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Title:
A CH3CN and HCO+ survey towards southern methanol masers associated with star formation
Authors:
Purcell, C. R.; Balasubramanyam, R.; Burton, M. G.; Walsh, A. J.; Minier, V.; Hunt-Cunningham, M. R.; Kedziora-Chudczer, L. L.; Longmore, S. N.; Hill, T.; Bains, I.; Barnes, P. J.; Busfield, A. L.; Calisse, P.; Crighton, N. H. M.; Curran, S. J.; Davis, T. M.; Dempsey, J. T.; Derragopian, G.; Fulton, B.; Hidas, M. G.; Hoare, M. G.; Lee, J.-K.; Ladd, E. F.; Lumsden, S. L.; Moore, T. J. T.; Murphy, M. T.; Oudmaijer, R. D.; Pracy, M. B.; Rathborne, J.; Robertson, S.; Schultz, A. S. B.; Shobbrook, J.; Sparks, P. A.; Storey, J.; Travouillion, T.
Affiliation:
AA(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AB(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Raman Research Institute, Sadashivanagar, Bangalore 560 080, India), AC(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AD(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AE(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Service d'Astrophysique, DAPNIA/DSM/CEA Saclay, 91191 Gif-sur-Yvette, France; AIM, Unité Mixte de Recherche, CEA-CNRS-Université Paris VII, UMR 7158, CEA/Saclay, 91191 Gif sur Yvette, France), AF(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AG(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; School of Physics, University of Sydney, NSW 2006, Australia), AH(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; CSIRO Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia), AI(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AJ(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AK(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; School of Physics, University of Sydney, NSW 2006, Australia), AL(School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT), AM(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; School of Physics and Astronomy, University of Wales, Cardiff, 5, The Parade, Cardiff CF24 3YB), AN(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AO(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AP(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Research School of Astronomy and Astrophysics, The Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia), AQ(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AR(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AS(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Centre for Astronomy, James Cook University, Townsville, QLD 4811, Australia), AT(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AU(School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT), AV(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Department of Pure and Applied Physics, Queen's University, Belfast BT7 1NN), AW(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; CSIRO Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia; Department of Physics, Bucknell University, Lewisburg, PA 17837, USA), AX(School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT), AY(Astrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Egerton Wharf, Birkenhead CH41 1LD), AZ(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA), BA(School of Physics, University of Sydney, NSW 2006, Australia), BB(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), BC(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA), BD(CSIRO Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia), BE(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), BF(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), BG(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), BH(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), BI(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; California Institute of Technology, 1200 E. California Blvd, Pasadena 91125, CA, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 367, Issue 2, pp. 553-576. (MNRAS Homepage)
Publication Date:
04/2006
Origin:
MNRAS
MNRAS Keywords:
surveys, stars: formation, stars: pre-main-sequence, ISM: abundances, HII regions, ISM: molecules
DOI:
10.1111/j.1365-2966.2005.09921.x
Bibliographic Code:
2006MNRAS.367..553P

Abstract

We present the initial results of a 3-mm spectral-line survey towards 83 methanol maser-selected massive star-forming regions. Here, we report observations of the J=5-4 and 6-5 rotational transitions of methyl cyanide (CH3CN) and the J=1-0 transition of HCO+ and H13CO+.

CH3CN emission is detected in 58 sources (70per cent of our sample). We estimate the temperature and column density for 37 of these using the rotational diagram (RD) method. The temperatures we derive range from 28-166K, and are lower than previously reported temperatures, derived from higher J transitions. We find that CH3CN is brighter and more commonly detected towards ultracompact HII (UCHII) regions than towards isolated maser sources. Detection of CH3CN towards isolated maser sources strongly suggests that these objects are internally heated and that CH3CN is excited prior to the UCHII phase of massive star formation.

HCO+ is detected towards 82 sources (99per cent of our sample), many of which exhibit asymmetric line profiles compared to H13CO+. Skewed profiles are indicative of inward or outward motions, however, we find approximately equal numbers of red- and blue-skewed profiles among all classes. Column densities are derived from an analysis of the HCO+ and H13CO+ line profiles.

80 sources have mid-infrared (mid-IR) counterparts: 68 seen in emission and 12 seen in absorption as `dark clouds'. Seven of the 12 dark clouds exhibit asymmetric HCO+ profiles, six of which are skewed to the blue, indicating infalling motions. CH3CN is also common in dark clouds, where it has a 90per cent detection rate.


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