J/MNRAS/456/1221 FGK dwarfs atmospheric parameters (Ryabchikova+, 2016)
Accuracy of atmospheric parameters of FGK dwarfs determined by spectrum fitting.
Ryabchikova T., Piskunov N., Pakhomov Y., Tsymbal V., Titarenko A.,
Sitnova T., Alexeeva S., Fossati L., Mashonkina L.
<Mon. Not. R. Astron. Soc., 456, 1221-1234 (2016)>
=2016MNRAS.456.1221R 2016MNRAS.456.1221R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Abundances
Keywords: methods: data analysis - methods: observational - stars: abundances -
stars: fundamental parameters
Abstract:
We performed extensive tests of the accuracy of atmospheric parameter
determination for FGK stars based on the spectrum fitting procedure
Spectroscopy Made Easy (sme). Our stellar sample consists of 13
objects, including the Sun, in the temperature range 5000-6600K and
metallicity range -1.4-/+0.4. The analysed stars have the advantage of
having parameters derived by interferometry. For each star, we use
spectra obtained with different spectrographs and different
signal-to-noise ratios (S/N). For the fitting, we adopted three
different sets of constraints and test how the derived parameters
depend upon the spectral regions (masks) used in sme. We developed and
implemented in sme a new method for estimating uncertainties in the
resulting parameters based on fitting residuals, partial derivatives,
and data uncertainties. For stars in the 5700-6600K range, the best
agreement with the effective temperatures derived by interferometry is
achieved when spectrum fitting includes the Hα and Hβ
lines, while for cooler stars the choice of the mask does not affect
the results. The derived atmospheric parameters do not strongly depend
on spectral resolution and S/N of the observations, while the
uncertainties in temperature and surface gravity increase with
increasing effective temperature, with minima at 50K in Teff and
0.1dex in logg, for spectra with S/N=150-200. A non-local
thermodynamic equilibrium (NLTE) analysis of the TiI/TiII and FeI/FeII
ionization equilibria and abundances determined from the atomic CI
(NLTE) and molecular CH species supports the parameters we derived
with sme by fitting the observed spectra including the hydrogen lines.
Description:
For the spectroscopic analysis, we choose the 13 MS stars including
the Sun (Table 1) in the 4900-6600K temperature range and with
metallicity between [Fe/H]=-1.5 and +0.3dex. All the stars,
except HD 149026, have, at least, one interferometric determination of
radius and effective temperature.
Spectra of the programme stars were obtained with different
spectrographs. Most data were extracted from the following archives:
the UVES/VLT and HARPS/3.6m spectrographs at ESO,2 the ELODIE/1.93-m
spectrograph3 at the Observatoire de Haute Provence, and the ESPaDONs
spectrograph at the Canada-France-Hawaii Telescope (CFHT).
Spectra of beta Vir and HD 103095 were obtained with the FOCES
spectrograph at 2.2-m telescope of the Calar Alto Observatory. One of
the spectra of 61 Vir was obtained with the Hamilton Echelle
Spectrograph attached to the Shane 3-m telescope of the Lick
Observatory. Spectra of few stars, including that of the Sun reflected
from Ganymede, were obtained with the HiReS/Keck spectrograph.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 137 76 List of investigated stars and spectrographs
used to collect the spectra
table2.dat 37 147 Atomic and molecular line parameters
tablea1.dat 19 312 Laboratory wavelengths of the mask m6
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- Name Star name
22- 29 A8 --- Spect Spectrograph
31- 36 I6 --- Res Resolution power
38- 48 A11 --- Prog Program ID
50 A1 --- n_Prog [a-e] Note on Prog (1)
52- 55 I4 --- S/N ? Average signal-to-noise ratio calculated
in the three wavelength ranges discussed
in Section 3.1
57- 58 A2 --- Mask Mask
60- 63 I4 K TeffS ? SME effective temperature
65- 67 I3 K e_TeffS ? rms uncertainty on TeffS
69- 72 F4.2 [cm/s2] loggS ? SME surface gravity
74- 76 F3.2 [cm/s2] e_loggS ? rms uncertainty on loggS
78- 82 F5.2 [-] [M/H]S ? SME metallicity
84- 86 F3.2 [-] e_[M/H]S ? rms uncertainty on [M/H]S
88- 91 I4 K TeffI ? Interferometry effective temperature
93- 95 I3 K e_TeffI ? rms uncertainty on TeffI
97-100 F4.2 [cm/s2] loggI ? Interferometry surface gravity
102-104 F3.2 [cm/s2] e_loggI ? rms uncertainty on loggI
106-107 I2 --- RefI ? Interferometry reference (2)
109-112 I4 K TeffO ? Other spectroscopy effective temperature
114-115 I2 K e_TeffO ? rms uncertainty on TeffO
117-120 F4.2 [cm/s2] loggO ? Other spectroscopy surface gravity
122-124 F3.2 [cm/s2] e_loggO ? rms uncertainty on loggO
126-130 F5.2 [-] [M/H]O ? Other spectroscopy metallicity
132-134 F3.2 [-] e_[M/H]O ? rms uncertainty on [M/H]O
136-137 I2 --- RefO ? Other spectroscopy reference (2)
--------------------------------------------------------------------------------
Note (1): Notes as follows
a = 05BC16, 05BH32A, 06AC12, 06AH20A
b = 076.C-0878, 183.C-0972, 074.C-0012, 60.A-9036
c = 265.C-5038, 067.C-0206, 077.C-0379, 087.D-0010, 088.C-0879
d = 06AF34, 06bd01, 06bf27, 07AC27
e = (Bagnulo et al., 2003, The Messenger 114, 10,
ESO Paranal Science Operations Team)
Note (2): References as follows:
1 = Boyajian et al. (2013ApJ...771...40B 2013ApJ...771...40B)
2 = Boyajian et al. (2015MNRAS.447..846B 2015MNRAS.447..846B)
3 = Tanner et al. (2015ApJ...800..115T 2015ApJ...800..115T)
4 = von Braun et al. (2014MNRAS.438.2413V 2014MNRAS.438.2413V)
5 = Bruntt (2009A&A...506..235B 2009A&A...506..235B)
6 = Bruntt et al. (2010MNRAS.405.1907B 2010MNRAS.405.1907B)
7 = Doyle et al. (2013, Cat. J/MNRAS/428/3164)
8 = Fuhrmann (1998A&A...338..161F 1998A&A...338..161F)
9 = Fuhrmann (2008MNRAS.384..173F 2008MNRAS.384..173F)
10 = Gonzalez et al. (2010, Cat. J/MNRAS/403/1368)
11 = Ramirez, Melendez & Asplund (2009, Cat. J/A+A/508/L17)
12 = Santos, Israelian & Mayor (2004, Cat. J/A+A/415/1153)
13 = Sitnova et al. (2015ApJ...808..148S 2015ApJ...808..148S)
14 = Sousa et al. (2006, Cat. J/A+A/458/873)
15 = Sousa et al. (2008, Cat. J/A+A/487/373)
16 = Torres et al. (2012, Cat. J/ApJ/757/161)
17 = Valenti & Fischer (2005, Cat. J/ApJS/159/141)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 0.1nm lambda Wavelength
12- 15 A4 ---- El+Ion Species
18- 22 F5.3 ---- log(gf) Oscillator strength
25- 30 F6.3 eV Exi Excitation energy
33- 37 A5 ---- Source Source code (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
1 = Jorgensen et al. (1996A&A...315..204J 1996A&A...315..204J)
2 = Fuhr et al. (1988, J. Phys. Chem. Ref. Data, 17, 4, Cat. VI/72)
3 = Kroll & Kock (1987A&AS...67..225K 1987A&AS...67..225K)
4 = Wood et al. (2013, Cat.J/ApJS/208/27)
5 = Raassen & Uylings (1998, Cat. J/A+A/340/300)
6 = Lawler et al. (2013ApJS..205...11L 2013ApJS..205...11L)
7 = Ryabchikova et al. (1999, Phys. Scr., T83, 162)
8 = Baschek et al. (1970A&A.....4..229B 1970A&A.....4..229B)
9 = Kurucz (2015, http://kurucz.harvard.edu/atoms.html)
10 = O'Brian et al. (1991, J. Opt. Soc. Am. B, 8, 1185)
11 = Ralchenko et al. (2010, NIST Atomic Spectra Database (ver. 4.0.0)
http://www.nist.gov/pml/data/asd.cfm)
12 = Blackwell et al. (1980A&A....81..340B 1980A&A....81..340B)
13 = Bard et al. (1991A&A...248..315B 1991A&A...248..315B)
14 = Hannaford et al. (1992A&A...259..301H 1992A&A...259..301H)
15 = Bard & Kock (1994A&A...282.1014B 1994A&A...282.1014B)
16 = May et al. (1974A&AS...18..405M 1974A&AS...18..405M)
17 = Allende Prieto et al. (2002ApJ...573L.137A 2002ApJ...573L.137A)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.3 0.1nm Lambda1 Lower value of wavelength interval
9 A1 --- --- [-]
10- 17 F8.3 0.1nm Lambda2 Upper value of wavelength interval
19 A1 --- Note [*] * indicates the beginning of each region
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 05-Aug-2016