Clash: The Enhanced Lensing Efficiency of the Highly Elongated Merging Cluster Macs J0416.1–2403

Zitrin, Adi; Meneghetti, M.; Umetsu, Keiichi; Broadhurst, Tom; Bartelmann, Matthias; Bouwens, Rychard; Bradley, Larry; Carrasco, Mauricio; Coe, Dan; Ford, H. C.; Kelson, Daniel D.; Koekemoer, Anton M.; Medezinski, Elinor; Moustakas, John; Moustakas, Leonidas A.; Nonino, M.; Postman, Marc; Rosati, P.; Seidel, G.; Seitz, S.; Sendra, Irene; Shu, Xinwen; Vega, Jesús; Zheng, Wei

doi:10.1088/2041-8205/762/2/l30

Cited by 187 publications

(220 citation statements)

References 52 publications

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“…In addition, we do not find any convincing counterimage (third image of a triple 'fold' configuration) for systems 14, 15, and 18. Zitrin et al (2013) presented a strong-lensing model with 23 systems identified in this cluster in the new CLASH (Postman et al 2012) data, producing in total 70 images. Due to the very elongated nature of the cluster mass distribution (Fig.…”

Section: Abell 2744mentioning

confidence: 99%

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

Richard¹,

Jauzac²,

Limousin³

et al. 2014

Monthly Notices of the Royal Astronomical Society

218

271

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Citation for published item:i h rdD tF nd t uz D wF nd vimousinD wF nd tulloD iF nd gl¡ ementD fF nd i elingD rF nd unei D tFE F nd etekD rF nd x t r j nD F nd ig miD iF nd vivermoreD F nd fowerD F @PHIRA 9w ss nd m gni( tion m ps for the ru le p e eles ope prontier pields lusters X impli tions for highEredshift studiesF9D wonthly noti es of the oy l estronomi l o ietyFD RRR @IAF ppF PTVEPVWF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTExtending over three Hubble Space Telescope (HST) cycles, the Hubble Frontier Fields (HFF) initiative constitutes the largest commitment ever of HST time to the exploration of the distant Universe via gravitational lensing by massive galaxy clusters. Here, we present models of the mass distribution in the six HFF cluster lenses, derived from a joint strong-and weak-lensing analysis anchored by a total of 88 multiple-image systems identified in existing HST data. The resulting maps of the projected mass distribution and of the gravitational magnification effectively calibrate the HFF clusters as gravitational telescopes. Allowing the computation of search areas in the source plane, these maps are provided to the community to facilitate the exploitation of forthcoming HFF data for quantitative studies of the gravitationally lensed population of background galaxies. Our models of the gravitational magnification afforded by the HFF clusters allow us to quantify the lensing-induced boost in sensitivity over blank-field observations and predict that galaxies at z > 10 and as faint as m(AB) = 32 will be detectable, up to 2 mag fainter than the limit of the Hubble Ultra Deep Field.

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Section: Abell 2744mentioning

confidence: 99%

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

Richard¹,

Jauzac²,

Limousin³

et al. 2014

Monthly Notices of the Royal Astronomical Society

218

271

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“…is a Light Traces Mass (LTM) method, so that both the galaxies and the dark matter follow the light distribution. The method is described in detail by Zitrin et al ( , 2013, and it is inspired by the LTM assumptions outlined by Broadhurst et al (2005). The model consists of two main components.…”

Section: Description Of the Inference Process And Error Estimationmentioning

confidence: 99%

“…Finally, individual galaxies can be assigned with free masses to be optimized by the minimization procedure, to allow more degrees of freedom deviating from the initial imposed LTM. This procedure has been shown to be very effective in locating multiple images in many clusters (e.g., Zitrin et al , 2012bZitrin et al , 2013Zitrin et al , 2015, even without any multiple images initially used as input (Zitrin et al 2012a). Most of the multiple images in MACSJ1149.5+2223 that were found by Zheng et al (2012) were identified with this method.…”

Section: Description Of the Inference Process And Error Estimationmentioning

confidence: 99%

“Refsdal” Meets Popper: Comparing Predictions of the Re-Appearance of the Multiply Imaged Supernova Behind MACSJ1149.5+2223

Treu

Brammer

Diego

et al. 2016

ApJ

Self Cite

113

161

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Supernova "Refsdal," multiply imaged by cluster MACS1149.5+2223, represents a rare opportunity to make a true blind test of model predictions in extragalactic astronomy, on a timescale that is short compared to a human lifetime. In order to take advantage of this event, we produced seven gravitational lens models with five independent methods, based on Hubble Space Telescope (HST) Hubble Frontier Field images, along with extensive spectroscopic follow-up observations by HST, the Very Large and the Keck Telescopes. We compare the model predictions and show that they agree reasonably well with the measured time delays and magnification ratios between the known images, even though these quantities were not used as input. This agreement is encouraging, considering that the models only provide statistical uncertainties, and do not include additional sources of uncertainties such as structure along the line of sight, cosmology, and the mass sheet degeneracy. We then present the model predictions for the other appearances of supernova "Refsdal." A future image will reach its peak in the first half of 2016, while another image appeared between 1994 and 2004. The past image would have been too faint to be detected in existing archival images. The future image should be approximately one-third as bright as the brightest known image (i.e., H 25.7 AB » mag at peak and H 26.7 AB » mag six months before peak), and thus detectable in single-orbit HST images. We will find out soon whether our predictions are correct.

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“…In the NFW model, instead of smoothing the galaxy distribution to obtain the cluster-wide component, the latter is represented with elliptical NFW density profiles, following Navarro, Frenk & White (1997). The best fit solution and accompanying errors are estimated via a long MCMC; see Zitrin et al (2013) for further details.…”

Section: Zitrinmentioning

confidence: 99%

Lens models under the microscope: comparison ofHubble Frontier Fieldcluster magnification maps

Priewe

Williams

Liesenborgs

et al. 2016

Mon. Not. R. Astron. Soc.

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Using the power of gravitational lensing magnification by massive galaxy clusters, the Hubble Frontier Fields provide deep views of six patches of the high redshift Universe. The combination of deep Hubble imaging and exceptional lensing strength has revealed the greatest numbers of multiply-imaged galaxies available to constrain models of cluster mass distributions. However, even with O(100) images per cluster, the uncertainties associated with the reconstructions are not negligible. The goal of this paper is to show the diversity of model magnification predictions. We examine 7 and 9 mass models of Abell 2744 and MACS J0416, respectively, submitted to the Mikulski Archive for Space Telescopes for public distribution in September 2015. The dispersion between model predictions increases from 30% at common low magnifications (µ ∼ 2) to 70% at rare high magnifications (µ ∼ 40). MACS J0416 exhibits smaller dispersions than Abell 2744 for 2 < µ < 10. We show that magnification maps based on different lens inversion techniques typically differ from each other by more than their quoted statistical errors. This suggests that some models underestimate the true uncertainties, which are primarily due to various lensing degeneracies. Though the exact mass sheet degeneracy is broken, its generalized counterpart is not broken at least in Abell 2744. Other, local degeneracies are also present in both clusters. Our comparison of models is complementary to the comparison of reconstructions of known synthetic mass distributions. By focusing on observed clusters, we can identify those that are best constrained, and therefore provide the clearest view of the distant Universe.

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Clash: The Enhanced Lensing Efficiency of the Highly Elongated Merging Cluster Macs J0416.1–2403

Cited by 187 publications

References 52 publications

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

“Refsdal” Meets Popper: Comparing Predictions of the Re-Appearance of the Multiply Imaged Supernova Behind MACSJ1149.5+2223

Lens models under the microscope: comparison ofHubble Frontier Fieldcluster magnification maps

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