High-resolution elemental abundance analysis of the Hyades supercluster★

Silva, G. M. De; Freeman, K. C.; Bland-Hawthorn, Joss; Asplund, Martin; Williams, M.; Holmberg, Johan

doi:10.1111/j.1365-2966.2011.18728.x

Cited by 36 publications

(52 citation statements)

References 52 publications

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“…To look for new members of close young associations or to identify the members of disrupted open clusters, it is crucial to have complementary information, such as that provided by the analysis of high-resolution spectra, which aims to derive the lithium abundance and Hα luminosity (e.g., Biazzo et al 2009;Guillout et al 2009;López-Santiago et al 2010;Fröhlich et al 2012) by the detailed differential abundance analysis (e.g., de Silva et al 2011;Pompéia et al 2011;Tabernero et al 2012) and by other existing criteria (e.g., Eggen 1995;Shkolnik et al 2012;Malo et al 2013;Gagné et al 2014). Our probabilistic methods are being used by Klutsch et al (in prep.…”

Section: Discussionmentioning

confidence: 99%

“…Nevertheless, at least some of the sources that share the same space motion must have a common origin because of the similarity of their age and abundances. In particular, the chemical tagging of the Hyades stream identified several stars that could likely belong to the eponymous open cluster (de Silva et al 2011;Pompéia et al 2011;Tabernero et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

Klutsch

Ferrero

Guillout

et al. 2014

A&A

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Context. Over the last century, the overdensities in the velocity distributions of nearby stars were attributed to stellar kinematic groups or moving groups. Although their reality was initially questioned, their existence is now supported by a confluence of evidence. Aims. To pursue investigations, quantitative methods should be clearly defined to identify new stars belonging to these groups. Here, we present two probabilistic methods to determine the likelihood of kinematic membership for possible candidates in five of the known young stellar kinematic groups -namely, Pleiades, IC 2391, Castor, Ursa Major, and Hyades -in which all are younger than 650 Myr. Methods. We tried different methods to handle kinematic data of their known members. We succeeded in developing two independent procedures able to identify new candidates of these five stellar stream. We tested the robustness of our two approaches by means of extensive Monte Carlo simulations. Results. Our methods are consistent with one another in more than 90% of cases and for almost all the stellar kinematic groups under scrutiny. The IC 2391 supercluster is an exception. Applying our statistical methods to a large sample of young low-mass stars, we confirmed almost all the likely members and good candidates of these stellar streams. We also proposed 39 additional candidates based on the agreement and the high likelihood of age and kinematic membership. Conclusions. These probabilistic methods are very powerful to reliably identify new candidate members of young stellar kinematic groups. However, the kinematic criteria alone are not sufficient to distinguish between coeval stars that are evaporated from open clusters and other field stars trapped by dynamical processes generated by galactic perturbations. The identification of stars belonging to the remnant of a past star-forming event can be possible with the help of additional information, such as indicators of chromospheric activity, age proxies (lithium abundance), and chemical composition.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

Klutsch

Ferrero

Guillout

et al. 2014

A&A

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“…This chemical tagging method has so far only been used in the three old SKGs: The Hercules stream (Bensby et al 2007) whose stars have different ages and chemistry (associated with dynamical resonances A&A 547, A13 (2012) namely a bar or spiral structure), HR 1614 (De Silva et al 2007b, and Wolf 630 (Bubar & King 2010) the last two appear to be true MGs (debris of star-forming aggregates in the disc). In addition, Soderblom & Mayor (1993), King et al (2003), King & Schuler (2005), and Ammler-von Eiff & Guenther (2009) Silva et al (2011) analysed 26 southern giant candidates finding also four candidate members. These results show that the Hyades Supercluster may not originate uniquely from the Hyades cluster.…”

Section: Introductionmentioning

confidence: 99%

Chemically tagging the Hyades Supercluster

Tabernero

Montes

Hernández

2012

A&A

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Stellar kinematic groups are kinematical coherent groups of stars that might have a common origin. These groups are dispersed throughout the Galaxy over time by the tidal effects of both Galactic rotation and disc heating, although their chemical content remains unchanged. The aim of chemical tagging is to establish that the abundances of every element in the analysis are homogeneus among the members. We study the case of the Hyades Supercluster to compile a reliable list of members (FGK stars) based on our chemical tagging analysis. For a total of 61 stars from the Hyades Supercluster, stellar atmospheric parameters (T eff , log g, ξ, and [Fe/H]) are determined using our code called StePar, which is based on the sensitivity to the stellar atmospheric parameters of the iron EWs measured in the spectra. We derive the chemical abundances of 20 elements and find that their [X/Fe] ratios are consistent with Galactic abundance trends reported in previous studies. The chemical tagging method is applied with a carefully developed differential abundance analysis of each candidate member of the Hyades Supercluster, using a well-known member of the Hyades cluster as a reference (vB 153). We find that only 28 stars (26 dwarfs and 2 giants) are members, i.e. that 46% of our candidates are members based on the differential abundance analysis. This result confirms that the Hyades Supercluster cannot originate solely from the Hyades cluster.

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“…This process begins with the evaporation of young clusters (e.g., Terlevich 1987;Murphy et al 2010). However, the majority of a star's surface abundances will remain constant as it evolves, and it is this persistence of the initial abundance pattern that allows stars from those initial groups to be "chemically tagged" as belonging together (e.g., De Silva et al 2011;.…”

Section: Introductionmentioning

confidence: 99%

Studying Young Stars with Large Spectroscopic Surveys

Martell¹

2015

Proc. IAU

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Abstract. Galactic archaeology is the study of the history of star formation and chemical evolution in the Milky Way, based on present-day stellar populations. Studies of young stars are a key anchor point for Galactic archaeology, since quantities like the initial mass function and the star formation rate can be studied directly in young clusters and star forming regions. Conversely, massive spectroscopic Galactic archaeology surveys can be used as a data source for young star studies.

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High-resolution elemental abundance analysis of the Hyades supercluster★

Cited by 36 publications

References 52 publications

Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

Chemically tagging the Hyades Supercluster

Studying Young Stars with Large Spectroscopic Surveys

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