NGC6888 and the star WR 136 are presented. We performed H
observations with a Fabry–Perot interferom-eter mounted at the focus of the 125-cm telescope and radio continuum (2.7 to 31 cm) and 21-cm H I observa-
tions with the RATAN-600 radio telescope. A thick expanding shell of neutral hydrogen 120 pc in diameter that
immediately surrounds the extended infrared shell was detected. This suggests that the infrared shell is a single
structure rather than a chance projection of physically unrelated objects. The radial velocity of the H I shell is
11
1 km s–1, the expansion velocity is 10 3 km s–1, and the mass of the neutral hydrogen in the shell is 104M
. The bright radio features that we detected in the region of the infrared shell all exhibit a flat spectrum typical of thermal emission from optically thin H II regions. The same inference is probably also true for the
nebula Simeiz 55. Our observations are consistent with the assumption of A.P. Marston that the extended shell
was formed by the stellar wind from the precursor of WR 136, but they do not rule out the identification with a
very old supernova remnant proposed by J. Nichols-Bohlin and R.A. Fesen, either. A revision of the distance
to the pulsar PSR J2013+3845 with inhomogeneity of the interstellar medium taken into account allows for its
formation during the same supernova explosion some 4
105 years ago.