Discovery of a Strongly Lensed Massive Quiescent Galaxy at z=2.636: Spatially Resolved Spectroscopy and Indications of Rotation

TL;DR

This paper reports the discovery and detailed analysis of a strongly lensed, massive, quiescent galaxy at z=2.636, revealing its spatially resolved stellar populations, rotation, and implications for galaxy evolution.

Contribution

It presents the first detection of rotation in a quiescent galaxy beyond z~1 and provides insights into angular momentum retention in galaxy progenitors.

Findings

Detected rotation in a high-redshift quiescent galaxy.

Measured a stellar velocity dispersion of 271 km/s.

Found no significant age gradient across the galaxy.

Abstract

We report the discovery of RG1M0150, a massive, recently quenched galaxy at z=2.636 that is multiply imaged by the cluster MACSJ0150.3-1005. We derive a stellar mass of log M_*=11.49+0.10-0.16 and a half-light radius of R_e,maj =1.8+-0.4 kpc. Taking advantage of the lensing magnification, we are able to spatially resolve a remarkably massive yet compact quiescent galaxy at z>2 in ground-based near-infrared spectroscopic observations using Magellan/FIRE and Keck/MOSFIRE. We find no gradient in the strength of the Balmer absorption lines over 0.6 R_e - 1.6 R_e, which are consistent with an age of 760 Myr. Gas emission in [NII] broadly traces the spatial distribution of the stars and is coupled with weak Halpha emission (log [NII]/Halpha = 0.6+-0.2), indicating that OB stars are not the primary ionizing source. The velocity dispersion within the effective radius is sigma_e = 271+-41 km/s. We detect rotation in the stellar absorption lines for the first time beyond z~1. Using a two-integral Jeans model that accounts for observational effects, we measure a dynamical mass of log M_dyn =11.24+-0.14 and V/sigma=0.70+-0.21. This is a high degree of rotation considering the modest observed ellipticity of 0.12+-0.08, but it is consistent with predictions from dissipational merger simulations that produce compact remnants. The mass of RG1M0150 implies that it is likely to become a slowly rotating elliptical. If it is typical, this suggests that the progenitors of massive ellipticals retain significant net angular momentum after quenching which later declines, perhaps through accretion of satellites.