File Magnitude.h¶
Utilities for converting between flux and magnitude in C++.
Use astropy.units
ABmag
and nJy
for converstions in python:
import astropy.units as u
mag = (flux*u.nJy).to_value(u.ABmag)
flux = (mag*u.ABmag).to_value(u.nJy)
-
namespace
lsst
Class for a simple mapping implementing a generic AstrometryTransform.
Remove all non-astronomical counts from the Chunk Exposure’s pixels.
Forward declarations for lsst::utils::Cache
For details on the Cache class, see the Cache.h file.
It uses a template rather than a pointer so that the derived classes can use the specifics of the transform. The class simplePolyMapping overloads a few routines.
A base class for image defects
Numeric constants used by the Integrate.h integrator routines.
Compute Image Statistics
- Note
Gauss-Kronrod-Patterson quadrature coefficients for use in quadpack routine qng. These coefficients were calculated with 101 decimal digit arithmetic by L. W. Fullerton, Bell Labs, Nov 1981.
- Note
The Statistics class itself can only handle lsst::afw::image::MaskedImage() types. The philosophy has been to handle other types by making them look like lsst::afw::image::MaskedImage() and reusing that code. Users should have no need to instantiate a Statistics object directly, but should use the overloaded makeStatistics() factory functions.
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namespace
utils
Functions
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double
nanojanskyToABMagnitude
(double flux)¶ Convert a flux in nanojansky to AB magnitude.
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double
ABMagnitudeToNanojansky
(double magnitude)¶ Convert an AB magnitude to a flux in nanojansky.
Variables
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const double
referenceFlux
= 1e23 * pow(10, ) * 1e9¶ The Oke & Gunn (1983) AB magnitude reference flux, in nJy (often approximated as 3631.0).
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double