Table 3: Galaxies studied by other investigators.
Galaxy S60/S100 D a25 $L_{\rm {FIR}}/D^2_{25}$ DIG morphology $^{\footnotesize a}$ Radio halo X-ray halo Refs.
    [Mpc] ['] [ $\rm {10^{40}~erg~s^{-1}~kpc^{-2}}$]   (thick disk)    
NGC 4217 0.2511 17.0   4.9 8.85 pl,pa     (9)
NGC 5403 0.2717 37.6   3.0 7.56 n     (7)
NGC 3556 0.3841 14.1   8.1 6.74 ee,h$_{\rm f}$? $\bullet$ $\bullet$ (1);(10);(11)
NGC 4013 0.2360 17.0   4.8 5.51 ee,f,h$_{\rm f}$     (9)
NGC 4631 0.4292   6.9 14.8 4.22 f,h$_{\rm f}$,pa $\bullet$ $\bullet$ (5); (8)
NGC 5777 0.3745 30.5   3.1 4.07 pl     (7)
NGC 4522 0.3235 16.8   3.5 2.15 ee,eh2,f     (6)
NGC 973 0.4541 66.1   3.7 2.12 n     (7)
UGC 3326 0.2696 56.4   3.4 1.86 pl     (7)
NGC 3432 0.3313   7.8   6.9 1.82 ee,eh2     (2)
NGC 55 0.4423   1.3 27.5 1.79 ee,eh2,f,pl,   $\circ$ (3);(4); (14)
NGC 4762 0.4286 16.8   7.6 1.78 n     (9)
NGC 5907 0.2788 14.9 11.7 1.64 d     (9)
UGC 2092 0.3281 82.1   3.0 0.99 pl     (7)
NGC 5746 0.1256 22.9   6.9 0.86 d,n     (9)
NGC 4565 0.2381   9.7 14.8 0.68 n     (8)
IC 2233 0.3464   7.7   4.6 0.32 pl $\circ$   (9);(12)
NGC 4244 0.1466   3.1 14.8 0.07 eh2 $\circ$   (5);(13)
NGC 4183   17.0   5.1   d     (1)
NGC 5023     6.0   5.9   pl?     (9)
UGC 9242   26.3   4.9   ee?     (5)
a a = arc(s), d = disk emission (only planar DIG), ee = extended emission (locally), eh2 = extraplanar H  II region(s), f = filament(s), h$_{\rm b}$ = bright halo, h$_{\rm f}$ = faint halo, n = no (e)DIG, pa = patch(es), pec = peculiar, pl = plume(s).

References: (1) Collins et al. (2000); (2) English & Irwin (1997); (3) Ferguson et al. (1996); (4) Hoopes et al. (1996); (5) Hoopes et al. (1999); (6) Kenney & Koopmann (1999); (7) Pildis et al. (1994); (8) Rand et al. (1992); (9) Rand (1996); (10) Wang et al. (2002); (11) Irwin et al. (2000); (12) Hummel et al. (1991); (13) Hummel et al. (1984); (14) Schlegel et al. (1997) ($\bullet$ = detection, $\circ$ = non-detection).


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