Clusters: Age Scales for Stellar Physics

Barrado, D.

doi:10.1051/eas/1680005

Cited by 12 publications

(7 citation statements)

References 217 publications

(236 reference statements)

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“…Jeffries et al 2014, Binks et al 2022. Additionally, stellar evolution models are especially uncertain at very young ages, making isochrone fitting less ideal for those cases (Barrado 2016). Determining isochronal ages from evolutionary models is beyond the scope of this work, but we still use colour-magnitude diagrams (CMDs) to validate the relative age scale determined in this section (Fig.…”

Section: Validation Of the Age Gradient With Isochrones And Possible ...mentioning

confidence: 99%

The star formation history of Upper Scorpius and Ophiuchus

Miret-Roig

Galli

Olivares

et al. 2022

A&A

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Context. Understanding how star formation begins and propagates through molecular clouds is a fundamental but still open question. One major difficulty in addressing this question is the lack of precise 3D kinematics and age information of young stellar populations. Thanks to Gaia's astrometry, large spectroscopic surveys, and improved age-dating methods, this picture is changing. Aims. We aim to study spatial and kinematic substructures of the region encompassed by Upper Scorpius and Ophiuchus star forming regions. We want to determine dynamical traceback ages and study the star formation history of the complex. Methods. We combined our spectroscopic observations with spectra in public archives and large radial velocity surveys to obtain a precise radial velocity sample to complement the Gaia astrometry. We used a Gaussian Mixture Model to identify different kinematic structures in the 6D space of positions and velocities. We applied an orbital traceback analysis to estimate a dynamical traceback age for each group and determine the place where it was born. Results. We identified seven different groups in this region. Four groups (ν Sco, β Sco, σ Sco and δ Sco) are part of Upper Scorpius, two groups (ρ Oph and α Sco) are in Ophiuchus, and another group (π Sco) is a nearby young population. We found an age gradient from the ρ Oph group (the youngest) to the δ Sco group ( 5 Myr), showing that star formation was a sequential process for the past 5 Myr. Our traceback analysis shows that Upper Scorpius and ρ Oph groups share a common origin. The closer group of π Sco is probably older, and the traceback analysis suggests that this group and the α Sco group have a different origin, likely related to other associations in the Sco-Cen complex. Conclusions. Our study shows that this region has a complex star formation history that goes beyond the current formation scenario, likely a result of stellar feedback from massive stars, supernovae explosions, and dynamic interactions between stellar groups and the molecular gas. In particular, we speculate that photo-ionisation from the massive δ Sco star could have triggered star formation first in the β Sco group and then in the ν Sco group. The perturbations of stellar orbits due to stellar feedback and dynamical interactions could also be responsible for the 1-3 Myr difference that we found between dynamical traceback ages and isochronal ages.

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Section: Validation Of the Age Gradient With Isochrones And Possible ...mentioning

confidence: 99%

The star formation history of Upper Scorpius and Ophiuchus

Miret-Roig

Galli

Olivares

et al. 2022

A&A

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“…Since the algorithm behind age determination in madys is based on isochronal fitting, the tool automatically inherits the same drawbacks of this technique, which have been the subject of extensive discussion in the literature (see, e.g., Soderblom 2010;Barrado 2016).…”

Section: Discussionmentioning

confidence: 99%

MADYS: the Manifold Age Determination for Young Stars

Bonavita

2022

A&A

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Context. The unrivalled astrometric and photometric capabilities of the Gaia mission have given new impetus to the study of young stars: both from an environmental perspective, as members of comoving star-forming regions, and from an individual perspective, as targets amenable to planet-hunting direct-imaging observations. Aims. In view of the large availability of theoretical evolutionary models, both fields would benefit from a unified framework that allows a straightforward comparison of physical parameters obtained by different stellar and substellar models. Methods. To this aim, we developed the Manifold Age Determination for Young Stars (madys), a flexible Python tool for the age and mass determination of young stellar and substellar objects. In this first release, madys automatically retrieves and crossmatches photometry from several catalogs, estimates interstellar extinction, and derives age and mass estimates for individual objects through isochronal fitting.Results. Harmonizing the heterogeneity of publicly available isochrone grids, the tool allows one to choose amongst 16 models, many of which with customizable astrophysical parameters, for a total of ∼ 110 isochrone grids. Several dedicated plotting functions are provided to allow for an intuitive visual perception of the numerical output. Conclusions. After extensive testing, we have made the tool publicly available. Here, we demonstrate the capabilities of madys, summarizing previously published results as well providing several new examples.

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Section: Discussionmentioning

confidence: 99%

Introducing MADYS: the Manifold Age Determination for Young Stars

Squicciarini,

Bonavita

2022

Preprint

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Context. The unrivalled astrometric and photometric capabilities of the Gaia mission have given new impetus to the study of young stars: both from an environmental perspective, as members of comoving star-forming regions, and from an individual perspective, as targets amenable to planet-hunting direct-imaging observations. Aims. In view of the large availability of theoretical evolutionary models, both fields would benefit from a unified framework that allows a straightforward comparison of physical parameters obtained by different stellar and substellar models. Methods. To this aim, we developed madys, a flexible Python tool for age and mass determination of young stellar and substellar objects. In this first release, madys automatically retrieves and cross-matches photometry from several catalogs, estimates interstellar extinction, and derives age and mass estimates for individual objects through isochronal fitting.Results. Harmonizing the heterogeneity of publicly-available isochrone grids, the tool allows to choose amongst 16 models, many of which with customizable astrophysical parameters, for a total of ∼ 110 isochrone grids. Several dedicated plotting function are provided to allow an intuitive visual perception of the numerical output. Conclusions. After extensive testing, we have made the tool publicly available (https://github.com/vsquicciarini/madys). We demonstrate here the capabilities of madys, summarising already published results as well providing several new examples.

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Clusters: Age Scales for Stellar Physics

Cited by 12 publications

References 217 publications

The star formation history of Upper Scorpius and Ophiuchus

The star formation history of Upper Scorpius and Ophiuchus

MADYS: the Manifold Age Determination for Young Stars

Introducing MADYS: the Manifold Age Determination for Young Stars

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