Detection of an oxygen emission line from a high-redshift galaxy in the reionization epoch

Inoue, Akio; Tamura, Motohide; Matsuo, Hiroshi; Mawatari, Ken; Shimizu, Ikkoh; Shibuya, Tetsuo; Ota, Kazuaki; Yoshida, Naoki; Zackrisson, Erik; Kashikawa, Nobunari; Kohno, Kotaro; Umehata, Hideki; Hatsukade, Bunyo; Iye, Masanori; Matsuda, Yoshihisa; Okamoto, Takashi; Yamaguchi, Yuki

doi:10.1126/science.aaf0714

Cited by 242 publications

(357 citation statements)

References 69 publications

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“…In Figure 6 we summarise spectral and spatial offset from literature studies observing SMG (SFR>1000 M yr −1 ) z >4 De Breuck et al 2014) and primeval galaxies with SFR< 100 M yr −1 and z>4 (Mallery et al 2012;Carilli et al 2013;Williams et al 2014;Maiolino et al 2015;Willott et al 2015;Capak et al 2015;Knudsen et al 2016Knudsen et al , 2017Pentericci et al 2016;Inoue et al 2016;Bradač et al 2017). Since this work does not focus on determining a correlation between the offsets and the galaxy properties, we also report the positional offset revealed in in high-z galaxies whose redshifts have not been spectroscopically confirmed in the optical yet ).…”

Section: Spatial and Spectral Offsetsmentioning

confidence: 99%

“…However, such offsets (either spatial, in velocity, or both) are also seen in some high-z SMG galaxies Decarli et al 2014;Pavesi et al 2016). Recent ALMA observations have revealed spatial and spectral offsets between FIR-lines, such as [Cii] and [Oiii], and optical emission (Willott et al 2015;Capak et al 2015;Inoue et al 2016;Knudsen et al 2016) also in normal high-redshift galaxies (z > 5), with modest SFR (< 100 M yr −1 ). Therefore, BDF − 3299 may not be a rare case.…”

Section: Spatial and Spectral Offsetsmentioning

confidence: 99%

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Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

190

237

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We present new ALMA observations of the [Oiii]88µm line and high angular resolution observations of the [Cii]158µm line in a normal star forming galaxy at z=7.1. Previous [Cii] observations of this galaxy had detected [Cii] emission consistent with the Lyα redshift but spatially slightly offset relative to the optical (UV-rest frame) emission. The new [Cii] observations reveal that the [Cii] emission is partly clumpy and partly diffuse on scales larger than about 1kpc.[Oiii] emission is also detected at high significance, offset relative to the optical counterpart in the same direction as the [Cii] clumps, but mostly not overlapping with the bulk of the [Cii] emission. The offset between different emission components (optical/UV and different far-IR tracers) is similar to that which is observed in much more powerful starbursts at high redshift. We show that the [Oiii] emitting clump cannot be explained in terms of diffuse gas excited by the UV radiation emitted by the optical galaxy, but it requires excitation by in-situ (slightly dust obscured) star formation, at a rate of about 7 M yr −1 . Within 20 kpc from the optical galaxy the ALMA data reveal two additional [Oiii] emitting systems, which must be star forming companions. We discuss that the complex properties revealed by ALMA in the z∼7.1 galaxy are consistent with expectations by recent models and cosmological simulations, in which differential dust extinction, differential excitation and different metal enrichment levels, associated with different subsystems assembling a galaxy, are responsible for the various appearance of the system when observed with distinct tracers.

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Section: Spatial and Spectral Offsetsmentioning

confidence: 99%

Section: Spatial and Spectral Offsetsmentioning

confidence: 99%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

190

237

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“…The difference with respect to the C IV and O III] FWHM is not surprising given the reprocessing of the line profile by the CGM and surrounding IGM. Including RXC J2248-ID3, there are now 11 > z 6 galaxies with Lyα profile and velocity offset measurements (see Figure 3( (Willott et al 2015;Bradač et al 2016;Inoue et al 2016;Pentericci et al 2016) or UV metal line detections (Stark et al 2015a(Stark et al , 2017 constrain the systemic redshift. We discuss trends with M UV and implications for the escape of Lyα from reionization-era galaxies in Section 4.…”

Section: Lymentioning

confidence: 99%

“…Deep near-infrared spectroscopy has revealed strong UV metal line emission in galaxies at = z 6 8 -with equivalent widths 5-10×larger than are typical at  z 2 (Stark et al 2015a(Stark et al , 2015b(Stark et al , 2017, while ALMA observations have begun to deliver detections of [C II] 158 μm and [O III] 88 μm emission in typical galaxies at > z 6 (Willott et al 2015;Bradač et al 2016;Inoue et al 2016;Pentericci et al 2016). Perhaps the most surprising result is the discovery of nebular C IVll1548, 1550 in a galaxy at z=7.045 (Stark et al 2015b), requiring an extremely hard radiation field capable of producing a large number of photons more energetic than 47.9 eV.…”

Section: Introductionmentioning

confidence: 99%

Evidence for a Hard Ionizing Spectrum from a z = 6.11 Stellar Population

Mainali¹,

Kollmeier

Stark³

et al. 2017

ApJL

135

219

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We present the Magellan/FIRE detection of highly ionized C IVλ1550 and O III]λ1666 in a deep infrared spectrum of the z=6.11 gravitationally lensed low-mass galaxy RXC J2248.7-4431-ID3, which has previously known Lyα. No corresponding emission is detected at the expected location of He IIλ1640. The upper limit on He II, paired with detection of O III] and C IV, constrains possible ionization scenarios. Production of C IV and O III] requires ionizing photons of 2.5-3.5 Ryd, but once in that state their multiplet emission is powered by collisional excitation at lower energies (∼0.5 Ryd). As a pure recombination line, He II emission is powered by 4 Ryd ionizing photons. The data therefore require a spectrum with significant power at 3.5 Ryd but a rapid drop toward 4.0 Ryd. This hard spectrum with a steep drop is characteristic of low-metallicity stellar populations, and less consistent with soft AGN excitation, which features more 4 Ryd photons and hence higher He II flux. The conclusions based on ratios of metal line detections to helium non-detection are strengthened if the gas metallicity is low. RXJ2248-ID3 adds to the growing handful of reionization-era galaxies with UV emission line ratios distinct from the general = z 2 3 -population in a way that suggests hard ionizing spectra that do not necessarily originate in AGNs.

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“…Recently, the Atacama Large Millimeter/ submillimeter Array (ALMA) has opened a new window, allowing us to exploit fine structure lines at rest-frame farinfrared (FIR) wavelengths to diagnose the ISM properties for these galaxy populations (e.g., Nagao et al 2012;Decarli et al 2014;Inoue et al 2016). The [C II]158 μm (  P P 2 3 2 2 1 2 ) is known to be the dominant coolant of the ISM and one of the brightest lines from star-forming galaxies in the FIR (e.g., Israel et al 1996).…”

Section: Introductionmentioning

confidence: 99%

ALMA Reveals Strong Emission in a Galaxy Embedded in a Giant Lyα Blob at z = 3.1

Umehata

Matsuda

Tamura

et al. 2017

ApJL

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe report the result from observations conducted with the Atacama Large Millimeter/submillimeter Array (ALMA) to detect [C II] 158 μm fine structure line emission from galaxies embedded in one of the most spectacular Lyα blobs (LABs) at z = 3.1, SSA22-LAB1. Of three dusty star-forming galaxies previously discovered by ALMA 860 μm dust continuum survey toward SSA22-LAB1, we detected the [C II] line from one, LAB1-ALMA3 at z = 3.0993±0.0004. No line emission was detected, associated with the other ALMA continuum sources or from three rest-frame UV/optical selected z spec ;3.1 galaxies within the field of view. For LAB1-ALMA3, we find relatively bright [C II] emission compared to the infrared luminosity (L emission could be causally related to the location within the giant LAB, although the relationship between extended Lyα emission and interstellar medium conditions of associated galaxies is yet to be understand.

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Detection of an oxygen emission line from a high-redshift galaxy in the reionization epoch

Cited by 242 publications

References 69 publications

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Evidence for a Hard Ionizing Spectrum from a z = 6.11 Stellar Population

ALMA Reveals Strong Emission in a Galaxy Embedded in a Giant Lyα Blob at z = 3.1

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