| Attribute name | Attribute type | Docstring | Unit |
|---|
| centroid | str | Centroiding method to use for objects in the field of view. "gaussian" and "moffat" use 2D fits to derive the centroid, "box" is a simple centroid in a square box. {gaussian,moffat,box} | |
| darcheck | str | Carry out a check of the theoretical DAR correction using source centroiding. If "correct" it will also apply an empirical correction. {none,check,correct} | |
| detsigma | float | Source detection sigma level to use. If this is negative, values between its absolute and 1.0 are tested with a stepsize of 0.1, to find an optimal solution. | |
| faccuracy | float | Factor of initial accuracy relative to mean positional accuracy of the measured positions to use for pattern matching. If this is set to zero, use the quadruples based method. | |
| lambdamax | float | Cut off the data above this wavelength after loading the pixel table(s). | |
| lambdamin | float | Cut off the data below this wavelength after loading the pixel table(s). | |
| lambdaref | float | Reference wavelength used for correction of differential atmospheric refraction. The R-band (peak wavelength ~7000 Angstrom) that is usually used for guiding, is close to the central wavelength of MUSE, so a value of 7000.0 Angstrom should be used if nothing else is known. A value less than zero switches DAR correction off. | |
| niter | int | Number of iterations of the astrometric fit. | |
| object_id | oidtype | The object identifier
The object identifier is an attribute shared by all persistent
instances. It is the prime key, by which object identity is established | |
| radius | float | Initial radius in pixels for pattern matching identification in the astrometric field. | |
| recipe_version | int | Version of the recipe | |
| rejsigma | float | Rejection sigma level of the astrometric fit. | |
| rotcenter | str | Center of rotation of the instrument, given as two comma-separated floating point values in pixels. | |
