Table 3.
Gaussian fits to the CO J = 2−1 integrated line brightness per beam for the detected emission in the southern field.
| Name | Offset | I2−1 | V2−1 | W2−1 | P2−1 | ΔV2−1 | rms2−1 |
|---|---|---|---|---|---|---|---|
| ... | arcsec | mK km s−1 | km s−1 | km s−1 | mK | km s−1 | mK |
| 562a | (−562,−1704) | 427 ± 84 (375) | −79.9 ± 0.4 | 4.3 ± 1.1 | 94 | −83,−77 | 16.9 |
| 562b | (−676,−1677) | 595 ± 104 (492) | −102.4 ± 0.6 | 7.2 ± 1.4 | 77 | −107,−98 | 16.1 |
| 562c | (−610,−1696) | 927 ± 100 (825) | −83.6 ± 0.3 | 6.0 ± 0.7 | 144 | −89,−80 | 17.2 |
| 562d | (−555,−1669) | 341 ± 67 (336) | −86.5 ± 0.5 | 4.5 ± 0.9 | 70 | −91,−82 | 13.4 |
Notes. The name of detected cloud clump is given in Col. 1. Column 2 gives the cloud clump offset with respect to the center of M 33. Column 3 gives the CO line intensity in main-beam temperature units computed as the area of the best-fit Gaussian function, in parentheses we list the values obtained by summing the flux in each channel of the selected spectral window. Columns 4 and 5 give the central velocity and the line width of the Gaussian fits, respectively. The signal peak and spectral window are given in Cols. 6 and 7, respectively. Column 8 gives the per channel noise level of the spectra (for a channel width of 2.6 km s−1).
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