Diffuse Lyα haloes around Lyα emitters at z=3: do dark matter distributions determine the Lyα spatial extents?

Matsuda, Yoshihisa; Yamada, Tōru; Hayashino, T.; Yamauchi, Ryosuke; Nakamura, Yuki; Morimoto, Naotake; Ouchi, Masami; Ono, Yoshiyasu; Umemura, Masayuki; Mori, Masao

doi:10.1111/j.1365-2966.2012.21143.x

Cited by 141 publications

(176 citation statements)

References 53 publications

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“…The latter, the detected fraction, comes only from the central, high surface brightness part of the Lyα emission from galaxies, and not from the extended Lyα halos of low surface brightness (Zheng et al 2011b;Steidel et al 2011;Matsuda et al 2012;Momose et al 2014). The detected fraction for Lyα emission at z = 2 to 3, inferred from comparing the Lyα luminosity density and Hα or H β luminosity density, is about 5% (e.g.…”

Section: Escape Fraction and Detected Fractionmentioning

confidence: 99%

“…An extended Lyα emitting halo below sky noise level, resulting from Lyα photons scattered by neutral gas in the circumgalactic and intergalactic media and clustered unresolved Lyα sources, is predicted to exist around a star-forming galaxy based on radiative transfer modeling (Zheng et al 2011b). Such diffuse Lyα emitting halos are detected from stacking analysis (Steidel et al 2011;Matsuda et al 2012;Momose et al 2014).…”

Section: Low Surface Brightness Lyα Halos Around Galaxiesmentioning

confidence: 99%

“…Recently, Martin et al (2014a,b) published the first results from the Cosmic Web Imager, an integral field spectrograph designed to map low surface brightness emission, detecting Lyα emission from filamentary structures around a z = 2.8 quasar as long as 250-400 proper kpc. Diffuse Lyα halos around high redshift galaxies have been found to be ubiquitous by Steidel et al (2011) and Matsuda et al (2012). Momose et al (2014) have assembled several samples of up to 3600 Lyα emitters from Subaru narrowband imaging at a range of redshifts from z = 2.2 to z = 6.6 and, after controlling for atmospheric and instrumental artifacts, they detect diffuse extended Lyα halos with exponential scale lengths of ∼ 5 − 10 kpc from z = 2.2 − 5.7.…”

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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: Escape Fraction and Detected Fractionmentioning

confidence: 99%

Section: Low Surface Brightness Lyα Halos Around Galaxiesmentioning

confidence: 99%

mentioning

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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“…Stacking is a common technique used across many different wavelength: γ -rays (e.g. Aleksić et al 2011), X-rays (Chaudhary et al 2012;George et al 2012), optical/nearinfrared (Zibetti et al 2007;González et al 2012;Matsuda et al 2012), mid-/far-infrared (e.g. Dole et al 2006), and radio (Boyle et al 2007;Ivison et al 2007;Hodge et al 2008Hodge et al , 2009Dunne et al 2009;Karim et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Estimating sizes of faint, distant galaxies in the submillimetre regime

Lindroos

Knudsen

Fan

et al. 2016

Mon. Not. R. Astron. Soc.

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We measure the sizes of redshift ∼ 2 star-forming galaxies by stacking data from the Atacama Large Millimeter/submillimeter Array (ALMA). We use a uv-stacking algorithm in combination with model fitting in the uv-domain and show that this allows for robust measures of the sizes of marginally resolved sources. The analysis is primarily based on the 344 GHz ALMA continuum observations centred on 88 sub-millimeter galaxies in the LABOCA ECDFS Submillimeter Survey (ALESS). We study several samples of galaxies at z ≈ 2 with M * ≈ 5 × 10 10 M , selected using near-infrared photometry (distant red galaxies, extremely red objects, sBzK-galaxies, and galaxies selected on photometric redshift). We find that the typical sizes of these galaxies are ∼ 0. 6 which corresponds to ∼ 5 kpc at z = 2, this agrees well with the median sizes measured in the near-infrared z-band (∼ 0. 6).We find errors on our size estimates of ∼ 0. 1 − 0. 2, which agree well with the expected errors for model fitting at the given signal-to-noise ratio. With the uv-coverage of our observations (18-160 m), the size and flux density measurements are sensitive to scales out to 2 . We compare this to a simulated ALMA Cycle 3 dataset with intermediate length baseline coverage, and we find that, using only these baselines, the measured stacked flux density would be an order of magnitude fainter. This highlights the importance of short baselines to recover the full flux density of high-redshift galaxies.

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“…Using the Lyα scale length from the double exponential model, we obtain a ratio of 4.6, whereas Steidel et al (2011) obtain a ratio of 7.4 for the global sample of LBGs and 8.8 for a subsample of Lyα emitters, suggesting that this system Lyα emission is less extended than these bigger objects compared to the continuum emission. We note that some of the differences may arise from the surrounding Mpc-scale environment, particularly the density of the circum-galactic medium, as concluded by Matsuda et al (2012). Wisotzki et al 2015 recently used the newly obtained MUSE data set on the Hubble Deep Field South to study a relatively large (26) sample of Lyα emitters on an object-to-object basis.…”

Section: Surface Brightness Profilesmentioning

confidence: 99%

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

Patrício¹,

Richard²,

Verhamme

2015

Proc. IAU

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Spatially resolved studies of high-redshift galaxies, an essential insight into galaxy formation processes, have been mostly limited to stacking or unusually bright objects. We present here the study of a typical (L * , M = 6 × 10 9 M ) young lensed galaxy at z = 3.5, observed with Multi Unit Spectroscopic Explorer (MUSE), for which we obtain 2D resolved spatial information of Lyα and, for the first time, of C III] emission. The exceptional signal-to-noise ratio of the data reveals UV emission and absorption lines rarely seen at these redshifts, allowing us to derive important physical properties (T e ∼ 15600 K, n e ∼ 300 cm −3 , covering fraction f c ∼ 0.4) using multiple diagnostics. Inferred stellar and gas-phase metallicities point towards a low-metallicity object (Z stellar = ∼0.07 Z and Z ISM < 0.16 Z ). The Lyα emission extends over ∼10 kpc across the galaxy and presents a very uniform spectral profile, showing only a small velocity shift which is unrelated to the intrinsic kinematics of the nebular emission. The Lyα extension is approximately four times larger than the continuum emission, and makes this object comparable to low-mass LAEs at low redshift, and more compact than the Lyman-break galaxies and Lyα emitters usually studied at high redshift. We model the Lyα line and surface brightness profile using a radiative transfer code in an expanding gas shell, finding that this model provides a good description of both observables.Key words: techniques: imaging spectroscopy -galaxies: abundances -galaxies: highredshift -galaxies: individual: SMACSJ2031.8-4036. I N T RO D U C T I O NDuring the past few decades, our understanding of galaxy formation and evolution has made significant progress thanks to the hundreds of high-redshift (z > 3) galaxies which have been detected in dedicated observing campaigns (e.g. Shapley et al. 2003;Vanzella et al. 2009;Stark et al. 2013). The main spectral feature used to confirm the distances of these galaxies is the Lyα emission, since it E-mail: vera.patricio@univ-lyon1.fr (VP); johan.richard@univ-lyon1.fr (JR) is the brightest emission line we can observe in distant sources. Unfortunately, many of these objects are too faint to show any other emission line at rest-frame UV wavelengths or, even less likely, continuum and absorption lines, offering a limited picture of the characteristics of high-redshift galaxies. The complexity of the Lyα resonant process, which depends not only on the gas dynamics but also on gas density and dust content, also requires the observation of non-resonant lines in order to robustly probe the physical properties of such galaxies.Stacking techniques, which combine spectra or images of dozens or even hundreds of objects in order to increase signal-to-noise ratio (e.g.

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Diffuse Lyα haloes around Lyα emitters at z=3: do dark matter distributions determine the Lyα spatial extents?

Cited by 141 publications

References 53 publications

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

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

Estimating sizes of faint, distant galaxies in the submillimetre regime

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

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