J/A+A/469/783 Code for automatic determination of EW (ARES) (Sousa+, 2007)
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 2007A&A...469..783S
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.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 25 480 Atomic parameters for iron lines
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda Central wavelength
9- 12 F4.2 eV EP Excitation potential
14- 19 F6.3 [-] loggf Oscillator strength
21- 25 F5.1 0.1pm EWsun Solar equivalent width (mÅ)
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Acknowledgements:
Sergio Sousa, sousasag(at)astro.up.pt
(End) Sergio Sousa [CAUP-Porto, Portugal], Patricia Vannier [CDS] 30-Mar-2007