WHAM Observations of H-alpha Emission from High Velocity Clouds in the M, A, and C Complexes

Details WHAM Observations of H-alpha Emission from High Velocity Clouds in the M, A, and C Complexes WHAM Observations of H-alpha Emission from High Velocity Clouds in the M, A, and C Complexes

1998-07-15

arxiv.org/abs/astro-ph/9807157v1

Astronomy and Astrophysics

Astrophysics

32 pages, 18 figures, to appear in ApJ (Sept. 10, 1998)

Scientific paper

10.1086/306103

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 H-alpha emission from all three complexes with intensities ranging from 0.06 R to 0.20 R. In every observed direction where there is significant high velocity H I gas seen in the 21 cm line we have found associated ionized hydrogen emitting the H-alpha line. The velocities of the H-alpha and 21 cm emission are well correlated in every case except one, but the intensities are not correlated. There is some evidence that the ionized gas producing the H-alpha emission envelopes the 21 cm emitting neutral gas but the H-alpha "halo", if present, is not large. If the H-alpha emission arises from the photoionization of the H I clouds, then the implied Lyman continuum flux F_{LC} at the location of the clouds ranges from 1.3 to 4.2 x 10^5 photons cm^{-2} s^{-1}. If, on the other hand, the ionization is due to a shock arising from the collision of the high-velocity gas with an ambient medium in the halo, then the density of the pre-shocked gas can be constrained. We have also detected the [S II] 6716 angstrom line from the M I cloud and have evidence that the [S II] to H-alpha ratio varies with location on the cloud.

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