Aperture photometry functions for Julia
In astronomy, aperture photometry is summing an image's pixel values within some region. It is often used to measure the brightness of objects (such as stars or galaxies) that extend over many pixels. While this is basically a simple sum operation, it is often desireable to account for noise (possibly stored in a separate array) and masked ("bad") pixels. It is also desirable to account for precise overlap between the region and pixel boundaries in order to reduce sampling noise in the aperture.
Example:
flux, fluxerr = sum_circle(data, 5.0, 5.0, 3.0)sum_circle(data, x, y, r; error=nothing, mask=nothing,
maskthresh=false, gain=1.0)Sum within a circle centered at x, y with radius r.
sum_circann(data, x, y, rin, rout; error=nothing, mask=nothing,
maskthresh=false, gain=1.0)Sum within the circular annulus with inner radius rin and outer radius rout.
sum_ellipse(data, x, y, a, b, theta; error=nothing, mask=nothing,
maskthresh=false, gain=1.0)Sum within the ellipse with semi-major axis a, semi-minor axis b and
angle theta (angle of semi-major axis measured counter-clockwise from the
positive x axis).
In all cases, data is a 2-d array and the sum and error on the sum are
returned. The exact overlap between pixels and the aperture is calculated.
The error is calculated as sqrt(sum(sigma_i^2) + flux/gain).
Optional arguments:
-
error: standard deviation uncertainty on each pixel. Can be an array, a scalar (in which case the value applies to all pixels in the aperture), ornothing, which is equivalent to zero. -
gain: conversion factor between data array values and Poisson counts. See formula for error calculation above. -
mask: array giving masked pixels. Any element type is accepted pixels are considered masked if the value of the mask array is strictly greater thanmaskthresh.
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