The Ara OB1a association

Baume, G.; Carraro, G.; Comerón, F.; Elía, G. C. de

doi:10.1051/0004-6361/201015497

Cited by 20 publications

(22 citation statements)

References 37 publications

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“…However, they warn that their age estimates might be significantly affected by the uncertainties in the birthline for G‐type stars (see ). More recently, Baume et al (2011) also found a handful of stars with Hα emission typical of accretors in the 20–30 Myr old cluster NGC 6167.…”

Section: Evolution and Metallicity Dependencymentioning

confidence: 89%

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

Spezzi¹,

Marchi²,

Panagia³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.We present a multiwavelength study of three star-forming regions, spanning the age range 1-14Myr, located between the 30 Doradus complex and supernova SN 1987A in the Large Magellanic Cloud (LMC). We reliably identify about 1000 pre-main-sequence (PMS) star candidates actively undergoing mass accretion and estimate their stellar properties and mass accretion rate (M). Our measurements represent the largest M data set of low-metallicity stars presented so far. As such, they offer a unique opportunity to study on a statistical basis the mass accretion process in the LMC and, more in general, the evolution of the mass accretion process around low-metallicity stars. We find that the typical M of PMS stars in the LMC is higher than for galactic PMS stars of the same mass, independently of their age. Taking into account the caveats of isochronal age and M estimates, the difference in M between the LMC and our Galaxy appears to be about an order of magnitude. We review the main mechanisms of disc dispersal and find indications that typically higher M are to be expected in low-metallicity environments. However, many issues of this scenario need to be clarified by future observations and modelling. We also find that, in the mass range 1-2M ⊙, M of PMS stars in the LMC increases with stellar mass as M ∝ M * b, with b≈ 1, i.e. slower than the second power law found for galactic PMS stars in the same mass regim

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Section: Evolution and Metallicity Dependencymentioning

confidence: 89%

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

Spezzi¹,

Marchi²,

Panagia³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Baume et al (2011), (2) Mel'nik & Dambis (2017), (3) Molina-Lera et al (2016), (4) Shull & Danforth (2019), (5) Chené et al (2019), (6) de la Fuente et al (2016), (7) Kurtev et al (2007), (8) Franciosini et al (2018) Gaia DR2 parallaxes. We also note the bulk of objects in our sample are between 2 and 4 kpc.…”

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confidence: 99%

Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – II. Cluster and association membership

Rate

Crowther

Parker

2020

Monthly Notices of the Royal Astronomical Society

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Galactic Wolf–Rayet (WR) star membership of star-forming regions can be used to constrain the formation environments of massive stars. Here, we utilize Gaia DR2 parallaxes and proper motions to reconsider WR star membership of clusters and associations in the Galactic disc, supplemented by recent near-infrared studies of young massive clusters. We find that only 18–36 per cent of 553 WR stars external to the Galactic Centre region are located in clusters, OB associations or obscured star-forming regions, such that at least 64 per cent of the known disc WR population are isolated, in contrast with only 13 per cent of O stars from the Galactic O star Catalogue. The fraction located in clusters, OB associations or star-forming regions rises to 25–41 per cent from a global census of 663 WR stars including the Galactic Centre region. We use simulations to explore the formation processes of isolated WR stars. Neither runaways, nor low-mass clusters, are numerous enough to account for the low cluster membership fraction. Rapid cluster dissolution is excluded as mass segregation ensures WR stars remain in dense, well-populated environments. Only low-density environments consistently produce WR stars that appeared to be isolated during the WR phase. We therefore conclude that a significant fraction of WR progenitors originate in low-density association-like surroundings which expand over time. We provide distance estimates to clusters and associations host to WR stars, and estimate cluster ages from isochrone fitting.

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“…The data are of very high quality, and represent a vast improvement over existing near-IR photometry. Therefore they are useful for a wide variety of studies such as open/embedded clusters (Borissova et al 2011;Baume et al 2011), globular clusters Moni Bidin et al 2011), distance scale (Majaess et al 2011), YSO censuses (Faimali et al, in prep. ), brown dwarfs (Folkes et al, in prep.…”

Section: Discussionmentioning

confidence: 99%

VVV DR1: The first data release of the Milky Way bulge and southern plane from the near-infrared ESO public survey VISTA variables in the Vía Láctea

Saito

Hempel

Minniti

et al. 2012

A&A

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346

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Context. The ESO public survey VISTA variables in the Vía Láctea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years. Aims. We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained. Methods. The observations are carried out on the 4-m VISTA telescope in the ZY JHK s filters. In addition to the multi-band imaging the variability monitoring campaign in the K s filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. Results. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZY JHK s filters taken in the 2010 observing season. The typical image quality is ∼0. 9−1. 0. The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHK s images in the disk area and 90% of the JHK s images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28 × 10 8 stellar sources in the bulge and 1.68 × 10 8 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63 × 10 8 stellar sources. About 10% of these are double detections because of overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHK s bands extend typically ∼4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for K s = 15−18 mag has rms ∼ 35−175 mas. Conclusions. The VVV Survey data products offer a unique dataset to map the stellar populations in the Galactic bulge and the adjacent plane and provide an exciting new tool for the study of the structure, content, and star-formation history of our Galaxy, as well as for investigations of the newly discovered star clusters, star-forming regions in the disk, high proper motion stars, asteroids, planetary nebulae, and other interesting objects.

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The Ara OB1a association

Cited by 20 publications

References 37 publications

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – II. Cluster and association membership

VVV DR1: The first data release of the Milky Way bulge and southern plane from the near-infrared ESO public survey VISTA variables in the Vía Láctea

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