The Low-Resolution DRAO Survey of HI Emission from the Galactic Plane. II.

In 2000, a survey of H I line emission in the Galactic plane between Galactic longitudes l = 72.degrees 2 and 149.degrees 0, covering latitudes from b = - 5.degrees 4 to 7.degrees 2, made using the 26 m telescope at the Dominion Radio Astrophysical Observatory, was published as part of the Canadian Galactic Plane Survey project. The survey with the 26 m telescope has now been extended to cover longitudes from l = 50.degrees 0 to 195.degrees 0, between the same latitude limits. In addition, a region at higher Galactic latitudes ( b = 7.degrees 4 - 24.degrees 0) has been surveyed between longitudes l = 96.degrees 4 and 120.degrees 2. As in the initial survey, spectra were observed at 0.degrees 2 intervals of longitude and latitude (0.33 half-power beamwidths). ( In an appendix, it is demonstrated that, when single-antenna data and interferometer data are to be combined, the single-antenna data must be sampled at an interval no greater than 0.5 times the half-power beamwidth of the single antenna. Coarser sampling will result in the introduction of spurious structure into the resulting images.) The spectral resolution is 1.32 km s(-1), and the LSR velocity range is - 260 - 161 km s(-1). The spectra have been corrected for stray radiation and have an estimated T-b scaling accuracy of 1% and an estimated rms noise in one channel (0.8245 km s(-1)) of 0.25 K. Regions of suspected strong H I self-absorption have been identified using a statistic characterizing the "complexity'' of the observed spectra. Comparison with spectra from the Leiden/ Dwingeloo Survey supports the conclusion from our earlier paper that a small percentage ( similar to 1% - 2%) of the spectra in the latter survey suffer from calibration errors exceeding 10%. A table of positions of the more discordant spectra is given.