J/ApJS/259/45 Abundances of northern bright TESS stars (Tautvaisiene+, 2022)
Chemical composition of bright stars in the northern hemisphere: star-planet
connection.
Tautvaisiene G., Mikolaitis S., Drazdauskas A., Stonkute E.,
Minkeviciute R., Pakstiene E., Kjeldsen H., Brogaard K., Chorniy Y.,
von Essen C., Grundahl F., Ambrosch M., Bagdonas V., Sharma A., Vazquez C.V.
<Astrophys. J. Suppl. Ser., 259, 45 (2022)>
=2022ApJS..259...45T 2022ApJS..259...45T
ADC_Keywords: Abundances; Radial velocities; Space velocities; Stars, distances;
Effective temperatures; Spectra, optical; Exoplanets
Keywords: High resolution spectroscopy
Abstract:
In fulfilling the aims of the planetary and asteroseismic research
missions, such as that of the NASA Transiting Exoplanet Survey
Satellite (TESS) space telescope, accurate stellar atmospheric
parameters and a detailed chemical composition are required as inputs.
We have observed high-resolution spectra for all 848 bright (V<8mag)
stars that are cooler than F5 spectral class in the area up to 12deg
surrounding the northern TESS continuous viewing zone and uniformly
determined the main atmospheric parameters, ages, orbital parameters,
velocity components, and precise abundances of up to 24 chemical
species (C(C2), N(CN), [OI], NaI, MgI, AlI, SiI, SiII, CaI, CaII,
ScI, ScII, TiI, TiII, VI, CrI, CrII, MnI, FeI, FeII, CoI, NiI, CuI,
and ZnI) for 740 slowly rotating stars. The analysis of
25 planet-hosting stars in our sample drove us to the following
conclusions: the dwarf stars hosting high-mass planets are more metal
rich than those with low-mass planets. We find slightly negative C/O
and Mg/Si slopes toward the stars with high-mass planets. All the
low-mass planet hosts in our sample show positive Δ[El/Fe]
versus condensation temperature slopes, in particular, the star with
the largest number of various planets. The high-mass planet hosts have
a diversity of slopes, but in more metal-rich, older, and cooler
stars, the positive elemental abundance slopes are more common.
Description:
Observations were carried out with the 1.65m telescope at the Moletai
Astronomical Observatory of Vilnius University in Lithuania, which is
equipped with the high-resolution Vilnius University Echelle
Spectrograph (VUES). This spectrograph has a wavelength coverage from
400 to 900nm in R∼36000, ∼51000, and ∼68000 resolution modes. For our
work, we used the ∼68000 mode for the M spectral type stars and the
∼36000 mode for other objects.
Like in Paper I (Tautvaisiene+, 2020, J/ApJS/248/19), we selected all
bright (V<8mag) F5 and cooler than Teff<6500K (corresponding to
approximately (B-V)>0.39mag) stars in the area surrounding previously
observed TESS northern continuous viewing zone (CVZ) up to 12°
around the northern ecliptic pole. In this way, we found 848 stars in
the selected field that met these criteria (see Figure 1), and we have
observed all of them during the period of 2019-2021. Of the observed
848 stars, we fully characterized a sample of 740 stars; see Section 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 457 740 Stellar properties
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2016-)
I/259 : The Tycho-2 Catalogue (Hog+ 2000)
II/328 : AllWISE Data Release (Cutri+ 2013)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
I/352 : Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)
V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007)
J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)
J/A+A/433/185 : Abundance analysis of 102 F and G dwarfs (Bensby+, 2005)
J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)
J/A+A/499/935 : RV curves of 42 Dra and HD 139357 (Dollinger+, 2009)
J/A+A/507/417 : Oxygen lines in solar granulation. I. (Pereira+, 2009)
J/ApJ/725/2349 : C/O vs Mg/Si of planetary systems (Delgado Mena+, 2010)
J/A+A/545/A32 : Chemical abundances of 1111 FGK stars (Adibekyan+, 2012)
J/A+A/545/A55 : Extrasolar planets. RVels of 5 stars (Boisse+, 2012)
J/A+A/552/A6 : F-G main-sequence star abund. (Gonzalez Hernandez+, 2013)
J/A+A/562/A71 : Abundances of solar neighbourhood dwarfs (Bensby+, 2014)
J/A+A/572/A33 : Abundances from Gaia-ESO Survey (Mikolaitis+, 2014)
J/A+A/566/A67 : Vel. curves of βCnc, µLeo and βUMi (Lee+, 2014)
J/A+A/571/A47 : Extensive linelist of CH in stellar atm. (Masseron+, 2014)
J/ApJS/211/5 : Line data for the Swan system 12C13C (Ram+, 2014)
J/ApJS/214/26 : Line lists for CN isotopes transitions (Sneden+, 2014)
J/A+A/580/A24 : Abundances in dwarfs, subgiants & giants (da Silva+, 2015)
J/ApJ/805/175 : Keck and APF radial velocities of HD7924 (Fulton+, 2015)
J/ApJ/818/34 : Radial velocity monitoring of 5 FGK stars (Endl+, 2016)
J/AJ/151/144 : ASPCAP weights for APOGEE chemical elements (Garcia+, 2016)
J/A+A/588/A145 : RVels of 8 stars with giant planets (Hebrard+, 2016)
J/A+A/604/A108 : UniDAM results (Mints+, 2017)
J/A+A/603/A30 : Evidence for two distinct giant planet pop. (Santos+, 2017)
J/AJ/153/136 : Planets & their host stars with Gaia plx (Stassun+, 2017)
J/A+A/599/A96 : [C/H] abundances of 1110 stars (Suarez-Andres+, 2017)
J/ApJ/865/68 : Abund. for 79 Sun-like stars within 100pc (Bedell+, 2018)
J/A+A/614/A84 : C/O vs Mg/Si ratios in G-type stars (Suarez-Andres+, 2018)
J/A+A/628/A49 : Spectroscopy of dwarf stars (Mikolaitis+, 2019)
J/A+A/623/A72 : Binarity of HIP stars from Gaia pm anomaly (Kervella+, 2019)
J/AJ/157/149 : Transit param. for planets around subgiants (Luhn+, 2019)
J/A+A/639/A50 : HD 164922 d HARPS-N time series (Benatti+, 2020)
J/A+A/636/L6 : HD 158259 SOPHIE radial velocities (Hara+, 2020)
J/MNRAS/495/3961 : Planet-hosting stars chemical compositions (Liu+, 2020)
J/AJ/159/90 : Li, C and O abundances of FGK stars (Stonkute+, 2020)
J/ApJS/248/19 : High-resolution sp. of TESS stars (Tautvaisiene+, 2020)
J/AJ/161/10 : Radial velocities for 4 host stars (Burt+, 2021)
J/A+A/655/A99 : Chemical abundances of 762 FGK stars (Delgado Mena+, 2021)
J/A+A/653/A160 : Updated radial velocities from Gaia DR2 (Seabroke+, 2021)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [TYC]
4- 14 A11 --- TYC Target name in Tycho-2 catalog (I/259)
16- 24 I9 --- TIC [7547890/470680809]? TESS identifier
(tic8, IV/38)
26- 29 I4 K Teff [3977/6414] Effective temperature
31- 33 I3 K e_Teff [37/274] Error of effective temperature
35- 38 F4.2 [cm.s-2] logg [0.51/4.48] log of surface gravity
40- 43 F4.2 [cm.s-2] e_logg [0.01/0.47] Error on logg
45- 49 F5.2 [-] [Fe/H] [-2.25/0.15] Metallicity
51- 54 F4.2 [-] e_[Fe/H] [0.01/0.24] Error of metallicity
56- 59 F4.2 km.s-1 Vt [0.5/2.74] Microturbulent velocity
61- 64 F4.2 km.s-1 e_Vt [0.15/0.4] Error on Vt
66- 72 F7.2 km.s-1 RV [-254.61/43.05] Radial velocity
74- 78 F5.2 km.s-1 e_RV [0/28.3] Error of radial velocity
80- 86 F7.4 [yr] logAge [8.29/10.07]? Log age of the star
88- 93 F6.4 [yr] e_logAge [0.025/0.4]? Error on logAge
95- 101 F7.2 km.s-1 Ulsr [-129/148] Heliocentric space velocity U
103- 107 F5.2 km.s-1 e_Ulsr [0/18] Error on Ulsr
109- 115 F7.2 km.s-1 Vlsr [-245/50] Heliocentric space velocity V
117- 121 F5.2 km.s-1 e_Vlsr [0.02/33] Error on Vlsr
123- 128 F6.2 km.s-1 Wlsr [-74.2/80] Heliocentric space velocity W
130- 134 F5.2 km.s-1 e_Wlsr [0.02/13] Error on Wlsr
136- 139 F4.2 kpc Dist [0.01/2.2] Distance
141- 145 F5.2 kpc RMean [4.3/11] Mean Galactocentric distance
147- 150 F4.2 kpc e_RMean [0/2.2] Error on Rmean
152- 155 F4.2 kpc Zmax [0.04/2.5] Maximum distance from
Galactic plane
157- 160 F4.2 kpc e_Zmax [0/0.3] Error on Zmax
162- 165 F4.2 [-] Ecc [0/0.94] Eccentricity of galactic orbit
167- 170 F4.2 [-] e_Ecc [0/0.07] Error on Ecc
172- 179 E8.2 [-] TD/D [0.0048/2.4e+52] Thick disk-to-thin
disk probability ratio
181- 185 F5.2 [-] [CI/H] [-1.1/0.3]? Abundance [CI/H]
187- 191 F5.2 [-] e_[CI/H] [0/0.15]? Error on CI abundance
193- 197 F5.2 [-] [NI/H] [-0.85/1.1]? Abundance [NI/H]
199- 202 F4.2 [-] e_[NI/H] [0/0.22]? Error on NI abundance
204- 208 F5.2 [-] [OI/H] [-0.6/0.38]? Abundance [OI/H]
210- 213 F4.2 [-] e_[OI/H] [0/0.15]? Error on OI abundance
215- 219 F5.2 [-] [NaI/H] [-2.6/0.4]? Abundance [NaI/H]
221- 224 F4.2 [-] e_[NaI/H] [0/0.12]? Error on NaI abundance
226- 230 F5.2 [-] [MgI/H] [-1.84/0.38] Abundance [MgI/H]
232- 235 F4.2 [-] e_[MgI/H] [0/0.17] Error on MgI abundance
237- 241 F5.2 [-] [AlI/H] [-2.22/0.3] Abundance [AlI/H]
243- 246 F4.2 [-] e_[AlI/H] [0/0.14] Error on AlI abundance
248- 252 F5.2 [-] [SiI/H] [-2.1/0.33] Abundance [SiI/H]
254- 257 F4.2 [-] e_[SiI/H] [0/0.1] Error on SiI abundance
259- 263 F5.2 [-] [SiII/H] [-2.1/0.33] Abundance [SiII/H]
265- 268 F4.2 [-] e_[SiII/H] [0/0.17] Error on SiII abundance
270- 274 F5.2 [-] [CaI/H] [-1.94/0.3] Abundance [CaI/H]
276- 279 F4.2 [-] e_[CaI/H] [0/0.16] Error on CaI abundance
281- 285 F5.2 [-] [CaII/H] [-2.02/0.26] Abundance [CaII/H]
287- 290 F4.2 [-] e_[CaII/H] [0/0.15] Error on CaII abundance
292- 296 F5.2 [-] [ScI/H] [-2.22/0.32]? Abundance [ScI/H]
298- 301 F4.2 [-] e_[ScI/H] [0/0.18]? Error on ScI abundance
303- 307 F5.2 [-] [ScII/H] [-2.23/0.3] Abundance [ScII/H]
309- 312 F4.2 [-] e_[ScII/H] [0/0.15] Error on ScII abundance
314- 318 F5.2 [-] [TiI/H] [-1.92/0.28] Abundance [TiI/H]
320- 323 F4.2 [-] e_[TiI/H] [0/0.14] Error on TiI abundance
325- 329 F5.2 [-] [TiII/H] [-1.9/0.33]? Abundance [TiII/H]
331- 334 F4.2 [-] e_[TiII/H] [0/0.15]? Error on TiII abundance
336- 340 F5.2 [-] [VI/H] [-2.34/0.28] Abundance [VI/H]
342- 345 F4.2 [-] e_[VI/H] [0/0.13] Error on VI abundance
347- 351 F5.2 [-] [CrI/H] [-2.21/0.23] Abundance [CrI/H]
353- 356 F4.2 [-] e_[CrI/H] [0/0.12] Error on CrI abundance
358- 362 F5.2 [-] [CrII/H] [-1.43/0.28]? Abundance [CrII/H]
364- 367 F4.2 [-] e_[CrII/H] [0/0.15]? Error on CrII abundance
369- 373 F5.2 [-] [MnI/H] [-2.88/0.27]? Abundance [MnI/H]
375- 378 F4.2 [-] e_[MnI/H] [0/0.14]? Error on MnI abundance
380- 384 F5.2 [-] [CoI/H] [-2.3/0.3]? Abundance [CoI/H]
386- 389 F4.2 [-] e_[CoI/H] [0/0.11]? Error on CoI abundance
391- 395 F5.2 [-] [NiI/H] [-2.3/0.27] Abundance [NiI/H]
397- 400 F4.2 [-] e_[NiI/H] [0/0.11] Error on NII abundance
402- 406 F5.2 [-] [CuI/H] [-2.51/0.33]? Abundance [CuI/H]
408- 411 F4.2 [-] e_[CuI/H] [0/0.13]? Error on CuI abundance
413- 417 F5.2 [-] [ZnI/H] [-2.21/0.24]? Abundance [ZnI/H]
419- 422 F4.2 [-] e_[ZnI/H] [0/0.18]? Error on ZnI abundance
424- 428 F5.2 [-] [FeI/H] [-2.27/0.23] Abundance [FeI/H]
430- 433 F4.2 [-] e_[FeI/H] [0/0.1] Error on FeI abundance
435- 439 F5.2 [-] [FeII/H] [-2.38/0.3] Abundance [FeII/H]
441- 444 F4.2 [-] e_[FeII/H] [0/0.18] Error on FeII abundance
446- 450 F5.2 [-] [a/FeI] [-0.07/0.32] Averaged MgI, SiI, SiII,
CaI, CaII, TiI, and TiII to FeI
abundance ratio
452- 455 F4.2 [-] e_[a/FeI] [0/0.45] Standard error on [a/FeI]
457 I1 --- Group [0/3]? Galactic sub-component (1)
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Note (1): Group as follows:
0 = thin disk (601 occurrences),
1 = metal-poor thick disk (121 occurrences),
2 = metal-rich thick disk (17 occurrences),
3 = halo (1 occurrence).
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History:
From electronic version of the journal
References:
Tautvaisiene et al. Paper I. 2020ApJS..248...19T 2020ApJS..248...19T Cat. J/ApJS/248/19
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Jun-2022