Parallax

pyLIMA.parallax.astropy_ephemerides.Earth_ephemerides(time_to_treat)

Find the Earth positions and speeds

Parameters:

time_to_treat (array, array of time to treat)

Returns:

Earth_position_speed

Return type:

list, [positions,speed]

pyLIMA.parallax.parallax.EN_trajectory_angle(piEN, piEE)

Find the angle between the North vector and the lens trajectory (at t0par). See https://ui.adsabs.harvard.edu/abs/2004ApJ…606..319G/abstract

Parameters:

  • piEN (float, the North parallax component)

  • piEE (float, the East parallax component)

Returns:

angle

Return type:

float, the angle of the lens trajectory in radians

pyLIMA.parallax.parallax.Earth_ephemerides(time_to_treat)

Compute the Earth positions and speeds

Parameters:

time_to_treat (array, the time in JD to treat)

Returns:

  • Earth_positions (array, the XYZ Earth positions)

  • Earth_speeds (array, the XYZ Earth speeds)

pyLIMA.parallax.parallax.Earth_telescope_sidereal_times(time_to_treat, sidereal_type='mean')

Compute the sidereal time for a given time

Parameters:

time_to_treat (array, the time in JD to treat)

Returns:

sidereal_time

Return type:

array, the sidereal_time (angle with vernal point) at time t

pyLIMA.parallax.parallax.annual_parallax(time_to_treat, earth_positions, t0_par)

Compute the position shift due to the Earth movement. See https://ui.adsabs.harvard.edu/abs/2004ApJ…606..319G/abstract

Parameters:

  • time_to_treat (array, the time in JD to treat)

  • earth_positions (array, the Earth ephemerides at time t)

  • t0_par (the time of reference)

Returns:

  • delta_Sun (array, the [X,Y,Z] position of the Sun relative to reference frame ()

  • t0_par)

pyLIMA.parallax.parallax.compute_parallax_curvature(piE, delta_positions)

Compute the curvature induce by the parallax of from deltas_positions of a telescope. See https://ui.adsabs.harvard.edu/abs/2004ApJ…606..319G/abstract

Parameters:

  • piE (array, [piEN,piEE] the parallax vector)

  • delta_positions (array, [d_N,d_E] the projected positions of the telescope)

Returns:

  • delta_tau (array, the x shift induced by the parallax)

  • delta_beta (array, the y shift induced by the parallax)

pyLIMA.parallax.parallax.parallax_combination(telescope, parallax_model, North_vector, East_vector)

Compute and set the deltas_positions attributes of the telescope object inside. deltas_positions is the offset between the position of the observatory at the time t, and the center of the Earth at the date t0_par. See https://ui.adsabs.harvard.edu/abs/2004ApJ…606..319G/abstract

Parameters:

  • telescope (object, a telescope object)

  • parallax_model (list, [str,float] the parallax model considered)

  • North_vector (array, the North projected vector in the plane of sky)

  • East_vector (array, the East projected vector in the plane of sky)

pyLIMA.parallax.parallax.space_ephemerides(telescope, time_to_treat, data_type='photometry')

Compute the ephemerides of telescope in Space via JPL Horizons

Parameters:

  • telescope (object, a telescope object)

  • time_to_treat (array, the time in JD to treat)

  • data_type (the type of data we treat in the telescope object)

Returns:

  • satellite_positions (array, the [X,Y,Z] positions of the spacecraft relative to)

  • Earth

  • spacecraft_positions (array, the [time,ra,dec,distance] position of the spacecraft)

pyLIMA.parallax.parallax.terrestrial_parallax(sidereal_times, altitude, longitude, latitude)

Compute the position shift due to the distance of the obervatories from the Earth center. See http://adsabs.harvard.edu/abs/1995MNRAS.276L..79H

Parameters:

  • sidereal_times (array, the sidereal times of the telescope)

  • altitude (float, the telescope altitude in meter)

  • lontitude (float, the telescope longitude in degree)

  • latitude (float, the telescope latitude in degree)

Returns:

  • delta_telescope (array, the [X,Y,Z] position of the telescope relative to Earth)

  • center