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KROSS-SAMI : a direct IFS comparison of the Tully-Fisher relation across 8 Gyr Since z ≈ 1.

Tiley, A. L. and Bureau, M. and Cortese, L. and Harrison, C. M. and Johnson, H. L. and Stott, J. P. and Swinbank, A. M. and Smail, I. and Sobral, D. and Bunker, A. J. and Glazebrook, K. and Bower, R. G. and Obreschkow, D. and Bryant, J. J. and Jarvis, M. J. and Bland-Hawthorn, J. and Magdis, G. and Medling, A. M. and Sweet, S. M. and Tonini, C. and Turner, O. J. and Sharples, R. M. and Croom, S. M. and Goodwin, M. and Konstantopoulos, I. S. and Lorente, N. P. F. and Lawrence, J. S. and Mould, J. and Owers, M. S. and Richards, S. N. (2019) 'KROSS-SAMI : a direct IFS comparison of the Tully-Fisher relation across 8 Gyr Since z ≈ 1.', Monthly notices of the Royal Astronomical Society., 482 (2). pp. 2166-2188.


We construct Tully–Fisher relations (TFRs), from large samples of galaxies with spatially resolved H α emission maps from the K-band Multi-Object Spectrograph (KMOS) Redshift One Spectroscopic Survey (KROSS) at z ≈ 1. We compare these to data from the Sydney-Australian-Astronomical-Observatory Multi-object Integral-Field Spectrograph (SAMI) Galaxy Survey at z ≈ 0. We stringently match the data quality of the latter to the former, and apply identical analysis methods and sub-sample selection criteria to both to conduct a direct comparison of the absolute K-band magnitude and stellar mass TFRs at z ≈ 1 and 0. We find that matching the quality of the SAMI data to that of KROSS results in TFRs that differ significantly in slope, zero-point, and (sometimes) scatter in comparison to the corresponding original SAMI relations. These differences are in every case as large as or larger than the differences between the KROSS z ≈ 1 and matched SAMI z ≈ 0 relations. Accounting for these differences, we compare the TFRs at z ≈ 1 and 0. For disc-like, star-forming galaxies we find no significant difference in the TFR zero-points between the two epochs. This suggests the growth of stellar mass and dark matter in these types of galaxies is intimately linked over this ≈8 Gyr period.

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Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:15 October 2018
Date deposited:21 November 2018
Date of first online publication:17 October 2018
Date first made open access:21 November 2018

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