The Runaways and Isolated O-Type Star Spectroscopic Survey of the SMC (Riots4)*

Lamb, J. B.; Oey, M. S.; Segura-Cox, Dominique; Graus, Andrew S.; Kiminki, Daniel C.; Golden-Marx, Jesse B.; Parker, J. W.

doi:10.3847/0004-637x/817/2/113

Cited by 53 publications

(82 citation statements)

References 79 publications

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“…A large fraction of the sample shows emission in the Balmer lines (Sect. 4), owing to their Oe/Be nature (e.g., Golden-Marx et al 2016;Lamb et al 2016). We manually trim out the core of the Balmer lines when emission is detected by visual inspection of each spectrum.…”

Section: Stellar Spectroscopic Analysismentioning

confidence: 99%

“…We find that the population of stars at log T eff [K] ≤ 4.3 largely corresponds to emission-line stars. There are 73 classical Be stars, as classified by Lamb et al (2016) at these temperatures. Figure 8 highlights the close correspondence between the position of the stars in the sHRD and the presence/absence of emission in the Balmer lines.…”

Section: Assignment Of Be Stars In the Shrdmentioning

confidence: 99%

“…Figure 11. The log T eff [K] obtained from spectroscopic analysis vs observed spectral type for the RIOTS4 sample classified by Lamb et al (2016). The stars at log T eff [K] < 4.3 generate a bimodality in spectral type due to being misplaced in log T eff [K].…”

Section: Assignment Of Be Stars In the Shrdmentioning

confidence: 99%

“…The Small Magellanic Cloud (SMC), due to its proximity (63 kpc, Graczyk et al 2014;Scowcroft et al 2016) and low metal content (Z/Z ∼ 0.2, e.g., Trundle et al 2007), is the best laboratory for this endeavor, and also extending the work of Castro et al (2014). The Runaways and Isolated O-Type Star Spectroscopic Survey of the Small Magellanic Cloud (RIOTS4; Lamb et al 2016) covers a large sample of field massive stars and provides an excellent spectroscopic sample to dissect the evolution of massive stars at the SMC metallicity. Here, we analyze the spectra of a large fraction of stars published by Lamb et al (2016) and new targets observed during multi-epoch follow-ups in the SMC Wing carried out within the same project.…”

Section: Introductionmentioning

confidence: 99%

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The spectroscopic Hertzsprung-Russell diagram of Galactic massive stars

Castro

Fossati

Langer

et al. 2014

A&A

130

181

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The distribution of stars in the Hertzsprung-Russell diagram narrates their evolutionary history and directly assesses their properties. Placing stars in this diagram however requires the knowledge of their distances and interstellar extinctions, which are often poorly known for Galactic stars. The spectroscopic Hertzsprung-Russell diagram (sHRD) tells similar evolutionary tales, but is independent of distance and extinction measurements. Based on spectroscopically derived effective temperatures and gravities of almost 600 stars, we derive for the first time the observational distribution of Galactic massive stars in the sHRD. While biases and statistical limitations in the data prevent detailed quantitative conclusions at this time, we see several clear qualitative trends. By comparing the observational sHRD with different state-of-the-art stellar evolutionary predictions, we conclude that convective core overshooting may be massdependent and, at high mass ( > ∼ 15 M ), stronger than previously thought. Furthermore, we find evidence for an empirical upper limit in the sHRD for stars with T eff between 10 000 and 32 000 K and, a strikingly large number of objects below this line. This over-density may be due to inflation expanding envelopes in massive main-sequence stars near the Eddington limit.

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Section: Stellar Spectroscopic Analysismentioning

confidence: 99%

Section: Assignment Of Be Stars In the Shrdmentioning

confidence: 99%

Section: Assignment Of Be Stars In the Shrdmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The spectroscopic Hertzsprung-Russell diagram of Galactic massive stars

Castro

Fossati

Langer

et al. 2014

A&A

130

181

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“…Similarly, no examples of rapid rotators are observed in N66 (Mokiem et al 2006). Lamb et al (2016) identify a large population of SMC field Oe stars, presumably arising from rapid rotation, although these too may result from close binary evolution. This in itself raises interesting questions, since if a significant population of sufficiently massive and low metallicity stars can be identified in the local Universe, but essentially none of these appear as viable GRB progenitors then the fraction of massive low metallicity stars creating GRBs must be small.…”

Section: O Starsmentioning

confidence: 99%

Gamma-Ray Burst Progenitors

et al. 2016

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We review our current understanding of the progenitors of both long and short duration gamma-ray bursts (GRBs). Constraints can be derived from multiple directions, and we use three distinct strands; (i) direct observations of GRBs and their host galaxies, (ii) parameters derived from modelling, both via population synthesis and direct numerical simulation and (iii) our understanding of plausible analog progenitor systems observed in the local Universe. From these joint constraints, we describe the likely routes that can drive massive stars to the creation of long GRBs, and our best estimates of the scenarios that can create compact object binaries which will ultimately form short GRBs, as well as the associated rates of both long and short GRBs. We further discuss how different the progenitors may be in the case of black hole engine or millisecond-magnetar models for the production of GRBs, and how central engines may provide a unifying theme between many classes of extremely luminous transient, from luminous and super-luminous supernovae to long and short GRBs.

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