  H II regions are the signposts of massive ($M\geq\,8\,M_\odot$) star-forming
sites in our Galaxy. It has been observed that the ionizing photon rate
inferred from the radio continuum emission of H II regions is significantly
lower ($\sim$ 90%) than that inferred from far-infrared fluxes measured by
IRAS. This discrepancy in the ionizing photon rates may arise due to there
being significant amounts of dust within the H II regions or the presence of
extended emission that is undetected by high-resolution radio interferometric
observations. Here, we study a sample of eight compact and ultracompact H II
regions with extended emission to explore its role in resolving the
discrepancy. We have used observations at the uGMRT (1.25-1.45 GHz) and data
from the GLOSTAR survey (4-8 GHz) to estimate the ionizing photon rate from the
radio continuum emission. We have also estimated the ionizing photon rate from
the infrared luminosity by fitting a spectral energy distribution function to
the infrared data from the GLIMPSE, MIPSGAL, and Hi-GAL surveys. The excellent
sensitivity of the radio observations to extended emission allows us to
investigate the actual fraction of ionizing photons that are absorbed by dust
in compact and ultracompact H II regions. Barring one source, we find a direct
association between the radio continuum emission from the compact and diffuse
components of the H II region. Our study shows that the ionizing photon rates
estimated using the radio and infrared data are within reasonable agreement
(5-28%) if we include the extended emission. We also find multiple candidate
ionizing stars in all our sources, and the ionizing photon rates from the radio
observations and candidate stars are in reasonable agreement.
