Thompson et al 2000), while SGR 1900+14 demonstrates that their progenitors can have masses as low as ∼15 M (Clark et al 2008;Davies et al in prep. ), also consistent with the current RSG population at the base of the Scutum Crux arm.…”
Section: Association With X-ray Binaries and Post Sne Compact Objectssupporting
confidence: 53%
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“…Taken together they raise the possibility that it could be physically associated with the putative star formation complex, with AX J1841.3−0455 located ∼equidistantly between RSGC2 and 3, and directly within the region identified by Garzón et al (1997) and López-Corredoira et al (1999) as showing a significant overdensity of "field" RSGs. The expected rate of SNe for such a complex would be fully consistent with the relative youth expected of magnetars (Thompson et al 2000), while SGR 1900+14 demonstrates that their progenitors can have masses as low as ∼15 M (Clark et al 2008;Davies et al in prep. ), also consistent with the current RSG population at the base of the Scutum Crux arm.…”
Section: Association With X-ray Binaries and Post Sne Compact Objectssupporting
confidence: 53%
“…Motivated by the hypothesis that RSGC1-3 delineate a star forming complex, we extended this search to this region (l = 25−30 • , b = ±1 • ), but again found no accreting X-ray binaries within it for a distance of 6±1kpc. Given the increasing evidence for a high binary fraction amongst massive stars (e.g., Clark et al 2008), the absence of any Be/X-ray binaries -systems consisting of a B0-3 V-IIIe primary and a neutron star accretor -is surprising, since one would expect them to be active at such an epoch (10-20 Myr; e.g., Portegies Zwart & Verbunt 1996). Nevertheless, one might suppose that a combination of their transient nature plus a SNe kick sufficient to either disrupt or rapidly eject a surviving binary from the complex may explain their lack of detection.…”
Section: Association With X-ray Binaries and Post Sne Compact Objectsmentioning
confidence: 99%
“…Wd1-30a, -36 and -53; Clark et al 2008;Ritchie et al, in prep. ) that provide a rich reservoir of progenitors from which systems such as Wd1-5, -13 and -44 may be drawn.…”
Section: Evolutionary Pathways For Massive Stars In Wd1mentioning
confidence: 99%
“…No other magnetar or young cooling neutron star candidate that could have formed the requisite companion to Wd1-5 has been identified in either the original dataset or subsequent multi-epoch X-ray observations (Muno et al 2006a;Clark et al 2008;Woods et al 2011). Conversely, despite extensive optical and near-IR surveys Crowther et al 2006a), no other plausible pre-SN binary companion to J1647-45 has been identified within the massive stellar population of Wd1.…”
Section: A Physical Connection Between Wd1-5 and Cxou J1647-45?mentioning
confidence: 99%
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