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We characterize the kinematic and chemical properties of $\sim$3,000Sagittarius (Sgr) stream stars, including K-giants, M-giants, and BHBs, selectfrom SEGUE-2, LAMOST, and SDSS separately in Integrals-of-Motion space. Theorbit 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 trailingsteam is $\sim$ 100 kpc. The metallicity distributions of Sgr K-, M-giants, andBHBs 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 thatthe trailing arm is on average more metal-rich than leading arm, and theK-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 halostars at lower metallicity ([Fe/H] $<\sim$ $-$1.0 dex), and then evolve down tolower [$\alpha$/Fe] than disk stars at higher metallicity, which is close tothe evolution pattern of $\alpha$-element of Milky Way dwarf galaxies. We find$V_Y$ and metallicity of K-giants have gradients along the direction ofline-of-sight from the Galactic center in $X$-$Z$ plane, and the K-giants showthat $V_Y$ increases with metallicity at [Fe/H] $>\sim-$1.5 dex. After dividingthe Sgr stream into bright and faint stream according to their locations inequatorial coordinate, the K-giants and BHBs show that the bright and faintstream present different $V_Y$ and metallicities, the bright stream is onaverage higher in $V_Y$ and metallicity than the faint stream.

Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars