New limb-darkening coefficients for Phoenix/1d model atmospheres - II. Calculations for 5000 K ≤ Teff ≤ 10 000 K Kepler, CoRot, Spitzer, uvby, UBVRIJHK, Sloan, and 2MASS photometric systems

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THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, methodology): “To estimate the amplitude of this effect for our simulated TESS detections, we adopt an appropriate value of u1 for each star using the tables of Claret et al. (2012) and Claret et al. (2013), which come from the PHOENIX stellar models.”
X-shooter spectroscopy of young stellar objects in Lupus (2017, methodology): “For the six selected targets, we fixed within the MOOG code the appropriate spectral resolution, the limbdarkening coefficients (taken from Claret et al. 2012), the veiling r6700, and the microturbulence ξ = 1.5 km/s, which is typical of young stars similar to our targets (see, e.g., D’Orazi et al.…”
Optimized transit detection algorithm to search for periodic transits of small planets (2019, methodology): “…the Kepler K2 EPIC catalog (Huber et al. 2016) using the automated catalog_info function of TLS. catalog_info also retrieves the quadratic limb-darkening coefficients for the Kepler bandpass (a = 0.7010, b = 0.0462) via a cross-match of the Claret et al. (2012) tables based on Teff and log (g).”