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Molecules, dust, and protostars in NGC 3503

Universidad de Chile. Repositorio Académico

 
Título Molecules, dust, and protostars in NGC 3503
 
Autor Cappa, C. E.
Vásquez, J.
Duronea, N. U.
Romero, G. A.
Barbá, R.
Bronfman Aguiló, Leonardo Jaime
 
Tema stars: formation
 
Descripción Artículo de publicación ISI.
Aims. We present here a follow-up study of the molecular gas and dust in the environs of the star forming region NGC 3503. This study aims at dealing with the interaction of the Hii  region NGC 3503 with its parental molecular cloud, and also with the star formation in the region, that was possibly triggered by the expansion of the ionization front against the parental cloud.
Methods. To analyze the molecular gas we use CO(J = 2 → 1), 13CO(J = 2 → 1), C18O(J = 2 → 1), and HCN(J = 3 → 2) line data obtained with the on-the-fly technique from the APEX telescope. To study the distribution of the dust, we make use of unpublished images at 870 μm from the ATLASGAL survey and IRAC-GLIMPSE archival images. We use public 2MASS and WISE data to search for infrared candidate young stellar objects (YSOs) in the region.
Results. The new APEX observations allowed the substructure of the molecular gas in the velocity range from ~−28 km s-1 to −23 km s-1 to be imaged in detail. The morphology of the molecular gas close to the nebula, the location of the PDR, and the shape of radio continuum emission suggest that the ionized gas is expanding against its parental cloud, and confirm the champagne flow scenario. We have identified several molecular clumps and determined some of their physical and dynamical properties such as density, excitation temperature, mass, and line width. Clumps adjacent to the ionization front are expected to be affected by the Hii  region, unlike those that are distant from it. We have compared the physical properties of the two kinds of clumps to investigate how the molecular gas has been affected by the Hii  region. Clumps adjacent to the ionization fronts of NGC 3503 and/or the bright rimmed cloud SFO 62  have been heated and compressed by the ionized gas, but their line width is not different from those that are too distant from the ionization fronts. We identified several candidate YSOs in the region. Their spatial distribution suggests that stellar formation might have been boosted by the expansion of the nebula. We discard the collect-and-collapse scenario and propose alternative mechanisms such as radiatively driven implosion on pre-existing molecular clumps or small-scale Jeans gravitational instabilities.
 
Fecha 2014-10-14T19:36:12Z
2015-03-13T13:02:05Z
2014-10-14T19:36:12Z
2015-03-13T13:02:05Z
2014-05
 
Tipo Artículo de revista
 
Enlace A&A 565, A30 (2014)
DOI: 10.1051/0004-6361/201322850
http://repositorio.uchile.cl/handle/2250/126490
 
Idioma en_US
 
Derechos Attribution-NonCommercial-NoDerivs 3.0 Chile
http://creativecommons.org/licenses/by-nc-nd/3.0/cl/
 
Publicador EDP Sciences