We present new optical , near-IR , and mid-IR observations of the young eruptive variable star V1647 Orionis that went into outburst in late 2004 for approximately two years .
Our observations were taken one year after the star had faded to its pre-outburst optical brightness and show that V1647 Ori is still actively accreting circumstellar material .
We compare and contrast these data with existing observations of the source from both pre-outburst and outburst phases .
From near-IR spectroscopy we identify photospheric absorption features for the first time that allow us to constrain the classification of the young star itself .
Our best fit spectral type is M0 \pm 2 sub-classes with a visual extinction of 19 \pm 2 magnitudes and a K-band veiling of r _ { K } \sim 1.5 \pm 0.2 .
We estimate that V1647 Ori has a quiescent bolometric luminosity of \sim 9.5 L _ { \odot } and a mass accretion rate of \sim 1 \times 10 ^ { -6 } M _ { \odot } yr ^ { -1 } .
Our derived mass and age , from comparison with evolutionary models , are 0.8 \pm 0.2 M _ { \odot } and \lesssim 0.5 Myrs , respectively .
The presence towards the star of shock excited optical [ S II ] and [ Fe II ] emission as well as near-IR H _ { 2 } and [ Fe II ] emission perhaps suggests that a new Herbig-Haro flow is becoming visible close to the star .