Revised Stellar Temperatures for Magellanic Cloud O Supergiants from Far Ultraviolet Spectroscopic Explorer and Very Large Telescope UV-Visual Echelle Spectrograph Spectroscopy

By P. Crowther, D. John Hillier, Christopher H. Evans, A. Fullerton, O. De Marco, A. Willis. 2002

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In Astronomy and Astrophysics

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Mass loss from hot massive stars (2008, methodology): “This scenario, however, would not only fail to produce the many RSG stars observed, but there is also observational evidence againstall WR-stars being in close binary systems (only 30-40% in the Magellanic Clouds, Foellmi et al 2003a,b).”
A Tale of Two Stars: The Extreme O7 Iaf+ Supergiant AV 83 and the OC7.5 III((f)) star AV 69 (2003, methodology): “As noted by Crowther et al. (2002), this makes the P v doublet an extremely useful clumping diagnostic, provided we have an independent estimate of its SMC abundance.”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, methodology): “For the Milky Way, LMC, and SMC, various studies using modern non-LTE analysis find fcl ≃ 10 (Crowther et al. 2002, Evans et al. 2004, Figer et al. 2002, Hillier et al. 2003, Massa et al. 2003, Puls et al. 2006), corresponding to Ṁ reductions by a factor of ∼3 with typical uncertainties of ∼30%.”
Stellar and wind properties of massive stars in the central parsec of the Galaxy (2006, background): “To name a few, their effective temperatures are lower (Martins et al. 2002; Crowther et al. 2002; Repolust et al. 2004) and their winds are highly clumped (Hillier et al. 2003; Bouret et al. 2005; Fullerton et al. 2006).”
Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars (2004, methodology): “The first evidences of wind clumping were found in WR stars for which small filling factors (f∞ ≈ 0.1) were derived too (Hamann & Koesterke 1998; Hillier & Miller 1999; Crowther et al. 2002a).”
The Discordance of Mass-Loss Estimates for Galactic O-Type Stars (2005, methodology): “Thus, the values of the derived stellar parameters for the primary sample are internally consistent and incorporate recent revisions to the temperature scale associated with O-type stars (Martins et al. 2002, 2005; Crowther et al. 2002; Bianchi & Garcia 2002; Herrero et al. 2002).”
The VLT-FLAMES survey of massive stars: observations centered on the Magellanic Cloud clusters NGC 330, NGC 346, NGC 2004, and the N11 region (2006, methodology): “A detailed atmospheric analysis of a VLT-UVES spectrum of this star was given by Crowther et al. (2002).”
The VLT-FLAMES survey of massive stars: evolution of surface N abundances and effective temperature scales in the Galaxy and Magellanic Clouds (2007, background): “17 line blanketing and non-LTE effects in the model atmospheres (Martins et al. 2002; Crowther et al. 2002, 2006; Massey et al. 2004, 2005).”
Stellar and wind parameters of Galactic O-stars - The influence of line-blocking/blanketing (2004, methodology): “Crowther et al. (2002) have presented an analysis of four supergiants in the LMC and SMC with similar but stronger trends, and Herrero et al. (2002) have analyzed seven Cyg OB2 stars by means of the latest, lineblanketed version of .”
The most massive stars in the Arches cluster (2007, background): “As previously recalled, we note however that recent studies indicate smallerf for O supergiants (Crowther et al. 2002a; Hillier et al. 2003; Bouret et al. 2005).”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, background): “WNL stars have similar effective temperatures and surface compositions as typical O-supergiants (see e.g. Crowther et al. 2002) but they show much stronger wind emission lines.”
The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars and Results from the Complete Sample (2005, background): “…may be too hot by as much as ∼ 20% (see, for example, Martins et al. 2002, Bianchi & Garcia 2002, Garcia & Bianchi 2004, and Repolust et al. 2004), while the results for the Magellanic Clouds are mixed (compare Crowther et al. 2002, Bouret et al. 2003, Hillier et al. 2003, and Martins et al. 2004).”
O stars with weak winds: the Galactic case (2005, methodology): “This effect is now well known and has been highlighted by several studies (Martins et al. 2002a, 2005, Crowther et al. 2002, Markova et al. 2004).”
The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters (2016, unknown): “C86: Conti, Garmany & Massey 1986; C02: Crowther et al. 2002; CW11: Crowther & Walborn 2011; CN16: Caballero-Nieves et al. (in preparation); G80: Gondhalekar et al. 1980; M03: Massa et al. 2003; M04: Massey et al. 2004; M05: Massey et al. 2005; M09: Massey et al. 2009; PC98: Prinja & Crowther 1998; ”
UBVJHK synthetic photometry of Galactic O stars (2006, background): “…allows realistic prediction of atmospheric structures andemergent spectra which are used to get quantitative constraints on the properties of massive stars (Crowther et al., 2002; Hillier et al., 2003; Bouret et al., 2003; Martins et al., 2004; Repolust, Puls & Herrero, 2004; Martins et al., 2005).”
On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars and Population III Stars (2006, background): “…of 10–20 or more from traditional mass-loss rates, while Bouret et al. (2005) require reductions by factors of 3 or more (see also Puls et al. 2006; Crowther et al. 2002; Hillier et al. 2003; Massa et al. 2003; Evans et al. 2004).3 In any case, large reductions in Ṁ are also needed to match the…”
The VLT-FLAMES Survey of Massive Stars: Observations in the Galactic Clusters NGC 3293, NGC 4755 and NGC 6611 ⋆ (2005, methodology): “In anticipation of the fact that the simultaneous arcs were disabled for the majority of our FLAMES observations in the Magellanic Clouds (because of the overspill discussed in Sect.”