Gravity and limb-darkening coefficients for the Kepler, CoRoT, Spitzer, uvby, UBVRIJHK, and Sloan photometric systems

By A. Claret, Steven Bloemen. 2011

872 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/716a698f42d95de078350d5cd031e67cc87b8682

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Citations in the corpus

Limb darkening and exoplanets: testing stellar model atmospheres and identifying biases in transit parameters (2015, methodology): “The second approach was to fit to 100-µ points obtained by interpolating the 17 angles given by the ATLAS models3 in a linear grid from µ = 0.01 to µ = 1.0 in 0.01 steps using a cubic spline, a procedure followed by Claret & Bloemen (2011), hereafter refered as CB114.”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, methodology): “We used the JKTEBOP code (Southworth 2008) assuming the limb darkening coefficients from Claret & Bloemen (2011) to simulate the transit light curve and determine the transit depth.”
SOAP 2.0: A TOOL TO ESTIMATE THE PHOTOMETRIC AND RADIAL VELOCITY VARIATIONS INDUCED BY STELLAR SPOTS AND PLAGES (2014, background): “(9) For a stellar effective temperature close to that of the Sun (5778 K), we choose γ1 = 0.29 and γ2 = 0.34 (Oshagh et al. 2013; Claret & Bloemen 2011; Sing 2010).”
CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C (2014, methodology): “We fit four limb darkening parameters using the perscription of Claret & Bloemen (2011), allowing the value for each limb darkening coeffecient to float as a free parameter.”
Limb and gravity-darkening coefficients for the TESS satellite at several metallicities, surface gravities, and microturbulent velocities (2016, background): “For details of these comparisons related to eclipsing binaries and planetary transits see for example Claret (2008), Southworth (2008), Claret (2009), Sing (2010), Howarth (2011), Claret & Bloemen (2011), Southworth (2012), Csizmadia et al. (2013), and Müller et al. (2013).”
The Orbital Eccentricity of Small Planet Systems (2018, methodology): “For the limb darkening coefficients, we used a Gaussian prior centered at values predicted from the table of Claret & Bloemen (2011) with a standard deviation of 0.1.”
Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, result): “Similarly, Claret & Bloemen (2011) compared their Kepler LDCs to those of Sing (2010) and found differences.”
One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c (2015, methodology): “For the limb darkening coefficient, we used the interpolated values from Claret & Bloemen (2011).”
THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX (2013, methodology): “Limbdarkening coefficients were fixed in the models to 0.3236 and 0.3052 as determined from the grid of Claret & Bloemen (2011).”
ALMOST ALL OF KEPLER'S MULTIPLE-PLANET CANDIDATES ARE PLANETS (2012, methodology): “The transit was described with the analytic formulae of Mandel & Agol (2002), and we adopted a non-linear limb darkening law with coefficients fixed based on the Claret & Bloemen (2011) tabulation for the Kepler band with stellar parameters from SME analysis.”
Detection of a transit of the super-Earth 55 Cancri e with warm Spitzer (2011, methodology): “These values were drawn from the theoretical tables of Claret & Bloemen (2011) for the IRAC 4.5 µm bandpass and for Teff= 5250 K, log g =4.5 and [Fe/H]=+0.3.”
ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES (2015, methodology): “We use a prior on the limb darkening based on stellar atmosphere models (Claret & Bloemen 2011) to speed up MCMC convergeance, but nevertheless allow the limb darkening parameters to vary to avoid this source of complications.”
TRANSIT TIMING OBSERVATIONS FROM KEPLER. VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS (2013, methodology): “We used our own code to fit the Mandel & Agol (2002) model, with a quadratic limb-darkening law, using coefficients that we interpolated from Claret & Bloemen (2011) tables, assuming log g = 4, solar metallicity, and Kepler Input Catalog temperature (Brown et al. 2011).”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “To obtain a limb-darkening solution consistent with theory, we used normal prior distributions for u1 and u2 based on theoretical values and 1-σ errors interpolated in the tables by Claret & Bloemen (2011).”
Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90 (2017, methodology): “We imposed Gaussian priors on the two limb-darkening coefficients, centered at values predicted by Claret & Bloemen (2011) for the host stars (using spectroscopic parameters from MacDonald et al. 2016 for Kepler-80, and parameters from Petigura et al. 2017 for Kepler-90).”
An asteroseismic view of the radius valley: stripped cores, not born rocky (2017, methodology): “A flat prior is used for all parameters except limb darkening, for which a Gaussian prior was used, with the mean value predicted from a Kurucz atmosphere table (Claret & Bloemen 2011) and a standard deviation of 0.1.”
LACK OF INFLATED RADII FOR KEPLER GIANT PLANET CANDIDATES RECEIVING MODEST STELLAR IRRADIATION (2011, neutral): “We assumed a quadratic law for the limb-darkening (LD) and used c1 = 2u1 + u2 and c2 = u1 − 2u2 as jump parameters, where u1 and u2 are the quadratic coefficients. u1 and u2 were drawn from the theoretical tables of Claret & Bloemen (2011) for the corresponding KIC Teff and log g values.”