| Issue |
A&A
Volume 477, Number 2, January II 2008
|
|
|---|---|---|
| Page(s) | L21 - L24 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361:20078967 | |
| Published online | 20 November 2007 | |
Letter to the Editor
The large scale dust lanes of the Galactic bar
1
CNRS-UMR 6213, Institut Utinam, Observatoire de Besançon, BP 1615, 25010 Besançon Cedex, France
2
Département de Physique et Centre Observatoire du Mont Mégantic, Université Laval, Québec, QC, G1K 7P4, Canada e-mail: douglas.marshall.1@ulaval.ca
3
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
Received:
31
October
2007
Accepted:
14
November
2007
Context.Trails of dust inside galactic bars are easily observable in external galaxies. However, information on the dust lanes of the Milky Way bar is harder to obtain due to our position within the Galactic disc.
Aims.By comparing the distribution of dust and gas in the central regions of the Galaxy, we aim to obtain new insights into the properties of the offset dust lanes leading the bar's major axis in the Milky Way.
Methods.On the one hand, the molecular emission of the dust lanes is extracted from the observed
CO 
distribution according to the interpretation of a dynamical model.
On the other hand, a three
dimensional extinction map of the Galactic central region constructed from near-infrared
observations is used as a tracer of the dust itself and clearly reveals
dust lanes in its face-on projection. Comparison of the position of both independent
detections of the dust lanes is performed in the 
plane.
Results.These two completely independent methods are used to provide a coherent picture of the dust lanes in the Milky Way bar. In both the gas and dust distributions, the dust lanes are found to be out of the Galactic plane, appearing at negative latitudes for l > 0° and at positive latitudes for l < 0°. However, even though there is substantial overlap between the two components, they are offset from one another with the dust appearing to lie closer to the b = 0° plane.
Conclusions. Two scenarios are proposed to explain the observed offset. The first involves grain destruction by the bar shock and reformation downstream. Due to the decrease in velocity caused by the shock, this occurs at lower z. The second assumes that the gas and dust remain on a common tilted plane, but that the molecular gas decouples from the Milky Way's magnetic field, itself strong enough to resist the shear of the bar's shock. The diffuse gas and dust remain coupled to the field and are carried further downstream. This second scenario has recently been suggested in order to explain observations of the barred galaxy NGC 1097.
Key words: Galaxy: structure / Galaxy: center / ISM: kinematics and dynamics / ISM: dust, extinction / Galaxy: kinematics and dynamics / infrared: ISM
© ESO, 2007
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