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

Yao, Yao; Chen, Guangwen; Liu, Haiyang; Chen, Xinkai; Lin, Zhoubin; Gao, Yongheng; Kong, Xu

doi:10.1051/0004-6361/202243104

Cited by 8 publications

(3 citation statements)

References 65 publications

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“…The aperture of the background is the same as the extraction of the blobs. We adopt the same method as [68] to fit emission lines, using the MPFIT code. The n e and the 1σ upper limit of T e are calculated by the PyNeb[69] code.…”

Section: Spectral Extraction and Fittingmentioning

confidence: 99%

Evidence for an intermediate mass black hole in a low-mass star-forming galaxy

Wang,

Yao,

et al. 2024

Preprint

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Intermediate Mass Black Holes (IMBHs) are the bridge of the gap between stellar mass black holes, which are around ten solar masses, and supermassive black holes, which can have millions to billions of solar masses. However, it is still challenging to detect and identify the existence of them with respect to supermassive black holes. We report the evidence of a hidden IMBH for a low-mass galaxy, MaNGA 9885-9102. This galaxy is originally selected from the MaNGA survey with distinctive bipolar Hα blobs at the minor axis. The bipolar feature can be associated with AGN activity, while the two blobs are classified as the HII regions on the BPT diagram, making the origins confusing. The Swift UV continuum shows that the two blobs do not have UV counterparts, suggesting that the source of ionization is out of the blobs. Consistent with this, the detailed photoionization models prefer to AGN rather than star-forming origin with a significance of 5.8σ. The estimated black hole mass is MBH ∼7.2× 105M⊙ from the central velocity dispersion of stars. Not only identifying an active IMBH, this work presents a new method to search for the light echo of IMBH in low-mass and dwarf galaxies of low metallicity, where the traditional BPT diagram fails.

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Section: Spectral Extraction and Fittingmentioning

confidence: 99%

Evidence for an intermediate mass black hole in a low-mass star-forming galaxy

Wang,

Yao,

et al. 2024

Preprint

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“…The following describes our PSF matching procedure. The overall process is similar to that of Yao et al (2022a), but some optimizations have been made.…”

Section: Point-spread Function Matchingmentioning

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

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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.

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“…We also mark the ID of some knots to facilitate the description of the star A179, page 8 of 13 . We adopt the α = 0.32, which is same to previous studies (e.g., Mannucci et al 2010;Yao et al 2022). The solid lines represent the best-fit relations based on orthogonal distance regression (odr).…”

Section: Scaling Relationsmentioning

confidence: 99%

Merger-induced star formation in the low-metallicity dwarf galaxy NGC 4809/4810

Gao,

Gu,

Liu

et al. 2023

A&A

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Context. The physical mechanisms driving starbursts in dwarf galaxies are unclear, and the effects of mergers on star formation in these galaxies are still uncertain. Aims. We explore how the merger process affects star formation in metal-poor dwarf galaxies by analyzing high spatial resolution (∼70 pc) integral field spectrograph observations of ionized gas. Methods. We used archival data from the Very Large Telescope/Multi Unit Spectroscopic Explorer to map the spatial distribution of strong emission lines (e.g., Hβ, Hα, [O III] λ5007, and [N II] λ6583) in the nearby merging star-forming dwarf galaxy system NGC 4809/4810. Results. We identify 112 star-forming knots scattered among the two galaxies, where the gas-phase metallicity distribution is inhomogeneous and mixes with metal-poor and metal-rich ionized gas. Star-forming knots at the interacting region show lower metallicity, the highest star formation rates (SFRs), and the highest ratio of the SFR to the resolved main-sequence relation (rMSR). Ionized gas exhibits an obvious northeast–southwest velocity gradient in NGC 4809, but appears to be mixed in NGC 4810. The high virial parameters and the stellar mass-size relation of the H II regions indicate that these regions are dominated by direct radiation pressure from massive stars (or clusters) and expand persistently. We find two different relations of the stellar mass surface density to stellar age in NGC 4809 and NGC 4810, and the stellar ages of NGC 4810 are systematically younger than those in NGC 4809. Conclusions. Our study suggests that the merging stage of two dwarf galaxies can induce starburst activities in the interaction areas despite the metal-deficient environment. Considering the high specific SFRs and different stellar ages, we propose that the interaction initially triggered star formation in NGC 4809 and then drove star formation in NGC 4810.

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

Cited by 8 publications

References 65 publications

Evidence for an intermediate mass black hole in a low-mass star-forming galaxy

Evidence for an intermediate mass black hole in a low-mass star-forming galaxy

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

Merger-induced star formation in the low-metallicity dwarf galaxy NGC 4809/4810

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