| Issue |
A&A
Volume 383, Number 1, FebruaryIII 2002
|
|
|---|---|---|
| Page(s) | 227 - 238 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20011739 | |
| Published online | 15 February 2002 | |
Automated spectroscopic abundances of A and F-type stars using echelle spectrographs*
I. Reduction of ELODIE spectra and method of abundance determination
Institut d'astronomie de l'Université de Lausanne, 1290 Chavannes-des-Bois, Switzerland
Corresponding author: D. Erspamer, Daniel.Erspamer@obs.unige.ch
Received:
11
October
2001
Accepted:
12
November
2001
This paper presents an automated method to determine
detailed abundances
for A and F-type stars. This method is applied on spectra taken with
the ELODIE spectrograph. Since the standard reduction procedure of
ELODIE is optimized to obtain accurate radial velocities
but not abundances, we present a more appropriate reduction
procedure based on IRAF. We describe an improvement of the method of
Hill & Landstreet ([CITE]) for obtaining 
,
microturbulence and
abundances by fitting a synthetic spectrum to the observed one. In
particular, the method of minimization is presented and
tested with Vega and the Sun. We show that it is
possible, in the case of the Sun, to recover the abundances of
27 elements well within 0.1 dex
of the commonly accepted values.
Key words: methods: numerical / techniques: spectroscopic / Sun: abundances / stars: abundances / stars: individual: Vega
© ESO, 2002
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.