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We present a high-resolution ($R \simeq 20,000$) near-infrared (9,100-13,500$\AA$) long-slit spectrum of P Cygni obtained with the newly commissionedWINERED spectrograph in Japan. In the obtained spectrum, we have found that thevelocity profiles of the [Fe II] emission lines are resolved into two peaks ata velocity of $\simeq220$ km s$^{-1}$ with a moderate dip in between and withadditional sub-peaks at $\simeq\pm100$~km~s$^{-1}$. The sub-peak component isconfirmed with the long-slit echellogram to originate in the known shell with aradius of $\simeq10^{\prime\prime}$, which was originally created by theoutburst in 1600 AD. On the other hand, the $\simeq220$ km s$^{-1}$ component,which dominates the [Fe II] flux from P Cygni, is found to be concentratedcloser to the central star with an apparent spatial extent of$\simeq3^{\prime\prime}$. The extent is much larger than the compact($<0^{\prime\prime}.1$) regions traced with hydrogen, helium, and metalpermitted lines. The velocity, estimated mass, and dynamical time of theextended emission-line region suggest that the region is an outer part of thestellar wind region. We suggest that the newly-identified emission-line regionmay trace a reverse shock due to the stellar wind overtaking the outburstshell.

A newly-identified emission-line region around P Cygni