Multiplicity of the red supergiant population in the young massive cluster NGC 330

Patrick, L. R.; Lennon, D. J.; Evans, C. J.; Sana, H.; Bodensteiner, J.; Britavskiy, N.; Dorda, R.; Herrero, A.; Negueruela, I.; Koter, A. de

doi:10.1051/0004-6361/201936741

Cited by 25 publications

(27 citation statements)

References 98 publications

(142 reference statements)

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“…We note that the isochrones reproduce the position of the RSGs and BSGs in the CMD very well. Patrick et al (2020) estimate the age of NGC 330 based on the population of RSGs (see also Britavskiy et al 2019). They find a cluster age of 45 ± 5 Myr, which agrees well with what is presented here.…”

Section: Color Magnitude Diagramsupporting

confidence: 85%

“…The 11 RSGs in NGC 330 are studied in greater detail in Patrick et al (2020), who derive spectral types following the classification criteria and method detailed in Dorda et al (2018). We adopted their spectral type classifications and include them in Table 2.…”

Section: Red and Blue Supergiantsmentioning

confidence: 99%

“…A more certain classification as Arp (1959, A59) and Robertson (1974, R74). Literature spectral types are from Patrick et al (2020, Feast & Black (1980, FB80) spectroscopic binary will only be possible when periodic radial velocity shifts are detected. In total, we find 36 candidate spectroscopic binaries in our sample.…”

Section: Spectroscopic Binariesmentioning

confidence: 99%

“…This cluster is situated in the Small Magellanic Cloud (SMC) at a distance of 60 ± 1 kpc (Harries et al 2003;Hilditch et al 2005;Deb & Singh 2010). Age estimates of NGC 330 vary between 26 and 45 Myr, which places it in the age range of interest for our purposes (Sirianni et al 2002;Martayan et al 2007b;Milone et al 2018;Patrick et al 2020) Several spectroscopic studies of the brightest stars in NGC 330 were conducted in the past, reporting a high Be star fraction of about 50% or higher (Feast 1972;Grebel et al 1992Grebel et al , 1996Lennon et al 1993;Mazzali et al 1996;Keller & Bessell 1998;Keller et al 1999). Based on these findings, Maeder et al (1999) concluded that the Be star fraction in the SMC is higher than that in the Large Magellanic Cloud and in the Milky Way.…”

Section: Introductionmentioning

confidence: 99%

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The young massive SMC cluster NGC 330 seen by MUSE

Bodensteiner

Sana

Wang

et al. 2021

A&A

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Context. Observations of massive stars in open clusters younger than ∼8 Myr have shown that a majority of them are in binary systems, most of which will interact during their life. While these can be used as a proxy of the initial multiplicity properties, studying populations of massive stars older than ∼20 Myr allows us to probe the outcome of these interactions after a significant number of systems have experienced mass and angular momentum transfer and may even have merged. Aims. Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity properties of the massive-star population in the dense core of the ∼40 Myr old cluster NGC 330 in the Small Magellanic Cloud in order to search for possible imprints of stellar evolution on the multiplicity properties. Methods. We obtained six epochs of VLT/MUSE observations operated in wide-field mode with the extended wavelength setup and supported by adaptive optics. We extracted spectra and measured radial velocities for stars brighter than mF814W = 19. We identified single-lined spectroscopic binaries through significant RV variability with a peak-to-peak amplitude larger than 20 km s−1. We also identified double-lined spectroscopic binaries, and quantified the observational biases for binary detection. In particular, we took into account that binary systems with similar line strengths are difficult to detect in our data set. Results. The observed spectroscopic binary fraction among stars brighter than mF814W = 19 (approximately 5.5 M⊙ on the main sequence) is fSBobs = 13.2 ± 2.0%. Considering period and mass ratio ranges from log(P) = 0.15−3.5 (about 1.4 to 3160 d), q = 0.1−1.0, and a representative set of orbital parameter distributions, we find a bias-corrected close binary fraction of fcl = 34−7+8%. This fraction seems to decline for the fainter stars, which indicates either that the close binary fraction drops in the B-type domain, or that the period distribution becomes more heavily weighted toward longer orbital periods. We further find that both fractions vary strongly in different regions of the color-magnitude diagram, which corresponds to different evolutionary stages. This probably reveals the imprint of the binary history of different groups of stars. In particular, we find that the observed spectroscopic binary fraction of Be stars (fSBobs = 2 ± 2%) is significantly lower than that of B-type stars (fSBobs = 9 ± 2%). Conclusions. We provide the first homogeneous radial velocity study of a large sample of B-type stars at a low metallicity ([Fe/H] ≲ −1.0). The overall bias-corrected close binary fraction (log(P) < 3.5 d) of the B-star population in NGC 330 is lower than the fraction reported for younger Galactic and Large Magellanic Cloud clusters in previous works. More data are needed, however, to establish whether the observed differences are caused by an age or a metallicity effect.

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Section: Color Magnitude Diagramsupporting

confidence: 85%

Section: Red and Blue Supergiantsmentioning

confidence: 99%

Section: Spectroscopic Binariesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The young massive SMC cluster NGC 330 seen by MUSE

Bodensteiner

Sana

Wang

et al. 2021

A&A

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“…Zapartas et al 2017). Observationally, ∼ 30% of RSGs are inferred to have a companion star in a wide orbit (Patrick et al 2019(Patrick et al , 2020. Although binary RSGs (RSG+RSG) have not been directly observed yet (Neugent et al 2020), there is no strong reason why they should not exist.…”

Section: Introductionmentioning

confidence: 99%

Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A

Hirai

Sato

Podsiadlowski

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We explore a new scenario for producing stripped-envelope supernova progenitors. In our scenario, the stripped-envelope supernova is the second supernova of the binary, in which the envelope of the secondary was removed during its red supergiant phase by the impact of the first supernova. Through 2D hydrodynamical simulations, we find that ∼50–90 % of the envelope can be unbound as long as the pre-supernova orbital separation is ≲ 5 times the stellar radius. Recombination energy plays a significant role in the unbinding, especially for relatively high mass systems (≳ 18 M⊙). We predict that more than half of the unbound mass should be distributed as a one-sided shell at about ∼10–100 pc away from the second supernova site. We discuss possible applications to known supernova remnants such as Cassiopeia A, RX J1713.7-3946, G11.2-0.3, and find promising agreements. The predicted rate is ∼0.35–1% of the core-collapse population. This new scenario could be a major channel for the subclass of stripped-envelope or type IIL supernovae that lack companion detections like Cassiopeia A.

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The Young Massive Small Magellanic Cloud Cluster NGC 330 Observed with MUSE

Bodensteiner

2022

Observational Imprints of Binary Evolution on B- And Be-Star Populations

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Multiplicity of the red supergiant population in the young massive cluster NGC 330

Cited by 25 publications

References 98 publications

The young massive SMC cluster NGC 330 seen by MUSE

The young massive SMC cluster NGC 330 seen by MUSE

Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A

The Young Massive Small Magellanic Cloud Cluster NGC 330 Observed with MUSE

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