The molecular environment of the Galactic star forming region G19.61–0.23
Author
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Santangelo, G.
Author
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Testi, L.
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Author
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Leurini, S.
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Author
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Walmsley, C. M.
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Author
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Cesaroni, R.
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Author
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Bronfman Aguiló, Leonardo
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Author
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Carey, S.
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Author
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Gregorini, L.
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Author
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Menten, K. M.
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Author
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Molinari, S.
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Noriega Crespo, A.
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Author
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Olmi, L.
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Author
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Schuller, F.
Admission date
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2014-01-07T15:54:02Z
Available date
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2014-01-07T15:54:02Z
Publication date
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2010-06-03
Cita de ítem
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A&A 520, A50 (2010)
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Identifier
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DOI: 10.1051/0004-6361/201014177
Identifier
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https://repositorio.uchile.cl/handle/2250/126004
General note
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Artículo de publicación ISI.
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Abstract
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Context. Although current facilities allow the study of Galactic star formation at high angular resolution, our current understanding
of the high-mass star-formation process is still very poor. In particular, we still need to characterize the properties of clouds giving
birth to high-mass stars in our own Galaxy and use them as templates for our understanding of extragalactic star formation.
Aims. We present single-dish (sub)millimeter observations of gas and dust in the Galactic high-mass star-forming region G19.61–0.23,
with the aim of studying the large-scale properties and physical conditions of the molecular gas across the region. The final aim is to
compare the large-scale (about 100 pc) properties with the small-scale (about 3 pc) properties and to consider possible implications
for extragalactic studies.
Methods. We have mapped CO isotopologues in the J = 1−0 transition using the FCRAO-14m telescope and the J = 2−1 transition
using the IRAM-30m telescope. We have also used APEX 870 μm continuum data from the ATLASGAL survey and FCRAO supplementary
observations of the 13CO J = 1−0 line from the BU-FCRAO Galactic Ring Survey, as well as the Spitzer infrared Galactic
plane surveys GLIMPSE and MIPSGAL to characterize the star-formation activity within the molecular clouds.
Results. We reveal a population of molecular clumps in the 13CO(1–0) emission, for which we derived the physical parameters, including
sizes and masses. Our analysis of the 13CO suggests that the virial parameter (ratio of kinetic to gravitational energy) varies
over an order of magnitude between clumps that are unbound and some that are apparently “unstable”. This conclusion is independent
of whether they show evidence of ongoing star formation. We find that the majority of ATLASGAL sources have MIPSGAL counterparts
with luminosities in the range 104–5 × 104 L and are presumably forming relatively massive stars. We compare our results
with previous extragalactic studies of the nearby spiral galaxies M31 and M33; and the blue compact dwarf galaxy Henize 2–10. We
find that the main giant molecular cloud surrounding G19.61–0.23 has physical properties typical for Galactic GMCs and which are
comparable to the GMCs in M31 and M33. However, the GMC studied here shows smaller surface densities and masses than the
clouds identified in Henize 2–10 and associated with super star cluster formation.