Table 2: Accurately known methanol transitions detected or potentially detectable in dark clouds, frequencies, lower state energies, line strengths, and laboratory and dark cloud references.

Masera		 Transition, Jk=b Frequency (MHz)c  $E_\ell^d$ (cm-1)  $S\mu^2$ (D2) Laboratory ref.e Dark cloud ref.f

I?		 $1_1\to1_1A^{\mp}$ 834.267(2) 11.705 1.2129 Radford (1972) Slysh et al. (1995b)
  $2_{1}\to2_{1}A^{\mp}$ 2502.7785(10) 14.904 0.6725 HD73 ND
I? $3_{1}\to3_{1}A^{\mp}$ 5005.32079(20) 19.703 0.4693 HD73 Kalenskii et al. (2004)
II $2_{0}\to3_{-1}E^f$ 12 178.595(3) 13.556 1.9848 Gaines et al. (1974) Walmsley et al. (1988)
II $2_{1}\to3_{0}E$ 19 967.3961(2) 18.803 0.9224 M 85  
I $2_{2}\to2_{1}E$ 24 934.382(5) 19.469 1.5948 Gaines et al. (1974)  
I $4_{-1}\to3_{0}E$ 36 169.265(30) 18.803 2.5184 T95  
  $1_{0}\to0_{0}A^+$ 48 372.4558(7) 00.000 0.8086 HD73 Friberg et al. (1988)
  $1_{0}\to0_{0}E$ 48 376.892(10) 9.122 0.8084 T95 Kaifu et al. (2004)
  $1_{0}\to2_{-1}E$ 60 531.489(10) 8.717 1.4742 This work NO
  $1_{1}\to2_{0}E$ 68 305.640(20) 13.963 0.4573 This work  
  $2_{1}\to1_{1}A^+$ 95 914.309(5) 11.705 1.2141 This work  
  $2_{-1}\to1_{-1}E$ 96 739.362(5) 5.490 1.2133 This work Friberg et al. (1988)
  $2_{0}\to1_{0}A^+$ 96 741.375(5) 1.614 1.6171 This work Friberg et al. (1988)
  $2_{0}\to1_{0}E$ 96 744.550(5) 10.736 1.6167 This work Friberg et al. (1988)
  $2_{1}\to1_{1}E$ 96 755.511(5) 16.241 1.2443 This work Menten et al. (1988)
  $2_{1}\to1_{1}A^-$ 97 582.804(7) 11.733 1.2141 This work  
II $3_{1}\to4_{0}A^{+}$ 107 013.803(5) 16.134 3.0088 This work  
II $0_{0}\to1_{-1}E$ 108 893.963(7) 5.490 0.9784 This work Turner (1998)
  $2_{2}\to1_{1}E$ 121 689.975(10) 16.241 2.8297 T95  
  $3_{1}\to2_{1}A^+$ 143 865.801(10) 14.904 2.1584 T95  
  $3_{0}\to2_{0}E$ 145 093.707(10) 13.963 2.4249 T95  
  $3_{-1}\to2_{-1}E$ 145 097.370(10) 8.717 2.1569 T95 Turner (1998)
  $3_{0}\to2_{0}A^+$ 145 103.152(10) 4.840 2.4257 T95 Turner (1998)
  $3_{1}\to2_{1}E$ 145 131.855(10) 19.469 2.2119 T95  
  $3_{1}\to2_{1}A^-$ 146 368.342(50) 14.988 2.1585 T95  
II $2_{1}\to3_{0}A^{+}$ 156 602.413(10) 9.681 1.9963 T95  
II $1_{0}\to1_{-1}E$ 157 270.851(10) 5.490 1.4611 T95  
II $3_{0}\to3_{-1}E$ 157 272.369(10) 13.556 3.3178 T95  
II $2_{0}\to2_{-1}E$ 157 276.058(10) 8.717 2.4090 T95  
  $1_{1}\to1_{0}E$ 165 050.195(10) 10.736 1.3466 T95  
  $2_{1}\to2_{0}E$ 165 061.156(10) 13.963 2.2373 T95  
  $3_{1}\to3_{0}E$ 165 099.271(10) 18.803 3.1170 T95  
  $3_{2}\to2_{1}E$ 170 060.581(10) 19.469 3.1205 T95 ND
  $4_{1}\to3_{1}A^+$ 191 810.509(10) 19.703 3.0352 T95 ND
  $4_{0}\to3_{0}E$ 193 415.367(10) 18.803 3.2327 T95 ND
  $4_{-1}\to3_{-1}E$ 193 441.610(10) 13.556 3.0330 T95 ND
  $4_{0}\to3_{0}A^+$ 193 454.361(10) 9.681 3.2342 T95 ND
  $4_{1}\to3_{1}A^-$ 195 146.760(10) 19.870 3.0353 T95 ND
For nomenclature see also notes to Table 1. a I and II mean that these lines are class I and II maser transitions, respectively, in some non-dark cloud regions (see Table 1). f Only references reporting the first detection of a line in cold ( $T\approx 10$ K) dark clouds are listed. For non-dark cloud astronomical references to first detections, see Lovas (2003). "ND'' means that no astronomical detection is reported in the latter reference; "NO'' means that the line is not observable from the ground. g This line appears in enhanced absorption (i.e. is over-cooled) against the cosmological microwave background radiation. References in italics report observations of a given line that did not yield its detection.

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