Ruprecht 147 DANCe

Olivares, J.; Bouy, H.; Sarro, L. M.; Miret-Roig, N.; Berihuete, A.; Bertin, E.; Barrado, D.; Huélamo, N.; Tamura, Motohide; Allen, Lori; Beletsky, Y.; Serre, Solveig; Cuillandre, Jean-Charles

doi:10.1051/0004-6361/201834924

Cited by 34 publications

(44 citation statements)

References 47 publications

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“…In this way we obtained E(B − V ) = 0.126 ± 0.023 mag, corresponding to A V = 0.391 ± 0.071 mag for a ratio of total to selective extinction of R V = 3.1. This is in good agreement with the value of E(B − V ) = 0.112 ± 0.029 mag derived in our earlier study of the Ruprecht 147 eclipsing system EPIC 219394517, and also with independent estimates for the cluster by Bragaglia et al (2018) and Olivares et al (2019).…”

Section: Absolute Dimensionssupporting

confidence: 92%

Eclipsing Binaries in the Open Cluster Ruprecht 147. II. Epic 219568666

Torres¹,

Vanderburg²,

Curtis³

et al. 2019

ApJ

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We report our spectroscopic monitoring of the detached, grazing, and slightly eccentric 12-day doublelined eclipsing binary EPIC 219568666 in the old nearby open cluster Ruprecht 147. This is the second eclipsing system to be analyzed in this cluster, following our earlier study of EPIC 219394517. Our analysis of the radial velocities combined with the light curve from the K2 mission yield absolute masses and radii for EPIC 219568666 of M 1 = 1.121 ± 0.013 M ⊙ and R 1 = 1.1779 ± 0.0070 R ⊙ for the F8 primary, and M 2 = 0.7334 ± 0.0050 M ⊙ and R 2 = 0.640 ± 0.017 R ⊙ for the faint secondary. Comparison with current stellar evolution models calculated for the known metallicity of the cluster points to a primary star that is oversized, as is often seen in active M dwarfs, but this seems rather unlikely for a star of its mass and with a low level of activity. Instead, we suspect a subtle bias in the radius ratio inferred from the photometry, despite our best efforts to avoid it, which may be related to the presence of spots on one or both stars. The radius sum for the binary, which bypasses this possible problem, indicates an age of 2.76 ± 0.61 Gyr that is in good agreement with a similar estimate from the binary in our earlier study.

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Section: Absolute Dimensionssupporting

confidence: 92%

Eclipsing Binaries in the Open Cluster Ruprecht 147. II. Epic 219568666

Torres¹,

Vanderburg²,

Curtis³

et al. 2019

ApJ

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“…We present in this section our strategy to search for new members of the Corona-Australis star-forming region based on the algorithm developed by Sarro et al (2014), which was later modified by Olivares et al (2019). Briefly, the methodology models the field and cluster populations using Gaussian mixture models (GMM) in a representation space that takes proper motions, parallaxes, and multi-band photometry together with the corresponding uncertainties and correlations (when available).…”

Section: Membership Analysismentioning

confidence: 99%

“…The three photometric bands (G, G BP , G RP ) given in Gaia-DR2 allowed us to construct colour-magnitude diagrams (CMD) using different combinations of them. We ran a random-forest classifier (as described by Olivares et al 2019) to measure the relative importance of the photometric features (i.e. magnitudes and colours).…”

Section: Representation Spacementioning

confidence: 99%

“…Once our solution converged, we generated a synthetic dataset and defined the optimum probability threshold p opt (as described in Sect. 4.2.7 of Olivares et al 2019) to perform a final classification of all sources in the field into cluster members (i.e. prob.…”

Section: Field and Cluster Modelmentioning

confidence: 99%

“…In Sect. 2 we describe our membership analysis to search for new members in Corona-Australis based on the methodology previously developed by our team (Sarro et al 2014;Olivares et al 2019). Section 3 is dedicated to the characterisation of the newly identified members in this study.…”

Section: Introductionmentioning

confidence: 99%

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Corona-Australis DANCe

Galli

Bouy

Olivares

et al. 2020

A&A

Self Cite

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Context. Corona-Australis is one of the nearest regions to the Sun with recent and ongoing star formation, but the current picture of its stellar (and substellar) content is not complete yet. Aims. We take advantage of the second data release of the Gaia space mission to revisit the stellar census and search for additional members of the young stellar association in Corona-Australis. Methods. We applied a probabilistic method to infer membership probabilities based on a multidimensional astrometric and photometric data set over a field of 128 deg2 around the dark clouds of the region. Results. We identify 313 high-probability candidate members to the Corona-Australis association, 262 of which had never been reported as members before. Our sample of members covers the magnitude range between G ≳ 5 mag and G ≲ 20 mag, and it reveals the existence of two kinematically and spatially distinct subgroups. There is a distributed “off-cloud” population of stars located in the north of the dark clouds that is twice as numerous as the historically known “on-cloud” population that is concentrated around the densest cores. By comparing the location of the stars in the HR-diagram with evolutionary models, we show that these two populations are younger than 10 Myr. Based on their infrared excess emission, we identify 28 Class II and 215 Class III stars among the sources with available infrared photometry, and we conclude that the frequency of Class II stars (i.e. “disc-bearing” stars) in the on-cloud region is twice as large as compared to the off-cloud population. The distance derived for the Corona-Australis region based on this updated census is d = 149.4 +0.4−0.4 pc, which exceeds previous estimates by about 20 pc. Conclusions. In this paper we provide the most complete census of stars in Corona-Australis available to date that can be confirmed with Gaia data. Furthermore, we report on the discovery of an extended and more evolved population of young stars beyond the region of the dark clouds, which was extensively surveyed in the past.

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The origin of free-floating planets

Miret-Roig

2023

Astrophys Space Sci

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Free-floating planets (FFPs) are the lightest products of star formation and they carry important information on the initial conditions of the environment in which they were formed. They were first discovered in the 2000 s but still few of them have been identified and confirmed due to observational challenges. This is a review of the last advances in the detection of these objects and the understanding of their origin. Several studies indicate that the observed fraction of FFPs outnumbers the prediction of turbulent fragmentation and suggest that many were formed in planetary systems that were later abandoned. The JWST will certainly constitute a new step further in the detection and characterisation of FFPs. To interpret these new observations, precise ages for the nearby star-forming regions in which they were formed will be necessary.

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Ruprecht 147 DANCe

Cited by 34 publications

References 47 publications

Eclipsing Binaries in the Open Cluster Ruprecht 147. II. Epic 219568666

Eclipsing Binaries in the Open Cluster Ruprecht 147. II. Epic 219568666

Corona-Australis DANCe

The origin of free-floating planets

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