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

Richard, Johan; Jauzac, Mathilde; Limousin, M.; Jullo, Eric; Clément, Benjamin; Ebeling, H.; Kneib, Jean-Paul; Atek, Hakim; Natarajan, Priya; Egami, Eiichi; Livermore, Rachael; Bower, Richard G.

doi:10.1093/mnras/stu1395

Cited by 218 publications

(290 citation statements)

References 61 publications

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“…powerful gravitational lens, the system has been investigated both in the strong- (Zitrin et al 2009;Limousin et al 2012;Richard et al 2014;Diego et al 2015b) and in the weak-lensing regimes (Jauzac et al 2012;Medezinski et al 2013), further underlining its position as one of the most complex, dynamically active, and massive clusters studied to date.…”

Section: Macs J0717 In the Hubble Frontier Field Eramentioning

confidence: 99%

“…Prior to the HFF observations, 16 multiple-image systems, comprising 48 individual images, had been reported (Johnson et al 2014;Richard et al 2014;Coe et al 2015). The analysis by Diego et al (2015b), using the first third of the data from the HFF observations, identified an additional 17 multiple-image systems, as well as 10 elongated features, assumed to be single images of lensed background galaxies.…”

Section: Previous Workmentioning

confidence: 99%

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Strong-lensing analysis of MACS J0717.5+3745 fromHubbleFrontier Fields observations: How well can the mass distribution be constrained?

Limousin

Richard

Jullo

et al. 2016

A&A

113

124

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We present a strong-lensing analysis of MACSJ0717.5+3745 (hereafter MACS J0717), based on the full depth of the Hubble Frontier Field (HFF) observations, which brings the number of multiply imaged systems to 61, ten of which have been spectroscopically confirmed. The total number of images comprised in these systems rises to 165, compared to 48 images in 16 systems before the HFF observations. Our analysis uses a parametric mass reconstruction technique, as implemented in the L software, and the subset of the 132 most secure multiple images to constrain a mass distribution composed of four large-scale mass components (spatially aligned with the four main light concentrations) and a multitude of galaxy-scale perturbers. We find a superposition of cored isothermal mass components to provide a good fit to the observational constraints, resulting in a very shallow mass distribution for the smooth (large-scale) component. Given the implications of such a flat mass profile, we investigate whether a model composed of "peaky" non-cored mass components can also reproduce the observational constraints. We find that such a non-cored mass model reproduces the observational constraints equally well, in the sense that both models give comparable total rms. Although the total (smooth dark matter component plus galaxy-scale perturbers) mass distributions of both models are consistent, as are the integrated two-dimensional mass profiles, we find that the smooth and the galaxy-scale components are very different. We conclude that, even in the HFF era, the generic degeneracy between smooth and galaxy-scale components is not broken, in particular in such a complex galaxy cluster. Consequently, insights into the mass distribution of MACS J0717 remain limited, emphasizing the need for additional probes beyond strong lensing. Our findings also have implications for estimates of the lensing magnification. We show that the amplification difference between the two models is larger than the error associated with either model, and that this additional systematic uncertainty is approximately the difference in magnification obtained by the different groups of modelers using pre-HFF data. This uncertainty decreases the area of the image plane where we can reliably study the high-redshift Universe by 50 to 70%.

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Section: Macs J0717 In the Hubble Frontier Field Eramentioning

confidence: 99%

Section: Previous Workmentioning

confidence: 99%

Strong-lensing analysis of MACS J0717.5+3745 fromHubbleFrontier Fields observations: How well can the mass distribution be constrained?

Limousin

Richard

Jullo

et al. 2016

A&A

113

124

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“…The core and cutoff radii are poorly constrained with an Einstein ring of about 6.2 kpc at z = 1.525. We therefore choose to fix r core = 0.15 kpc (e.g., Limousin et al 2007;Richard et al 2014), and r cut = 100 kpc (e.g., Brainerd et al 1996), which are typical values for isolated galaxies. Varying these values within our observational constraints changes the mass estimate by < 10 %.…”

Section: Lens Modeling and Source Reconstructionmentioning

confidence: 99%

Planck’s dusty GEMS

Cañameras

Nesvadba

Kneißl

et al. 2017

A&A

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We study the properties of the foreground galaxy of the Ruby, the brightest gravitationally lensed high-redshift galaxy on the sub-millimeter sky as probed by the Planck satellite, and part of our sample of Planck's Dusty GEMS. The Ruby consists of an Einstein ring of 1.4 diameter at z = 3.005 observed with ALMA at 0.1 resolution, centered on a faint, red, massive lensing galaxy seen with HST/WFC3, which itself has an exceptionally high redshift, z = 1.525 ± 0.001, as confirmed with VLT/X-Shooter spectroscopy. Here we focus on the properties of the lens and the lensing model obtained with LENSTOOL. The rest-frame optical morphology of this system is strongly dominated by the lens, while the Ruby itself is highly obscured, and contributes less than 10 % to the photometry out to the K band. The foreground galaxy has a lensing mass of (3.70 ± 0.35) × 10 11 M . Magnification factors are between 7 and 38 for individual clumps forming two image families along the Einstein ring. We present a decomposition of the foreground and background sources in the WFC3 images, and stellar population synthesis modeling with a range of star-formation histories for Chabrier and Salpeter initial mass functions (IMFs). Only the stellar mass range obtained with the latter agrees well with the lensing mass. This is consistent with the bottom-heavy IMFs of massive high-redshift galaxies expected from detailed studies of the stellar masses and mass profiles of their low-redshift descendants, and from models of turbulent gas fragmentation. This may be the first direct constraint on the IMF in a lens at z = 1.5, which is not a cluster central galaxy.

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“…Five teams have provided amplification maps for the six HFF clusters, using different methods and assumptions on the mass models (Bradač et al 2009;Richard et al 2014;Merten et al 2011;Zitrin et al 2013;Johnson et al 2014;Mohammed et al 2014). Jauzac et al (2014) have used the Frontier Fields data to search for multiple-image objects in MACSJ0416.1−2403 data.…”

Section: Magnificationmentioning

confidence: 99%

“…The new flagship program of HST, the Frontier Fields (hereafter, HFFs) started at the end of 2013, and employs deep observations combined with gravitational lensing to observe six massive galaxy clusters along with six deep blank fields. Recent papers have shown that ultra faint galaxies (m F160W ∼31−32 AB) will be detected in HFF data (Yue et al 2014;Richard et al 2014), and that the number of z ≥ 8 objects expected in these data is > ∼ 130 (Coe et al 2015).…”

Section: Introductionmentioning

confidence: 98%

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

Laporte

Streblyanska

Kim

et al. 2015

A&A

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Context. The Hubble Space Telescope (HST) Frontier Fields (HFFs) project started at the end of 2013 with the aim of providing extremely deep images of six massive galaxy clusters. One of the main goals of this program is to push several telescopes to their limits to provide the best current view of the earliest stages of the Universe. The analysis of the initial data has already demonstrated the huge capabilities of the program. Aims. We present a detailed analysis of z ∼ 8 objects behind the HFFs lensing cluster, MACSJ0416.1-2403, combining 0.3−1.6 µm imaging from HST, ground-based K s imaging from VLT HAWK-I, and 3.6 µm and 4.5 µm Spitzer Space Telescope. The images probe to 5σ depths of ≈29 AB for HST, 25.6 AB for HAWK-I, and ≈0.310 and 0.391 µJy at 3.6 and 4.5 µm, respectively. With these datasets, we assess the photometric properties of z ∼ 8 galaxies in this field, as well as their distribution in luminosity, to unprecedented sensitivity. Methods. We applied the classical Lyman break (LB) technique, which combines non detection criteria in bands blueward of the Lyman break at z ∼ 8 and color-selection in bands redward of the break. To avoid contamination by mid-z interlopers, we required a strong break between optical and near-infrared data. We determined the photometric properties of z ∼ 8 selected candidates using spectral energy distribution (SED)-fitting with standard library templates. The luminosity function at z ∼ 8 is computed using a Monte-Carlo method taking advantage of the SED-fitting results. A piece of cautionary information is gleaned from new deep optical photometry of a previously identified z ∼ 8 galaxy in this cluster, which is now firmly detected as a mid-z interloper with a strong ≈1.5 mag Balmer break (between F606W and F125W). Using the SED of this interloper, we estimated the contamination rate of our MACSJ0416.1−2403 sample, and that of previous samples in Abell 2744 that were based on HFF data, we highlight the dangers of pushing the LB technique too close to the photometry limits. Results. Our selection reliably recovers four objects with m F160W ranging from 26.0 to 27.9 AB that are located in modestamplification regions (µ < 2.4). Two of the objects display a secondary break between the IRAC 3.6 µm and 4.5 µm bands, which could be associated to the Balmer break or emission lines at z ∼ 8. The SED-fitting analysis suggests that all of these objects favor high-z solutions with no reliable secondary solutions. The candidates generally have star formation rates around ∼10 M /yr and sizes ranging from 0.2 to 0.5 kpc, which agrees well with previous observations and expectations for objects in the early Universe. The sample size and luminosity distribution are consistent with previous findings.

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

Cited by 218 publications

References 61 publications

Strong-lensing analysis of MACS J0717.5+3745 fromHubbleFrontier Fields observations: How well can the mass distribution be constrained?

Strong-lensing analysis of MACS J0717.5+3745 fromHubbleFrontier Fields observations: How well can the mass distribution be constrained?

Planck’s dusty GEMS

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

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