Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars. (arXiv:1909.12558v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yang_C/0/1/0/all/0/1">Chengqun Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_X/0/1/0/all/0/1">Xiang-Xiang Xue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jing Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">Chao Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Bo Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rix_H/0/1/0/all/0/1">Hans-Walter Rix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_L/0/1/0/all/0/1">Lan Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_G/0/1/0/all/0/1">Gang Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tian_H/0/1/0/all/0/1">Hao Tian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhong_J/0/1/0/all/0/1">Jing Zhong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xing_Q/0/1/0/all/0/1">Qianfan Xing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Y/0/1/0/all/0/1">Yaqian Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Chengdong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlin_J/0/1/0/all/0/1">Jeffrey L. Carlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_J/0/1/0/all/0/1">Jiang Chang</a>

We characterize the kinematic and chemical properties of $sim$3,000
Sagittarius (Sgr) stream stars, including K-giants, M-giants, and BHBs, select
from SEGUE-2, LAMOST, and SDSS separately in Integrals-of-Motion space. The
orbit of Sgr stream is quite clear from the velocity vector in $X$-$Z$ plane.
Stars traced by K-giants and M-giants present the apogalacticon of trailing
steam is $sim$ 100 kpc. The metallicity distributions of Sgr K-, M-giants, and
BHBs present that the M-giants are on average the most metal-rich population,
followed by K-giants and BHBs. All of the K-, M-giants, and BHBs indicate that
the trailing arm is on average more metal-rich than leading arm, and the
K-giants show that the Sgr debris is the most metal-poor part. The
$alpha$-abundance of Sgr stars exhibits a similar trend with the Galactic halo
stars at lower metallicity ([Fe/H] $sim-$1.5 dex. After dividing
the Sgr stream into bright and faint stream according to their locations in
equatorial coordinate, the K-giants and BHBs show that the bright and faint
stream present different $V_Y$ and metallicities, the bright stream is on
average higher in $V_Y$ and metallicity than the faint stream.

We characterize the kinematic and chemical properties of $sim$3,000
Sagittarius (Sgr) stream stars, including K-giants, M-giants, and BHBs, select
from SEGUE-2, LAMOST, and SDSS separately in Integrals-of-Motion space. The
orbit of Sgr stream is quite clear from the velocity vector in $X$-$Z$ plane.
Stars traced by K-giants and M-giants present the apogalacticon of trailing
steam is $sim$ 100 kpc. The metallicity distributions of Sgr K-, M-giants, and
BHBs present that the M-giants are on average the most metal-rich population,
followed by K-giants and BHBs. All of the K-, M-giants, and BHBs indicate that
the trailing arm is on average more metal-rich than leading arm, and the
K-giants show that the Sgr debris is the most metal-poor part. The
$alpha$-abundance of Sgr stars exhibits a similar trend with the Galactic halo
stars at lower metallicity ([Fe/H] $<sim$ $-$1.0 dex), and then evolve down to
lower [$alpha$/Fe] than disk stars at higher metallicity, which is close to
the evolution pattern of $alpha$-element of Milky Way dwarf galaxies. We find
$V_Y$ and metallicity of K-giants have gradients along the direction of
line-of-sight from the Galactic center in $X$-$Z$ plane, and the K-giants show
that $V_Y$ increases with metallicity at [Fe/H] $>sim-$1.5 dex. After dividing
the Sgr stream into bright and faint stream according to their locations in
equatorial coordinate, the K-giants and BHBs show that the bright and faint
stream present different $V_Y$ and metallicities, the bright stream is on
average higher in $V_Y$ and metallicity than the faint stream.

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