Table 2.
Overview of the observations.
| BAT ID | Telescope | Project Code | Obs. Year/Month | σcube | Chan. Width | Synthesized Beam (PA) |
|---|---|---|---|---|---|---|
| (mJy beam−1) | (km s−1) | (arcsec × arcsec) (deg) | ||||
| 33 | VLA* | AH417(C), AH372(D) | Nov90, Nov89 | 0.28 | 10.3 | 49.5 × 44.3 (+46.8) |
| 64 | VLA* | 20A-123a, 23B-079b | Mar20, Nov23 | 0.52 | 20.0 | 40.7 × 36.1 (+81.8) |
| 83 | ATCA | C3311c | Aug19 | 1.14 | 20.0 | 221.7 × 84.1 (+1.2) |
| 96 | VLA* | 20A-123a, 23B-079b | Mar20, Oct23 | 1.43 | 20.0 | 49.8 × 33.7 (+16.0) |
| 129 | VLA* | AL516(D) | Oct81, Jul00 | 0.60 | 20.6 | 59.6 × 52.8 (+72.9) |
| 133 | GMRT | 20_034 | Aug11 | 0.81 | 27.5 | 27.5 × 17.3 (+23.6) |
| 310 | VLA | 23B-079b | Nov23 | 0.64 | 20.0 | 71.7 × 55.7 (−66.0) |
| 382 | VLA* | 20A-123a, 23B-079b | Feb20, Nov23 | 0.46 | 20.0 | 38.5 × 36.0 (+84.6) |
| 385 | VLA | AL516(D) | Aug00 | 1.23 | 20.6 | 102.8 × 50.5 (−68.1) |
| 400 | VLA* | 20A-123a, 23B-079b | Feb20, Oct23 | 0.45 | 20.0 | 32.5 × 22.5 (−65.5) |
| 451 | VLA | AG645(D) | Feb03 | 0.91 | 20.6 | 65.1 × 56.5 (−82.1) |
| 484 | WSRT | Shafi et al. (2015) | Jan04 | 0.12 | 16.5 | 32.9 × 29.1 (+4.3) |
| 654 | VLA | 16A-269(C) | Mar16 | 0.41 | 20.0 | 22.5 × 15.4 (+6.5) |
| 665 | VLA* | AW701(C), AP270(D) | Aug93, Dec93 | 0.42 | 20.6 | 33.4 × 31.3 (+70.8) |
| 687 | VLA* | 20A-123a, 23B-079b | Apr20, Nov23 | 0.46 | 20.0 | 22.4 × 17.7 (−35.3) |
| 733 | VLA* | 20A-123a, 23B-079b | May20, Nov23 | 0.95 | 20.0 | 44.2 × 32.7 (+36.5) |
| 766 | VLA | 23B-079b | Nov23 | 0.60 | 20.0 | 53.5 × 50.0 (−26.3) |
| 828 | VLA* | 20A-123a, 23B-079b | May20, Oct23 | 0.48 | 20.0 | 43.0 × 27.4 (−38.2) |
| 1162 | VLA* | 20A-123a, 23B-079b | Mar20, Nov23 | 0.47 | 20.0 | 42.3 × 29.5 (+48.1) |
| 1184 | VLA* | 14B-396(C), AE175(D) | Nov14, Jun10 | 0.39 | 20.0 | 39.9 × 30.7 (+5.5) |
| 1198 | VLA* | AL542(C), AL516(D) | Sep01, Jul00 | 0.37 | 20.6 | 35.1 × 32.1 (−1.4) |
| 1202 | VLA* | 20A-123a, 23B-079b | Mar20, Jan24 | 0.50 | 20.0 | 35.0 × 32.4 (−80.1) |
Notes. The observational information of our sample for the VLA and ATCA observations, and collected archival data, including the GMRT. The channel width is smoothed to ∼20 km s−1, except NGC 262 and NGC 3079 for which the initial channel resolutions were used. Our own observations are footnoted – aPI: Aeree Chung, bPI: Jeein Kim, cPI: O. Ivy Wong, *C- and D-configuration data combined.
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