LAMOST Spectroscopic Survey of the Galactic Anticentre (LSS-GAC): the second release of value-added catalogues

Xiang, Maosheng; Liu, X.-W.; Yuan, Haibo; Huo, Zhi-Ying; Huang, Yang; Wang, C.; Chen, Bingqiu; Ren, Juanjuan; Zhang, H.-W.; Tian, Zhijia; Yang, Y. G.; Shi, Jianrong; Zhao, Jingkun; Li, J.; Zhao, Yi; Cui, Xiangqun; Li, G.-P.; Hou, Yonghui; Zhang, Y.; Zhang, W.; Wang, J.-L.; Wu, Yue; Cao, Zihuang; Yan, Han; Yan, Tai-Sheng; Luo, A-Li; Zhang, H.-T.; Bai, Zhong-Rui; Yuan, Hailong; Dong, Yiqiao; Lei, Ya-Juan; Li, G.-W.

doi:10.1093/mnras/stx129

Cited by 68 publications

(48 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Note that the M V is derived directly from the spectra with a multivariate regression method based on kernel-based principal component analysis (KPCA), utilizing the LAMOST and Hipparcos ) common stars as training dataset (Xiang et al 2017b,c). With the absolute magnitudes, stellar distance is deduced from the distance modulus, utilizing interstellar extinction derived with the 'star pair' method (Yuan et al 2013Xiang et al 2017c). A comparison with distance inferred from the Gaia TGAS parallax (Gaia Collaboration et al 2016) indicates that our distance estimates reach a precision of 12% given the relatively high spectral S/N of the LAMOST-TGAS common stars, and the systematic error is negligible.…”

Section: The Data Samplementioning

confidence: 90%

Stellar Mass Distribution and Star Formation History of the Galactic Disk Revealed by Mono-age Stellar Populations from LAMOST

Xiang¹,

Shi²,

Liu³

et al. 2018

ApJS

View full text Add to dashboard Cite

We present a detailed determination and analysis of 3D stellar mass distribution of the Galactic disk for mono-age populations using a sample of 0.93 million main-sequence turn-off and subgiant stars from the LAMOST Galactic Surveys. Our results show (1) all stellar populations younger than 10 Gyr exhibit strong disk flaring, which is accompanied with a dumpy vertical density profile that is best described by a sech n function with index depending on both radius and age; (2) Asymmetries and wave-like oscillations are presented in both the radial and vertical direction, with strength varying with stellar populations; (3) As a contribution by the Local spiral arm, the mid-plane stellar mass density at solar radius but 400-800 pc (3-6 • ) away from the Sun in the azimuthal direction has a value of 0.0594 ± 0.0008 M ⊙ /pc 3 , which is 0.0164 M ⊙ /pc 3 higher than previous estimates at the solar neighborhood. The result causes doubts on the current estimate of local dark matter density; (4) The radial distribution of surface mass density yields a disk scale length evolving from ∼4 kpc for the young to ∼2 kpc for the old populations. The overall population exhibits a disk scale length of 2.48 ± 0.05 kpc, and a total stellar mass of 3.6(±0.1) × 10 10 M ⊙ assuming R ⊙ = 8.0 kpc, and the value becomes 4.1(±0.1) × 10 10 M ⊙ if R ⊙ = 8.3 kpc; (5) The disk has a peak star formation rate (SFR) changing from 6-8 Gyr at the inner to 4-6 Gyr ago at the outer part, indicating an inside-out assemblage history. The 0-1 Gyr population yields a recent disk total SFR of 1.96 ± 0.12 M ⊙ /yr.

show abstract

Section: The Data Samplementioning

confidence: 90%

Stellar Mass Distribution and Star Formation History of the Galactic Disk Revealed by Mono-age Stellar Populations from LAMOST

Xiang¹,

Shi²,

Liu³

et al. 2018

ApJS

View full text Add to dashboard Cite

show abstract

“…We separately analyse the velocity ellipsoids generated from the combination of 5d phase space information from Gaia DR2 (Brown et al 2018), together with radial velocities from the LAMOST DR4 value added catalogue (Cui et al 2012;Xiang et al 2017). This enables us to analyse the velocity ellipsoids with an independent catalogue of stars.…”

Section: The Lamost Dr4 and Gaia Dr2mentioning

confidence: 99%

The tilt of the local velocity ellipsoid as seen by Gaia

Everall

Evans

Belokurov

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The Gaia Radial Velocity Spectrometer (RVS) provides a sample of 7 224 631 stars with full six-dimensional phase space information. Bayesian distances of these stars are available from the catalogue of Schönrich et al. (2019). We exploit this to map out the behaviour of the velocity ellipsoid within 5 kpc of the Sun. We find that the tilt of the disc-dominated RVS sample is accurately described by the relation α = (0.952 ± 0.007) arctan(|z|/R), where (R, z) are cylindrical polar coordinates. This corresponds to velocity ellipsoids close to spherical alignment (for which the normalising constant would be unity) and pointing towards the Galactic centre. Flattening of the tilt of the velocity ellipsoids is enhanced close to the plane and Galactic centre, whilst at high elevations far from the Galactic center the population is consistent with exact spherical alignment. Using the LAMOST catalogue cross-matched with Gaia DR2, we construct thin disc and halo samples of reasonable purity based on metallicity. We find that the tilt of thin disc stars straddles α = (0.909 − 1.038) arctan(|z|/R), and of halo stars straddles α = (0.927 − 1.063) arctan(|z|/R). We caution against the use of reciprocal parallax for distances in studies of the tilt, as this can lead to serious artefacts.

show abstract

“…We build a sample of 5,175 RC stars from Ting et al 2018 which is constructed using data from the APOGEE (Apache Point Observatory Galactic Evolution Experiment, Majewski et al 2017) and LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope, Xiang et al 2017) surveys. Ting et al 2018 build a RC sample of 92,249 Milky Way stars from APOGEE DR14 and LAMOST DR3 data with ∼ 3% contamination from red giant stars.…”

Section: Red Clump Datamentioning

confidence: 99%

An Ultraviolet–Optical Color–Metallicity Relation for Red Clump Stars Using GALEX and Gaia

Mohammed

Schiminovich

Hawkins

et al. 2019

ApJ

View full text Add to dashboard Cite

Although core helium-burning red clump (RC) stars are faint at ultraviolet wavelengths, their ultraviolet-optical color is a unique and accessible probe of their physical properties. Using data from the GALEX All Sky Imaging Survey, Gaia Data Release 2 and the SDSS APOGEE DR14 survey, we find that spectroscopic metallicity is strongly correlated with the location of an RC star in the UVoptical color magnitude diagram. The RC has a wide spread in (NUV -G) 0 color, over 4 magnitudes, compared to a 0.7-magnitude range in (G BP -G RP ) 0 . We propose a photometric, dust-corrected, ultraviolet-optical (NUV -G) 0 color-metallicity [Fe/H] relation using a sample of 5,175 RC stars from APOGEE. We show that this relation has a scatter of 0.28 dex and is easier to obtain for large, wide-field samples than spectroscopic metallicities. Importantly, the effect may be comparable to the spread in RC color attributed to extinction in other studies.

show abstract

LAMOST Spectroscopic Survey of the Galactic Anticentre (LSS-GAC): the second release of value-added catalogues

Cited by 68 publications

References 30 publications

Stellar Mass Distribution and Star Formation History of the Galactic Disk Revealed by Mono-age Stellar Populations from LAMOST

Stellar Mass Distribution and Star Formation History of the Galactic Disk Revealed by Mono-age Stellar Populations from LAMOST

The tilt of the local velocity ellipsoid as seen by Gaia

An Ultraviolet–Optical Color–Metallicity Relation for Red Clump Stars Using GALEX and Gaia

Contact Info

Product

Resources

About