Further support for a trio of mass-to-light deviations in Abell 370: free-form <scp>grale</scp> lens inversion using BUFFALO strong lensing data

Ghosh, Agniva; Williams, Liliya L. R.; Liesenborgs, Jori; Acebrón, Ana; Jauzac, Mathilde; Koekemoer, Anton M.; Mahler, Guillaume; Niemiec, Anna; Steinhardt, Charles L.; Faisst, Andreas L.; Lagattuta, David J.; Natarajan, Priyamvada

doi:10.1093/mnras/stab1196

Cited by 17 publications

(13 citation statements)

References 65 publications

(111 reference statements)

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“…Each run starts with a random seed producing a similar but different map. Constrained by the required computational resources, the number of independent G runs (i.e., 40), is consistent with our previous works (Ghosh et al 2021(Ghosh et al , 2020. In this work, we are using a reconstruction area of 0.62 Mpc × 0.62 Mpc and the smallest resolution cell (projected Plummer sphere) has a radius of ∼ 4 kpc.…”

Section: Results: Mass Reconstructionsupporting

confidence: 61%

“…Comparison between reconstructions that use different lens inversion methods is probably the best way to accomplish that. In Ghosh et al (2021) we carried out such a comparison for the merging cluster Abell 370, based on the data from Hubble Frontier Fields (HFF) and Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO) strong lensing data sets. For this work on A1689 we conclude that on spatial scales of about 100 kpc and above, most, and probably all mass reconstructions agree.…”

Section: Discussionmentioning

confidence: 99%

“…It is ideally suited for reconstructions with numerous multiple images, available with HST data. The fact that the number of its model parameters exceeds the number of data constraints allows a fuller exploration of degenerate mass distributions (Mohammed et al 2014;Sebesta et al 2016Sebesta et al , 2019Meneghetti et al 2017;Williams et al 2018;Ghosh et al 2020Ghosh et al , 2021. We refer the readers to see section 3.1 of Ghosh et al (2020, hereafter, G20), for a concise description of the modus operandi of G .…”

Section: Method: Strong Lens Reconstruction Using Gmentioning

confidence: 99%

“…While simply-parametrized priors are astrophysically motivated, they describe the average properties of galaxies and clusters, and may fail to correctly capture the mass distribution, especially in merging and non fully equilibrium clusters. Because of their high sensitivity to lensed images, free-form methods can detect cluster mass features that elude parametric methods (Ghosh et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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An excursion into the core of the cluster lens Abell 1689

Ghosh¹,

Adams²,

Williams³

et al. 2022

Preprint

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Abell 1689 is a well studied cluster of galaxies and one of the largest gravitational lens systems ever observed. We have obtained a reconstruction of the cluster Abell 1689 using G , a free-form lens inversion method that relies exclusively on the multiple image data. Non-inclusion of any data related to cluster member galaxies ensures an unbiased measure of the mass distribution, which is the most notable feature of this method. We used two different sets of multiply lensed systems from the available strong lensing data -one containing only the secure systems (107 images), and the other containing all available systems, only excluding some very non-secure systems (151 images). Both the reconstructions produced similar mass distributions whose circularly symmetric radial profiles are well fit with the Navarro-Frenk-White (NFW) profile with concentration parameter values, 𝑐 ∼ 6.8. For the very well-constrained central ∼100 kpc region of the cluster we made detailed comparison of the G reconstructed lensing mass and stellar mass retrieved by the Spectral Energy Distribution (SED) fitting software ++. We found an offset in the light peak of the Brightest Cluster Galaxy (BCG) and its associated lensing mass peak, of about 10 kpc. We also found a light-unaccompanied mass peak in this region, whose location agrees with features retrieved by some of the earlier reconstructions using different methodologies. Both the light-unaccompanied mass peak and the BCG offset are consistent with dark matter self-interaction cross-section 𝜎 1cm 2 /g, while the mass peak is in tension with larger cross-sections.

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Section: Results: Mass Reconstructionsupporting

confidence: 61%

Section: Discussionmentioning

confidence: 99%

Section: Method: Strong Lens Reconstruction Using Gmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

An excursion into the core of the cluster lens Abell 1689

Ghosh¹,

Adams²,

Williams³

et al. 2022

Preprint

Self Cite

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show abstract

“…Strong lensing observations permit a very effective determination of the total mass enclosed within the multiple images of a single background source, but the same amount of mass can be obtained with relatively different mass distribution models (e.g. Limousin et al 2016;Ghosh et al 2021). This implies that the parameters that define a model often have a certain degree of degeneracy between them, which corresponds to a possible transfer of mass between the various components.…”

Section: Introductionmentioning

confidence: 99%

Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Granata

Mercurio

Grillo

et al. 2022

A&A

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Aims. From accurate photometric and spectroscopic information, we build the Fundamental Plane (FP) relation for the early-type galaxies of the cluster Abell S1063. We use this relation to develop an improved strong lensing model of the cluster, and we decompose the cluster’s cumulative projected total mass profile into its stellar, hot gas, and dark matter mass components. We compare our results with the predictions of cosmological simulations. Methods. We calibrate the FP using Hubble Frontier Fields photometry and data from the Multi Unit Spectroscopic Explorer on the Very Large Telescope. The FP allows us to determine the velocity dispersions of all 222 cluster members included in the model from their measured structural parameters. As for their truncation radii, we test a proportionality relation with the observed half-light radii. Fixing the mass contribution of the hot gas component from X-ray data, the mass density distributions of the diffuse dark matter haloes are optimised by comparing the observed and model-predicted positions of 55 multiple images of 20 background sources distributed over the redshift range 0.73 − 6.11. We determine the uncertainties on the model parameters with Monte Carlo Markov chains. Results. We find that the most accurate predictions of the positions of the multiple images are obtained when the truncation radii of the member galaxies are approximately 2.3 times their effective radii. Compared to earlier work on the same cluster, our model allows for the inclusion of some scatter on the relation between the total mass and the velocity dispersion of the cluster members. We notice a lower statistical uncertainty on the value of some model parameters. For instance, the main dark matter halo of the cluster has a core radius of 86 ± 2 kpc: the uncertainty on this value decreases by more than 30% with respect to previous work. Taking advantage of a new estimate of the stellar mass of all cluster members from the HST multi-band data, we measure the cumulative two-dimensional mass profiles out to a radius of 350 kpc for all baryonic and dark matter components of the cluster. At the outermost radius of 350 kpc, we obtain a baryon fraction of 0.147 ± 0.002. We study the stellar-to-total mass fraction of the high-mass cluster members in our model, finding good agreement with the observations of wide galaxy surveys and some disagreement with the predictions of halo occupation distribution studies based on N-body simulations. Finally, we compare the features of the sub-haloes as described by our model with those predicted by high-resolution hydrodynamical simulations. We obtain compatible results in terms of the stellar over total mass fraction. On the other hand, we report some discrepancies both in terms of the maximum circular velocity, which is an indication of the halo compactness, and the sub-halo total mass function in the central cluster regions.

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Strong Lensing by Galaxy Clusters

Natarajan,

Williams,

Bradač

et al. 2024

Space Sci Rev

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Galaxy clusters as gravitational lenses play a unique role in astrophysics and cosmology: they permit mapping the dark matter distribution on a range of scales; they reveal the properties of high and intermediate redshift background galaxies that would otherwise be unreachable with telescopes; they constrain the particle nature of dark matter and are a powerful probe of global cosmological parameters, like the Hubble constant. In this review we summarize the current status of cluster lensing observations and the insights they provide, and offer a glimpse into the capabilities that ongoing, and the upcoming next generation of telescopes and surveys will deliver. While many open questions remain, cluster lensing promises to remain at the forefront of discoveries in astrophysics and cosmology.

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Further support for a trio of mass-to-light deviations in Abell 370: free-form grale lens inversion using BUFFALO strong lensing data

Abstract: A version of this article was published in error on 28 April 2021 and has been temporarily removed. The Publisher apologizes for any inconvenience.

Cited by 17 publications

References 65 publications

An excursion into the core of the cluster lens Abell 1689

An excursion into the core of the cluster lens Abell 1689

Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Strong Lensing by Galaxy Clusters

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