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Resolving a dusty, star-forming SHiZELS galaxy at z = 2.2 with HST, ALMA, and SINFONI on kiloparsec scales

Cochrane, R.K. and Best, P.N. and Smail, I. and Ibar, E. and Cheng, C. and Swinbank, A.M. and Molina, J. and Sobral, D. and Dudzevi\vci\=ut\.e, U. (2021) 'Resolving a dusty, star-forming SHiZELS galaxy at z = 2.2 with HST, ALMA, and SINFONI on kiloparsec scales.', Monthly Notices of the Royal Astronomical Society, 503 (2). pp. 2622-2638.


We present ∼0.15 arcsec spatial resolution imaging of SHiZELS-14, a massive (⁠M∗∼1011M⊙⁠), dusty, star-forming galaxy at z = 2.24. Our rest-frame ∼1kpc-scale, matched-resolution data comprise four different widely used tracers of star formation: the Hα emission line (from SINFONI/VLT), rest-frame UV continuum (from HST F606W imaging), the rest-frame far-infrared (from ALMA), and the radio continuum (from JVLA). Although originally identified by its modest Hα emission line flux, SHiZELS-14 appears to be a vigorously star-forming (⁠SFR∼1000M⊙yr−1⁠) example of a submillimetre galaxy, probably undergoing a merger. SHiZELS-14 displays a compact, dusty central starburst, as well as extended emission in Hα and the rest-frame optical and FIR. The UV emission is spatially offset from the peak of the dust continuum emission, and appears to trace holes in the dust distribution. We find that the dust attenuation varies across the spatial extent of the galaxy, reaching a peak of at least AH α ∼ 5 in the most dusty regions, although the extinction in the central starburst is likely to be much higher. Global star-formation rates inferred using standard calibrations for the different tracers vary from ∼10−1000M⊙yr−1⁠, and are particularly discrepant in the galaxy’s dusty centre. This galaxy highlights the biased view of the evolution of star-forming galaxies provided by shorter wavelength data.

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Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:10 February 2021
Date deposited:25 August 2021
Date of first online publication:19 February 2021
Date first made open access:25 August 2021

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