Table 2
Observed transitions, frequencies, beam sizes, and telescope efficiencies.
| Line | Freq. (MHz)(a) | θHPBW (”)(b) |  |
|---|---|---|---|
| D13CN 1 → 0 | 71 175.07 | 24 | 0.36 |
| D15N13C 1 → 0 | 72 310.79 | 24 | 0.36 |
| DCN 1 → 0 | 72 414.69 | 24 | 0.36 |
| DN13C 1 → 0 | 73 367.75 | 24 | 0.35 |
| D15NC 1 → 0 | 75 286.77 | 24 | 0.33 |
| DNC 1 → 0 | 76 305.70 | 23 | 0.32 |
| H13C15N 1 → 0 | 83 727.58 | 21 | 0.27 |
| H15N13C 1 → 0 | 85 258.92 | 21 | 0.26 |
| HC15N 1 → 0 | 86 054.97 | 21 | 0.25 |
| H13CN 1 → 0 | 86 339.92 | 21 | 0.25 |
| HN13C 1 → 0 | 87 090.83 | 21 | 0.24 |
| HCN 1 → 0 | 88 631.60 | 20 | 0.24 |
| H15NC 1 → 0 | 88 865.69 | 20 | 0.24 |
| HNC 1 → 0(c) | 90 663.57 | 27 | 0.85 |
Notes. (a)The frequencies shown here do not consider hyperfine splitting. The frequencies are taken from the CDMS catalog (Müller et al. 2001, 2005; Endres et al. 2016) except those of the DN13C and D15NC lines, taken from the SLAIM catalog, available in Splatalogue (Remijan et al. 2007).(b)Yebes 40 m and IRAM 30 m telescope efficiencies taken from the Yebes 40 m technical information webpage and IRAM 30m efficiencies wiki, respectively. (c)Data from the IRAM 30 m Large Program GEMS (PI. Asunción Fuente).
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