Interstellar dust radiates at far infrared wavelengths. There is no trace of the shell in this IRAS image at a wavelength of 0.1 millimeter. The emission that is visible is probably not related to the shell. It is mainly dust in the Perseus spiral arm that is in the foreground. One possible exception is a faint infrared source identified by Digel et al. (1994), that could be associated with the CO cloud discovered by Digel et al. (1994).

This is Figure 5 from the paper by Stil & Irwin (2001). The white contours show the outline of the molecular cloud. The black contours outline radio continuum emission at a wavelength of 21 cm from ionized hydrogen. The ionized hydrogen (HII region) was discovered by De Geus et al. (1993), and has the same velocity as the molecular cloud. The grayscales display the atomic hydrogen with the same velocity as the CO cloud and the HII region. All of the atomic hydrogen is part of he shell GSH 138-01-94. The white crosses indicate the brightest areas of the optical emission of the HII region. The black + indicates the star that is probably responsible for the ionization of the HII region (see De Geus et al. 1993) Back