Magnelli, B; Ivison, RJ; Lutz, D; Valtchanov, I; Farrah, D; Berta, S; Bertoldi, F; ... Wuyts, S; + view all Magnelli, B; Ivison, RJ; Lutz, D; Valtchanov, I; Farrah, D; Berta, S; Bertoldi, F; Bock, J; Cooray, A; Ibar, E; Karim, A; Le Floc'h, E; Nordon, R; Oliver, SJ; Page, M; Popesso, P; Pozzi, F; Rigopoulou, D; Riguccini, L; Rodighiero, G; Rosario, D; Roseboom, I; Wang, L; Wuyts, S; - view fewer (2015) The far-infrared/radio correlation and radio spectral index of galaxies in the SFR-M∗ plane up to z~2*. Astronomy and Astrophysics , 573 , Article A45. 10.1051/0004-6361/201424937.

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Abstract

We study the evolution of the radio spectral index and far-infrared/radio correlation (FRC) across the star-formation rate - stellar masse (i.e. SFR-M∗) plane up to z ~ 2. We start from a stellar-mass-selected sample of galaxies with reliable SFR and redshift estimates. We then grid the SFR-M∗ plane in several redshift ranges and measure the infrared luminosity, radio luminosity, radio spectral index, and ultimately the FRC index (i.e. qFIR) of each SFR-M∗-z bin. The infrared luminosities of our SFR-M∗-z bins are estimated using their stacked far-infrared flux densities inferred from observations obtained with the Herschel Space Observatory. Their radio luminosities and radio spectral indices (i.e. α, where Sν ∝ ν-α) are estimated using their stacked 1.4 GHz and 610 MHz flux densities from the Very Large Array and Giant Metre-wave Radio Telescope, respectively. Our far-infrared and radio observations include the most widely studied blank extragalactic fields - GOODS-N, GOODS-S, ECDFS, and COSMOS - covering a total sky area of ~2.0 deg2. Using this methodology, we constrain the radio spectral index and FRC index of star-forming galaxies with M∗ > 1010 M⊙ and 0 <z< 2.3. We find that α1.4 GHz 610 MHz does not evolve significantly with redshift or with the distance of a galaxy with respect to the main sequence (MS) of the SFR-M∗ plane (i.e. Δlog(SSFR)MS = log[SSFR(galaxy)/SSFRMS(M∗,z)]). Instead, star-forming galaxies have a radio spectral index consistent with a canonical value of 0.8, which suggests that their radio spectra are dominated by non-thermal optically thin synchrotron emission. We find that the FRC index, qFIR, displays a moderate but statistically significant redshift evolution as qFIR(z) = (2.35 ± 0.08) × (1 + z)-0.12 ± 0.04, consistent with some previous literature. Finally, we find no significant correlation between qFIR and Δlog(SSFR)MS, though a weak positive trend, as observed in one of our redshift bins (i.e. Δ [qFIR]/Δ [Δlog(SSFR)MS] = 0.22 ± 0.07 at 0.5 <z< 0.8), cannot be firmly ruled out using our dataset.

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