Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission

[2204.00831] Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission Skip to main content Search Submit Donate Log in Search arXiv Press Enter to search · Advanced search Astrophysics > Astrophysics of Galaxies arXiv:2204.00831 (astro-ph) [Submitted on 2 Apr 2022 ( v1 ), last revised 15 Aug 2026 (this version, v2)] Title: Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission Authors: Tsutomu T. Takeuchi (1,2), Suchetha Cooray (3,4,5), Luca Cortese (6,7), O. Ivy Wong (8), Barbara Catinella (6,7), Shuntaro A. Yoshida ((1) Nagoya University, (2) Institute of Statistical Mathematics, (3) Stanford University, (4) SLAC National Accelerator Laboratory, (5) Tohoku University, (6) ICRAR, (7) ASTRO 3D, (8) CSIRO Space & Astronomy) View a PDF of the paper titled Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission, by Tsutomu T. Takeuchi (1 and 17 other authors View PDF HTML (experimental) Abstract: We investigate the frequency dependence of the low-frequency infrared (IR)--radio correlation for nearby galaxies drawn from the {\sl Herschel} Reference Survey (HRS), using radio continuum observations from the GaLactic and Extragalactic All-sky MWA (GLEAM) survey obtained with the Murchison Widefield Array (MWA). The GLEAM survey provides densely sampled flux densities across 20 sub-bands spanning 72--231 MHz, allowing detailed characterization of the low-frequency radio spectral energy distribution (SED). We analyze 18 nearby galaxies detected by GLEAM and examine the frequency dependence of the IR--radio correlation coefficient $q_\nu$. Among these galaxies, three sources show Seyfert or LINER signatures and may contain non-negligible AGN contributions to the radio continuum emission. We therefore use the remaining 15 predominantly star-forming galaxies as the primary sample for deriving the main calibration results. For the majority of the sample, the low-frequency radio continuum is well described by a single power-law spectral model from the GLEAM frequency range up to 1.5 GHz, with a median spectral index of $\gamma=-0.63$. The ensemble-averaged $q_\nu$ relation and its intrinsic scatter provide a practical calibration for converting low-frequency radio luminosities into star formation rates (SFRs), while explicitly quantifying the associated systematic uncertainty. Our results indicate that the low-frequency IR--radio correlation remains stable across the MWA bands for nearby star-forming galaxies, supporting the use of low-frequency radio continuum as a dust-unbiased tracer of star formation in the local Universe. These results provide a local benchmark for interpreting low-frequency radio continuum surveys and for future studies of radio-based SFR tracers with next-generation facilities such as the Square Kilometre Array (SKA). Comments: 13 pages, 7 figures, 2 tables, published in PASJ. Adjusted to the published version Subjects: Astrophysics of Galaxies (astro-ph.GA) Cite as: arXiv:2204.00831 [astro-ph.GA] (or arXiv:2204.00831v2 [astro-ph.GA] for this version) https://doi.org/10.48550/arXiv.2204.00831 Focus to learn more arXiv-issued DOI via DataCite Related DOI : https://doi.org/10.1093/pasj/psag096 Focus to learn more DOI(s) linking to related resources Submission history From: Tsutomu Takeuchi T. [ view email ] [v1] Sat, 2 Apr 2022 10:44:47 UTC (8,672 KB) [v2] Sat, 15 Aug 2026 16:37:39 UTC (10,731 KB) Full-text links: Access Paper: View a PDF of the paper titled Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission, by Tsutomu T. 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