The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

Elson, Rebecca A. W.; Sigurd̵sson, Steinn; Davies, Melvyn B.; Hurley, Jarrod R.; Gilmore, G.

doi:10.1046/j.1365-8711.1998.01948.x

Cited by 69 publications

(100 citation statements)

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“…In order to simulate the effect of unresolved binaries to the modeled sequence of 4 Myr old PMS stars we randomly applied a brightening of no more than V ' 1 mag and a reddening P0.13 mag, assuming different binary fractions. It is worth noting that Elson et al (1998) measured a binary fraction in the young rich LMC cluster NGC 1818, and found 35% AE 5% in the core. This is roughly comparable to the Galactic values that are considered here.…”

Section: Simulation Of the Observed Pms Broadeningmentioning

confidence: 99%

NGC 346 in the Small Magellanic Cloud. III. Recent Star Formation and Stellar Clustering Properties in the Bright HiiRegion N66

Hennekemper

Gouliermis

Henning

et al. 2008

ApJ

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In the third part of our photometric study of the star-forming region NGC 346/ N66 and its surrounding field in the Small Magellanic Cloud (SMC), we focus on the large number of low-mass pre-main-sequence (PMS) stars revealed by the Hubble Space Telescope observations with the Advanced Camera for Surveys. We investigate the origin of the observed broadening of the PMS population in the V À I; V color-magnitude diagram. The most likely explanations are either the presence of differential reddening or an age spread among the young stars. Assuming the latter, simulations indicate that we cannot exclude the possibility that stars in NGC 346 might have formed in two distinct events occurring about 10 and 5 Myr ago, respectively. We find that the PMS stars are not homogeneously distributed across NGC 346, but instead are grouped in at least five different clusters. On spatial scales from 0.8 00 to 8 00 (0.24Y2.4 pc at the distance of the SMC) the clustering of the PMS stars as computed by a two-point angular correlation function is self-similar with a power-law slope % À0:3. The clustering properties are quite similar to Milky Way star-forming regions like Orion OB or Oph. Thus molecular cloud fragmentation in the SMC seems to proceed on the same spatial scales as in the Milky Way. This is remarkable given the differences in metallicity and hence dust content between SMC and Milky Way star-forming regions.

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Section: Simulation Of the Observed Pms Broadeningmentioning

confidence: 99%

NGC 346 in the Small Magellanic Cloud. III. Recent Star Formation and Stellar Clustering Properties in the Bright HiiRegion N66

Hennekemper

Gouliermis

Henning

et al. 2008

ApJ

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“…The accurate measurement of the properties and structure of many populous star clusters also became possible (e.g. Mighell et al 1996; Elson et al 1998; Rich et al 2000; Rich, Shara & Zurek 2001; Gouliermis et al 2004; Kerber, Santiago & Brocato 2007).…”

Section: Introductionmentioning

confidence: 99%

“…Binary fraction f b : Elson et al (1998), using the shape of the main sequence in a deep CMD (obtained with the HST ) for the LMC cluster NGC 1818, determined a binary fraction from ∼0.20 to ∼0.35, from the centre to the outer parts of the cluster. These binary fractions refer only to binaries with a high primary/secondary mass ratio, say of above 0.7, because these are the only ones that separate clearly from the single‐star main sequence in CMDs.…”

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confidence: 99%

The star-formation history of the Small Magellanic Cloud star cluster NGC 419

Rubele

Kerber

Girardi

2010

Monthly Notices of the Royal Astronomical Society

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The rich Small Magellanic Cloud (SMC) star cluster NGC 419 has recently been found to present both a broad main‐sequence turn‐off and a dual red clump of giants in the sharp colour–magnitude diagrams (CMDs) derived from the High‐Resolution Channel of the Advanced Camera for Surveys onboard the Hubble Space Telescope. In this work, we apply to the NGC 419 data the classical method of star‐formation‐history (SFH) recovery through CMD reconstruction, deriving for the first time this function for a star cluster with multiple turn‐offs. The values for the cluster metallicity, reddening, distance and binary fraction were varied within the limits allowed by present observations. The global best‐fitting solution is an excellent fit to the data, reproducing all the CMD features with striking accuracy. The corresponding star‐formation rate is provided together with estimates of its random and systematic errors. Star formation is found to last for at least 700 Myr, and to have a marked peak in the middle of this interval, for an age of 1.5 Gyr. Our findings argue in favour of multiple star‐formation episodes (or continuous star formation) being at the origin of the multiple main‐sequence turn‐offs in Magellanic Cloud clusters with ages of about 1 Gyr. It remains to be tested whether alternative hypotheses, such as a main‐sequence spread caused by rotation, could produce similarly good fits to the data.

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“…Elson et al 1998;Hu et al 2010, and references therein), interestingly, the places where the youngest most massive stars are likely to reside. This is intuitively exemplified by the much higher fraction of low-and high-mass X-ray binaries found in both globular clusters and actively star-forming regions (e.g.…”

Section: Binary Star Scenariosmentioning

confidence: 99%

Gamma-Ray Burst Progenitors

Levan¹,

Crowther²,

Grijs³

et al. 2016

Gamma-Ray Bursts

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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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The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

Cited by 69 publications

References 0 publications

NGC 346 in the Small Magellanic Cloud. III. Recent Star Formation and Stellar Clustering Properties in the Bright HiiRegion N66

NGC 346 in the Small Magellanic Cloud. III. Recent Star Formation and Stellar Clustering Properties in the Bright HiiRegion N66

The star-formation history of the Small Magellanic Cloud star cluster NGC 419

Gamma-Ray Burst Progenitors

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