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Kinematical Structure of the Local Interstellar Medium

Published online by Cambridge University Press:  12 April 2016

R. Génova ,
J. E. Beckman  and
J. Rodríguez Álamo
R. Génova
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain
J. E. Beckman
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain
J. Rodríguez Álamo
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain

Abstract

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Observations of interstellar Na I in the spectra of 93 stars within 315 pc from the Sun show that it lies in a tunnel of gas moving away from Scorpio-Centaurus and is surrounded by gas moving toward the Galactic center.

Gas approaches the Sun from Scorpio-Centaurus expanding from (r, l, b)=(160 pc, 313°7, +28°2) with LSR velocity 15.3 km s−1. The radius of this shell is 153 pc.

We identify these clouds:

D: velocity vector (υ d, l d, b d)=(+7.2 km s−1, 305°1, −13°5), above and below the Galactic plane (GP) in the range of Galactic longitudes 357°–55°.

C: velocity vector (υ c, l c, b c)=(+11.5 km s−1, 349°0, −35°2), above and below the GP in the range 30°≤l≤110°.

M: velocity vector (υ m, l m, b m)=(+21.9 km s−1, 34°2, +1°5), above and below the GP in the range 100°≤l≤130°.

P: velocity vector (υ p, l p, b p)=(+13.8 km s−1, 244°9, +5°4), above and below the GP from l~120° to the limit of our data at l~210°.

E: velocity vector (υ e, l e, b e)=(+16.8 km s−1, 208°4, +6°2) in the range 160°≤l≤185° and −10°≤b≤–35°.

A: velocity vector (υ a, l a, b a)=(+12.9 km s−1, 73°6, −5°6) towards the Galactic anti-center, below the GP.

I: velocity vector (υ i, l i, b i)=(+37.7 km s−1, 132°8, −64°3) towards the Galactic anti-center, above the GP.

Type
Part IV Clouds, Ionized Gas, and Particles in the Local ISM
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 195 - 198
Copyright
Copyright © Springer-Verlag 1998

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