2017ApJ...848...51D

We present a multiwavelength data analysis of IRAS 05463+2652 (hereafter I05463+2652) to study star formation mechanisms. A shell-like structure around I05463+2652 is evident in the Herschel column density map, which is not associated with any ionized emission. Based on the Herschel submillimeter images, several parsec-scale filaments (including two elongated filaments, "s-fl" and "nw-fl" having lengths of ∼6.4 and ∼8.8 pc, respectively) are investigated in the I05463+2652 site. The Herschel temperature map depicts all these features in a temperature range of ∼11-13 K. 39 clumps are identified and have masses between ∼70–945 M_☉. The majority of clumps (having M_clump 300 M_☉) are distributed toward the shell-like structure. 175 young stellar objects (YSOs) are selected using the photometric 1-5 µm data and a majority of these YSOs are distributed toward the four areas of high column density ( 5×10²¹ cm^–2; A_V ∼ 5.3 mag) in the shell-like structure, where massive clumps and a spatial association with filament(s) are also observed. The knowledge of observed masses per unit length of elongated filaments and critical mass length reveals that they are supercritical. The filament "nw-fl" is fragmented into five clumps (having M_clump∼100–545 M_☉) and contains noticeable YSOs, while the other filament "s-fl" is fragmented into two clumps (having M_clump∼170–215 M_☉) without YSOs. Together, these observational results favor the role of filaments in the star formation process in I05480+2545. This study also reveals the filament "s-fl," containing two starless clumps, at an early stage of fragmentation.