期刊
ASTRONOMY & ASTROPHYSICS
卷 518, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201014552
关键词
galaxies: evolution; galaxies: starburst; infrared: galaxies; submillimeter: galaxies; radio continuum: galaxies
资金
- CSA (Canada)
- NAOC (China)
- CEA, CNES, CNRS (France)
- ASI (Italy)
- MCINN (Spain)
- SNSB (Sweden)
- STFC (UK)
- NASA (USA)
- BMVIT (Austria)
- ESA-PRODEX (Belgium)
- CEA/CNES (France)
- DLR (Germany)
- CICYT/MCYT (Spain)
- STFC [PP/E001173/1, ST/G002630/1, ST/H002456/1, ST/F007019/1, ST/F002858/1, PP/E005306/1, ST/H001530/1, ST/G007039/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E005306/1, ST/G002630/1, ST/F007019/1, ST/G007039/1, ST/H002456/1, PP/E001181/1, ST/F002858/1, PP/E001173/1] Funding Source: researchfish
- UK Space Agency [ST/G003874/1] Funding Source: researchfish
We set out to determine the ratio, q(IR), of rest-frame 8-1000-mu m 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-mu m 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 lambda(obs) = 24-1250 mu m, 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-circle dot 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 similar to 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-mu m-selected sample we identify a small number of far-IR-bright outliers, and see trends of q(IR) with L1.4 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) proportional to (1+ z)(gamma), where gamma = -0.04 +/- 0.03 at z = 0 -2; however, discounting the least reliable data at z < 0.5 we find gamma = -0.26 +/- 0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by < 10-mu Jy radio activity amongst ordinary star-forming galaxies at z > 1.
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