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A large portion of the Galaxy (ℓ = 123 • to 164 • , b = −6 • to −35 •), which samples regions of the Local (Orion) spiral arm and the more distant Perseus arm, has been mapped with the Wisconsin H-Alpha Mapper (WHAM) in the [S II] λ6716 and [N II] λ6583 lines. By comparing these data with the maps from the WHAM Hα Sky Survey, we begin an investigation of(More)
The first observations of the recently completed Wisconsin H-Alpha Mapper (WHAM) facility include a study of emission lines from high velocity clouds in the M, A, and C complexes, with most of the observations on the M I cloud. We present results including clear detections of Hα emission from all three complexes with intensities ranging from 0.06 to 0.20 R.(More)
The Wisconsin H-Alpha Mapper (WHAM) has completed a survey in Balmer α of the entire Northern sky above declination −30 •. This survey provides the first calibrated, velocity-resolved map of the Hα emission from the Galaxy. With one-degree spatial resolution, 12 km s −1 velocity resolution, and sensitivity to features as faint as 0.1 R (EM ∼ 0.2 cm −6 pc),(More)
The extremely faint, temperature sensitive " auroral " emission line [N II] λ5755 has been detected from the low density ionized gas along the sight line toward l = 130. o 0, b = −7. o 5 using the Wisconsin Hα Mapper (WHAM). The intensity of this emission line, relative to the red nebular line [N II] λ6584, is found to be twice that observed in bright,(More)
The Wisconsin Hα Mapper (WHAM) Northern Sky Survey has revealed a loop of H II reaching 1300 pc from the Galactic midplane above the Cas OB6 association in the Perseus sprial arm. This enormous feature surrounds and extends far above the " W4 Chimney " identified by Normandeau et al. and appears to be associated with the star formation activity near the(More)
We have identified 85 regions of enhanced Hα emission at |b| > 10 • subtending approximately 1 • or less on the Wisconsin Hα Mapper (WHAM) sky survey. These high latitude " WHAM point sources " have Hα fluxes of 10 −11 to 10 −9 erg cm −2 s −1 , radial velocities within about 70 km s −1 of the LSR, and line widths that range from less than 20 km s −1 to(More)
It has been suggested that high velocity clouds may be distributed throughout the Local Group and are therefore not in general associated with the Milky Way galaxy. With the aim of testing this hypothesis, we have made observations in the Hα line of high velocity clouds selected as the most likely candidates for being at larger than average distances. We(More)