2020A&A...642A.176T


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.20CEST21:05:35

2020A&A...642A.176T - Astronomy and Astrophysics, volume 642A, 176-176 (2020/10-1)

The chemical evolution of the dwarf spheroidal galaxy Sextans.

THELER R., JABLONKA P., LUCCHESI R., LARDO C., NORTH P., IRWIN M., BATTAGLIA G., HILL V., TOLSTOY E., VENN K., HELMI A., KAUFER A., PRIMAS F. and SHETRONE M.

Abstract (from CDS):

We present our analysis of the FLAMES dataset targeting the central 25' region of the Sextans dwarf spheroidal galaxy (dSph). This dataset is the third major part of the high-resolution spectroscopic section of the ESO large program 171.B-0588(A) obtained by the Dwarf galaxy Abundances and Radial-velocities Team. Our sample is composed of red giant branch stars down to V∼20.5mag, the level of the horizontal branch in Sextans, and allows users to address questions related to both stellar nucleosynthesis and galaxy evolution. We provide metallicities for 81 stars, which cover the wide [Fe/H]=-3.2 to -1.5dex range. The abundances of ten other elements are derived: Mg, Ca, Ti, Sc, Cr, Mn, Co, Ni, Ba, and Eu. Despite its small mass, Sextans is a chemically evolved system, showing evidence of a contribution from core-collapse and Type Ia supernovae as well as low-metallicity asymptotic giant branch stars (AGBs). This new FLAMES sample offers a sufficiently large number of stars with chemical abundances derived with high accuracy to firmly establish the existence of a plateau in [α/Fe] at ∼0.4dex followed by a decrease above [Fe/H]~-2dex. These features reveal a close similarity with the Fornax and Sculptor dSphs despite their very different masses and star formation histories, suggesting that these three galaxies had very similar star formation efficiencies in their early formation phases, probably driven by the early accretion of smaller galactic fragments, until the UV-background heating impacted them in different ways. The parallel between the Sculptor and Sextans dSph is also striking when considering Ba and Eu. The same chemical trends can be seen in the metallicity region common to both galaxies, implying similar fractions of SNeIa and low-metallicity AGBs. Finally, as to the iron-peak elements, the decline of [Co/Fe] and [Ni/Fe] above [Fe/H]~-2 implies that the production yields of Ni and Co in SNeIa are lower than that of Fe. The decrease in [Ni/Fe] favours models of SNeIa based on the explosion of double-degenerate sub-Chandrasekhar mass white dwarfs.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: abundances - galaxies: dwarf - galaxies: evolution

VizieR on-line data: <Available at CDS (J/A+A/642/A176): table2.dat=table6.dat table9.dat-table13.dat>

Status at CDS : Examining the need for a new acronym. // Tables of objects will be appraised for possible ingestion in SIMBAD.

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Sculptor Dwarf Galaxy G 01 00 09.4 -33 42 32   9.79 8.6 8.81   ~ 1179 4
2 NAME Fornax Dwarf Spheroidal G 02 39 59.3 -34 26 57   9.02 7.4     ~ 1545 1
3 NAME Carina dSph G 06 41 36.7 -50 57 58   22.14 11.0 19.47   ~ 1031 0
4 NAME Dwarf Elliptical Galaxy in Sex G 10 13 02.9 -01 36 53   12 10.4     ~ 746 0
5 NAME UMi Galaxy G 15 09 11.34 +67 12 51.7   13.60 10.6     ~ 1221 0
6 NAME Dra dSph G 17 20 14.335 +57 55 16.39   12.40 10.6     ~ 1209 1

    Equat.    Gal    SGal    Ecl

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2021.06.20-21:05:36

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