3 Results

A total number of about 7 000 spectra has been obtained with a grid spacing of 3' in the ¹²CO (J=1-0) line. The mapped region covers most of the selected area (see Fig. 1), and is presented with dotted lines in Fig. 2. The total CO line intensity map, integrated from $v_{\rm LSR} = -25$ to 15 km s^-1, which covers the whole emission range, is represented in Fig. 2. There are several warm clumps in the main emission region, some of which correspond to regions with strong dust emission. The overlayed filled circles in Fig. 2 are the IRAS point sources with S₆₀ > 1 Jy and S₁₀₀>S₆₀. Outside the main emission area, several small patches of molecular gas are also present. Overall, spatial coincidence and close morphological similarity is found between the CO emission and the FIR dust emission as in the case of an isolated cloud (see Fig. 1). The correlation between CO emission and FIR dust emission will be discussed in Sect. 6.

We present our survey results in two standard ways: l-b contour maps integrated over a range of velocity bins, and v-b contour maps integrated over a range of longitude bins. Maps at individual velocities are shown in Fig. 3. The velocity coverage of each map is 1.3 km s^-1, which corresponds to two channels of the 250 KHz filterbank. Only $v_{\rm LSR} = -24.72$ km s^-1 to +13.00 km s^-1 is presented in this figure, as little emission is found in the rest of the velocity range. As in Fig. 2, the dotted box indicates the mapped area. The CO emission toward the Galactic Anticenter is generally weak, and the lowest contour of Fig. 3 is set to 1 K km s^-1 ($\sim 4\sigma$). In addition to contours, we employ grey-scale to discriminate the weaker emission regions from the stronger emission regions, which often appear in the typical survey data.

Figure 4 is a sequence of b-v maps integrated for $0\hbox{$.\mkern-4mu^\prime$}25$along the longitude direction, corresponding to 5 pixels in our sampling. The lowest contour is set to 2.5 K ($\sim 5 \sigma$), and a grey-scale is employed to discriminate the weaker emission region as in the case of Fig. 3. These figures represent some obviously separate clouds overlapping along the same lines of sight, which will be described in the following section.