Journal
ASTROPHYSICAL JOURNAL
Volume 728, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/728/2/102
Keywords
Galaxy: halo; Galaxy: kinematics and dynamics; solar neighborhood
Categories
Funding
- Anglo-Australian Observatory
- Astrophysical Institute Potsdam
- Australian National University
- Australian Research Council
- French National Research Agency
- German Research foundation
- Istituto Nazionale di Astrofisica at Padova
- Johns Hopkins University
- National Science Foundation of the USA [AST-0908326]
- W.M. Keck foundation
- Macquarie University
- Netherlands Research School for Astronomy
- Natural Sciences and Engineering Research Council of Canada
- Slovenian Research Agency
- Swiss National Science Foundation
- Science & Technology Facilities Council of the UK
- Opticon
- Strasbourg Observatory
- Universities of Groningen, Heidelberg and Sydney
- European Research Council (Galactica) [ERC-StG 240271]
- STFC [PP/D001528/1, ST/G002509/1, PP/D001242/1, ST/G002479/1, ST/F002432/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G002509/1, PP/D001242/1, ST/H00243X/1, ST/F002432/1, ST/G002479/1, PP/D001528/1] Funding Source: researchfish
- UK Space Agency [PP/D006570/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908326] Funding Source: National Science Foundation
Ask authors/readers for more resources
We identify a new, nearby (0.5 kpc less than or similar to d less than or similar to 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 degrees < l < 75 degrees and -70 degrees < b < -50 degrees, with heliocentric line-of-sight velocities V-los similar to -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 Besancon Galaxy model and newly developed code Galaxia. The metallicity distribution function and isochrone fit in the log g-T-eff plane suggest that the stream consists of a 10Gyr old population with [M/H] similar to -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.
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