Near-infrared characterization of ultra-diffuse galaxies in Abell 2744 by <i>JWST</i>/NIRISS imaging

Ikeda, Ryota; Morishita, Takahiro; Tsukui, Takafumi; Vulcani, Benedetta; Trenti, Michele; Metha, Benjamin; Acebrón, Ana; Bergamini, P.; Grillo, C.; Iono, Daisuke; Mercurio, A.; Rosati, P.; Vanzella, E.

doi:10.1093/mnras/stad1692

Cited by 3 publications

(1 citation statement)

References 72 publications

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“…For these measurements, we randomly selected 100 circular apertures per field of view of 2 2 × 2 2, corresponding to a single JWST/ NIRCam module. Overall, the JWST NIRCam images exhibit surface brightness limits deeper than 25 mag arcsec 2 ~for the short-wavelength filters and 26 mag arcsec 2 ~for the longwavelength filters, which even enables the detection of low surface brightness galaxies (Ikeda et al 2023)…”

Section: Hst and Jwst/nircam Imagesmentioning

confidence: 96%

Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Lee,

Park,

Hwang

et al. 2024

ApJ

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A recent study from the Horizon Run 5 (HR5) cosmological simulation has predicted that galaxies with log M * / M ⊙ ≲ 10 in the cosmic morning (10 ≳ z ≳ 4) dominantly have disk-like morphology in the ΛCDM universe, which is driven by the tidal torque in the initial fluctuations of matter. For a direct comparison with observation we identify a total of about 19,000 James Webb Space Telescope (JWST) galaxies with log M * / M ⊙ > 9 at z = 0.6–8.0 utilizing deep JWST/NIRCam images of publicly released fields, including North Ecliptic Pole Time-Domain Fields, Next Generation Deep Extragalactic Exploratory Public survey, Cosmic Evolution Early Release Science Survey, Cosmic Evolution Survey, UltraDeep Survey, and SMACS J0723-7327. We estimate their stellar masses and photometric redshifts with the redshift dispersion of σ NMAD = 0.009 and an outlier fraction of only about 6%. We classify galaxies into three morphological types, disks, spheroids, and irregulars, applying the same criteria used in the HR5 study. The morphological distribution of the JWST galaxies shows that disk galaxies account for 60%–70% at all redshift ranges. However, in the high-mass regime ( log M * / M ⊙ ≳ 11 ), spheroidal morphology becomes the dominant type. This implies that the mass growth of galaxies is accompanied by a morphological transition from disks to spheroids. The fraction of irregulars is about 20% or less at all masses and redshifts. All the trends in the morphology distribution are consistently found in the six JWST fields. These results are in close agreement with the results from the HR5 simulation, particularly confirming the prevalence of disk galaxies at small masses in the cosmic morning and noon.

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Section: Hst and Jwst/nircam Imagesmentioning

confidence: 96%

Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Lee,

Park,

Hwang

et al. 2024

ApJ

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The star formation histories of quiescent ultra-diffuse galaxies and their dependence on environment and globular cluster richness

Ferré-Mateu,

Gannon,

Forbes

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We derive the stellar population parameters of 11 quiescent ultra-diffuse galaxies (UDGs) from Keck/KCWI data. We supplement these with 14 literature UDGs, creating the largest spectroscopic sample of UDGs to date (25). We find a strong relationship between their α-enhancement and their star formation histories: UDGs that formed on very short time-scales have elevated [Mg/Fe] abundance ratios, whereas those forming over extended periods present lower values. Those forming earlier and faster are overall found in high-density environments, being mostly early infalls into the cluster. No other strong trends are found with infall times. We analyse the stellar mass–metallicity, age–metallicity, and [Mg/Fe]–metallicity relations of the UDGs, comparing them to other types of low mass galaxies. Overall, UDGs scatter around the established stellar mass–metallicity relations of classical dwarfs. We find that GC-rich UDGs have intermediate-to-old ages, but previously reported trends of galaxy metallicity and GC richness are not reproduced with this spectroscopic sample due to the existence of GC-rich UDGs with elevated metallicities. In addition, we also find that a small fraction of UDGs could be ‘failed-galaxies’, supported by their GC richness, high alpha-abundance, fast formation time-scales and that they follow the mass–metallicity relation of z ∼2 galaxies. Finally, we also compare our observations to simulated UDGs. We caution that there is not a single simulation that can produce the diverse UDG properties simultaneously, in particular the low metallicity failed galaxy like UDGs.

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JWST Photometry of Globular Clusters in A2744. II. Luminosity and Color Distributions

Harris,

Reina-Campos

2024

ApJ

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Deep JWST imaging of the giant galaxy cluster A2744, at redshift z = 0.308, is used to explore the features of its rich population of globular clusters (GCs), building on our initial survey of the system. We use the photometry of more than 10,000 GCs over a 3 mag range to construct the GC luminosity function and color distribution. These results now specifically account for photometric incompleteness as a function of location relative to the five giant galaxies that dominate the gravitational potential of A2744. The total GC population in A2744 is estimated at N GC ≥ 1.1 × 105, consistent with its high total mass. We also directly compare the observed distributions with theoretical predictions for GC populations drawn from the recent EMP-Pathfinder simulations, viewed at the same 3.5 Gyr look-back time as the cluster. The simulations match the observations well, with the only notable disagreement being that the simulations predict larger numbers of GCs at high metallicity formed after z ≃ 2 than are seen in the data.

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Near-infrared characterization of ultra-diffuse galaxies in Abell 2744 by JWST/NIRISS imaging

Cited by 3 publications

References 72 publications

Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

The star formation histories of quiescent ultra-diffuse galaxies and their dependence on environment and globular cluster richness

JWST Photometry of Globular Clusters in A2744. II. Luminosity and Color Distributions

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