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Extensive and independent observations of Type Ia supernova (SN Ia) SN 2013dyare presented, including a larger set of $UBVRI$ photometry and optical spectrafrom a few days before the peak brightness to $\sim$ 200 days after explosion,and ultraviolet (UV) photometry spanning from $t \approx -10$ days to $t\approx\ +15$ days referring to the $B$ band maximum. The peak brightness(i.e., $M_{\rm B} = -19.65 \pm 0.40$ mag, $L_{\rm max} = [1.95 \pm 0.55] \times10^{43}$ erg s$^{-1}$) and the mass of synthesised $^{56}$Ni (i.e.,$M$($^{56}$Ni) = 0.90 $\pm$ 0.26 M$_{\odot}$) are calculated, and they conformto the expectation for a SN Ia with a slow decline rate (i.e., $\Deltam_{15}(B)$ = 0.90 $\pm$ 0.03 mag, Phillips 1993). However, the near infrared(NIR) brightness of this SN (i.e., $M_{\rm H} = -17.33 \pm 0.30$ mag) is atleast 1.0 mag fainter than usual. Besides, spectroscopy classification revealsthat SN 2013dy resides on the border of "core normal" and "shallow silicon"subclasses in the Branch et al. (2009) classification scheme, or on the borderof the "normal velocity" SNe Ia and 91T/99aa-like events in the Wang et al.(2009a) system. These suggest that SN 2013dy is a slow-declining SN Ia locatedon the transitional region of nominal spectroscopic subclasses and might not bea typical normal sample of SNe Ia.

UV-Optical Observation of Type Ia Supernova SN 2013dy in NGC 7250