Unveiling the physical conditions in NGC 6910
  Deep and wide-field optical photometric observations along with
multiwavelength archival datasets have been employed to study the physical
properties of the cluster NGC 6910. The study also examines the impact of
massive stars to their environment. The age, distance and reddening of the
cluster are estimated to be $\sim$4.5 Myr, $1.72\pm0.08$ kpc, and $
E(B-V)_{min}= 0.95$ mag, respectively. The mass function slope ($\Gamma =
-0.74\pm0.15$ in the cluster region is found to be flatter than the Salpeter
value (-1.35), indicating the presence of excess number of massive stars. The
cluster also shows mass segregation towards the central region due to their
formation processes. The distribution of warm dust emission is investigated
towards the central region of the cluster, showing the signature of the impact
of massive stars within the cluster region. Radio continuum clumps powered by
massive B-type stars (age range $\sim$ 0.07-0.12 Myr) are traced, which are
located away from the center of the stellar cluster NGC 6910 (age $\sim$ 4.5
Myr). Based on the values of different pressure components exerted by massive
stars, the photoionized gas associated with the cluster is found to be the
dominant feedback mechanism in the cluster. Overall, the massive stars in the
cluster might have triggered the birth of young massive B-type stars in the
cluster. This argument is supported with evidence of the observed age gradient
between the cluster and the powering sources of the radio clumps.
