A new non-linear limb-darkening law for LTE stellar atmosphere models III - Sloan filters: Calculations for –5.0 ≤ log [M/H] ≤ +1, 2000 K ≤ T$\mathsf{_{eff}}$ ≤ 50 000 K at several surface gravities

By A. Claret. 2004

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Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/404db526925148ba037f3da14809e4f0d5afbfca

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Citations in the corpus

High-precision photometry by telescope defocussing. I. The transiting planetary system WASP-5 (2009, methodology): “We have adopted the values of the properties obtained using the Claret models, in order to retain homogeneity with the analyses of Southworth (2009).”
The Transit Light Curve Project. V. System Parameters and Stellar Rotation Period of HD 189733 (2006, methodology): “We fixed the limb-darkening coefficients at the values calculated by Claret (2000, 2004) for observations of a star with the observed spectral properties.12 We also investigated the effect of fitting for the limb-darkening parameters, as discussed below.”
HAT-P-1b: A Large-Radius, Low-Density Exoplanet Transiting One Member of a Stellar Binary (2006, methodology): “W e used the values for the stellar radius and m ass(and theiruncertainties)determ ined above,and coe cientsforstellarlim b darkening forthe Sloan z- lter by Claret (2004).”
Transiting exoplanets from the CoRoT space mission . VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert (2008, background): “According to Claret (2004) for a given value of Teff and log g, the ua and ub values change slightly from one filter to another.”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, background): “Theoretical LD coefficients have been taken from Van Hamme (1993), Claret (2000, 2004a) and Claret & Hauschildt (2003).”
HATSouth: A Global Network of Fully Automated Identical Wide-Field Telescopes (2012, methodology): “The light curve is generated with white and red noise appropriate for the magnitude of the star, with quadratic limb darkening parameters from Claret (2004) appropriate for the stellar atmospheric parameters, random transit phase, and with cos i uniformly distributed between 0 and (R⋆ + RP )/a…”
Misaligned spin-orbit in the XO-3 planetary system?† (2008, methodology): “We adopted the orbital parameters of Table 2, a projected stellar rotation velocity V sin I of 18.5 km s−1, and a linear limb-darkening coefficient = 0.69 from Claret (2004), for Teff = 6250 K and log g = 4.0 dex.”
HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD (2009, methodology): “Alternatively, limb-darkening coefficients are taken from look-up tables, such as that of Claret (2004), which depend on stellar atmospheric parameters, primarily effective temperature.”
CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, neutral): “For the Nickel Z-band data we adopted from Claret (2004): µ1 = 0.353±0.35, µ2 = 0.255±0.025.”
TRANSIT DETECTION IN THE MEarth SURVEY OF NEARBY M DWARFS: BRIDGING THE CLEAN-FIRST, SEARCH-LATER DIVIDE (2012, methodology): “The transits are limbdarkened, using quadratic coefficients for an M4 dwarf (Claret 2004).”
HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field (2008, methodology): “Note that the previously discussed limb darkening coefficients, γ (z) 1 , γ (z) 2 , γ (I) 1 and γ (I) 2 have been taken from the tables of Claret (2004) by interpolation to the above-mentioned SME values for Teff , log g⋆, and [Fe/H].”
The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b (2006, methodology): “…high signal-to-noise ratio to justify this treatment; instead, we fix both combinations of the R and I limb-darkening parameters at the values estimated by Claret (2004) for a star of the observed effective temperature, surface gravity, and metallicity (see Table 5 of McCullough et al. 2006).”
WASP-19b: THE SHORTEST PERIOD TRANSITING EXOPLANET YET DISCOVERED (2010, methodology): “Finally, to derive the final parameters, we use the fourcoefficient limb darkening model by Claret (2004, 2000) with the ATLAS model atmospheres, an effective temperature of 5500 K, and a log g of 4.5.”
Large-scale magnetic topologies of late M dwarfs⋆ (2008, background): “We further assume that continuum limb-darkening varies linearly with the cosine of the limb angle (with a slope of u = 0.6964, Claret 2004).”