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J/A+A/519/L3 Lithium content of omega Cen (Monaco+, 2010)
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Beginning of ReadMe :J/A+A/519/L3 Lithium content of omega Cen (Monaco+, 2010)
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The lithium content of omega Centauri. New clues to the cosmological Li
problem from old stars in external galaxies.
Monaco L., Bonifacio P., Sbordone L., Villanova S., Pancino E.
<Astron. Astrophys., 519, L3-3 (2010)>
=2010A&A...519L...3M
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ADC_Keywords: Clusters, globular ; Stars, dwarfs ; Abundances
Keywords: nuclear reactions, nucleosynthesis, abundances - stars: abundances -
stars: population II - cosmology: observations -
globular clusters: individual: omega Cen - galaxies: abundances
Abstract:
A discrepancy has emerged between the cosmic lithium abundance
inferred by the WMAP satellite measurement coupled with the prediction
of the standard big-bang nucleosynthesis theory, and the constant Li
abundance measured in metal-poor halo dwarf stars (the so-called Spite
plateau). Several models are being proposed to explain this
discrepancy, involving either new physics, in situ depletion, or the
efficient depletion of Li in the pristine Galaxy by a generation of
massive first stars. The realm of possibilities may be narrowed
considerably by observing stellar populations in different galaxies,
which have experienced different evolutionary histories.
The omega Centauri stellar system is commonly considered as the
remnant of a dwarf galaxy accreted by the Milky Way. We investigate
the lithium content of a conspicuous sample of unevolved stars in this
object.
Description:
We obtained moderate resolution (R=17000) spectra for 91
main-sequence/early sub-giant branch (MS/SGB) omega Cen stars using
the FLAMES-GIRAFFE/VLT spectrograph. Lithium abundances were derived
by matching the equivalent width of the LiI resonance doublet at
6708AA to the prediction of synthetic spectra computed with
different Li abundances. Synthetic spectra were computed using the
SYNTHE code along with ATLAS-9 model atmospheres. The stars effective
temperatures are derived by fitting the wings of the Halpha line
with synthetic profiles. Observations were taken on three nights of
27-29 April 2007 using the FLAMES/VLT spectrograph at ESO Paranal.