Notes. “Our detections” and “Our nondetections” were all obtained between August and December 2001. Col. (1): molecular line, (o) = ortho, (p) = para; Col. (2): redshifted frequency, adopting z = 0.88582; Col. (3): approximate rest frequency; Cols. (4) and (5): local standard of rest velocities and full width to half power (FWHP) line widths, in case of SO 1₀ ← 0₁ for both the broad and the narrow component; Cols. (6) and (7): continuum source-covering factor (see also Sect. 4.1 and Henkel et al. 2009) and corresponding peak optical depth(s); Col. (8): peak optical depths for a continuum source-covering factor of 0.38; Col. (9): estimated 1σ uncertainties in percent of the optical depth. Remarks (last column): the 6-digit numbers provide the epoch of our observations with day, month, and year from left to right. 1: possibly two line components. 2: Galactic line, tentative detection. A continuum source-covering factor of unity has been adopted. 3: E- and A-transitions seen in the same spectrum (Fig. 1). The intensities are consistent with a line strength ratio of 1:3.8. 4: upper 1σ limits of τ; spectra were smoothed to ~10 km s^-1 channels. 5: extrapolated continuum flux densities: 7.1 Jy (14 GHz) and 3.5 Jy (45 GHz). 6: calculated from Table 10 of Muller et al. (2011). 7: τ values of Menten et al. (1999) and Muller et al. (2011) agree well.