Table 2
CO detections and their line parameters.
| Source | Line | Backend | Int. time | v0 | FWHM | Resol. | Tmb | rms | ICO | MH2 | ||||
| [min] | [km s-1] | [km s-1] | [km s-1] | [mK] | [mK] | [mK km s-1] | [106M⊙] | |||||||
|
|
||||||||||||||
| HaR-2 | CO(2–1) | FTS | 268 | 2224 ± 2 | 18 | ± | 3 | 4 | 9.8 | 2.0 | 186 | ± | 29 | |
| Source-1(1) | CO(2–1) | WILMA | 232 | 2579 ± 2 | 25 | ± | 5 | 5 | 6.4 | 1.7 | 173 | ± | 29 | |
| Source-1(2) | CO(2–1) | WILMA | 232 | 2732 ± 2 | 16 | ± | 5 | 5 | 5.6 | 1.7 | 99 | ± | 25 | |
|
|
||||||||||||||
| HaR-2 | CO(1–0) | WILMA | 318 | 2218 ± 4 | 26 | ± | 7 | 10 | 3.2 | 1.5 | 88 | ± | 25 | 1.1 |
| CO(2–1) | WILMA | 586 | 2226 ± 2 | 24 | ± | 6 | 10 | 6.3 | 1.6 | 163 | ± | 29 | ||
| HaR-1 | CO(1–0) | WILMA | 229 | 2212 ± 4 | 35 | ± | 13 | 10 | 5.2 | 2.3 | 199 | ± | 54 | 2.4 |
| HaR-2-4 | CO(1–0) | WILMA | 665 | 2404 ± 2 | 12 | ± | 3 | 10 | 4.0 | 1.4 | 54 | ± | 16 | 0.7 |
| NGC 4388 | CO(1–0) | WILMA | 87 | 2505 ± 2 | 289 | ± | 5 | 5 | 54.0 | 4.8 | 17 000 | ± | 276 | 205 |
| CO(2–1) | WILMA | 82 | 2493 ± 4 | 275 | ± | 7 | 5 | 67 | 8.9 | 20 000 | ± | 490 | ||
Notes. First three rows correspond to observing run 195-13. Both components shown in Fig. 2 for Source-1 are listed. H2 masses were calculated as MH2[M⊙ ] = 4.4πR2[pc] ICO[K km s-1], which uses a Galactic CO conversion factor of 2.0 × 1020 [cm-2 (K km s-1)-1] and a correction factor of 1.36 to account for heavy elements. A distance to the Virgo Cluster of 17.5 Mpc (Mei et al. 2007) was used to calculate the CO(1–0) beam radius as source radius. HaR-2 includes data taken in the first run only for CO(1–0), and data combined from both runs for CO(2–1).
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