survey data adopted in this paper. In the selected wide-scale area, these surveys offer to examine the distribution of H$_{2}$ column densities, dust temperatures, dust clumps, ionized gas, YSOs, and gas kinematics as well as the embedded structures/morphologies.

In order to study the gas distribution toward the selected target area, the present paper employs the molecular $^{13}$CO (J=1–0) and C$^{18}$O (J=1–0) line data from the FUGIN survey [@umemoto17]. In the survey, the multi-beam receiver, FOur-beam REceiver System on the 45-m Telescope [FOREST; @minamidani16; @nakajima19], was used for the observations. The FUGIN molecular line data are calibrated in main beam temperature ($T_\mathrm{mb}$) [see @umemoto17 for more details]. The typical rms noise level ($T_\mathrm{mb}$) is $\sim$0.7 K for both the $^{13}$CO and C$^{18}$O lines [@umemoto17]. To improve sensitivities, we smoothed the FUGIN data cube with a Gaussian function having a half power beam width of 35$''$.

  Survey                                                                                       band/line(s)            Resolution ($\arcsec$)    Reference   
  ---------------------------------------------------------------------------------- -------------------------------- ------------------------ ------------- --
  NRAO VLA Sky Survey (NVSS)                                                                      21 cm                       $\sim$46           @condon98   
  FUGIN survey                                                                        $^{13}$CO, C$^{18}$O (J = 1–0)          $\sim$20          @umemoto17   
  APEX Telescope Large Area Survey of the Galaxy (ATLASGAL)                                     870 $\mu$m                   $\sim$19.2         @schuller09  
  [*Herschel*]{} Infrared Galactic Plane Survey (Hi-GAL)                                      70–500 $\mu$m                 $\sim$5.8–37        @molinari10  
  [*Spitzer*]{} MIPS Inner Galactic Plane 