Wide-Field Wide-Band Imaging With The EVLA : Initial Results With Images And Error Estimates

Details Wide-Field Wide-Band Imaging With The EVLA : Initial Results With Images And Error Estimates Wide-Field Wide-Band Imaging With The EVLA : Initial Results With Images And Error Estimates

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21535701r&link_type=abstract

American Astronomical Society, AAS Meeting #215, #357.01; Bulletin of the American Astronomical Society, Vol. 42, p.540

Astronomy and Astrophysics

Astrophysics

Scientific paper

The introduction of broad-band receivers into radio interferometry has opened up new opportunities for the study of wide-band continuum emission from a vast range of astrophysical objects. The large instantaneous bandwidths have been designed to provide high dynamic range continuum imaging capabilities superior to that of existing radio interferometers, as well as detailed measurements of the spectral structure of astrophysical sources. However, to take full advantage of such instruments, we need image reconstruction algorithms that are sensitive to the effects of combining measurements from a large range of frequencies (namely varying angular resolution and uv-coverage, varying antenna fields-of-view, and the spectral structure of the sky brightness distribution).
In this talk I will present images of continuum Stokes-I emission, spectral index and spectral curvature for three radio sources - CygnusA, M87 and 3C286, along with error bars and comparisons with existing spectral information about these sources. These images were derived from wide-band 1-2 GHz (E)VLA data, using a new wide-field wide-band imaging algorithm developed as part of this thesis project. These results and their error-bars will illustrate our current ability to (a) take advantage of the multi-frequency uv-coverage while reconstructing both spatial and spectral structure for compact, extended and moderately resolved sources, (b) construct spectral index and spectral curvature maps at an angular resolution given by the highest frequency in the band, and (c) correct for the frequency-dependence of the antenna primary beam.
The algorithms presented here will allow observers to extract the full scientific benefit of the instantaneously-wideband data that will start flowing from the EVLA within the next few months [Perley et al., arXiv:0909.1585v1]. Early versions of these algorithms have been implemented and are being tested in the CASA software package.

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