Table 1
Observations of 14NH3 lines in the radio and submillimetre wavelengths.
| Transition | Rest frequencya | Energya,b | Telescope/instrument | Band | Ref. for |
|---|---|---|---|---|---|
| JK(sym) | (MHz) | (K) | line freq. | ||
| 11(a)–11(s) | 23 694.4955(2) | 23.26 | VLA | K (radio) | 1 |
| 22(a)–22(s) | 23 722.6333(2) | 64.45 | VLA | K (radio) | 1 |
| 33(a)–33(s) | 23 870.1292(2) | 123.54 | VLA | K (radio) | 1 |
| 44(a)–44(s) | 24 139.4163(2) | 200.52 | VLA | K (radio) | 2 |
| 55(a)–55(s) | 24 532.9887(2) | 295.37 | VLA | K (radio) | 2 |
| 66(a)–66(s) | 25 056.03(1) | 408.06 | VLA | K (radio) | 3 |
| v2 = 1 21(s)–11(a) | 140 141.807(23) | 1421.59 | IRAM/EMIR | E150 | 4 |
| 10(s)–00(a) | 572 498.160(2) | 27.48 | Herschel/HIFI | 1b | 5 |
| 21(s)–11(a) | 1 168 452.39(2) | 79.34 | Herschel/HIFI | 5a | 6 |
| 20(a)–10(s) | 1 214 852.94(2) | 85.78 | Herschel/HIFI | 5a | 6 |
| 21(a)–11(s) | 1 215 245.71(2) | 80.45 | Herschel/HIFI | 5a | 6 |
| 30(s)–20(a) | 1 763 524.4(1) | 170.42 | Herschel/HIFI | 7a | 7 |
| 31(s)–21(a) | 1 763 601.2(1) | 165.09 | Herschel/HIFI | 7a | 7 |
| 32(s)–22(a) | 1 763 823.2(1) | 149.10 | Herschel/HIFI | 7a | 7 |
| 31(a)–21(s) | 1 808 934.6(1) | 166.16 | Herschel/HIFI | 7b | 7 |
| 32(a)–22(s) | 1 810 380.0(1) | 150.19 | Herschel/HIFI | 7b | 7 |
Notes. a The NH3 experimental line frequencies and upper-level energies are retrieved from the calculations and compilations by Yu et al. (2010). Code for original references are given in the last column. These values are the same as those in the Jet Propulsion Laboratory (JPL) catalogue (Pickett et al. 1998). The numbers shown in parentheses are the uncertainties corresponding to the last digit(s) of the quoted frequencies. The line frequencies are generally consistent with previous calculations by Poynter & Margolis (1983), except for 20 (a )–10(s) near 1214.9 GHz where the difference is about 6 MHz (~1.4 km s−1).
References. (1) Kukolich (1967); (2) Kukolich & Wofsy (1970); (3) Poynter & Kakar (1975); (4) Belov et al. (1998); (5) Cazzoli et al. (2009); (6) Winnewisser et al. (1996); (7) Yu et al. (2010).
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