The VLT-FLAMES Tarantula Survey

Dunstall, P. R.; Dufton, P. L.; Sana, H.; Evans, C. J.; Howarth, Ian D.; Simón‐Díaz, S.; Mink, S. E. de; Langer, N.; Apellániz, J. Maíz; Taylor, W. D.

doi:10.1051/0004-6361/201526192

Cited by 159 publications

(253 citation statements)

References 37 publications

(39 reference statements)

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“…Although our binary prescription is consistent with Dunstall et al (2015)'s findings, we also tested the hypothesis of a binary population similar to that found by Sana et al (2013) for O-type stars. Figure 11 shows the SFH recovered assuming a binary fraction of 50% and a uniform distribution of q.…”

Section: Binariessupporting

confidence: 80%

Hubble Tarantula Treasury Project. V. The Star Cluster Hodge 301: The Old Face of 30 Doradus*

Cignoni

Sabbi

Marel

et al. 2016

ApJ

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Based on color-magnitude diagrams (CMDs) from the Hubble Space TelescopeHubble Tarantula Treasury Project (HTTP) survey, we present the star formation history of Hodge301, the oldest star cluster in the Tarantula Nebula. The HTTP photometry extends faint enough to reach, for the first time, the cluster pre-main sequence (PMS) turnon, where the PMS joins the main sequence. Using the location of this feature, along with synthetic CMDs generated with the latest PARSEC models, we find that Hodge301 is older than previously thought, with an age between 26.5 and 31.5 Myr. From this age, we also estimate that between 38 and 61 Type II supernovae exploded in the region. The same age is derived from the main sequence turn-off, whereas the age derived from the postmain sequence stars is younger and between 20 and 25 Myr. Other relevant parameters are a total stellar mass of ≈8800±800M e and average reddening E(B − V ) ≈ 0.22-0.24 mag, with a differential reddening δE (B − V )≈0.04 mag.

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Section: Binariessupporting

confidence: 80%

Hubble Tarantula Treasury Project. V. The Star Cluster Hodge 301: The Old Face of 30 Doradus*

Cignoni

Sabbi

Marel

et al. 2016

ApJ

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“…Welty et al 2006;van Loon et al 2013), and, via multi-epoch observations, the binary properties of massive stars (e.g. Bosch et al 2009;Sana et al 2013;Dunstall et al 2015).…”

Section: Introductionmentioning

confidence: 99%

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

Evans

Loon

Hainich

et al. 2015

A&A

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We present spectral classifications from optical spectroscopy of 263 massive stars in the north-eastern region of the Large Magellanic Cloud. The observed two-degree field includes the massive 30 Doradus star-forming region, the environs of SN1987A, and a number of star-forming complexes to the south of 30 Dor. These are the first classifications for the majority (203) of the stars and include eleven double-lined spectroscopic binaries. The sample also includes the first examples of early OC-type spectra (AAΩ 30 Dor 248 and 280), distinguished by the weakness of their nitrogen spectra and by C IV λ4658 emission. We propose that these stars have relatively unprocessed CNO abundances compared to morphologically normal O-type stars, indicative of an earlier evolutionary phase. From analysis of observations obtained on two consecutive nights, we present radial-velocity estimates for 233 stars, finding one apparent single-lined binary and nine (>3σ) outliers compared to the systemic velocity; the latter objects could be runaway stars or large-amplitude binary systems and further spectroscopy is required to investigate their nature.

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“…Direct measurements of the orbital period distribution further confirm the relative abundance of short-period binaries, with at least 20% of all OB-type binaries having a period of less than a week; and 40% to 50%, a period of less than a month Kobulnicky et al 2014;Dunstall et al 2015;Almeida et al 2017).…”

Section: A Lack Of Short-period Systems?mentioning

confidence: 77%

“…This is in stark contrast to the overall properties of small and large samples of fully formed, mainsequence massive stars (Kouwenhoven, et al 2007;Sana et al 2012Sana et al , 2013aKiminki & Kobulnicky 2012;Kobulnicky et al 2014;Dunstall et al 2015;Almeida et al 2017). These works have indeed established that 40% to 50% of OB-type binaries have a period of one month or less, with large RV amplitudes (∆v rad > 100 km s −1 ).…”

Section: Introductionmentioning

confidence: 94%

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A dearth of short-period massive binaries in the young massive star forming region M 17

Sana

Ramírez-Tannus

Koter

et al. 2017

A&A

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Aims. The formation of massive stars remains poorly understood and little is known about their birth multiplicity properties. Here, we aim to quantitatively investigate the strikingly low radial-velocity dispersion measured for a sample of 11 massive pre-and nearmain-sequence stars (σ 1D = 5.6 ± 0.2 km s −1 ) in the very young massive star forming region M 17, in order to obtain first constraints on the multiplicity properties of young massive stellar objects. Methods. We compute the radial-velocity dispersion of synthetic populations of massive stars for various multiplicity properties and we compare the obtained σ 1D distributions to the observed value. We specifically investigate two scenarios: a low binary fraction and a dearth of short-period binary systems. Results. Simulated populations with low binary fractions ( f bin = 0.12 +0.16 −0.09 ) or with truncated period distributions (P cutoff > 9 months) are able to reproduce the low σ 1D observed within their 68%-confidence intervals. Furthermore, parent populations with f bin > 0.42 or P cutoff < 47 d can be rejected at the 5%-significance level. Both constraints are in stark contrast with the high binary fraction and plethora of short-period systems in few Myr-old, well characterized OB-type populations. To explain the difference in the context of the first scenario would require a variation of the outcome of the massive star formation process. In the context of the second scenario, compact binaries must form later on, and the cut-off period may be related to physical length-scales representative of the bloated pre-main-sequence stellar radii or of their accretion disks. Conclusions. If the obtained constraints for the M 17's massive-star population are representative of the multiplicity properties of massive young stellar objects, our results may provide support to a massive star formation process in which binaries are initially formed at larger separations, then harden or migrate to produce the typical (untruncated) power-law period distribution observed in few Myr-old OB binaries.

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The VLT-FLAMES Tarantula Survey

Cited by 159 publications

References 37 publications

Hubble Tarantula Treasury Project. V. The Star Cluster Hodge 301: The Old Face of 30 Doradus*

Hubble Tarantula Treasury Project. V. The Star Cluster Hodge 301: The Old Face of 30 Doradus*

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

A dearth of short-period massive binaries in the young massive star forming region M 17

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