Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-23T23:36:18.321Z Has data issue: false hasContentIssue false
  • English
  • Français

A double core in the Auriga-California Molecular Cloud

Published online by Cambridge University Press:  13 January 2020

Sarolta Zahorecz ,
Daniel Molnar ,
Alex Kraus  and
Toshikazu Onishi
Sarolta Zahorecz
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: [email protected] Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan Eötvös Loránd University, Department of Astronomy, Pázmány Péter sétány 1/A, 1117, Budapest, Hungary
Daniel Molnar
Affiliation:
Osservatorio Astronomico di Cagliari, Via della Scienza, 5, 09047 Cuccuru Angius, Selargius CA, Italy
Alex Kraus
Affiliation:
Max Planck Institut fúr Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany
Toshikazu Onishi
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Planck cold clump G163.82-8.44 is part of the Auriga-California Molecular Cloud. It was observed with Herschel PACS and SPIRE instruments as part of the Herschel open time key programme Galactic Cold Cores. Follow-up ground-based molecular line observation of NH3 was performed to the densest part of the filament with the Effelsberg-100m telescope. We detected two different velocity components with a separation of 0.5 km/s. We performed radiative transfer modeling with two 3-dimensional spheres to characterise the temperature and density of the dense cores. We have found that the temperatures of the two cores are almost the same, 10.8 K and 11.1 K and their mass and size ratios are 1:10 and 1:5, respectively.

Keywords

radiative transfermolecular dataISM: structurestars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 335 - 336
Copyright
© International Astronomical Union 2020 

References

Juvela, M. 1997, A&A, 322, 943 Google Scholar
Juvela, M., et al. 2012, A&A, 518, L93 Google Scholar
Juvela, M., et al. 2012, A&A, 541, A12 Google Scholar
Juvela, M., et al. 2018, A&A, 614, A83 Google Scholar
Könyves, V., et al. 2007, A&A, 463, 1227 Google Scholar
Montillaud, J., et al. 2015, A&A, 584, A92 Google Scholar
Collaboration, Planck, et al. 2011, A&A, 536, A23 Google Scholar
Rivera-Ingraham, A., et al. 2016, A&A, 591, A90 Google Scholar
Rivera-Ingraham, A., et al. 2017, A&A, 601, A94 Google Scholar
Tauber, J. A., et al. 2010, A&A, 520, A1 Google Scholar
Tóth, L. V., et al. 2002, A&A, 395, 663 Google Scholar
Tóth, L. V., et al. 2004, A&A, 420, 533 Google Scholar
Tóth, L. V., et al. 2017, IAUS, 316, 133 Google Scholar