The HI supershell GS 118+01-44 and its role in the interstellar medium
  We carry out a multiwavelength study to characterize the HI supershell
designated GS 118+01-44, and to analyse its possible origin. A multiwavlength
study has been carried out to study the supershell and its environs. We
performed an analysis of the HI, CO, radio continuum, and infrared emission
distributions. The Canadian Galactic Plane Survey (CGPS) HI data reveals that
GS 118+01-44 is centred at (l, b) = (117.7, 1.4) with a systemic velocity of
-44.3 km/s. According to Galactic rotation models this structure is located at
3.0 +- 0.6 kpc from the Sun. There are several HII regions and three supernova
remnants (SNRs) catalogued in the region. On the other hand, the analysis of
the temperature spectral index distribution shows that in the region there is a
predominance of non-thermal emission. Infrared emission shows that cool
temperatures dominate the area of the supershell. Concerning the origin of the
structure, we found that even though several OB stars belonging to Cas OB5 are
located in the interior of GS 118+01-44, an analysis of the energy injected by
these stars through their stellar winds indicates that they do not have
sufficient energy to create GS 118+01-44. Therefore, an additional energy
source is needed to explain the genesis of GS 118+01-44. On the other hand, the
presence of several HII regions and young stellar object candidates in the
edges of GS 118+01-44 shows that the region is still active in forming new
stars.
