Physical and chemical structure of high-mass star-forming regions Unraveling chemical complexity with CORE: the NOEMA large program
Por:
Gieser, C., Beuther, H., Semenov, D., Ahmadi, A., Suri, S., Möller T., Beltran, M. T., Klaassen, P., Zhang, Q., Urquhart, J. S., Henning, Th., Feng, S., Galvan-Madrid, R., De Souza Magalhães V., Moscadelli, L., Longmore, S., Leurini, S., Kuiper, R., Peters, T., Menten, K. M., Csengeri, T., Fuller, G., Wyrowski, F., Lumsden, S., Sanchez-Monge, A., Maud, L., Linz, H., Palau, A., Schilke, P., Pety, J., Pudritz, R., Winters, J. M., Pietu, V.
Publicada:
15 abr 2021
Resumen:
Aims. Current star formation research centers the characterization of
the physical and chemical properties of massive stars, which are in the
process of formation, at the spatial resolution of individual high-mass
cores.
Methods. We use sub-arcsecond resolution (similar to 0 `'.4)
observations with the NOrthern Extended Millimeter Array at 1.37 mm to
study the dust emission and molecular gas of 18 high-mass star-forming
regions. With distances in the range of 0.7-5.5 kpc, this corresponds to
spatial scales down to 300-2300 au that are resolved by our
observations. We combined the derived physical and chemical properties
of individual cores in these regions to estimate their ages. The
temperature structures of these regions are determined by fitting the
H2CO and CH3CN line emission. The density profiles are inferred from the
1.37 mm continuum visibilities. The column densities of 11 different
species are determined by fitting the emission lines with XCLASS.
Results. Within the 18 observed regions, we identified 22 individual
cores with associated 1.37 mm continuum emission and with a radially
decreasing temperature profile. We find an average temperature power-law
index of q = 0.4 +/- 0.1 and an average density power-law index of p =
2.0 +/- 0.2 on scales that are on the order of several 1000 au.
Comparing these results with values of p derived from the literature
presumes that the density profiles remain unchanged from clump to core
scales. The column densities relative to N((CO)-O-18) between pairs of
dense gas tracers show tight correlations. We applied the
physical-chemical model MUlti Stage ChemicaL codE to the derived column
densities of each core and find a mean chemical age of similar to 60 000
yr and an age spread of 20 000-100 000 yr. With this paper, we release
all data products of the CORE project.
Conclusions. The CORE sample reveals well-constrained density and
temperature power-law distributions. Furthermore, we characterized a
large variety in molecular richness that can be explained by an age
spread that is then confirmed by our physical-chemical modeling. The hot
molecular cores show the greatest number of emission lines, but we also
find evolved cores at an evolutionary stage in which most molecules are
destroyed and, thus, the spectra appear line-poor once again.
Filiaciones:
Gieser, C.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Beuther, H.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Semenov, D.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Department of Chemistry, Ludwig Maximilian University, Butenandtstr. 5-13, Munich, 81377, Germany
Ahmadi, A.:
Leiden University, Niels Bohrweg 2, Leiden, 2333 CA, Netherlands
Suri, S.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Möller T.:
I. Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, Koln, 50937, Germany
Beltran, M. T.:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze, 50125, Italy
Klaassen, P.:
Uk Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom
Zhang, Q.:
Center for Astrophysics, Harvard and Smithsonian, 60 Garden Street, Cambridge, MA 02138, United States
Urquhart, J. S.:
Centre for Astrophysics and Planetary Science, University of Kent, Canterbury, CT2 7NH, United Kingdom
Henning, Th.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Feng, S.:
Academia Sinica Institute of Astronomy and Astrophysics, Roosevelt Rd, Taipei, 10617, Taiwan
Cas Key Laboratory of Fast, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China
National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Galvan-Madrid, R.:
Instituto de Radioastronomía y Astrofísica (IRyA), UNAM, Apdo. Postal 72-3 (Xangari), Morelia, Michoacán, 58089, Mexico
De Souza Magalhães V.:
Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Saint Martin d'Hères, 38406, France
Moscadelli, L.:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze, 50125, Italy
Longmore, S.:
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, United Kingdom
Leurini, S.:
INAF, Osservatorio Astronomico di Cagliari, Via della Scienza 5, Selargius (CA), 09047, Italy
Kuiper, R.:
Institute of Astronomy and Astrophysics, University of Tübingen, Auf der Morgenstelle 10, Tübingen, 72076, Germany
Peters, T.:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Garching, 85748, Germany
Menten, K. M.:
Max Planck Institut for Radioastronomie, Auf dem Hügel 69, Bonn, 53121, Germany
Csengeri, T.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Fuller, G.:
Physics Department, UMIST, PO Box 88, Manchester, M60 1QD, United Kingdom
Wyrowski, F.:
Max Planck Institut for Radioastronomie, Auf dem Hügel 69, Bonn, 53121, Germany
Lumsden, S.:
School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, United Kingdom
Sanchez-Monge, A.:
I. Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, Koln, 50937, Germany
Maud, L.:
European Southern Observatory, Karl-Schwarzschild-Str. 2, Garching, 85748, Germany
Linz, H.:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
Palau, A.:
Instituto de Radioastronomía y Astrofísica (IRyA), UNAM, Apdo. Postal 72-3 (Xangari), Morelia, Michoacán, 58089, Mexico
Schilke, P.:
I. Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, Koln, 50937, Germany
Pety, J.:
Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Saint Martin d'Hères, 38406, France
LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, Paris, 75014, France
Pudritz, R.:
Department of Physics and Astronomy, McMaster University, 1280 Main St. W, Hamilton, ON L8S 4M1, Canada
Winters, J. M.:
Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Saint Martin d'Hères, 38406, France
Pietu, V.:
Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Saint Martin d'Hères, 38406, France
Hybrid Gold, Green Accepted, Green
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