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Title:
The interstellar medium in Andromeda's dwarf spheroidal galaxies - I. Content and origin of the interstellar dust
Authors:
De Looze, Ilse; Baes, Maarten; Bendo, George J.; Fritz, Jacopo; Boquien, Médéric; Cormier, Diane; Gentile, Gianfranco; Kennicutt, Robert C.; Madden, Suzanne C.; Smith, Matthew W. L.; Young, Lisa
Affiliation:
AA(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK; Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ), AB(Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium), AC(UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK), AD(Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium; Instituto de Radioastronomía y Astrofísica, IRyA, UNAM, Campus Morelia, A.P. 3-72, C.P. 58089 Michoacán, Mexico), AE(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK; Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. U. de Antofagasta, 02800 Antofagasta, Chile), AF(Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle Str. 2, D-69120 Heidelberg, Germany), AG(Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium; Astrophysical Institute, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussels, Belgium), AH(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AI(Laboratoire AIM, CEA, Université Paris VII, IRFU/Service d'Astrophysique, Bat. 709, F-91191 Gif-sur-Yvette, France), AJ(School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK), AK(Physics Department, New Mexico Institute of Mining and Technology, Socorro, NM 87801, USA; Academia Sinica Institute of Astronomy and Astrophysics, PO Box 23-141, Taipei 10617, Taiwan, R.O.C.)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 459, Issue 4, p.3900-3916 (MNRAS Homepage)
Publication Date:
07/2016
Origin:
OUP
Astronomy Keywords:
galaxies: dwarf, galaxies: individual: NGC 147, galaxies: individual: NGC 185, galaxies: individual: NGC 205, Local Group, infrared: ISM
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stw868
Bibliographic Code:
2016MNRAS.459.3900D

Abstract

Dwarf spheroidal galaxies are among the most numerous galaxy population in the Universe, but their main formation and evolution channels are still not well understood. The three dwarf spheroidal satellites (NGC 147, NGC 185, and NGC 205) of the Andromeda galaxy are characterized by very different interstellar medium properties, which might suggest them being at different galaxy evolutionary stages. While the dust content of NGC 205 has been studied in detail in an earlier work, we present new Herschel dust continuum observations of NGC 147 and NGC 185. The non-detection of NGC 147 in Herschel SPIRE maps puts a strong constraint on its dust mass (<=128^{+124}_{-68} M&sun;). For NGC 185, we derive a total dust mass Md = 5.1±1.0 × 103 M&sun;, which is a factor of ˜2-3 higher than that derived from ISO and Spitzer observations and confirms the need for longer wavelength observations to trace more massive cold dust reservoirs. We, furthermore, estimate the dust production by asymptotic giant branch (AGB) stars and supernovae (SNe). For NGC 147, the upper limit on the dust mass is consistent with expectations of the material injected by the evolved stellar population. In NGC 185 and NGC 205, the observed dust content is one order of magnitude higher compared to the estimated dust production by AGBs and SNe. Efficient grain growth, and potentially longer dust survival times (3-6 Gyr) are required to account for their current dust content. Our study confirms the importance of grain growth in the gas phase to account for the current dust reservoir in galaxies.
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