A Remarkably Luminous Galaxy at Z = 11.1 Measured With Hubble Space Telescope Grism Spectroscopy

Oesch, Pascal; Brammer, Gabriel; Dokkum, Pieter van; Illingworth, G. D.; Bouwens, Rychard; Labbé, Ivo; Franx, Marijn; Momcheva, Ivelina; Ashby, M. L. N.; Fazio, G. G.; González, Valentino; Holden, B.; Magee, D.; Skelton, Rosalind E.; Smit, Renske; Spitler, Lee R.; Trenti, Michele; Willner, S. P.

doi:10.3847/0004-637x/819/2/129

Cited by 463 publications

(444 citation statements)

References 61 publications

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“…Indeed, spectroscopic confirmation has recently been obtained for three UV-luminous (M 22 UV~-mag) galaxies at z 7.5 8.7 -with H 25.1 AB selected from CANDELS fields (Roberts-Borsani et al 2016), one at z 8.7 (Zitrin et al 2015) and one at z 11 (GN-z11; Oesch et al 2016). Furthermore, the lower spatial resolution of ground-based observations, compared to HST data, can blend the signal from mergers or from physically unrelated objects and hence make them appear as single sources (e.g., Bowler et al 2017), resulting in an over-estimate of the bright end of the LF and an underestimate of the LF at lower luminosities.…”

Section: = -+mentioning

confidence: 98%

“…As a consistency check, we also derived R e using SExtractor. (R 0.6 0.3 e,circ =  for the brightest known galaxy at the highest redshift, with luminosity similar to that of our sample; Oesch et al 2016). Moreover, because the evolution of the characteristic luminosity of the UV LF is small for z 4 10 - Finkelstein et al 2015;Bowler et al 2017;Ono et al 2017), and considering that our sources constitute the very bright end of the UV LF, the absolute magnitude corresponding to a constant cumulative number density should evolve very little over z 4 10…”

Section: Size Measurementmentioning

confidence: 99%

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HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

Stefanon

Labbé

Bouwens

et al. 2017

ApJ

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We report on the discovery of three especially bright candidate z 8 phot  galaxies. Five sources were targeted for follow-up with the mag, 5s) NIR data from the UltraVISTA DR3 release, deep ground-based optical imaging from the CFHTLS and Suprime-Cam programs, and Spitzer/IRAC mosaics combining observations from the SMUVS and SPLASH programs. Through the refined spectral energy distributions, which now also include new HyperSuprimeCam g-, r-, i-, z-, and Y-band data, we confirm that 3/5 galaxies have robust z 8.0 8.7phot~-, consistent with the initial selection. The remaining 2/5 galaxies have a nominal z 2 phot~. However, with HST data alone, these objects have increased probability of being at z 9 . We measure mean UV continuum slopes 1.74 0.35 b = - for the three z 8 9 -galaxies, marginally bluer than similarly luminous z 4 6 -in CANDELS but consistent with previous measurements of similarly luminous galaxies at z 7 . The circularized effective radius for our brightest source is 0.9±0.3kpc, similar to previous measurements for a bright z 11 galaxy and bright z 7 galaxies. Finally, enlarging our sample to include the six brightest z 8 LBGs identified over UltraVISTA (i.e., including three other sources from Labbé et al.) we estimate for the first time the volume density of galaxies at the extreme bright end (M 22 UV~-mag) of the z 8 UV luminosity function. Despite this exceptional result, the still large statistical uncertainties do not allow us to discriminate between a Schechter and a double-power-law form.

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Section: = -+mentioning

confidence: 98%

Section: Size Measurementmentioning

confidence: 99%

HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

Stefanon

Labbé

Bouwens

et al. 2017

ApJ

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“…Thanks to WFC3, detections of z∼8 candidates are now relatively commonplace (e.g., Finkelstein et al 2010;Labbé et al 2010;McLure et al 2011;Yan et al 2011;Bradley et al 2012). The current measurement of the cosmic star formation history extends to less than 500 Myr after the Big Bang (e.g., Ellis et al 2013;Oesch et al 2013Oesch et al , 2016Bouwens et al 2015a;Finkelstein et al 2015; but see Brammer et al 2013;Pirzkal et al 2013), albeit with very small numbers of candidates at z>9. HSTʼs observations of high-redshift galaxies have placed important constraints on cosmological measures of reionization (e.g., Bouwens et al 2015b;Finkelstein et al 2015;Robertson et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

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576

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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“…Over the past few years, ground-and space-based observations have allowed a statistically significant data set to be collected for z;6-10 Lyman Break galaxies (LBGs; Bouwens et al 2010Bouwens et al , 2011Bouwens et al , 2015bCastellano et al 2010;McLure et al 2010McLure et al , 2013Oesch et al 2010Oesch et al , 2013Oesch et al , 2016Bradley et al 2012;Bowler et al 2014Bowler et al , 2015Atek et al 2015;Livermore et al 2016). In this work, our aim is to revisit the constraints allowed on the WDM particle mass by combining these "galaxy" data sets with the latest limits on the cosmological electron scattering optical depth inferred by Planck.…”

Section: Introductionmentioning

confidence: 99%

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Dayal

Choudhury

Bromm

et al. 2017

ApJ

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We compare model results from a semi-analytic (merger-tree based) framework for high-redshift (z;5-20) galaxy formation against reionization indicators, including the Planck electron scattering optical depth (τ es ) and the ionizing photon emissivity (ṅ ion ), to shed light on the reionization history and sources in Cold (CDM) and Warm Dark Matter (WDM; particle masses of m x =1.5, 3, and 5 keV) cosmologies. This model includes all ofthe key processes of star formation, supernova feedback, the merger/accretion/ejectiondriven evolution of gas and stellar mass and the effect of the ultra-violet background (UVB), created during reionization, in photo-evaporating the gas content of galaxies in halos with M h 10 9  M . We find that the delay in the start of reionization in light (1.5 keV) WDM models can be compensated by a steeper redshift evolution of the ionizing photon escape fraction and a faster mass assembly, resulting in reionization ending at comparable redshifts (z;5.5) in all the dark matter models considered. We find thatthe bulk of the reionization photons come from galaxies with a halo mass of M h 10 9  M and a UV magnitude of −15M UV −10 in CDM. The progressive suppression of low-mass halos with decreasing m x leads to a shift in the "reionization" population to larger halo masses of M h 10 9  M and −17M UV −13 for 1.5 keV WDM. We find that current observations of τ es and the ultra violet luminosity function are equally compatible with all the (cold and warm) dark matter models considered in this work. Quantifying the impact of the UVB on galaxy observables (luminosity functions, stellar mass densities, andstellar to halo mass ratios) for different DM models, we propose that global indicators including the redshift evolution of the stellar mass density and the stellar mass-halo mass relation, observable with the James Webb Space Telescope, can be used to distinguish between CDM and WDM (1.5 keV) cosmologies.

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A Remarkably Luminous Galaxy at Z = 11.1 Measured With Hubble Space Telescope Grism Spectroscopy

Cited by 463 publications

References 61 publications

HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

The Frontier Fields: Survey Design and Initial Results

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

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