Volume 565, May 2014
|Number of page(s)||19|
|Section||Interstellar and circumstellar matter|
|Published online||29 April 2014|
Molecules, dust, and protostars in NGC 3503⋆
Instituto Argentino de Radioastronomia,
CONICET, CCT-La Plata, C.C.5.,
2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque s/n, 1900 La Plata, Argentina
3 Departamento de Astronomía, Universidad de Chile, Casilla 36-D Santiago, Chile
4 Departamento de Física, Universidad de La Serena, Cisternas 1200 Norte, Casilla 601 La Serena, Chile
Accepted: 19 February 2014
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 To study the distribution of the dust, we make use of unpublished images at 870 μm from the ATLASGAL survey and IRAC-GLIMPSE archival images.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.
Key words: stars: formation / HII regions / ISM: molecules / ISM: individual objects: NGC 3503
Tables 5 and 6 are available in electronic form at http://www.aanda.org
© ESO, 2014
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