A Search for Population Iii Galaxies in Clash. I. Singly Imaged Candidates at High Redshift

Rydberg, Claes-Erik; Zackrisson, Erik; Zitrin, Adi; Guaita, L.; Melinder, Jens; Asadi, Saghar; Gonzalez, J. E.; Östlin, Göran; Strom, T.

doi:10.1088/0004-637x/804/1/13

Cited by 10 publications

(15 citation statements)

References 92 publications

(109 reference statements)

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“…Estimates of Cluster Caustic Transits for Pop III stars: To estimate the caustic transit rate and duration for Pop III stars, we first need to evaluate the plausible limits to the transverse velocities of massive lensing clusters, their typical caustic lengths, and the possible effects from microlensing. A Pop III caustictransit observing program with JWST should select the best lensing clusters with matching prior HST/ACS and WFC3 images, such as the Hubble Frontier Field clusters (HFF; e.g., Lotz et al 2017;Kawamata et al 2016;Lagattuta et al 2017;Acebron et al 2017;Mahler et al 2018) or the CLASH clusters (e.g., Postman et al 2012;Rydberg et al 2015). Given the significant differences in the allowed v T -values between the three HFF clusters discussed in W18, we adopt an upper limit of V T , s < ∼ 1000 km s −1 .…”

Section: B Luminosity Density From Pop III Star Mass-luminosity Relmentioning

confidence: 99%

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

Windhorst

Alpaslan

Andrews

et al. 2018

ApJS

112

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Recent near-infrared power-spectra and panchromatic Extragalactic Background Light (EBL) measurements provide upper limits on the integrated near-infrared surface brightness (SB > ∼ 31mag arcsec −2 at 2µm) that may come from Population III (Pop III) stars and possible accretion disks around resulting stellar-mass black holes (BHs) in the epoch of First Light, broadly taken from z 7-17. Physical parameters for zero metallicity Pop III stars at z > ∼ 7 can be estimated from MESA stellar evolution models through helium-depletion, and for BH accretion disks from quasar microlensing results and multicolor accretion models. Second-generation non-zero metallicity stars can form at higher multiplicity, so that BH accretion disks may be fed by Roche-lobe overflow from lower-mass companions in their AGB stage. The near-infrared SB constraints can be used to calculate the number of caustic transits behind lensing clusters that the James Webb Space Telescope (JWST) and the next generation 25-39 m ground-based telescopes may detect for both Pop III stars and stellar mass BH accretion disks. Because Pop III stars and stellar mass BH accretion disks have sizes of a few×10 −11 arcsec at z > ∼ 7, typical caustic magnifications can be µ 10 4 -10 5 , with rise times of hours and decline times of < ∼ 1 year for cluster transverse velocities of v T < ∼ 1000 km s −1 . Microlensing by intracluster medium objects can modify transit magnifications, and lengthen visibility times. Depending on BH masses, accretion-disk radii and feeding efficiencies, stellar-mass BH accretion-disk caustic transits could outnumber those from Pop III stars. To observe Pop III caustic transits directly may require monitoring 3-30 lensing clusters to AB < ∼ 29 mag over a decade or more. Such a program must be started with JWST at the start of Cycle 1, and -depending on the role of microlensing in the Intra Cluster Light (ICL) -should be continued for decades with the next generation 25-39 m ground-based telescopes, where both JWST and the ground-based facilities each will play a unique and strongly complementary role.

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Section: B Luminosity Density From Pop III Star Mass-luminosity Relmentioning

confidence: 99%

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

Windhorst

Alpaslan

Andrews

et al. 2018

ApJS

112

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“…The method, described in more detail in Rydberg et al (2015), uses χ 2 as well as crossvalidation (see Singh 1981) to fit the observational data to the four different model grids (Section 3). The χ 2 -fitting was carried out with the publicly available Le Phare (Ilbert et al 2006) code while cross-validation was done with a program we developed called Observational Data Scanner (ODS).…”

Section: Resultsmentioning

confidence: 99%

“…the photometricredshift distribution and the photometric-fLyα distribution, are calculated using the cross-validation technique described in Rydberg et al (2015). For each z or fLyα, the model (for the considered grid) with the highest cross-validation value (i.e.…”

Section: Extremely Strong Optical Emission Lines (Such As [O Iii]mentioning

confidence: 99%

“…Zheng et al 2012;Coe et al 2013;Bradley et al 2014;Vanzella et al 2014). In a companion paper (Rydberg et al 2015) we presented a search for Pop III LAE candidates at z 6 in CLASH, which resulted in two singly-imaged candidates with best-fitting redshifts at z ≈ 8. These candidatesif confirmed spectroscopically -might like the aforementioned Roberts-Borsani objects be the highest-redshift extreme LAEs detected so far.…”

Section: Introductionmentioning

confidence: 99%

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A Multiply-Imaged z ∼ 6.3 Lyman Alpha Emitter candidate behind Abell 2261

Rydberg

Zitrin

Zackrisson

et al. 2017

Mon. Not. R. Astron. Soc.

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While the Lyman-α (Lyα) emission line serves as an important tool in the study of galaxies at z 6, finding Lyα emitters (LAE) at significantly higher redshifts has been more challenging, probably because of the increasing neutrality of the intergalactic medium above z ∼ 6. Galaxies with extremely high rest-frame Lyα equivalent widths, EW(Lyα) 150Å, at z > 6 are good candidates for Lyα follow-up observations, and can stand out in multiband imaging surveys because of their unusual colors. We have conducted a photometric search for such objects in the Cluster Lensing And Supernova survey with Hubble (CLASH), and report here the identification of three likely gravitationally-lensed images of a single LAE candidate at z ∼ 6.3, behind the galaxy cluster Abell 2261 (z = 0.225). In the process, we also measured with Keck/MOSFIRE the first spectroscopic redshift of a multiply-imaged galaxy behind Abell 2261, at z = 3.337. This allows us to calibrate the lensing model, which in turn is used to study the properties of the candidate LAE. Population III galaxy spectral energy distribution (SED) model fits to the CLASH broadband photometry of the possible LAE provide a slightly better fit than Population I/II models. The best fitted model suggests intrinsic EW(Lyα) ≈ 160Å after absorption in the interstellar and intergalactic medium. Future spectroscopic observations will examine this prediction as well as shed more light on the morphology of this object, which indicates it may be a merger of two smaller galaxies.

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“…8 Short of relying on gravitational lensing to magnify the light from less massive Pop III clusters (e.g. Rydberg et al 2015;Windhorst 8 The number density of DCBH seeds in general and of DCBH seeds formed in halos irradiated by quasars at high redshift is not well-constrained, in part due to its sensitive dependence on the radiative flux required for their formation (e.g. Habouzit et al 2016 Frost et al 2009;de Souza et al 2014;Hartwig et al 2018), this is perhaps the most promising strategy for finding Pop III stars with the JWST.…”

Section: Detectability and Search Strategymentioning

confidence: 99%

Extreme Primordial Star Formation Enabled by High-redshift Quasars

Johnson

Aykutalp

2019

ApJ

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High redshift quasars emit copious X-ray photons which heat the intergalactic medium to temperatures up to ∼ 10 6 K. At such high temperatures the primordial gas will not form stars until it is assembled into dark matter haloes with masses of up to ∼ 10 11 M ⊙ , at which point the hot gas collapses and cools under the influence of gravity. Once this occurs, there is a massive reservoir of primordial gas from which stars can form, potentially setting the stage for the brightest Population (Pop) III starbursts in the early Universe. Supporting this scenario, recent observations of quasars at z ∼ 6 have revealed a lack of accompanying Lyman α emitting galaxies, consistent with suppression of primordial star formation in haloes with masses below ∼ 10 10 M ⊙ . Here we model the chemical and thermal evolution of the primordial gas as it collapses into such a massive halo irradiated by a nearby quasar in the run-up to a massive Pop III starburst. We find that within ∼ 100 kpc of the highest redshift quasars discovered to date the Lyman-Werner flux produced in the quasar host galaxy may be high enough to stimulate the formation of a direct collapse black hole (DCBH). A survey with single pointings of the NIRCam instrument at individual known high-z quasars may be a promising strategy for finding Pop III stars and DCBHs with the James Webb Space Telescope.

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A Search for Population Iii Galaxies in Clash. I. Singly Imaged Candidates at High Redshift

Cited by 10 publications

References 92 publications

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

A Multiply-Imaged z ∼ 6.3 Lyman Alpha Emitter candidate behind Abell 2261

Extreme Primordial Star Formation Enabled by High-redshift Quasars

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