Table 1.

The properties of the simulated galaxies at |$z=0$|⁠. The columns are (1) model name; (2) halo mass defined by the FoF algorithm; (3) halo virial radius; (4) total stellar mass; (5) BH mass; (6) half-mass radius of young stars; (7) half-mass radius of total stars; and (8) gas fraction within the halo.

Run|$\frac{M_{\rm halo}}{10^{10}~{\rm {\rm M}_{\odot }}}$||$\frac{R_{200}}{\rm kpc}$||$\frac{M_{\star }}{\rm 10^{10}~{\rm M}_{\odot }}$||$\frac{M_{\rm BH}}{\rm 10^{7}~{\rm M}_{\odot }}$||$\frac{R_{\rm young~star,~1/2}}{\rm kpc}$||$\frac{R_{\rm total~star,~1/2}}{\rm kpc}$||$\frac{f_{\rm gas}}{\rm per~cent}$|
Au3NoRad135.77185.695.964.7810.062.484.40
Au3StarRad132.54184.254.499.1314.711.603.53
Au6NoRad98.79167.063.143.4113.434.536.78
Au6StarRad97.50166.332.482.787.754.017.10
Au16NoRad133.70184.795.162.7114.615.987.21
Au16StarRad136.29185.974.194.4118.506.158.51
Au5NoRad110.63173.484.103.572.651.504.16
Au5StarRad111.54173.963.174.682.841.375.67
Au15NoRad93.18163.842.212.076.861.607.20
Au15StarRad91.97163.121.872.734.121.796.48
Run|$\frac{M_{\rm halo}}{10^{10}~{\rm {\rm M}_{\odot }}}$||$\frac{R_{200}}{\rm kpc}$||$\frac{M_{\star }}{\rm 10^{10}~{\rm M}_{\odot }}$||$\frac{M_{\rm BH}}{\rm 10^{7}~{\rm M}_{\odot }}$||$\frac{R_{\rm young~star,~1/2}}{\rm kpc}$||$\frac{R_{\rm total~star,~1/2}}{\rm kpc}$||$\frac{f_{\rm gas}}{\rm per~cent}$|
Au3NoRad135.77185.695.964.7810.062.484.40
Au3StarRad132.54184.254.499.1314.711.603.53
Au6NoRad98.79167.063.143.4113.434.536.78
Au6StarRad97.50166.332.482.787.754.017.10
Au16NoRad133.70184.795.162.7114.615.987.21
Au16StarRad136.29185.974.194.4118.506.158.51
Au5NoRad110.63173.484.103.572.651.504.16
Au5StarRad111.54173.963.174.682.841.375.67
Au15NoRad93.18163.842.212.076.861.607.20
Au15StarRad91.97163.121.872.734.121.796.48
Table 1.

The properties of the simulated galaxies at |$z=0$|⁠. The columns are (1) model name; (2) halo mass defined by the FoF algorithm; (3) halo virial radius; (4) total stellar mass; (5) BH mass; (6) half-mass radius of young stars; (7) half-mass radius of total stars; and (8) gas fraction within the halo.

Run|$\frac{M_{\rm halo}}{10^{10}~{\rm {\rm M}_{\odot }}}$||$\frac{R_{200}}{\rm kpc}$||$\frac{M_{\star }}{\rm 10^{10}~{\rm M}_{\odot }}$||$\frac{M_{\rm BH}}{\rm 10^{7}~{\rm M}_{\odot }}$||$\frac{R_{\rm young~star,~1/2}}{\rm kpc}$||$\frac{R_{\rm total~star,~1/2}}{\rm kpc}$||$\frac{f_{\rm gas}}{\rm per~cent}$|
Au3NoRad135.77185.695.964.7810.062.484.40
Au3StarRad132.54184.254.499.1314.711.603.53
Au6NoRad98.79167.063.143.4113.434.536.78
Au6StarRad97.50166.332.482.787.754.017.10
Au16NoRad133.70184.795.162.7114.615.987.21
Au16StarRad136.29185.974.194.4118.506.158.51
Au5NoRad110.63173.484.103.572.651.504.16
Au5StarRad111.54173.963.174.682.841.375.67
Au15NoRad93.18163.842.212.076.861.607.20
Au15StarRad91.97163.121.872.734.121.796.48
Run|$\frac{M_{\rm halo}}{10^{10}~{\rm {\rm M}_{\odot }}}$||$\frac{R_{200}}{\rm kpc}$||$\frac{M_{\star }}{\rm 10^{10}~{\rm M}_{\odot }}$||$\frac{M_{\rm BH}}{\rm 10^{7}~{\rm M}_{\odot }}$||$\frac{R_{\rm young~star,~1/2}}{\rm kpc}$||$\frac{R_{\rm total~star,~1/2}}{\rm kpc}$||$\frac{f_{\rm gas}}{\rm per~cent}$|
Au3NoRad135.77185.695.964.7810.062.484.40
Au3StarRad132.54184.254.499.1314.711.603.53
Au6NoRad98.79167.063.143.4113.434.536.78
Au6StarRad97.50166.332.482.787.754.017.10
Au16NoRad133.70184.795.162.7114.615.987.21
Au16StarRad136.29185.974.194.4118.506.158.51
Au5NoRad110.63173.484.103.572.651.504.16
Au5StarRad111.54173.963.174.682.841.375.67
Au15NoRad93.18163.842.212.076.861.607.20
Au15StarRad91.97163.121.872.734.121.796.48
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