Detalles de publicación
PP 014159
BUBBLY: A method for detecting and characterizing interstellar bubbles using Fabry-Perot spectroscopy
1Instituto de Astrofsica de Canarias, C/Va Lactea s/n, E-38205 La Laguna, Tenerife, Spain
2Department of Astrophysics, University of La Laguna, E-38205 La Laguna, Tenerife, Spain
3CSIC, 2806 Madrid, Spain
4National Observatory of Athens
5Laboratoire d'Astrophysique de Marseille, Aix Marseille Universite, CNRS, F-13388, Marseille, France
We present a new method for the detection and characterization of expansion in galaxy
discs based on H alpha Fabry-Perot spectroscopy, taking advantage of the high spatial and
velocity resolution of our instrument (GH FaS). The method analyses multi-peaked
emission line pro les to nd expansion along the line of sight on a point-by-point
basis. At this stage we have centred our attention on the large scale structures of
expanding gas associated with HII regions which show a characteristic pattern of
expansion velocities, of order 100 km/s, as a result of both bubble shape and projection
e ects. We show an example of the expansion map obtained with our method from
a superbubble detected in the Antennae galaxies. We use the information obtained
from the method to measure the relevant physical parameters of the superbubbles,
including their ages which can be used to date young star clusters.
discs based on H alpha Fabry-Perot spectroscopy, taking advantage of the high spatial and
velocity resolution of our instrument (GH FaS). The method analyses multi-peaked
emission line pro les to nd expansion along the line of sight on a point-by-point
basis. At this stage we have centred our attention on the large scale structures of
expanding gas associated with HII regions which show a characteristic pattern of
expansion velocities, of order 100 km/s, as a result of both bubble shape and projection
e ects. We show an example of the expansion map obtained with our method from
a superbubble detected in the Antennae galaxies. We use the information obtained
from the method to measure the relevant physical parameters of the superbubbles,
including their ages which can be used to date young star clusters.