HIGH-RESOLUTION SPECTROSCOPY OF A YOUNG, LOW-METALLICITY OPTICALLY THIN L = 0.02L* STAR-FORMING GALAXY AT z = 3.12*

Vanzella, E.; Barros, S. de; Cupani, G.; Karman, W.; Grönke, Max; Balestra, I.; Coe, Dan; Mignoli, M.; Brusa, M.; Calura, F.; Caminha, G. B.; Caputi, K.; Castellano, M.; Christensen, L.; Comastri, A.; Cristiani, S.; Dijkstra, Mark; Fontana, A.; Giallongo, E.; Giavalisco, Mauro; Gilli, R.; Grazian, A.; Grillo, C.; Koekemoer, Anton M.; Meneghetti, M.; Nonino, M.; Pentericci, L.; Rosati, P.; Schaerer, D.; Verhamme, Anne; Vignali, C.; Zamorani, G.

doi:10.3847/2041-8205/821/2/l27

Cited by 115 publications

(195 citation statements)

References 48 publications

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“…We revisit here the physical size of the object at z = 3.1169 studied by Vanzella et al (2016a) and perform SED-fitting using the full depth HFF photometry. Among the sources presented in this work, this is the system with the highest signal-to-noise ratio in the HFF photometry (ranging between 20 and > 50 for the three multiple images).…”

Section: The Strongly Lensed Systemsmentioning

confidence: 99%

“…In this work we study five systems detected behind two Hubble Frontier fields at redshift 3.1169, 3.235 and three at 6.145 extracted from deep MUSE observations of Karman et al (2016), Vanzella et al (2016a) and Caminha et al (2016c). Specifically, we provide novel estimates for the size, dynamical mass and SED-fitting using the full-depth HFF photometry and near-infrared spectroscopy for the ob- Figure 1.…”

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confidence: 99%

“…A still open question concerns the nature of the objects belonging to this luminosity domain: are we dealing with dwarf galaxies (e.g., Finlator et al 2017), Hii galaxies (e.g., Terlevich et al 2016), super star-clusters, or extremely compact star clusters or clumps? (i.e., with sizes of the order of a few tens of parsec, Bouwens et al 2016b;Kawamata et al 2015;Livermore et al 2015;Vanzella et al 2016a;Ellis et al 2001). In order to answer this question, we need to derive a few basic physical quantities such as the stellar mass, the star-formation rate, as well as the size of these systems.…”

mentioning

confidence: 99%

“…High-precision lens models can be built using a large number of multiply lensed sources spanning a large redshift range, which however need to be spectrosopically identified with ground-based or HST grism observations (Treu et al 2015). In particular, in combination with the very efficient integral field spectrograph MUSE on the VLT (Bacon et al 2010) 1 , the identification and characterization of Lyman-α emitting galaxies near the flux limit of the Hubble imaging data, in lensed and blank fields, has become possible (e.g., Karman et al 2016;Caminha et al 2016c;Vanzella et al 2016a).…”

mentioning

confidence: 99%

“…ject at z = 3.1169 behind the galaxy cluster AS1063 (named ID11, also discussed in Vanzella et al (2016a); ). The redshift of the remaining four objects have been presented in Caminha et al (2016c) and used to constrain the lens model of MACS J0416.…”

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confidence: 99%

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Paving the way for the JWST: witnessing globular cluster formation at z > 3

Vanzella¹,

Calura²,

Meneghetti³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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173

213

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We report on five compact, extremely young (< 10 Myr) and blue (β U V < −2.5, F λ = λ β ) objects observed with VLT/MUSE at redshift 3.1169, 3.235, in addition to three objects at z = 6.145. These sources are magnified by the Hubble Frontier Field galaxy clusters MACS J0416 and AS1063. Their de-lensed half light radii (R e ) are between 16 to 140 pc, the stellar masses are 1 − 20 × 10 6 M , the magnitudes are m U V = 28.8 − 31.4 (−17 < M U V < −15) and specific star formation rates can be as large as ∼ 800 Gyr −1 . Multiple images of these systems are widely separated in the sky (up to 50 ) and individually magnified by factors 3-40. Remarkably, the inferred physical properties of two objects are similar to those expected in some globular cluster formation scenarios, representing the best candidate proto-globular clusters (proto-GC) discovered so far. Rest-frame optical high dispersion spectroscopy of one of them at z = 3.1169 yields a velocity dispersion σ v 20 km s −1 , implying a dynamical mass dominated by the stellar mass. Another object at z = 6.145, with de-lensed31.4), shows a stellar mass and a star-formation rate surface density consistent with the values expected from popular GC formation scenarios. An additional star-forming region at z = 6.145, with de-lensed m U V 32, a stellar mass of 0.5 ×10 6 M and a star formation rate of 0.06 M yr −1 is also identified. These objects currently represent the faintest spectroscopically confirmed star-forming systems at z > 3, elusive even in the deepest blank fields. We discuss how proto-GCs might contribute to the ionization budget of the universe and augment Lyα visibility during reionization. This work underlines the crucial role of JWST in characterizing the restframe optical and near-infrared properties of such low-luminosity high−z objects.

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Section: The Strongly Lensed Systemsmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Paving the way for the JWST: witnessing globular cluster formation at z > 3

Vanzella¹,

Calura²,

Meneghetti³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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173

213

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Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results

Eldridge

Stanway

Xiao

et al. 2017

Publ. Astron. Soc. Aust.

792

719

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The Binary Population and Spectral Synthesis (BPASS) suite of binary stellar evolution models and synthetic stellar populations provides a framework for the physically motivated analysis of both the integrated light from distant stellar populations and the detailed properties of those nearby. We present a new version 2.1 data release of these models, detailing the methodology by which BPASS incorporates binary mass transfer and its effect on stellar evolution pathways, as well as the construction of simple stellar populations. We demonstrate key tests of the latest BPASS model suite demonstrating its ability to reproduce the colours and derived properties of resolved stellar populations, including wellconstrained eclipsing binaries. We consider observational constraints on the ratio of massive star types and the distribution of stellar remnant masses. We describe the identification of supernova progenitors in our models, and demonstrate a good agreement to the properties of observed progenitors. We also test our models against photometric and spectroscopic observations of unresolved stellar populations, both in the local and distant Universe, finding that binary models provide a self-consistent explanation for observed galaxy properties across a broad redshift range. Finally, we carefully describe the limitations of our models, and areas where we expect to see significant improvement in future versions.

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Witnessing globular cluster formation at z ∼ 3–10 with JWST and ELT

Renzini

2019

Proc. IAU

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HIGH-RESOLUTION SPECTROSCOPY OF A YOUNG, LOW-METALLICITY OPTICALLY THIN L = 0.02L* STAR-FORMING GALAXY AT z = 3.12*

Cited by 115 publications

References 48 publications

Paving the way for the JWST: witnessing globular cluster formation at z > 3

Paving the way for the JWST: witnessing globular cluster formation at z > 3

Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results

Witnessing globular cluster formation at z ∼ 3–10 with JWST and ELT

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