The Fundamental Plane of cluster spheroidal galaxies at z$\sim 1.3$. Evidence for mass-dependent evolution

Abstract

We present spectroscopic observations obtained at the {\it Large Binocular Telescope} in the field of the cluster XLSSJ0223-0436 at $z=1.22$. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at $z=1.27$ (8 galaxies) and XMMJ2235-2557 at $z=1.39$ (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at $z\sim 1.3$ is offset and { rotated ($\sim 3\sigma$)} with respect to the local FP. The offset corresponds to a mean evolution $\Delta$\rm{log}(M${}_{dyn}$/L${}_B$)=(-0.5$\pm$0.1)$z$. High-redshift galaxies follow a steeper mass-dependent M${}_{dyn}$/L${}_B$-M${}_{dyn}$ relation than local ones. Assuming $\Delta$ log$(M_{dyn}/L_B)$=$\Delta$ log$(M^{\ast }/L_B)$, higher-mass galaxies (log(M${}_{dyn}$/M${}_{\odot }$)$\ge$11.5) have a higher-formation redshift ($z_f\ge$6.5) than lower-mass ones ($z_f\le$2 for log(M${}_{dyn}$/M${}_{\odot }$$\le$10)), with a median $z_f\simeq 2.5$ for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M${}_{dyn}$/M${}^{\ast }$ varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M${}^{\ast }/L_B$) accounts for the observed evolution of M${}_{dyn}/L_B$ for M${}_{dyn}$$>10^{11}$ M${}_{\odot }$ galaxies, while accounts for $\sim$85\% of the evolution at M${}_{dyn}$$<10^{11}$ M${}_{\odot }$. We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population account for the observed discrepancy at masses $<10^{11}$ M${}_{\odot }$. [Abridged]

19 pages (including appendices), 16 figures, 5 tables, accepted for publication in MNRAS

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