Galaxy cluster cores as seen with VLT/MUSE: New strong-lensing analyses of RX J2129.4 + 0009, MS 0451.6 − 0305, and MACS J2129.4 − 0741

Jauzac, Mathilde; Klein, Baptiste; Kneib, Jean-Paul; Richard, Johan; Rexroth, Markus; Schäfer, Christoph; Verdier, Aurélien

doi:10.1093/mnras/stab2270

Cited by 21 publications

(11 citation statements)

References 98 publications

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“…The morphology and the lensing models of MRG-M0138, MRG-M2129, MRG-M0150, MRG-M0454 and MRG-M1341 are studied thoroughly in the literature (Zitrin et al 2014;Umetsu et al 2014;Toft et al 2017;Newman et al 2018;Sharon et al 2020;Zalesky & Ebeling 2020;Jauzac et al 2021;Man et al 2021;Rodney et al 2021). MRG-S1522 has a published lensing model, too (Sharon et al 2020).…”

Section: Constraining Photometric Fluxes and Morphologiesmentioning

confidence: 99%

REQUIEM-2D: A diversity of formation pathways in a sample of spatially-resolved massive quiescent galaxies at z~2

Akhshik¹,

Whitaker²,

Leja³

et al. 2022

Preprint

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REQUIEM-2D (REsolving QUIEscent Magnified galaxies with 2D grism spectroscopy) is comprised of a sample of 8 massive (log M * /M > 10.6) strongly lensed quiescent galaxies at z ∼ 2. REQUIEM-2D combines the natural magnification from strong gravitational lensing with the high spatial-resolution grism spectroscopy of Hubble Space Telescope through a spectrophotometric fit to study spatially resolved stellar populations. We show that quiescent galaxies in the REQUIEM-2D survey have diverse formation histories manifesting as a gradient in stellar ages, including examples of (1) a younger central region supporting outside-in formation, (2) flat age gradients that show evidence for both spatially-uniform early formation or inside-out quenching, and (3) regions at a fixed radial distance having different ages (such asymmetries cannot be recovered when averaging stellar population measurements azimuthally). The typical dust attenuation curve for the REQUIEM-2D galaxies is constrained to be steeper than Calzetti's law in the UV and generally consistent with A V < 1. Combined together and accounting for the different physical radial distances and formation time-scales,

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Section: Constraining Photometric Fluxes and Morphologiesmentioning

confidence: 99%

REQUIEM-2D: A diversity of formation pathways in a sample of spatially-resolved massive quiescent galaxies at z~2

Akhshik¹,

Whitaker²,

Leja³

et al. 2022

Preprint

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“…Integral field observations with the Multi-Unit Spectroscopic Explorer (MUSE) at the VLT have contributed invaluably to strong lensing modeling (see, e.g. Karman et al 2015;Grillo et al 2015Grillo et al , 2016Vanzella et al 2021;Caminha et al 2019;Jauzac et al 2021;Bergamini et al 2021;Richard et al 2021;Granata et al 2022). Thanks to its tremendous efficiency and sensitivity to line emitters, this instrument has expanded the list of confirmed strongly lensed galaxies available for mapping the matter distribution and made unprecedented resolution possible in several galaxy clusters.…”

Section: Introductionmentioning

confidence: 99%

The probability of galaxy-galaxy strong lensing events in hydrodynamical simulations of galaxy clusters

Meneghetti¹,

Ragagnin²,

Borgani³

et al. 2022

Preprint

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Context. Meneghetti et al. (2020) recently reported an excess of galaxy-galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the ΛCDM cosmological model. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in the ΛCDM cosmology. Aims. We quantify the impact of the numerical resolution and AGN feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations. Methods. We repeat the analysis of Meneghetti et al. ( 2020) on cluster-size halos simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Results. We find that improving the mass resolution by a factor of ten and twenty-five, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of the gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor between three and six. However, we notice that such simulations form overly massive subhalos whose contribution to the lensing cross-section would be significant while their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross-sections are subhalos with smaller masses, that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent in simulations. Conclusions. Based on these results, we reaffirm the tension, previously reported in Meneghetti et al. (2020), between observations of GGSL and theoretical expectations in the framework of the ΛCDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty reproducing the stellar mass function and the internal structure of galaxies simultaneously.

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“…2020) combined strong and weak lensing constraints to reconstruct the density field of MS 0451 in a 6 × 6 Mpc 2 area. For the cluster centre, they adopted the best-fit strong lensing mass model from Jauzac et al (2021). For the largescale structures, they measured the weak lensing shear signal of background galaxies from the HST images and reconstructed the projected (2D) mass distribution by using LENSTOOL (Jullo et al 2007;Jullo & Kneib 2009) and the method presented in Jauzac et al (2015).…”

Section: Sample 2 (Photometric Redshifts)mentioning

confidence: 99%

Ram pressure stripping in the z ∼ 0.5 galaxy cluster MS 0451.6-0305

Durret

Degott

Lobo

et al. 2022

A&A

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Context. The pressure exerted by the ambient hot X-ray gas on cluster galaxies can lead to the presence of ram pressure stripped (RPS) galaxies, characterized by asymmetric shapes, and, in some cases, tails of blue stars and/or X-ray gas, with increased star formation. Aims. With the aim of increasing the known sample of RPS galaxies at redshift z ∼ 0.5, notably higher than most RPS samples presently known, we extended our searches for such galaxies to the cluster MS 0451.6-0305. Methods. Our study is based on Hubble Space Telescope (HST) imaging in the F814W band (corresponding to a restframe wavelength of 529 nm), covering a region of about 6 × 6 Mpc2, an eight magnitude ground-based catalogue with photometric redshifts, and a spectroscopic redshift catalogue. We defined as cluster members a spectroscopic redshift sample of 359 galaxies within ±4σv of the mean cluster velocity, and a photometric redshift sample covering the [0.48, 0.61] range. We searched for RPS galaxies in the HST images and tested the error on their classification with a Zooniverse collaboration. We also computed the phase space diagram of RPS candidates in the spectroscopic sample. Finally, we ran the LePhare stellar population synthesis code through the GAZPAR interface to analyze and compare the properties of RPS and non-RPS galaxies. Results. We find 56 and 273 RPS candidates in the spectroscopic and photometric redshift samples, respectively. They are distributed throughout the cluster and tend to avoid high density regions. The phase space diagram gives the percentages of virialized, backsplash, and infall galaxies. RPS galaxy candidates typically show rather high star formation rates, young ages, and relatively low masses. We compare all our results to those previously obtained for the massive merging cluster MACS J0717+3745, at a similar redshift. Conclusions. This study increases by at least 56 objects if we only consider galaxies with spectroscopic redshifts, and probably much more if galaxies with photometric redshifts are taken into account. This study increases the number of RPS candidates at redshift z > 0.5, and confirms that they host, on average, younger stellar populations and strongly form stars when compared with non-RPS counterparts. The fact that RPS candidates with spectroscopic and with photometric redshifts have comparable properties shows that large samples of such objects could be gathered based on multi-band photometry only, a promising result in view of the very large imaging surveys planned in the coming years (DES, Euclid, LSST, etc.).

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Galaxy cluster cores as seen with VLT/MUSE: New strong-lensing analyses of RX J2129.4 + 0009, MS 0451.6 − 0305, and MACS J2129.4 − 0741

Cited by 21 publications

References 98 publications

REQUIEM-2D: A diversity of formation pathways in a sample of spatially-resolved massive quiescent galaxies at z~2

REQUIEM-2D: A diversity of formation pathways in a sample of spatially-resolved massive quiescent galaxies at z~2

The probability of galaxy-galaxy strong lensing events in hydrodynamical simulations of galaxy clusters

Ram pressure stripping in the z ∼ 0.5 galaxy cluster MS 0451.6-0305

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