The Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift 6

Ouchi, Masami; Shimasaku, Kazuhiro; Akiyama, Masayuki; Sekiguchi, K.; Furusawa, Hisanori; Okamura, S.; Kashikawa, Nobunari; Iye, Masanori; Kodama, Tadayuki; Saito, Tomoki; Sasaki, Toshiyuki; Simpson, Chris; Takata, Tadafumi; Yamada, Tōru; Yamanoi, Hitomi; Yoshida, Makiko; Yoshida, Michitoshi

doi:10.1086/428499

Cited by 260 publications

(394 citation statements)

References 37 publications

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“…5 makes up a distinct redshift system with Lyα emission falling in the bottom quarter of the filter. Such features are also seen in maps of the HDF-N. A similar structured distribution at z ∼ 5.7 has recently been reported by Ouchi et al (2005) for the Subaru XMM Deep Field.…”

Section: Large-scale Structuresupporting

confidence: 85%

Spectroscopic studies of $z \sim5.7$ and $z\sim6.5$ galaxies: implications for reionisation

Cowie

Capak

et al. 2005

Proc. IAU

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Abstract. The recent development of large, complete samples which identify high-redshift galaxies at z ∼ 5.7 and z ∼ 6.5 from deep, wide-field surveys provides detailed information on the earliest galaxies, their numbers, spatial and kinematic distributions, and implications for early reionisation of the IGM. In this contribution we present results of spectroscopic studies of z ∼ 5.7 and z ∼ 6.5 galaxies identified from our deep, Lyman alpha narrow-band and multicolour surveys conducted with the SuprimeCam mosaic CCD camera on the 8.3-m Subaru telescope and observed with the DEIMOS multi-object spectrograph on Keck. The luminosity function of the z ∼ 6.5 galaxies is shown to be similar to the luminosity function of the z ∼ 5.7 galaxy samples, suggesting that a substantial star-forming population is already in place at z ∼ 6.5. Comparisons of both individual and stacked spectra of galaxies in these two samples show that the Lyman alpha emission profiles, equivalent widths, and continuum break strengths do not substantially change over this redshift interval. The wide-field nature of the surveys also permits mapping of the large-scale distribution of high-redshift galaxies in spatial structures extending across individual SuprimeCam fields (∼ 60 Mpc). Field-to-field variations in the number of objects at z ∼ 6.5 may shortly be able to place constraints on the porosity of the reionisation boundary.

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Section: Large-scale Structuresupporting

confidence: 85%

Spectroscopic studies of $z \sim5.7$ and $z\sim6.5$ galaxies: implications for reionisation

Cowie

Capak

et al. 2005

Proc. IAU

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“…Therefore, we cannot evaluate the departure of the twopoint correlation function from a single power, which is caused by the transition from the large scale (two galaxies residing in separate dark matter halo) to the small scale clustering regime (galaxies sharing a single halo, e.g. Ouchi et al 2005).…”

Section: Clustering Of Hα Emittersmentioning

confidence: 99%

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe

Sobral

2015

Mon. Not. R. Astron. Soc.

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We carried out the largest (> 3.5 × 10 5 Mpc 3 , 26 deg 2 ) Hα narrow band survey to date at z ∼ 0.2 in the SA22, W2 and XMMLSS extragalactic fields. Our survey covers a large enough volume to overcome cosmic variance and to sample bright and rare Hα emitters up to an observed luminosity of ∼ 10 42.4 erg s −1 , equivalent to ∼ 11M yr −1 . Using our sample of 220 sources brighter than > 10 41.4 erg s −1 (> 1M yr −1 ), we derive Hα luminosity functions, which are well described by a Schechter function with φ * = 10 −2.85±0.03 Mpc −3 and L * Hα = 10 41.71±0.02 erg s −1 (with a fixed faint end slope α = −1.35). We find that surveys probing smaller volumes (∼ 3 × 10 4 Mpc 3 ) are heavily affected by cosmic variance, which can lead to errors of over 100 per cent in the characteristic density and luminosity of the Hα luminosity function. We derive a star formation rate density of ρ SFRD = 0.0094 ± 0.0008 M yr −1 , in agreement with the redshift-dependent Hα parametrisation from Sobral et al. (2013). The two-point correlation function is described by a single power law ω(θ ) = (0.159 ± 0.012)θ (−0.75±0.05) , corresponding to a clustering length of r 0 = 3.3 ± 0.8 Mpc/h. We find that the most luminous Hα emitters at z ∼ 0.2 are more strongly clustered than the relatively fainter ones. The L * Hα Hα emitters at z ∼ 0.2 in our sample reside in ∼ 10 12.5−13.5 M dark matter haloes. This implies that the most star forming galaxies always reside in relatively massive haloes or group-like environments and that the typical host halo mass of star-forming galaxies is independent of redshift if scaled by L Hα /L * Hα (z), as proposed by Sobral et al. (2010).

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“…This means that, if we assume the galaxy bias for LAEs at log L Lyα ∼ 43 to be b ∼ 2.4-4 (e.g. Ouchi et al 2005Ouchi et al , 2010Kovač et al 2007;Chiang et al 2013), and the faint LAEs are correctly tracing the matter density of this field, the bias for brighter LAEs must be b ∼ 20-40.…”

Section: Implications For Galaxy Formationmentioning

confidence: 99%

The environments of Ly α blobs – I. Wide-field Ly α imaging of TN J1338−1942, a powerful radio galaxy at z ≃ 4.1 associated with a giant Ly α nebula★

Saito

Matsuda

Lacey

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift 6

Cited by 260 publications

References 37 publications

Spectroscopic studies of $z \sim5.7$ and $z\sim6.5$ galaxies: implications for reionisation

Spectroscopic studies of $z \sim5.7$ and $z\sim6.5$ galaxies: implications for reionisation

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

The environments of Ly α blobs – I. Wide-field Ly α imaging of TN J1338−1942, a powerful radio galaxy at z ≃ 4.1 associated with a giant Ly α nebula★

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