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The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types

De Looze, Ilse and Cornier, Diane and Lebouteiller, Vianney and Madden, Suzanne and Baes, Marten and Bendo, George J. and Boquien, Médéric and Boselli, Alessandro and Clements, David L. and Cortese, Luca and Cooray, Asantha and Galametz, Maud and Galliano, Frédéric and Graciá-Carpio, Javier and Isaak, Kate and Karczewski, Oskar Ł. and Parkin, Tara J. and Pellegrini, Eric W. and Rémy-Ruyer, Aurélie and Spinoglio, Luigi and Smith, Matthew W. L. and Sturm, Eckhard (2014) The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types. Astronomy and Astrophysics, 568 . Art. No. A62. ISSN 0004-6361.

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Aims. We analyze the applicability of far-infrared fine-structure lines [Cii] 158 μm, [Oi] 63 μm, and [Oiii] 88 μm to reliably trace the star formation rate (SFR) in a sample of low-metallicity dwarf galaxies from the Herschel Dwarf Galaxy Survey and, furthermore, extend the analysis to a broad sample of galaxies of various types and metallicities in the literature. Methods. We study the trends and scatter in the relation between the SFR (as traced by GALEX FUV and MIPS 24 μm) and far-infrared line emission, on spatially resolved and global galaxy scales, in dwarf galaxies. We assemble far-infrared line measurements from the literature and infer whether the far-infrared lines can probe the SFR (as traced by the total infrared luminosity) in a variety of galaxy populations. Results. In metal-poor dwarfs, the [Oi]_(63) and [Oiii]_(88) lines show the strongest correlation with the SFR with an uncertainty on the SFR estimates better than a factor of 2, while the link between [Cii] emission and the SFR is more dispersed (uncertainty factor of 2.6). The increased scatter in the SFR–L_([CII]) relation toward low metal abundances, warm dust temperatures, and large filling factors of diffuse, highly ionized gas suggests that other cooling lines start to dominate depending on the density and ionization state of the gas. For the literature sample, we evaluate the correlations for a number of different galaxy populations. The [Cii] and [Oi]_(63) lines are considered to be reliable SFR tracers in starburst galaxies, recovering the star formation activity within an uncertainty of factor 2. For sources with composite and active galactic nucleus (AGN) classifications, all three FIR lines can recover the SFR with an uncertainty factor of 2.3. The SFR calibrations for ultra-luminous infrared galaxies (ULIRGs) are similar to starbursts/AGNs in terms of scatter but offset from the starburst/AGN SFR relations because of line deficits relative to their total infrared luminosity. While the number of detections of the FIR fine-structure lines is still very limited at high redshift for [Oi]_(63) and [Oiii]_(88), we provide an SFR calibration for [Cii].

Item Type:Article
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URLURL TypeDescription Paper
Boquien, Médéric0000-0003-0946-6176
Clements, David L.0000-0002-9548-5033
Cortese, Luca0000-0002-7422-9823
Cooray, Asantha0000-0002-3892-0190
Galametz, Maud0000-0002-0283-8689
Smith, Matthew W. L.0000-0002-3532-6970
Additional Information:© 2014 ESO. Received 14 August 2013. Accepted 7 May 2014. Published online 14 August 2014. I.D.L. is a postdoctoral researcher of the FWO-Vlaanderen (Belgium). V.L. is supported by a CEA/Marie Curie Eurotalents fellowship. This research was supported by the Agence Nationale pour la Recherche (ANR) through the programme SYMPATICO (Programme Blanc Projet ANR-11-BS56- 0023). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/ MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (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 and UKSA (UK); and NASA (USA).
Funding AgencyGrant Number
Marie Curie FellowshipUNSPECIFIED
Agence Nationale pour la Recherche (ANR)ANR-11-BS56-0023
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
Subject Keywords:Galaxy: abundances, galaxies: dwarf, galaxies: ISM, galaxies: star formation
Record Number:CaltechAUTHORS:20141017-094313833
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Official Citation:The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types Ilse De Looze, Diane Cormier, Vianney Lebouteiller, Suzanne Madden, Maarten Baes, George J. Bendo, Médéric Boquien, Alessandro Boselli, David L. Clements, Luca Cortese, Asantha Cooray, Maud Galametz, Frédéric Galliano, Javier Graciá-Carpio, Kate Isaak, Oskar Ł. Karczewski, Tara J. Parkin, Eric W. Pellegrini, Aurélie Rémy-Ruyer, Luigi Spinoglio, Matthew W. L. Smith and Eckhard Sturm A&A 568 A62 (2014) DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:50484
Deposited By: Ruth Sustaita
Deposited On:17 Oct 2014 17:24
Last Modified:17 Nov 2019 05:42

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