The embedded ring-like feature and star formation activities in
  G35.673-00.847
  We present a multi-wavelength study to probe the star formation (SF) process
in 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 images
reveal a semi-ring-like feature (associated with ionized gas emission) and an
embedded 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 is
originated 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 ionized
gas emission, indicating that the ring-like feature is unlikely to be produced
by the ionizing feedback from a massive star. Several embedded Herschel clumps
and young stellar objects (YSOs) are identified in the MCG35.6, tracing the
ongoing SF activities within the cloud. The polarization information from the
Planck and GPIPS data trace the plane-of-sky magnetic field, which is oriented
parallel 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 almost
regularly spaced manner along the ring-like feature and contain noticeable
YSOs. Based on the analysis of the polarization and molecular line data, three
subregions containing the clumps are found to be magnetically supercritical in
the ring-like feature. Altogether, the existence of the ring-like feature and
the SF activities on its edges can be explained by the magnetic field mediated
process as simulated by Li & Nakamura (2002).
