Table 1
Properties of the Mice galaxies culled from the literature.
| Parameter | NGC 4676A (NW)/IC 819 | NGC 4676B (SE)/IC 820 |
|
|
||
| RA (EquJ2000) | 12h46m10.110s | 12h46m11.237s |
| Dec (EquJ2000) | +30d43m54.9s | +30d43m21.87s |
| CALIFA ID | 577 | 939 |
| SDSS objid | 587739721900163101 | 587739721900163099 |
| Redshifta | 0.02206 | 0.02204 |
| r-band magnitudeb | 13.22 | 13.03 |
| M(H i) [109 M⊙]c | 3.6 | 4.0 |
| M(H2) [109 M⊙]d | 5.7 | 3.6 |
| Mdyn (109 M⊙e | 74 | 129 |
| LFIR [1010L⊙]f | 3.3 | 0.9 |
| LX, 0.5−2 keV [1040 erg s-1]g | 0.6 | 1.2 |
| LX, 2−10 keV [1040 erg s-1]g | 0.9 | 1.5 |
Notes. Physical parameters have been converted to the same distance and Hubble parameter used in this paper (95.5 Mpc; H0 = 70.4 km s-1 Mpc-1). The unresolved pair is also known as Arp 242 and IRAS 12437+3059.
From H i 21 cm (de Vaucouleurs et al. 1991).
From a growth curve analysis of the SDSS r-band image (Walcher et al., in prep.). The SDSS catalogue magnitude for NGC 4676B is incorrect (see also Sect. 5.3).
Yun & Hibbard (2001) for NGC 4676A and Casoli et al. (1991) for NGC 4676B.
From optical extent and H i line width (Hibbard & van Gorkom 1996).
LFIR as defined by Helou et al. (1988). The Mice are not individually resolved by IRAS; these estimates from Yun & Hibbard (2001) are from the total FIR flux and 1.4 GHz radio continuum ratio.
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