Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0

Galaxy morphology is one of the most fundamental ways to describe galaxy properties, but the morphology we observe may be affected by wavelength and spatial resolution, which may introduce systematic bias when comparing galaxies at different redshift. Taking advantage of the broad wavelength coverag...

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Vydáno v:The Astrophysical journal Ročník 954; číslo 2; s. 113 - 124
Hlavní autoři: Yao, Yao, Song, Jie, Kong, Xu, Fang, Guanwen, Zhang, Hong-Xin, Chen, Xinkai
Médium: Journal Article
Jazyk:angličtina
Vydáno: Philadelphia The American Astronomical Society 01.09.2023
IOP Publishing
Témata:
Astrophysics
Classification
Galactic evolution
Galaxies
Galaxy classification systems
Galaxy evolution
Galaxy structure
High-redshift galaxies
Morphology
Nonparametric statistics
Parameters
Red shift
Spatial resolution
Stars & galaxies
Stellar evolution
ISSN:0004-637X, 1538-4357
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Shrnutí:Galaxy morphology is one of the most fundamental ways to describe galaxy properties, but the morphology we observe may be affected by wavelength and spatial resolution, which may introduce systematic bias when comparing galaxies at different redshift. Taking advantage of the broad wavelength coverage from optical to near-IR and the high-resolution NIRCam instrument of the JWST, we measure the nonparametric morphological parameters of a total of 1376 galaxies at z ≃ 0.8–3.0 in the CEERS field through an optimized code called statmorph _ csst . We divide our sample into three redshift intervals and investigate the wavelength and redshift dependence of the morphological parameters. We also explore how the widely used galaxy type classification methods based on the morphological parameters depend on wavelength and spatial resolution. We find that there are variations in all morphological parameters with rest-frame wavelength ( λ rf ), especially at the short-wavelength end, and that λ rf mainly affects the classification between late- and early-type galaxies. As λ rf increases, the galaxies on the G – M 20 diagram move to the upper left with a slope of −0.23 ± 0.03 on average. We find that spatial resolution mainly affects the merger identification. The merger fraction in F200W resolution can be ≳2 times larger than that in F444W resolution. Furthermore, we compare the morphological parameter evolution of galaxies with different stellar masses. We find that there are differences in the morphological evolution of high- and low-mass (log M * ≥ 10 and 9 < log M * < 10) galaxies in the studied redshift range, which may be caused by their different evolutionary paths.
Bibliografie:Galaxies and Cosmology
AAS45972
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SourceType-Scholarly Journals-1
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ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ace7b5