Clash: New Multiple Images Constraining the Inner Mass Profile of Macs J1206.2–0847

Zitrin, Adi; Rosati, P.; Nonino, M.; Grillo, C.; Postman, Marc; Coe, Dan; Seitz, S.; Eichner, T.; Broadhurst, Tom; Jouvel, S.; Balestra, I.; Mercurio, A.; Scodeggio, M.; Benı́tez, N.; Bradley, Larry; Ford, H. C.; Host, Ö.; Jiménez-Teja, Y.; Koekemoer, Anton M.; Zheng, Wei; Bartelmann, Matthias; Bouwens, Rychard; Czoske, O.; Donahue, M.; Graur, Or; Graves, Genevieve J.; Infante, L.; Jha, Saurabh W.; Kelson, Daniel D.; Lahav, O.; Lazkoz, Ruth; Lemze, Doron; Lombardi, Marco; Maoz, Dan; McCully, C.; Medezinski, Elinor; Melchior, P.; Meneghetti, M.; Merten, Julian; Molino, A.; Moustakas, Leonidas A.; Ogaz, Sara; Patel, Brandon; Regoes, E.; Riess, Adam G.; Rodney, Steven A.; Umetsu, Keiichi; Wel, Arjen van der

doi:10.1088/0004-637x/749/2/97

Cited by 66 publications

(91 citation statements)

References 44 publications

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“…For the χ 2 we used a positional error of σ pos = 1. 4, which was found to be a reasonable value accounting for large-scale structure and matter along the line of sight (see Zitrin et al 2012b and references therein). The multiple-image input comprises 35 constraints, where the number of degrees of freedom (dof) is 26 and 22 for the eGaussian and eNFW models, respectively, yielding, correspondingly, χ 2 /dof = 2.18 and χ 2 /dof = 1.35.…”

Section: Results and Comparison Of The Two Modelsmentioning

confidence: 81%

“…Indeed, various clusters around z ∼ 0.5 show prominent lensing features (giant arcs and many multiple images; Zitrin et al 2012aZitrin et al , 2012b. Interestingly, the largest gravitational lens, MACS J0717.5+3745 (z = 0.55; Zitrin et al 2009a), is formed by several merging clumps possibly at the tip of a filament (Limousin et al 2012;Jauzac et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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

Zitrin

Meneghetti

Umetsu

et al. 2012

ApJ

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190

205

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We perform a strong lensing analysis of the merging galaxy cluster MACS J0416.1−2403 (M0416; z = 0.42) in recent CLASH/HST observations. We identify 70 new multiple images and candidates of 23 background sources in the range 0.7 z phot 6.14 including two probable high-redshift dropouts, revealing a highly elongated lens with axis ratio 5:1, and a major axis of ∼100 (z s ∼ 2). Compared to other well-studied clusters, M0416 shows an enhanced lensing efficiency. Although the critical area is not particularly large ( 0.6 ; z s ∼ 2), the number of multiple images, per critical area, is anomalously high. We calculate that the observed elongation boosts the number of multiple images, per critical area, by a factor of ∼2.5×, due to the increased ratio of the caustic area relative to the critical area. Additionally, we find that the observed separation between the two main mass components enlarges the critical area by a factor of ∼2. These geometrical effects can account for the high number (density) of multiple images observed. We find in numerical simulations that only ∼4% of the clusters (with M vir 6 × 10 14 h −1 M ) exhibit critical curves as elongated as in M0416.

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Section: Results and Comparison Of The Two Modelsmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

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

Zitrin

Meneghetti

Umetsu

et al. 2012

ApJ

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190

205

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“…Kneib et al 1996) to constrain the detailed mass distribution in cluster cores as well as to probe the mass distributions of samples of X-ray-selected clusters out to the virial radius (e.g. Smith et al 2005;Ebeling et al 2009;Richard et al 2010b;Zitrin et al 2012). Importantly, lensing also enables the study of distant background galaxies that would be unobservable without the magnification provided by the cluster lens (e.g.…”

Section: G R Av I Tat I O Na L L E N S I N Gmentioning

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

223

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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“…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

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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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Clash: New Multiple Images Constraining the Inner Mass Profile of Macs J1206.2–0847

Cited by 66 publications

References 44 publications

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

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

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

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