Hostname: page-component-586b7cd67f-g8jcs Total loading time: 0 Render date: 2024-11-26T17:51:09.999Z Has data issue: false hasContentIssue false
  • English
  • Français

A 3D map of the Milky Way’s disk as traced by classical Cepheids

Published online by Cambridge University Press:  14 May 2020

Xiaodian Chen Open the ORCID record for Xiaodian Chen [Opens in a new window] ,
Shu Wang ,
Licai Deng ,
Richard de Grijs ,
Chao Liu Open the ORCID record for Chao Liu [Opens in a new window]  and
Hao Tian Open the ORCID record for Hao Tian [Opens in a new window]
Xiaodian Chen
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China email: [email protected]
Shu Wang
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China email: [email protected]
Licai Deng
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China email: [email protected] Department of Astronomy, China West Normal University, Nanchong637009, China
Richard de Grijs
Affiliation:
Department of Physics and Astronomy, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia Research Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia International Space Science Institute–Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing100190, China
Chao Liu
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China email: [email protected]
Hao Tian
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, 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.

We have collected 2330 Cepheids to establish an intuitive 3D map of the Milky Way’s disk. As regards the warp amplitude, the Cepheid disk agrees well with the gas disk for radii up to 15 kpc. However, the mean line of nodes (LON) of the Cepheid disk deviates from the Galactic Center–Sun direction by 17.5±1.0°. This is a new and different result compared with previous results. The LON is not stable at any given radius, but it twists. The twisted pattern suggests that the formation of the Milky Way’s warp is dominated by the massive inner disk. The kinematic warp defined by the Cepheids is also in concordance with the spatial warp. In the 2020 era, the anticipated increasing number of new Cepheids will provide a key opportunity to view our Milky Way’s disk as a whole, and we expect that our knowledge of the disk’s main structural features will be much improved.

Keywords

Galaxy: diskGalaxy: structurestars: variables: Cepheidsstars: distances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 6 - 9
Copyright
© International Astronomical Union 2020

References

Chen, X., de Grijs, R., & Deng, L. 2017, MNRAS, 464, 111910.1093/mnras/stw2390CrossRefGoogle Scholar
Chen, X., Wang, S., Deng, L., et al. 2018, ApJ, 859, 13710.3847/1538-4357/aabfbcCrossRefGoogle Scholar
Chen, X., Wang, S., Deng, L., et al. 2018, ApJS, 237, 2810.3847/1538-4365/aad32bCrossRefGoogle Scholar
Chen, X., Wang, S., Deng, L., et al. 2019, Nat. Astron., 3, 32010.1038/s41550-018-0686-7CrossRefGoogle Scholar
Drimmel, R. & Spergel, D. N. 2001, ApJ, 556, 18110.1086/321556CrossRefGoogle Scholar
Heinze, A. N., Tonry, J. L., Denneau, L., et al. 2018, AJ, 156, 24110.3847/1538-3881/aae47fCrossRefGoogle Scholar
Jayasinghe, T., Kochanek, C. S., Stanek, K. Z., et al. 2018, MNRAS, 477, 314510.1093/mnras/sty838CrossRefGoogle Scholar
Levine, E. S., Blitz, L., & Heiles, C. 2006, ApJ, 643, 88110.1086/503091CrossRefGoogle Scholar
López-Corredoira, M., Cabrera-Lavers, A., Garzón, F., et al. 2002, A&A, 394, 883Google Scholar
Poggio, E., Drimmel, R., Lattanzi, M. G., et al. 2018, MNRAS, 481, L2110.1093/mnrasl/sly148CrossRefGoogle Scholar
Ripepi, V., Molinaro, R., Musella, I., et al. 2019, A&A, 625, A14Google Scholar
Romero-Gómez, M., Mateu, C., Aguilar, L., et al. 2019, A&A, 627, A150Google Scholar
Shen, J. & Sellwood, J. A. 2006, MNRAS, 370, 210.1111/j.1365-2966.2006.10477.xCrossRefGoogle Scholar
Skowron, D. M., Skowron, J., Mróz, P., et al. 2019, Science, 365, 47810.1126/science.aau3181CrossRefGoogle Scholar
Wang, S., Chen, X., de Grijs, R., et al. 2018, ApJ, 852, 7810.3847/1538-4357/aa9d99CrossRefGoogle Scholar
Wang, S. & Chen, X. 2019, ApJ, 877, 11610.3847/1538-4357/ab1c61CrossRefGoogle Scholar