English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Galaxy morphology is one of the most fundamental ways to describe galaxyproperties, but the morphology we observe may be affected by wavelength andspatial resolution, which may introduce systematic bias when comparing galaxiesat different redshift. Taking advantage of the broad wavelength coverage fromoptical to near-IR and high resolution NIRCam instrument of JWST, we measurethe non-parametric morphological parameters of a total of 1376 galaxies at$z\simeq$0.8-3.0 in the CEERS field through an optimized code called{\tt\string statmorph\_csst}. We divide our sample into three redshiftintervals and investigate the wavelength- and redshift-dependence of themorphological parameters. We also explore how the widely-used galaxy typeclassification methods based on the morphological parameters depend onwavelength and spatial resolution. We find that there are variations in allmorphological parameters with rest-frame wavelength ($\lambda_{\rm rf}$),especially at the short wavelength end, and the $\lambda_{\rm rf}$ mainlyaffects the classification between late-type and early-type galaxy. As the$\lambda_{\rm rf}$ increases, the galaxies on the $G-M_{20}$ diagram move tothe upper left with a slope of -0.23$\pm$0.03 on average. We find that spatialresolution mainly affects the merger identification. The merger fraction inF200W resolution can be $\ga$2 times larger than that in F444W resolution.Furthermore, We compare the morphological parameter evolution of galaxies withdifferent stellar masses. We find that there are differences in themorphological evolution of high- and low-mass (log$M_*\geqslant$10 and9$<$log$M_*<$10) galaxies in the studied redshift range, which may be caused bytheir different evolution paths.

Evolution of Non-parametric Morphology of Galaxies in the JWST CEERS Field at $z\simeq$0.8-3.0