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Table A.1.

All relevant quantities for the dSphs and galaxy clusters.

Galaxy log 10 ( L V L ) $ \log _{10}(\frac {L_{{\textrm {V}}}}{{\textrm {L}}_{\odot }}) $ r 1 / 2 pc $ \frac {r_{1/2}}{{\textrm {pc}}} $ log 10 ( g N m s 2 ) $ \log _{10}(\frac {g_{{\textrm {N}}}}{{\mathrm {m\,s}}^{-2}}) $ log 10 ( a m s 2 ) $ \log _{10}(\frac {a}{{\mathrm {m\,s}}^{-2}}) $ p ρ ¯ 10 2 M pc 3 $ \frac {\bar {\rho }}{10^{-2}{\mathrm {M}}_{\odot }{\mathrm {pc}}^{-3}} $
Carina 5.57(20) 273(45) -12.15(27) -10.81(18) 3.51(59) 7.6±5.5
Draco 5.45(8) 244(9) -12.18(14) -10.48(12) 5.04(90) 8.1±2.7
Fornax 7.31(12) 792(58) -11.35(17) -10.77(8) 2.68(26) 17.2±7.4
Leo I 6.74(12) 298(29) -11.06(18) -10.56(6) 2.78(33) 87±41
Leo II 5.87(12) 219(52) -11.67(26) -10.71(14) 3.22(51) 30±24
Sculptor 6.36(20) 311(46) -11.48(26) -10.58(13) 3.37(61) 32±22
Sextans 5.64(20) 748(66) -12.96(24) -11.09(15) 3.59(39) 0.44±0.26
Bootes I 4.29(8) 283(7) -13.47(14) -11.14(15) 3.91(38) 0.36±0.12
Canes V. I 5.08(8) 647(27) -13.40(14) -11.06(5) 4.05(18) 0.186±0.062
Canes V. II 4.10(8) 101(5) -12.76(14) -10.69(19) 4.69(93) 5.1±1.8
Coma B. 3.46(24) 79(6) -13.19(27) -10.59(16) 5.9(12) 2.5±1.6
Hydra II 3.87(12) 88(17) -12.88(28) -10.65(87) 5.1(49) 4.6±3.1
Leo IV 3.91(8) 149(47) -13.30(30) -11.15(47) 3.8(11) 1.0±1.0)
Leo T 5.57(7) 160(10) -11.70(14) -10.47(19) 4.2(12) 38±13
Segue II 2.94(12) 43(6) -13.17(20) -10.81(87) 4.7(36) 4.6±2.6

NGC 147 7.84(4) 672(23) -10.67(12) -10.43(6) 2.47(29) 96±27
NGC 185 7.84(4) 565(7) -10.52(12) -10.00(4) 8.6(42) 161±43
NGC 205 8.52(4) 594(107) -9.88(19) -9.70(15) 1.18(87) 660±400
And II 6.85(8) 1355(142) -12.27(16) -11.21(11) 2.82(20) 1.19±0.53
And V 5.55(8) 365(57) -12.43(19) -10.53(11) 5.12(81) 3.1±1.7
And VI 6.44(8) 537(54) -11.88(16) -10.55(11) 4.11(60) 7.5±3.2
And VII 6.98(12) 965(52) -11.85(17) -10.77(7) 3.27(27) 4.5±1.8
And IX 4.97(44) 582(23) -13.42(45) -10.70(17) 5.5(11) 0.20±0.21
And X 5.13(40) 312(41) -12.72(43) -11.32(27) 3.00(49) 1.9±1.9
And XIV 5.37(20) 434(212) -12.76(48) -11.20(29) 3.22(63) 1.2±1.9
And XV 5.69(12) 294(12) -12.11(17) -11.28(31) 2.61(39) 8.1±3.2
And XVI 5.53(12) 164(9) -11.76(17) -10.70(17) 3.36(56) 32±13
And XVII 5.34(16) 299(31) -12.47(21) -10.86(44) 3.7(13) 3.4±1.9
And XXIII 6.00(20) 1034(97) -12.88(24) -11.32(13) 3.11(26) 0.38±23
And XXIV 5.32(20) 633(52) -13.14(24) -11.09(87) 3.8(21) 0.35±0.20
And XXVIII 5.39(16) 285(12) -12.37(20) -11.09(29) 3.09(55) 4.4±2.1
And XXIX 5.33(12) 377(30) -12.68(18) -11.08(19) 3.38(42) 1.67±0.74
And XXXI 6.61(28) 1231(132) -12.43(32) -11.08(9) 3.16(32) 0.91±0.70
Cetus 6.44(8) 791(75) -12.22(16) -11.07(11) 3.00(24) 2.33±0.98
Perseus I 6.04(28) 391(143) -12.00(45) -11.36(88) 2.44(94) 8±10

Notes. Above the horizontal line are Milky Way satellites; below it are Andromeda satellites. The columns are, from left to right: the name of the galaxy, the V-band-luminosity, LV, the half-light-radius, r1/2, the Newtonian acceleration, gN, observationally deduced acceleration, a, the p parameter from p-Laplacian p (Eq. (1)), and the mean density, ρ ¯ $ \bar {\rho } $. The first four quantities were adopted from Lelli et al. (2017) and p and ρ ¯ $ \bar {\rho } $ were calculated from them.

The uncertainty deviates from the data by Lelli et al. (2017), because it has been symmetrized.

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