analyse_source

sitelle.source.analyse_source(source, cube, plot=False, return_fit_params=False)

Convenience method to spatially analyse a source. A 30x30 pixels ‘flux map’ is build from the sum of a few frames around each detected lines for the source.

Two analysis are then performed:

• Aperture photometry from the center of the source, to estimate a flux growth function and fit it with a custom erf function.
• A Gaussian 2D fit of the PSF on the flux map

This method can be used in a parallel process. :param source: A row from a DataFrame containing detected sources. Should have columns xpos, ypos (Not astropy convention), velocity, *_detected whare * is a line name, containing True or False for each line. :type source: Series :param cube: SpectralCube instance where we are looking at the source :type cube: SpectralCube :param plot: (Optional) If True, the two fits are plotted :type plot: bool, Default = False :param return_fit_params: (Optional) If True, returns the full fits parameters :type return_fit_params: bool, Default = False

Returns:res – A dictionnary containing all the relevant fitted quantities.

Parameter	Description
flux_map_ks_pvalue	Estimates the ‘randomness’ of the flux map, i.e if it’s just noise or if we actually have a signal
flux_r	Flux at different radius r
flux_err_r	Flux error varying with r
erf_amplitude	Amplitude estimated from erf fit
erf_amplitude_err	Amplitude error
erf_xfwhm	x-axis fwhm from erf fit
erf_yfwhm	y-axis fwhm from erf fit
erf_fwhm	Fwhm defined as r at which half of the max flux is reached
flux_fraction_3	Ratio between flux measured at 3 pixels from the center and max flux
model_flux_fraction_15	Ratio between estimated flux at 15 pixels from the center and max flux
modeled_flux_r	Modeled flux varying with r
psf_snr	Ratio between amplitude of the 2D fit and noise in the flux map
psf_amplitude	Amplitude of the 2D fit
psf_xfwhm	x-axis fwhm from 2D fit
psf_yfwhm	y-axis fwhm from 2D fit
psf_ks_pvalue	Randomness of the residuals map

Return type:dict