The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at <i>z</i> = 3

Matsuda, Yoshihisa; Yamada, Tohru; Hayashino, T.; Yamauchi, Ryosuke; Nakamura, Yuki; Morimoto, Naotake; Ouchi, Masami; Ono, Yoshiyasu; Kousai, K.; Nakamura, Etsuko; Horie, Masaaki; Fujii, Takeshi; Umemura, Masayuki; Mori, Masao

doi:10.1111/j.1745-3933.2010.00969.x

Cited by 132 publications

(180 citation statements)

References 62 publications

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“…The number of known LABs is still not very large. For example, a narrow-band imaging survey with the Subaru/Suprime-Cam revealed 14 LAB candidates with a mayor axis diameter larger than 100 kpc (Matsuda et al 2011). Their shapes range from circular to filamentary.…”

Section: The Cosmic Web In Emissionmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

178

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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Section: The Cosmic Web In Emissionmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

178

130

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“…This strong absorption has also been observed using Keck/HIRES , which confirmed that this absorption is consistent with the superposition of the intergalactic Lyα forest rather than LLSs or DLAs. In the upper right panel, we present an absorption system at similar redshift as the galaxy overdensity (z = 3.09), with an effective optical depth on 15 h Giant Lyα nebulae (also known as Lyα blobs, LABs) are characterized by a high luminosity of the Lyα line emission (L (Lyα)10 43 erg s −1 ) and a spatially large Lyα emitting region from tens of kiloparsec (kpc) up to intergalactic scales of hundreds of kpc (e.g., Matsuda et al 2005Matsuda et al , 2011Yang et al 2009Yang et al , 2010Yang et al , 2014. Previous studies suggest that LABs are strongly clustered sources.…”

Section: Ssa22 Protocluster At Z = 31mentioning

confidence: 99%

Mapping the Most Massive Overdensity Through Hydrogen (Mammoth). I. Methodology

Cai

Fan

Peirani

et al. 2016

ApJ

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Modern cosmology predicts that a galaxy overdensity (e.g., protocluster) will be associated with a large intergalactic medium gas reservoir, which can be traced by Lyα forest absorption. We have undertaken a systematic study of the relation between Coherently Strong intergalactic Lyα Absorption systems (CoSLAs), which have the highest optical depth (τ) in the τ distribution, and mass overdensities on the scales of ∼10-20 h −1 comoving Mpc. On such large scales, our cosmological simulations show a strong correlation between the effective optical depth (τ eff ) of the CoSLAs and the three-dimensional mass overdensity. In spectra with moderate signal-tonoise ratio, however, the profiles of CoSLAs can be confused with individual high column density absorbers. For z>2.6, where the corresponding Lyβ is redshifted to the optical, we have developed a selection technique to distinguish between these two alternatives. We have applied this technique to ∼6000 sight lines provided by Sloan Digital Sky Survey III quasar survey at z = 2.6-3.3 with a continuum-to-noise ratio greater than 8, and we present a sample of five CoSLA candidates with τ eff on 15 h −1 Mpc greater than 4.5× the mean optical depth. At lower redshifts of z<2.6, where the background quasar density is higher, the overdensity can be traced by intergalactic absorption groups using multiple sight lines with small angular separations. Our overdensity searches fully use the current and next generation of Lyα forest surveys, which cover a survey volume of >1 (h −1 Gpc) 3 . Systems traced by CoSLAs will yield a uniform sample of the most massive overdensities at z>2 to provide stringent constraints to models of structure formation.

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“…When studied in detail, these systems show complex morphologies, obscured active galactic nuclei (AGNs), and/or associated star-forming galaxies (e.g., Francis et al 1996;Ivison et al 1998;Steidel et al 2000;Palunas et al 2004;Chapman et al 2004;Matsuda et al 2004Matsuda et al , 2007Basu-Zych & Scharf 2004;Dey et al 2005;Geach et al 2007;Smith et al 2008;Prescott et al 2009;Ouchi et al 2009;Yang et al 2011). There is strong evidence that the largest Lyα nebulae are rare (Saito et al 2006;Yang et al 2009Yang et al , 2010Prescott 2009;Matsuda et al 2011) and typically reside in the most overdense regions of the universe (e.g., Palunas et al 2004;Matsuda et al 2004Matsuda et al , 2005Matsuda et al , 2009Saito et al 2006;Prescott et al 2008;Yang et al 2009). …”

Section: Introductionmentioning

confidence: 99%

RESOLVING THE GALAXIES WITHIN A GIANT Lyα NEBULA: WITNESSING THE FORMATION OF A GALAXY GROUP?

Prescott

Dey

Brodwin

et al. 2012

ApJ

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Detailed analysis of the substructure of Lyα nebulae can put important constraints on the physical mechanisms at work and the properties of galaxies forming within them. Using high-resolution Hubble Space Telescope (HST) imaging of a Lyα nebula at z ≈ 2.656, we have taken a census of the compact galaxies in the vicinity, used optical/near-infrared colors to select system members, and put constraints on the morphology of the spatially extended emission. The system is characterized by (1) a population of compact, low-luminosity (∼0.1 L * ) sources-17 primarily young, small (R e ≈ 1-2 kpc), disky galaxies including an obscured active galactic nucleus-that are all substantially offset ( 20 kpc) from the line-emitting nebula; (2) the lack of a central galaxy at or near the peak of the Lyα emission; and (3) several nearly coincident, spatially extended emission components-Lyα, He ii, and UV continuum-that are extremely smooth. These morphological findings are difficult to reconcile with theoretical models that invoke outflows, cold flows, or resonant scattering, suggesting that while all of these physical phenomena may be occurring, they are not sufficient to explain the powering and large extent of Lyα nebulae. In addition, although the compact galaxies within the system are irrelevant as power sources, the region is significantly overdense relative to the field galaxy population (by at least a factor of four). These observations provide the first estimate of the luminosity function of galaxies within an individual Lyα nebula system and suggest that large Lyα nebulae may be the seeds of galaxy groups or low-mass clusters.

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The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

Cited by 132 publications

References 62 publications

Star formation sustained by gas accretion

Star formation sustained by gas accretion

Mapping the Most Massive Overdensity Through Hydrogen (Mammoth). I. Methodology

RESOLVING THE GALAXIES WITHIN A GIANT Lyα NEBULA: WITNESSING THE FORMATION OF A GALAXY GROUP?

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