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Date and Time of the Query: 2019-08-19 T20:54:48 PDT
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For refcode 2006ApJ...651L.111M:
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2006ApJ...651L.111M The Effect of Star Formation on the Far-Infrared -- Radio Correlation within Galaxies E. J. Murphy, G. Helou, R. Braun, J. D. P. Kenney, L. Armus, D. Calzetti, B. T. Draine, R. C. Kennicutt, Jr., H. Roussel, F. Walter, G. J. Bendo, B. Buckalew, D. A. Dale, C. W. Engelbracht, J. D. T. Smith, and M. D. Thornley Abstract. Using data obtained for 12 galaxies as part of the Spitzer Infrared Nearby Galaxies Survey (SINGS) and the Westerbork Synthesis Radio Telescope (WSRT) SINGS radio continuum survey, we study how star formation activity affects the far-infrared -- radio correlation within galaxies by testing a phenomenological model that describes the radio image as a smeared version of the far-infrared image. The physical basis of this description is that cosmic-ray (CR) electrons will diffuse measurably farther than the mean free path of dust-heating photons before decaying by synchrotron radiation. This description works well in general. Galaxies with higher infrared surface brightnesses have best-fit smoothing scale lengths of a few hundred parsecs, substantially shorter than those for lower surface brightness galaxies. We interpret this result to suggest that galaxies with higher disk-averaged star formation rates have had a recent episode of enhanced star formation and are characterized by a higher fraction of young CR electrons that have traveled only a few hundred parsecs from their acceleration sites in supernova remnants compared to galaxies with lower star formation activity. Key words: ISM: Cosmic Rays, Infrared: Galaxies, Radio Continuum: Galaxies =========================================================================== 2008ApJ...672L..85M Erratum: "The Effect of Star Formation on the Far-Infrared-Radio Correlation within Galaxies" (ApJ, 651, L111 [2006]) Murphy, E. J.; Helou, G.; Braun, R.; Kenney, J. D. P.; Armus, L.; Calzetti, D.; Draine, B. T.; Kennicutt, R. C., Jr.; Roussel, H.; Walter, F.; Bendo, G. J.; Buckalew, B.; Dale, D. A.; Engelbracht, C. W.; Smith, J. D. T.; Thornley, M. D. Abstract. We noticed an error in the coefficient of equation (3); the correct equation is (({tau}_cool_)/yr)~5.7x10^7^({nu}/GHz)^-1/2^(B/{mu}G)^1/2^((U_B_+U_rad_) /(10^-12^ ergs cm^-3^))^-1^. (1)This did not impact the results or conclusions made in the rest of the text. All calculations using this equation were in fact correct. ===========================================================================
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