To investigate the physical processes , we present observational results of the sites S234 , V582 , and IRAS 05231+3512 situated toward l = 171 \arcdeg .7–174 \arcdeg .1 .
Based on the CO line data , we find that these sites are not physically connected , and contain at least one filament ( with length > 7 pc ) .
The observed line masses ( M _ { line,obs } ) of the filaments associated with V582 and IRAS 05231+3512 are \sim 37 and \sim 28 M _ { \odot } pc ^ { -1 } , respectively .
These filaments are characterized as thermally supercritical , and harbor several clumps .
Groups of infrared-excess sources and massive B-type stars are observed toward the filament containing V582 , while a very little star formation ( SF ) activity is found around IRAS 05231+3512 .
Our results favour radial collapse scenario in the filaments harboring V582 and IRAS 05231+3512 .
In the site S234 , two filaments ( i.e .
ns1 ( M _ { line,obs } \sim 130 M _ { \odot } pc ^ { -1 } ) and ns2 ( M _ { line,obs } \sim 45 M _ { \odot } pc ^ { -1 } ) ) are identified as thermally supercritical .
An extended temperature structure at 27-30 K surrounds a relatively cold ( \sim 19 K ) \sim 8.9 pc long filament ns1 .
At least four condensations ( M _ { clump } \sim 70–300 M _ { \odot } ) are seen in ns1 , and are devoid of the GMRT 610 MHz radio emission .
The filament ns2 hosting clumps is devoid of ongoing SF , and could be at an early stage of fragmentation .
An intense SF activity , having the SF efficiency \sim 3.3 % and SF rate \sim 40–20 M _ { \odot } Myr ^ { -1 } ( for t _ { sf } \sim 1–2 Myr ) , is observed in ns1 .
The feedback of massive stars in S234 seems to explain the observed SF in the filament ns1 .