exosim.tasks.astrosignal.estimatePlanetarySignal#

Attributes#

batman_spec

Classes#

EstimatePlanetarySignal

This task estimates the planetary signal.

Module Contents#

batman_spec[source]#
class EstimatePlanetarySignal[source]#

Bases: exosim.tasks.astrosignal.estimateAstronomicalSignal.EstimateAstronomicalSignal

This task estimates the planetary signal. The signal parameters are extracted from the sky configuration file. This Task is a wrapper for the batman package: it parses the planet parameters and computes the transit model. The transit model is computed at the input wavelength grid. By default, the transit type is set to ‘primary’ (i.e. the planet transits in front of the star). The planetary sarius can be parsed as a string (path to a file) or as a float (in units of stellar radii). If a file is indicated, the planetary radius is binned or interpolated to the input wavelength grid.

Based on Batman package by L. Kreidberg (https://ui.adsabs.harvard.edu/abs/2015PASP..127.1161K/abstract).

model(timeline, wl_grid, ch_parameters={}, source_parameters={})[source]#
Parameters:
Returns:

returns the planetary signal in a 2D array (wavelength, time)

Return type:

ArrayType

load_rp(path, wl)[source]#

Load the planet radius from a file and rebin it to the input wavelength grid.

Parameters:

  • path (str) – Path to the file containing the planet radius data. The file must include columns named “Wavelength” and “rp/rs” representing the wavelengths and the corresponding planet radius (in units of stellar radii), respectively.

  • wl (astropy.units.Quantity) – Wavelength grid onto which the planet radius data will be interpolated.

Returns:

Array of planet radius values (rp/rs) interpolated onto the specified wavelength grid.

Return type:

np.ndarray

Notes

The function reads the data using ascii.read and then applies linear interpolation via interp1d to bin the planet radius values to the provided wavelength grid. Extrapolation is enabled for wavelengths that fall outside the range of the data.

load_ldc(path, wl)[source]#

Load the limb darkening coefficients from a file and rebin them to the input wavelength grid.

Parameters:

  • path (str) – Path to the file containing the limb darkening coefficients data. The file must include a column representing the wavelength (e.g. “wavelength” or “wl”) and one or more columns with the corresponding limb darkening coefficients.

  • wl (astropy.units.Quantity) – The wavelength grid to which the limb darkening coefficients will be rebinned.

Returns:

An array of rebinned limb darkening coefficients. If the file contains multiple coefficient columns, the resulting array will be 2-dimensional with shape (n_coeff, len(wl)), where n_coeff is the number of coefficient columns.

Return type:

np.ndarray

Notes

The function utilises ascii.read to load the data from the file. The wavelength column is identified using the find_key function by searching for keys such as “wavelength” or “wl”. Each remaining column is rebinned to the provided wavelength grid using the rebin function.

get_t14(inc, sma, period, rp)[source]#

t14 Calculates the transit time based on the work of Seager, S., & Mallen-Ornelas, G. 2003, ApJ, 585, 1038

Parameters:
Returns:

transit duration – Returns the transit duration

Return type:

astropy.units.Quantity