Candidate Population III stellar complex at <i>z</i> = 6.629 in the MUSE Deep Lensed Field

Vanzella, E.; Meneghetti, M.; Caminha, G. B.; Castellano, M.; Calura, F.; Rosati, P.; Grillo, C.; Dijkstra, Mark; Grönke, Max; Sani, E.; Mercurio, A.; Tozzi, P.; Nonino, M.; Cristiani, S.; Mignoli, M.; Pentericci, L.; Gilli, R.; Treu, Tommaso; Caputi, K.; Cupani, G.; Fontana, A.; Grazian, A.; Balestra, I.

doi:10.1093/mnrasl/slaa041

Cited by 57 publications

(53 citation statements)

References 32 publications

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“…In the northern part, the MUSE data used in our analysis is much deeper and we find no discrepancy for the sources in common with (Caminha et al 2017a). Vanzella et al (2020b) present one source at z = 6.63 from the deep observations, which was also identified in our muselet catalogue. The deeper data provide us with additional redshifts (not used in previous published models) for 15 systems and 33 multiple images in that region, including 11 systems newly discovered with MUSE as faint Lyman-α emitters.…”

Section: Macs0416mentioning

confidence: 55%

“…Overall, the same strategy as for the GTO campaign has been followed for these observations, and were combined with GTO data when overlapping. Similarly, additional exposure time in the northern part of the FF cluster MACS0416 has been obtained as part of ESO programme 0100.A-0764 (PI: Vanzella, Vanzella et al 2020b), and combined with the GTO observations.…”

Section: Muse Archival Datamentioning

confidence: 99%

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An atlas of MUSE observations towards twelve massive lensing clusters

Richard

Claeyssens

Lagattuta

et al. 2021

A&A

113

131

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Context. Spectroscopic surveys of massive galaxy clusters reveal the properties of faint background galaxies thanks to the magnification provided by strong gravitational lensing. Aims. We present a systematic analysis of integral-field-spectroscopy observations of 12 massive clusters, conducted with the Multi Unit Spectroscopic Explorer (MUSE). All data were taken under very good seeing conditions (∼0″.6) in effective exposure times between two and 15 h per pointing, for a total of 125 h. Our observations cover a total solid angle of ∼23 arcmin2 in the direction of clusters, many of which were previously studied by the MAssive Clusters Survey, Frontier Fields (FFs), Grism Lens-Amplified Survey from Space and Cluster Lensing And Supernova survey with Hubble programmes. The achieved emission line detection limit at 5σ for a point source varies between (0.77–1.5) × 10−18 erg s−1 cm−2 at 7000 Å. Methods. We present our developed strategy to reduce these observational data, detect continuum sources and line emitters in the datacubes, and determine their redshifts. We constructed robust mass models for each cluster to further confirm our redshift measurements using strong-lensing constraints, and identified a total of 312 strongly lensed sources producing 939 multiple images. Results. The final redshift catalogues contain more than 3300 robust redshifts, of which 40% are for cluster members and ∼30% are for lensed Lyman-α emitters. Fourteen percent of all sources are line emitters that are not seen in the available HST images, even at the depth of the FFs (∼29 AB). We find that the magnification distribution of the lensed sources in the high-magnification regime (μ = 2–25) follows the theoretical expectation of N(z) ∝ μ−2. The quality of this dataset, number of lensed sources, and number of strong-lensing constraints enables detailed studies of the physical properties of both the lensing cluster and the background galaxies. The full data products from this work, including the datacubes, catalogues, extracted spectra, ancillary images, and mass models, are made available to the community.

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Section: Macs0416mentioning

confidence: 55%

Section: Muse Archival Datamentioning

confidence: 99%

An atlas of MUSE observations towards twelve massive lensing clusters

Richard

Claeyssens

Lagattuta

et al. 2021

A&A

113

131

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“…Additionally, ionizing radiation is similarly able to escape through these channels resulting in Lyα fluorescence off of infalling or nearby gas (see, e.g., Mas-Ribas & Dijkstra 2016). Such cavities are similarly suggested to induce Lyα and Lyman continuum escape in the rare class of Lyman continuum emitting galaxies observed at high redshifts (see, e.g., Shapley et al 2016;Vanzella et al 2016Vanzella et al , 2018Vanzella et al , 2020.…”

Section: Explaining the Lyα-uv Offsetsmentioning

confidence: 99%

The size and pervasiveness of Ly α–UV spatial offsets in star-forming galaxies at z ∼ 6

Lemaux

Fuller

Bradač

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We study the projected spatial offset between the ultraviolet continuum and Lyα emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Lyα properties of galaxies observed in slit spectroscopy. While we find that ∼40% of galaxies in our sample show significant projected spatial offsets ($|\Delta _{\rm {Ly}\alpha -\rm {UV}}|$), we find a relatively modest average projected offset of $|\widetilde{\Delta }_{\rm {Ly}\alpha -\rm {UV}}|$ = 0.61±0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10%, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $|\Delta _{\rm {Ly}\alpha -\rm {UV}}|$ with redshift. In our sample, UV-bright galaxies ($\widetilde{L_{UV}}/L^{\ast }_{UV}=0.67$) showed offsets a factor of three greater than their fainter counterparts ($\widetilde{L_{UV}}/L^{\ast }_{UV}=0.10$), 0.89±0.18 vs. 0.27±0.05 proper kpc, respectively. The presence of companion galaxies and early-stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Lyα fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Lyα flux due to offsets was quantified. It was found that the differential loss of Lyα photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (<0.4″). However, for the largest offsets, if they are mostly perpendicular to the slit major axis, slit losses were found to be extremely severe in cases where slit widths of ≤1″ were employed, such as those planned for James Webb Space Telescope/NIRSpec observations.

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“…Pop III stars are expected to have high LyC emissivity and may play a significant role in the early phase of reionization (e.g., Sokasian et al 2004). However, observational evidence for this stellar population is still inconclusive (e.g., Kashikawa et al 2012;Rydberg et al 2015;Vanzella et al 2020), and its characteristics, e.g., the initial mass function and the LyC emissivity, are unknown. Theoretically, Pop III star clusters can be formed even at z ∼ 2-3, depending on the efficiency of the IGM metalenrichment (e.g., Tornatore et al 2007;Johnson 2010;de Souza et al 2011).…”

Section: Surveys Of Pop Iii-dominated Galaxiesmentioning

confidence: 99%

“…The metal-free stellar population, the so-called Population III (Pop III) stars (e.g., Carlberg 1981), can be an important ionizing source, particularly in the early phase of the reionization process (e.g., Sokasian et al 2004). Because their characteristics, such as the initial mass function (IMF), are unknown observationally owing to the lack of information (Nagao et al 2005;Nagao et al 2008;Kashikawa et al 2012;Vanzella et al 2020), identifying Pop III clusters and revealing their nature are highly relevant to understanding their role in reionization.…”

Section: Introductionmentioning

confidence: 99%

CHORUS. I. Cosmic HydrOgen Reionization Unveiled with Subaru: Overview

Inoue

Yamanaka

Ouchi

et al. 2020

Publications of the Astronomical Society of Japan

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To determine the dominant sources for cosmic reionization, the evolution history of the global ionizing fraction, and the topology of the ionized regions, we have conducted a deep imaging survey using four narrow-band (NB) and one intermediate-band (IB) filters on the Subaru/Hyper Suprime-Cam (HSC), called Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS). The central wavelengths and full-widths-at-half-maximum of the CHORUS filters are, respectively, 386.2 nm and 5.5 nm for NB387, 526.0 nm and 7.9 nm for NB527, 717.1 nm and 11.1 nm for NB718, 946.2 nm and 33.0 nm for IB945, and 971.2 nm and 11.2 nm for NB973. This combination, including NB921 (921.5 nm and 13.5 nm) from the Subaru Strategic Program with HSC (HSC SSP), is carefully designed, as if they were playing a chorus, to observe multiple spectral features simultaneously, such as Lyman continuum, Lyα, C iv, and He ii for $z$ = 2–7. The observing field is the same as that of the deepest footprint of the HSC SSP in the COSMOS field and its effective area is about 1.6 deg2. We present an overview of the CHORUS project, which includes descriptions of the filter design philosophy, observations and data reduction, multiband photometric catalogs, assessments of the imaging quality, measurements of the number counts, and example use cases for the data. All the imaging data, photometric catalogs, masked pixel images, data of limiting magnitudes and point spread functions, results of completeness simulations, and source number counts are publicly available through the HSC SSP database.

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Candidate Population III stellar complex at z = 6.629 in the MUSE Deep Lensed Field

Cited by 57 publications

References 32 publications

An atlas of MUSE observations towards twelve massive lensing clusters

An atlas of MUSE observations towards twelve massive lensing clusters

The size and pervasiveness of Ly α–UV spatial offsets in star-forming galaxies at z ∼ 6

CHORUS. I. Cosmic HydrOgen Reionization Unveiled with Subaru: Overview

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