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J/A+A/615/A31       PTPS stars IV.                   (Deka-Szymankiewicz+, 2018)

The Penn State - Torun Centre for Astronomy Planet Search stars, IV. Dwarfs and the complete sample Deka-Szymankiewicz B., Niedzielski A.T., Adamczyk M., Adamow M., Nowak G., Wolszczan A. <Astron. Astrophys. 615, A31 (2018)> =2018A&A...615A..31D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Effective temperatures ; Stars, masses Keywords: stars: fundamental parameters - stars: atmospheres - stars: late-type - techniques: spectroscopic - planetary systems Abstract: Our knowledge of the intrinsic parameters of exoplanets is as precise as our determinations of their stellar hosts parameters. In the case of radial velocity searches for planets, stellar masses appear to be crucial. But before estimating stellar masses properly, detailed spectroscopic analysis is essential. With this paper we conclude a general spectroscopic description of the Pennsylvania-Torun Planet Search (PTPS) sample of stars. We aim at a detailed description of basic parameters of stars representing the complete PTPS sample. We present atmospheric and physical parameters for dwarf stars observed within the PTPS along with updated physical parameters for the remaining stars from this sample after the first Gaia data release. We used high resolution (R=60000) and high signal-to-noise-ratio (S/N=150-250) spectra from the Hobby-Eberly Telescope and its High Resolution Spectrograph. Stellar atmospheric parameters were determined through a strictly spectroscopic local thermodynamic equilibrium analysis (LTE) of the equivalent widths of FeI and FeII lines. Stellar masses, ages, and luminosities were estimated through a Bayesian analysis of theoretical isochrones. Description: We present Teff, logg, [Fe/H], micrturbulence velocities, absolute radial velocities, and rotational velocities for 156 stars from the dwarf sample of PTPS. For most of these stars these are the first determinations. We refine the definition of PTPS subsamples of stars (giants, subgiants, and dwarfs) and update the luminosity classes for all PTPS stars. Using available Gaia and Hipparcos parallaxes, we redetermine the stellar parameters (masses, radii, luminosities, and ages) for 451 PTPS stars. The complete PTPS sample of 885 stars is composed of 132 dwarfs, 238 subgiants, and 515 giants. The PTPS extends toward much less metal abundant and much more distant stars than other planet search projects aimed at detecting planets around evolved stars; 29% of our targets belong to the Galactic thick disc and 2% belong to the halo. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 102 111 Stars rejested from the PTPS sample after CCF analysis table3.dat 292 885 Stellar parameters for 885 PTPS stars table4.dat 292 29 Stellar parameters for 29 stars with inconsistent parameters
See also: J/A+A/547/A91 : Spectroscopic analysis of 348 red giants (Zielinski+, 2012) J/A+A/569/A55 : Abundances and vsini for 348 red giants (Adamow+, 2014) J/A+A/587/A119 : Masses and luminosities for 342 stars (Adamczyk+, 2016) J/A+A/585/A73 : PTPS stars. III. The evolved stars sample (Niedzielski+, 2016) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Tycho Tycho designation (NNNN-NNNNN-N) 14- 19 I6 --- HD ? HD identification 22- 29 A8 --- BD BD identification 32- 35 I4 K Teff Effective temperature (1) 38- 40 I3 K e_Teff rms uncertainty on Teff 43- 46 F4.2 [cm/s2] logg Stellar surface gravitational acceleration (10 49- 52 F4.2 [cm/s2] e_logg rms uncertainty on logg 54- 61 F8.3 km/s RV Absolute radial velocity 63- 67 F5.2 km/s e_RV rms uncertainty on RV 70- 78 F9.3 d MJD Epoch of radial velocity (MJD) 81-102 A22 --- Note Notes (2)
Note (1): Effective temperatures and logg estimates from Adamow (2010, Master's thesis, UMK, Torun, Poland). Note (2): Notes as follows: SB2 = binary star VCCF = variable CCF FCCF = flat CCF
Byte-by-byte Description of file: table3.dat table4.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Tycho Tycho designation (NNNN-NNNNN-N) 14- 19 I6 --- HD ? HD identification 20 A1 --- m_HD [AB] Multiplicity index on HD 22- 30 A9 --- BD BD identification 32- 42 A11 --- SpType Spectral type from SIMBAD 44- 48 F5.2 mag Vmag Brightness in V 50- 53 F4.2 mag B-V B-V colour index 55- 60 F6.2 mas plx Adopted parallax 62- 66 F5.2 mas e_plx rms uncertainty on plx 69- 73 F5.2 km/s vrot ? Rotational velocity 76- 80 F5.2 km/s e_vrot ? rms uncertainty on vrot 82- 85 F4.2 mag (B-V)0 Intrinsic B-V colour index 88- 92 F5.2 mag VMAG Absolute magnitude in V 95- 99 F5.2 mag BC Bolometric correction in V 101-103 A3 --- SpClass Obtained spectral class 105 A1 --- Method Type of method used (1) 107-110 I4 K Teff Effective temperature 112-114 I3 K e_Teff rms uncertainty on Teff 116-119 F4.2 [cm/s2] logg Stellar surface gravitational acceleration 121-124 F4.2 [cm/s2] e_logg rms uncertainty on logg 126-129 F4.2 km/s vt Microturbulence velocity 131-134 F4.2 km/s e_vt rms uncertainty on vt 136-140 F5.2 [-] [Fe/H] Stellar metallicity 142-145 F4.2 [-] e_[Fe/H] rms uncertainty on [Fe/H] 147-153 F7.2 km/s RV ? Absolute radial velocity 156-159 F4.2 km/s e_RV ? rms uncertainty on RV 161-169 F9.3 d MJD ? Epoch of radial velocity (MJD) 171-178 F8.2 pc Dist Distance (obtained from parallax) 180-186 F7.2 pc e_Dist rms uncertainty on Dist 189-194 F6.2 deg GLON Galactic longitude 197-202 F6.2 deg GLAT Galactic latitude 204-211 F8.2 pc z Distance from Galactic plane 213-220 F8.2 km/s Uvel Velocity towards Galactic Center 222-229 F8.2 km/s Vvel Velocity in the direction of the rotation of the Galaxy 231-237 F7.2 km/s Wvel Velocity towards North Galactic Pole 240-244 A5 --- Popul Galactic Population 246-250 F5.2 [Lsun] logL logarithm of luminosity 252-255 F4.2 [Lsun] e_logL rms uncertainty in logL 257-260 F4.2 Msun M Stellar mass 262-266 F5.3 Msun e_M rms uncertainty in M 268-272 F5.2 [yr] logAge logarithm of stellar age 274-278 F5.3 [yr] e_logAge rms uncertainty in logAge 280-284 F5.2 Rsun R Stellar radius 286-290 F5.2 Rsun e_R rms uncertainty in R 292 I1 --- Note [1/3] Source of original data (2)
Note (1): Stellar parameters determined by parallaxes from: G = Gaia H = Hipparcos B = Bayesian method Note (2): Origin of spectroscopic analysis of stellar parameters: 1 = Zielinski et al. (2012, Cat. J/A+A/547/A91) 2 = Niedzielski et al. (2016, Cat. J/A+A/585/A73) 3 = This work
Acknowledgements: Beata Deka-Szymankiewicz, bdeka(at) References: Zielinski et al., Paper I 2012A&A...547A..91Z, Cat. J/A+A/547/A91 Adamow et al., Paper II 2014A&A...569A..55A, Cat. J/A+A/569/A55 Adamczyk et al., 2016A&A...587A.119A, Cat. J/A+A/587/A119 Niedzielski et al., Paper III 2016A&A...585A..73N, Cat. J/A+A/585/A73
(End) B. Deka-Szymankiewicz [CA UMK Torun, Poland], P. Vannier [CDS] 10-Jan-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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