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Article: The dawning of the stream of Aquarius in RAVE

TitleThe dawning of the stream of Aquarius in RAVE
Authors
KeywordsSolar neighborhood
Galaxy: halo
Galaxy: kinematics and dynamics
Issue Date2011
Citation
Astrophysical Journal, 2011, v. 728, n. 2 How to Cite?
AbstractWe identify a new, nearby (0.5 kpc ≲ d ≲ 10 kpc) stream in data from the RAdial Velocity Experiment (RAVE). As the majority of stars in the stream lie in the constellation of Aquarius, we name it the Aquarius Stream. We identify 15 members of the stream lying between 30° < l < 75° and -70° < b < -50°, with heliocentric line-of-sight velocities V los ∼ -200 km s-1. The members are outliers in the radial velocity distribution, and the overdensity is statistically significant when compared to mock samples created with both the Besançon Galaxy model and newly developed code Galaxia. The metallicity distribution function and isochrone fit in the log g-Teff plane suggest that the stream consists of a 10Gyr old population with [M/H] ∼ -1.0. We explore relations to other streams and substructures, finding that the stream cannot be identified with known structures: it is a new, nearby substructure in the Galaxy's halo. Using a simple dynamical model of a dissolving satellite galaxy, we account for the localization of the stream. We find that the stream is dynamically young and therefore likely the debris of a recently disrupted dwarf galaxy or globular cluster. The Aquarius stream is thus a specimen of ongoing hierarchical Galaxy formation, rare for being right in the solar suburb. © 2011. The American Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/209017
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorWilliams, Mary E K-
dc.contributor.authorSteinmetz, Matthias-
dc.contributor.authorSharma, Sanjib-
dc.contributor.authorBland-Hawthorn, Joss Bland-
dc.contributor.authorDe Jong, Roelof S.-
dc.contributor.authorSeabroke, George M.-
dc.contributor.authorHelmi, Amina-
dc.contributor.authorFreeman, Kenneth C.-
dc.contributor.authorBinney, James J.-
dc.contributor.authorMinchev, Ivan-
dc.contributor.authorBienaymé, Olivier-
dc.contributor.authorCampbell, Randy D.-
dc.contributor.authorFulbright, Jon P.-
dc.contributor.authorGibson, Brad K.-
dc.contributor.authorGilmore, Gerard F.-
dc.contributor.authorGrebel, Eva K.-
dc.contributor.authorMunari, Ulisse-
dc.contributor.authorNavarro, Julio F.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSiebert, Arnaud-
dc.contributor.authorSiviero, Alessandro-
dc.contributor.authorWatson, Fred G.-
dc.contributor.authorWyse, Rosemary F G-
dc.contributor.authorZwitter, Tomaž-
dc.date.accessioned2015-03-23T02:31:10Z-
dc.date.available2015-03-23T02:31:10Z-
dc.date.issued2011-
dc.identifier.citationAstrophysical Journal, 2011, v. 728, n. 2-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/209017-
dc.description.abstractWe identify a new, nearby (0.5 kpc ≲ d ≲ 10 kpc) stream in data from the RAdial Velocity Experiment (RAVE). As the majority of stars in the stream lie in the constellation of Aquarius, we name it the Aquarius Stream. We identify 15 members of the stream lying between 30° < l < 75° and -70° < b < -50°, with heliocentric line-of-sight velocities V los ∼ -200 km s-1. The members are outliers in the radial velocity distribution, and the overdensity is statistically significant when compared to mock samples created with both the Besançon Galaxy model and newly developed code Galaxia. The metallicity distribution function and isochrone fit in the log g-Teff plane suggest that the stream consists of a 10Gyr old population with [M/H] ∼ -1.0. We explore relations to other streams and substructures, finding that the stream cannot be identified with known structures: it is a new, nearby substructure in the Galaxy's halo. Using a simple dynamical model of a dissolving satellite galaxy, we account for the localization of the stream. We find that the stream is dynamically young and therefore likely the debris of a recently disrupted dwarf galaxy or globular cluster. The Aquarius stream is thus a specimen of ongoing hierarchical Galaxy formation, rare for being right in the solar suburb. © 2011. The American Astronomical Society.-
dc.languageeng-
dc.relation.ispartofAstrophysical Journal-
dc.subjectSolar neighborhood-
dc.subjectGalaxy: halo-
dc.subjectGalaxy: kinematics and dynamics-
dc.titleThe dawning of the stream of Aquarius in RAVE-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/728/2/102-
dc.identifier.scopuseid_2-s2.0-84891182950-
dc.identifier.volume728-
dc.identifier.issue2-
dc.identifier.eissn1538-4357-

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