On the massive stellar population of the super star cluster Westerlund 1
By J. Clark, I. Negueruela, P. Crowther, S. Goodwin. 2005
211 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/889c420ca23047c8614adeac72f6b0d2cb225612
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Citations in the corpus
- TOWARD A UNIFICATION OF STAR FORMATION RATE DETERMINATIONS IN THE MILKY WAY AND OTHER GALAXIES (2011, background): “Prominent excluded clusters include Westerlund 1, one of the most massive young clusters in the Milky Way (Clark et al. 2005), and several Red Supergiant Clusters (Figer et al. 2006; Davies et al. 2007; Alexander et al. 2009), all of which contain significant populations of Wolf-Rayet stars, yellow…”
- MOLECULAR CLOUDS TOWARD THE SUPER STAR CLUSTER NGC 3603; POSSIBLE EVIDENCE FOR A CLOUD–CLOUD COLLISION IN TRIGGERING THE CLUSTER FORMATION (2013, unknown): “– 25 – – 26 – – 27 – – 28 – – 29 – – 30 – – 31 – – 32 – – 33 – – 34 – – 35 – – 36 – – 38 – (2008); 7, Clark et al. (2010, 2005); reference2 shows paper of molecular clouds; 8 Furukawa et al. (2009b); Ohama et al. (2010) – 39 – – 40 – Note.”
- SPITZER SAGE INFRARED PHOTOMETRY OF MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD (2009, background): “…a distance of 48.1 kpc; Macri et al. 2006), and 8 pc in M33 (at a distance of 964 kpc; Bonanos et al. 2006), while typical OB associations have sizes of tens of parsecs (but half-light radii of several parsecs), and young massive clusters can have sizes smaller than a parsec (Clark et al. 2005).”
- Gas expulsion and the destruction of massive young clusters (2006, unknown): “…found in merging and interacting galaxies such as NGC 7252 (Miller et al. 1997) and NGC 6745 (de Grijs et al. 2003),1 as well as the Large Magellanic Cloud (LMC) (Elson, Fall & Freeman 1989; Elson 1991; Mackey & Gilmore 2003), and even within our own Galaxy (especially Wd 1, see Clark et al. 2005).”
- Discovery of an Extraordinarily Massive Cluster of Red Supergiants (2006, background): “The cluster mass is extraordinary, perhaps trailing only Westerlund 1, as the most massive young cluster in the Galaxy (Clark et al. 2005).”
- A Neutron Star with a Massive Progenitor in Westerlund 1 (2005, background): “This is consistent with the range measured for other cluster members, NH = [1.4 − 2.9] × 1022 cm−2, where the dispersion can be accounted for by variable extinction caused by a foreground molecular cloud (see Clark et al. 2005).”
- A Massive Cluster of Red Supergiants at the Base of the Scutum-Crux Arm (2007, background): “Until recently, only Westerlund 1 [Wd 1; Clark et al. 2005), the Arches Cluster (Figer et al. 2002), the Quintuplet Cluster (Figer et al. 1999), and the Galactic center (GC) cluster (Figer et al. 2004) were known to be massive enough and young enough to harbor statistically significant numbers of…”
- Young Massive Star Clusters (2010, background): “Currently the most massive young cluster known in our Galaxy is Westerlund 1 (Clark et al. 2005).”
- Physical Properties of Wolf-Rayet Stars (2006, background): “Remarkably few Milky Way clusters host both RSG and WR stars, with the notable exception of Westerlund 1 (Clark et al. 2005); this suggests that the mass range common to both populations is fairly narrow.”
- A census of the Wolf–Rayet content in Westerlund 1 from near-infrared imaging and spectroscopy (2006, methodology): “…K-band calibration for our (non-dusty) WR stars to estimate the distance and extinction, revealing ∼5.0 kpc and AKS = 0.96 ± 0.14 mag, in reasonable agreement with previous studies based upon yellow hypergiants and pre-main-sequence stars (Clark et al. 2005; Brandner et al., in preparation).”