We modelled the distribution and the kinematics of HI in the inner Milky Way (R < Ro) at latitude b = 0∘ assuming axi-symmetry. We fitted the line profiles of the LAB 21-cm survey using an iterative approach based on the tangent-point method. The resulting model reproduces the H I data remarkably well, with significant differences arising only for R < 2 kpc. This suggests that, despite the presence of a barred potential, the neutral gas in the inner Milky Way is distributed in a fairly axi-symmetric disc.
Marasco, A., Fraternali, F. (2012). How axi-symmetric is the inner HI disc of the Milky Way?. EPJ WEB OF CONFERENCES, 19, 4-6 [10.1051/epjconf/20121908007].
How axi-symmetric is the inner HI disc of the Milky Way?
MARASCO, ANTONINO;FRATERNALI, FILIPPO
2012
Abstract
We modelled the distribution and the kinematics of HI in the inner Milky Way (R < Ro) at latitude b = 0∘ assuming axi-symmetry. We fitted the line profiles of the LAB 21-cm survey using an iterative approach based on the tangent-point method. The resulting model reproduces the H I data remarkably well, with significant differences arising only for R < 2 kpc. This suggests that, despite the presence of a barred potential, the neutral gas in the inner Milky Way is distributed in a fairly axi-symmetric disc.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
