  We present the results of near-infrared imaging and spectroscopic
observations of the young, core-collapse supernova remnant (SNR) G11.2-0.3. In
the [Fe II] 1.644 um image, we first discover long, clumpy [Fe II] filaments
within the radio shell of the SNR, together with some faint, knotty features in
the interior of the remnant. We have detected several [Fe II] lines and HI Br-G
line toward the peak position of the bright southeastern [Fe II] filament. The
derived extinction is large (Av=13 mag) and it is the brightest [Fe II]
filament detected toward SNRs to date. By analyzing two [Fe II] 1.644 um images
obtained in 2.2 yrs apart, we detect a proper motion corresponding to an
expansion rate of 0.''035 (0.''013) /yr [or 830 (310) km/s]. We also discover
two small H2 filaments. One is bright and along the SE boundary of the radio
shell, while the other is faint and just outside of its NE boundary. We have
detected H2 (2-1) S(3) line toward the former filament and derive an excitation
temperature of 2,100 K. We suggest that the H2 filaments are dense clumps in a
presupernova circumstellar wind swept up by the SNR shock while the [Fe II]
filaments are probably composed of both shocked wind material and shocked
supernova (SN) ejecta. The distribution of [Fe II] filaments may indicate that
the SN explosion in G11.2-0.3 was asymmetric as in Cassiopeia A. Our results
support the suggestion that G11.2-0.3 is a remnant of a SN IIL/b interacting
with a dense red supergiant wind.
