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research article

Origin of stellar prolate rotation in a cosmologically simulated faint dwarf galaxy

Cardona-Barrero, Salvador
•
Battaglia, Giuseppina
•
Di Cintio, Arianna
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July 1, 2021
Monthly Notices Of The Royal Astronomical Society

Stellar prolate rotation in dwarf galaxies is rather uncommon, with only two known galaxies in the Local Group showing such feature (Phoenix and And II). Cosmological simulations show that in massive early-type galaxies prolate rotation likely arises from major mergers. However, the origin of such kinematics in the dwarf galaxies regime has only been explored using idealized simulations. Here, we made use of hydrodynamical cosmological simulations of dwarfs galaxies with stellar mass between 3 x 10(5) and 5 x 10(8) M-circle dot to explore the formation of prolate rotators. Out of 27 dwarfs, only one system showed clear rotation around the major axis, whose culprit is a major merger at z = 1.64, which caused the transition from an oblate to a prolate configuration. Interestingly, this galaxy displays a steep metallicity gradient, reminiscent of the one measured in Phoenix and And II: this is the outcome of the merger event that dynamically heats old, metal-poor stars, and of the centrally concentrated residual star formation. Major mergers in dwarf galaxies offer a viable explanation for the formation of such peculiar systems, characterized by steep metallicity gradients and prolate rotation.

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Type
research article
DOI
10.1093/mnrasl/slab059
Web of Science ID

WOS:000722248100009

Author(s)
Cardona-Barrero, Salvador
•
Battaglia, Giuseppina
•
Di Cintio, Arianna
•
Revaz, Yves  
•
Jablonka, Pascale  
Date Issued

2021-07-01

Publisher

OXFORD UNIV PRESS

Published in
Monthly Notices Of The Royal Astronomical Society
Volume

505

Issue

1

Start page

L100

End page

L105

Subjects

Astronomy & Astrophysics

•

galaxies: formation

•

local group

•

andromeda ii

•

merger

•

kinematics

•

identification

•

evolution

Peer reviewed

REVIEWED

Written at

EPFL

EPFL units
LASTRO  
Available on Infoscience
December 4, 2021
Use this identifier to reference this record
https://infoscience.epfl.ch/handle/20.500.14299/183644
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