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The radio astronomy community is currently building a number of phased arraytelescopes. The calibration of these telescopes is hampered by the fact thatcovariances of signals from closely spaced antennas are sensitive to noisecoupling and to variations in sky brightness on large spatial scales. Theseeffects are difficult and computationally expensive to model. We propose tomodel them phenomenologically using a non-diagonal noise covariance matrix. Theparameters can be estimated using a weighted alternating least squares (WALS)algorithm iterating between the calibration parameters and the additivenuisance parameters. We demonstrate the effectiveness of our method using datafrom the low frequency array (LOFAR) prototype station.

Self-Calibration of Radio Astronomical Arrays With Non-Diagonal Noise Covariance Matrix