MacConnell and Frye published findings on six new stars showing strong neutral helium lines whose spectra appeared different from other "hydrogen deficient" stars, on objective prism plates from Cerro Tololo, Chile. By the end of the school year, Bidelman resigned to accept the position of Director of the Warner and Swasey Observatory and Chairman of Astronomy at Case Western Reserve University (CWRU) in Ohio. Case Western Reserve University (1970–2011) Bidelman directed the Warner and Swasey Observatory from 1970 to 1975, and was a Professor of astronomy from 1970 to 1986. In June 1970, Bidelman began as Chairman and Director. Bidelman's office was at the old Taylor Road Observatory, given to the University by the Warner & Swasey Company in 1920. Due to light pollution from the city of Cleveland, by the 1950s viewing was difficult and the Burrell Schmidt telescope was relocated ~30 miles away to Geauga County. In 1973, Bidelman and MacConnell provided data on a variety of B-emission (Be) and shell stars, peculiar stars, weak-metal stars and other bright stars of the southern hemisphere, covering ~81% of the southern sky. They said when completed, Houk's more comprehensive study would "provide spectral date of inestimable value to stellar astronomers" and should supersede their report, but they did it as an "early result" study. Using CTIO objective –prism plates they found nearly 800 previously unknown A-type peculiar stars. They also found 34 weak G-band giants stars in the southern hemisphere. Their study was called a "major contribution" in providing data to help identify the relatively rare Population II stars. It created an unbiased sample, and doubled the number of known peculiar A-type (Ap) stars. After nineteen years of study by various investigators, in 2014, Beers et al. studied 302 of the Bidelman-MacConnell possible weak-metal stars and concluded that a metal-weak thick disk (MWTD) is present in the Milky Way galaxy, and noted its importance in understanding the development of our galaxy. In 1962 and 1966, Bidelman had reported that the wavelength of λ 3984 varied somewhat from star to star, and stated differences in the ratios of mercury isotopes could be the reason. Bidelman was the first to note this, and in 1974, Michaud, Reeves and Charland, considering the isotopic abundances to be real, and that Hg was in fact overabundant and not an artifact of blending, suggested the mercury overabundances were due to radiation pressure that caused the element