A new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in stellar Spectra (ARES)

By Sérgio F. Sousa, Nuno C. Santos, G. Israelian, M. Mayor, M. M. O. A. D. Lisboa, Observatorio Astronomico de Lisboa, Lisbon., Portugal Porto, Porto, P. O. D. Geneve and 9 more. 2007

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Aims. 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. Methods. 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 manual ones obtained in the standard way. The results shows a small systematic difference, always below 1.5 mA. This can be explained by errors in the manual measurements caused by subjective continuum determination. The code works better and faster than others tested before.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8d7810f3b290c72eb1ee6c2ee3d260af6c0faf77

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Citations in the corpus

Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample. Revising the metallicity-planet correlation (2011, methodology): “The EWs were automatically measured with the ARES3 code (Automatic Routine for line Equivalent widths in stellar Spectra - Sousa et al.,2007) that reproduces with success the common “manual“ and interactive determination of EW measurements.”
Precise radial velocities of giant stars. III. Spectroscopic stellar parameters (2007, methodology): “The mean differences between the EWs measured with ARES and IRAF are: 〈EWARES − EWIRAF〉 = 1.6 mÅ and 2.2 mÅ, with standard deviations of 6.6 mÅ and 2.6 mÅ, for the ‘cool’ and ‘hot’ star respectively.”
Spectroscopic parameters for 451 stars in the HARPS GTO planet search program - Stellar [Fe/H] and the frequency of exo-Neptunes (2008, methodology): “Therefore, we used the large, extended line-list presented in Sousa et al. (2007) and applied this method to the sample.”
SOPHIE velocimetry of Kepler transit candidates VII. A false-positive rate of 35% for Kepler close-in giant candidates (2012, methodology): “For KOI-197, the spectrum had a total S/N sufficiently high (around 50 at 6700 Å) for us to use the automatic code ARES (Sousa et al. 2007) to measure the EWs for the almost 300 lines used in the analysis.”
THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET (2014, methodology): “For comparison, the analysis on the Sun using the HARPS reflection spectrum of Ganymede provided by Sousa et al. (2007) results in Teff = 5781 ± 22 K, log g = 4.45 ± 0.06, ξt = 1.03 ± 0.04 km s−1, [Fe/H] = 0.00 ± 0.02, which are perfectly consistent with the canonical values for the Sun.”
Gaia FGK benchmark stars: Metallicity (2013, methodology): “The EW determination of the Fe lines was carried out with the ARES code (Sousa et al. 2007).”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, methodology): “Another contributing factor is that the HARPS data were analysed using an equivalent-width pipeline (ARES; Sousa et al. 2007), whereas ASPCAP uses a cross-correlation technique.”
Chemical abundances of 451 stars from the HARPS GTO planet search program - Thin disc, thick disc, and planets (2009, methodology): “This was completed with the ARES5 program (Sousa et al. 2007).”
ULySS: a full spectrum fitting package (2009, background): “This is usually an interactive task and requiresa specialised expertise, although this is becoming less true with time (e. g.,Sousa et al. 2007).”
The Gaia-ESO Survey: the analysis of high-resolution UVES spectra of FGK-type stars (2014, methodology): “The EW determination of all the lines was carried out with the ARES code.”
SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, methodology): “To measure the equivalent widths of the iron lines, the code ARES is used (Automatic Routine for line Equivalent widths in stellar Spectra - Sousa et al. 2007).”
Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, methodology): “The authors used a set of FeI and FeII lines whose quivalent widths (EW) were measured using the the ARES3 code (automatic routine for line equivalent widths in stellar spectra - Sousa et al. 2007)4.”