Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-18T23:06:24.459Z Has data issue: false hasContentIssue false
  • English
  • Français

Galactic disk structure as revealed by LAMOST A stars

Published online by Cambridge University Press:  07 March 2018

B.-Q. Chen ,
X.-W. Liu ,
H.-B. Yuan ,
Y. Huang ,
M.-S. Xiang ,
C. Wang ,
Z.-J. Tian  and
H.-W. Zhang
B.-Q. Chen
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected] LAMOST fellow
X.-W. Liu
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected]
H.-B. Yuan
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing100875, P.R.China
Y. Huang
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected] LAMOST fellow
M.-S. Xiang
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing100012, P.R.China LAMOST fellow
C. Wang
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected]
Z.-J. Tian
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected] LAMOST fellow
H.-W. Zhang
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P.R.China email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Using the spectroscopic distances of over 0.12 million A-type stars selected from the LAMOST Spectroscopic Survey of the Galactic Anti-center (LSS-GAC), we map their three-dimensional number density distributions in the Galaxy. These stellar number density maps allow an investigation of the Galactic young age thin disk structure with no a priori assumptions about the functional form of its components. The data show strong evidence for a significant flaring young disk. A more detail analysis show that the stellar flaring have different behaviours between the Northern and the Southern Galactic disks. The maps also reveal spatially coherent, kpc-scale stellar substructure in the thin disk. Finally, we detect the Perseus arm stellar overdensity at R ~ 10 kpc.

Keywords

Galaxy: diskGalaxy: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 208 - 209
Copyright
Copyright © International Astronomical Union 2018 

References

Chen, B.-Q., et al. 2017, MNRAS, 464, 2545 Google Scholar
Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1 Google Scholar
Liu, X.-W., et al. 2014, in IAU Symposium, Vol. 298, IAU Symposium, ed. Feltzing, S., Zhao, G., Walton, N. A., & Whitelock, P., 310–321Google Scholar
Sun, N.-C., et al. 2015, Research in Astronomy and Astrophysics, 15, 1342 Google Scholar
Xiang, M.-S., et al. 2017a, MNRAS, 464, 3657 CrossRefGoogle Scholar
Xiang, M.-S., et al. 2017b, MNRAS, 467, 1890 Google Scholar
Yuan, H.-B., et al. 2015, MNRAS, 448, 855 CrossRefGoogle Scholar