The far-infrared/radio correlation as probed by Herschel
The far-infrared/radio correlation as probed by Herschel
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DOI：
10.1051/0004-6361/201014552
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发表时间：
2010-05
影响因子：
6.5
通讯作者：
R. Ivison;R. 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;J. Bock;Á. Bongiovanni;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;A. Cava;J. Cepa;P. Chanial;A. Cimatti;M. Cirasuolo;D. Clements;A. Conley;L. Conversi;A. Cooray;A. Cooray;E. Daddi;H. Dominguez;C. Dowell;C. Dowell;E. Dwek;S. Eales;D. Farrah;N. F. 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;L. Levenson;N. Lu;D. Lutz;S. Madden;B. Maffei;G. Magdis;G. Mainetti;R. Maiolino;L. Marchetti;G. Morrison;A. Mortier;H. Nguyen;H. Nguyen;R. Nordon;B. O’Halloran;S. Oliver;A. Omont;F. Owen;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Pérez-Fournon;A. P. Garćıa;A. Poglitsch;M. Pohlen;P. Popesso;F. Pozzi;J. Rawlings;G. Raymond;D. Rigopoulou;D. Rigopoulou;L. Riguccini;D. Rizzo;G. Rodighiero;I. Roseboom;M. Rowan‐Robinson;A. Saintonge;M. S. Portal;P. Santini;B. Schulz;D. Scott;N. Seymour;L. Shao;D. Shupe;A. Smith;J. Stevens;E. Sturm;M. Symeonidis;L. Tacconi;M. Trichas;K. Tugwell;Mattia Vaccari;I. Valtchanov;J. Vieira;L. Vigroux;Lian-Tao Wang;R. Ward;G. Wright;C. Xu;M. Zemcov;M. Zemcov
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作者：
R. Ivison;R. 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;J. Bock;Á. Bongiovanni;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;A. Cava;J. Cepa;P. Chanial;A. Cimatti;M. Cirasuolo;D. Clements;A. Conley;L. Conversi;A. Cooray;A. Cooray;E. Daddi;H. Dominguez;C. Dowell;C. Dowell;E. Dwek;S. Eales;D. Farrah;N. F. 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;L. Levenson;N. Lu;D. Lutz;S. Madden;B. Maffei;G. Magdis;G. Mainetti;R. Maiolino;L. Marchetti;G. Morrison;A. Mortier;H. Nguyen;H. Nguyen;R. Nordon;B. O’Halloran;S. Oliver;A. Omont;F. Owen;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Pérez-Fournon;A. P. Garćıa;A. Poglitsch;M. Pohlen;P. Popesso;F. Pozzi;J. Rawlings;G. Raymond;D. Rigopoulou;D. Rigopoulou;L. Riguccini;D. Rizzo;G. Rodighiero;I. Roseboom;M. Rowan‐Robinson;A. Saintonge;M. S. Portal;P. Santini;B. Schulz;D. Scott;N. Seymour;L. Shao;D. Shupe;A. Smith;J. Stevens;E. Sturm;M. Symeonidis;L. Tacconi;M. Trichas;K. Tugwell;Mattia Vaccari;I. Valtchanov;J. Vieira;L. Vigroux;Lian-Tao Wang;R. Ward;G. Wright;C. Xu;M. Zemcov;M. Zemcov
We set out to determine the ratio, q(IR), of rest-frame 8-1000um flux, S(IR), to monochromatic radio flux, S(1.4GHz), for galaxies selected at far-IR and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, and to identify any far-IR-bright outliers - useful laboratories for exploring why the far-IR/radio correlation is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-um and 1.4-GHz samples, obtained in GOODS-N using Herschel (HerMES; PEP) and the VLA. We determine bolometric IR output using ten bands spanning 24-1250um, exploiting data from PACS and SPIRE, 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 z, spanning log L(IR) = 11-12 L(sun) and z=0-2, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies, we see tentative evidence of a break in the flux ratio, q(IR), at L(1.4GHz) ~ 10^22.7 W/Hz, where AGN are starting to dominate the radio power density, and of weaker correlations with z and T(d). From our 250-um-selected sample we identify a small number of far-IR-bright outliers, and see trends of q(IR) with L(1.4GHz), L(IR), T(d) and z, 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) goes as (1+z)^gamma, where gamma = -0.04 +/- 0.03 at z=0-2; however, discounting the least reliable data at z 1.
