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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea3.dat 436 953 Fundamental parameters for 602 stars, observed with four different spectrographs
Byte-by-byte Description of file: tablea3.dat
Bytes Format Units Label Explanations
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)
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). Note (5): Temperature was derived by using photometric colour relations and tabulated values from Casagrande et al. (2010A&A...512A..54C, Cat. J/A+A/512/A54), Mann et al. (2015ApJ...804...64M, Cat. J/ApJ/804/64), Pecaut and Mamajek (2013ApJS..208....9P, Cat. J/ApJS/208/9) or Gonzalez-Hernandez and Bonifacio (2009A&A...497..497G, Cat. J/A+A/497/497).
Acknowledgements: Maritza Soto, maritsoto(at)
(End) Maritza Soto [Chile], Patricia Vannier [CDS] 21-Mar-2018
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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