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Determining star formation rates for infrared galaxies



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Rieke, G. H. and Alonso Herrero, A. and Weiner, B. J. and Pérez González, Pablo Guillermo and Blaylock, M. and Donley, J. L. and Marcillac, D. (2009) Determining star formation rates for infrared galaxies. Astrophysical journal, 692 (1). pp. 556-573. ISSN 0004-637X


Official URL: http://dx.doi.org/10.1088/0004-637X/692/1/556



We show that measures of star formation rates (SFRs) for infrared galaxies using either single-band 24 μm or extinction-corrected Paα luminosities are consistent in the total infrared luminosity = L(TIR) ~ 10^10 L_☉ range. MIPS 24 μm photometry can yield SFRs accurately from this luminosity upward: SFR(M_☉ yr^–1) = 7.8 × 10^–10 L(24 μm, L_☉) from L(TIR) = 5× 10^9 L_☉ to 10^11 L_☉ and SFR = 7.8 × 10^–10 L(24 μm, L_☉)(7.76 × 10^–11 L(24))^0.048 for higher L(TIR). For galaxies with L(TIR) ≥ 10^10 L_☉, these new expressions should provide SFRs to within 0.2 dex. For L(TIR) ≥ 10^11 L_☉, we find that the SFR of infrared galaxies is significantly underestimated using extinction-corrected Paα (and presumably using any other optical or near-infrared recombination lines). As a part of this work, we constructed spectral energy distribution templates for eleven luminous and ultraluminous purely star forming infrared galaxies and over the spectral range 0.4 μm to 30 cm. We use these templates and the SINGS data to construct average templates from 5 μm to 30 cm for infrared galaxies with L(TIR) = 5× 10^9 to 10^13 L_☉. All of these templates are made available online.

Item Type:Article
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© 2009 The American Astronomical Society. All rights reserved.
We are grateful for helpful discussions with Phil Appleton, Chad Engelbracht, and Robert Kennicutt. We also thank Daniela Calzetti for providing the Paα measurements, Jennifer Sierchio for resampling the LIRG and ULIRG SEDs onto a common wavelength scale, Eckhard Sturm for providing the PACS response curves, and Alistair Glasse for providing MIRI response curves. We also thank the FIDEL team, led by Mark Dickinson, for the data presented in Figures 17 and 18. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. This research has used the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory under contract with NASA. It also makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. Support for this work was provided by NASA through JPL/Caltech contract 1255094 and by NAG5-12318 from NASA/Goddard to the University of Arizona. Funding for the DEEP2 survey has been provided by NSF grants AST95- 09298, AST-0071048, AST-0071198, AST-0507428, and AST- 0507483 as well as NASA LTSA grant NNG04GC89G. P. G. Pérez González acknowledges support from the grants PNAYA ´ 2006–02358 and PNAYA 2006–15698–C02–02 and from the Ramón y Cajal Program, financed by the Spanish Government and the European Union.

Uncontrolled Keywords:Initial mass function; Spitzer-space-telescope; Multiband imaging photometer; Active galactic nuclei; Submillimeter galaxies; Nearby galaxies; Forming galaxies; H-alpha; Radio correlation; Spiral galaxies
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:38660
Deposited On:29 Jul 2016 14:11
Last Modified:10 Dec 2018 15:05

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