Differential Rotation of the Halo Traced by K-giant Stars

We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling the rotational velocity distribution with both the halo and disk components, we find that the rotational velocity of the halo population dec...

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Published inThe Astrophysical journal Vol. 899; no. 2; pp. 110 - 121
Main Authors Tian, Hao, Liu, Chao, Wang, Yougang, Xu, Yan, Yang, Chengqun, Zhang, Bo, Xue, Xiang-Xiang
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.08.2020
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Abstract We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling the rotational velocity distribution with both the halo and disk components, we find that the rotational velocity of the halo population decreases almost linearly with increasing vertical distance to the Galactic disk plane, Z, at fixed galactocentric radius, R. The samples are separated into two parts with and . We derive that the decreasing rates along Z for the two subsamples are −3.07 0.63 and −1.89 0.37 km s−1 kpc−1, respectively. Comparing with the TNG simulations, we suggest that this trend is caused by the interaction between the disk and halo. The results from the simulations show that only an oblate halo can provide a decreasing rotational velocity with increasing Z. This indicates that the Galactic halo is oblate with galactocentric radius . On the other hand, the flaring of the disk component (mainly the thick disk) is clearly traced by this study; with R between 12 and 20 kpc, the disk can vertically extend to above the disk plane. What is more interesting is that we find the Gaia-Enceladus-Sausage component has a significant contribution only in the halo with , i.e., a fraction of 23%-47%, while in the outer subsample, the contribution is too low to be well constrained.
AbstractList We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling the rotational velocity distribution with both the halo and disk components, we find that the rotational velocity of the halo population decreases almost linearly with increasing vertical distance to the Galactic disk plane, Z, at fixed galactocentric radius, R. The samples are separated into two parts with and . We derive that the decreasing rates along Z for the two subsamples are −3.07 0.63 and −1.89 0.37 km s−1 kpc−1, respectively. Comparing with the TNG simulations, we suggest that this trend is caused by the interaction between the disk and halo. The results from the simulations show that only an oblate halo can provide a decreasing rotational velocity with increasing Z. This indicates that the Galactic halo is oblate with galactocentric radius . On the other hand, the flaring of the disk component (mainly the thick disk) is clearly traced by this study; with R between 12 and 20 kpc, the disk can vertically extend to above the disk plane. What is more interesting is that we find the Gaia-Enceladus-Sausage component has a significant contribution only in the halo with , i.e., a fraction of 23%-47%, while in the outer subsample, the contribution is too low to be well constrained.
We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling the rotational velocity distribution with both the halo and disk components, we find that the rotational velocity of the halo population decreases almost linearly with increasing vertical distance to the Galactic disk plane, Z, at fixed galactocentric radius, R. The samples are separated into two parts with \(6\lt R\lt 12\,\mathrm{kpc}\) and \(12\lt R\lt 20\,\mathrm{kpc}\). We derive that the decreasing rates along Z for the two subsamples are −3.07 ± 0.63 and −1.89 ± 0.37 km s−1 kpc−1, respectively. Comparing with the TNG simulations, we suggest that this trend is caused by the interaction between the disk and halo. The results from the simulations show that only an oblate halo can provide a decreasing rotational velocity with increasing Z. This indicates that the Galactic halo is oblate with galactocentric radius \(R\lt 20\,\mathrm{kpc}\). On the other hand, the flaring of the disk component (mainly the thick disk) is clearly traced by this study; with R between 12 and 20 kpc, the disk can vertically extend to \(6\sim 10\,\mathrm{kpc}\) above the disk plane. What is more interesting is that we find the Gaia–Enceladus–Sausage component has a significant contribution only in the halo with \(R\lt 12\,\mathrm{kpc}\), i.e., a fraction of 23%–47%, while in the outer subsample, the contribution is too low to be well constrained.
We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling the rotational velocity distribution with both the halo and disk components, we find that the rotational velocity of the halo population decreases almost linearly with increasing vertical distance to the Galactic disk plane, Z , at fixed galactocentric radius, R . The samples are separated into two parts with and . We derive that the decreasing rates along Z for the two subsamples are −3.07 ± 0.63 and −1.89 ± 0.37 km s −1 kpc −1 , respectively. Comparing with the TNG simulations, we suggest that this trend is caused by the interaction between the disk and halo. The results from the simulations show that only an oblate halo can provide a decreasing rotational velocity with increasing Z . This indicates that the Galactic halo is oblate with galactocentric radius . On the other hand, the flaring of the disk component (mainly the thick disk) is clearly traced by this study; with R between 12 and 20 kpc, the disk can vertically extend to above the disk plane. What is more interesting is that we find the Gaia–Enceladus–Sausage component has a significant contribution only in the halo with , i.e., a fraction of 23%–47%, while in the outer subsample, the contribution is too low to be well constrained.
Author Liu, Chao
Xu, Yan
Yang, Chengqun
Zhang, Bo
Tian, Hao
Wang, Yougang
Xue, Xiang-Xiang
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Snippet We use K-giant stars selected from the LAMOST DR5 to study the variation of the rotational velocity of the Galactic halo at different space positions. Modeling...
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SubjectTerms Astronomical models
Astrophysics
Computer simulation
Differential rotation
Enceladus
Galactic disk
Galactic halos
Giant stars
K giant stars
Milky Way disk
Milky Way dynamics
Milky Way evolution
Milky Way Galaxy
Milky Way rotation
Milky Way stellar halo
Velocity
Velocity distribution
Title Differential Rotation of the Halo Traced by K-giant Stars
URI https://iopscience.iop.org/article/10.3847/1538-4357/aba1ec
https://www.proquest.com/docview/2434864160
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