A REVISED EFFECTIVE TEMPERATURE SCALE FOR THE KEPLER INPUT CATALOG

By M. Pinsonneault, D. An, J. Molenda–Żakowicz, W. Chaplin, T. Metcalfe, H. Bruntt. 2011

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We present a catalog of revised effective temperatures for stars observed in long-cadence mode in the Kepler Input Catalog (KIC). We use Sloan Digital Sky Survey (SDSS) griz filters tied to the fundamental temperature scale. Polynomials for griz color–temperature relations are presented, along with correction terms for surface gravity effects, metallicity, and statistical corrections for binary companions or blending. We compare our temperature scale to the published infrared flux method (IRFM) scale for VTJKs in both open clusters and the Kepler fields. We find good agreement overall, with some deviations between (J − Ks)-based temperatures from the IRFM and both SDSS filter and other diagnostic IRFM color–temperature relationships above 6000 K. For field dwarfs, we find a mean shift toward hotter temperatures relative to the KIC, of order 215 K, in the regime where the IRFM scale is well defined (4000 K to 6500 K). This change is of comparable magnitude in both color systems and in spectroscopy for stars with Teff below 6000 K. Systematic differences between temperature estimators appear for hotter stars, and we define corrections to put the SDSS temperatures on the IRFM scale for them. When the theoretical dependence on gravity is accounted for, we find a similar temperature scale offset between the fundamental and KIC scales for giants. We demonstrate that statistical corrections to color-based temperatures from binaries are significant. Typical errors, mostly from uncertainties in extinction, are of order 100 K. Implications for other applications of the KIC are discussed.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/18dd813a3ce69631e28cc63940088228a062a6c8

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Citations in the corpus

Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes (2017, methodology): “Finally, we collected griz photometry from the Kepler Input Catalog (KIC, Brown et al. 2011), corrected to the SDSS scale following Pinsonneault et al. (2012), 2MASS JHK, Tycho B VT T , and TGAS parallaxes (Gaia Collaboration et al. 2016a, 2016b; Lindegren et al. 2016) for each star.”
Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes (2016, background): “…of the host stars, often resulting in quite different conclusions as to the radius distribution of the Kepler target stars and thus their transiting planetary companions (see, e.g., Mann et al. 2012; Pinsonneault et al. 2012; Dressing & Charbonneau 2013; Huber et al. 2014; Gaidos et al. 2016).”
The California-Kepler Survey. VII. Precise Planet Radii Leveraging Gaia DR2 Reveal the Stellar Mass Dependence of the Planet Radius Gap (2018, background): “For Kepler field stars, there are significant degeneracies between reddening and photometric Teff that result in uncertainties of ≈200K (see Pinsonneault et al. 2012 and P17).”
TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, background): “…parameter estimates of Kepler targets are subject to systematic uncertainties (Brown et al. 2011; Mann et al. 2012; Muirhead et al. 2012; Pinsonneault et al. 2012; Dressing & Charbonneau 2013; Everett et al. 2013; Gaidos & Mann 2013) and multiplicity/blend effects (Cartier et al. 2014;…”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, methodology): “To 2 http://keplerebs.villanova.edu 3 http://simbad.u-strasbg.fr/simbad/ A34, page 6 of 15 have a homogeneous set of temperatures we used those derived by Pinsonneault et al. (2012), who recalibrated the KIC photometry in the SDSS griz filters using YREC models.”
Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, methodology): “…widths with those from peak-bagging of 42 giants in NGC 6819 by Handberg et al. (2016, submitted) where we adopt an uncertainty of 100 K on Teff for all stars, and 19 red giants by Corsaro et al. (2015) where we adopt Teff values from Pinsonneault et al. (2012) (from the infra-red flux method).”
THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “We adopted effective temperatures based on the griz SDSS filters (Fukugita et al. 1996) from Pinsonneault et al. (2012), using the KIC extinction map.”
A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars (2020, background): “Ground-based photometry obtained from different surveys can also exhibit substantial offsets at the & 0.01 mag level, as shown for example in the various photometric surveys which have targeted the Kepler field (e.g. Pinsonneault et al. 2012; Greiss et al. 2012).”
PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, methodology): “For these stars, the stellar temperatures are updated using the methodology of Pinsonneault et al. (2012) where possible, but the surface gravity estimates are still based on the KIC narrow-band photometry.”
Target Selection for the SDSS-IV APOGEE-2 Survey (2017, methodology): “Giants are identified using Teff < 5500 K and log g < 3.5, and dwarfs with 5000 ≤ Teff ≤ 6500 K and log g > 3.5; pre-observation temperature and gravity estimates come from the revised Kepler Input Catalog (Huber et al. 2014) and the corrected temperature scale of Pinsonneault et al. (2012).”
The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars (2017, methodology): “Both Pinsonneault et al. (2012) and Huber et al. (2014) apply ad hoc corrections to the photometric Teff which grow to 400K at 6500K.”
Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life (2014, methodology): “…Kepler were estimated by Bayesian inference and a combination of Kepler Input Catalog photometry (Brown et al. 2011) corrected to the Sloan system (Pinsonneault et al. 2012), the Dartmouth Stellar Evolution models (Dotter et al. 2008) and priors on stellar metallicity, age, mass, and distance…”
THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS (2013, background): “Pinsonneault et al. (2012) found effective temperatures that are typically ∼200K hotter than listed in the KIC.”
They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, methodology): “After correction of the KIC to the SDSS system using Pinsonneault et al. (2012) and Eqn.”
The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, methodology): “Because of systematic differences between Teff scales between catalogs (Pinsonneault et al. 2012), we encourage adding 100 K systematic uncertainty in quadrature (116 K total uncertainty) for applications beyond internal comparisons within the CKS catalog.”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “In this case, however, it should be kept in mind that the scatter around the empirical J − KS relation is quite large, partly stemming from its limited colour baseline, and that it seems to underestimate Teff above 6000 K (Pinsonneault et al. 2012).”