Stellar limb-darkening coefficients for CoRot and Kepler

By D. Sing. 2009

259 citations recorded by the source corpus.

Transiting exoplanets provide unparalleled access to the fundamental parameters of both extrasolar planets and their host stars. We present limb-darkening coefficients (LDCs) for the exoplanet hunting CoRot and Kepler missions. The LDCs are calculated with ATLAS stellar atmospheric model grids and span a wide range of Teff, log g, and metallically [M/H]. Both CoRot and Kepler contain wide, nonstandard response functions, and are producing a large inventory of high-quality transiting lightcurves, sensitive to stellar limb darkening. Comparing the stellar model limb darkening to results from the first seven CoRot planets, we find better fits are found when two model intensities at the limb are excluded in the coefficient calculations. This calculation method can help to avoid a major deficiency present at the limbs of the 1D stellar models.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/aa566c4ea544a21679b479f52927533f3fd5d8eb

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In Astronomy and Astrophysics

1. Jon Fortney
2. D. Charbonneau
3. N. Madhusudhan
4. J. Winn
5. J. Johnson
6. D. Deming
7. J. Southworth
8. Sara Seager

In Instrumentation

1. D. Charbonneau
2. Jon Fortney
3. J. Southworth
4. J. Winn
5. J. Johnson
6. Timothy Morton
7. A. Showman
8. H. Knutson

Citations in the corpus

• MODELING KEPLER TRANSIT LIGHT CURVES AS FALSE POSITIVES: REJECTION OF BLEND SCENARIOS FOR KEPLER-9, AND VALIDATION OF KEPLER-9 d, A SUPER-EARTH-SIZE PLANET IN A MULTIPLE SYSTEM (2010, methodology): “Kepler limb-darkening coefficients have been computed by Sing (2010) and also A. Prsa;23 (4) extension to any optical or near-infrared passband.”
• THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET (2014, methodology): “The linear and quadratic limbdarkening coefficients ua = 0.40 ± 0.07 and ub = 0.27 ± 0.10 agree well with values predicted by Kurucz stellar models for the Kepler bandpass (Sing 2010), i.e., ua = 0.390 ± 0.006 and ub = 0.264 ± 0.004.”
• The Complete Transmission Spectrum of WASP-39b with a Precise Water Constraint (2017, methodology): “We account for stellar limb darkening using a 4- parameter limb-darkening law (Claret 2000; Sing 2010).”
• 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 (2012, background): “…increase in high-quality light curves from double-lined eclipsing binaries obtained with automatic telescopes (Claret 2008), light curves of planetary transits (including observations obtained with space telescopes (Claret 2009; Sing 2010; Howarth 2011), or microlensing events (Zub et al. 2011).”
• Gravity and limb-darkening coefficients for the Kepler, CoRoT, Spitzer, uvby, UBVRIJHK, and Sloan photometric systems (2011, methodology): “Specifically for transits obtained with the CoRoT space mission, Sing (2010) used his method – which combines LSM and exclusion of limb intensities – to compare his theoretical predictions with semi-empirical LDCs.”
• 3.6 AND 4.5 μm PHASE CURVES AND EVIDENCE FOR NON-EQUILIBRIUM CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HD 189733b (2012, methodology): “We fix the planet’s period to the value from Knutson et al. (2009a), and take our limb-darkening coefficients in each bandpass from Sing (2010)13 assuming an ATLAS stellar atmosphere model with Teff = 5100 K, log(g) = 5.0, and [Fe/H]=0 (Bouchy et al. 2005).”
• HST hot-Jupiter transmission spectral survey: detection of potassium in WASP-31b along with a cloud deck and Rayleigh scattering (2014, methodology): “To account for the effects of limb-darkening on the transit light curve, we adopted the four parameter non-linear limb-darkening law, calculating the coefficients with ATLAS stellar models (Teff=6250, log g=4.5, [Fe/H]= -0.2) following Sing (2010).”
• Hubble Space Telescope transmission spectroscopy of the exoplanet HD 189733b: high‐altitude atmospheric haze in the optical and near‐ultraviolet with STIS (2011, methodology): “(2) For the 1D models, we followed the procedures of Sing (2010) using 1D Kurucz ATLAS models2 and the transmission function of the G430L grating (see Table 1).”
• 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).”
• 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).”
• Limb darkening and exoplanets: testing stellar model atmospheres and identifying biases in transit parameters (2015, methodology): “…exoplanetary transit, observers usually model the effects of limb darkening by either fitting the limb-darkening coefficients (LDCs) of a given law or fixing some (or all) of them using tabulated values (see e.g., Claret & Bloemen 2011; Sing 2010, for some recent tables using the Kepler bandpass).”
• EXPERIMENTAL LIMITS ON PRIMORDIAL BLACK HOLE DARK MATTER FROM THE FIRST 2 YR OF KEPLER DATA (2013, methodology): “To create the simulated microlensing light curves we use the full limb-darkened microlensing formula (Witt & Mao 1994; corrected in Equation (13) of Cieplak & Griest 2013) with linear limb-darkening coefficients calculated using the Sing (2010) model grid for each Kepler source star (Paper II).”
• CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, unknown): “For the Kepler data we used the coefficients listed by Sing (2010): µ1 = 0.521± 0.056, and µ2 = 0.225± 0.052.”
• An HST optical-to-near-IR transmission spectrum of the hot Jupiter WASP-19b: detection of atmospheric water and likely absence of TiO (2013, unknown): “We used the Kurucz (1993) 1D ATLAS stellar atmospheric models4 and a three-parameter limb-darkening law of the form I (μ) I (1) = 1 − c2(1 − μ) − c3(1 − μ3/2) − c4(1 − μ2) (6) as described in Sing (2010).”
• ORBITAL PHASE VARIATIONS OF THE ECCENTRIC GIANT PLANET HAT-P-2b (2013, methodology): “(6) For the transit portion of the light curves we use four parameter nonlinear limb-darkening coefficients for each bandpass calculated by Sing (2010), where we assume a stellar atmosphere with Teff = 6290 K, log(g) = 4.138, and [Fe/H]=+0.14 (Pál et al. 2010).”
• Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, background): “In the 1D case, Sing et al. (2009) and Sing (2010) found that a four-parameter law broke down for small µ, where µ = cos(θ), and θ is the angle in radial direction from the disc centre.”
• Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, background): “Similarly, Claret & Bloemen (2011) compared their Kepler LDCs to those of Sing (2010) and found differences.”
• Hubble Space Telescope hot Jupiter transmission spectral survey: a detection of Na and strong optical absorption in HAT-P-1b (2013, methodology): “Initially, the values for the four limb darkening coefficients were derived from the 1D ATLAS theoretical stellar models of Kurucz8, following the procedures described in Sing (2010).”
• The Hubble Space Telescope PanCET Program: Exospheric Mg ii and Fe ii in the Near-ultraviolet Transmission Spectrum of WASP-121b Using Jitter Decorrelation (2019, methodology): “To account for the effects of limbdarkening on the NUV transit light curve, we adopted the four parameter non-linear limb-darkening law, calculating the coefficients as described in Sing (2010).”