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tokens: Figures 2 (a)–(f) show compressed spectra from 85 to 101 GHz toward CO Peak 1, NQC2, N79, N44C, N11B, N113, and N159W, respectively. In the preparation of these data, we corrected slight intensity variations among the subscans for 1.5 hr by using the intensity of the strongest line of the observing band. For the compressed spectra, we subtracted the baseline by using the fifth-order polynomial over the 2.2 GHz region. Although the standing waves caused by the telescope system are still visible, we were readily able to identify emission lines, because the typical line width observed toward the target sources (5 km s −1 ) is narrower than the period of the standing waves. Lines are identified with the aid of the spectral line database CDMS (Müller et al. 2001 , 2005 ). We used the 13 CO line velocity ( V LSR ) of 229, 266, 285, 282, 232, 235, and 238 km s −1 for CO Peak 1, NQC2, N11B, N44C, N79, N113, and N159W, respectively, to identify the molecular lines. We detected eight molecules (CO, 13 CO, CS, SO, CCH, HCO + , HCN, and HNC) in the seven sources, c -C 3 H 2 in N79, N44C, N11B, N113, and N159W, and CN in N79, N44C, and N113 (Table 4 ). N 2 H + is marginally detected in N113 and N159W. The detection criterion is that the line is detected at the expected velocity with the significance of 5 σ or higher in the integrated intensity. Note that the c -C 3 H 2 line was not covered with the frequency setting for CO Peak 1. Since line intensities in CO Peak 1 and NQC2 are typically weaker by a factor of 2 than the other sources, fewer lines were detected in these sources. The signal-to-noise ratio is rather poor for N113 and N159W in comparison with the previous studies (Chin et al. 1997 ; Heikkilä et al. 1999 ; Wang et al. 2009 ), and hence, only strong lines were detected in this study. Figure 2. Compressed spectra observed toward CO Peak 1 (a), NQC2 (b), N79 (c), N44C (d), N11B (e), N113 (f), N159W (g). The spectrum of the spiral arm of M51 is taken from Watanabe et al. ( 2014 ) (h). The composite spectrum of a translucent cloud is prepared by averaging the intensities of HCN, HCO + , HNC, CS, and SO observed toward 38 translucent clouds by Turner ( 1995a , 1995b , 1996 ), and Turner et al. ( 1997 ) (i). The spectrum of Orion KL (j) and NGC 2264 CMM3 (k) are taken from Watanabe et al. ( 2015 ). Note that the vertical scale is different from source to source. Table 4 Observed Line Parameters Notes. The errors are 1 σ . The upper limits are 3 σ . a Assumed. The spectral profile of each molecular line is shown in Figures 3 and 4 . For Figures 3 and 4 and Table 4 , the baselines are subtracted in a narrow range (typically 100 MHz) by using the fifth-order polynomials to remove the base line ripples. We conducted Gaussian fitting to each base-line-subtracted spectral line to obtain the V LSR , Δ v , and the peak T MB , where the observed frequencies are converted to the LSR velocities based on the rest frequency of each transition given in CDMS.