Spectral utilities

excalibuhr.utils Module

Functions

PolyfitClip(x, y, order[, mask, clip, max_iter])	Perform weighted least-square polynomial fit, iterratively cliping pixels above a certain sigma threshold
SpecConvolve(in_wlen, in_flux, out_res[, ...])	Convolve the input spectrum to a lower resolution with a Gaussian kernel.
SpecConvolve_GL(in_wlen, in_flux, out_res, gamma)	Convolve the input spectrum to a lower resolution with a Voigt kernel, i.e. the convolution of a Gaussian and a Lorentzian kernel.
align_jitter(dt, err, pix_shift[, tw, debug])	apply flat fielding
combine_frames(dt, err[, collapse, clip, ...])	combine multiple images or spectra with error propogation
create_eso_recipe_config(eso_recipe, ...)	tomasstolker/pycrires Internal method for creating a configuration file with default values for a specified EsoRex recipe.
detector_shotnoise(im, ron[, GAIN, NDIT])	calculate the detector shotnoise map
extract_blaze(im, badpix, trace[, f0, fw, sigma])	Collpase 2D image along the cross-dispersion direction in an order-by-order basis.
extract_spec(det, det_err, badpix, trace, ...)	Extract 1D spectra from detector images
flat_fielding(det, err, flat[, debug])	apply flat fielding
func_wlen_optimization(poly, *args)	cost function for optimizing wavelength solutions
genline(wlen, wlen_id)	generate lamp model spectra for specific wavelength settings from linelist
get_PHOENIX_stellar_model(temp, wave_cut[, logg])	Get the PHOENIX stellar model.
im_order_cut(im, trace)	Cut out individual orders from the detector image
instrument_response(std, tellu, temp, vsini)	Method for calibrating spectral shape using standard star observations.
master_flat_norm(det, badpix, trace, slit_meta)	normalize master flat frame and extract balze function
measure_Gaussian_center(y, peaks, width)	measure the centers of lines by fitting guassian profiles
molecfit(input_path, spec[, wave_range, ...])	A wrapper of molecfit for telluric correction
optimal_extraction(D_full, V_full, bpm_full, ...)	Optimal extraction based on Horne(1986).
order_trace(det, badpix, slitlen[, ...])	Trace the spectral orders
peak_slit_fraction(im, trace)	locate the peak signal along the slit
readout_artifact(det, det_err, badpix, trace)	Correct for readout noise artifacts that appear like vertical strips by subtracting the inter-order average value in each column on detector.
remove_skylight(D_full, V_full, M_bpm, ...)	Remove sky background in a 2D detector image.
remove_starlight(D_full, V_full, spec_star, ...)	[EXPERIMENTAL!] Remove starlight contamination at the position of the widely separated companion in a 2D detector image.
rot_int_cmj(wave, flux, vsini[, epsilon, ...])	Adapted from Carvalho & Johns-Krull (2023).
slit_curve(fpet, une, badpix, trace, ...[, ...])	Trace the curvature of the slit and determine the wavelength solution
slit_polyval(xx, meta)	evaluate slit curvature polynomials given the pixel grid
spectral_rectify_interp(im_list, badpix, ...)	Correct for the slit-tilt by interpolating to a pixel-grid
trace_polyval(xx, tw)	evaluate trace polynomials given the pixel grid
trace_rectify_interp(im_list, trace[, debug])	Correct for the curvature of traces by interpolating to a pixel-grid pivoting on the middle of the detector
util_master_dark(dt[, combine_mode, badpix_clip])	combine dark frames; generate bad pixel map and readout noise frame
util_master_flat(dt, dark[, combine_mode, ...])	combine flat frames; generate bad pixel map
wlen_solution(fluxes, errs, w_init, transm_spec)	Method for refining wavelength solution using a quadratic polynomial correction Poly(p0, p1, p2).