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Skynet Algorithm for Single-dish Radio Mapping. I. Contaminant-cleaning, Mapping, and Photometering Small-scale Structures

  • Authors: J. R. Martin, D. E. Reichart, D. A. Dutton, M. P. Maples, T. A. Berger, F. D. Ghigo, J. B. Haislip, O. H. Shaban, A. S. Trotter, L. M. Barnes, M. L. Paggen, R. L. Gao, C. P. Salemi, G. I. Langston, S. Bussa, J. A. Duncan, S. White, S. A. Heatherly, J. B. Karlik, E. M. Johnson, J. E. Reichart, A. C. Foster, V. V. Kouprianov, S. Mazlin, and J. Harvey

2019 The Astrophysical Journal Supplement Series 240 12.

  • Provider: AAS Journals

Caption: Figure 47.

Top row: background- and RFI-subtracted data from the right panel of Figure 43 surface-modeled with fixed weighting scales θw = 2/3 (left), 1/2 (middle), and 1/3 (right) beamwidths and zoomed in on the source. Square-root scaling is used to emphasize fainter structures. Middle row: surface models from the top row, at the locations of the background- and RFI-subtracted data (1) minus these data (residuals) and (2) re-surface-modeled for visualization. These weighting scales underestimate the peak of the source, but only by ≈4%, ≈2%, and <1%, respectively, and overestimate the base of the source, corresponding to additional blurring of the source, but only by ≈1%, ≈1/2%, and <1/4%, respectively. Weighting scales θw < 1/3 beamwidths serve only to better visualize sub-Nyquist scale structures, such as contaminants. Bottom row: same as the top row, but with fixed weighting scales θw = 1/6, 1/9, and 1/12 beamwidths. These weighting scales are too small (i.e., θw is sufficiently smaller than ﹩4/3\times {\theta }_{\mathrm{gap}}\approx 4/3\times 1/5﹩ beamwidths = 0.27 beamwidths) that the surface model is not always well constrained between data points.

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