Tully-Fisher relation of late-type galaxies at 0.6 ≤ z ≤ 2.5

¹ Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS UMR 7550, 67000 Strasbourg, France
² University of Strasbourg Institute for Advanced Study, 5 allée du Général Rouvillois, 67083 Strasbourg, France
³ Department of Physics and Astronomy, University of the Western Cape, Cape Town 7535, South Africa
⁴ INFN-Sezione di Trieste, Via Valerio 2, 34127 Trieste, Italy
⁵ IFPU Institute for Fundamental Physics of the Universe, Via Beirut, 2, 34151 Trieste, Italy
⁶ SISSA International School for Advanced Studies, Via Bonomea 265, 34136 Trieste, Italy
⁷ Department of Physics, Indian Institute of Technology, Hyderabad, Telangana 502284, India

Received: 19 November 2023
Accepted: 13 June 2024

Abstract

We present a study of the stellar and baryonic Tully-Fisher relation within the redshift range of 0.6 ≤ z ≤ 2.5, utilizing observations of star-forming galaxies. This dataset comprises of disk-like galaxies spanning a stellar mass range of 8.89 ≤ log(M_star [M_⊙]) ≤ 11.5, a baryonic mass range of 9.0 ≤ log(M_bar [M_⊙]) ≤ 11.5, and a circular velocity range of 1.65 ≤ log(V_c [km/s]) ≤ 2.85. We estimated the stellar masses of these objects using spectral energy distribution fitting techniques, while the gas masses were determined via scaling relations. Circular velocities were directly derived from the rotation curves (RCs), after meticulously correcting for beam smearing and pressure support. Our analysis confirms that our sample adheres to the fundamental mass-size relations of galaxies and reflects the evolution of velocity dispersion in galaxies, in line with previous findings. This reaffirms the reliability of our photometric and kinematic parameters (i.e., M_star and V_c), thereby enabling a comprehensive examination of the Tully-Fisher relation. To attain robust results, we employed a novel orthogonal likelihood fitting technique designed to minimize intrinsic scatter around the best-fit line, as required at high redshifts. For the stellar Tully-Fisher relation, we obtained a slope of α = 3.03 ± 0.25, an offset of β = 3.34 ± 0.53, and an intrinsic scatter of ζ_int = 0.08 dex. Correspondingly, the baryonic Tully-Fisher relation yielded α = 3.21 ± 0.28, β = 3.16 ± 0.61, and ζ_int = 0.09 dex. Our findings indicate a subtle deviation in the stellar and baryonic Tully-Fisher relation with respect to local studies, which is most likely due to the evolutionary processes governing disk formation.