  In the interstellar medium, the amide-type molecules play an important role
in the formation of the prebiotic molecules in the hot molecular cores or
high-mass star formation regions. The complex amide-related molecule cyanamide
(NH$_{2}$CN) is known as one of the rare interstellar molecule which has played
a major role in the formation of urea (NH$_{2}$CONH$_{2}$). In this article, we
presented the detection of the emission lines of cyanamide (NH$_{2}$CN) towards
the hot molecular core G10.47+0.03 between the frequency range 158.49$-$160.11
GHz using the Atacama Large Millimeter/submillimeter Array (ALMA)
interferometric radio telescope. The estimated column density of the emission
lines of NH$_{2}$CN using the rotational diagram model was $N$(NH$_{2}$CN) =
(6.60$\pm$0.1)$\times$10$^{15}$ cm$^{-2}$ with rotational temperature
($T_{rot}$) = 201.2$\pm$3.3 K. The fractional abundance of NH$_{2}$CN with
respect to H$_{2}$ towards G10.47+0.03 was $f$(NH$_{2}$CN) =
5.076$\times$10$^{-8}$. Additionally, we estimated the NH$_{2}$CN/NH$_{2}$CHO
abundance ratio towards the G10.47+0.03 was 0.170, which was nearly similar
with NH$_{2}$CN/NH$_{2}$CHO abundance ratio towards IRAS 16293$-$2422 B and Sgr
B2 (M). We found that the observed abundance of NH$_{2}$CN with respect to
H$_{2}$ towards G10.47+0.03 fairly agrees with the theoretical value predicted
by Garrod (2013). We also discussed the possible formation and destruction
pathways of NH$_{2}$CN.
