Characterization of dense Planck clumps observed with Herschel and SCUBA-2

Emma Elisa Mannfors, Mika Juvela

Tutkimustuotos: ArtikkelijulkaisuArtikkeliTieteellinenvertaisarvioitu


Context. Though the basic processes of star-formation (SF) are well-known, more research is needed on SF across multiple scales and environments. To form a complete picture of SF regions, data from both continuum and molecular line observations is necessary.
Aims. We aim to characterize a diverse selection of dense, potentially star forming cores, clumps, and clouds within the Milky Way in terms of their dust emission and SF activity. These clouds are selected based on their high column densities as estimated from previous Herschel and JCMT SCUBA-2 observations.
Methods. We estimate dust properties by fitting Herschel observations with modified blackbody functions, study the relationship between dust temperature and dust opacity spectral index β, and estimate column densities. We use FellWalker to find dense clumps in SCUBA-2 850 μm emission and examine the masses and sizes of the clumps. YSOs from four catalogs are associated with the clumps. We estimate the gravitational stability of the clumps with virial analysis. The clumps are categorized as starless, prestellar, or protostellar.
Results. We find 529 dense clumps, which are regions of high column density (N(H2) 10 22  cm −2 ) and low temperature (T ∼ 14–18 K). Temperature and opacity spectral index β appear to be anticorrelated (β ∝ T −0.5 ). Masses of the sources range from 0.04 M0 to 1371 M0 . Mass, linear size, and temperature are correlated with distance. Furthermore, estimated gravitational stability is dependent on distance, with more distant clumps appearing more virially bound. Finally, we present a catalog of properties of the clumps.
Conclusions. Our sources present a large array of SF regions, from high-latitude nearby diffuse clouds to large SF complexes nearthe Galactic center. Analysis of these regions will continue with the addition of molecular line data, which will allow us to study thedensest regions of the clumps in more detail.
LehtiAstronomy & Astrophysics
TilaJätetty - 21 helmikuuta 2020
OKM-julkaisutyyppiA1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä, vertaisarvioitu


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