A free-form mass model of the Hubble Frontier Fields cluster AS1063 (RXC J2248.7−4431) with over one hundred constraints

Diego, J. M.; Broadhurst, T.; Wong, Jess; Silk, Joseph; Lim, Jeremy; Zheng, Wei; Lam, Daniel; Ford, H. C.

doi:10.1093/mnras/stw865

Cited by 50 publications

(47 citation statements)

References 54 publications

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“…The reliability of our method has been demonstrated with both simulated data (Sendra et al 2014) and observations of the lensing standard Abell 1689, (Diego et al 2015a) and our subsequent HFF work (Lam et al 2014;Diego et al 2015bDiego et al , 2015cDiego et al , 2016aDiego et al , 2016b. In particular we have stressed the ability of our models to account for the independent information contained in the relative fluxes of multiply lensed sources.…”

Section: Introductionmentioning

confidence: 73%

“…These deepest observations with the HST and Planck satellites may together be consistent in indicating a later and more sudden onset of galaxy formation than widely anticipated. Empirically, it appears that consistency is seen between the downwardly revised "instantaneous redshift" of reionization, z;8, when most of the cosmologically distributed hydrogen had become reionized (Planck Collaboration et al 2016) with the tentative claim of an accelerated decline in the integrated star formation rate at z>8 (Oesch et al 2010(Oesch et al , 2013 and supported by a absence of any galaxy detected beyond ;11.0 (Oesch et al 2016), despite increasingly deep Hubble Frontier Field imaging (Zheng et al 2012;Lam et al 2014;Diego et al 2015bDiego et al , 2015cDiego et al , 2016aDiego et al , 2016b. Late reionization is also supported by a marked decline above z7 in the incidence of Lyα emission from high-redshift galaxy spectroscopy, which can be reproduced by photoionizaton models with a much higher neutral fraction than anticipated (Choudhury et al 2015;Mesinger et al 2015), indicating later galaxy and QSO formation (Madau & Haardt 2015).…”

Section: Discussionmentioning

confidence: 99%

“…We have applied this method to all of the HFF fields and some CLASH clusters, taking advantage of the increasing numbers of multiply lensed images and their photometric and spectroscopic redshifts as the input data (Lam et al 2014;Diego et al 2015bDiego et al , 2015cDiego et al , 2016aDiego et al , 2016b. We have made these models available to the community so that they may be compared to those derived by other teams.…”

Section: Introductionmentioning

confidence: 99%

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GEOMETRIC CORROBORATION OF THE EARLIEST LENSED GALAXY AT z ≃ 10.8 FROM ROBUST FREE-FORM MODELLING

Chan

Broadhurst

Lim

et al. 2017

ApJ

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A multiply lensed galaxy, MACS0647-JD, with a probable photometric redshift of -+  z 10.7 0.4 0.6 is claimed to constitute one of the very earliest known galaxies, formed well before reionization was completed. However, spectral evidence that MACS0647-JD lies at high redshift has proven infeasible and so here we seek an independent-lensing-based "geometric redshift" derived from the angles between the three lensed images of MACS0647-JD, using our free-form mass model (WSLAP+) for the lensing cluster MACSJ0647.7+7015 (at z = 0.591). Our lens model uses the nine sets of multiple images, including those of MACS0647-JD, identified by the CLASH survey toward this cluster. We convincingly exclude the low-redshift regime of z<3, for which convoluted critical curves are generated by our method, as the solution bends to accommodate the wide angles of MACS0647-JD for this low redshift. Instead, a best fit to all sets of lensed galaxy positions and redshifts provides a geometric redshift of -+  z 10.8 0.4 0.3 for MACS0647-JD, strongly supporting the higher photometric redshift solution. Importantly, we find a tight linear relation between the relative brightnesses of all nine sets of multiply lensed images and their relative magnifications as predicted by our model. This agreement provides a benchmark for the quality of the lens model, and establishes the robustness of our free-form lensing method for measuring model-independent geometric source distances and for deriving objective central cluster mass distributions. After correcting for its magnification the luminosity of MACS0647-JD remains relatively high at M UV = −19.4, which is within a factor of a few in flux of some surprisingly luminous z;10-11 candidates discovered recently in Hubble blank field surveys.

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Section: Introductionmentioning

confidence: 73%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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GEOMETRIC CORROBORATION OF THE EARLIEST LENSED GALAXY AT z ≃ 10.8 FROM ROBUST FREE-FORM MODELLING

Chan

Broadhurst

Lim

et al. 2017

ApJ

Self Cite

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“…The deep HST data have resulted in an unprecedented set of strong-lensed arcs and multiple images for constraining the cluster potentials (e.g., Jauzac et al 2014Jauzac et al , 2015Lam et al 2014;Diego et al 2015Diego et al , 2016Wang et al 2015;Kawamata et al 2016), doubling or tripling the number of multiple images (Table 5, Figure 8). Subsequent observations with the GLASS HST WFC3/IR grism GO program (Schmidt et al 2014;Treu et al 2015; see 10.17909/ T9KG60) and new ground-based spectroscopic campaigns have greatly increased the number and accuracy of the redshifts for the background lensed FF galaxies (Ebeling et al 2014;Johnson et al 2014;Richard et al 2014;Balestra et al 2015;Grillo et al 2015;Hoag et al 2016).…”

Section: Lensing Models and Predictionsmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

587

574

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What are the faintest distant galaxies we can see with the Hubble Space Telescope (HST) now, before the launch of the James Webb Space Telescope? This is the challenge taken up by the Frontier Fields, a Director's discretionary time campaign with HST and the Spitzer Space Telescope to see deeper into the universe than ever before. The Frontier Fields combines the power of HST and Spitzer with the natural gravitational telescopes of massive highmagnification clusters of galaxies to produce the deepest observations of clusters and their lensed galaxies ever obtained. Six clusters-Abell 2744, MACSJ0416.1-2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063, and Abell 370-have been targeted by the HST ACS/WFC and WFC3/IR cameras with coordinated parallel fields for over 840 HST orbits. The parallel fields are the second-deepest observations thus far by HST with 5σ point-source depths of ∼29th ABmag. Galaxies behind the clusters experience typical magnification factors of a few, with small regions magnified by factors of 10-100. Therefore, the Frontier Field cluster HST images achieve intrinsic depths of ∼30-33 mag over very small volumes. Spitzer has obtained over 1000 hr of Director's discretionary imaging of the Frontier Field cluster and parallels in IRAC 3.6 and 4.5 μm bands to 5σ point-source depths of ∼26.5, 26.0 ABmag. We demonstrate the exceptional sensitivity of the HST Frontier Field images to faint high-redshift galaxies, and review the initial results related to the primary science goals.

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“…In these cases, we assume the image has the same redshift as the system. For systems 44 and under (except where otherwise specified), we use Diego et al (2016b) as the coordinate reference. The systems with ID's greater than that use Karman et al (2017) for the coordinate reference.…”

Section: Idmentioning

confidence: 99%

Exploring effects on magnifications due to line-of-sight galaxies in the Hubble Frontier Fields

Raney

Keeton

Brennan

2019

Monthly Notices of the Royal Astronomical Society

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Cluster lensing has become an important tool in the search for high redshift galaxies through its ability to magnify sources. In order to determine the intrinsic properties of these galaxies, lensing mass models must be constructed to determine the magnification of the images. These models are traditionally two-dimensional, focusing on the mass within the cluster and either ignoring or approximating any contribution from line-of-sight galaxies. In this paper, we present the first full set of three-dimensional mass models of the six Hubble Frontier Fields and use them to test for systematic biases in magnifications due to using the traditional 2D approach. We find that omitting foreground or background galaxies causes image position offsets between 0.1-0.4", a non-negligible fraction of the typical 0.3-0.7" residuals of current state-of-the-art models. We also find that median image magnifications can shift by up to 6%, though it is dependent on the field. This can be alleviated in some cases by approximating the mass in the lensing plane, but a 5% magnification bias still exists in other cases; image position offsets are also improved, but are still present at 0.10".

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A free-form mass model of the Hubble Frontier Fields cluster AS1063 (RXC J2248.7−4431) with over one hundred constraints

Cited by 50 publications

References 54 publications

GEOMETRIC CORROBORATION OF THE EARLIEST LENSED GALAXY AT z ≃ 10.8 FROM ROBUST FREE-FORM MODELLING

GEOMETRIC CORROBORATION OF THE EARLIEST LENSED GALAXY AT z ≃ 10.8 FROM ROBUST FREE-FORM MODELLING

The Frontier Fields: Survey Design and Initial Results

Exploring effects on magnifications due to line-of-sight galaxies in the Hubble Frontier Fields

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