A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshift<i>z</i>= 3.1

Matsuda, Yoshihisa; Yamada, Tōru; Hayashino, T.; Tamura, H.; Yamauchi, Ryosuke; Ajiki, Masaru; Fujita, Shinobu S.; Murayama, Takashi; Nagao, Tohru; Ohta, Kouji; Okamura, S.; Ouchi, Masami; Shimasaku, Kazuhiro; Shioya, Yasuhiro; Taniguchi, Yoshiaki

doi:10.1086/422020

Cited by 317 publications

(573 citation statements)

References 46 publications

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“…Later, Narrow band Lyα imaging has identified additional z = 3.1 galaxies (LAEs) in a larger region around the original spike, extending for more than 60 Mpc comoving (Hayashino et al 2004;Yamada et al 2012) and thought to trace several dark matter filaments intersecting to form a density peak (Matsuda et al 2005). Overdensities of Lyα absorbers (Hayashino et al 2004), Lyα blobs (Steidel et al 2000;Matsuda et al 2004Matsuda et al , 2011, AGN (Lehmer et al 2009) and submillimeter galaxies (Geach et al 2005(Geach et al , 2014Tamura et al 2009;Umehata et al 2014) have also been detected.…”

Section: The Ssa22 Protoclustermentioning

confidence: 97%

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

Hine

Geach

Alexander

et al. 2015

Mon. Not. R. Astron. Soc.

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The overdense environments of protoclusters of galaxies in the early Universe (z > 2) are expected to accelerate the evolution of galaxies, with an increased rate of stellar mass assembly and black hole accretion compared to co-eval galaxies in the average density 'field'. These galaxies are destined to form the passive population of massive galaxies that dominate the cores of rich clusters today. While signatures of the accelerated growth of galaxies in the SSA22 protocluster (z = 3.1) have been observed, the mechanism driving this remains unclear. Here we show an enhanced rate of galaxy-galaxy mergers could be responsible. We morphologically classify Lyman-break Galaxies (LBGs) in the SSA22 protocluster and compare these to those of galaxies in the field at z = 3.1 as either active mergers or non-merging using Hubble Space Telescope ACS/F814W imaging, probing the rest-frame ultraviolet stellar light. We measure a merger fraction of 48±10 per cent for LBGs in the protocluster compared to 30±6 per cent in the field. Although the excess is marginal, an enhanced rate of mergers in SSA22 hints that galaxy-galaxy mergers are one of the key channels driving accelerated star formation and AGN growth in protocluster environments.

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Section: The Ssa22 Protoclustermentioning

confidence: 97%

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

Hine

Geach

Alexander

et al. 2015

Mon. Not. R. Astron. Soc.

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“…For illustrative purposes, we include in the same figure the results of other studies targeting radio galaxies (Reuland et al 2003;VillarMartín et al 2007), radio-loud quasars (Heckman et al 1991b), Lyα blobs (Matsuda et al 2004;Prescott et al 2009),and other radio-quiet quasars (Bergeron et al 1999;Christensen et al 2006;North et al 2012). We stress that this comparison is only qualitative because these studies have different sensitivity limits, redshifts, methods, and definitions of sizes.…”

Section: Morphology Of the Nebulaementioning

confidence: 99%

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗

Borisova

Cantalupo

Lilly

et al. 2016

ApJ

272

536

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Direct Lyα imaging of intergalactic gas atz 2 has recently revealed giant cosmological structures around quasars, e.g., the Slug Nebula. Despite their high luminosity, the detection rate of such systems in narrow-band and spectroscopic surveys is less than 10%, possibly encoding crucial information on the distribution of gas around quasars and the quasar emission properties. In this study, we use the MUSE integral-field instrument to perform a blind survey for giant a Ly nebulae around 17 bright radio-quiet quasars at < < z 3 4 that does not suffer from most of the limitations of previous surveys. After data reduction and analysis performed with specifically developed tools, we found that each quasar is surrounded by giant a Ly nebulae with projected sizes larger than 100 physical kiloparsecs and, in some cases, extending up to 320 kpc. The circularly averaged surface brightness profiles of the nebulae appear to be very similar to each other despite their different morphologies and are consistent with power laws with slopes»-1.8. The similarity between the properties of all these nebulae and the Slug Nebula suggests a similar origin for all systems and that a large fraction of gas around bright quasars could be in a relatively "cold" (T ∼ 10 4 K) and dense phase. In addition, our results imply that such gas is ubiquitous within at least 50 kpc from bright quasars at < < z 3 4 independently of the quasar emission opening angle, or extending up to 200 kpc for quasar isotropic emission.

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“…Finally, Prescott et al (2008) completed a survey of z ∼ 2.7 LAEs around a so-called Lyα blob (e.g. Steidel et al 2000;Matsuda et al 2004;Dey et al 2005;Nilsson et al 2006). They argued that the central part of their field is overdense, and determined a number density of 0.0021 Mpc −3 .…”

Section: Surface Density Sizes and Sfrmentioning

confidence: 99%

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

Nilsson¹,

Tapken²,

Møller

et al. 2009

A&A

155

237

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Context. Narrow-band surveys to detect Lyα emitters are powerful tools for identifying high, and very high, redshift galaxies. Although samples are increasing at redshifts z = 3−6, the nature of these galaxies is still poorly known. The number of galaxies detected at redshifts below z ∼ 3 are also small. Aims. We study the properties of z = 2.25 Lyα emitters and compare them with those of z > 3 Lyα emitters.Methods. We present narrow-band imaging made with the MPG/ESO 2.2m telescope and the WFI (Wide Field Imager) detector. Using this data, we have searched for emission-line objects. We find 170 candidate typical Lyα emitters and 17 candidates that we regard as high UV-transmission Lyα emitters. We have derived the magnitudes of these objects in 8 photometric bands from u * to K s , and studied whether they have X-ray and/or radio counterparts. Results. We demonstrate that there has been significant evolution in the properties of Lyα emitters between redshift z ∼ 3 and z = 2.25. The spread in spectral energy distributions (SEDs) at the lower redshift is larger and we detect a significant AGN contribution in the sample. The distribution of the equivalent widths is narrower than at z ∼ 3, with only a few candidates with rest-frame equivalent width above the predicted limit of 240 Å. The star formation rates derived from the Lyα emission compared to those derived from the UV emission are lower by on average a factor of ∼1.8, indicative of a significant absorption by dust. Conclusions. Lyα emitters at redshift z = 2.25 may be more evolved than Lyα emitters at higher redshift. The red SEDs imply more massive, older and/or dustier galaxies at lower redshift than observed at higher redshifts. The decrease in equivalent widths and star formation rates indicate more quiescent galaxies, with in general less star formation than in higher redshift galaxies. At z = 2.25, AGN appear to be more abundant and also to contribute more to the Lyα emitting population.

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A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshiftz= 3.1

Cited by 317 publications

References 46 publications

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

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A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshiftz= 3.1

Cited by 317 publications

References 46 publications

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE∗

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

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UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗