HI in the galactic halo

Details HI in the galactic halo HI in the galactic halo

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...332l..61k&link_type=abstract

Astronomy and Astrophysics, v.332, p.L61-L64 (1998)

Astronomy and Astrophysics

Astrophysics

42

Galaxy: Halo, Galaxy: Kinematics And Dynamics, Radio Lines: Ism

Scientific paper

We find solid evidence for diffuse Hi gas at substantial z heights in our Galaxy, with a velocity dispersion of sigma = 60 kms(-1) and a vertical projected column density of N_sc Hi = 1.4 *10(19) cm(-2) . This pervasive component of the emission spectrum could be identified in the Leiden/Dwingeloo 21-cm Survey (LDS) after increasing the accuracy further by correcting the observations for reflections from the ground. Investigations of receiver bandpass and stray radiation effects could not explain this component as an artifact of the instrumentation. Assuming that the distribution of mass and pressure perpendicular to the galactic plane is in hydrostatic equilibrium with the galactic potential, we derive a vertical exponential scale height of h_z =~ 4.4 kpc for the observed diffuse high-dispersion Hi component. The radial distribution is characterized by the corresponding galactocentric scale length A_1 =~ 15 kpc.

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