Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Min Bao
Yanmei Chen
Qirong Yuan
Yong Shi
Dmitry Bizyaev
Xiaoling Yu
Shuai Feng
Xiao Cao
Yulong Gao
Qiusheng Gu
Ying Yu
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 disk, more active star formation in the center 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 locating in the galactic center 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.
Peer Review Status:
Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： 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 ($\rm \Delta log(O/H)_{diff}$), metallicity offset from the best-fitted stellar mass-metallicity relationship of galaxies in pairs ($\rm \Delta log(O/H)_{MS}$), as compared to "fake" pairs. By looking at $\rm \Delta log(O/H)_{diff}$ and $\rm \Delta log(O/H)_{MS}$ 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.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Yuren Zhou
Yanmei Chen
Yong Shi
Dmitry Bizyaev
Hong Guo
Min Bao
Haitong Xu
Xiaoling Yu
Joel R. Brownstein
Abstract： We select 456 gas-star kinematically misaligned galaxies from the internal Product Launch-10 of MaNGA survey, including 74 star-forming (SF), 136 green-valley (GV) and 206 quiescent (QS) galaxies. We find that the distributions of difference between gas and star position angles for galaxies have three local peaks at $\sim0^{\circ}$, $90^{\circ}$, $180^{\circ}$. The fraction of misaligned galaxies peaks at $\log(M_*/M_{\odot})\sim10.5$ and declines to both low and high mass end. This fraction decreases monotonically with increasing SFR and sSFR. We compare the global parameters including gas kinematic asymmetry $V_{\mathrm{asym}}$, HI detection rate and mass fraction of molecular gas, effective radius $R_e$, S\'{e}rsic index $n$ as well as spin parameter $\lambda_{R_e}$ between misaligned galaxies and their control samples. We find that the misaligned galaxies have lower HI detection rate and molecular gas mass fraction, smaller size, higher S\'{e}rsic index and lower spin parameters than their control samples. The SF and GV misaligned galaxies are more asymmetric in gas velocity fields than their controls. These observational evidences point to the gas accretion scenario followed by angular momentum redistribution from gas-gas collision, leading to gas inflow and central star formation for the SF and GV misaligned galaxies. We propose three possible origins of the misaligned QS galaxies: (1) external gas accretion; (2) merger; (3) GV misaligned galaxies evolve into QS galaxies.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Lan Wang
Zheng Zheng
Cai-Na Hao
Rui Guo
Ran Li
Lei Qian
Lizhi Xie
Yong Shi
Hu Zou
Yixian Cao
Yanmei Chen
Xiaoyang Xia
Abstract： A sample of 279 massive red spirals was selected optically by Guo et al. (2020), among which 166 galaxies have been observed by the ALFALFA survey. In this work, we observe HI content of the rest 113 massive red spiral galaxies using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). 75 of the 113 galaxies have HI detection with a signal-to-noise ratio (S/N) greater than 4.7. Compared with the red spirals in the same sample that have been observed by the ALFALFA survey, galaxies observed by FAST have on average a higher S/N, and reach to a lower HI mass. To investigate why many red spirals contain a significant amount of HI mass, we check color profiles of the massive red spirals using images observed by the DESI Legacy Imaging Surveys. We find that galaxies with HI detection have bluer outer disks than the galaxies without HI detection, for both ALFALFA and FAST samples. For galaxies with HI detection, there exists a clear correlation between galaxy HI mass and g-r color at outer radius: galaxies with higher HI masses have bluer outer disks. The results indicate that optically selected massive red spirals are not fully quenched, and the HI gas observed in many of the galaxies may exist in their outer blue disks.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： Distance-redshift diagrams probe expansion history of the Universe. We show that the stellar mass-binding energy (massE) relation of galaxies proposed in our previous study offers a new distance ruler at cosmic scales. By using elliptical galaxies in the main galaxy sample of the Sloan Digital Sky Survey Data Release 7, we construct a distance-redshift diagram over the redshift range from 0.05 to 0.2 with the massE ruler. The best-fit dark energy density is 0.675+-0.079 for flat Lambda-CDM, consistent with those by other probes. At the median redshift of 0.11, the median distance is estimated to have a fractional error of 0.34%, much lower than those by supernova (SN) Ia and baryonic acoustic oscillation (BAO) and even exceeding their future capability at this redshift. The above low-z measurement is useful for probing dark energy that dominates at the late Universe. For a flat dark energy equation of state model (flat wCDM), the massE alone constrains w to an error that is only a factor of 2.2, 1.7 and 1.3 times larger than those by BAO, SN Ia, and cosmic microwave background (CMB), respectively.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Haitong Xu
Yanmei Chen
Yong Shi
Yuren Zhou
Dmitry Bizyaev
Min Bao
Minje Beom
José G. Fernández-Trincado
Xiao Cao
Abstract： We select 456 galaxies with kinematically misaligned gas and stellar components from 9546 parent galaxies in MaNGA, and classify them into 72 star-forming galaxies, 142 green-valley galaxies and 242 quiescent galaxies. Comparing the spatial resolved properties of the misaligned galaxies with control samples closely match in the D$_n$4000 and stellar velocity dispersion, we find that: (1) the misaligned galaxies have lower values in $V_{\rm gas}/{\sigma}_{\rm gas}$ and $V_{\rm star}/{\sigma}_{\rm star}$ (the ratio between ordered to random motion of gas and stellar components) across the entire galaxies than their control samples; (2) the star-forming and green-valley misaligned galaxies have enhanced central concentrated star formation than their control galaxies. The difference in stellar population between quiescent misaligned galaxies and control samples is small; (3) gas-phase metallicity of the green valley and quiescent misaligned galaxies are lower than the control samples. For the star forming misaligned galaxies, the difference in metallicity between the misaligned galaxies and their control samples strongly depends on how we select the control samples. All these observational results suggest external gas accretion influences the evolution of star forming and green valley galaxies, not only in kinematics/morphologies, but also in stellar populations. However, the quiescent misaligned galaxies have survived from different formation mechanisms.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Min Bao
Yanmei Chen
Pengpei Zhu
Yong Shi
Dmitry Bizyaev
Ling Zhu
Meng Yang
Minje Beom
Joel R. Brownstein
Richard R. Lane
Abstract： Using the integral field unit (IFU) data from Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, we select a sample of 101 galaxies with counter-rotating stellar disks and regularly-rotating ionized gas disk. We classify the 101 galaxies into four types based on the features of their stellar velocity fields. The relative fractions and stellar population age radial gradients of the four types are different in blue cloud (BC), green valley (GV) and red sequence (RS) populations. We suggest different formation scenarios for the counter-rotating stellar disks, and the key factors in the formation of counter-rotating stellar disks include: (1) the abundance of pre-existing gas in progenitor, (2) the efficiency in angular momentum consumption.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： We select 753 S0 galaxies from the internal Product Lauch-10 of MaNGA survey (MPL-10) and find that $\sim$11% of S0 galaxies show gas-star kinematic misalignments, which is higher than the misaligned fraction in spiral ($\sim$1%) and elliptical galaxies ($\sim$6%) in MPL-10. If we only consider the emission-line galaxies (401 emission-line S0s), the misaligned fraction in S0s increases to $\sim$20%. In S0s, the kinematic misalignments are more common than the merger remnant features ($\sim$8%). Misaligned S0s have lower masses of stellar components and dark matter halos than S0s with merger remnant features. Based on the $NUV-r$ versus $M_*$ diagram, we split galaxies into three populations: blue cloud (BC), green valley (GV) and red sequence, finding that BC and GV misaligned S0s have positive $\mathrm{D}_n4000$ radial gradients which indicates younger stellar population in the central region than the outskirts. Through comparing the misaligned S0s with a control sample for the whole S0 galaxy sample, we find that the BC and GV misaligned S0s show younger stellar population at $R\lesssim R_e$ and older population at $R\gtrsim R_e$ than the control samples. Considering the high incidence of kinematic misalignments in S0 galaxies and the properties of environments and stellar populations, we propose misaligned gas accretion as an important formation pathway for S0s.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： In this study we demonstrate that stellar masses of galaxies (Mstar) are universally correlated through a double power law function with the product of the dynamical velocities (Ve) and sizes to one-fourth power (Re^0.25) of galaxies, both measured at the effective radii. The product VeRe^0.25 represents the fourth root of the total binding energies within effective radii of galaxies. This stellar mass-binding energy correlation has an observed scatter of 0.14 dex in log(VeRe^0.25) and 0.46 dex in log(Mstar). It holds for a variety of galaxy types over a stellar mass range of nine orders of magnitude, with little evolution over cosmic time. A toy model of self-regulation between binding energies and supernovae feedback is shown to be able to reproduce the observed slopes, but the underlying physical mechanisms are still unclear. The correlation can be a potential distance estimator with an uncertainty of 0.2 dex independent of the galaxy type.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
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) the SN locations have smaller velocity dispersion, lower metallicity, and younger stellar population than galaxy centers. This is a natural result of radius gradients of all these parameters. The SN location and the 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.
Peer Review Status:Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： We select 753 S0 galaxies from the internal Product Lauch-10 of MaNGA survey (MPL-10) and find that $\sim$11% of S0 galaxies show gas-star kinematic misalignments, which is higher than the misaligned fraction in spiral ($\sim$1%) and elliptical galaxies ($\sim$6%) in MPL-10. If we only consider the emission-line galaxies (401 emission-line S0s), the misaligned fraction in S0s increases to $\sim$20%. In S0s, the kinematic misalignments are more common than the merger remnant features ($\sim$8%). Misaligned S0s have lower masses of stellar components and dark matter halos than S0s with merger remnant features. Based on the $NUV-r$ versus $M_*$ diagram, we split galaxies into three populations: blue cloud (BC), green valley (GV) and red sequence, finding that BC and GV misaligned S0s have positive $\mathrm{D}_n4000$ radial gradients which indicates younger stellar population in the central region than the outskirts. Through comparing the misaligned S0s with a control sample for the whole S0 galaxy sample, we find that the BC and GV misaligned S0s show younger stellar population at $R\lesssim R_e$ and older population at $R\gtrsim R_e$ than the control samples. Considering the high incidence of kinematic misalignments in S0 galaxies and the properties of environments and stellar populations, we propose misaligned gas accretion as an important formation pathway for S0s.
Peer Review Status:Awaiting Review
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