Task: imcfn Purpose: Compute confusion noise for an interferometer image Categories: image analysis IMCFN computes confusion noise in an interferometer image owing to the presence of unresolved background sources. At each location (x0,y0) in the output image, the variance of the confusion noise is given by the product of 2 integrals var(x0,y0) = I1 * I2(x0,y0) where I1 is the source integral defined by - Smax I1 = | N(S) S**2 dS - Smin and I2 is the beam integral defined by -- I2(x0,y0) = || [SB(x-x0,y-y0) * PB(x,y)]**2 dx dy -- Thus, at the desired output location (x0,y0), the synthesized beam is shifted to the location (x0,y0), and then the product of the shifted beam and the primary beam is formed, and then that product squared is summed over the size of the synthesized beam image. The user is told what the source integral value is. Thus, you can in fact rescale the output image to other flux density ranges just by knowing the square root of the flux integral. The program can run without an input beam or output image whereupon just the source integral is done. This can be useful because the computation of the beam integral is very slow, as for each output pixel, a sum over an image the size of the synthesized beam must be done. The user inputs the differential and normalized source count function N(S)/N0(S) where S is the flux density. The units of N(S) are counts/Jy/steradian. The user also specifies N0, which is a cosmological normalization, usually a power law of S. This function is input via a power law and/or polynomial. A break flux density is given below which the power law is used and above which the polynomial is used. In the help file, examples are given for keyword values for the 20cm number counts. These results come from Windhorst et al 1993, ApJ, 405, 409 Key: beam Synthesised dirty beam image (must be power of 2). No default. Key: out Confusion noise (sigma) image (1/2 size of beam image) in Jy Key: flux 3 numbers (Jy). flux(1) and flux(2) define the range of flux densities for which the confusion noise is calculated. flux(3) is the break point below which the power law is used, and above which the polynomial is used. Set flux(3) above flux(2) if you wish to use only the power law. Set flux(3) below flux(1) if you wish to use only the polynomial. No defaults. For the 20cm counts, the break point is flux(3) = 1E-4 Jy The polynomial coefficients are good from flux(3) to flux(2) = 10 Jy. The power law is good from flux(1) = 1E-5 Jy to flux(3) = 1E-4 Jy. Below 1E-5 Jy the function is unknown, but must turn over and converge so as not to distort the CMB spectrum. Key: poly N(S)/N0(S) specified as a polynomial of up to 5th order fit to log10(N/N0 counts/Jy/sr) vs log10(S Jy) You input up to 6 polynomial coefficients (low to high order). For the 20cm number counts, the polynomial coefficients are 2.519192, -0.139680, -0.302235, 0.067539, 0.046945, 0.005320 See the flux keyword for the acceptable range. Key: power N(S)/N0(S) (counts/Jy/sr) specified as a power law a * S**p where S is in Jy and you give a and p. For the 20cm number counts, the power law is a = 195 and p = 0.45 See the flux keyword for the acceptable range. Key: n0 The normalization factor N0 = f * S**b where S is in Jy You give f and b. For the 20cm number counts, f = 1.0 and b = -2.5 Key: device Plot device on which to plot the differential normalized and un-normalized source count functions. You can specify a plot device but not an output or beam image if you just want to see the plots but don't want to spend ages computing the beam integral. Revision: 1.9, 2021/06/02 04:45:09 UTC

Generated by miriad@atnf.csiro.au on 02 Jun 2021