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Table 3.
Physical parameters of NGC 1365 compared with those of NGC 1377.
| Object | Rotation | Or | Radius | Rotation or | Mass | Period | Remarks | |
|---|---|---|---|---|---|---|---|---|
| outflow | axis | or size | outflow vel. | dyn. (a) | Gas (b) | or age | ||
| PA [°] | Incl. [°] | [kpc pc−1] | [km s−1] | [×109 M⊙] | [Myr] | |||
| NGC 1365 | ||||||||
| Disk (c) | 130 | 50 | 22 | ≈270 | 360 | 13 | ≈500 | H I mass |
| Bar (c)(d) | 50 | 10 | 180 | 13 (d) | 340 | Stellar mass | ||
| Disk | 50 | 10 | 310 | 220 | 9 | 200 | H2 mass | |
| Disk | 2 | 310 | 44 | 2.8 | 40 | |||
| Disk/torus (b) | 1 | 230 | 12 | 2.4 | 27 | “Star formation gas ring”, | ||
| Outer torus | ≈130 | ≈50 | 800 | 185 | 6 | 27 | with solid body rotation | |
| Outer torus | 500 | 115 | 1.5 | 27 | as visualized in Fig. A.1 | |||
| Nuclear engine: | ||||||||
| Inner torus (d) | ≈160 | ≈63 | 26 | ≈100 | 0.06 | 0.007 | 1.6 | Note torus axis tilt (d), caused by ≈30° precession angle |
| Black hole (d) | 0.004 | Rapidly spinning SMBH | ||||||
| Nuclear outflows: | ||||||||
| Radio jet (c)(e) | ≈135 | ≈20 | ≈400 | 0.7c? | Table 2; Inclination caused by nuclear engine tilt | |||
| CO outflow (f) | ≈135 | ≈20 | ≈400 | ≈70 | 5.9 | Sect. 4.3.1 and ref. (d); Inclination by nuclear engine tilt | ||
| (≈80) | (≈2200) | (≈23) | (90) | Unlikely inclination alternative; See Sect. 4.3.2 | ||||
| O III bi-cone (g) | 130 | 50 | ±2500 | ±200 | − | 0.001 | ≈12 | Hollow, wide angle (±50°) ionized gas “fountain” |
| H I outflow | ≈160 | 2000 | ±200 | ≈10 | Fig. 7; Desorption/dissociation from icy grains? | |||
| NGC 1377 | ||||||||
| Nuclear disk (h) | 15 | ≈0 | 29 | 75 | 0.04 | 0.017 | ||
| CO outflow (h) | 15 | ≈0 | 200 | 140 | − | 0.01−0.05 | 1.4 | Opening angle ≈60−70° |
| Map area (j) | 15 | ≈0 | − | − | 0.16 | Size: 4″ × 4″ | ||
| Accretion disk (j) | 15 | ≈0 | ≈10 | 110 | 0.03 | 0.018 | ≈1 | Rotation period |
| Bipolar CO jet (j) | 15 | ±(10−25) (k) | ±150 | 240−850 (m) | − | 0.002−0.02 (m) | 0.2−0.7 | Precession period: 0.3−1.1 |
Notes.
(a)
This paper, Eq. (2).
(b)
This paper, Sect. 4.1.
(d)
Combes et al. (2019), who (in their Table 4) list an inner torus tilt, with an uncertainty of ±10°.
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