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Interaction between OB stars and the interstellar medium

Published online by Cambridge University Press:  26 May 2016

Monica Relaño Pastor ,
John E. Beckman  and
Maite Rozas
Monica Relaño Pastor
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38200 La Laguna, Tenerife, España
John E. Beckman
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38200 La Laguna, Tenerife, España Consejo Superior de Investigaciones Científicas (CSIC), España
Maite Rozas
Affiliation:
Observatorio Astronómico Nacional de San Pedro Mártir, UNAM, 22860 Ensenada, BC, México

Abstract

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From the emission line map in Hα over the full face of the spiral galaxy NGC 3359, we analyze the internal velocity structure of the H ii region population. The emission line profiles show central peaks, with turbulent velocity widths of ≤20 km s–1, and also broad shallow wings, with typical velocities of ~50 km s–1, with respect to the rest velocity of the H ii region. We verify the identification of these wings as due to expanding gas, quantify the energy involved, and suggest physical models for their interpretation, as the effects of mechanical and radiative outflows from the central OB stellar cluster.

Type
Part 4. Feedback from Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 738 - 739
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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