Utils¶

Row from a TCE DataFrame containing the columns period, tdur, and t0. period and tdur are in days, and t0 is in BJD.

A tuple containing the period, transit duration, and transit epoch (t0), in that order.

One-dimensional array of time values.

Transit duration in the same units as time. Used to set the spline knot spacing.

Order of the spline. Default is 3 for cubic splines.

Multiplier applied to the transit duration to set the spline knot spacing. Default is 3.0.

Spline design matrix evaluated at the normalized time values.

One-dimensional array of time values.

Piecewise polynomial design matrix with separate quadratic trends for each continuous time segment.

World Coordinate System transformation object.

Right ascension in degrees.

Declination in degrees.

Pixel column and row coordinates corresponding to the input sky coordinates.

Target right ascension in degrees.

Target declination in degrees.

Shape of the target pixel file (e.g., (n_rows, n_cols)), used to estimate the search radius.

Search radius in arcseconds. Used when mission is not specified and pixel size is unknown (default 60).

Mission name. If mission is 'tess' or 'kepler', search radius is based on tpf_shape rather than radius.

Table of sources from Gaia DR3 within the search radius, including 'ID', 'Gmag', 'pmra', 'pmdec', 'RA_ICRS', 'DE_ICRS'. Returns None if no sources found.

Source data containing at least: - 'RA_ICRS', 'DE_ICRS' in degrees - 'pmRA', 'pmDE' in mas/yr

World Coordinate System transformation object.

Observation epoch to propagate coordinates to.

Sky coordinates of catalog sources propagated to the observation epoch.

Pixel coordinates of the sources as arrays of column and row positions.

Fit parameters containing 'amplitude', 'centerx', and 'centery'.

PRF model object used to evaluate the expected spatial flux distribution. For example, a KeplerPRF or TESSPRF object.

2D array of observed pixel values.

2D array of per-pixel uncertainties.

CCD reference position as (row_origin, col_origin).

Shape of the image stamp as (n_rows, n_cols).

Flattened array of finite, uncertainty-weighted residuals.

If no finite residuals can be calculated from the input pixels.

Fit parameters containing centerx, centery, and amplitude_i for each TCE index i.

PRF model object used to evaluate the expected spatial flux distribution, such as a KeplerPRF or TESSPRF object.

Array of 2D pixel data for each TCE with shape (n_tces, n_rows, n_cols).

Array of per-pixel uncertainties with the same shape as data.

CCD reference position as (row_origin, col_origin).

Shape of the image stamp as (n_rows, n_cols).

Indices of TCEs that produce non-zero transit models and are included in the fit.

Mapping from the original TCE index to its column index in data and data_err.

Flattened array of finite, concatenated residuals across all valid TCEs.

If no valid residuals can be calculated for any TCE.

Fit parameters containing centerra, centerdec, and amplitude_i for each valid quarter or sector.

List of lkprf PRF model objects, one for each observation.

List of transit depth maps for each observation.

List of per-pixel uncertainties corresponding to data_list.

List of WCS objects used to convert sky coordinates to pixel coordinates for each observation.

List of CCD reference positions as (row_origin, col_origin) for each observation.

List of image stamp shapes as (n_rows, n_cols).

List of mappings from TCE indices to their corresponding columns in the transit depth maps.

Indices of observations containing the TCE being fitted.

Index of the TCE being fitted.

Flattened array of finite, concatenated residuals across all valid observations.

If no valid residuals can be calculated for any observation.