Titlebook: How does the Galaxy work?; A Galactic Tertulia Emilio J. Alfaro,Enrique Pérez,José Franco Conference proceedings 2004 Springer Science+Bus

门窗的侧柱

Hi Clouds Beyond the Galactic Disk, new data show that in the inner parts of the Milky Way the disk-halo interface is composed of many discrete HI clouds. The clouds lie in a layer more than one kpc thick and follow Galactic rotation. Their origin and evolution is unknown. In the outer Galaxy, the new data show that the high-velocity

BRIEF

The Wham Northern Sky Survey and the Nature of the Warm Ionized Medium in the Galaxy,ehensive picture of both the distribution and kinematics of diffuse ionized gas in the Galaxy. WHAM continues to advance our understanding of the physical conditions of the warm ionized medium through observations of other optical emission lines throughout the Galactic disk and halo. We discuss some

软弱

The Structure of Galactic Hydrogen on the Largest Scales,y (IGPS). The IGPS is in the process of imaging the H . throughout the disk of the Milky Way with sensitivity to angular scales between 2 arcminutes and several degrees. Using these data we are revisiting long-standing questions about the large-scale structure of H . in the Galaxy, especially in the

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grounded

Ionization of the Galactic Halo, fundamental problem for the understanding of the halo is the nature of the energy sources that ionize the warm gas and create the hot gas. Most of the energy sources in the Galaxy, e.g. hot stars and supernova remnants, are primarily confined to a relatively thin disk (∼several hundred pc) in contr

municipality

anthesis

Pericarditis

,Brackett-γ Line Survey of the Ionized Hydrogen in the Galactic Plane,ryogenic Fabry-Perot spectrometer. For this survey fields were selected along the Galactic plane from 358° to 43° longitude. The velocity range of the observed emission features ranges from −10 km s. to 90 km s. (LSR). Typical detected intensities correspond to emission measures of about 1000 cm. pc

摇晃

Leaky H II Regions and Heliumionization in the Reynolds Layer,an typical of H ii regions. We construct 3D photoionization models of the diffuse ionized gas and show that the ionizing spectra escaping from leaky H . regions can provide a solution to the He./H. problem. Depending on the spectral type of the ionizing source(s) and the fractional leakage from the

PANIC

Reynolds Layers in Nearby Galaxies: The Face-On View,asic cause of the ionization of the diffuse ionized gas in galaxy discs, and by implication are the chief cause of the Reynolds layer in the Milky Way, and refer the reader to models based on these observations which go further, geometrically, to confirm this conclusion.