*The median values are computed over the observed field, for each velocity range, and for a signal-to-noise ratio |$\mathit {SNR}>5$|⁠. (1) Name of the structure identified in the given velocity range. (2) Velocity range identified from the PV diagrams (see figure 5 and subsection 3.2). (3) Optical depth of the |$^{13}\rm {CO}$| emission calculated using equation (1) from Shimajiri et al. (2014), assuming an excitation temperature of 10 K in local thermodynamic equilibrium (LTE) conditions, and a filling factor of 1. The peak brightness temperature of the |$^{13}\rm {CO}$| emission over the observed region has been derived using the MOMENT task in MIRIAD for each velocity range. (4) |$\mathit {FWHM}$| line width of the |$^{13}\rm {CO}$| spectra derived using the MOMENT task in MIRIAD for each velocity range. (5) H₂ molecular gas column density derived from |$^{13}\rm {CO}$| column densities calculated using equation (2) from Shimajiri et al. (2014), assuming a fractional abundance of |$^{13}\rm {CO}$| with respect to H₂ of 1.7 × 10⁻⁶ (Frerking et al. 1982). (6) Extent of the emitting structure along the line of sight estimated from the column density given in (5) for a critical density of 2 × 10³ cm⁻³. (7) to (10) Same as (3) to (6) for the C¹⁸O emission, with a fractional abundance of C¹⁸O with respect to H₂ of 1.7 × 10⁻⁷ and a critical density of 5 × 10³ cm⁻³.

^†Median values for the five structures.