Table 3.
p values from hypothesis testing for residual galaxy properties.
| Residual | KS | AD | LP | CU | Nuc w.r.t. non-nuc |
|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) |
| g′−r′ [mag] | 0.003 | 0.003 | 0.003 | 0.007 | Redder |
| log10(n) | 0.334 | 0.250 | 0.458 | 0.352 | – |
| log10(Re [arcsec]) | 0.653 | 0.250 | 0.555 | 0.430 | – |
 [mag arcsec−2] |
0.083 | 0.096 | 0.180 | 0.216 | – |
| C | 0.015 | 0.040 | 0.096 | 0.121 | More concentrated (a) |
| A | 0.012 | 0.008 | 0.002 | 0.002 | Less asymmetric |
| S | 0.141 | 0.208 | 0.386 | 0.342 | – |
| G | 0.129 | 0.250 | 0.390 | 0.483 | – |
| M20 | 0.096 | 0.038 | 0.004 | 0.001 | Lower scatter |
| Δ(g′−r′) [mag] | 0.026 | 0.010 | 0.027 | 0.018 | Redder outskirts |
Notes. The null hypothesis that the residual galaxy properties (1) between nucleated and non-nucleated galaxies in our sample are drawn from the same distribution. The alternative hypothesis is that the null hypothesis is false. The Kolmogorov-Smirnov (2), Anderson-Darling (3), Lepage (4), and Cucconi (5) statistics were used for each galaxy quantity. The p values were calculated for the galaxies within overlapping stellar masses (106.4 M⊙ < M* < 1010.7 M⊙; Col. (3) from Fig. 13). p values below the significance level α = 0.05 are shown in bold. We also describe the difference in residual properties for nucleated galaxies as compared to non-nucleated galaxies (6) for those that have significant test statistic(s).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.