The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗ plane up to z~2
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...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2015-01, Vol.573, p.A45 |
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| creator | Magnelli, B. Ivison, R. J. 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, S. J. Page, M. Popesso, P. Pozzi, F. Rigopoulou, D. Riguccini, L. Rodighiero, G. Rosario, D. Roseboom, I. Wang, L. Wuyts, S. |
| description | 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 |
| doi_str_mv | 10.1051/0004-6361/201424937 |
| format | Article |
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J. ; 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, S. J. ; Page, M. ; Popesso, P. ; Pozzi, F. ; Rigopoulou, D. ; Riguccini, L. ; Rodighiero, G. ; Rosario, D. ; Roseboom, I. ; Wang, L. ; Wuyts, S.</creator><creatorcontrib>Magnelli, B. ; Ivison, R. J. ; 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, S. J. ; Page, M. ; Popesso, P. ; Pozzi, F. ; Rigopoulou, D. ; Riguccini, L. ; Rodighiero, G. ; Rosario, D. ; Roseboom, I. ; Wang, L. ; Wuyts, S.</creatorcontrib><description>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 GHz610 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.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201424937</identifier><language>eng</language><publisher>EDP Sciences</publisher><subject>Flux ; Flux density ; Galaxies ; galaxies: evolution ; galaxies: formation ; galaxies: high-redshift ; galaxies: starburst ; infrared: galaxies ; Luminosity ; Planes ; Radio ; Red shift ; Spectra</subject><ispartof>Astronomy and astrophysics (Berlin), 2015-01, Vol.573, p.A45</ispartof><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c353t-3994cb0c637e1aea32e7d88d50d1736a38701cb99822fbb0e05caa73c449f5a33</citedby><cites>FETCH-LOGICAL-c353t-3994cb0c637e1aea32e7d88d50d1736a38701cb99822fbb0e05caa73c449f5a33</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,3727,27924,27925</link.rule.ids></links><search><creatorcontrib>Magnelli, B.</creatorcontrib><creatorcontrib>Ivison, R. J.</creatorcontrib><creatorcontrib>Lutz, D.</creatorcontrib><creatorcontrib>Valtchanov, I.</creatorcontrib><creatorcontrib>Farrah, D.</creatorcontrib><creatorcontrib>Berta, S.</creatorcontrib><creatorcontrib>Bertoldi, F.</creatorcontrib><creatorcontrib>Bock, J.</creatorcontrib><creatorcontrib>Cooray, A.</creatorcontrib><creatorcontrib>Ibar, E.</creatorcontrib><creatorcontrib>Karim, A.</creatorcontrib><creatorcontrib>Le Floc’h, E.</creatorcontrib><creatorcontrib>Nordon, R.</creatorcontrib><creatorcontrib>Oliver, S. J.</creatorcontrib><creatorcontrib>Page, M.</creatorcontrib><creatorcontrib>Popesso, P.</creatorcontrib><creatorcontrib>Pozzi, F.</creatorcontrib><creatorcontrib>Rigopoulou, D.</creatorcontrib><creatorcontrib>Riguccini, L.</creatorcontrib><creatorcontrib>Rodighiero, G.</creatorcontrib><creatorcontrib>Rosario, D.</creatorcontrib><creatorcontrib>Roseboom, I.</creatorcontrib><creatorcontrib>Wang, L.</creatorcontrib><creatorcontrib>Wuyts, S.</creatorcontrib><title>The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗ plane up to z~2</title><title>Astronomy and astrophysics (Berlin)</title><description>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 GHz610 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.</description><subject>Flux</subject><subject>Flux density</subject><subject>Galaxies</subject><subject>galaxies: evolution</subject><subject>galaxies: formation</subject><subject>galaxies: high-redshift</subject><subject>galaxies: starburst</subject><subject>infrared: galaxies</subject><subject>Luminosity</subject><subject>Planes</subject><subject>Radio</subject><subject>Red shift</subject><subject>Spectra</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqNkb1u3DAQhAnDBnK28wRpWKZRjuRSJFXGh_gHuCCB_5KOWFGUTVuWFFIHXFwELt2nyPv5SSzhgqtdLXbxzWAxQ8gHzj5xlvM5Y0xmChSfC8alkAXoHTLjEkTGtFS7ZLYl3pH9lO7GVXADMxIubz2tMWahrSNGX80jVqGjrovRNziErqXYVnRzTb13Q8SGhrbya9rV9AYbXAefxgsdRquL4_OXp79fX57_0b7B1tNVT4eOPv4Rh2Svxib59__nAbk6_nK5OM2W307OFp-XmYMchgyKQrqSOQXac_QIwuvKmCpnFdegEIxm3JVFYYSoy5J5ljtEDU7Kos4R4IB83Pj2sfu18mmwDyE530zfdKtkuTaKa2HUW1CVFzkDzUYUNqiLXUrR17aP4QHjb8uZnTqwU8J2SthuOxhV2UYV0uDXWwnGe6s06Nwa9sPK5eL6-_XRT3sEr5I8iVs</recordid><startdate>201501</startdate><enddate>201501</enddate><creator>Magnelli, B.</creator><creator>Ivison, R. 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J.</au><au>Lutz, D.</au><au>Valtchanov, I.</au><au>Farrah, D.</au><au>Berta, S.</au><au>Bertoldi, F.</au><au>Bock, J.</au><au>Cooray, A.</au><au>Ibar, E.</au><au>Karim, A.</au><au>Le Floc’h, E.</au><au>Nordon, R.</au><au>Oliver, S. J.</au><au>Page, M.</au><au>Popesso, P.</au><au>Pozzi, F.</au><au>Rigopoulou, D.</au><au>Riguccini, L.</au><au>Rodighiero, G.</au><au>Rosario, D.</au><au>Roseboom, I.</au><au>Wang, L.</au><au>Wuyts, S.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗ plane up to z~2</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2015-01</date><risdate>2015</risdate><volume>573</volume><spage>A45</spage><pages>A45-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><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 GHz610 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.</abstract><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201424937</doi></addata></record> |
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| ispartof | Astronomy and astrophysics (Berlin), 2015-01, Vol.573, p.A45 |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Flux Flux density Galaxies galaxies: evolution galaxies: formation galaxies: high-redshift galaxies: starburst infrared: galaxies Luminosity Planes Radio Red shift Spectra |
| title | The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗ plane up to z~2 |
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