Table 1.

Toy-model predictions for the correlations of integrated h4 with each of axis ratio q, rotation-to-dispersion ratio (V/σ)e, and spatially resolved h4. Selecting round galaxies (q ≥ 0.75) or galaxies with low (V/σ)e enhances the correlation between integrated and resolved h4 .

Subsetq(V/σ)e|$h_4 \, (\mathrm{local})$|
(1)(2)(3)(4)(5)
(1)all0.26−0.510.68
(2)(V/σ)e ≤ 0.50.12−0.120.98
(3)(V/σ)e > 0.50.33−0.490.63
(4)q ≥ 0.750.18−0.300.91
(5)q < 0.750.08−0.740.54
Subsetq(V/σ)e|$h_4 \, (\mathrm{local})$|
(1)(2)(3)(4)(5)
(1)all0.26−0.510.68
(2)(V/σ)e ≤ 0.50.12−0.120.98
(3)(V/σ)e > 0.50.33−0.490.63
(4)q ≥ 0.750.18−0.300.91
(5)q < 0.750.08−0.740.54

Note. Columns: (1) row index (2) subset of the models used; (3) Spearman’s rank correlation coefficient ρ between integrated h4 and q; (4) same as (3), but for (V/σ)e ; (5) same as (3), but for spatially resolved h4 .

Table 1.

Toy-model predictions for the correlations of integrated h4 with each of axis ratio q, rotation-to-dispersion ratio (V/σ)e, and spatially resolved h4. Selecting round galaxies (q ≥ 0.75) or galaxies with low (V/σ)e enhances the correlation between integrated and resolved h4 .

Subsetq(V/σ)e|$h_4 \, (\mathrm{local})$|
(1)(2)(3)(4)(5)
(1)all0.26−0.510.68
(2)(V/σ)e ≤ 0.50.12−0.120.98
(3)(V/σ)e > 0.50.33−0.490.63
(4)q ≥ 0.750.18−0.300.91
(5)q < 0.750.08−0.740.54
Subsetq(V/σ)e|$h_4 \, (\mathrm{local})$|
(1)(2)(3)(4)(5)
(1)all0.26−0.510.68
(2)(V/σ)e ≤ 0.50.12−0.120.98
(3)(V/σ)e > 0.50.33−0.490.63
(4)q ≥ 0.750.18−0.300.91
(5)q < 0.750.08−0.740.54

Note. Columns: (1) row index (2) subset of the models used; (3) Spearman’s rank correlation coefficient ρ between integrated h4 and q; (4) same as (3), but for (V/σ)e ; (5) same as (3), but for spatially resolved h4 .

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