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http://hdl.handle.net/20.500.12386/30097
Title: | A LOFAR-IRAS cross-match study: the far-infrared radio correlation and the 150 MHz luminosity as a star-formation rate tracer | Authors: | Wang, L. Gao, F. Duncan, K. J. Williams, W. L. Rowan-Robinson, M. Sabater, J. Shimwell, T. W. BONATO, MATTEO Calistro-Rivera, G. Chyży, K. T. Farrah, D. Gürkan, G. Hardcastle, M. J. McCheyne, I. PRANDONI, ISABELLA READ, SHAUN CONISBEE Röttgering, H. J. A. Smith, D. J. B. |
Issue Date: | 2019 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 631 | First Page: | A109 | Abstract: | <BR /> Aims: We aim to study the far-infrared radio correlation (FIRC) at 150 MHz in the local Universe (at a median redshift ⟨z⟩∼0.05) and improve the use of the rest-frame 150 MHz luminosity, L<SUB>150</SUB>, as a star-formation rate (SFR) tracer, which is unaffected by dust extinction. <BR /> Methods: We cross-match the 60 μm selected Revised IRAS Faint Source Survey Redshift (RIFSCz) catalogue and the 150 MHz selected LOFAR value-added source catalogue in the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) Spring Field. We estimate L<SUB>150</SUB> for the cross-matched sources and compare it with the total infrared (IR) luminosity, L<SUB>IR</SUB>, and various SFR tracers. <BR /> Results: We find a tight linear correlation between log L<SUB>150</SUB> and log L<SUB>IR</SUB> for star-forming galaxies, with a slope of 1.37. The median q<SUP>IR</SUP> value (defined as the logarithm of the L<SUB>IR</SUB> to L<SUB>150</SUB> ratio) and its rms scatter of our main sample are 2.14 and 0.34, respectively. We also find that log L<SUB>150</SUB> correlates tightly with the logarithm of SFR derived from three different tracers, i.e., SFR<SUB>Hα</SUB> based on the Hα line luminosity, SFR<SUB>60</SUB> based on the rest-frame 60 μm luminosity and SFR<SUB>IR</SUB> based on L<SUB>IR</SUB>, with a scatter of 0.3 dex. Our best-fit relations between L<SUB>150</SUB> and these SFR tracers are, log L<SUB>150</SUB> (L<SUB>☉</SUB>) = 1.35(±0.06) × log SFR<SUB>Hα</SUB> (M<SUB>☉</SUB> yr<SUP>-1</SUP>) + 3.20(±0.06), log L<SUB>150</SUB> (L<SUB>☉</SUB>) = 1.31(±0.05) × log SFR<SUB>60</SUB> (M<SUB>☉</SUB> yr<SUP>-1</SUP>) + 3.14(±0.06), and log L<SUB>150</SUB> (L<SUB>☉</SUB>) = 1.37 (±0.05) × log SFR<SUB>IR</SUB> (M<SUB>☉</SUB> yr<SUP>-1</SUP>) + 3.09(±0.05), which show excellent agreement with each other. | URI: | http://hdl.handle.net/20.500.12386/30097 | URL: | http://arxiv.org/abs/1909.04489v1 https://www.aanda.org/articles/aa/full_html/2019/11/aa35913-19/aa35913-19.html |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201935913 | Bibcode ADS: | 2019A&A...631A.109W | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Wang+19.pdf | postprint | 1.27 MB | Adobe PDF | View/Open |
aa35913-19.pdf | Pdf editoriale | 640.46 kB | Adobe PDF | View/Open |
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