  We present optical and ultraviolet (UV) observations of a luminous type Ia
supernova (SN Ia) SN 2015bq characterized by the early flux excess. This SN
reaches a B-band absolute magnitude at $M_B = -19.68 \pm 0.41$ mag and a peak
bolometric luminosity at $L = (1.75 \pm 0.37) \times 10^{43}$ erg s$^{-1}$,
with a relatively small post-maximum decline rate [$\Delta m_{15}(B) = 0.82 \pm
0.05$ mag]. The flux excess observed in the light curves of SN 2015bq a few
days after the explosion, especially seen in the UV bands, might be due to the
radioactive decay of $^{56}$Ni mixed into the surface. The radiation from the
decay of the surface $^{56}$Ni heats the outer layer of this SN. It produces
blue $U-B$ color followed by monotonically reddening in the early phase,
dominated iron-group lines, and weak intermediate-mass elements absorption
features in the early spectra. The scenario of enhanced $^{56}$Ni in the
surface is consistent with a large amount of $^{56}$Ni ($M_{ \rm ^{56}{\rm
Ni}}$ = 0.97 $\pm 0.20$ $M_{\odot}$) synthesized during the explosion. The
properties of SN 2015bq are found to locate between SN 1991T and SN 1999aa,
suggesting the latter two subclasses of SNe Ia may have a common origin.
