Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog

By G. Takeda, Eric B. Ford, A. Sills, F. Rasio, Debra A. Fischer, J. Valenti. 2006

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We derive detailed theoretical models for 1074 nearby stars from the SPOCS (Spectroscopic Properties of Cool Stars) Catalog. The California and Carnegie Planet Search has obtained high-quality (R ≃ 70,000-90,000, S/N ≃ 300-500) echelle spectra of over 1000 nearby stars taken with the Hamilton spectrograph at Lick Observatory, the HIRES spectrograph at Keck, and UCLES at the Anglo Australian Observatory. A uniform analysis of the high-resolution spectra has yielded precise stellar parameters (Teff, log g, v sin i, [M/H], and individual elemental abundances for Fe, Ni, Si, Na, and Ti), enabling systematic error analyses and accurate theoretical stellar modeling. We have created a large database of theoretical stellar evolution tracks using the Yale Stellar Evolution Code (YREC) to match the observed parameters of the SPOCS stars. Our very dense grids of evolutionary tracks eliminate the need for interpolation between stellar evolutionary tracks and allow precise determinations of physical stellar parameters (mass, age, radius, size and mass of the convective zone, surface gravity, etc.). Combining our stellar models with the observed stellar atmospheric parameters and uncertainties, we compute the likelihood for each set of stellar model parameters separated by uniform time steps along the stellar evolutionary tracks. The computed likelihoods are used for a Bayesian analysis to derive posterior probability distribution functions for the physical stellar parameters of interest. We provide a catalog of physical parameters for 1074 stars that are based on a uniform set of high-quality spectral observations, a uniform spectral reduction procedure, and a uniform set of stellar evolutionary models. We explore this catalog for various possible correlations between stellar and planetary properties, which may help constrain the formation and dynamical histories of other planetary systems.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a3577ae0af0be9c89251553c63b1bd3bd2cc0e3c

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Citations in the corpus

TRANSIT TIMING OBSERVATIONS FROM KEPLER. IV. CONFIRMATION OF FOUR MULTIPLE-PLANET SYSTEMS BY SIMPLE PHYSICAL MODELS (2012, methodology): “From these values we performed a Bayesian analysis using Yonsei-Yale stellar isochrones (Yi et al. 2001) to extract best-fit and 68% confidence regions on M⋆ and R⋆ (e.g. Pont & Eyer 2004; Takeda et al. 2007).”
The Ages of Stars (2007, methodology): “In the Takeda et al. (2007) study, which was able to use some of the highest quality data available for FGK stars, only 2/3 of the stars ended up with a well-defined age in the sense that a clear peak was present above the 60% probability level.”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “From Teff and the luminosity, we determine the stellar mass, radius, and an age estimate by associating those observed properties with a model from the stellar interior calculations of Takeda et al. (2007, 2008).”
Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. II. Radii, Masses, and Ages (2016, unknown): “More sophisticated statistical treatments, particularly Bayesian estimates (e.g., Jørgensen & Lindegren 2005; Takeda et al. 2007), are needed to obtain unbiased ages and, even then, uncertainties can be large.”
Retired A Stars and Their Companions: Exoplanets Orbiting Three Intermediate-Mass Subgiants (2007, methodology): “Differences between our inferred values and those from Takeda et al. (2007) had an rms scatter of 7% in mass, 12% in radius, with a median offset of -2% and -4% in each parameter, respectively.”
Tidal Evolution of Close-in Extrasolar Planets (2007, background): “Stellar masses and radii come from a variety of sources: Bakos et al. 2007a; Bakos et al. 2007b; Da Silva et al. 2006; Fischer & Valenti 2005; Moutou et al. 2006; Saffe et al. 2006; Gorda & Svechnikov 1996; and Takeda et al. 2007.”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, methodology): “The only stellar mass information needed in §3 is for the announced and candidate planets, for which we use the accurate Takeda et al. (2007) or Valenti & Fischer (2005) masses.”
DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE STAR GJ 504 (2013, background): “This is also consistent with the arguably most detailed Bayesian isochronal analysis of Takeda et al. (2007), which was a study meant to improve on the analysis of Valenti & Fischer (2005) using the same input data, and which gives an age limit of <760 Myr.”
The Milky Way’s stellar disk (2013, methodology): “2) For stars near the main-sequence turn-off and on the horizontal branch, the isochrones for a given metallicity are widely spread enabling good age determinations: Takeda et al. (2007) obtained a relative age precision for their stars with log g < 4.2 of ≃15%.”
OBSERVATIONAL EVIDENCE FOR TIDAL DESTRUCTION OF EXOPLANETS (2009, background): “Figure 6 shows a histogram of stellar ages for a large population of nearby F, G, and K stars, as reported by Takeda et al. (2007).”
A SUPER-EARTH TRANSITING A NAKED-EYE STAR (2011, methodology): “The radius prior is based on the interferometrically measured stellar radius (von Braun et al. 2011), and the mass prior is based on the analysis of the stellar spectroscopic properties by Takeda et al. (2007).”
A New Planet around an M Dwarf: Revealing a Correlation between Exoplanets and Stellar Mass (2007, background): “Analyses of the local stellar population show that stars have a wide range of abundances at ages from 1 to 10 Gyr, with a 0.2 dex scatter in [Fe/H] over this age range (Edvardsson et al. 1993; Nordström et al. 2004; Takeda et al. 2007).”
Five Planets Orbiting 55 Cancri (2007, methodology): “Takeda et al. (2007) have also derived modified stellar evolutionary models using the Yale Stellar Evolution Code to match the observed spectroscopic parameters from Valenti & Fischer (2005).”
TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, methodology): “We held the stellar mass fixed, adopting values from Takeda et al. (2007).”