Table 3.
Galaxy properties and ram pressure parameters.
| Galaxy | M* | MHI | vsys | σv | Σ* | ΣHI | ρICM | dcluster | Velocity |
|---|---|---|---|---|---|---|---|---|---|
| name | log(M⊙) | log(M⊙) | (km s−1) | (km s−1) | (M⊙ kpc−2) | (cm−2) | (cm−3) | (kpc) | substructure |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| NGC 3312 | 11.07 ± 0.11 | 9.83 | 2851 | 690 | 8.5 × 107 | 2.4 × 1020 | 2.5 × 10−4 | 550 | Foreground |
| NGC 3314a | 10.58 ± 0.12 | 9.43 | 2849 | 690 | 7.5 × 107 | 2.4 × 1020 | 1.1 × 10−4 | 800 | Foreground |
| NGC 3314b | 8.85 | 4657 | 440 | 2.5 × 108 | 2.4 × 1020 | 9.1 × 10−4 | 300 | Bkgrd/clstr core | |
| LEDA 753342 | 8.79 ± 0.16 | 8.62 | 2743 | – | – | – | – | – | Foreground |
Notes. (1) galaxy name; (2) stellar mass derived from WISE; (3) measured H I mass; we assume a typical measurement error of ∼15%; see also Appendix A; (4) systemic velocity in the barycentric frame measured from the H I data by SoFiA; (5) assumed velocity dispersion for the subgroup along the line-of-sight to which the galaxies belong; (6) estimated stellar mass surface density in the disk where ram pressure is occurring; (7) estimated H I column density at which gas is being stripped; (8) derived ICM density; (9) implied distance to the cluster center based on the Hayakawa et al. (2006) Beta model; (10) group classification along the line-of-sight. Quantities derived assuming all galaxies are at the distance of the Hydra cluster, D = 58.6 Mpc. The stellar masses of NGC 3314a/b cannot be disentangled, and so are reported together.
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