Subgalactic Scaling Relations with T
               <sub>e</sub>-based Metallicities of Low-metallicity Regions in Galaxies: Metal-poor Gas Inflow May Have Important Effects?

Yao, Yao; Liu, Haiyang; Kong, Xu; Gao, Yongheng; Chen, Guangwen; Chen, Xinkai; Liang, Zhixiong; Lin, Zhoubin; Tang, Yimeng; Zhang, Hong Xin

doi:10.3847/1538-4357/ac3b55

Cited by 5 publications

(8 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We adopted a process similar to that described by Yao et al (2022) in MaNGA to process these spectra. For each galaxy, we cut out a 40 × 40 datacube from the field it belongs to and performed spectral fitting for each spaxel.…”

Section: Spectral Fittingmentioning

confidence: 99%

See 1 more Smart Citation

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Yao

Chen

Liu

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Aims. Galaxies in the local universe have a spatially resolved star-forming main sequence (rSFMS) and mass–metallicity relation (rMZR). We know that the global mass–metallicity relation (MZR) results from the integral of the rMZR, and it evolves with redshift. However, the evolution of the rMZR with redshift is still unclear because the spatial resolution and signal-to-noise ratio are low. Currently, too few observations beyond the local universe are available, and only simulations can reproduce the evolution of the rMZR with redshift. Methods. We selected ten emission-line galaxies with an average redshift of z ∼ 0.26 from the MUSE-Wide DR1. We obtained the spatially resolved star formation rate (SFR) and metallicity from integral field spectroscopy (IFS), as well as the stellar mass surface density from 3D-HST photometry. We derived the rSFMS and rMZR at z ∼ 0.26 and compared them with those of local galaxies. Results. We find that the rSFMS of galaxies at z ∼ 0.26 has a slope of ∼0.771. The rMZR exists at z ∼ 0.26, showing a similar shape to that of the local universe, but a lower average metallicity that is about ∼0.11 dex lower than the local metallicity. In addition, we also study the spatially resolved fundamental metallicity relation (rFMR) of these galaxies. However, there is no obvious evidence that an rFMR exists at z ∼ 0.26, and it is not an extension of rMZR at a high SFR. Conclusions. Similar to their global versions, the rSFMS and rMZR of galaxies also evolve with redshift. At fixed stellar mass, galaxies at higher redshift show a higher SFR and lower metallicity. These suggest that the evolution of the global galaxy properties with redshift may result from integrating the evolution of the spatially resolved galaxy properties.

show abstract

Section: Spectral Fittingmentioning

confidence: 99%

“…However, the [O iii]λ4363 auroral line is too weak to be observed. Only a few studies (Yao et al 2022) have used the low-redshift IFS survey, let alone the high redshift. Therefore, we used the strong-line calibration relation to calculate the abundance.…”

Section: Oxygen Abundancementioning

confidence: 99%

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Yao

Chen

Liu

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In this work, we adopt a similar process to Yao et al (2022) in MaNGA to process these spectra. For each galaxy, we cut out a 40×40 datacube from the field it belongs to and performs spectral fitting for each spaxel.…”

Section: Spectral Fittingmentioning

confidence: 99%

“…However, the [O iii]λ4363 auroral line is too weak to be observed. Only a few studies used (Yao et al 2022) the low redshift IFS survey, let alone the high redshift. Therefore, we use the strong-line calibration relation to calculate the abundance.…”

Section: Oxygen Abundancementioning

confidence: 99%

Spatially resolved mass-metallicity relation at z~0.26 from the MUSE-Wide Survey

Yao,

Chen,

Liu

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Aims. There is a spatially resolved star-forming main sequence (rSFMS) and mass-metallicity relation (rMZR) of galaxies in local universe. We know that the global mass-metallicity relation (MZR) results from the integral of rMZR, and it will evolve with the redshift. However, the evolution of rMZR with redshift is still unclear due to the low spatial resolution and signal-to-noise ratio. There are currently too few observations beyond local universe, and only simulations can reproduce the evolution of rMZR with redshift. Methods. In this work, we select ten emission-line galaxies with an average redshift of z ∼ 0.26 from MUSE-Wide DR1. We obtain the spatially resolved star formation rate (SFR) and metallicity from the integral field spectroscopy (IFS), as well as the stellar mass surface density from the 3D-HST photometry. We derive the rSFMS and rMZR at z ∼ 0.26 and compare them with local galaxies. Results. We find the rSFMS of galaxies at z ∼ 0.26 has a slope of ∼0.771. The rMZR exists at z ∼ 0.26, showing a similar shape to the local universe but a lower average metallicity about ∼0.11 dex than the local one. In addition, we also study their spatially resolved fundamental metallicity relation (rFMR). However, there is no obvious evidence that rFMR exists at z ∼0.26 and it is not an extension of rMZR at a high SFR. Conclusions. Similar to their global versions, the rSFMS and rMZR of galaxies also evolve with redshift. Given the fixed stellar mass, galaxies at higher redshift show higher SFR and lower metallicity. These suggest that the evolution of the global galaxy properties with redshift may result from integrating the evolution of spatially resolved properties of galaxies.

show abstract

“…These methods are more objective than manual visual inspection and enable comparison between results from different researchers. In recent years, with the rapid evolution of computer technology, machine-learning algorithms for galaxy morphological classification and merger identification have been widely developed and utilized (e.g., Domínguez Sánchez et al 2018;Tang et al 2020;Yao et al 2022b;Fang et al 2023). At the same time, the powerful computing power has also facilitated a lot of galaxy morphological studies based on cosmological simulation (e.g., Snyder et al 2015;Bignone et al 2017;Rodriguez-Gomez et al 2019;Bignone et al 2020), which provides a direct way to link observed morphology with physical processes.…”

Section: Introductionmentioning

confidence: 99%

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

Yao,

Song,

Kong

et al. 2023

ApJ

View full text Add to dashboard Cite

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.

show abstract

Subgalactic Scaling Relations with T _e-based Metallicities of Low-metallicity Regions in Galaxies: Metal-poor Gas Inflow May Have Important Effects?

Cited by 5 publications

References 47 publications

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Spatially resolved mass-metallicity relation at z~0.26 from the MUSE-Wide Survey

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

Contact Info

Product

Resources

About

Subgalactic Scaling Relations with T e-based Metallicities of Low-metallicity Regions in Galaxies: Metal-poor Gas Inflow May Have Important Effects?

Cited by 5 publications

References 47 publications

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Spatially resolved mass–metallicity relation at z ∼ 0.26 from the MUSE-Wide Survey

Spatially resolved mass-metallicity relation at z~0.26 from the MUSE-Wide Survey

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

Contact Info

Product

Resources

About

Subgalactic Scaling Relations with T _e-based Metallicities of Low-metallicity Regions in Galaxies: Metal-poor Gas Inflow May Have Important Effects?