Based on the updated M giant star catalog selected from Large Sky Area Multi-Object Fiber Spectroscopic Telescope DR9,we identify substructures within the integrals-of-motion space through the Friends-of-Friends clust...Based on the updated M giant star catalog selected from Large Sky Area Multi-Object Fiber Spectroscopic Telescope DR9,we identify substructures within the integrals-of-motion space through the Friends-of-Friends clustering algorithm.We obtain members belonging to several known substructures:the Sagittarius stream,Galactic Anticenter Substructure(GASS),Gaia-Enceladus-Sausage(GES),Splash,and the high-αdisk.Furthermore,we also identify two groups which cannot be clearly associated with previously known substructures.Our findings confirm the existence of metal-rich constituents within the GES,representing newly formed stars that originated from the metal-enriched gas delivered during the GES merger event and subsequently evolved.Additionally,this study further expands the sample of GASS,high-αdisk,and Splash stars.Analysis of these metal-rich M giant stars as members of the GES,Splash,and high-αdisk components supports an evolution scenario for the early Milky Way,as proposed by previous studies.In this scenario,stars initially formed in a high-α primordial disk were dynamically heated by the massive accretion event(GES).This process redistributed stellar orbits,creating the Splash population,while the undisturbed portion of the primordial disk persisted as the present-day high-αdisk component.展开更多
In our previous work,we identified~100,000 metal-poor stars([Fe/H]<-1.0)from the LAMOST Survey.This work estimates their chemical abundances and explores the origin and evolution of the Galactic metal-poor disk.Our...In our previous work,we identified~100,000 metal-poor stars([Fe/H]<-1.0)from the LAMOST Survey.This work estimates their chemical abundances and explores the origin and evolution of the Galactic metal-poor disk.Our chemo-dynamical analysis reveals four main populations within the metal-poor disk:(1)a primordial disk older than 12 Gyr with[Fe/H]>-1.5;(2)debris stars from the progenitor galaxy of Gaia±Sausage±Enceladus(GSE),but now residing in the Galactic disk;(3)the metal-poor tail of the metal-rich,high-αdisk formed10±12 Gyr ago,with metallicity lower limit extending to-2.0;(4)the metal-poor tail of the metal-rich,low-αdisk younger than 8 Gyr,reaching a lower metallicity limit of-1.8.These results reveal the presence of a primordial disk and show that both high-αand low-αdisks reach lower metallicities than previously thought.Analysis of merger debris reveals that Wukong,with extremely low metallicity,likely originates from merger events distinct from GSE.Additionally,three new substructures are identified:ShangGu-1,characterized by unusual[Fe/H]-eccentricity correlations;ShangGu-2,possibly heated disk stars;and ShangGu-3,which can be divided into four subgroups based on differing orbital directions,with two aligning with the previously known Nyx and Nyx-2.展开更多
The structural parameters of a galaxy can be used to gain insight into its formation and evolution history.In this paper,we strive to compare the Milky Way’s structural parameters to other,primarily edge-on,spiral ga...The structural parameters of a galaxy can be used to gain insight into its formation and evolution history.In this paper,we strive to compare the Milky Way’s structural parameters to other,primarily edge-on,spiral galaxies in order to determine how our Galaxy measures up to the Local Universe.For our comparison,we use the galaxy structural parameters gathered from a variety of literature sources in the optical and near-infrared wave bands.We compare the scale length,scale height,and disk flatness for both the thin and thick disks,the thick-to-thin disk mass ratio,the bulge-to-total luminosity ratio,and the mean pitch angle of the Milky Way’s spiral arms to those in other galaxies.We conclude that many of the Milky Way’s structural parameters are largely ordinary and typical of spiral galaxies in the Local Universe,though the Galaxy’s thick disk appears to be appreciably thinner and less extended than expected from zoom-in cosmological simulations of Milky Way-mass galaxies with a significant contribution of galaxy mergers involving satellite galaxies.展开更多
We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data,taking into account selection effects.We assume the selection function,which can be altered during...We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data,taking into account selection effects.We assume the selection function,which can be altered during observations and data reductions,of the spectroscopic survey is based on photometric colors and magnitude.Then the underlying selection function for a line-of-sight can be recovered well by comparing the distribution of the spectroscopic stars in a color-magnitude plane with that of the photometric dataset.Subsequently,the stellar density profile along a line-of-sight can be derived from the spectroscopically measured stellar density profile multiplied by the selection function.The method is validated using Galaxia mock data with two different selection functions.We demonstrate that the derived stellar density profiles reconstruct the true ones well not only for the full set of targets,but also for sub-populations selected from the full dataset.Finally,the method is applied to map the density pro-files for the Galactic disk and halo,using the LAMOST RGB stars.The Galactic disk extends to about R=19 kpc,where the disk still contributes about 10%to the total stellar surface density.Beyond this radius,the disk smoothly transitions to the halo without any truncation,bending or breaking.Moreover,no over-density corresponding to the Monoceros ring is found in the Galactic anti-center direction.The disk shows moderate north-south asymmetry at radii larger than 12 kpc.On the other hand,the R-Z tomographic map directly shows that the stellar halo is substantially oblate within a Galactocentric radius of 20 kpc and gradually becomes nearly spherical beyond 30 kpc.展开更多
We report a detailed investigation of the bulk motions of the nearby Galactic stellar disk, based on three samples selected from the LSS-GAC DR2： a global sample containing 0.57 million FGK dwarfs out to ～2 kpc, a l...We report a detailed investigation of the bulk motions of the nearby Galactic stellar disk, based on three samples selected from the LSS-GAC DR2： a global sample containing 0.57 million FGK dwarfs out to ～2 kpc, a local subset of the global sample consisting of ～5400 stars within 150 pc, and an anti-center sample containing ～4400AFGK dwarfs and red clump stars within windows a few degrees wide centered on the Galactic Anti-center. The global sample is used to construct a three-dimensional map of bulk motions of the Galactic disk from the solar vicinity out to ～2 kpc with a spatial resolution of ～250 pc. Typical values of the radial and vertical components of bulk motion range from-15 km s-1to 15 km s-1; in contrast, the lag behind the circular motion dominates the azimuthal component by up to ～15 km s-1. The map reveals spatially coherent, kpc-scale stellar flows in the disk, with typical velocities of a few tens of km s-1. Bending- and breathing-mode perturbations are clearly visible,and vary smoothly across the disk plane. Our data also reveal higher-order perturbations, such as breaks and ripples, in the profiles of vertical motion versus height. From the local sample, we find that stars from different populations exhibit very different patterns of bulk motion. Finally, the anti-center sample reveals a number of peaks in stellar number density in the line-of-sight velocity versus distance distribution, with the nearer ones apparently related to the known moving groups. The ＂velocity bifurcation＂ reported by Liu et al. at Galactocentric radii 10–11 kpc is confirmed. However,just beyond this distance, our data also reveal a new triple-peaked structure.展开更多
This paper is an initial stage of consideration of the general problem of joint modeling of the vertical structure of a Galactic flat subsystem and the average surface of the disk of the Galaxy,taking into account the...This paper is an initial stage of consideration of the general problem of joint modeling of the vertical structure of a Galactic flat subsystem and the average surface of the disk of the Galaxy,taking into account the natural and measurement dispersions.We approximate the average surface of the Galactic disk in the region covered by the data with a general(polynomial)model and determine its parameters by minimizing the squared deviations of objects along the normal to the model surface.The smoothness of the model,i.e.,its order n,is optimized.An outlier elimination algorithm is applied.The developed method allows us to simultaneously identify significant details of the Galactic warping and estimate the offset z_(⊙) of the Sun relative to the average(in general,non-flat)surface of the Galactic disk and the vertical scale of the object system under consideration for an arbitrary area of the disk covered by data.The method is applied to data on classical Cepheids.Significant local extremes of the average disk surface model were found based on Cepheid data:the minimum in the first Galactic quadrant and the maximum in the second.A well-known warp(lowering of the disk surface)in the third quadrant has been confirmed.The optimal order of the model describing all these warping details was found to be n_(o)=4.The local(for a small neighborhood of the Sun,n_(o)=0)estimate of z_(⊙)=28.1±6.1|_(stat).±1.3|_(cal).pc is close to the non-local(taking into account warping,n_(o)=4)z_(⊙)=27.1±8.8|_(stat.-1.2)^(+1.3)|_(cal).pc(statistical and calibration uncertainties are indicated),which suggests that the proposed modeling method eliminates the influence of warping on the z_(⊙) estimate.However,the non-local estimate of the vertical standard deviation of Cepheids σ_(p)=132.0±3.7|_(stat.-5.9)^(+6.3)|_(cal).pc differs significantly from the local σ_(ρ)=76.5±4.4|_(stat.-3.4)^(+3.6)|_(cal).pc,which implies the need to introduce more complex models for the vertical distribution outside the Sun’s vicinity.展开更多
基金supported by the National Key Research and Development Program of China No.2024YFA1611902the National Natural Science Foundation of China(NSFC)under grants Nos.12273027 and 12588202+3 种基金the Innovation Team Funds of China West Normal University under grant No.KCXTD2022-6CAS Project for Young Scientists in Basic Research under grants Nos.YSBR-062 and YSBR-092the Strategic Priority Research Program of Chinese Academy of Sciences under grant No.XDB1160102the science research grant from the China Manned Space Project with No.CMS-CSST-2025-A11.
文摘Based on the updated M giant star catalog selected from Large Sky Area Multi-Object Fiber Spectroscopic Telescope DR9,we identify substructures within the integrals-of-motion space through the Friends-of-Friends clustering algorithm.We obtain members belonging to several known substructures:the Sagittarius stream,Galactic Anticenter Substructure(GASS),Gaia-Enceladus-Sausage(GES),Splash,and the high-αdisk.Furthermore,we also identify two groups which cannot be clearly associated with previously known substructures.Our findings confirm the existence of metal-rich constituents within the GES,representing newly formed stars that originated from the metal-enriched gas delivered during the GES merger event and subsequently evolved.Additionally,this study further expands the sample of GASS,high-αdisk,and Splash stars.Analysis of these metal-rich M giant stars as members of the GES,Splash,and high-αdisk components supports an evolution scenario for the early Milky Way,as proposed by previous studies.In this scenario,stars initially formed in a high-α primordial disk were dynamically heated by the massive accretion event(GES).This process redistributed stellar orbits,creating the Splash population,while the undisturbed portion of the primordial disk persisted as the present-day high-αdisk component.
基金supported by the National Natural Science Foundation of China(NSFC,grant Nos.11988101 and12222305)National Key R&D Program of China No.2024YFA1611900Guoshoujing Telescope(the Large Sky Area Multi-Object Fiber Spectroscopic Telescope,LAMOST)is a National Major Scientific Project built by the Chinese Academy of Sciences。
文摘In our previous work,we identified~100,000 metal-poor stars([Fe/H]<-1.0)from the LAMOST Survey.This work estimates their chemical abundances and explores the origin and evolution of the Galactic metal-poor disk.Our chemo-dynamical analysis reveals four main populations within the metal-poor disk:(1)a primordial disk older than 12 Gyr with[Fe/H]>-1.5;(2)debris stars from the progenitor galaxy of Gaia±Sausage±Enceladus(GSE),but now residing in the Galactic disk;(3)the metal-poor tail of the metal-rich,high-αdisk formed10±12 Gyr ago,with metallicity lower limit extending to-2.0;(4)the metal-poor tail of the metal-rich,low-αdisk younger than 8 Gyr,reaching a lower metallicity limit of-1.8.These results reveal the presence of a primordial disk and show that both high-αand low-αdisks reach lower metallicities than previously thought.Analysis of merger debris reveals that Wukong,with extremely low metallicity,likely originates from merger events distinct from GSE.Additionally,three new substructures are identified:ShangGu-1,characterized by unusual[Fe/H]-eccentricity correlations;ShangGu-2,possibly heated disk stars;and ShangGu-3,which can be divided into four subgroups based on differing orbital directions,with two aligning with the previously known Nyx and Nyx-2.
文摘The structural parameters of a galaxy can be used to gain insight into its formation and evolution history.In this paper,we strive to compare the Milky Way’s structural parameters to other,primarily edge-on,spiral galaxies in order to determine how our Galaxy measures up to the Local Universe.For our comparison,we use the galaxy structural parameters gathered from a variety of literature sources in the optical and near-infrared wave bands.We compare the scale length,scale height,and disk flatness for both the thin and thick disks,the thick-to-thin disk mass ratio,the bulge-to-total luminosity ratio,and the mean pitch angle of the Milky Way’s spiral arms to those in other galaxies.We conclude that many of the Milky Way’s structural parameters are largely ordinary and typical of spiral galaxies in the Local Universe,though the Galaxy’s thick disk appears to be appreciably thinner and less extended than expected from zoom-in cosmological simulations of Milky Way-mass galaxies with a significant contribution of galaxy mergers involving satellite galaxies.
基金supported by the Strategic Priority Research Program“The Emergence of Cosmological Structures”of the Chinese Academy of Sciences(Grant No.XDB09000000)the National Key Basic Research Program of China(2014CB845700)+1 种基金the National Natural Science Foundation of China(Grant Nos.11373032 and 11333003)a National Major Scientific Project built by the Chinese Academy of Sciences.Funding for the project has been provided by the project has been provided by the National Development and Reform Commission
文摘We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data,taking into account selection effects.We assume the selection function,which can be altered during observations and data reductions,of the spectroscopic survey is based on photometric colors and magnitude.Then the underlying selection function for a line-of-sight can be recovered well by comparing the distribution of the spectroscopic stars in a color-magnitude plane with that of the photometric dataset.Subsequently,the stellar density profile along a line-of-sight can be derived from the spectroscopically measured stellar density profile multiplied by the selection function.The method is validated using Galaxia mock data with two different selection functions.We demonstrate that the derived stellar density profiles reconstruct the true ones well not only for the full set of targets,but also for sub-populations selected from the full dataset.Finally,the method is applied to map the density pro-files for the Galactic disk and halo,using the LAMOST RGB stars.The Galactic disk extends to about R=19 kpc,where the disk still contributes about 10%to the total stellar surface density.Beyond this radius,the disk smoothly transitions to the halo without any truncation,bending or breaking.Moreover,no over-density corresponding to the Monoceros ring is found in the Galactic anti-center direction.The disk shows moderate north-south asymmetry at radii larger than 12 kpc.On the other hand,the R-Z tomographic map directly shows that the stellar halo is substantially oblate within a Galactocentric radius of 20 kpc and gradually becomes nearly spherical beyond 30 kpc.
基金supported by the National Key Basic Research Program of China (2014CB845700)
文摘We report a detailed investigation of the bulk motions of the nearby Galactic stellar disk, based on three samples selected from the LSS-GAC DR2： a global sample containing 0.57 million FGK dwarfs out to ～2 kpc, a local subset of the global sample consisting of ～5400 stars within 150 pc, and an anti-center sample containing ～4400AFGK dwarfs and red clump stars within windows a few degrees wide centered on the Galactic Anti-center. The global sample is used to construct a three-dimensional map of bulk motions of the Galactic disk from the solar vicinity out to ～2 kpc with a spatial resolution of ～250 pc. Typical values of the radial and vertical components of bulk motion range from-15 km s-1to 15 km s-1; in contrast, the lag behind the circular motion dominates the azimuthal component by up to ～15 km s-1. The map reveals spatially coherent, kpc-scale stellar flows in the disk, with typical velocities of a few tens of km s-1. Bending- and breathing-mode perturbations are clearly visible,and vary smoothly across the disk plane. Our data also reveal higher-order perturbations, such as breaks and ripples, in the profiles of vertical motion versus height. From the local sample, we find that stars from different populations exhibit very different patterns of bulk motion. Finally, the anti-center sample reveals a number of peaks in stellar number density in the line-of-sight velocity versus distance distribution, with the nearer ones apparently related to the known moving groups. The ＂velocity bifurcation＂ reported by Liu et al. at Galactocentric radii 10–11 kpc is confirmed. However,just beyond this distance, our data also reveal a new triple-peaked structure.
文摘This paper is an initial stage of consideration of the general problem of joint modeling of the vertical structure of a Galactic flat subsystem and the average surface of the disk of the Galaxy,taking into account the natural and measurement dispersions.We approximate the average surface of the Galactic disk in the region covered by the data with a general(polynomial)model and determine its parameters by minimizing the squared deviations of objects along the normal to the model surface.The smoothness of the model,i.e.,its order n,is optimized.An outlier elimination algorithm is applied.The developed method allows us to simultaneously identify significant details of the Galactic warping and estimate the offset z_(⊙) of the Sun relative to the average(in general,non-flat)surface of the Galactic disk and the vertical scale of the object system under consideration for an arbitrary area of the disk covered by data.The method is applied to data on classical Cepheids.Significant local extremes of the average disk surface model were found based on Cepheid data:the minimum in the first Galactic quadrant and the maximum in the second.A well-known warp(lowering of the disk surface)in the third quadrant has been confirmed.The optimal order of the model describing all these warping details was found to be n_(o)=4.The local(for a small neighborhood of the Sun,n_(o)=0)estimate of z_(⊙)=28.1±6.1|_(stat).±1.3|_(cal).pc is close to the non-local(taking into account warping,n_(o)=4)z_(⊙)=27.1±8.8|_(stat.-1.2)^(+1.3)|_(cal).pc(statistical and calibration uncertainties are indicated),which suggests that the proposed modeling method eliminates the influence of warping on the z_(⊙) estimate.However,the non-local estimate of the vertical standard deviation of Cepheids σ_(p)=132.0±3.7|_(stat.-5.9)^(+6.3)|_(cal).pc differs significantly from the local σ_(ρ)=76.5±4.4|_(stat.-3.4)^(+3.6)|_(cal).pc,which implies the need to introduce more complex models for the vertical distribution outside the Sun’s vicinity.
