Xiaoling Yu

Qujing Normal University

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Papers

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i-10 index

Research Trends

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Document Type

Co-Authors

Qiusheng Gu

Nanjing University

Yong Shi

Nanjing University

Yongyun Chen

Qujing Normal University

Dingrong Xiong

Yunnan Observatories

Songlin Li

ARC Centre of Excellence for All-sky Astrophysics

Jianhang Chen

European Southern Observatory

Yanmei Chen

Sichuan University

Xiaotong Guo

Anqing Normal University

Nan Ding

Kunming University

L. Bing

Centre National de la Recherche Scientifique

Cooperative Institutions

Chinese Academy of Sciences

Nanjing University

University of Chinese Academy of Sciences

Centre National de la Recherche Scientifique

CEA Paris-Saclay

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

Université Paris Cité

National Astronomical Observatories

Sorbonne Paris Cité

Délégation Paris 7

Author Statistics

Papers

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Probing possible effects of circumgalactic media on the metal content of galaxies through the mass–metallicity relationship

Monthly Notices of the Royal Astronomical Society (2021)

Sai Zhai Yong Shi Jianhang Chen L. Bing Yanmei Chen

The circumgalactic medium (CGM) connects the gas between the interstellar medium (ISM) and the intergalactic medium, which plays an important role in galaxy evolution. We use the stellar mass-metallicity relationship to investigate whether sharing the CGM will affect the distribution of metals in galaxy pairs. The optical emission lines from the Sloan Digital Sky Survey Data Release (SDSS DR7) are used to measure the gas-phase metallicity. We find that there is no significant difference in the distribution of the metallicity difference between two members in star forming-star forming pairs ($\rm Δlog(O/H)_{diff}$), metallicity offset from the best-fitted stellar mass-metallicity relationship of galaxies in pairs ($\rm Δlog(O/H)_{MS}$), as compared to "fake" pairs. By looking at $\rm Δlog(O/H)_{diff}$ and $\rm Δlog(O/H)_{MS}$ as a function of the star formation rate (SFR), specific star formation rate (sSFR), and stellar mass ratio, no difference is seen between galaxies in pairs and control galaxies. From our results, the share of the CGM may not play an important role in shaping the evolution of metal contents of galaxies.

Stellar mass

10.1093/mnras/stab1017

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Spatially resolved properties of supernova host galaxies in SDSS-IV MaNGA

Research in Astronomy and Astrophysics (2021)

Hongxuan Zhang Yanmei Chen Yong Shi Min Bao Xiaoling Yu

Abstract We crossmatch galaxies from Mapping Nearby Galaxies at Apache Point Observatory with the Open Supernova Catalog, obtaining a total of 132 SNe within MaNGA bundle. These 132 SNe can be classified into 67 Type Ia and 65 Type CC. We study the global and local properties of supernova host galaxies statistically. Type Ia SNe are distributed in both star-forming galaxies and quiescent galaxies, while Type CC SNe are all distributed along the star-forming main sequence. As the stellar mass increases, the Type Ia/CC number ratio increases. We find: (1) there is no obvious difference in the interaction possibilities and environments between Type Ia SN hosts and a control sample of galaxies with similar stellar mass and SFR distributions, except that Type Ia SNe tend to appear in galaxies which are more bulge-dominated than their controls. For Type CC SNe, there is no difference between their hosts and the control galaxies in galaxy morphology, interaction possibilities as well as environments; (2) compared to galaxy centers, the SN locations have smaller velocity dispersion, lower metallicity, and younger stellar population. This is a natural result of radius gradients for all these parameters. The SN location and its symmetrical position relative to the galaxy center, as well as regions with similar effective radii have very similar [Mg/Fe], gas-phase metallicity, gas velocity dispersion and stellar population age.

Velocity dispersion

Stellar population

Peculiar galaxy

Stellar mass

10.1088/1674-4527/21/12/306

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The H i-rich ultra-diffuse galaxies follow the extended Schmidt law

Monthly Notices of the Royal Astronomical Society (2023)

Sai Zhai Yong Shi Zhi-Yu Zhang Junzhi Wang Yu Gao

ABSTRACT The ${\rm H\, {\small I}}$-rich ultra-diffuse galaxies (HUDGs) offer a unique case for studies of star formation laws as they host low star formation efficiency and low-metallicity environments where gas is predominantly atomic. We collect a sample of six HUDGs in the field and investigate their location in the extended Schmidt law ($\Sigma _{\text{SFR }} \propto \left(\Sigma _{\text{star}}^{0.5} \Sigma _{\text{gas}}\right)^{1.09}$). They are consistent with this relationship well (with deviations of only 1.1σ). Furthermore, we find that HUDGs follow the tight correlation between the hydrostatic pressure in the galaxy mid-plane and the quantity on the x-axis ($\rm log(\Sigma _{star}^{0.5}\Sigma _{gas})$) of the extended Schmidt law. This result indicates that these HUDGs can be self-regulated systems that reach the dynamical and thermal equilibrium. In this framework, the stellar gravity compresses the disc vertically and counteracts the gas pressure in the galaxy mid-plane to regulate the star formation as suggested by some theoretical models.

Sigma

Hydrostatic equilibrium

Star (game theory)

Ram pressure

10.1093/mnras/stad3424

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Citations (1)

Jets, accretion and spin in supermassive black holes

Research in Astronomy and Astrophysics (2024)

Yongyun Chen Qiusheng Gu J. H. Yang J. H. Fan Xiaoling Yu

Abstract The theoretical model suggests that relativistic jets of active galactic nuclei (AGNs) rely on the black hole spin and/or accretion. We study the relationship between jet, accretion, and spin using supermassive black hole samples with reliable spin of black holes. Our results are as follows: (1) There is a weak correlation between radio luminosity and the spin of the black hole for our sample, which may imply that the jet of the supermassive black hole in our sample depends on the other physical parameters besides black hole spins, such as accretion disk luminosity. (2) The jet power of a supermassive black hole can be explained by the hybrid model with magnetic field of corona. (3) There is a significant correlation between radio-loudness and black hole spin for our sample. These sources with high radio-loudness tend to have high black hole spins. These results provide observational evidence that the black hole spin may explain the bimodal phenomena of radio-loud and radio-quiet AGNs.

Accretion disc

Gamma-ray burst progenitors

10.1088/1674-4527/ad8627

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The Variability of the Narrow-line Seyfert 1 Galaxies from the Pan-STARRS’s View

Research in Astronomy and Astrophysics (2021)

Hongtao Wang Yan-Ping Su Xue Ge Yongyun Chen Xiaoling Yu

By means of the data sets from the Pan-STARRAS1 survey, we have systematically examined the relationship between the variability characteristics and the physical parameters of the largest NLS1 galaxy sample up to now. The results are summarized as follows: (1). We find significant anti-correlations between variability amplitude and absolute magnitude in g, r, i, z and y bands, which are consistent with the results in previous works. (2) The correlations between the variability amplitude in optical band and many physical parameters (e.g., {\lambda}L(5100 {\AA}), black hole mass, Eddington ratio, R4570 and R5007) are investigated. The results show the variability amplitude is significantly anti-correlated with L(5100 {\AA}), MBH, Eddington ratio and R4570, but positively correlated with R5007. The relation could be explained by the simple standard accretion disk model. (3) We further investigate the relationship between optical variability and radio luminosity/radio-loudness. The results present weak positive correlation in g and r bands, but insignificant correlation in i, z and y bands. The large error of the approximate fraction of the host galaxy in i, z and y bands may lead to insignificant correlations.

Line (geometry)

Doubly ionized oxygen

10.1088/1674-4527/ac3895

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The beaming effect and γ-ray emission for Fermi blazars

Research in Astronomy and Astrophysics (2016)

Yongyun Chen Xiong Zhang Dingrong Xiong Si-Ju Wang Xiaoling Yu

We study the γ-ray luminosity and beaming effect for Fermi blazars. Our results are as follows. (i) There are significant correlations between γ-ray luminosity and radio core luminosity, and between γ-ray luminosity and Rv, which suggests that the γ-ray emissions have a strong beaming effect. (ii) Using the Lext/Mabs as an indicator of environment effects, we find that there is no significant correlation between γ-ray luminosity and Lext/Mabs for all sources when we remove the effect of redshift. Flat spectrum radio quasars considered alone also do not show a significant correlation, but BL Lacertae objects (BL Lacs) still show a significant correlation when we remove the effect of redshift. These results suggest that the γ-ray emission may be affected by the environment on a kiloparsec scale for BL Lacs.

10.1088/1674-4527/16/1/013

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A Cuspy Dark Matter Halo

The Astrophysical Journal (2021)

Yong Shi Zhi-Yu Zhang Junzhi Wang Jianhang Chen Qiusheng Gu

Abstract The cusp–core problem is one of the main challenges of the cold dark matter paradigm on small scales; the density of a dark matter halo is predicted to rise rapidly toward the center as ρ ( r ) ∝ r α with α between −1 and −1.5, while such a cuspy profile has not been clearly observed. We have carried out the spatially resolved mapping of gas dynamics toward a nearby ultradiffuse galaxy (UDG), AGC 242019. The derived rotation curve of dark matter is well fitted by the cuspy profile as described by the Navarro–Frenk–White model, while the cored profiles including both the pseudo-isothermal and Burkert models are excluded. The halo has α = −(0.90 ± 0.08) at the innermost radius of 0.67 kpc, M halo = (3.5 ± 1.2) × 10 10 M ⊙ , and a small concentration of 2.0 ± 0.36. The UDG AGC 242019 challenges alternatives of cold dark matter by constraining the particle mass of fuzzy dark matter to be <0.11 × 10 −22 or >3.3 × 10 −22 eV, the cross section of self-interacting dark matter to be <1.63 cm 2 g −1 , and the particle mass of warm dark matter to be >0.23 keV, all of which are in tension with other constraints. The modified Newtonian dynamics is also inconsistent with a shallow radial acceleration relationship of AGC 242019. For the feedback scenario that transforms a cusp to a core, AGC 242019 disagrees with the stellar-to-halo mass ratio dependent model but agrees with the star formation threshold dependent model. As a UDG, AGC 242019 is in a dwarf-sized halo with weak stellar feedback, late formation time, normal baryonic spin, and low star formation efficiency (SFR/gas).

Cuspy halo problem

Modified Newtonian dynamics

Cold dark matter

Warm dark matter

10.3847/1538-4357/abd777

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Citations (28)

Erratum: An early-type galaxy with an inner star-forming disc

Monthly Notices of the Royal Astronomical Society (2018)

Songlin Li Yong Shi Yanmei Chen Martha Tabor Dmitry Bizyaev

Star (game theory)

10.1093/mnras/sty2299

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SDSS-IV MaNGA: enhanced star formation in galactic-scale outflows

Monthly Notices of the Royal Astronomical Society (2021)

Min Bao Yanmei Chen Qirong Yuan Yong Shi Dmitry Bizyaev

ABSTRACT Using the integral field unit (IFU) data from Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, we collect a sample of 36 star-forming galaxies that host galactic-scale outflows in ionized gas phase. The control sample is matched in the three-dimensional parameter space of stellar mass, star formation rate, and inclination angle. Concerning the global properties, the outflows host galaxies tend to have smaller size, more asymmetric gas disc, more active star formation in the centre, and older stellar population than the control galaxies. Comparing the stellar population properties along axes, we conclude that the star formation in the outflows host galaxies can be divided into two branches. One branch evolves following the inside-out formation scenario. The other located in the galactic centre is triggered by gas accretion or galaxy interaction, and further drives the galactic-scale outflows. Besides, the enhanced star formation and metallicity along minor axis of outflows host galaxies uncover the positive feedback and metal entrainment in the galactic-scale outflows. Observational data in different phases with higher spatial resolution are needed to reveal the influence of galactic-scale outflows on the star formation progress in detail.

Stellar population

10.1093/mnras/stab1201

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Citations (4)

BLACK HOLE MASS, JET POWER, AND ACCRETION IN AGNs

The Astronomical Journal (2015)

Yongyun Chen Xiong Zhang Dingrong Xiong Xiaoling Yu

We study the relation between accretion, black hole mass, and jet power in active galactic nuclei (AGNs) using a large group of blazars detected by the Fermi Large Area Telescope and radio galaxies. Our main results are as follows. (1) The jet power of flat spectrum radio quasars (FSRQs) and the FRII high-excitation galaxy (HEG) depends on the black hole mass, which suggests that the FSRQs and FRII HEG are in the radiation-pressure-dominated regime. The jet power of BL Lacs and the FRI low-excitation galaxy (LEG) depends on the accretion, which suggests that the BL Lacs and FRI LEG are in the gas-pressure-dominated regime. (2) We find that most of FSRQs and BL Lacs have , which suggests that the Blandford–Znajek mechanism is insufficient to explain the jet power of these objects. (3) The FSRQs are roughly separated from BL Lacs by Ledlow–Owen's dividing line in the plane, which supports the unified scheme of AGNs. (4) The FSRQs and BL Lacs have a clear division at , and the distribution of Eddington ratios of BL Lacs and FSRQs exhibits a bimodal nature, which implies that the accretion mode of FSRQs may be different from that of BL Lacs. (5) We find a significant correlation between broad-line luminosity and jet power, which supports a direct tight connection between jet power and accretion.

Black hole (networking)

10.1088/0004-6256/150/1/8

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Citations (22)