A GEOMETRICALLY SUPPORTED
                    <i>z</i>
                    ∼ 10 CANDIDATE MULTIPLY IMAGED BY THE HUBBLE FRONTIER FIELDS CLUSTER A2744

Zitrin, Adi; Zheng, Wei; Broadhurst, Tom; Moustakas, John; Lam, Daniel; Shu, Xinwen; Huang, Xu; Diego, J. M.; Ford, H. C.; Lim, Jeremy; Bauer, F. E.; Infante, L.; Kelson, Daniel D.; Molino, A.

doi:10.1088/2041-8205/793/1/l12

Cited by 142 publications

(186 citation statements)

References 40 publications

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“…One of them, UDFj-39546284, has already been found to be possibly an EELG at redshift ∼2 (Brammer et al 2013;Capak et al 2013). More candidates are found in the ongoing Hubble Frontier Fields Zitrin et al 2014;Ishigaki et al 2014). As there are not enough spectral observations to confirm the redshifts, properly considering the contamination of EELGs is quite necessary for these samples.…”

Section: Impact On the Selection Of Z ∼ 10 Galaxiesmentioning

confidence: 99%

Clash: Extreme Emission-Line Galaxies and Their Implication on Selection of High-Redshift Galaxies

Huang

Zheng

Wang

et al. 2015

ApJ

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We utilize the Cluster Lensing And Supernova survey with Hubble observations of 25 clusters to search for extreme emission-line galaxies (EELGs). The selections are carried out in two central bands: F105W (Y 105 ) and F125W (J 125 ), as the flux of the central bands could be enhanced by the presence of [O iii] λλ4959, 5007 at redshifts of ∼0.93-1.14 and 1.57-1.79, respectively. The multiband observations help to constrain the equivalent widths (EWs) of emission lines. Thanks to cluster lensing, we are able to identify 52 candidates down to an intrinsic limiting magnitude of 28.5 and to a rest-frame [O iii] λλ4959, 5007 EW of 3700 Å. Our samples include a number of EELGs at lower luminosities that are missed in other surveys, and the extremely high EW can only be found in such faint galaxies. These EELGs can mimic a dropout feature similar to that of high-redshift galaxies and contaminate the color-color selection of high-redshift galaxies when the signal-to-noise ratio is limited or the band coverage is incomplete.

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Section: Impact On the Selection Of Z ∼ 10 Galaxiesmentioning

confidence: 99%

Clash: Extreme Emission-Line Galaxies and Their Implication on Selection of High-Redshift Galaxies

Huang

Zheng

Wang

et al. 2015

ApJ

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“…Interestingly, despite 2 magnitudes of magnification and the great depth of this imaging, no galaxy has yet been discovered beyond the most distant galaxies already known at z ∼ 10 (Coe et al 2013;Zitrin et al 2014;Zheng et al 2014;Oesch et al 2014;Coe, Bradley & Zitrin 2015;Ishigaki et al 2015). This difficulty is not due to the filter choice, which in principle can access Lymanbreak galaxies out to z 12.0.…”

Section: Introductionmentioning

confidence: 99%

“…To date, the HFF program has revealed unprecedented numbers of multiply lensed galaxies reaching a limit of z 9.6 (Zitrin et al 2014). Interestingly, despite 2 magnitudes of magnification and the great depth of this imaging, no galaxy has yet been discovered beyond the most distant galaxies already known at z ∼ 10 (Coe et al 2013;Zitrin et al 2014;Zheng et al 2014;Oesch et al 2014;Coe, Bradley & Zitrin 2015;Ishigaki et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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

Diego

Broadhurst

Wong

et al. 2016

Mon. Not. R. Astron. Soc.

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We derive a free-form mass distribution for the massive cluster AS1063 (z=0.348) using the completed optical imaging from the Hubble Frontier Fields programme. Based on a subset of 11 multiply lensed systems with spectroscopic redshift we produce a lens model that is accurate enough to unveil new multiply lensed systems, totalling over a 100 arclets, and to estimate their redshifts geometrically. Consistency is found between this precise model and that obtained using only the subset of lensed sources with spectroscopically measured redshifts.Although a relatively large elongation of the mass distribution is apparent relative to the X-ray map, no significant offset is found between the centroid of our mass distribution and that of the X-ray emission map, suggesting a relatively relaxed state for this cluster. For the well resolved lensed images we provide detailed model comparisons to illustrate the precision of our model and hence the reliability of our de-lensed sources. A clear linear structure is associated with one such source extending 23 kpc in length, that could be an example of jet-induced star formation, at redshift z ≈ 3.1.

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“…To date, a large number of primeval galaxies have been identified thanks to the Lyman Break technique (e.g. McLure et al 2013;Bradley et al 2014;Finkelstein et al 2015;Schmidt et al 2014;Bouwens et al 2015Bouwens et al , 2016Oesch et al 2014Oesch et al , 2015Zitrin et al 2014;Calvi et al 2016;Infante et al 2015;Ishigaki et al 2015;Kawamata et al 2016;McLeod et al 2015). To further our understanding on the formation and evolution of such primeval objects, we must investigate their nature and physical properties through multi-band spectroscopic observations.…”

Section: Introductionmentioning

confidence: 99%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

187

237

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We present new ALMA observations of the [Oiii]88µm line and high angular resolution observations of the [Cii]158µm line in a normal star forming galaxy at z=7.1. Previous [Cii] observations of this galaxy had detected [Cii] emission consistent with the Lyα redshift but spatially slightly offset relative to the optical (UV-rest frame) emission. The new [Cii] observations reveal that the [Cii] emission is partly clumpy and partly diffuse on scales larger than about 1kpc.[Oiii] emission is also detected at high significance, offset relative to the optical counterpart in the same direction as the [Cii] clumps, but mostly not overlapping with the bulk of the [Cii] emission. The offset between different emission components (optical/UV and different far-IR tracers) is similar to that which is observed in much more powerful starbursts at high redshift. We show that the [Oiii] emitting clump cannot be explained in terms of diffuse gas excited by the UV radiation emitted by the optical galaxy, but it requires excitation by in-situ (slightly dust obscured) star formation, at a rate of about 7 M yr −1 . Within 20 kpc from the optical galaxy the ALMA data reveal two additional [Oiii] emitting systems, which must be star forming companions. We discuss that the complex properties revealed by ALMA in the z∼7.1 galaxy are consistent with expectations by recent models and cosmological simulations, in which differential dust extinction, differential excitation and different metal enrichment levels, associated with different subsystems assembling a galaxy, are responsible for the various appearance of the system when observed with distinct tracers.

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A GEOMETRICALLY SUPPORTED z ∼ 10 CANDIDATE MULTIPLY IMAGED BY THE HUBBLE FRONTIER FIELDS CLUSTER A2744

Cited by 142 publications

References 40 publications

Clash: Extreme Emission-Line Galaxies and Their Implication on Selection of High-Redshift Galaxies

Clash: Extreme Emission-Line Galaxies and Their Implication on Selection of High-Redshift Galaxies

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

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

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