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Millimetre molecular lines in Planck cold clumps

Published online by Cambridge University Press:  27 October 2016

Paul A. Jones ,
Maria R. Cunningham ,
L. Viktor Tóth ,
Tie Liu  and
John A. P. Lopez
Paul A. Jones
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
Maria R. Cunningham
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
L. Viktor Tóth
Affiliation:
Department of Astronomy, Loránd Eötvös University, Budapest, Hungary
Tie Liu
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon, Korea
John A. P. Lopez
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
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Abstract

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Galactic cold clumps have been identified from the Planck data (Planck Collaboration, 2011a, 2011b, 2015) as 10 342 cold (7 - 19 K) sources that stand out against a warmer environment, with the Early Cold Cores as a subsample of 915 most reliable detections. There is CO emission associated with the Planck Cold Clumps (PCCs), which has been observed with ground-based radio telescopes at higher resolution (Wu et al. 2012, Liu et al. 2014). A subset of PCCs have also been observed with Herschel at higher resolution (Juvela et al. 2012).

A southern sub-sample of the PCCs has been observed with the Mopra 22-m telescope to study the molecular gas. The Mopra telescope has 3-mm, 7-mm and 12-mm bands, with broadband correlator configuration 8-GHz wide with 0.27-MHz channels, or multiple zoom bands 137-MHz wide with 33-KHz channels, within the 8 GHz.

During the 2013 southern winter season we observed 10 clumps. This included observations in the 3-mm band of 12CO, 13CO and C18O and lines around 89 GHz (e.g. HCN, HCO+ and HNC), in the 7-mm band (e.g. CS) and in the 12-mm band (e.g. NH3). These observations were heterogenous, with sources selected by LST in gaps between observations of other projects, and band chosen by weather (i.e. in conditions unsuitable for higher frequencies, lower frequency bands were observed). During the 2014 season we observed 34 positions in 22 clumps, with zoom mode observations of lines around 89 GHz. This was a more well-defined sample of sources.

The mapping of the CO lines shows good spatial correlation of the CO with the dust column density The CO isotoplogues show high optical depth in 12CO and 13CO. The lines of HCN, HCO+ and HNC are weak, but detected in many of the 2014 sample. We are modelling the line results to determine column densities, excitation temperatures and abundances, using tools such as radex (van der Tak et al. 2007).

Keywords

ISM: moleculesISM: kinematics and dynamicsradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 60
Copyright
Copyright © International Astronomical Union 2016 

References

Juvela, M., et al., 2012, A&A, 541, A12 Google Scholar
Liu, T., et al., 2014, arXiv, arXiv:1410.6979Google Scholar
Planck Collaboration, 2011a, A&A, 536, A22 Google Scholar
Planck Collaboration, 2011b, A&A, 536, A23 Google Scholar
Planck Collaboration, 2015, arXiv, arXiv:1502.01599Google Scholar
van der Tak, F. F. S., Black, J. H., Schöier, F. L., Jansen, D. J., & van Dishoeck, E. F., 2007, A&A, 468, 627 Google Scholar
Wu, Y., Liu, T., Meng, F., Li, D., Qin, S.-L., & Ju, B.-G., 2012, ApJ, 756, 76 Google Scholar