A core in a star-forming disc as evidence of inside-out growth in the early Universe

Baker, William M.; Tacchella, Sandro; Johnson, Benjamin D.; Nelson, Erica; Suess, Katherine A.; D’Eugenio, Francesco; Curti, Mirko; de Graaff, Anna; Ji, Zhiyuan; Maiolino, Roberto; Robertson, Brant; Scholtz, Jan; Alberts, Stacey; Arribas, Santiago; Boyett, Kristan; Bunker, Andrew J.; Carniani, Stefano; Charlot, Stephane; Chen, Zuyi; Chevallard, Jacopo; Curtis-Lake, Emma; Danhaive, A. Lola; DeCoursey, Christa; Egami, Eiichi; Eisenstein, Daniel J.; Endsley, Ryan; Hausen, Ryan; Helton, Jakob M.; Kumari, Nimisha; Looser, Tobias J.; Maseda, Michael V.; Puskás, Dávid; Rieke, Marcia; Sandles, Lester; Sun, Fengwu; Übler, Hannah; Williams, Christina C.; Willmer, Christopher N. A.; Witstok, Joris

doi:10.1038/s41550-024-02384-8

Nat Astron

2024

DOI: 10.1038/s41550-024-02384-8

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A core in a star-forming disc as evidence of inside-out growth in the early Universe

William M. Baker,

Sandro Tacchella,

Benjamin D. Johnson

et al.

Abstract: The physical processes that establish the morphological evolution and the structural diversity of galaxies are key unknowns in extragalactic astrophysics. Here we report the finding of the morphologically mature galaxy JADES-GS+53.18343−27.79097, which existed within the first 700 million years of the Universe’s history. This star-forming galaxy with a stellar mass of 400 million solar masses consists of three components: a highly compact core with a half-light radius of less than 100 pc, an actively star-form… Show more

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2024

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Cited by 5 publications

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A dormant overmassive black hole in the early Universe

Juodžbalis,

Maiolino,

Baker

et al. 2024

Nature

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Recent observations have found a large number of supermassive black holes already in place in the first few hundred million years after the Big Bang, many of which seem to be overmassive relative to their host galaxy stellar mass when compared with local relation1–9. Several different models have been proposed to explain these findings, ranging from heavy seeds to light seeds experiencing bursts of high accretion rate10–16. Yet, current datasets are unable to differentiate between these various scenarios. Here we report the detection, from the JADES survey, of broad Hα emission in a galaxy at z = 6.68, which traces a black hole with a mass of about 4 × 108M⊙ and accreting at a rate of only 0.02 times the Eddington limit. The black hole to host galaxy stellar mass ratio is about 0.4—that is, about 1,000 times above the local relation—whereas the system is closer to the local relations in terms of dynamical mass and velocity dispersion of the host galaxy. This object is most likely an indication of a much larger population of dormant black holes around the epoch of reionization. Its properties are consistent with scenarios in which short bursts of super-Eddington accretion have resulted in black hole overgrowth and massive gas expulsion from the accretion disk; in between bursts, black holes spend most of their life in a dormant state.

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A dormant overmassive black hole in the early Universe

Juodžbalis,

Maiolino,

Baker

et al. 2024

Nature

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JADES: primaeval Lyman α emitting galaxies reveal early sites of reionization out to redshift z ~ 9

Witstok,

Maiolino,

Smit

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Given the sensitivity of the resonant Lyman-α (Lyα) transition to absorption by neutral hydrogen, observations of Lyα emitting galaxies (LAEs) have been widely used to probe the ionising capabilities of reionisation-era galaxies and their impact on the intergalactic medium (IGM). However, prior to JWST our understanding of the contribution of fainter sources and of ionised ‘bubbles’ at earlier stages of reionisation remained uncertain. Here, we present the characterisation of three exceptionally distant LAEs at z > 8, newly discovered by JWST/NIRSpec in the JADES survey. These three similarly bright (MUV ≈ −20 mag) LAEs exhibit small Lyα velocity offsets from the systemic redshift, ΔvLy$α$ ≲ 200 km s−1, yet span a range of Lyα equivalent widths (15 Å, 31 Å, and 132 Å). The former two show moderate Lyα escape fractions ($f_\text{esc, {Ly$\alpha $}} \approx 10\%$), whereas Lyα escapes remarkably efficiently from the third ($f_\text{esc, {Ly$\alpha $}} \approx 72\%$), which moreover is very compact (half-light radius of 90 ± 10 pc). We find these LAEs are low-mass galaxies dominated by very recent, vigorous bursts of star formation accompanied by strong nebular emission from metal-poor gas. We infer the two LAEs with modest fesc, Ly$α$, one of which reveals evidence for ionisation by an active galactic nucleus, may have reasonably produced small ionised bubbles preventing complete IGM absorption of Lyα. The third, however, requires a ∼3 physicalMpc bubble, indicating faint galaxies have contributed significantly. The most distant LAEs thus continue to be powerful observational probes into the earlier stages of reionisation.

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A Merger-driven Scenario for Clumpy Galaxy Formation in the Epoch of Reionization: Physical Properties of Clumps in the FirstLight Simulation

Nakazato,

Ceverino,

Yoshida

2024

ApJ

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Recent JWST observations with superb angular resolution have revealed the existence of clumpy galaxies at high redshift through the detection of rest-frame optical emission lines. We use the FirstLight simulation to study the properties of (sub)galactic clumps that are bright in the [O III] λ5007 line with flux greater than ∼10−18 erg s−1 cm−2, to be detected by JWST. For 62 simulated galaxies that have stellar masses of (0.5–6) × 1010 M ⊙ at z = 5, we find clumps in 1828 snapshots in the redshift range z = 9.5–5.5. The clumps are identified by the surface density of the star formation rate (SFR). About one-tenth of the snapshots show the existence of clumpy systems with two or more components. Most of the clumps are formed by mergers and can be characterized by their ages: central clumps dominated by stellar populations older than 50 Myr, and off-centered clumps dominated by younger stellar populations with specific SFRs of ∼50 Gyr−1. The latter type of young clumps is formed from gas debris in the tidal tails of major mergers with baryonic mass ratios of 1 ≤ q < 4. The merger-induced clumps are short-lived and merge within a dynamical time of several tens of million years. The number density of the clumpy systems is estimated to be ∼10−5 cMpc−3, which is large enough to be detected in recent JWST surveys.

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A core in a star-forming disc as evidence of inside-out growth in the early Universe

Cited by 5 publications

References 108 publications

A dormant overmassive black hole in the early Universe

A dormant overmassive black hole in the early Universe

JADES: primaeval Lyman α emitting galaxies reveal early sites of reionization out to redshift z ~ 9

A Merger-driven Scenario for Clumpy Galaxy Formation in the Epoch of Reionization: Physical Properties of Clumps in the FirstLight Simulation

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