ldtk: Limb Darkening Toolkit

@article{Parviainen2015ldtkLD,
  title={ldtk: Limb Darkening Toolkit},
  author={Hannu Parviainen and Suzanne Aigrain},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2015},
  volume={453},
  pages={3821-3826}
}
We present a Python package LDTk that automates the calculation of custom stellar limb darkening (LD) profiles and model-specific limb darkening coefficients (LDC) using the library of PHOENIX-generated specific intensity spectra by Husser et al. (2013). The aim of the package is to facilitate analyses requiring custom generated limb darkening profiles, such as the studies of exoplanet transits--especially transmission spectroscopy, where the transit modelling is carried out for custom narrow… 

Figures and Tables from this paper

The Ariel 0.6 - 7.8 μm stellar limb-darkening coefficients

We provide here tables of stellar limb-darkening coefficients (LDCs) for the Ariel ESA M4 space mission. These tables include LDCs corresponding to different wavelength bins and white bands for the

The ExoTETHyS Package: Tools for Exoplanetary Transits around Host Stars

The first release of the open-source python package ExoTETHyS is presented, which aims to provide a stand-alone set of tools for modeling spectro-photometric observations of the transiting exoplanets, with a new calculator of stellar limb-darkening coefficients that outperforms the existing software by one order of magnitude in terms of light-curve model accuracy.

The EBLM project

Some M-dwarfs around F-/G-type stars have been measured to be hotter and larger than predicted by stellar evolution models. Inconsistencies between observations and models need to be addressed with

Directly Determined Properties of HD 97658 from Interferometric Observations

We conducted interferometric observations with the CHARA Array of transiting super-Earth host HD 97658 and measured its limb-darkened angular diameter to be θ LD = 0.314 ± 0.004 mas. The combination

Analytic Planetary Transit Light Curves and Derivatives for Stars with Polynomial Limb Darkening

We derive analytic, closed-form solutions for the light curve of a planet transiting a star with a limb-darkening profile that is a polynomial function of the stellar elevation, up to an arbitrary

Broadband transmission spectroscopy of HD 209458b with ESPRESSO: evidence for Na, TiO, or both

Context. The detection and characterization of exoplanet atmospheres is currently one of the main drivers pushing the development of new observing facilities. In this context, high-resolution

Greening of the brown-dwarf desert

Context. Although more than 2000 brown dwarfs have been detected to date, mainly from direct imaging, their characterisation is difficult due to their faintness and model-dependent results. In the

Chromatic line-profile tomography to reveal exoplanetary atmospheres: application to HD 189733b

Transmission spectroscopy can be used to constrain the properties of exoplanetary atmospheres. During a transit, the light blocked from the atmosphere of the planet leaves an imprint in the light

Optical Transmission Spectroscopy of the Terrestrial Exoplanet LHS 3844b from 13 Ground-based Transit Observations

Atmospheric studies of spectroscopically accessible terrestrial exoplanets lay the groundwork for comparative planetology between these worlds and the solar system terrestrial planets. LHS 3844b is a

Detectability of shape deformation in short-period exoplanets

Context. Short-period planets are influenced by the extreme tidal forces of their parent stars. These forces deform the planets causing them to attain nonspherical shapes. The nonspherical shapes,
...

References

SHOWING 1-10 OF 22 REFERENCES

Limb darkening and exoplanets: testing stellar model atmospheres and identifying biases in transit parameters

Limb-darkening is fundamental in determining transit lightcurve shapes, and is typically modeled by a variety of laws that parametrize the intensity profile of the star that is being transited.

Testing the limb-darkening coefficients measured from eclipsing binaries

Aims. The numerical methods used to compute limb-darkening coefficients (LDCs) are still a matter of discussion. To improve this scenario, we have revised our earlier calculations and compare the new

On stellar limb darkening and exoplanetary transits

This paper examines how to compare stellar limb-darkening coefficients evaluated from model atmospheres with those derived from photometry. Different characterizations of a given model atmosphere can

High-precision stellar limb-darkening measurements - A transit study of 38 Kepler planetary candidates

Context. Planetary transit light curves are influenced by a variety of fundamental parameters, such as the orbital geometry and the surface brightness distribution of the host star. Stellar limb

Does the HD 209458 planetary system pose a challenge to the stellar atmosphere models

Aims. There are very few comparisons between theoretical and empirical limb-darkening coefficients (LDCs). To develop this scenario, we analyse the case of the HD 209458 planetary system for which 10

Theoretical gravity and limb-darkening coefficients for the MOST satellite photometric system

Aims. We present new calculations of limb and gravity-darkening coefficients to be used as input in many fields of stellar physics such as synthetic light curves of double-lined eclipsing binaries

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

Aims. The knowledge of how the specific intensity is distributed over the stellar disk is crucial for interpreting the light curves of extrasolar transiting planets, double-lined eclipsing binaries,

Stellar limb-darkening coefficients for CoRot and Kepler

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

High-Precision Limb-Darkening Measurement of a K3 Giant Using Microlensing

We obtain high-precision limb-darkening measurements in five bands (V, VE, IE, I, and H) for the K3 III (Teff = 4200 K, [Fe/H] = +0.3, log g = 2.3) source of the Galactic bulge microlensing event

The effect of stellar limb darkening values on the accuracy of the planet radii derived from photometric transit observations

Context. The radius of an exoplanet is one of its most important parameters. Studies of planetary interiors and their evolution require 1% precision in the radius determination. Transiting exoplanets