Upper limits on the mass and luminosity of Population III-dominated galaxies

Yajima, Hidenobu; Khochfar, Sadegh

doi:10.1093/mnrasl/slw249

Cited by 25 publications

(18 citation statements)

References 47 publications

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“…We analyze halos with masses down to M G = 4.62 × 10 7 M that consist of approximately 330 DM particles. Taken as whole, we see that Pop III galaxies are not very massive and are comparable to the theoretical limits, 1.5 × 10 8 M to 1.1 × 10 9 M , discussed in Yajima & Khochfar (2017) for z = 7. The most massive Pop III-dominated galaxies in our simulation occur at z = 9 and 10, before reionization.…”

Section: The Galaxy Mass-metallicity Relationsupporting

confidence: 82%

Following the Cosmic Evolution of Pristine Gas. II. The Search for Pop III–bright Galaxies

Sarmento

Scannapieco

Cohen

2018

ApJ

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Direct observational searches for Population III (Pop III) stars at high redshift are faced with the question of how to select the most promising targets for spectroscopic follow-up. To help answer this, we use a large-scale cosmological simulation, augmented with a new subgrid model that tracks the fraction of pristine gas, to follow the evolution of high-redshift galaxies and the Pop III stars they contain. We generate rest-frame ultraviolet (UV) luminosity functions for our galaxies and find that they are consistent with current z ≥ 7 observations. Throughout the redshift range 7 ≤ z ≤ 15 we identify "Pop III-bright" galaxies as those with at least 75% of their flux coming from Pop III stars. While less than 1% of galaxies brighter than m UV,AB = 31.4 mag are Pop III-bright in the range 7 ≤ z ≤ 8, roughly 17% of such galaxies are Pop III-bright at z = 9, immediately before reionization occurs in our simulation. Moving to z = 10, m UV,AB = 31.4 mag corresponds to larger, more luminous galaxies and the Pop III-bright fraction falls off to 5%. Finally, at the highest redshifts, a large fraction (29% at z = 14 and 41% at z = 15) of all galaxies are Pop III-bright regardless of magnitude. While m UV,AB = 31.4 mag galaxies are extremely rare during this epoch, we find that 13% of galaxies at z = 14 are Pop III-bright with m UV,AB ≤ 33 mag, an intrisic magnitude within reach of the James Webb Space Telescope using lensing. Thus, we predict that the best redshift to search for luminous Pop III-bright galaxies is just before reionization, while lensing surveys for fainter galaxies should push to the highest redshifts possible.

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Section: The Galaxy Mass-metallicity Relationsupporting

confidence: 82%

Following the Cosmic Evolution of Pristine Gas. II. The Search for Pop III–bright Galaxies

Sarmento

Scannapieco

Cohen

2018

ApJ

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“…There is a possibility that strong UV radiation from Pop III stellar populations enhance the Lyα luminosity (e.g., Schaerer 2002). In our deep NIR spectroscopy, we find that there are no detections of He II emission line from CR7, Himiko, nor our 7 bright LAEs which are observed with NIR Yajima & Khochfar (2017), Pop III-dominated galaxies at z ≃ 7 have a Lyα luminosity of LLyα ≃ 3.0 × 10 42 − 2.1 × 10 43 erg s −1 which is slightly lower than that of our bright LAEs. However, we cannot obtain the conclusion that Pop III stellar populations exist in bright LAEs from the current data of He II measurements.…”

Section: Properties Of Bright Laes At Z ≃mentioning

confidence: 52%

SILVERRUSH. III. Deep optical and near-infrared spectroscopy for Lyα and UV-nebular lines of bright Lyα emitters at z = 6–7

Shibuya

Ouchi

Harikane

et al. 2017

Publications of the Astronomical Society of Japan

138

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We present Lyα and UV-nebular emission line properties of bright Lyα emitters (LAEs) at z = 6 − 7 with a luminosity of log L Lyα /[erg s −1 ] = 43 − 44 identified in the 21-deg 2 area of the SILVERRUSH early sample developed with the Subaru Hyper Suprime-Cam (HSC) survey data. Our optical spectroscopy newly confirm 21 bright LAEs with clear Lyα emission, and contribute to make a spectroscopic sample of 96 LAEs at z = 6 − 7 in SILVERRUSH. From the spectroscopic sample, we select 7 remarkable LAEs as bright as Himiko and CR7 objects, and perform deep Keck/MOSFIRE and Subaru/nuMOIRCS near-infrared spectroscopy reaching the 3σ-flux limit of ∼ 2 × 10 −18 erg s −1 for the UV-nebular emission lines of He IIλ1640, C IVλλ1548, 1550, and O III]λλ1661, 1666. Except for one tentative detection of C IV, we find no strong UV-nebular lines down to the flux limit, placing the upper limits of the rest-frame equivalent widths (EW 0 ) of ∼ 2 − 4Å for C IV, He II, and O III] lines. Here we also investigate the VLT/X-SHOOTER spectrum of CR7 whose 6σ detection of He II is claimed by Sobral et al.Although two individuals and the ESO-archive service carefully re-analyze the X-SHOOTER data that are used in the study of Sobral et al., no He II signal of CR7 is detected, supportive of weak UV-nebular lines of the bright LAEs even for CR7. Spectral properties of these bright LAEs are thus clearly different from those of faint dropouts at z ∼ 7 that have strong UV-nebular lines shown in the various studies. Comparing these bright LAEs and the faint dropouts, we find anti-correlations between the UV-nebular line EW 0 and UV-continuum luminosity, which are similar to those found at z ∼ 2 − 3.

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“…Smidt et al (2016) demonstrated, using Enzo (Bryan et al 2014) and radiative transfer in post-processing, that an AGN powered by a black hole of mass 3 × 10 7 M accreting at f Edd = 0.25-0.9 can account for the observations. Additional radiative processes have been suggested to prevent pristine gas from collapsing for long enough to accumulate the required high masses, but it is challenging to reproduce the required 10 7 M of Pop III stars (Xu et al 2016;Visbal et al 2016;Yajima & Khochfar 2017).…”

Section: What Have We Learned From Cr7?mentioning

confidence: 99%

Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes

Woods

Agarwal²,

Bromm

et al. 2019

Publ. Astron. Soc. Aust.

162

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In recent years, the discovery of massive quasars at $z\sim7$ has provided a striking challenge to our understanding of the origin and growth of supermassive black holes in the early Universe. Mounting observational and theoretical evidence indicates the viability of massive seeds, formed by the collapse of supermassive stars, as a progenitor model for such early, massive accreting black holes. Although considerable progress has been made in our theoretical understanding, many questions remain regarding how (and how often) such objects may form, how they live and die, and how next generation observatories may yield new insight into the origin of these primordial titans. This review focusses on our present understanding of this remarkable formation scenario, based on the discussions held at the Monash Prato Centre from November 20 to 24, 2017, during the workshop ‘Titans of the Early Universe: The Origin of the First Supermassive Black Holes’.

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Upper limits on the mass and luminosity of Population III-dominated galaxies

Cited by 25 publications

References 47 publications

Following the Cosmic Evolution of Pristine Gas. II. The Search for Pop III–bright Galaxies

Following the Cosmic Evolution of Pristine Gas. II. The Search for Pop III–bright Galaxies

SILVERRUSH. III. Deep optical and near-infrared spectroscopy for Lyα and UV-nebular lines of bright Lyα emitters at z = 6–7

Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes

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