Table 2
Configurations of the interferometric observations.
| VLA | WSRT | GMRT | |
|
|
|||
| No. of galaxies observed | 7* | 18 | 20** |
| Allocated observing time(hr) | 20 | 234 | 193 |
| Configuration | C | maxi-short | fixed |
| Freq. of observations (MHz) | 1362−1407 | 1362−1417 | 1380−1415 |
| Bandwidth(MHz) | 3.125 | 10.0 | 8.0 |
| Number of channels | 128 | 1024 | 256 |
| Channel width(kHz [km s-1]) | 24.4 [5.23] | 9.77 [2.09] | 31.3 [6.69] |
| Integration time(s) | 30 | 60 | 16.9 |
| No. of antennas used | 23 | 11−13 | 18−21 |
| Maximum baseline(km) | 3.4 | 2.7 | 26 |
| Minimum baseline(m) | 35 | 36 | 100 |
| Primary beam(arcmin) | 30 | 36 | 24 |
| Synthesized beam(arcsec) | 13.4 × 15.3 | 14.6 × 22.7 | 12.9 × 16.4 |
| rms noise(mJy/beam) | 0.71 | 0.55 | 0.64 |
Notes. The stated frequency of observations gives the range of central frequencies. The channel width in km s-1 is for a frequency of 1400 MHz. No. of antennas used is the number used in the Fourier transforms. Maximum and minimum baseline are valid for a complete array without projection effects. Synthesized beam sizes and rms noise levels are average values, where the rms noise is measured in individual channel maps. All observations were carried out in dual-polarization.
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