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Linking dust emission to fundamental properties in galaxies: the low-metallicity picture

Rémy-Ruyer, A. and Madden, S. C. and Galliano, F. and Lebouteiller, V. and Baes, M. and Bendo, G. J. and Boselli, A. and Ciesla, L. and Cormier, D. and Cooray, A. and Cortese, L. and De Looze, I. and Doublier-Pritchard, V. and Galametz, M. and Jones, A. P. and Karczewski, O. Ł. and Lu, N. and Spinoglio, L. (2015) Linking dust emission to fundamental properties in galaxies: the low-metallicity picture. Astronomy and Astrophysics, 582 . Art. No. A121. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20151208-092008533

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Abstract

Aims. In this work, we aim to provide a consistent analysis of the dust properties from metal-poor to metal-rich environments by linking them to fundamental galactic parameters. Methods. We consider two samples of galaxies: the Dwarf Galaxy Survey (DGS) and the Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel (KINGFISH), totalling 109 galaxies, spanning almost 2 dex in metallicity. We collect infrared (IR) to submillimetre (submm) data for both samples and present the complete data set for the DGS sample. We model the observed spectral energy distributions (SED) with a physically-motivated dust model to access the dust properties: dust mass, total-IR luminosity, polycyclic aromatic hydrocarbon (PAH) mass fraction, dust temperature distribution, and dust-to-stellar mass ratio. Results. Using a different SED model (modified black body), different dust composition (amorphous carbon in lieu of graphite), or a different wavelength coverage at submm wavelengths results in differences in the dust mass estimate of a factor two to three, showing that this parameter is subject to non-negligible systematic modelling uncertainties. We find half as much dust with the amorphous carbon dust composition. For eight galaxies in our sample, we find a rather small excess at 500 μm (≤1.5σ). We find that the dust SED of low-metallicity galaxies is broader and peaks at shorter wavelengths compared to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The PAH mass fraction and dust temperature distribution are found to be driven mostly by the specific star formation rate, sSFR, with secondary effects from metallicity. The correlations between metallicity and dust mass or total-IR luminosity are direct consequences of the stellar mass-metallicity relation. The dust-to-stellar mass ratios of metal-rich sources follow the well-studied trend of decreasing ratio for decreasing sSFR. The relation is more complex for low-metallicity galaxies with high sSFR, and depends on the chemical evolutionary stage of the source (i.e. gas-to-dust mass ratio). Dust growth processes in the ISM play a key role in the dust mass build-up with respect to the stellar content at high sSFR and low metallicity. Conclusions. We conclude that the evolution of the dust properties from metal-poor to metal-rich galaxies derives from a complex interplay between star formation activity, stellar mass, and metallicity.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201526067 DOIArticle
http://arxiv.org/abs/1507.05432arXivDiscussion Paper
ORCID:
AuthorORCID
Cooray, A.0000-0002-3892-0190
Cortese, L.0000-0002-7422-9823
Galametz, M.0000-0002-0283-8689
Lu, N.0000-0002-8948-1044
Additional Information:© 2015 ESO. Received 10 March 2015. Accepted 14 July 2015. The authors would like to thank R. Asano for providing the evolutionary tracks for his model for Fig. 11, and H. Hirashita and T. Takeuchi for interesting discussions on the chemical evolution models. This research was made possible through the financial support of the Agence Nationale de la Recherche (ANR) through the programme SYMPATICO (Program Blanc Projet ANR-11-BS56-0023) and also through the EU FP7 funded project DustPedia (Grant No. 606847). IDL is a postdoctoral researcher of the FWO-Vlaanderen (Belgium). This research has made use of the NASA/IPAC Extragalactic Database (NED) and of the NASA/IPAC Infrared Science Archive, which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. PACS has been developed by MPE (Germany); UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by Cardiff University (UK); Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); SNSB (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Agence Nationale pour la Recherche (ANR)ANR-11-BS56-0023
European Research Council (ERC)606847
NASA/JPL/CaltechUNSPECIFIED
Bundesministerium für Verkehr, Innovation und Technologie (BMVIT)UNSPECIFIED
ESA-PRODEX (Belgium)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Deutschen Zentrums für Luft- und Raumfahrt (DLR)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Comisión Interministerial de Ciencia y Tecnología (CICYT)UNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Stockholm ObservatoryUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
NASAUNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
Ministerio de Ciencia y Tecnologia (MCYT)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Subject Keywords:dust, extinction, evolution, galaxies: dwarf, galaxies: evolution, infrared: ISM, infrared: galaxies
Record Number:CaltechAUTHORS:20151208-092008533
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151208-092008533
Official Citation:Linking dust emission to fundamental properties in galaxies: the low-metallicity picture A. Rémy-Ruyer, S. C. Madden, F. Galliano, V. Lebouteiller, M. Baes, G. J. Bendo, A. Boselli, L. Ciesla, D. Cormier, A. Cooray, L. Cortese, I. De Looze, V. Doublier-Pritchard, M. Galametz, A. P. Jones, O. Ł. Karczewski, N. LuA. Rémy-Ruyer, S. C. Madden, F. Galliano, V. Lebouteiller, M. Baes, G. J. Bendo, A. Boselli, L. Ciesla, D. Cormier, A. Cooray, L. Cortese, I. De Looze, V. Doublier-Pritchard, M. Galametz, A. P. Jones, O. Ł. Karczewski, N. Lu and L. Spinoglio A&A, 582 (2015) A121 DOI: http://dx.doi.org/10.1051/0004-6361/201526067
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62687
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:08 Dec 2015 20:04
Last Modified:17 Nov 2019 05:33

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