Bibcode
de Boer, T. J. L.; Tolstoy, E.; Lemasle, B.; Saha, A.; Olszewski, E. W.; Mateo, M.; Irwin, M. J.; Battaglia, G.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 572, id.A10, 14 pp.
Fecha de publicación:
12
2014
Revista
Número de citas
53
Número de citas referidas
50
Descripción
We present deep photometry of the Carina dwarf spheroidal galaxy in the
B and V filters from CTIO/MOSAIC out to and beyond the tidal radius of
rell ≈ 0.48 degrees. The accurately calibrated photometry
is combined with spectroscopic metallicity distributions of red giant
branch (RGB) stars to determine the detailed star formation and chemical
evolution history of Carina. The star formation history (SFH) confirms
the episodic formation history of Carina and quantifies the duration and
strength of each episode in great detail as a function of radius from
the centre. Two main episodes of star formation occurred at old (>8
Gyr) and intermediate (2-8 Gyr) ages, both enriching stars starting from
low metallicities ([Fe/H] < - 2 dex). By dividing the SFH into two
components, we determine that 60 ± 9 percent of the total number
of stars formed within the intermediate-age episode. Furthermore, within
the tidal radius (0.48 degrees or 888 pc) a total mass in stars of 1.07
± 0.08 × 106 M⊙ was formed,
giving Carina a stellar mass-to-light ratio of 1.8 ± 0.8. By
combining the detailed SFH with spectroscopic observations of RGB stars,
we determined the detailed age-metallicity relation of each episode and
the timescale of α-element evolution of Carina from individual
stars. The oldest episode displays a tight age-metallicity relation
during ≈6 Gyr with steadily declining α-element abundances and
a possible α-element "knee" visible at [Fe/H] ≈ - 2.5 dex. The
intermediate-age sequence displays a more complex age-metallicity
relation starting from low metallicity and a sequence in α-element
abundances with a slope much steeper than observed in the old episode,
starting from [Fe/H] = -1.8 dex and [Mg/Fe] ≈ 0.4 dex and declining
to Mg-poor values ([Mg/Fe] ≤ - 0.5 dex). This clearly indicates that
the two episodes of star formation formed from gas with different
abundance patterns, which is inconsistent with simple evolution in an
isolated system.
Tables 1-3 are only available in electronic at the CDS via anonymous ftp
to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/572/A10Appendices
are available in electronic form at http://www.aanda.org
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