Member Stars of the GD-1 Tidal Stream from the SDSS, LAMOST, and Gaia Surveys

Huang, Y.; Chen, B. -Q.; Zhang, H. -W.; Yuan, H. -B.; Xiang, M. -S.; Wang, C.; Tian, Z. -J.; Liu, X. -W.

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Journal Article

Member Stars of the GD-1 Tidal Stream from the SDSS, LAMOST, and Gaia Surveys

MPS-Authors

Huang, Y.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chen, B. -Q.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zhang, H. -W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Yuan, H. -B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Xiang, M. -S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tian, Z. -J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu, X. -W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2019ApJ...877...13H
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Citation

Huang, Y., Chen, B.-.-Q., Zhang, H.-.-W., Yuan, H.-.-B., Xiang, M.-.-S., Wang, C., et al. (2019). Member Stars of the GD-1 Tidal Stream from the SDSS, LAMOST, and Gaia Surveys. The Astrophysical Journal, 877.

Cite as: https://hdl.handle.net/21.11116/0000-0005-D0E6-C

Abstract

With the photometric data from the SDSS survey, the spectroscopic data from the SDSS/SEGUE and the LAMOST surveys, and the astrometric data from the Gaia DR2, we have identified 67 highly probable member stars of the GD-1 cold stellar stream spread along almost its entire length (i.e., from 126¬∞ to 203¬∞ in R.A.). With the accurate spectroscopic (i.e., metallicity and line-of-sight velocity) and astrometric (i.e., proper motions) information, the position-velocity diagrams, i.e., œï ₁-Œº _Œ±, œï ₁-Œº _Œ¥, and œï ₁-v _gsr, of the GD-1 stream are well mapped. The stream has an average metallicity [Fe/H] = ‚àí1.96. The rich information of member stars of the stream now available allow one not only to model its origin, but also to place strong constraints on the mass distribution and the gravitational potential of the Milky Way.