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We present a multi-wavelength study to probe the star formation (SF) processin the molecular cloud linked with the G35.673-00.847 site (hereafter MCG35.6),which is traced in a velocity range of 53-62 km/s. Multi-wavelength imagesreveal a semi-ring-like feature (associated with ionized gas emission) and anembedded face-on ring-like feature (without the NVSS 1.4 GHz radio emission;where 1-sigma ~ 0.45 mJy/beam) in the MCG35.6. The semi-ring-like feature isoriginated by the ionizing feedback from a star with spectral type B0.5V-B0V.The central region of the ring-like feature does not contain detectable ionizedgas emission, indicating that the ring-like feature is unlikely to be producedby the ionizing feedback from a massive star. Several embedded Herschel clumpsand young stellar objects (YSOs) are identified in the MCG35.6, tracing theongoing SF activities within the cloud. The polarization information from thePlanck and GPIPS data trace the plane-of-sky magnetic field, which is orientedparallel to the major axis of the ring-like feature. At least five clumps(having M_clump ~ 740 - 1420 M_sun) seem to be distributed in an almostregularly spaced manner along the ring-like feature and contain noticeableYSOs. Based on the analysis of the polarization and molecular line data, threesubregions containing the clumps are found to be magnetically supercritical inthe ring-like feature. Altogether, the existence of the ring-like feature andthe SF activities on its edges can be explained by the magnetic field mediatedprocess as simulated by Li & Nakamura (2002).

The embedded ring-like feature and star formation activities in G35.673-00.847