  We present the first ground-based CCD ($\lambda < 1\mu$m) image of an
extrasolar planet. Using MagAO's VisAO camera we detected the extrasolar giant
planet (EGP) $\beta$ Pictoris b in $Y$-short ($Y_S$, 0.985 $\mu$m), at a
separation of $0.470 \pm 0.010''$ and a contrast of $(1.63 \pm 0.49) \times
10^{-5}$. This detection has a signal-to-noise ratio of 4.1, with an
empirically estimated upper-limit on false alarm probability of 1.0%. We also
present new photometry from the NICI instrument on the Gemini-South telescope,
in $CH_{4S,1\%}$ ($1.58$ $\mu m$), $K_S$ ($2.18\mu m$), and $K_{cont}$ (2.27
$\mu m$). A thorough analysis of our photometry combined with previous
measurements yields an estimated near-IR spectral type of L$2.5\pm1.5$,
consistent with previous estimates. We estimate log$(L_{bol}/L_{Sun})$ = $-3.86
\pm 0.04$, which is consistent with prior estimates for $\beta$ Pic b and with
field early-L brown dwarfs. This yields a hot-start mass estimate of $11.9 \pm
0.7$ $M_{Jup}$ for an age of $21\pm4$ Myr, with an upper limit below the
deuterium burning mass. Our $L_{bol}$ based hot-start estimate for temperature
is $T_{eff}=1643\pm32$ K (not including model dependent uncertainty). Due to
the large corresponding model-derived radius of $R=1.43\pm0.02$ $R_{Jup}$, this
$T_{eff}$ is $\sim$$250$ K cooler than would be expected for a field L2.5 brown
dwarf. Other young, low-gravity (large radius), ultracool dwarfs and
directly-imaged EGPs also have lower effective temperatures than are implied by
their spectral types. However, such objects tend to be anomalously red in the
near-IR compared to field brown dwarfs. In contrast, $\beta$ Pic b has near-IR
colors more typical of an early-L dwarf despite its lower inferred temperature.
