BasicPSFPhotometry¶

class
photutils.
BasicPSFPhotometry
(group_maker, bkg_estimator, psf_model, fitshape, finder=None, fitter=<astropy.modeling.fitting.LevMarLSQFitter object>, aperture_radius=None)[source]¶ Bases:
object
This class implements a PSF photometry algorithm that can find sources in an image, group overlapping sources into a single model, fit the model to the sources, and subtracting the models from the image. This is roughly equivalent to the DAOPHOT routines FIND, GROUP, NSTAR, and SUBTRACT. This implementation allows a flexible and customizable interface to perform photometry. For instance, one is able to use different implementations for grouping and finding sources by using
group_maker
andfinder
respectivelly. In addition, sky background estimation is performed bybkg_estimator
.Parameters: group_maker : callable or
GroupStarsBase
group_maker
should be able to decide whether a given star overlaps with any other and label them as beloging to the same group.group_maker
receives as input anTable
object with columns named asid
,x_0
,y_0
, in whichx_0
andy_0
have the same meaning ofxcentroid
andycentroid
. This callable must return anTable
with columnsid
,x_0
,y_0
, andgroup_id
. The columngroup_id
should cotain integers starting from1
that indicate which group a given source belongs to. See, e.g.,DAOGroup
.bkg_estimator : callable, instance of any
BackgroundBase
subclass, or Nonebkg_estimator
should be able to compute either a scalar background or a 2D background of a given 2D image. See, e.g.,MedianBackground
. If None, no background subtraction is performed.psf_model :
astropy.modeling.Fittable2DModel
instancePSF or PRF model to fit the data. Could be one of the models in this package like
DiscretePRF
,IntegratedGaussianPRF
, or any other suitable 2D model. This object needs to identify three parameters (position of center in x and y coordinates and the flux) in order to set them to suitable starting values for each fit. The names of these parameters should be given asx_0
,y_0
andflux
.prepare_psf_model
can be used to prepare any 2D model to match this assumption.fitshape : int or length2 arraylike
Rectangular shape around the center of a star which will be used to collect the data to do the fitting. Can be an integer to be the same along both axes. E.g., 5 is the same as (5, 5), which means to fit only at the following relative pixel positions: [2, 1, 0, 1, 2]. Each element of
fitshape
must be an odd number.finder : callable or instance of any
StarFinderBase
subclasses or Nonefinder
should be able to identify stars, i.e. compute a rough estimate of the centroids, in a given 2D image.finder
receives as input a 2D image and returns anTable
object which contains columns with names:id
,xcentroid
,ycentroid
, andflux
. In whichid
is an integervalued column starting from1
,xcentroid
andycentroid
are center position estimates of the sources andflux
contains flux estimates of the sources. See, e.g.,DAOStarFinder
. Iffinder
isNone
, initial guesses for positions of objects must be provided.fitter :
Fitter
instanceFitter object used to compute the optimized centroid positions and/or flux of the identified sources. See
fitting
for more details on fitters.aperture_radius : float or None
The radius (in units of pixels) used to compute initial estimates for the fluxes of sources. If
None
, one FWHM will be used if it can be determined from the`psf_model
.Notes
Note that an ambiguity arises whenever
finder
andinit_guesses
(keyword argument fordo_photometry
) are both notNone
. In this case,finder
is ignored and initial guesses are taken frominit_guesses
. In addition, an warning is raised to remaind the user about this behavior.If there are problems with fitting large groups, change the parameters of the grouping algorithm to reduce the number of sources in each group or input a
star_groups
table that only includes the groups that are relevant (e.g. manually remove all entries that coincide with artifacts).References
 [1] Stetson, Astronomical Society of the Pacific, Publications,
 (ISSN 00046280), vol. 99, March 1987, p. 191222. Available at: http://adsabs.harvard.edu/abs/1987PASP…99..191S
Attributes Summary
aperture_radius
fitshape
Methods Summary
__call__
(*args, **kwargs)Performs PSF photometry. do_photometry
(*args, **kwargs)Perform PSF photometry in image
.get_residual_image
()Returns an image that is the result of the subtraction between the original image and the fitted sources. nstar
(image, star_groups)Fit, as appropriate, a compound or single model to the given star_groups
.Attributes Documentation

aperture_radius
¶

fitshape
¶
Methods Documentation

__call__
(*args, **kwargs)[source]¶ Performs PSF photometry. See
do_photometry
for more details including the__call__
signature.

do_photometry
(*args, **kwargs)[source]¶ Perform PSF photometry in
image
.This method assumes that
psf_model
has centroids and flux parameters which will be fitted to the data provided inimage
. A compound model, in fact a sum ofpsf_model
, will be fitted to groups of stars automatically identified bygroup_maker
. Also,image
is not assumed to be background subtracted. Ifinit_guesses
are notNone
then this method usesinit_guesses
as initial guesses for the centroids. If the centroid positions are set asfixed
in the PSF modelpsf_model
, then the optimizer will only consider the flux as a variable.Parameters: image : 2D arraylike,
ImageHDU
,HDUList
Image to perform photometry.
init_guesses: `~astropy.table.Table`
Table which contains the initial guesses (estimates) for the set of parameters. Columns ‘x_0’ and ‘y_0’ which represent the positions (in pixel coordinates) for each object must be present. ‘flux_0’ can also be provided to set initial fluxes. If ‘flux_0’ is not provided, aperture photometry is used to estimate initial values for the fluxes. Additional columns of the form ‘<parametername>_0’ will be used to set the initial guess for any parameters of the
psf_model
model that are not fixed.Returns: output_tab :
Table
or NoneTable with the photometry results, i.e., centroids and fluxes estimations and the initial estimates used to start the fitting process. Uncertainties on the fitted parameters are reported as columns called
<paramname>_unc
provided that the fitter object contains a dictionary calledfit_info
with the keyparam_cov
, which contains the covariance matrix. Ifparam_cov
is not present, uncertanties are not reported.

get_residual_image
()[source]¶ Returns an image that is the result of the subtraction between the original image and the fitted sources.
Returns: residual_image : 2D arraylike, ImageHDU
,HDUList

nstar
(image, star_groups)[source]¶ Fit, as appropriate, a compound or single model to the given
star_groups
. Groups are fitted sequentially from the smallest to the biggest. In each iteration,image
is subtracted by the previous fitted group.Parameters: image : numpy.ndarray
Backgroundsubtracted image.
star_groups :
Table
This table must contain the following columns:
id
,group_id
,x_0
,y_0
,flux_0
.x_0
andy_0
are initial estimates of the centroids andflux_0
is an initial estimate of the flux. Additionally, columns named as<param_name>_0
are required if any other parameter in the psf model is free (i.e., thefixed
attribute of that parameter isFalse
).Returns: result_tab :
Table
Astropy table that contains photometry results.
image : numpy.ndarray
Residual image.