English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/210776
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:


Kinematic and metallicity properties of the Aquarius dwarf galaxy from FORS2 MXU spectroscopy⋆

AuthorsHermosa Muñoz, L.; Taibi, S.; Battaglia, G.; Iorio, G.; Rejkuba, M.; Leaman, R.; Cole, A. A.; Irwin, M.; Jablonka, P.; Kacharov, N.; McConnachie, A.; Starkenburg, E.; Tolstoy, E.
KeywordsTechniques: spectroscopic
Galaxies: dwarf
Local Group
Galaxies: kinematics and dynamics
Galaxies: abundances
Galaxies: stellar content
Issue Date2020
PublisherEDP Sciences
CitationAstronomy and Astrophysics - Les Ulis 634: A10 (2020)
AbstractContext. Dwarf galaxies found in isolation in the Local Group (LG) are unlikely to have interacted with the large LG spirals, and therefore environmental effects such as tidal and ram-pressure stripping should not be the main drivers of their evolution. Aims. We provide insight into the internal mechanisms shaping LG dwarf galaxies by increasing our knowledge of the internal properties of isolated systems. Here we focus on the evolved stellar component of the Aquarius dwarf galaxy, whose kinematic and metallicity properties have only recently started to be explored. Methods. Spectroscopic data in the region of the near-infrared Ca II triplet lines has been obtained with FORS2 at the Very Large Telescope for 53 red giant branch (RGB) stars. These data are used to derive line-of-sight (l.o.s.) velocities and [Fe/H] of the individual RGB stars. Results. We derive a systemic velocity of 142.2(-1.8)(+1.8) kms(-1) in agreement with previous determinations from both the HI gas and stars. The internal kinematics of Aquarius appears to be best modelled by a combination of random motions (l.o.s. velocity dispersion of 10.3(-1.3)(+1.6)kms(-1)) and linear rotation (with a gradient -5.0(-1.9)(+1.6) km s(-1) arcmin(-1)) along a PA = 139(-27)(+17) deg, broadly consistent with the optical projected major axis. This rotation signal is significantly misaligned or even counter-rotating to that derived from the HI gas. We also find the tentative presence of a mild negative metallicity gradient and indications that the metal-rich stars have a colder velocity dispersion than the metal-poor ones. Conclusions. This work represents a significant improvement with respect to previous measurements of the RGB stars of Aquarius as it doubles the number of member stars already studied in the literature. We speculate that the misaligned rotation between the HI gas and evolved stellar component might have been the result of recent accretion of HI gas, or re-accretion after gas-loss due to internal stellar feedback.© ESO 2020
Publisher version (URL)http://dx.doi.org/10.1051/0004-6361/201936136
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2020aa36136-19.pdf876,79 kBAdobe PDFThumbnail
Show full item record
Review this work

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.