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We present optical ($B$, $V$, $R_{\rm c}$, $I_{\rm c}$ and $y$) and nearinfrared ($J$, $H$ and $K_{\rm s}$) photometric and spectroscopic observationsof a classical nova V1280 Scorpii for five years from 2007 to 2011. Ourphotometric observations show a declining event in optical bands shortly afterthe maximum light which continues $\sim$ 250 days. The event is most probablycaused by a dust formation. The event is accompanied by a short ($\sim$ 30days) re-brightening episode ($\sim$ 2.5 mag in $V$), which suggests are-ignition of the surface nuclear burning. After 2008, the $y$ bandobservations show a very long plateau at around $y$ = 10.5 for more than 1000days until April 2011 ($\sim$ 1500 days after the maximum light). The nova hadtaken a very long time ($\sim$ 50 months) before entering the nebular phase(clear detection of both [\ion{O}{iii}] 4959 and 5007) and is still continuingto generate the wind caused by H-burning. The finding suggests that V1280 Scois going through the historically slowest evolution. The interval from themaximum light (2007 February 16) to the beginning of the nebular phase islonger than any previously known slow novae: V723 Cas (18 months), RR Pic (10months), or HR Del (8 months). It suggests that the mass of a white dwarf inthe V1280 Sco system might be 0.6 $M_\mathrm{\sun}$ or smaller. The distance,based on our measurements of the expansion velocity combined with the directlymeasured size of the dust shell, is estimated to be 1.1 $\pm$ 0.5 kpc.

Five-Year Optical and Near Infrared Observations of the Extremely Slow Nova V1280 Scorpii