tokens: the site S234. The data were observed with the Giant Metrewave Radio Telescope (GMRT) facility on 2016 December 8 (Proposal Code: 31_025; PI: L. K. Dewangan). The radio data reduction was carried out using the AIPS software, in a similar manner to that given in Mallick et al. ( 2012 , 2013 ). The synthesized beam size and the rms noise of the final 610 MHz continuum map are 56 × 46 and 120 μ Jy/beam, respectively. It is expected, specifically at low frequencies, that a sufficient amount of background emission will increase the antenna temperature while observing the source. Hence, we corrected the final GMRT map at 610 MHz for system temperature (see Omar et al. 2002 ; Mallick et al. 2012 , 2013 ; Baug et al. 2015 ). More details about the procedure adopted for correction of system temperature can be found in Mallick et al. ( 2012 , 2013 ). 2.2 Archival Data Sets The multi-wavelength data sets are also retrieved from different surveys (e.g., the NRAO VLA Sky Survey (NVSS; λ = 21 cm; resolution = 45′′; Condon et al. 1998 ), the Five College Radio Astronomy Observatory (FCRAO) 12 CO (1–0) and 13 CO (1–0) line data ( λ = 2.6, 2.7 mm; resolution ∼45′′; Heyer et al. 1998 ; Brunt 2004 ), the Herschel Infrared Galactic Plane Survey (Hi-GAL; λ = 70, 160, 250, 350, 500 μ m; resolutions = 58, 12′′, 18′′, 25′′, 37′′; Molinari et al. 2010 ), the Wide Field Infrared Survey Explorer ( WISE ; λ = 3.4, 4.6, 12, 22 μ m; resolutions = 61, 64, 65, 12′′; Wright et al. 2010 ), the Warm- Spitzer IRAC 3.6 and 4.5 μ m photometric data (GLIMPSE360; λ = 3.6, 4.5 μ m; resolution = 2′′; Whitney et al. 2011 ), the UKIRT NIR Galactic Plane Survey (GPS; λ = 1.25, 1.65, 2.2 μ m; resolution ∼08; Lawrence et al. 2007 ), the Two Micron All Sky Survey (2MASS; λ = 1.25, 1.65, 2.2 μ m; resolution = 25; Skrutskie et al. 2006 ), and the Isaac Newton Telescope (INT) Photometric H α Survey of the Northern Galactic Plane (IPHAS; λ = 0.6563 μ m; resolution ∼1′′; Drew et al. 2005 )). One can learn more details of these data sets and their analysis procedures in Dewangan et al. ( 2017e ). 3 Results 3.1 Extended Features in the Direction of l = 1717–1741 To explore the extended and embedded features toward l = 1717–1741, we have employed the submillimeter image at 250 μ m, a radio continuum map at 1.4 GHz (having an rms sensitivity of ∼0.45 mJy/beam; Condon et al. 1998 ), and 12 CO ( J = 1–0) line data (having a velocity resolution of 0.25 km s −1 and an rms sensitivity of 0.25 K; Heyer et al. 1996 , 1998 ). These data enable us to depict cold dust, ionized gas, and molecular gas in the sites. Figure 1 (a) displays the submillimeter image at 250 μ m overlaid with the 1.4 GHz continuum emission contours. Figure 1 (b) shows the 12 CO emission contour map at [−17.75, −1.0] km s −1 . We have labeled at least six objects (i.e., S237, S234, IRAS 05253+3504, IRAS 05231+3512, IRAS 05220+3455, and V582) in Figures 1 (a) and (b). The submillimeter image traces a spherical shell morphology of the site
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