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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 25 480 Atomic parameters for iron lines
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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)
Acknowledgements: Sergio Sousa, sousasag(at)astro.up.pt
(End) Sergio Sousa [CAUP-Porto, Portugal], Patricia Vannier [CDS] 30-Mar-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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