VLT/MUSE observations of SDSS J1029+2623: towards a high-precision strong lensing model

TL;DR

This paper models the mass distribution of galaxy cluster SDSS J1029+2623 using strong lensing data, achieving high positional accuracy and providing insights for cosmological measurements.

Contribution

It presents a detailed strong lensing analysis with new spectroscopic data, identifying multiple images and constructing precise mass models for the cluster.

Findings

Accurate reproduction of multiple image positions within 0.2 arcseconds.

Estimated cluster mass of approximately 2.1 x 10^{14} solar masses within 300 kpc.

Predicted quasar image time delays consistent with observations.

Abstract

We present a strong lensing analysis of the galaxy cluster SDSS J1029+2623 at $z=0.588$, one of the few currently known lens clusters with multiple images of a background ($z=2.1992$) quasar with a measured time delay. We use archival Hubble Space Telescope multi-band imaging and new Multi Unit Spectroscopic Explorer follow-up spectroscopy to build an accurate lens mass model, a crucial step towards future cosmological applications. The spectroscopic data enable the secure identification of 57 cluster members and of two nearby perturbers along the line-of-sight. We estimate the inner kinematics of a sub-set of 20 cluster galaxies to calibrate the scaling relations parametrizing the sub-halo mass component. We also reliably determine the redshift of 4 multiply imaged sources, provide a tentative measurement for one system, and report the discovery of a new four-image system. The final catalog comprises 26 multiple images from 7 background sources, spanning a wide redshift range, from 1.02 to 5.06. We present two parametric lens models, with slightly different cluster mass parametrizations. The observed positions of the multiple images are accurately reproduced within approximately $0''.2$, the three image positions of the quasar within only $\sim0''.1$. We estimate a cluster projected total mass of $M(<300~ {\rm kpc}) \sim 2.1 \times 10^{14}~ M_{\odot}$, with a statistical uncertainty of a few percent. Both models, that include a small galaxy close to one of the quasar images, predict magnitude differences and time delays between the quasar images that are consistent with the observations.