Subaru Deep Survey. IV. Discovery of a Large-Scale Structure at Redshift ≃5

Shimasaku, Kazuhiro; Ouchi, Masami; Okamura, S.; Kashikawa, Nobunari; Doi, Mamoru; Furusawa, Hisanori; Hamabe, M.; Hayashino, T.; Kawabata, Koji S.; Kimura, Masahiko; Kodaira, Keiichi; Komiyama, Yutaka; Matsuda, Yoshihisa; Miyazaki, Masayuki; Miyazaki, Satoshi; Nakata, Fumiaki; Ohta, Kouji; Ohyama, Youichi; Sekiguchi, M.; Shioya, Yasuhiro; Tamura, H.; Taniguchi, Yuki; Yagi, Masafumi; Yamada, Tōru; Yasuda, Naoki

doi:10.1086/374880

Cited by 136 publications

(137 citation statements)

References 31 publications

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“…Adopting the normalization of the power spectrum σ 8 = 0.81 (Komatsu et al 2011) and the approximation for the mass variance with the top-hat window, σ (R) = σ 8 (R/r 8 ) −β (Mo et al 2010) with β ≈ 0.7 (CDM shape parameter Γ = 0.2), and the linear growth rate in the non-zero cosmological constant (Carroll et al 1992), ≈3.3 at z = 3.1, we obtain the σ (R) = (δρ/ρ 0 ) 2 1/2 at the corresponding comoving scale (R ≈ 32 Mpc) at z = 3.1 is ≈ 0.11. The observed density variation among the five general fields, (δN/N 0 ) LAE = −0.38 (SXDS-N) to + 0.21 (SDF), is comparable with the value, if we consider that the Lyα emitters trace mass distribution with the linear biasing factor b ∼ 2-6, as obtained in the previous study of Lyα emitters at z = 2-5 from the analysis of the twopoint correlation functions (Shimasaku et al 2003;Gawiser et al 2007;Guaita et al 2010). On the other hand, the density excess of the SSA22-Sb1 with (δN/N 0 ) LAE = 1.13 ± 0.01 even at this scale is unexpectedly large, more than ≈10× the mass fluctuation, which implies that the field is the very rare, >5σ LAE peak with b = 2 (Gawiser et al 2007).…”

Section: Discussionsupporting

confidence: 85%

“…More than a few high-density regions of the Lyα emitters and star-forming galaxies at high redshift have been studied (Keel et al 1999;Steidel et al 2000Steidel et al , 2005Shimasaku et al 2003;Palunas et al 2004;Hayashino et al 2004;Matsuda et al 2004Matsuda et al , 2009Matsuda et al , 2010 Kuiper et al 2010;Yang et al 2010). Among them, the structure at z = 3.09 in the SSA22 region, specifically the area around the original selected survey area at 22 h (Cowie et al 1990), is one of the most prominent and interesting ones.…”

Section: Introductionmentioning

confidence: 99%

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PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

Yamada

Nakamura

Matsuda

et al. 2012

The Astronomical Journal

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We present the results of the extensive narrowband survey of Lyα emission-line objects at z = 3.1 in the 1.38 deg 2 area surrounding the high-density region of star-forming galaxies at z = 3.09 in the SSA22 field, as well as in the 1.04 deg 2 area of the three separated general blank fields. In total, of 2161 Lyα emitters, there are 1394 in the SSA22 fields and 767 in the general fields detected at the narrowband AB magnitude limit of 25.73, which corresponds to the line flux of ≈1.8 × 10 −17 erg s −1 cm −2 or the luminosity of ≈1.5 × 10 42 erg s −1 at z = 3.1, above the observed equivalent-width threshold, ≈190 Å. The average surface number density of the emitters at z = 3.1 in the general fields above the thresholds is 0.20 ± 0.01 arcmin −2 . The SSA22 high-density region at z = 3.09, whose peak local density is six times that of the average, is found to be the most prominent outstanding structure in the whole surveyed area and is firmly identified as a robust "protocluster." We also compared the overdensity of the 100 arcmin 2 and 700 arcmin 2 areas which contain the protocluster with the expected fluctuation of the dark matter as well as those of the model galaxies in cosmological simulations. We found that the peak height values of the overdensity are 8-10 and 3-4 times the expected standard deviations for the counts of Lyα emitters at z = 3.1 in the corresponding volume, respectively. We conclude that the structure at z = 3.09 in the SSA22 field is a very significant and rare density peak up to the scale of ≈60 Mpc.

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Section: Discussionsupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

Yamada

Nakamura

Matsuda

et al. 2012

The Astronomical Journal

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156

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“…For example, Steidel et al (2000) used narrow-band imaging to map the extent of a large-scale structure at z ∼ 3.09, discovered in a survey for continuum-selected Lyman-break galaxies. Shimasaku et al (2003) serendipitously found a large-scale structure at z ∼ 4.9 while searching for Lyα emitters in the Subaru Deep Field. Their results demonstrate that Mpc-scaled structures have already formed by z ∼ 4.9 and that Lyα emitters must be very biased tracers of mass in the early Universe.…”

Section: Introductionmentioning

confidence: 98%

“…Bahcall et al 1997). The narrow-band imaging technique can efficiently select objects with a strong Lyα line in a narrow redshift range, and is therefore ideal for finding and investigating overdense regions at high redshift (Steidel et al 2000;Shimasaku et al 2003;Palunas et al 2004). For example, Steidel et al (2000) used narrow-band imaging to map the extent of a large-scale structure at z ∼ 3.09, discovered in a survey for continuum-selected Lyman-break galaxies.…”

Section: Introductionmentioning

confidence: 99%

Discovery of six Lyα emitters near a radio galaxy at z ~ 5.2

Venemans¹,

Röttgering²,

Overzier³

et al. 2004

A&A

105

145

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Abstract. We present the results of narrow-band and broad-band imaging with the Very Large Telescope of the field surrounding the radio galaxy TN J0924-2201 at z = 5.2. Fourteen candidate Lyα emitters with a rest-frame equivalent width of >20 Å were detected. Spectroscopy of 8 of these objects showed that 6 have redshifts similar to that of the radio galaxy. The density of emitters at the redshift of the radio galaxy is estimated to be a factor 1.5-6.2 higher than in the field, and comparable to the density of Lyα emitters in radio galaxy protoclusters at z = 4.1, 3.1 and 2.2. The Lyα emitters near TN J0924-2201 could therefore be part of a structure that will evolve into a massive cluster. These observations confirm that substantial clustering of Lyα emitters occurs at z > 5 and support the idea that radio galaxies pinpoint high density regions in the early Universe.

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“…While this technique has been successful in observing large numbers of structures or protostructures in the high-redshift universe, it is not at all clear whether such environments are typical progenitors of lower redshift clusters or are exceptional in some way, which limits their usefulness in contextualizing results at lower redshifts. Additionally, narrow-band and spectroscopic searches of Lyman α emitter (LAEs) populations in (somewhat) random regions of the sky have revealed protostructures in the very high-redshift universe (e.g., Shimasaku et al 2003;Ouchi et al 2005;Lemaux et al 2009;Toshikawa et al 2012). However, such surveys cover rather limited portions of the sky and are only effective at observing overdensities of emission line objects, a population that, while being readily observed at high redshift because of the relative ease of obtaining redshifts of emission line objects, is the subdominant population in the early universe (see, e.g., Shapley et al 2003).…”

mentioning

confidence: 99%

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Lemaux

Cucciati

Tasca

et al. 2014

A&A

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Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we performed a systematic search for overdense environments in the early universe (z > 2) and report here on the discovery of Cl J0227-0421, a massive protocluster at z = 3.29. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, δ gal = 10.5 ± 2.8, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated by a variety of methods to be ∼3 × 10 14 M at z ∼ 3.3, which, evolved to z = 0 results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics that are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample.

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Subaru Deep Survey. IV. Discovery of a Large-Scale Structure at Redshift ≃5

Cited by 136 publications

References 31 publications

PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

Discovery of six Lyα emitters near a radio galaxy at z ~ 5.2

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

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