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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742705.0, MPI für Astronomie / Publikationen_mpia
Peanut-shaped metallicity distributions in bulges of edge-on galaxies: the case of NGC 4710
Authors:Gonzalez, O. A.; Debattista, V. P.; Ness, M.; Erwin, P.; Gadotti, D. A.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:466
Issue / Number:1
Start Page:L93
End Page:L97
Audience:Not Specified
Abstract / Description:Bulges of edge-on galaxies are often boxy/peanut-shaped (B/PS), and unsharp masks reveal the presence of an X shape. Simulations show that these shapes can be produced by dynamical processes driven by a bar which vertically thickens the centre. In the Milky Way, which contains such a B/PS bulge, the X-shaped structure is traced by the metal-rich stars but not by the metal-poor ones. Recently, Debattista et al. interpreted this property as a result of the varying effect of the bar on stellar populations with different starting kinematics. This kinematic fractionation model predicts that cooler populations at the time of bar formation go on to trace the X shape, whereas hotter populations are more uniformly distributed. As this prediction is not specific to the Milky Way, we test it with Multi Unit Spectroscopic Explorer (MUSE) observations of the B/PS bulge in the nearby galaxy NGC 4710. We show that the metallicity map is more peanut-shaped than the density distribution itself, in good agreement with the prediction. This result indicates that the X-shaped structure in B/PS bulges is formed of relatively metal-rich stars that have been vertically redistributed by the bar, whereas the metal-poor stars have a more uniform, box-shaped distribution.
Free Keywords:galaxies: bulges; galaxies: evolution; galaxies: formation; galaxies: stellar content; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnrasl/slw232
URL:http://adsabs.harvard.edu/abs/2017MNRAS.466L..93G
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