VLT/UVES Abundances in Four Nearby Dwarf Spheroidal Galaxies. I. Nucleosynthesis and Abundance Ratios

Shetrone, Matthew; Venn, Kim A.; Tolstoy, Eline; Primas, F.; Hill, V.; Kaufer, A.

doi:10.1086/345966

Cited by 495 publications

(895 citation statements)

References 93 publications

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“…We have no stars in common with Shetrone et al (2003) or Venn et al (2011), and only one star in common with the UVES study of Koch et al (2008), our MKV0948 is his…”

Section: Comparison With Previous Workmentioning

confidence: 92%

“…The samples of Shetrone et al (2003), Koch et al (2008) and Venn et al (2011) also include stars with similarly low [Ca/Fe]. Both the spread and the extremes are much less pronounced than for [Mg/Fe].…”

Section: Magnesiummentioning

confidence: 97%

“…It consists of 5 stars for Shetrone et al (2003), 10 stars Koch et al (2008) and 9 stars for Venn et al (2011), of which 4 are overlapping with Koch et al (2008). We also have 1 star in common with Koch et al (2008).…”

Section: α-Elementsmentioning

confidence: 99%

“…This scatter is also seen in the RGB stars measured in the Sculptor dSph (Hill et al, 2011). Our sample, combined with Shetrone et al (2003) and Venn et al (2011) (Hill et al, 2011). This can be interpreted as an increasing contribution of the s-process from AGB stars (Shetrone et al, 2001).…”

Section: Neutron-capture Elementsmentioning

confidence: 99%

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VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

Lemasle

Hill

Tolstoy

et al. 2012

A&A

191

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Context. The ages of individual Red Giant Branch stars can range from 1 Gyr old to the age of the Universe, and it is believed that the abundances of most chemical elements in their photospheres remain unchanged with time (those that are not affected by the first dredge-up). This means that they trace the interstellar medium in the galaxy at the time the star formed, and hence the chemical enrichment history of the galaxy. Aims. Colour-Magnitude Diagram analysis has shown the Carina dwarf spheroidal to have had an unusually episodic star formation history and this is expected to be reflected in the abundances of different chemical elements. Methods. We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R≈20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.

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“…We have no stars in common with Shetrone et al (2003) or Venn et al (2011), and only one star in common with the UVES study of Koch et al (2008), our MKV0948 is his…”

Section: Comparison With Previous Workmentioning

confidence: 92%

Section: Magnesiummentioning

confidence: 97%

Section: α-Elementsmentioning

confidence: 99%

Section: Neutron-capture Elementsmentioning

confidence: 99%

See 2 more Smart Citations

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

Lemasle

Hill

Tolstoy

et al. 2012

A&A

191

View full text Add to dashboard Cite

show abstract

“…In spite of being overall metal-poor, all dSph galaxies that were studied spectroscopically so far show a spread of metallicities of typically 1 dex in [Fe/H] or more (e.g., Shetrone et al 2001Shetrone et al , 2003Bonifacio et al 2004). There appears to be a trend of increasing intermediate-age population fractions with increasing distance from the Milky Way among the Galactic dSphs (van den Bergh 1994; Grebel 1997), which may be due to the environmental impact of the Milky Way.…”

Section: Comparing Stellar Populations and Star Formation Historiesmentioning

confidence: 99%

Near-field cosmology with Local Group dwarf spheroidals

Grebel¹

2005

Proc. IAU

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Abstract. The Local Group offers an excellent laboratory for near-field cosmology by permitting us to use the resolved stellar content of its constituent galaxies as probes of galaxy formation and evolution, which in turn is an important means for testing cosmological models of hierarchical structure formation. In this review, we discuss the the least massive, yet most numerous type of galaxy in the Local Group, the dwarf spheroidal galaxies, and compare their properties to cosmological predictions. In particular, we point out problems found with a simple building block scenario and with effects expected from reionization. We show that the star formation histories of dSphs are inconsistent with the predicted cessation of star formation after reionization; instead, extended star formation episodes are observed. The Galactic dSphs contain in part prominent intermediate-age populations, whereas the Galactic halo does not. Conversely, the M31 dSphs are almost entirely old, while the M31 halo contains a substantial intermediate-age population. These differences in the population structure as well as the differences in the modes of star formation inferred from [α/Fe] ratios make dSphs unlikely major contributors to the build-up of the Galactic and M31 halo unless most of the accretion occurred at early epochs. On the other hand, there is clear evidence for ongoing harassment and accretion of a number of dSphs.

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Complexity in small‐scale dwarf spheroidal galaxies

Koch

2009

Reviews in Modern Astronomy

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Abstract. Our knowledge about the chemical evolution of the more luminous dwarf spheroidal (dSph) galaxies is constantly growing. However, little is known about the enrichment of the ultrafaint systems recently discovered in large numbers in large Sky Surveys. Low-resolution spectroscopy and photometric data indicate that these galaxies are predominantly metal-poor. On the other hand, the most recent high-resolution abundance analyses indicate that some of these galaxies experienced highly inhomogenous chemical enrichment, where star formation proceeds locally on the smallest scales. Furthermore, these galaxy-contenders appear to contain very metal-poor stars with [Fe/H]< −3 dex and could be the sites of the first stars. Here, we consider the presently available chemical abundance information of the (ultra-) faint Milky Way satellite dSphs. In this context, some of the most peculiar element and inhomogeneous enrichment patterns will be discussed and related to the question of to what extent the faintest dSph candidates and outer halo globular clusters could have contributed to the metal-poor Galactic halo.

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VLT/UVES Abundances in Four Nearby Dwarf Spheroidal Galaxies. I. Nucleosynthesis and Abundance Ratios

Cited by 495 publications

References 93 publications

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

Near-field cosmology with Local Group dwarf spheroidals

Complexity in small‐scale dwarf spheroidal galaxies

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