Star formation toward the H~II region IRAS 10427-6032
  The formation and properties of star clusters formed at the edges of H II
regions are poorly known. We study stellar content, physical conditions, and
star formation processes around a relatively unknown young H II region IRAS
10427-6032, located in the southern outskirts of the Carina Nebula. We make use
of near-IR data from VISTA, mid-IR from Spitzer and WISE, far-IR from Herschel,
sub-mm from ATLASGAL, and 843 MHz radio-continuum data. Using multi-band
photometry, we find a total of 5 Class I and 29 Class II young stellar object
(YSO) candidates, most of which newly identified, in the 5'$\times$5' region
centered on the IRAS source position. Modeling of the spectral energy
distribution for selected YSO candidates using radiative transfer models shows
that most of these candidates are intermediate mass YSOs in their early
evolutionary stages. A majority of the YSO candidates are found to be
coincident with the cold dense clump at the western rim of the H II region.
Lyman continuum luminosity calculation using radio emission indicates the
spectral type of the ionizing source to be earlier than B0.5-B1. We identified
a candidate massive star possibly responsible for the H II region with an
estimated spectral type B0-B0.5. The temperature and column density maps of the
region constructed by performing pixel-wise modified blackbody fits to the
thermal dust emission using the far-IR data show a high column density
shell-like morphology around the H II region, and low column density (0.6
$\times$ 10$^{22}$ cm$^{-2}$) and high temperature ($\sim$21 K) matter within
the H II region. Based on the morphology of the region in the ionized and the
molecular gas, and the comparison between the estimated timescales of the H II
region and the YSO candidates in the clump, we argue that the enhanced
star-formation at the western rim of the H II region is likely due to
compression by the ionized gas.
