PANORAMIC SURVEY OF Lyα EMITTERS AT<i>z</i>= 3.1

Yamada, Tohru; Nakamura, Yuki; Matsuda, Yoshihisa; Hayashino, T.; Yamauchi, Ryosuke; Morimoto, Naotake; Kousai, K.; Umemura, Masayuki

doi:10.1088/0004-6256/143/4/79

Cited by 88 publications

(172 citation statements)

References 72 publications

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“…Figure 5 shows the redshift distributions of the protocluster galaxies within this region. The number of the galaxies at 3.04 z spec 3.12 within this radius are 18 for our sample, 45 for the sample confirmed with optical spectroscopic observations (Steidel et al 2003;Lehmer et al 2009a;Matsuda et al 2005;Yamada et al 2012), and 60 for the combined sample where we use our own redshifts for the overlapping objects. The redshift selection functions for LBGs and the photo-z-selected galaxies are uniform at a redshift range from z = 3.04-3.12 while LAEs were nonuniformly selected in z = 3.062-3.125 and preferentially picked up around z ≈ 3.09 due to the narrowband selection shown in the middle panel of Figure 5.…”

Section: The Mass Of the Ssa22 Protoclustersupporting

confidence: 76%

“…Consequently, the region within 1.5 Mpc in physical (≈3.3 arcmin) from the density peak, indicated with the black large circle in Figure 1, was observed almost uniformly. This region is also uniformly covered with optical spectroscopic observations (Steidel et al 2003;Lehmer et al 2009a;Matsuda et al 2005;Yamada et al 2012). We here estimate the mass enclosed within this region.…”

Section: The Mass Of the Ssa22 Protoclustersupporting

confidence: 53%

“…Flux standard stars for the Notes. a Number of the galaxies confirmed with redshifts at 3.04 z spec 3.12. b Number of the galaxies confirmed with redshifts at z < 3.04 and z > 3.12. c Number of the LAEs selected with the narrow-band filter NB497, which is sensitive to the Lyα emission line at z = 3.062-3.125 Yamada et al 2012). The numbers in the brackets show the number of the galaxies with the BV − NB497 color excess above 4σ significance.…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

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NIR SPECTROSCOPIC OBSERVATION OF MASSIVE GALAXIES IN THE PROTOCLUSTER ATz= 3.09

Kubo

Yamada

Ichikawa

et al. 2015

ApJ

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We present the results of near-infrared spectroscopic observations of the K-band-selected candidate galaxies in the protocluster at z = 3.09 in the SSA22 field. We observed 67 candidates with K AB < 24 and confirmed redshifts of the 39 galaxies at 2.0 < z spec < 3.4. Of the 67 candidates, 24 are certainly protocluster members with 3.04 z spec 3.12, which are massive red galaxies that have been unidentified in previous optical observations of the SSA22 protocluster. Many distant red galaxies (J − K AB > 1.4), hyper extremely red objects (J − K AB > 2.1), Spitzer MIPS 24 μm sources, active galactic nuclei (AGNs) as well as the counterparts of Lyα blobs and the AzTEC/ASTE 1.1 mm sources in the SSA22 field are also found to be protocluster members. The mass of the SSA22 protocluster is estimated to be ∼2-5 × 10 14 M , and this system is plausibly a progenitor of the most massive clusters of galaxies in the current universe. The reddest (J − K AB 2.4) protocluster galaxies are massive galaxies with M star ∼ 10 11 M showing quiescent star formation activities and plausibly dominated by old stellar populations. Most of these massive quiescent galaxies host moderately luminous AGNs detected by X-ray. There are no significant differences in the [O iii] λ5007/Hβ emission line ratios and [O iii] λ5007 line widths and spatial extents of the protocluster galaxies from those of massive galaxies at z ∼ 2-3 in the general field.

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Section: The Mass Of the Ssa22 Protoclustersupporting

confidence: 76%

Section: The Mass Of the Ssa22 Protoclustersupporting

confidence: 53%

Section: Observations and Data Reductionsmentioning

confidence: 99%

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NIR SPECTROSCOPIC OBSERVATION OF MASSIVE GALAXIES IN THE PROTOCLUSTER ATz= 3.09

Kubo

Yamada

Ichikawa

et al. 2015

ApJ

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“…The protocluster has been traced over a 60 × 10 Mpc 2 (comoving) region using narrowband imaging at rest-frame Lyα wavelengths, which also reveals a significant overdensity of Lyα Emitters (LAEs; e.g. Hayashino et al 2004;Matsuda et al 2005;Yamada et al 2012a) and regions of extended ( 30 kpc) Lyα emission (often termed Lymanalpha blobs, LABs; e.g. Steidel et al 2000;Matsuda et al 2004;Yamada et al 2012a) when compared to the field.…”

mentioning

confidence: 99%

“…Hayashino et al 2004;Matsuda et al 2005;Yamada et al 2012a) and regions of extended ( 30 kpc) Lyα emission (often termed Lymanalpha blobs, LABs; e.g. Steidel et al 2000;Matsuda et al 2004;Yamada et al 2012a) when compared to the field. The SSA 22 protocluster therefore provides an ideal environment to test whether galaxy and BH growth is accelerated in a distant high-density environment.…”

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confidence: 99%

ALMA observations of az≈ 3.1 protocluster: star formation from active galactic nuclei and Lyman-alpha blobs in an overdense environment

Alexander

Simpson

Harrison

et al. 2016

Mon. Not. R. Astron. Soc.

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We exploit ALMA 870 µm observations to measure the star-formation rates (SFRs) of eight X-ray detected Active Galactic Nuclei (AGNs) in a z ≈ 3.1 protocluster, four of which reside in extended Ly α haloes (often termed Ly α blobs: LABs). Three of the AGNs are detected by ALMA and have implied SFRs of ≈ 220-410 M yr −1 ; the non detection of the other five AGNs places SFR upper limits of < ∼ 210 M yr −1 . The mean SFR of the protocluster AGNs (≈ 110-210 M yr −1 ) is consistent (within a factor of ≈ 0.7-2.3) with that found for co-eval AGNs in the field, implying that the galaxy growth is not significantly accelerated in these systems. However, when also considering ALMA data from the literature, we find evidence for elevated mean SFRs (up-to a factor of ≈ 5.9 over the field) for AGNs at the protocluster core, indicating that galaxy growth is significantly accelerated in the central regions of the protocluster. We also show that all of the four protocluster LABs are associated with an ALMA counterpart within the extent of their Ly α emission. The SFRs of the ALMA sources within the LABs (≈ 150-410 M yr −1 ) are consistent with those expected for co-eval massive star-forming galaxies in the field. Furthermore, the two giant LABs (with physical extents of > ∼ 100 kpc) do not host more luminous star formation than the smaller LABs, despite being an order of magnitude brighter in Ly α emission. We use these results to discuss star formation as the power source of LABs.

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Observations of Ly$$\alpha $$ Emitters at High Redshift

Ouchi

2019

Lyman-Alpha as an Astrophysical and Cosmological Tool

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In this series of lectures, I review our observational understanding of highz Lyα emitters (LAEs) and relevant scientific topics. Since the discovery of LAEs in the late 1990s, significant progresses in LAE studies have been made over the past two decades by deep multi-wavelength observations. More than ten (one) thousand(s) of LAEs have been identified photometrically (spectroscopically) in optical and near-infrared data, and the redshifts of these LAEs range from z ∼ 0 to z ∼ 10. These large samples of LAEs are useful to address two major astrophysical issues, galaxy formation and cosmic reionization. Statistical studies have revealed the general picture of LAEs' physical properties: young stellar populations, remarkable luminosity function evolutions, compact morphologies, highly ionized inter-stellar media (ISM) with low metal/dust contents, low masses of dark-matter halos. Typical LAEs represent low-mass high-z galaxies, high-z analogs of dwarf galaxies, some of which are thought to be candidates of population III galaxies. These observational studies have also pinpointed rare bright Lyα sources extended over ∼ 10 − 100 kpc, dubbed Lyα blobs, whose physical origins are under debate. LAEs are used as probes of cosmic reionization history through the Lyα damping wing absorption given by the neutral hydrogen of the inter-galactic medium (IGM), which complement the cosmic microwave background radiation and 21cm observations targeting the epoch of reionization. The low-mass and highly-ionized population of LAEs can be major sources of cosmic reionization, and physical parameters including the ionizing photon escape fraction have been extensively investigated. The budget of ionizing photons for cosmic reionization has been constrained, although there remain large observational uncertainties in the parameters. Beyond these two established topics of LAEs, galaxy formation and cosmic reionization, several new usages of LAEs for science frontiers have been suggested such as the distribution of HI gas in the circum-galactic medium and filaments of large-scale structures. Ongoing 10 mclass optical telescope programs and future telescope projects, such as JWST, ELTs,

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PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

Cited by 88 publications

References 72 publications

NIR SPECTROSCOPIC OBSERVATION OF MASSIVE GALAXIES IN THE PROTOCLUSTER ATz= 3.09

NIR SPECTROSCOPIC OBSERVATION OF MASSIVE GALAXIES IN THE PROTOCLUSTER ATz= 3.09

ALMA observations of az≈ 3.1 protocluster: star formation from active galactic nuclei and Lyman-alpha blobs in an overdense environment

Observations of Ly$$\alpha $$ Emitters at High Redshift

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