The Frontier Fields lens modelling comparison project

Meneghetti, M.; Natarajan, Priyamvada; Coe, Dan; Contini, Elisa; Lucia, G. De; Giocoli, Carlo; Acebrón, Ana; Borgani, S.; Bradač, Maruša; Diego, J. M.; Hoag, Austin; Ishigaki, Masafumi; Johnson, Traci L.; Jullo, Eric; Kawamata, Ryota; Lam, Daniel; Limousin, M.; Liesenborgs, Jori; Oguri, Masamune; Sebesta, Kevin; Sharon, Keren; Williams, Liliya L. R.; Zitrin, Adi

doi:10.1093/mnras/stx2064

Cited by 214 publications

(264 citation statements)

References 167 publications

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“…Whereas the recovered density using fitnessTD,2009 only lies within 10% of κR in a relatively small region, the correspondence for the newly proposed fitness measure clearly covers a much larger region, with main differences where the mass peaks in the true model are located. This MSD effect can also be seen in the right panel, where the magnification is shown for a source at a redshift of z = 9, similar to figs 21 and 22 of Meneghetti et al (2017). Note that this redshift dependence causes the actual magnification of the images, which correspond to other redshifts, to differ.…”

Section: Time Delayssupporting

confidence: 64%

“…In the third scenario, (C), a situation like one that could be encountered in practice is considered: similar to the weak lensing information that was made available for the mock clusters Ares and Hera (Meneghetti et al 2017), 12,000 random source ellipticities at random redshifts were transformed by the real gravitational lens model, the result of which is shown in the third panel of the figure. These ellipticities were then distributed over a number of redshift bins, chosen to contain the same interval 0.1 in D ds /Ds space.…”

Section: Simulated Lens and Reconstructionsmentioning

confidence: 99%

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Extended lens reconstructions with grale: exploiting time-domain, substructural, and weak lensing information

Liesenborgs

Williams

Wagner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The information about the mass density of galaxy clusters provided by the gravitational lens effect has inspired many inversion techniques. In this article, updates to the previously introduced method in Grale are described, and explored in a number of examples. The first looks into a different way of incorporating time delay information, not requiring the unknown source position. It is found that this avoids a possible bias that leads to "over-focusing" the images, i.e. providing source position estimates that lie in a considerably smaller region than the true positions. The second is inspired by previous reconstructions of the cluster of galaxies MACS J1149.6+2223, where a multiply-imaged background galaxy contained a supernova, SN Refsdal, of which four additional images were produced by the presence of a smaller cluster galaxy. The inversion for the cluster as a whole, was not able to recover sufficient detail interior to this quad. We show how constraints on such different scales, from the entire cluster to a single member galaxy, can now be used, allowing such small scale substructures to be resolved. Finally, the addition of weak lensing information to this method is investigated. While this clearly helps recover the environment around the strong lensing region, the mass sheet degeneracy may make a full strong and weak inversion difficult, depending on the quality of the ellipticity information at hand. We encounter ring-like structure at the boundary of the two regimes, argued to be the result of combining strong and weak lensing constraints, possibly affected by degeneracies.

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Section: Time Delayssupporting

confidence: 64%

Section: Simulated Lens and Reconstructionsmentioning

confidence: 99%

Extended lens reconstructions with grale: exploiting time-domain, substructural, and weak lensing information

Liesenborgs

Williams

Wagner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The lens inversion method used in this paper is based on the reconstruction code Grale. The publicly available Grale software implements a flexible, free-form, adaptive grid lens inversion method, based on a genetic algorithm (Liesenborgs et al 2006(Liesenborgs et al , 2007Mohammed et al 2014;Meneghetti et al 2017). A Grale run starts with an initial coarse uniform grid in the lens plane populated by a basis set, such as projected Plummer density spheres (See Appendix B).…”

Section: Methodsmentioning

confidence: 99%

Free-form grale lens inversion of galaxy clusters with up to 1000 multiple images

Ghosh

Williams

Liesenborgs

2020

Monthly Notices of the Royal Astronomical Society

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In the near future, ultra deep observations of galaxy clusters with HST or JWST will uncover 300 − 1000 lensed multiple images, increasing the current count per cluster by up to an order of magnitude. This will further refine our view of clusters, leading to a more accurate and precise mapping of the total and dark matter distribution in clusters, and enabling a better understanding of background galaxy population and their luminosity functions. However, to effectively use that many images as input to lens inversion will require a re-evaluation of, and possibly upgrades to the existing methods. In this paper we scrutinize the performance of the free-form lens inversion method Grale in the regime of 150 − 1000 input images, using synthetic massive galaxy clusters. Our results show that with an increasing number of input images, Grale produces improved reconstructed mass distributions, with the fraction of the lens plane recovered at better than 10% accuracy increasing from 40 − 50% for ∼150 images to 65% for ∼ 1000 images. The reconstructed time delays imply a more precise measurement of H 0 , with 1% bias. While the fidelity of the reconstruction improves with the increasing number of multiple images used as model constraints, ∼ 150 to ∼1000, the lens plane rms deteriorates from ∼ 0.11 to ∼ 0.28 . Since lens plane rms is not necessarily the best indicator of the quality of the mass reconstructions, looking for an alternative indicator is warranted.

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“…Similarly, Donahue et al (2016) examined the morphological properties of all 25 CLASH clusters with Chandra X-ray data (Donahue et al 2014) and compared them with those inferred from Bolocam SZE maps of the intracluster gas (Sayers et al 2013;Czakon et al 2015) and those from mass maps based on HST strong and weak lensing (hereafter HST-GL; Zitrin et al 2015). The lensing maps used are based on parametric modeling assuming that light traces mass for the galaxy-scale mass components (see Meneghetti et al 2017). They found a strong correlation between PAs as measured from the X-ray, SZE, and HST-GL maps inside a consistent metric aperture of radius 350 h kpc 1 -(∼0.2r vir for these clusters).…”

Section: Cluster Misalignment Statisticsmentioning

confidence: 99%

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Umetsu

Sereno

Tam

et al. 2018

ApJ

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We reconstruct the two-dimensional (2D) matter distributions in 20 high-mass galaxy clusters selected from the CLASH survey by using the new approach of performing a joint weak gravitational lensing analysis of 2D shear and azimuthally averaged magnification measurements. This combination allows for a complete analysis of the field, effectively breaking the mass-sheet degeneracy. In a Bayesian framework, we simultaneously constrain the mass profile and morphology of each individual cluster, assuming an elliptical Navarro-Frenk-White halo characterized by the mass, concentration, projected axis ratio, and position angle (PA) of the projected major axis. We find that spherical mass estimates of the clusters from azimuthally averaged weak-lensing measurements in previous work are in excellent agreement with our results from a full 2D analysis. Combining all 20 clusters in our sample, we detect the elliptical shape of weak-lensing halos at the 5σ significance level within a scale of 2 h Mpc 1 -. The median projected axis ratio is 0.67±0.07 at a virial mass of M M 15.2 2.8 10 vir 14 = ´ ( ) , which is in agreement with theoretical predictions from recent numerical simulations of the standard collisionless cold dark matter model. We also study misalignment statistics of the brightest cluster galaxy, X-ray, thermal Sunyaev-Zel'dovich effect, and strong-lensing morphologies with respect to the weak-lensing signal. Among the three baryonic tracers studied here, we find that the X-ray morphology is best aligned with the weak-lensing mass distribution, with a median misalignment angle of PA 21We also conduct a stacked quadrupole shear analysis of the 20 clusters assuming that the X-ray major axis is aligned with that of the projected mass distribution. This yields a consistent axis ratio of 0.67±0.10, suggesting again a tight alignment between the intracluster gas and dark matter.

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The Frontier Fields lens modelling comparison project

Cited by 214 publications

References 167 publications

Extended lens reconstructions with grale: exploiting time-domain, substructural, and weak lensing information

Extended lens reconstructions with grale: exploiting time-domain, substructural, and weak lensing information

Free-form grale lens inversion of galaxy clusters with up to 1000 multiple images

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

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