Cookies

We use cookies to ensure that we give you the best experience on our website. You can change your cookie settings at any time. Otherwise, we'll assume you're OK to continue.

Durham University

Department of Physics

Staff profile

Publication details for Prof Richard Bower

Tiley, A. L. , Bureau, M. Cortese, L. Harrison, C. M. , Johnson, H. L. , Stott, J. P. Swinbank, A. M. , Smail, I. , Sobral, D. Bunker, A. J. Glazebrook, K. Bower, R. G. , Obreschkow D. Bryant, J. J. Jarvis, M. J. Bland-Hawthorn, J. Magdis, G. Medling, A. M. Sweet, S. M. Tonini, C. Turner, O. J. Sharples, R. M. , Croom, S. M. Goodwin, M., Konstantopoulos, I. S., Lorente, N. P. F. Lawrence, J. S. Mould, J., Owers, M. S. & 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): 2166–2188.

Author(s) from Durham

Abstract

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.