Ivison, R. J. and Blain, A. and Bock, J. and Cooray, A. and Dowell, C. D. and Levenson, L. and Lu, N. and Nguyen, H. T. and Schulz, B. and Shupe, D. L. and Vieira, J. and Xu, C. K. and Zemcov, M. (2010) The far-infrared/radio correlation as probed by Herschel. Astronomy and Astrophysics, 518 . Art. No. L31. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20101202-100221983
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We set out to determine the ratio, q_(IR), of rest-frame 8–1000-μm flux, S_(IR), to monochromatic radio flux, S_(1.4 GHz), for galaxies selected at far-infrared (IR) and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, T_d, and to identify any far-IR-bright outliers – useful laboratories for exploring why the far-IR/radio correlation (FIRRC) is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-μm and 1.4-GHz samples, obtained using Herschel and the Very Large Array (VLA) in GOODS-North (-N). We determine bolometric IR output using ten bands spanning λ_(obs) = 24−1250 μm, exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an L_(IR)-matched sample, designed to reveal evolution of q_(IR) with redshift, spanning log L_(IR) = 11–12 L_⊙ and z = 0−2, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies in GOODS-N, we see tentative evidence of a break in the flux ratio, q_(IR), at L_(1.4 GHz) ~ 10^(22.7) WHz^(−1) where active galactic nuclei (AGN) are starting to dominate the radio power density, and of weaker correlations with redshift and T_d. From our 250-μm-selected sample we identify a small number of far-IR-bright outliers, and see trends of q_(IR) with L_(1.4 GHz), L_(IR), T_d and redshift, noting that some of these are inter-related. For our L_(IR-)matched sample, there is no evidence that q_(IR) changes significantly as we move back into the epoch of galaxy formation: we find q_(IR) ∝ (1+z)^γ, where γ = −0.04 ± 0.03 at z = 0 − 2; however, discounting the least reliable data at z < 0.5 we find γ = −0.26 ± 0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by <10-μJy radio activity amongst ordinary star-forming galaxies at z > 1.
|Additional Information:||© 2010 ESO. Received 30 March 2010, Accepted 23 April 2010, Published Online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). 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); 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 (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, 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 (Italy), and CICYT/MCYT (Spain).|
|Subject Keywords:||galaxies: evolution, galaxies: starburst, infrared: galaxies, submillimeter: galaxies, radio continuum: galaxies|
|Official Citation:||The far-infrared/radio correlation as probed by Herschel R. J. Ivison, B. Magnelli, E. Ibar, P. Andreani, D. Elbaz, B. Altieri, A. Amblard, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodríguez, A. Cava, J. Cepa, P. Chanial, A. Cimatti, M. Cirasuolo, D. L. Clements, A. Conley, L. Conversi, A. Cooray, E. Daddi, H. Dominguez, C. D. Dowell, E. Dwek, S. Eales, D. Farrah, N. Förster Schreiber, M. Fox, A. Franceschini, W. Gear, R. Genzel, J. Glenn, M. Griffin, C. Gruppioni, M. Halpern, E. Hatziminaoglou, K. Isaak, G. Lagache, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, G. Magdis, G. Mainetti, R. Maiolino, L. Marchetti, G. E. Morrison, A. M. J. Mortier, H. T. Nguyen, R. Nordon, B. O'Halloran, S. J. Oliver, A. Omont, F. N. Owen, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, A. M. Pérez García, A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J. I. Rawlings, G. Raymond, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, B. Schulz, D. Scott, N. Seymour, L. Shao, D. L. Shupe, A. J. Smith, J. A. Stevens, E. Sturm, M. Symeonidis, L. Tacconi, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, J. Vieira, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu and M. Zemcov A&A 518 L31 (2010) DOI: 10.1051/0004-6361/201014552|
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|Deposited By:||Benjamin Perez|
|Deposited On:||02 Dec 2010 20:45|
|Last Modified:||30 Jan 2017 21:03|
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