Evolution of galaxy scaling relations in clusters at 0.5 < z < 1.5^⋆

¹ Department of Astrophysics, University of Vienna, 1180 Vienna, Austria
e-mail: jm.perez@univie.ac.at
² Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, Tenerife, Spain
³ Universidad de La Laguna, Dpto. Astrofísica, 38206 La Laguna, Tenerife, Spain
⁴ Departamento de Física Teórica and CIAFF, Universidad Autónoma de Madrid, 28049 Madrid, Spain

Received: 4 August 2019
Accepted: 23 July 2020

Abstract

Aims. We present new gas kinematic observations with the OSIRIS instrument at the GTC for galaxies in the Cl1604 cluster system at z ∼ 0.9. These observations together with a collection of other cluster samples at different epochs analyzed by our group are used to study the evolution of the Tully-Fisher, velocity-size, and specific angular momentum-stellar mass relations in dense environments over cosmic time.

Methods. We used 2D and 3D spectroscopy to analyze the kinematics of our cluster galaxies and extract their maximum rotation velocities (V_max), which were used as the common parameter in all scaling relations under scrutiny. We determined the structural parameters of our objects by fitting surface brightness profiles to the images of our objects, while stellar-mass values were computed by fitting the spectral energy distribution by making use of extensive archival optical to near-IR photometry. Our methods were consistently applied to all our cluster samples. This makes them ideal for an evolutionary comparison.

Results. Up to redshift one, our cluster samples show evolutionary trends compatible with previous observational results in the field and in accordance with semianalytical models and hydrodynamical simulations concerning the Tully-Fisher and velocity-size relations. However, we find a drop of a factor ∼3 in disk sizes and an average B-band luminosity enhancement ⟨ΔM_B⟩∼2 mag by z ∼ 1.5. We discuss the role that different cluster-specific interactions may play in producing this observational result. In addition, we find that our intermediate-to-high redshift cluster galaxies follow parallel sequences with respect to the local specific angular momentum to stellar mass relation, although they display lower specific angular momentum values than field samples at similar redshifts. This may be explained by the stronger interacting nature of dense environments in comparison with the field.