• DOI:10.1051/0004-6361/202039564
• Corpus ID: 222090039

A new high-precision strong lensing model of the galaxy cluster MACS J0416.1−2403

@article{Bergamini2020ANH,
  title={A new high-precision strong lensing model of the galaxy cluster MACS J0416.1−2403},
  author={Pietro Bergamini and Piero Rosati and Eros Vanzella and Gabriel Bartosch Caminha and Claudio Grillo and Amata Mercurio and Massimo Meneghetti and Giuseppe Angora and Francesco Calura and Mario Nonino and Paolo Tozzi},
  journal={arXiv: Astrophysics of Galaxies},
  year={2020}
}

• P. Bergamini, P. Rosati, +8 authors P. Tozzi
• Published 30 September 2020
• Physics
• arXiv: Astrophysics of Galaxies

We present a new high-precision parametric strong lensing model of the galaxy cluster MACS J0416.1-2403, at z=0.396, which takes advantage of the MUSE Deep Lensed Field (MDLF, Vanzella et al. 2020b), with 17.1h integration in the North-East region of the cluster, and Hubble Frontier Fields data. We spectroscopically identify 182 multiple images from 48 background sources at 0.9<z<6.2, and 171 cluster member galaxies. Several multiple images are associated to individual clumps in multiply lensed resolved sources. By defining a new metric, which is sensitive to the gradients of the deflection field, we show that we can accurately reproduce the positions of these star-forming knots despite their vicinity to the model critical lines. The high signal-to-noise spectra of the MDLF enables the measurement of the internal velocity dispersion of 64 cluster galaxies, down to m(F160W)=22. This allows us to independently estimate the contribution of the subhalo mass component of the lens model from the measured Faber-Jackson scaling relation. Our best reference model, which represents a significant step forward compared to our previous analyses, is selected from a comparative study of different mass parametrizations. The r.m.s. displacement between the observed and model-predicted image positions is only 0.40", 33% smaller than in all previous models. The mass model appears to be particularly well constrained in the MDLF region. We characterize the robustness of the magnification map at varying distances from the model critical lines and the total projected mass profile of the cluster.