Abstract
We use observations of the neutral atomic hydrogen (HI) 21-cm emission line to study the spatial distribution of the HI gas in a 80° × 90° region of the Galaxy halo. The HI column densities in the range of 3–11 × 10 20 cm − 2 have been estimated for some of the studied regions. In our map—obtained with a spectral sensitivity of ∼2 K—we do not detect any HI 21-cm emission line above 2 σ at Galactic latitudes higher than ∼46°. This report summarizes our contribution presented at the conference on the origin and evolution of barionic Galaxy halos.
Highlights
Neutral atomic hydrogen (HI) is the most abundant element in the interstellar medium, and its 21-cm emission line is a powerful tool to trace the structure and dynamics of the Milky WayGalaxy (Kalverla and Jürgen [1])
There is a galaxy halo composed of HI gas with densities of 10−3 cm−3 that extends in vertical height up to a distance of ∼4 kpc, and radially HI gas is detected in the outskirts (&35 kpc) of the Milky Way (Kalverla and Jürgen [1])
Using data obtained from the small SALSA telescope, we were able to obtain a peak-intensity map of the HI 21-cm emission line for a 80◦ × 90◦ region of the Milky Way
Summary
Neutral atomic hydrogen (HI) is the most abundant element in the interstellar medium, and its 21-cm emission line is a powerful tool to trace the structure and dynamics of the Milky WayGalaxy (Kalverla and Jürgen [1]). There is a galaxy halo composed of HI gas with densities of 10−3 cm−3 that extends in vertical height up to a distance of ∼4 kpc, and radially HI gas is detected in the outskirts (&35 kpc) of the Milky Way (Kalverla and Jürgen [1]). All these important features have been discovered mainly thanks to studies carried out using the HI
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