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gastro
0.1.0
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This is the simplest model: we fit one scale per CCD and we do not align the exposures. More...
#include <photmodel.h>
Public Member Functions | |
| CCDgStars (unsigned int nstarmax=2000, unsigned int nccdmax=35) | |
| void | InitPars (Vect &pars) const |
| Initialize the fit from the PhotFitter information. More... | |
| int | NGroups () const |
| parameter groups | |
| unsigned int | GroupIndex (int igroup) const |
| group index | |
| unsigned int | Size (int igroup=-1) const |
| return the max size of the model | |
| unsigned int | NPar (int igroup=-1) const |
| return the size of the parameter std::list | |
| unsigned int | NFittedPhotFactors () const |
| return the total number of fitted phot factors | |
| unsigned int | NFittedStars () const |
| return the total number of fitted stars | |
| bool | CanCompute (const MeasuredStar &var, Vect &pars) const |
| set the pars(i) to 1 (if the corresponding par is a ref) or 2 (if the corresponding par is fitted) leave it to zero otherwise | |
| void | InitIndexTables (Vect const &pars) |
| Init the index tables. | |
| bool | Compute (const MeasuredStar &var, const Vect &pars, double &val, Vect &deriv) const |
| main method: compute the model value and its derivatives | |
| void | SetRefCCD (unsigned int ccd, double scale=1.) |
| Declare a given CCD as reference. | |
| void | ReleaseRefCCD (unsigned int ccd) |
| void | SetExclCCD (unsigned int ccd) |
| int | GetPhotFactorIndex (MeasuredStar const &) const |
| return the ccdimage photometric factor index in the parameter std::vector we give the measured star because we may also need information on other stuff, such as star related information. More... | |
| int | GetStarFluxIndex (MeasuredStar const &) const |
| return the star flux index in the parameter std::vector we give the measured star in arg because we may also need information on other stuff, such as the obs band for example. More... | |
| void | UpdateFittedStar (FittedStar &fs, Vect const &pars, Vect const &epars) const |
| update the internal parameters of the fitted star | |
This is the simplest model: we fit one scale per CCD and we do not align the exposures.
There is one (possibly more) CCD chosen as a reference CCD
f_measured(star,ccd) = scale(ccd) * f_fitted(star)
| int CCDgStars::GetPhotFactorIndex | ( | MeasuredStar const & | ms | ) | const |
return the ccdimage photometric factor index in the parameter std::vector we give the measured star because we may also need information on other stuff, such as star related information.
| int CCDgStars::GetStarFluxIndex | ( | MeasuredStar const & | ms | ) | const |
return the star flux index in the parameter std::vector we give the measured star in arg because we may also need information on other stuff, such as the obs band for example.
| void CCDgStars::InitPars | ( | Vect & | pars | ) | const |
Initialize the fit from the PhotFitter information.
Initialize the parameter std::vector assign the fitted pars to FP_INFINITE and the reference (fixed) pars to their normal value
Maybe useful sometimes maybe we cannot initiate anything with a FP_INFINITE parameter std::vector
1.8.6
