J/A+A/615/A76 Spectroscopic parameters of stars (SPECIES). I. (Soto+, 2018)
Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES).
I. Code description and dwarf stars catalogue.
Soto M.G., Jenkins J.S.
<Astron. Astrophys. 615, A76 (2018)>
=2018A&A...615A..76S 2018A&A...615A..76S (SIMBAD/NED BibCode)
ADC_Keywords: Fundamental catalog ; Stars, dwarfs ; Stars, fundamental
Keywords: techniques: spectroscopic - stars: abundances - fundamental parameters
Abstract:
The detection and subsequent characterisation of exoplanets are
intimately linked to the characteristics of their host star.
Therefore, it is necessary to study the star in detail in order to
understand the formation history and characteristics of their
companion(s). Our aims are to develop a community tool that allows the
automated calculation of stellar parameters for a large number of
stars, using high resolution echelle spectra and minimal photometric
magnitudes, and introduce the first catalogue of these measurements in
this work. We measured the equivalent widths of several iron lines and
used them to solve the radiative transfer equation assuming local
thermodynamic equilibrium in order to obtain the atmospheric
parameters (Teff, [Fe/H], logg, and ξ_t). We then used these values
to derive the abundance of 11 chemical elements in the stellar
photosphere (Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Ni, Cu, and Zn). Rotation
and macroturbulent velocity were obtained using temperature
calibrators and synthetic line profiles to match the observed spectra
isochrones, we were able to derive the mass, radius, and age for each
star using a Bayesian approach. SPECIES obtains bulk parameters that
are in good agreement with measured values from different existing
catalogues, including when different methods are used to derive them.
We find discrepancies in the chemical abundances for some elements
with respect to other works, which could be produced by differences in
Teff, or in the line list or the atomic line data used to derive them.
We also obtained analytic relations to describe the correlations
between different parameters, and we implemented new methods to better
handle these correlations, which provides a better description of the
uncertainties associated with the measurements.
Description:
Fundamental parameters (temperature, metallicity, surface gravity,
microturbulence, rotational and macroturbulent velocity, mass, age,
radius, and abundance for 11 chemical elements) for 602 dwarf stars,
using spectra from the HARPS, FEROS, UVES, and/or HIRES instruments.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea3.dat 436 953 Fundamental parameters for 602 stars, observed
with four different spectrographs
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Object name
11- 15 A5 --- Inst Spectrograph (1)
17- 24 F8.3 km/s RV Radial velocity of the source
26- 30 F5.2 [Sun] [Fe/H] Metallicity
32- 36 F5.3 [Sun] e_[Fe/H] Uncertainty on metallicity
38- 43 F6.1 K T Temperature
45- 51 F7.3 K e_T Uncertainty on temperature
53- 57 F5.3 [cm/s2] logg Surface gravity
59- 63 F5.3 [cm/s2] e_logg Uncertainty on surface gravity
65- 69 F5.3 km/s vt Microturbulence velocity
71- 76 F6.3 km/s e_vt Uncertainty on vt
78- 80 I3 --- nFeI Number of FeI lines
82- 83 I2 --- nFeII Number of FeII lines
85 I1 --- Note1 [1/2] exception code (2)
87- 92 F6.3 km/s vsini Rotational velocity
94- 98 F5.3 km/s e_vsini Uncertainty on vsini
100-105 F6.3 km/s vmac Macroturbulence velocity
107-111 F5.3 km/s e_vmac Uncertainty on vmac
113-117 F5.2 [Sun] [Na/H] ?=- NaI abundance
119-123 F5.3 [Sun] e_[Na/H] ?=- Uncertainty on NaI abundance
125 I1 --- nNaI Number of NaI lines
127-131 F5.2 [Sun] [Mg/H] ?=- MgI abundance
133-137 F5.3 [Sun] e_[Mg/H] ?=- Uncertainty on MgI abundance
139 I1 --- nMgI Number of MgI lines
141-145 F5.2 [Sun] [Al/H] ?=- AlI abundance
147-151 F5.3 [Sun] e_[Al/H] ?=- Uncertainty on AlI abundance
153 I1 --- nAlI Number of AlI lines
155-159 F5.2 [Sun] [Si/H] ?=- SiI abundance
161-165 F5.3 [Sun] e_[Si/H] ?=- Uncertainty on SiI abundance
167-168 I2 --- nSiI Number of SiI lines
170-174 F5.2 [Sun] [Ca/H] ?=- CaI abundance
176-180 F5.3 [Sun] e_[Ca/H] ?=- Uncertainty on CaI abundance
182-183 I2 --- nCaI Number of CaI lines
185-189 F5.2 [Sun] [TiI/H] ?=- TiI abundance
191-195 F5.3 [Sun] e_[TiI/H] ?=- Uncertainty on TiI abundance
197-198 I2 --- nTiI Number of NiI lines
200-204 F5.2 [Sun] [TiII/H] ?=- TiII abundance
206-210 F5.3 [Sun] e_[TiII/H] ?=- Uncertainty on TiII abundance
212 I1 --- nTiII Number of TiII lines
214-218 F5.2 [Sun] [Cr/H] ?=- CrI abundance
220-224 F5.3 [Sun] e_[Cr/H] ?=- Uncertainty on CrI abundance
226-227 I2 --- nCrI Number of CrI lines
229-233 F5.2 [Sun] [Mn/H] ?=- MnI abundance
235-239 F5.3 [Sun] e_[Mn/H] ?=- Uncertainty on MnI abundance
241 I1 --- nMnI Number of MnI lines
243-247 F5.2 [Sun] [Ni/H] ?=- NiI abundance
249-253 F5.3 [Sun] e_[Ni/H] ?=- Uncertainty on NiI abundance
255-256 I2 --- nNiI Number of NiI lines
258-262 F5.2 [Sun] [Cu/H] ?=- CuI abundance
264-268 F5.3 [Sun] e_[Cu/H] ?=- Uncertainty on CuI abundance
270 I1 --- nCuI Number of CuI lines
272-276 F5.2 [Sun] [Zn/H] ?=- ZnI abundance
278-280 F3.1 [Sun] e_[Zn/H] ?=- Uncertainty on ZnI abundance
282 I1 --- nZnI Number of ZnI lines
284 I1 --- NoteFe [1/2] exception in Fe abundance (3)
286 I1 --- NoteTi [1/2] exception in Ti abundance (3)
288-293 F6.3 [Sun] [FeI/H] Neutral Fe abundance
295-300 F6.3 [Sun] [FeII/H] ?=- Ionized Fe abundance
302-306 F5.3 Msun Mass Stellar mass (4)
308-312 F5.3 Msun E_Mass Upper mass uncertainty (4)
314-318 F5.3 Msun e_Mass Lower mass uncertainty (4)
320-325 F6.3 Gyr Age Stellar age (4)
327-331 F5.3 Gyr E_Age Upper age uncertainty (4)
333-337 F5.3 Gyr e_Age Lower age uncertainty (4)
339-343 F5.3 [cm/s2] isologg Isochrone derived surface gravity (4)
345-349 F5.3 [cm/s2] E_isologg Upper iso_logg uncertainty (4)
351-355 F5.3 [cm/s2] e_isologg Lower iso_logg uncertainty (4)
357-362 F6.3 Rsun Radius Stellar radius (4)
364-368 F5.3 Rsun E_Radius Upper radius uncertainty (4)
370-374 F5.3 Rsun e_Radius Lower radius uncertainty (4)
376-378 A3 --- uTp [no yes] use Tphoto ?
380-382 A3 --- uvt [no yes] use vt=1.2km/s ?
384-386 A3 --- uisologg [no yes] use isologg ?
388-393 F6.3 km/s e_vt2 Alternative vt uncertainty
395-401 F7.3 K e_T2 Alternative T uncertainty
403-408 F6.1 K Tphoto Photometric temperature (5)
410-417 F8.3 K e_Tphoto Uncertainty on Tphoto (5)
419-436 A18 --- r_Tphoto Source of Tphoto (5)
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Note (1): Spectrograph used to obtain the spectra.
Note (2): Exception code as follows:
1 = Convergence in the atmospheric parameters was reached
2 = No convergence was reached
Note (3): Exception code as follows:
1 = Agreement between the neutral and ionized species
2 = No agreement between neutral and ionized species
Note (4): Derived by interpolating through the grid of MIST evolutionary
models from Dotter (2016ApJS..222....8D 2016ApJS..222....8D).
Note (5): Temperature was derived by using photometric colour relations and
tabulated values from
Casagrande et al. (2010A&A...512A..54C 2010A&A...512A..54C, Cat. J/A+A/512/A54),
Mann et al. (2015ApJ...804...64M 2015ApJ...804...64M, Cat. J/ApJ/804/64),
Pecaut and Mamajek (2013ApJS..208....9P 2013ApJS..208....9P, Cat. J/ApJS/208/9) or
Gonzalez-Hernandez and Bonifacio (2009A&A...497..497G 2009A&A...497..497G, Cat. J/A+A/497/497).
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Acknowledgements:
Maritza Soto, maritsoto(at)ug.uchile.cl
(End) Maritza Soto [Chile], Patricia Vannier [CDS] 21-Mar-2018