v1.2.0

[BearBearCodes]

• Changed AB magnitude calculation to interpolate the passband to the spectrum resolution (#7)
• Added PSF convolution to all sources using CASTOR PSFs (#11)
  • The fraction of flux enclosed within the aperture is estimated from the supersampled simulated images before binning down to the telescope's resolution. This works for any aperture with that is arbitrarily centred on the source. In this way, this change fixes the normalization limitation from v1.1.1, whose reference flux assumed galaxy sources were centred on and unrotated relative to the aperture
  • Now all photometry calculations use the fraction of flux enclosed within the aperture to calculate the electrons produced per second on the detector due to the source. Note that the reference flux, which determines what we consider to be 100% of the flux, is always based on the noiseless image, i.e., with no PSF convolution
    • An enclosed flux fraction of 100% corresponds to the magnitude of the source that the user set. So if the user normalizes a spectrum to, say, an AB magnitude of 25, then this AB magnitude will be the AB magnitude of the source if 100% of its flux was contained within the aperture. If the user selects an aperture that only contains 50% of the flux, however, the effective AB magnitude will be dimmer
  • The photometry ETC is now 100% pixel-based, even for point sources. Changing any pixel in the source_weights attribute, which gives the fraction of the total flux contained within the pixel, will change the photometry calculations

See the changelog for more details.

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This discussion was created from the release v1.2.0.