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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 Eupk 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.

d Potentially blended with telluric CO2 R(8) absorption at 967.707233 cm−1.

e Potentially blended with telluric o-H2O –110,11 absorption at 948.262881 cm−1.

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