Table 2
List of MIR NH3 ν2 transitions searched with the TEXES instrument at the NASA IRTF under the programme 2016B064 and their previous detection in evolved stars.
Transition | Wavelength | Wavenumbera | Eup∕k | Aulb | Previous detection | Ref. for |
---|---|---|---|---|---|---|
(μm) | (cm−1) | (K) | (s−1) | in evolved starsc | detection | |
sQ(1, 1) | 10.33060 | 967.997763 | 1414.86 | 7.94 | ||
sQ(2, 2)d | 10.33337 | 967.738421 | 1455.67 | 10.57 | ||
sQ(3, 3) | 10.33756 | 967.346340 | 1514.19 | 11.60 | ||
sQ(4, 4) | 10.34324 | 966.814717 | 1590.39 | 12.67 | ||
sQ(5, 5) | 10.35035 | 966.151127 | 1684.27 | 13.20 | ||
sQ(6, 6) | 10.35890 | 965.353911 | 1795.79 | 13.58 | ||
aR(0, 0) | 10.50667 | 951.776244 | 1369.39 | 5.49 | IRC +10420, VX Sgr | 1 |
VY CMa | 1, 2 | |||||
NML Cyg | 2 | |||||
IRC +10216 | 2, 3, 4, 5 | |||||
sP(1, 0)e | 10.54594 | 948.232047 | 1391.77 | 14.88 | NML Cyg | 2 |
aQ(1, 1) | 10.73390 | 931.627754 | 1363.67 | 7.74 | ||
aQ(2, 2) | 10.73730 | 931.333249 | 1404.43 | 10.32 | IRC +10216 | 2, 4, 6, 7 |
VY CMa | 1, 2, 8 | |||||
o Cet | 9 | |||||
aQ(3, 3) | 10.74394 | 930.757028 | 1462.69 | 11.60 | VY CMa | 2 |
IRC +10216 | 2, 4, 8 | |||||
aQ(4, 4) | 10.75387 | 929.898108 | 1538.44 | 12.36 | IRC +10216 | 4 |
aQ(5, 5) | 10.76711 | 928.754479 | 1631.64 | 12.86 | ||
aQ(6, 6) | 10.78373 | 927.323036 | 1742.27 | 13.22 | IRC +10216 | 2, 4, 6 |
VY CMa | 2, 8 | |||||
Notes. a The uncertainties of the wavenumbers are smaller than 0.000004 cm −1 (~ 0.0013 km s−1). The wavenumbers and uncertainties are computed from the data in supplementary material 6 of Chen et al. (2006), which is also publicly available at https://library.osu.edu/projects/msa/jmsa_06.htm.
b The Einstein A coefficient. The values are retrieved from Table S1 of Yu et al. (2010, supplementary material).
c Additional ν2 transitions have been detected towards the red hypergiants VY CMa and NML Cyg by Goldhaber (1988) and towards IRC +10216 by Holler (1999; quoted in Monnier et al. 2000b). Schrey (1986) also reported detection of sQ(2, 1) or sQ(2, 2) absorption towards the Mira-type AGB star R Leonis; however, the purported detection had very low S/N ratios in the spectra and the position of the more probable sQ(2, 2) line was too far away from the suspected absorption features.
References. (1) McLaren & Betz (1980); (2) Goldhaber (1988); (3) Betz & McLaren (1980); (4) Keady & Ridgway (1993); (5) Fonfría et al. (2017); (6) Betz et al. (1979); (7) Monnier et al. (2000c); (8) Monnier et al. (2000b); (9) Betz & Goldhaber (1985).
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