Properties of the AuriGaia and AuriDESI mock catalogues. Columns: (1) halo number, (2) virial mass, (3) stellar mass within the virial radius (excluding satellites), (4) disc scale length, (5) circular rotation velocity at 8 kpc from the galactic centre, (6) accreted stellar mass, (7) total stellar mass of the top 10 most massive progenitors in the accreted halo visible to DESI, (8) stellar mass from the top 10 most massive progenitors visible to DESI (excluding satellites), (9)–(11) ratio of mass of MAIN-BLUE, MAIN-RED, and MAIN-BROAD targets, respectively, to the total stellar halo mass visible to DESI, and (12) ratio of in situ stellar mass outside 10 kpc to the total halo mass. The last row gives values for the Milky Way. Columns (1)–(5) are taken from Grand et al. (2018b) and values for the Milky Way are taken from Bland-Hawthorn & Gerhard (2016). The remaining columns are obtained from the mock catalogues described in this paper.
| Halo . | |$\frac{M_{\rm {vir}}}{(10^{12}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_*}{(10^{10}\, \mathrm{M_{\odot }})}$| . | |$\frac{R_d}{(\rm {kpc})}$| . | |$\frac{V_c (\mathrm{R_{\odot }})}{(\rm {km\, s^{-1})}}$| . | |$\frac{M_{*,\rm {acc}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10,DESI}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{f_{\rm {blue}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {red}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {broad}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {ins,\gt 10kpc}}}{\mathrm{ per\,cent}}$| . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Au 6 | 1.01 | 6.1 | 3.3 | 224.7 | 7.86 | 7.66 | 1.40 | 71 | 26 | 2.6 | 18.03 |
| Au 16 | 1.50 | 7.9 | 6.0 | 217.5 | 9.34 | 8.67 | 1.81 | 71 | 27 | 2.5 | 38.01 |
| Au 21 | 1.42 | 8.2 | 3.3 | 231.7 | 19.37 | 19.06 | 3.54 | 75 | 23 | 2.1 | 26.74 |
| Au 23 | 1.50 | 8.3 | 5.3 | 240.0 | 14.35 | 13.71 | 2.20 | 71 | 25 | 3.9 | 33.25 |
| Au 24 | 1.47 | 7.8 | 6.1 | 219.2 | 12.54 | 11.89 | 1.84 | 76 | 28 | 2.3 | 34.97 |
| Au 27 | 1.70 | 9.5 | 3.2 | 254.5 | 15.40 | 14.38 | 2.54 | 72 | 25 | 3.7 | 23.66 |
| MW | 1.3 ± 0.3 | 6 ± 1 | 2.6 ± 0.5 | 238 ± 15 |
| Halo . | |$\frac{M_{\rm {vir}}}{(10^{12}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_*}{(10^{10}\, \mathrm{M_{\odot }})}$| . | |$\frac{R_d}{(\rm {kpc})}$| . | |$\frac{V_c (\mathrm{R_{\odot }})}{(\rm {km\, s^{-1})}}$| . | |$\frac{M_{*,\rm {acc}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10,DESI}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{f_{\rm {blue}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {red}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {broad}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {ins,\gt 10kpc}}}{\mathrm{ per\,cent}}$| . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Au 6 | 1.01 | 6.1 | 3.3 | 224.7 | 7.86 | 7.66 | 1.40 | 71 | 26 | 2.6 | 18.03 |
| Au 16 | 1.50 | 7.9 | 6.0 | 217.5 | 9.34 | 8.67 | 1.81 | 71 | 27 | 2.5 | 38.01 |
| Au 21 | 1.42 | 8.2 | 3.3 | 231.7 | 19.37 | 19.06 | 3.54 | 75 | 23 | 2.1 | 26.74 |
| Au 23 | 1.50 | 8.3 | 5.3 | 240.0 | 14.35 | 13.71 | 2.20 | 71 | 25 | 3.9 | 33.25 |
| Au 24 | 1.47 | 7.8 | 6.1 | 219.2 | 12.54 | 11.89 | 1.84 | 76 | 28 | 2.3 | 34.97 |
| Au 27 | 1.70 | 9.5 | 3.2 | 254.5 | 15.40 | 14.38 | 2.54 | 72 | 25 | 3.7 | 23.66 |
| MW | 1.3 ± 0.3 | 6 ± 1 | 2.6 ± 0.5 | 238 ± 15 |
Properties of the AuriGaia and AuriDESI mock catalogues. Columns: (1) halo number, (2) virial mass, (3) stellar mass within the virial radius (excluding satellites), (4) disc scale length, (5) circular rotation velocity at 8 kpc from the galactic centre, (6) accreted stellar mass, (7) total stellar mass of the top 10 most massive progenitors in the accreted halo visible to DESI, (8) stellar mass from the top 10 most massive progenitors visible to DESI (excluding satellites), (9)–(11) ratio of mass of MAIN-BLUE, MAIN-RED, and MAIN-BROAD targets, respectively, to the total stellar halo mass visible to DESI, and (12) ratio of in situ stellar mass outside 10 kpc to the total halo mass. The last row gives values for the Milky Way. Columns (1)–(5) are taken from Grand et al. (2018b) and values for the Milky Way are taken from Bland-Hawthorn & Gerhard (2016). The remaining columns are obtained from the mock catalogues described in this paper.
| Halo . | |$\frac{M_{\rm {vir}}}{(10^{12}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_*}{(10^{10}\, \mathrm{M_{\odot }})}$| . | |$\frac{R_d}{(\rm {kpc})}$| . | |$\frac{V_c (\mathrm{R_{\odot }})}{(\rm {km\, s^{-1})}}$| . | |$\frac{M_{*,\rm {acc}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10,DESI}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{f_{\rm {blue}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {red}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {broad}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {ins,\gt 10kpc}}}{\mathrm{ per\,cent}}$| . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Au 6 | 1.01 | 6.1 | 3.3 | 224.7 | 7.86 | 7.66 | 1.40 | 71 | 26 | 2.6 | 18.03 |
| Au 16 | 1.50 | 7.9 | 6.0 | 217.5 | 9.34 | 8.67 | 1.81 | 71 | 27 | 2.5 | 38.01 |
| Au 21 | 1.42 | 8.2 | 3.3 | 231.7 | 19.37 | 19.06 | 3.54 | 75 | 23 | 2.1 | 26.74 |
| Au 23 | 1.50 | 8.3 | 5.3 | 240.0 | 14.35 | 13.71 | 2.20 | 71 | 25 | 3.9 | 33.25 |
| Au 24 | 1.47 | 7.8 | 6.1 | 219.2 | 12.54 | 11.89 | 1.84 | 76 | 28 | 2.3 | 34.97 |
| Au 27 | 1.70 | 9.5 | 3.2 | 254.5 | 15.40 | 14.38 | 2.54 | 72 | 25 | 3.7 | 23.66 |
| MW | 1.3 ± 0.3 | 6 ± 1 | 2.6 ± 0.5 | 238 ± 15 |
| Halo . | |$\frac{M_{\rm {vir}}}{(10^{12}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_*}{(10^{10}\, \mathrm{M_{\odot }})}$| . | |$\frac{R_d}{(\rm {kpc})}$| . | |$\frac{V_c (\mathrm{R_{\odot }})}{(\rm {km\, s^{-1})}}$| . | |$\frac{M_{*,\rm {acc}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{M_{*,\rm {top 10,DESI}}}{(10^{9}\, \mathrm{M_{\odot }})}$| . | |$\frac{f_{\rm {blue}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {red}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {broad}}}{\mathrm{ per\,cent}}$| . | |$\frac{f_{\rm {ins,\gt 10kpc}}}{\mathrm{ per\,cent}}$| . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Au 6 | 1.01 | 6.1 | 3.3 | 224.7 | 7.86 | 7.66 | 1.40 | 71 | 26 | 2.6 | 18.03 |
| Au 16 | 1.50 | 7.9 | 6.0 | 217.5 | 9.34 | 8.67 | 1.81 | 71 | 27 | 2.5 | 38.01 |
| Au 21 | 1.42 | 8.2 | 3.3 | 231.7 | 19.37 | 19.06 | 3.54 | 75 | 23 | 2.1 | 26.74 |
| Au 23 | 1.50 | 8.3 | 5.3 | 240.0 | 14.35 | 13.71 | 2.20 | 71 | 25 | 3.9 | 33.25 |
| Au 24 | 1.47 | 7.8 | 6.1 | 219.2 | 12.54 | 11.89 | 1.84 | 76 | 28 | 2.3 | 34.97 |
| Au 27 | 1.70 | 9.5 | 3.2 | 254.5 | 15.40 | 14.38 | 2.54 | 72 | 25 | 3.7 | 23.66 |
| MW | 1.3 ± 0.3 | 6 ± 1 | 2.6 ± 0.5 | 238 ± 15 |
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