A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

XV. The Hα luminosity function of the Virgo cluster^⋆

¹ Aix-Marseille Univ., CNRS, CNES, LAM, Marseille, France
e-mail: alessandro.boselli@lam.fr
² Università di Milano-Bicocca, Piazza della Scienza 3, 20100 Milano, Italy
³ INAF – Osservatorio Astronomico di Brera, Via Brera 28, 20121 Milano, Italy
⁴ National Research Council of Canada, Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
⁵ AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, Observatoire de Paris, PSL University, 91191 Gif-sur-Yvette Cedex, France
⁶ Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astropysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
⁷ Waterloo Centre for Astrophysics, University of Waterloo, 200 University Ave. W., Waterloo, Ontario N2L3G1, Canada
⁸ Centro de Astronomiá (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, 1270398 Antofagasta, Chile
⁹ Department of Astrophysics, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
¹⁰ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
¹¹ STFC UK Astronomy Technology Centre, The Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
¹² Department of Physics & Astronomy, University of Alabama in Huntsville, 3001 Sparkman Drive, Huntsville, AL 35899, USA

Received: 27 March 2023
Accepted: 16 May 2023

Abstract

We use a complete set of deep narrow-band imaging data for 384 galaxies gathered during the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) to derive the first Hα luminosity function of the Virgo cluster within its virial radius. The data, which are sensitive to the emission of a single O-early B ionising star, allow us to cover the whole dynamic range of the Hα luminosity function (10³⁶ ≤ L(Hα)≤10⁴² erg s⁻¹). After they are corrected for [NII] contamination and dust attenuation, the data are used to derive the star formation rate function in the range 10⁻⁴ ≲ SFR ≲ 10 M_⊙ yr⁻¹. These luminosity functions are derived for gas-rich and gas-poor systems and for objects belonging to the different substructures of the Virgo cluster. They are then compared to those derived at other frequencies or using different tracers of star formation in Virgo, in other nearby and high-z clusters, in the field, and finally to those predicted by the IllustrisTNG cosmological hydrodynamical simulations (TNG50 and TNG100). The Hα luminosity function of the Virgo cluster is fairly flat (α = −1.07 when fitted with a Schechter function) in the range 10^38.5 ≲ L(Hα)≲10^40.5 erg s⁻¹, and it abruptly decreases at lower luminosities. When compared to those derived for other nearby clusters and for the field, the slope and the characteristic luminosity of the Schechter function change as a function of the dynamical mass of the system, of the temperature of the X-rays gas, and of the dynamical pressure exerted on the interstellar medium of galaxies moving at high velocity within the intracluster medium. All these trends can be explained in a scenario in which the activity of star formation of galaxies is reduced in massive clusters due to their hydrodynamical interaction with the surrounding medium, suggesting once again that ram-pressure stripping is the dominant mechanism affecting galaxy evolution in local clusters of dynamical mass M_cluster ≳ 10¹⁴ M_⊙. The comparison with the IllustrisTNG cosmological hydrodynamical simulations shows a more pronounced decrease at the faint end of the distribution. If the Virgo cluster is representative of typical nearby clusters of similar mass, this difference suggests that the stripping process in simulated galaxies in these environments is more efficient than observed.