DEVILS/MIGHTEE/GAMA/DINGO: the impact of SFR time-scales on the SFR-radio luminosity correlation

Author:

Cook Robin H W1ORCID,Davies Luke J M1ORCID,Rhee Jonghwan12ORCID,Hale Catherine L3ORCID,Bellstedt Sabine1ORCID,Thorne Jessica E1ORCID,Delvecchio Ivan4ORCID,Collier Jordan D567,Dodson Richard1ORCID,Driver Simon P1ORCID,Holwerda Benne W8ORCID,Jarvis Matt J39ORCID,Knowles Kenda10ORCID,Lagos Claudia12ORCID,Maddox Natasha11ORCID,Meyer Martin1,Robotham Aaron S G1ORCID,Roychowdhury Sambit12,Rozgonyi Kristof12ORCID,Seymour Nicholas13ORCID,Siudek Malgorzata1415ORCID,Whiting Matthew7,Whittam Imogen39ORCID

Affiliation:

1. ICRAR, The University of Western Australia , 35 Stirling Highway, Crawley, WA 6009 , Australia

2. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia

3. Oxford Astrophysics , Denys Wilkinson Building, University of Oxford, Keble Rd, Oxford OX1 3RH , UK

4. INAF – Osservatorio Astronomico di Brera , via Brera 28, I-20121, Milano, Italy & via Bianchi 46, I-23807 Merate , Italy

5. The Inter-University Institute for Data Intensive Astronomy (IDIA), Department of Astronomy , University of Cape Town, Private Bag X3, Rondebosch 7701 , South Africa

6. School of Science, Western Sydney University , Locked Bag 1797, Penrith NSW 2751 , Australia

7. CSIRO, Space and Astronomy , PO Box 1130, Bentley, WA 6102 , Australia

8. University of Louisville, Department of Physics and Astronomy , 102 Natural Science Building, Louisville, KY 40292 USA

9. Department of Physics and Astronomy, University of the Western Cape , Robert Sobukwe Road, Bellville 7535 , South Africa

10. Centre for Radio Astronomy Techniques and Technologies, Department of Physics and Electronics , Rhodes University, P.O. Box 94, Makhanda 6140 , South Africa

11. School of Physics, H.H. Wills Physics Laboratory , Tyndall Avenue, University of Bristol, Bristol BS8 1TL , UK

12. University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität , Scheinerstr. 1, D-81679 München , Germany

13. International Centre for Radio Astronomy Research, Curtin University , Bentley, WA 6102 , Australia

14. Institute of Space Sciences (ICE, CSIC) , Campus UAB, Carrerde Can Magrans, s/n, E-08193 Barcelona , Spain

15. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , E-08193 Bellaterra (Barcelona) , Spain

Abstract

ABSTRACT The tight relationship between infrared luminosity (LTIR) and 1.4 GHz radio continuum luminosity ($L_\mathrm{1.4\, GHz}$) has proven useful for understanding star formation free from dust obscuration. Infrared emission in star-forming galaxies typically arises from recently formed, dust-enshrouded stars, whereas radio synchrotron emission is expected from subsequent supernovae. By leveraging the wealth of ancillary far-ultraviolet – far-infrared photometry from the Deep Extragalactic VIsible Legacy Survey and Galaxy and Mass Assembly surveys, combined with 1.4 GHz observations from the Meer Karoo Array Telescope International GHz Tiered Extragalactic Exploration survey and Deep Investigation of Neutral Gas Origin projects, we investigate the impact of time-scale differences between far-ultraviolet – far-infrared and radio-derived star formation rate (SFR) tracers. We examine how the spectral energy distribution (SED)-derived star formation histories (SFHs) of galaxies can be used to explain discrepancies in these SFR tracers, which are sensitive to different time-scales. Galaxies exhibiting an increasing SFH have systematically higher LTIR and SED-derived SFRs than predicted from their 1.4 GHz radio luminosity. This indicates that insufficient time has passed for subsequent supernovae-driven radio emission to accumulate. We show that backtracking the SFR(t) of galaxies along their SED-derived SFHs to a time several hundred megayears prior to their observed epoch will both linearize the SFR–$L_\mathrm{1.4\, GHz}$ relation and reduce the overall scatter. The minimum scatter in the SFR(t)–$L_\mathrm{1.4\, GHz}$ is reached at 200 – 300 Myr prior, consistent with theoretical predictions for the time-scales required to disperse the cosmic ray electrons responsible for the synchrotron emission.

Funder

Hintze Family Charitable Foundation

STFC

UKRI

Leverhulme Trust

Publisher

Oxford University Press (OUP)

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