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Title:
The gas-to-dust mass ratio of Centaurus A as seen by Herschel
Authors:
Parkin, T. J.; Wilson, C. D.; Foyle, K.; Baes, M.; Bendo, G. J.; Boselli, A.; Boquien, M.; Cooray, A.; Cormier, D.; Davies, J. I.; Eales, S. A.; Galametz, M.; Gomez, H. L.; Lebouteiller, V.; Madden, S.; Mentuch, E.; Page, M. J.; Pohlen, M.; Remy, A.; Roussel, H.; Sauvage, M.; Smith, M. W. L.; Spinoglio, L.
Affiliation:
AA(Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada), AB(Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada), AC(Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada), AD(Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium), AE(UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL), AF(Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille, Cedex 13, France), AG(Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille, Cedex 13, France), AH(Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA), AI(CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France), AJ(School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA), AK(School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA), AL(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA), AM(School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA), AN(CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France), AO(CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France), AP(Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada), AQ(Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT), AR(School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA), AS(CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France), AT(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, France), AU(CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France), AV(School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA), AW(Istituto di Fisica dello Spazio Interplanetario, INAF, Via del Fosso del Cavaliere 100, I-00133 Rome, Italy)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 422, Issue 3, pp. 2291-2301. (MNRAS Homepage)
Publication Date:
05/2012
Origin:
WILEY
Astronomy Keywords:
galaxies: individual: Centaurus A, galaxies: ISM, infrared: ISM, submillimetre: ISM
Abstract Copyright:
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
DOI:
10.1111/j.1365-2966.2012.20778.x
Bibliographic Code:
2012MNRAS.422.2291P

Abstract

We present photometry of the nearby galaxy NGC 5128 (Centaurus A) observed with the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on board the Herschel Space Observatory, at 70, 160, 250, 350 and 500 mum, as well as new CO J= 3-2 observations taken with the HARP-B instrument on the James Clerk Maxwell Telescope (JCMT). Using a single-component modified blackbody, we model the dust spectral energy distribution within the disc of the galaxy using all five Herschel wavebands and find dust temperatures of ˜30 K towards the centre of the disc and a smoothly decreasing trend to ˜20 K with increasing radius. We find a total dust mass of (1.59 ± 0.05) × 107 M&sun; and a total gas mass of (2.7 ± 0.2) × 109 M&sun;. The average gas-to-dust mass ratio is 103 ± 8, but we find an interesting increase in this ratio to approximately 275 towards the centre of Cen A. We discuss several possible physical processes that may be causing this effect, including dust sputtering, jet entrainment and systematic variables such as the XCO factor. Dust sputtering by X-rays originating in the active galactic nucleus or the removal of dust by the jets is our most favoured explanation. a PACS values are divisive and SPIRE values are multiplicative. b These uncertainties are for the pixels at their native pixel scale, as listed in this table. c We have ignored the fact that the SPIRE calibration errors are correlated between all three bands and our total 7 per cent error comprises 5 per cent correlated error and 5 per cent uncorrelated error.
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