Fine vita al Pronto Soccorso

Conte, Philippe Le

doi:10.1016/s1286-9341(22)47494-1

Cited by 2 publications

(2 citation statements)

References 14 publications

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“…Recent numerical simulations were able to demonstrate that a bulge can also form from a hot thick disk (Ghosh et al 2023). Disks at high redshifts (z ∼ 4-5) have been observed by the Atacama Large Millimeter/submillimeter Array (Parlanti et al 2023;Roman-Oliveira et al 2023) and JWST (Ferreira et al 2023) and even bars have been clearly observed at z > 2 (Costantin et al 2023;Guo et al 2023;Le Conte et al 2023). At early times, the emergence of stellar bars can be rapid when the dark matter fractions in the centers of disk galaxies are low (Bland-Hawthorn et al 2023).…”

Section: Introductionmentioning

confidence: 91%

Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3

Liao,

Li,

Simion

et al. 2024

ApJ

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We explore the chemodynamical properties of the Galaxy in the azimuthal velocity V ϕ and metallicity [Fe/H] space using red giant stars from Gaia Data Release 3. The row-normalized V ϕ –[Fe/H] maps form a coherent sequence from the bulge to the outer disk, clearly revealing the thin/thick disk and the Splash. The metal-rich stars display bar-like kinematics, while the metal-poor stars show dispersion-dominated kinematics. The intermediate-metallicity population (−1 < [Fe/H]< − 0.4) can be separated into two populations, one that is bar-like, i.e., dynamically cold ( σ V R ∼ 80 km s−1) and fast-rotating (V ϕ ≳ 100 km s−1), and the Splash, which is dynamically hot ( σ V R ∼ 110 km s−1) and slow-rotating (V ϕ ≲ 100 km s−1). We compare the observations in the bulge region with an Auriga simulation where the last major merger event occurred ∼10 Gyr ago: only stars born around the time of the merger reveal a Splash-like feature in the V ϕ –[Fe/H] space, suggesting that the Splash is likely merger-induced, predominantly made up of heated disk stars and the starburst associated with the last major merger. Since the Splash formed from the proto-disk, its lower metallicity limit coincides with that of the thick disk. The bar formed later from the dynamically hot disk with [Fe/H] > − 1 dex, with the Splash not participating in the bar formation and growth. Moreover, with a set of isolated evolving N-body disk simulations, we confirm that a nonrotating classical bulge can be spun up by the bar and develop cylindrical rotation, consistent with the observations for the metal-poor stars.

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Section: Introductionmentioning

confidence: 91%

Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3

Liao,

Li,

Simion

et al. 2024

ApJ

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“…Suess et al (2022) find that starforming galaxies are more concentrated in terms of their stellar mass than in their rest-frame optical light at 1.0 < z < 2.5 compared to previous estimates using HST data. Costantin et al (2023a) find galaxy disks hosting stellar bars at redshifts as high as z ≈ 3 (see also Guo et al 2023;Le Conte et al 2023), suggesting that galaxy disks like those in the local Universe may have been in place much earlier than anticipated. Recently, Pandya et al (2023) found that the majority of low-mass galaxies at z > 1 are prolate, cigar-shaped systems instead of oblate disks.…”

Section: Introductionmentioning

confidence: 92%

Evolution of the Size–Mass Relation of Star-forming Galaxies Since z = 5.5 Revealed by CEERS

Ward,

de la Vega,

Mobasher

et al. 2024

ApJ

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We combine deep imaging data from the CEERS early release JWST survey and Hubble Space Telescope imaging from CANDELS to examine the size–mass relation of star-forming galaxies and the morphology–quenching relation at stellar masses M ⋆ ≥ 109.5 M ⊙ over the redshift range 0.5 < z < 5.5. In this study with a sample of 2450 galaxies, we separate star-forming and quiescent galaxies based on their star formation activity and confirm that star-forming and quiescent galaxies have different morphologies out to z = 5.5, extending the results of earlier studies out to higher redshifts. We find that star-forming and quiescent galaxies have typical Sérsic indices of n ∼ 1.3 and n ∼ 4.3, respectively. Focusing on star-forming galaxies, we find that the slope of the size–mass relation is nearly constant with redshift, as was found previously, but shows a modest increase at z ∼ 4.2. The intercept in the size–mass relation declines out to z = 5.5 at rates that are similar to what earlier studies found. The intrinsic scatter in the size–mass relation is relatively constant out to z = 5.5.

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Fine vita al Pronto Soccorso

Cited by 2 publications

References 14 publications

Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3

Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3

Evolution of the Size–Mass Relation of Star-forming Galaxies Since z = 5.5 Revealed by CEERS

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