Table 1
Class I methanol maser transitions at 3 mm.
| CH3OH transition | Rest frequency | Eup | ncrit | Beam size | Vres | rms | ηf | ηmb | Scaling factor |
|---|---|---|---|---|---|---|---|---|---|
| (MHz) | (K) | (cm−3) | (″) | (km s−1) | (Jy) | (Jy K−1) | |||
| 5−1 − 40 E | 84 521.169(10) | 40.4 | 1.04 × 105 | 29 | 0.80 | 0.2 | 0.95 | 0.81 | 5.82 |
| 80 − 71 A+ | 95 169.463(10) | 83.5 | 7.29 × 105 | 26 | 0.71 | 0.2 | 0.95 | 0.81 | 5.82 |
| 11−1 − 10−2 E | 104 300.414(7) | 158.6 | 1.49 × 106 | 24 | 0.65 | 0.2 | 0.94 | 0.78 | 5.98 |
Notes. Columns 1−4 give the transition, rest frequency, upper energy level, and critical density of each methanol line. The rest frequency is adopted from Müller et al. (2004), and the critical density (calculated using a gas kinetic temperature of 100 K) is from Yang et al. (2022). Columns 5−10 give the beam size, velocity resolution, typical observed noise level, forward efficiency, main beam efficiency, and scaling factor to convert antenna temperature to flux density. Detailed information on the IRAM 30-meter telescope can be found at https://publicwiki.iram.es/Iram30mEfficiencies.
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