Table 2.
Properties of our sample of MaNGA galaxies with the circumnuclear region classified as INT type.
| Name | d | Msp | i | RINT | Rσgas | log LINT, Ha | log ΣHa, C | log σgas, c | log σgas, HIIobs |
|---|---|---|---|---|---|---|---|---|---|
| (Mpc) | (M⊙) | (°) | (kpc) | (kpc) | (erg s−1) | (L⊙ pc−2) | (km s−1) | (km s−1) | |
| 8077 12704 | 97.2 | 10.38 | 31.0 | 1.77 | 2.24 | 39.41 | −1.200 | 1.744 | 1.844 |
| 8080 06104 | 147.4 | 11.09 | 29.6 | 1.22 | 1.61 | 40.06 | −0.344 | 1.959 | 1.862 |
| 8085 12704 | 123.5 | 10.66 | 60.6 | 1.84 | 2.25 | 39.98 | −0.498 | 1.915 | 1.859 |
| 8135 12703 | 210.1 | 10.69 | 55.9 | 2.43 | 3.32 | 39.72 | −1.326 | 1.849 | 1.837 |
| 8137 12703 | 158.7 | 10.89 | 45.1 | 2.25 | 2.89 | 40.12 | −0.618 | 1.927 | 1.853 |
| 8138 12704 | 128.3 | 11.36 | 54.3 | 1.13 | 2.34 | 40.06 | −0.096 | 2.140 | 1.872 |
| 8141 12704 | 199.1 | 10.63 | 41.4 | 1.41 | 3.62 | 39.58 | −0.830 | 1.734 | 1.852 |
| 8329 06103 | 135.3 | 10.57 | 54.8 | 1.48 | 2.13 | 39.95 | −0.530 | 1.883 | 1.895 |
| 8623 06104 | 398.5 | 11.28 | 34.1 | 2.32 | 4.36 | 41.05 | 0.265 | 2.094 | 1.871 |
| 8990 09102 | 139.8 | 10.69 | 49.0 | 0.85 | 2.21 | 39.69 | −0.272 | 1.897 | 1.870 |
| 9027 12701 | 136.3 | 11.00 | 43.7 | 1.16 | 1.82 | 40.09 | −0.139 | 1.896 | 1.867 |
| 9039 06102 | 261.3 | 11.34 | 41.2 | 2.64 | 3.49 | 40.63 | −0.242 | 2.159 | 1.903 |
| 9041 12702 | 137.6 | 10.88 | 59.7 | 0.84 | 2.84 | 39.52 | −0.421 | 1.819 | 1.882 |
| 9042 12702 | 309.3 | 11.02 | 53.4 | 2.51 | 4.88 | 40.79 | 0.042 | 2.031 | 1.867 |
| 9500 09102 | 180.1 | 10.21 | 40.8 | 1.20 | 3.28 | 39.71 | −0.590 | 1.630 | 1.872 |
| 9506 09102 | 113.5 | 10.29 | 67.2 | 1.00 | 3.99 | 39.41 | −0.662 | 1.483 | 1.871 |
| 9868 12705 | 306.1 | 11.13 | 48.1 | 1.98 | 4.83 | 40.61 | −0.069 | 2.040 | 1.884 |
Notes. The columns show the name (the MaNGA number), the galaxy distance d in Mpc, the spectroscopic stellar mass Msp in solar masses, the kinematic inclination angle i, the radius of the zone of the influence of the AGN on the radiation RINT in kpc, the radius of the zone of the enhanced gas velocity dispersion Rσgas in kpc, the Hα line luminosity of the zone of AGN influence RINT, Hα the central surface brightness in the Hα line ΣHα, C in L⊙ pc−2, the central gas velocity dispersion σgas, c in km s−1, the median value of the observed (non corrected for the instrumental profile) gas velocity dispersions for all the spaxels with the H II-region-like spectra σgas, HIIobs in km s−1.
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