Volume 556, August 2013
|Number of page(s)||36|
|Section||Interstellar and circumstellar matter|
|Published online||26 July 2013|
In Table A.1, we present a frequency-sorted table of the transitions detected in the survey. In the first six columns, we give the database properties of each transition. Columns 7–10 give the Gaussian fit velocity and width, and their associated formal uncertainties. Columns 11–14 give the peak and integrated intensity, and associated uncertainty. Blending is indicated in column 15, by a B: followed by an identification of the blended line (only one B: line is given also for multiple overlapping blends). Line profile parameters (vlsr, FWHM, Tmb) are not given for the lines which are blended. For some species, such as OH and SH+, the line parameters were determined by fitting models of the hyperfine line profile to the data, these results can be seen in Table 2 and Fig. 3 and plotted with red dashed lines in figures showing examples of the data.
Transitions detected in the HIFI spectral survey of OMC-2 FIR 4.
© ESO, 2013
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