DISCOVERY OF
                    <i>z</i>
                    ∼ 8 GALAXIES IN THE HUBBLE ULTRA DEEP FIELD FROM ULTRA-DEEP WFC3/IR OBSERVATIONS

Bouwens, Rychard; Illingworth, G. D.; Oesch, Pascal; Stiavelli, M.; Dokkum, Pieter van; Trenti, Michele; Magee, D.; Labbé, Ivo; Franx, Marijn; Carollo, C. M.; González, Valentino

doi:10.1088/2041-8205/709/2/l133

Cited by 360 publications

(573 citation statements)

References 33 publications

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“…The dustcorrected results of Bouwens et al (2010) imply ρSFR = 0.19 +0.08 −0.06 M⊙yr −1 Mpc −3 at z = 2.55, and from our measurement, ρSFR = (0.28 ± 0.07)(3/bα) M⊙yr −1 Mpc −3 . This means that bα > 3.0 is needed for our measurement not to imply detection of more Lyα photons than are actually produced at more than the 1 − σ level.…”

Section: Star Formation Rate Densitysupporting

confidence: 76%

“…The references are given in Section 5. The shaded area represents the range of dust corrected UV estimates compiled by Bouwens et al (2010).…”

Section: Star Formation Rate Densitymentioning

confidence: 99%

“…If an intrinsic β-dust extinction relationship is assumed, (usually that measured empirically from z ∼ 0 galaxies by Meurer et al 1999), one can use observations of β for high redshift galaxies to infer a dust-corrected UV luminosity and then star formation rate. This has been done by several authors, including Bouwens et al (2009Bouwens et al ( ,2010. In Figure 13 we show as a blue band the compilation of dust-corrected UV star formation densities from Bouwens et al (2010) computed using this technique.…”

Section: Star Formation Rate Densitymentioning

confidence: 99%

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Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

Croft¹,

Miralda-Escudé²,

Zheng³

et al. 2016

Mon. Not. R. Astron. Soc.

106

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We detect the large-scale structure of Lyα emission in the Universe at redshifts z = 2 − 3.5 by measuring the cross-correlation of Lyα surface brightness with quasars in the Sloan Digital Sky Survey (SDSS/BOSS). We use nearly a million spectra targeting Luminous Red Galaxies (LRGs) at z < 0.8, after subtracting a best fit model galaxy spectrum from each one, as an estimate of the high-redshift Lyα surface brightness. The quasar-Lyα emission cross-correlation we detect has a shape consistent with a linear ΛCDM model with Ω m = 0.30 +0.10 −0.07 . The predicted amplitude of this crosscorrelation is proportional to the product of the mean Lyα surface brightness, µ α , the amplitude of mass density fluctuations, and the quasar and Lyα emission bias factors. Using published cosmological observations to constrain the amplitude of mass fluctuations and the quasar bias factor, we infer the value of the product µ α (b α /3) = (3.9±0.9)×10 −21 erg s −1 cm −2Å−1 arcsec −2 , where b α is the Lyα emission linear bias factor. If the dominant sources of Lyα emission we measure are star forming galaxies, we infer a total mean star formation rate density of ρ SFR = (0.28 ± 0.07)(3/b α ) yr −1 Mpc −3 at z = 2 − 3.5. For b α = 3, this value is a factor of 21 − 35 above previous estimates relying on individually detected Lyα emitters, although it is consistent with the total star-formation density derived from dust-corrected, continuum UV surveys. Our observations therefore imply that 97% of the Lyα emission in the Universe at these redshifts is undetected in previous surveys of Lyα emitters. Our detected Lyα emission is also much greater, by at least an order of magnitude, than that measured from stacking analyses of faint halos surrounding previously detected Lyα emitters, but we speculate that it arises from similar low surface brightness Lyα halos surrounding all luminous star-forming galaxies. We also detect a redshift space anisotropy of the quasar-Lyα emission cross-correlation, finding evidence at the 3.0σ level that it is radially elongated, contrary to the prediction for linear gravitational evolution, but consistent with distortions caused by radiative-transfer effects, as predicted by Zheng et al. (2011). Our measurements represent the first application of the intensity mapping technique to optical observations.

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Section: Star Formation Rate Densitysupporting

confidence: 76%

“…The references are given in Section 5. The shaded area represents the range of dust corrected UV estimates compiled by Bouwens et al (2010).…”

Section: Star Formation Rate Densitymentioning

confidence: 99%

Section: Star Formation Rate Densitymentioning

confidence: 99%

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Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

Croft¹,

Miralda-Escudé²,

Zheng³

et al. 2016

Mon. Not. R. Astron. Soc.

106

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“…The diagram also includes SFR density determinations at z 7 and z 8 from Bouwens et al, and values from earlier studies at z < 4. Dust corrections are applied and are already negligible by z 7 Bouwens et al 2010Bouwens et al , 2009. Note how the SFR steadily increases with time in the early universe until reaching a maximum at an age of 2.5 Gyr (z ∼ 3-2).…”

Section: Star-formation History Of the Universementioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

171

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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“…As of 2016 there are now ∼1000 candidate objects, encompassing a wide range of luminosities, identified (e.g. Bouwens et al 2010Bouwens et al , 2011Bouwens et al , 2014aBouwens et al ,b, 2015aOesch et al 2010Oesch et al , 2013Oesch et al , 2014Oesch et al , 2015Oesch et al , 2016Bunker et al 2010;Wilkins et al 2010Wilkins et al , 2011aFinkelstein et al 2010Finkelstein et al , 2012Finkelstein et al , 2015Lorenzoni et al 2011Lorenzoni et al , 2013McLure et al 2011McLure et al , 2013Ellis et al 2013;Laporte et al 2014Laporte et al , 2015Laporte et al , 2016Schmidt et al 2014;McLeod et al 2015;McLeod, McLure & Dunlop 2016;Atek et al 2015a, Atek et al2015b) with the first small samples now identified at z ∼ 10 and beyond.…”

Section: Introductionmentioning

confidence: 99%

The photometric properties of galaxies in the early Universe

Wilkins

Feng

DiMatteo

et al. 2016

Mon. Not. R. Astron. Soc.

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We use the large cosmological hydro-dynamic simulation BlueTides to predict the photometric properties of galaxies during the epoch of reionisation (z = 8 − 15). These properties include the rest-frame UV to near-IR broadband spectral energy distributions, the Lyman continuum photon production, the UV star formation rate calibration, and intrinsic UV continuum slope. In particular we focus on exploring the effect of various modelling assumptions, including the assumed choice of stellar population synthesis model, initial mass function, and the escape fraction of Lyman continuum photons, upon these quantities. We find that these modelling assumptions can have a dramatic effect on photometric properties leading to consequences for the accurate determination of physical properties from observations. For example, at z = 8 we predict that nebular emission can account for up-to 50% of the rest-frame R-band luminosity, while the choice of stellar population synthesis model can change the Lyman continuum production rate up to a factor of ×2.

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DISCOVERY OF z ∼ 8 GALAXIES IN THE HUBBLE ULTRA DEEP FIELD FROM ULTRA-DEEP WFC3/IR OBSERVATIONS

Cited by 360 publications

References 33 publications

Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

Star formation sustained by gas accretion

The photometric properties of galaxies in the early Universe

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