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J/A+A/469/783 Code for automatic determination of EW (ARES) (Sousa+, 2007)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table2.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/469/783
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-r--r--r-- 1 cats archive 12480 Mar 30 2007 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :J/A+A/469/783 Code for automatic determination of EW (ARES) (Sousa+, 2007)
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A new code for automatic determination of equivalent widths:
Automatic Routine for line Equivalent widths in stellar Spectra (ARES).
Sousa S.G., Santos N.C., Israelian G., Mayor M., Monteiro M.J.P.F.G.
<Astron. Astrophys. 469, 783 (2007)>
=2007A&A...469..783S
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ADC_Keywords: Atomic physics ; Equivalent widths
Keywords: methods: data analysis - methods: spectroscopy - stars: abundances -
stars: fundamental parameters
Abstract:
We present a new automatic code (ARES) for determining equivalent
widths of the absorption lines present in stellar spectra. We also
describe its use for determining fundamental spectroscopic stellar
parameters. The code is written in C++ based on the standard method of
determining EWs and is available for the community. The code automates
the manual procedure that the users normally carry out when using
interactive routines such as the splot routine implemented in IRAF.
Results.We test the code using both simulated and real spectra with
different levels of resolution and noise and comparing its
measurements to the
Description:
Table 2 contains the Atomic parameters and measured solar equivalent
widths for FeII and Fe I lines.