We analyze the hitherto available space-based X-ray data as well as ground-based optical data of the X-ray transient 080109/SN 2008D .
From the data we suggest that ( i ) The initial transient ( \lesssim 800 sec ) is attributed to the reverse shock emission of a mildly relativistic ( \Gamma \sim a few ) outflow stalled by the dense stellar wind .
( ii ) The subsequent X-ray afterglow ( \lesssim 2 \times 10 ^ { 4 } sec ) can be ascribed to the forward shock emission of the outflow , with a kinetic energy \sim 10 ^ { 46 } erg , when sweeping up the stellar wind medium .
( iii ) The late X-ray flattening ( \gtrsim 2 \times 10 ^ { 4 } sec ) is powered by the fastest non-decelerated component of SN 2008D ’ s ejecta .
( iv ) The local event rate of X-ray transient has a lower limit of \sim 1.6 \times 10 ^ { 4 } ~ { } { yr ^ { -1 } ~ { } Gpc ^ { -3 } } , indicating a vast majority of X-ray transients have a wide opening angle of \gtrsim 100 ^ { \circ } .
( v ) Transient 080109/SN 2008D indicates a continuum from GRB-SN to under-luminous GRB-/XRF-SN to X-ray transient-SN and to ordinary Ibc SN ( if not every Ibc SN has a relativistic jet ) , as shown in Figure 2 of this Letter .