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. Author manuscript; available in PMC: 2017 Mar 3.
Published in final edited form as: Astron Astrophys. 2017 Feb 21;599:A20. doi: 10.1051/0004-6361/201629445

Table 1.

Properties of the observed lines: wavelength (λ), transition, critical density (ncrit), upper level energy temperature (Eu/k), and Einstein coefficient (Aij). Numbers in parenthesis are power of 10. The critical densities have been calculated using the collisional rates with a) ortho-H2 (Offer et al. 1994), b) He (Hammami et al. 2008; Hammami et al. 2009), c) H2 (Yang et al. 2010), d) H0 (Launay & Roueff 1977), and e) para-H2 (Dubernet & Grosjean 2002; Phillips et al. 1996).

λ [µm] transition ncrit [cm−3] Eu/k [K] Aij [s−1]
OH 84.6 2Π3/2 J=7/2-5/2+ 1 (10)a 291 5.20 (-01)
OH 119.4 2Π3/2 J=5/2+-3/2 1 (09)a 120 1.38 (-01)
CH+ 119.8 J=3-2 4 (09)b 240 2.20 (-01)
CH+ 179.6 J=2-1 6 (08)b 120 6.10 (-02)
CH+ 359.0 J=1-0 7 (07)b 40 6.36 (-03)
CO 137.3 J=19-18 5 (06)c 1050 6.65 (-04)
13CO 227.1 J=12-11 2 (06)c 412 1.52 (-04)
C18O 341.5 J=8-7 6 (05)c 190 4.47 (-05)
[CII] 157.7 2P3/2-2P1/2 3 (03)d 91 2.29 (-06)
[OI] 145.5 3P0-3P1 2 (05)d 327 1.66 (-05)
H2O 269.3 111-000 1 (09)e 53 1.84 (-02)
H2O 398.7 211-200 3 (08)e 137 7.05 (-03)