COMPLETING THE CENSUS OF Lyα EMITTERS AT THE REIONIZATION EPOCH $^,$

Kashikawa, Nobunari; Shimasaku, Kazuhiro; Matsuda, Yoshihisa; Egami, Eiichi; Jiang, Linhua; Nagao, Tohru; Ouchi, Masami; Malkan, Matthew A.; Hattori, Takashi; Ota, Kazuaki; Taniguchi, Yoshiaki; Okamura, S.; Ly, Chun; Iye, Masanori; Furusawa, Hisanori; Shioya, Yasuhiro; Shibuya, Tetsuo; Ishizaki, Yoshifumi; Toshikawa, Jun

doi:10.1088/0004-637x/734/2/119

Cited by 264 publications

(586 citation statements)

References 94 publications

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“…However, this decline can be compensated by an increase in either fα/fc or Tα (in an increasingly ionized IGM). Comparing our model Lyα LFs to observations (Kashikawa et al 2011) we found that allowing for clumped dust (p > ∼ 0.7), the observations can be reproduced for χHI 0.5 − 10 −4 , fesc 0.05 − 0.5 and fα/fc = 0.6 − 1.8 within a 1σ error.…”

Section: The Modelsupporting

confidence: 64%

“…In this section, we use the ACF of theoretical LAEs for each of these best-fit combinations (that match the Lyα LF to within a 1-σ error as summarised in Table 1) Table 1. For the χ HI value shown in Column 1, we summarise the fα/fc ratio required to best fit the simulated Lyα LF to observations (Kashikawa et al 2011) within 1σ limits in columns 2-4 with subscripts showing the fesc value used (Hutter et al 2014 to narrow the joint constraints on χHI , fesc and fα/fc. We start by describing our procedure for obtaining LAE ACFs, which depends both on the depth along the LOS (Peebles 1980) since all galaxies are projected to a plane perpendicular to the LOS, as well as the chosen field of view (FoV), which should be comparable to that observed (Kashikawa et al 2006).…”

Section: Constraints From Lae Clusteringmentioning

confidence: 99%

“…As seen from this equation, even a neutral hydrogen fraction as low as 10 −5 can lead to a significant attenuation of Lyα photons at high-z , making them extremely sensitive probes of H I in the IGM. As a result, a class of high-z galaxies called Lyman Alpha Emitters (LAEs), detected by means of their Lyα line (at 1216Å in the rest frame), have become popular probes of reionization, with statistically significant samples available in the reionization epoch, at z 5.7 and 6.6 (Malhotra et al 2005;Taniguchi et al 2005;Shimasaku et al 2006;Hu et al 2010;Kashikawa et al 2006;Ouchi et al 2010;Kashikawa et al 2011). Indeed, a number of theoretical papers have used semi-analytic (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

Hutter

Dayal

Müller

2015

Monthly Notices of the Royal Astronomical Society

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We calculate Lyman Alpha Emitter (LAE) angular correlation functions (ACFs) at z 6.6 and the fraction of lifetime (for the 100 Myrs preceding z 6.6) galaxies spend as Lyman Break Galaxies (LBGs) or as LBGs with Lyman Alpha (Lyα) emission using a model that combines SPH cosmological simulations (GADGET-2), dust attenuation and a radiative transfer code (pCRASH). The ACFs are a powerful tool that significantly narrows the 3D parameter space allowed by LAE Lyα and UV luminosity functions (LFs) alone. With this work, we simultaneously constrain the escape fraction of ionizing photons f esc = 0.05 − 0.5, the mean fraction of neutral hydrogen in the intergalactic medium (IGM) χ HI < ∼ 0.01 and the dust-dependent ratio of the escape fractions of Lyα and UV continuum photons f α /f c = 0.6 − 1.2. Our results show that reionization has the largest impact on the amplitude of the ACFs, and its imprints are clearly distinguishable from those of f esc and f α /f c . We also show that galaxies with a critical stellar mass of M * = 10 8.5 (10 9.5 )M produce enough luminosity to stay visible as LBGs (LAEs). Finally, the fraction of time during the past 100 Myrs prior to z = 6.6 a galaxy spends as a LBG or as a LBG with Lyα emission increases with the UV magnitude (and the stellar mass M * ): considering observed (dust and IGM attenuated) luminosities, the fraction of time a galaxy spends as a LBG (LAE) increases from 65% to 100% ( 0 − 100%) as M U V decreases from M U V = −18.0 to −23.5 (M * increases from 10 8 − 10 10.5 M ). Thus in our model the brightest (most massive) LBGs most often show Lyα emission.

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Section: The Modelsupporting

confidence: 64%

Section: Constraints From Lae Clusteringmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

Hutter

Dayal

Müller

2015

Monthly Notices of the Royal Astronomical Society

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“…The distribution of onsource integration times is illustrated in Figure 5. Kashikawa et al (2006) and Ly07, and the 2008-2009 data have been discussed in Kashikawa et al (2011). In brief, we constructed 22 slitmasks with 1″ slit widths, and used the 830 line mm −1 grating and GG495 order-cut filter.…”

Section: Mmt/hectospec Observing Programmentioning

confidence: 99%

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

Ly¹,

Malhotra²,

Malkan³

et al. 2016

ApJS

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Deep rest-frame optical spectroscopy is critical for characterizing and understanding the physical conditions and properties of the ionized gas in galaxies. Here, we present a new spectroscopic survey called "Metal Abundances across Cosmic Time" or  , which will obtain rest-frame optical spectra for ∼3000 emission-line galaxies. This paper describes the optical spectroscopy that has been conducted with MMT/Hectospec and Keck/DEIMOS for ≈1900 z = 0.1-1 emission-line galaxies selected from our narrowband and intermediate-band imaging in the Subaru Deep Field. In addition, we present a sample of 164 galaxies for which we have measured the weak [O III] λ4363 line (66 with at least 3σ detections and 98 with significant upper limits). This nebular emission line determines the gas-phase metallicity by measuring the electron temperature of the ionized gas. This paper presents the optical spectra, emission-line measurements, interstellar properties (e.g., metallicity, gas density), and stellar properties (e.g., star formation rates, stellar mass). Paper II of the  survey (Ly et al.) presents the first results on the stellar mass-gas metallicity relation at z1 using the sample with [O III]λ4363 measurements.

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“…The Lyα line is predicted to be the dominant spectral signature in young galaxies (Charlot & Fall 1993;Schaerer 2003), and combined with its rest-frame wavelength in the UV, one obtains a very efficient tool for detecting galaxies at 2 < z < 7 in the optical window from ground-based telescopes. Therefore, this potential has often been used to assemble large samples of star-forming galaxies at high redshift (e.g., Gronwall et al 2007;Nilsson et al 2009;Ouchi et al 2010;Hayes et al 2010;Cassata et al 2011;Kashikawa et al 2011). Lyα-based Figure 13 and Tables 1 and 2 are available in electronic form at http://www.aanda.org…”

Section: Introductionmentioning

confidence: 99%

Influence of physical galaxy properties on Lyαescape in star-forming galaxies

Atek

Kunth

Schaerer

et al. 2014

A&A

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Context. Among the different observational techniques used to select high-redshift galaxies, the hydrogen recombination line Lymanalpha (Lyα) is of particular interest because it gives access to the measurement of cosmological quantities such as the star formation rate (SFR) of distant galaxy populations. However, interpreting this line and calibrating such observables are still subject to serious uncertainties. Aims. In this context, it important to understand the mechanisms responsible for the attenuation of Lyα emission, and under what conditions the Lyα emission line can be used as a reliable star formation diagnostic tool. Methods. We used a sample of 24 Lyα emitters at z ∼ 0.3 with an optical spectroscopic follow-up to calculate the Lyα escape fraction and its dependence upon different physical properties. We also examined the reliability of Lyα as a SFR indicator. We combined these observations with a compilation of Lyα emitters selected at z = 0−0.3 from the literature to assemble a larger sample. Results. We confirm that the Lyα escape fraction clearly depends on the dust extinction following the relation f esc (Lyα) = C Lyα × 10 −0.4 E(B−V) k Lyα where k Lyα ∼ 6.67 and C Lyα = 0.22. However, the correlation does not follow the expected curve for a simple dust attenuation. A higher attenuation can be attributed to a scattering process, while f esc (Lyα) values that are clearly above the continuum extinction curve can be the result of various mechanisms that can lead to an enhancement of the Lyα output. We also observe that the strength of Lyα and the escape fraction appear unrelated to the galaxy metallicity. Regarding the reliability of Lyα as a SFR indicator, we show that the deviation of SFR(Lyα) from the true SFR (as traced by the UV continuum) is a function of the observed SFR(UV), which can be seen as the decrease in f esc (Lyα) with increasing UV luminosity. Moreover, we observe redshift dependence of this relationship, revealing the underlying evolution of f esc (Lyα) with redshift.

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COMPLETING THE CENSUS OF Lyα EMITTERS AT THE REIONIZATION EPOCH $^,$

Cited by 264 publications

References 94 publications

Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

Influence of physical galaxy properties on Lyαescape in star-forming galaxies

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