The HI Distribution Observed toward a Halo Region of the Milky Way
Observatorio Astronómico de Quito, Escuela Politécnica Nacional, Av. Gran Colombia S/N, Quito 170403, Ecuador
Author to whom correspondence should be addressed.
Academic Editor: Emilio Elizalde
Received: 18 July 2017 / Revised: 23 August 2017 / Accepted: 24 August 2017 / Published: 28 August 2017
PDF [456 KB, uploaded 28 August 2017]
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
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
at Galactic latitudes higher than ∼46°. This report summarizes our contribution presented at the conference on the origin and evolution of barionic Galaxy halos.
This is an open access article distributed under the Creative Commons Attribution License
which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited (CC BY 4.0).
Printed Edition Available!
A printed edition of this Special Issue is available here
Share & Cite This Article
MDPI and ACS Style
López, E.; Armijos, J.; Llerena, M.; Aldás, F. The HI Distribution Observed toward a Halo Region of the Milky Way. Galaxies 2017, 5, 45.
López E, Armijos J, Llerena M, Aldás F. The HI Distribution Observed toward a Halo Region of the Milky Way. Galaxies. 2017; 5(3):45.
López, Ericson; Armijos, Jairo; Llerena, Mario; Aldás, Franklin. 2017. "The HI Distribution Observed toward a Halo Region of the Milky Way." Galaxies 5, no. 3: 45.
Show more citation formats
Show less citations formats
Note that from the first issue of 2016, MDPI journals use article numbers instead of page numbers. See further details here.
[Return to top]
For more information on the journal statistics, click here
Multiple requests from the same IP address are counted as one view.