Table 1
General properties of Centaurus A and the northern outer filament (Morganti et al. 1991) at the intersection with the H i shell (Schiminovich et al. 1994).
| Source | Centaurus A | Outer filaments |
|
|
||
| z, vLSR(km.s-1) | 0.001826, ~ 545 | 0.001826 |
| distance (kpc) | 0 | ~ 13.5 a |
| DA, DL (Mpc) | 3.42b | |
| Scale (pc/′′) | 16.5b | |
|
|
||
| RA (J2000) |
|
|
| Dec (J2000) | −43:01:09.8 | −42:49:32.0 |
| LFUV(erg s-1) | 3.5 × 1042 c | 3.2 × 1040 |
| SFRFUV(M⊙ yr-1) | 0.16d | 1.4 × 10-3 d |
| LFIR(L⊙) | 9.3 × 109 c | 3.2 × 107 |
| SFRFIR(M⊙ yr-1) | 1.6d | 5.5 × 10-3 e |
| LTIR(L⊙) | – | 3.3 × 107 |
| SFRTIR(M⊙ yr-1) | – | 4.9 × 10-3 d |
|
|
||
| MH2(M⊙) | 3.3 × 108 f | > 1.7 × 107 g |
| tdep(Gyr) | 0.2 | > 4.3 |
Notes. For the outer filament, all luminosities were estimated on a region of 10′ × 12′ ~ 10 × 12kpc (Fig. 2; Auld et al. 2012). The FIR and TIR luminosity were computed on the 40−500 and 3−1100μm ranges, they do not contain a great contribution of old stars (Rejkuba et al. 2001) and are relevant tracers of star formation. The molecular gas mass and the molecular depletion time are derived for a fixed αCO.
Charmandaris et al. (2000), in the shell S1.
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