Table 1
Studied ammonia lines showing at least potential maser features.
| Line | ν | Eup | Species | V | Ref. |
|---|---|---|---|---|---|
| (J, K) | (MHz) | (K) | (km s–1) | ||
| (5,2) | 20371.450 | 406.7 | para | 57 | 1 |
| (5,3) | 21285.275 | 380.4 | ortho | 57 | 2 |
| (5,4) | 22653.022 | 343.3 | para | 54+57 | 3 |
| (6,2) | 18884.695 | 577.6 | para | 54 | 2 |
| (6,3) | 19757.538 | 551.3 | ortho | 57 | 4 |
| (6,4) | 20994.617 | 514.3 | para | 57 | 5 |
| (6,6) | 25056.025 | 408.1 | ortho | 45 | 6 |
| (7,3) | 18017.337 | 750.2 | ortho | 54 | 5 |
| (7,4) | 19218.465 | 713.5 | para | 54 | 2 |
| (7,5) | 20804.830 | 666.0 | para | 54 | 3 |
| (7,6) | 22924.940 | 607.8 | ortho | 45+50 | 2 |
| (7,7) | 25715.182 | 538.6 | para | 45+50 | 2 |
| (8,5) | 18808.507 | 893.3 | para | 54 | 2 |
| (8,6) | 20719.221 | 835.5 | ortho | 45+54 | 7 |
| (9,6) | 18499.390 | 1090.9 | ortho | 45–67 | 4 |
| (9,7) | 20735.452 | 1022.6 | para | 54 | 2 |
| (9,8) | 23657.471 | 943.3 | para | 54 | 3 |
| (10,7) | 18285.434 | 1306.1 | para | 54 | 2 |
| (10,9) | 24205.287 | 1137.6 | ortho | 45+50 | 2 |
| (11,9) | 21070.739 | 1449.9 | ortho | 45+50+54 | 7 |
Notes. Frequencies (column 2) and upper state energies, Eup (column 3), were taken from the Jet Propulsion Laboratory (JPL) molecular line catalog (Pickett et al. 1998) and the Cologne Database for Molecular Spectroscopy (CDMS; Müller et al. 2005; Endres et al. 2016). Differences between lower and upper state energies correspond to approximately 1 K. Column 4 provides the ammonia species (ortho or para), while column 5 shows the approximate velocities of the maser components. Note that the term 45 km s–1 has been taken from Henkel et al. (2013). Because of a positive velocity drift, actual velocities tend to be higher by typically 2–4 km s–1. The last column provides a reference to the first detection of the respective maser line in the interstellar medium. 1: This paper; 2: Henkel et al. (2013); 3: Mauersberger et al. (1987); 4: Madden et al. (1986); 5: Mei et al. (2020); 6: Beuther et al. (2007); 7: Walsh et al. (2007).
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