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http://hdl.handle.net/20.500.12386/27324
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Kastner, Joel H. | en_US |
dc.contributor.author | SACCO, GIUSEPPE GERMANO | en_US |
dc.contributor.author | Rodriguez, David | en_US |
dc.contributor.author | Punzi, Kristina | en_US |
dc.contributor.author | Zuckerman, B. | en_US |
dc.contributor.author | Vican Haney, Laura | en_US |
dc.date.accessioned | 2020-09-11T13:35:30Z | - |
dc.date.available | 2020-09-11T13:35:30Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27324 | - |
dc.description.abstract | The Galex Nearby Young Star Survey (GALNYSS) has yielded a sample of ∼2000 UV-selected objects that are candidate nearby (D≲ 150 {pc}), young (age ∼ 10-100 Myr), late-type stars. Here, we evaluate the distances and ages of the subsample of (19) GALNYSS stars with Gaia Data Release 1 (DR1) parallax distances D≤slant 120 {pc}. The overall youth of these 19 mid-K to early-M stars is readily apparent from their positions relative to the loci of main-sequence stars and giants in Gaia-based color-magnitude and color-color diagrams constructed for all stars detected by Galex and the Wide-field Infrared Space Explorer for which parallax measurements are included in DR1. The isochronal ages of all 19 stars lie in the range ∼10-100 Myr. Comparison with Li-based age estimates indicates a handful of these stars may be young main-sequence binaries rather than pre-main sequence stars. Nine of the 19 objects have not previously been considered as nearby, young stars, and all but one of these are found at declinations north of +30°. The Gaia DR1 results presented here indicate that the GALNYSS sample includes several hundred nearby, young stars, a substantial fraction of which have not been previously recognized as having ages ≲ 100 {Myr}. | en_US |
dc.language.iso | eng | en_US |
dc.title | Nearby Young, Active, Late-type Dwarfs in Gaia's First Data Release | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aa7065 | en_US |
dc.identifier.scopus | 2-s2.0-85020722044 | en_US |
dc.identifier.isi | 000402310800007 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aa7065 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 841 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 73 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...841...73K | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0002-6893-2221 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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