1. 1 Owen, Rudnick, Eilek, Rau, Bhatnagar, Kogan Relics and Jets in Abell 2256 at 1.5 GHz. EVLA data : 1-2 GHz Lband A merging rich cluster of galaxies. Z=0.058, D=270Mpc. 1-2 GHz, 20-arcmin on a side (1.6Mpc)

2. 2 Owen, Rudnick, Eilek, Rau, Bhatnagar, Kogan Relics and Jets in Abell 2256 at 1.5 GHz. EVLA data : 1-2 GHz Lband Intensity-weighted Spectral Index between 1 and 2 GHz.

3. 3 Hercules A Z=0.154 radio galaxy. D=710 Mpc, 1 arcsec=3.4 Kpc 4-9 GHz color-coded spectro-intensity image ( redder = older). Resolution of 1 Kpc EVLA data : 1 through 9 GHz, all four configurations. Shocks in western lobe indicate repeated ejection Cotton & Perley

4. 4 M82 – The Prototype Nearby Starburst Galaxy - Deep C-band VLA image, combining A and B configuration data - Resolution is 0.35 arcseconds ( 5pc at distance of M82 ) - Extreme nuclear starburst driving a superwind > 1Kpc above disk - Visible are : SNR and some HII regions throughout the star-forming disk Marvil, Owen, Eilek

5. 5 Galactic Supernova Remnant : G55.7+3.4 EVLA data : 1-2 GHz. Algorithms : W-Projection, Multi-Scale, Multi-Frequency Synthesis. 1 Jy total flux 24 arcmin (PB: 30 arcmin) 10 micro Jy RMS 2x2 degree FOV Bhatnagar, Rau, Green, Rupen

6. 6 Example of wide-field sensitivity because of large instantaneous bandwidths. Wideband Primary beam has a shelf of sensitivity to very wide fields, and no 'null'. G55.7+3.4 : Galactic supernova remnant : 4 x 4 degree field-of-view from one EVLA pointing 1 Jy total flux 24 arcmin (PB: 30 arcmin) 10 micro Jy RMS Bhatnagar, Rau, Green, Rupen

7. 7 NTERMS = 1 Rms : 9 mJy -- 1 mJy DR : 1600 -- 13000 NTERMS = 2 Rms : 1 mJy -- 0.2 mJy DR : 10,000 -- 17,000 NTERMS = 4 Rms 0.14 mJy -- 80 uJy DR : >110,000 -- 180,000 NTERMS = 3 Rms : 0.2 mJy -- 85 uJy DR : 65,000 -- 170,000 Improvement in Dynamic-Range with the use of higher-order spectral modeling during wideband image reconstruction. 3C286 field, 20 minutes of data between 1 and 2 GHz. Rau, Cornwell

8. 8 50% of PB IC10 dwarf galaxy. C-band : 4-8 GHz. Comparison of spectral-index maps made with traditional and more recent methods. Left : Cube imaging, post-deconvolution PB-correction per frequency, smoothing to lowest resolution, spectral-index fits Right : Wideband imaging to reconstruct intensity and spectra simultaneously, post- deconvolution wideband PB-correction Heesen, Rau, Rupen, Brinks, Hunter,

9. 9 50% of PB Comparison of algorithms to correct for wide-field and wide-band instrumental effects. Simulation of EVLA data at L-Band. Innermost contour is the 50% level of the PB. Bhatnagar, Rau Top Left : Narrow-band imaging with post-deconvolution PB-correction Top Right : MT-MFS with post-deconvolution PB-correction Bottom Left : MT-MFS with A-Projection. Bottom Right : MT-MFS with WideBand A-Projection

10. 10 SS433 and the W50 nebula VLA - C-band Mosaic (narrow-band, multi-scale) Golap, Goss

11. 11 The sickle region near the Galactic Center ( narrow-band, multi-scale, mosaic ) Comparison of IR, 1870 nm and Radio 1.2cm (25 GHz)