Table 1: Physical properties of the sample.

Galaxy		 d i $L_{\rm 1.4~GHz}$ $L_{\rm FIR}$ $L_{\rm B_{T}^{0}}$ $L_{\rm UV}$ $L_{\rm H\alpha}$ $L_{\rm X,soft}$ ${\it SFR}_{\rm FIR}$ ${\it SFR}_{\rm H\alpha }$ $\dot{E}_{\rm A}^{\rm tot}$ $L_{\rm FIR}/D_{25}^{2}$ $M_{\rm bar}$ $M_{H {\sc i}}$ $M_{\rm dust}$
  [Mpc] $[\hbox{$^\circ$ }]$ [ $10^{38}~{\rm erg\ s^{-1}}$] [ $10^{43}~{\rm erg\ s^{-1}}$] [ $10^{40}~{\rm erg\ s^{-1}}$] [ ${M}_{\odot}\ {\rm yr}^{-1}$] [ $10^{-3}~{\rm erg~s^{-1} cm^{-2}}$] [ $10^{40}~{\rm erg\ s^{-1}\ kpc^{-2}}$] [ $10^{10}~{M}_{\odot}$] [ $10^{6}~{M}_{\odot}$]

(1)		 (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15)

NGC 0891		 9.5 88 1.19a 9.62 5.59 0.11 3.54h 0.70r 4.32 0.28 3.90u 6.92 10.6 0.45 2.02
NGC 3044 17.2 84 0.62b 4.06 3.61 -- 8.83j 0.09r 1.83 0.70 0.94g 8.52 3.28 0.64 0.49
NGC 3221 54.8 77 3.29b 36.0 8.28 -- -- 1.07r 16.2 -- 2.20u 13.5 1.63 1.70 6.55
NGC 3628 10.0 80 0.93b 7.66 6.54 0.12 2.30k 0.74r 3.45 0.18 12.2u 8.24 11.3 0.38 0.85
NGC 3877 12.1 83 0.10b 1.92 2.34 0.12 -- 0.02r 0.86 -- 0.77u 5.14 1.28 0.17 0.52
NGC 4631 7.5 86 1.22b 6.63 7.00 1.15 14.3k 0.78r 2.99 1.13 0.83g 7.76 2.56 0.68 0.69
NGC 4634 19.1 83 0.21c 2.53 1.46 0.14 6.40j 0.15r 1.14 0.51 2.62u 12.4 1.63 0.05 0.58
NGC 4666 20.2 80 2.64b 23.0 7.56 1.01 57.5d 1.42r 10.3 4.55 4.46g 31.9 5.44 0.61 3.77
NGC 5775 26.7 84 2.82b 25.7 8.05 -- 23.4l 1.55r 11.6 1.85 3.26g 24.6 6.09 0.97 4.39

M 82		 3.6 82 2.10b 20.9 16.7 0.06 14.4h 5.15k 9.39 1.14 19.6$^{\ ~}$ 151 1.86 0.16 0.54
NGC 0253 2.6 79 0.53b 7.93 3.42 0.11 4.90h 0.55k 3.57 0.39 2.74$^{\ ~}$ 18.3 10.6 0.60 0.41
NGC 1482 22.1 58 3.04b 20.1 10.4 -- 9.60k 3.70k 9.65 0.76 64.9$^{\ ~}$ 80.7 3.58 0.06 1.16
NGC 3079 17.1 85 5.88b 21.3 6.94 0.76 9.00k 3.20k 9.60 0.71 33.6$^{\ ~}$ 13.7 14.1 1.10 2.74
NGC 4244 3.6 85 0.002c 0.11 0.54 0.01 0.42k 0.007k 0.05 0.03 0.05g 0.36 0.62 0.09 0.06
NGC 4945 3.7 78 1.51c 12.5 5.05 -- 2.40k 0.34k 5.62 0.19 4.50u 27.1 5.24 0.09 1.69
NGC 6503 5.2 75 0.03b 0.46 0.69 0.11 0.76k 0.07k 0.21 0.06 1.00$^{\ ~}$ 4.04 1.17 0.13 0.13

NGC 0055		 1.6 80 0.02a 0.95 0.79 0.09 2.00m 0.31s 0.12 0.16 0.11$^{\ }$ 1.12 5.65 0.16 0.05
NGC 1511 17.5 72 0.82f 10.1 3.21 -- 3.63n 0.26n 4.54 0.29 0.34n 32.4 0.92 0.54 0.77
NGC 3556 14.1 79 1.71b 9.92 8.05 0.62 7.60i 2.00t 4.46 0.60 2.85e 6.96 3.97 0.93 1.70
NGC 4522 16.0 79 0.10c 0.60 1.42 0.10 1.30o 0.89o 0.27 0.10 0.58$^{\ ~}$ 2.00 1.55 0.05 0.21
NGC 4565 9.7 89 0.22b 1.60 7.47 0.07 1.20p 0.26p 0.72 0.09 0.09g 0.80 16.5 1.30 1.19
NGC 4656 7.5 90 0.02b 0.48 1.78 0.02 1.41v 0.03p 0.22 0.11 0.05g 0.44 1.81 0.39 0.04
NGC 5907 14.9 86 0.35b 4.32 2.74 0.01 5.57q 0.05p 1.89 0.44 0.14g 1.63 15.4 1.38 2.56
Notes: Columns (1) to (3): name, distance, and inclination of the target; Col. (4): radio continuum luminosities measured at 1.49 GHz; Col. (5): FIR-luminosities calculated from revised IRAS S60 and S100 flux densities (Sanders et al. 2003); Col. (6): total $B_{\rm {T}}^{\rm0}$ luminosities calculated from RC3 (de Vaucouleurs 1991) and corrected for redshift, Galactic, and internal extinction, assuming reddening values from (Burstein & Heiles 1982); Col. (7): de-reddened UV-continuum luminosities measured at 1650 Å (Rifatto et al. 1995) and 1550 Å (Code & Welch 1982), respectively. The UV flux for NGC 4656 has been determined at 2270 Å (Maoz et al. 1996). No correction for redshift has been applied; Col. (8): H $\alpha+[N {\sc ii}]$-luminosities, uncorrected for extinction and [N II]-contamination; Col. (9): integrated (disk+halo) diffuse X-ray luminosities obtained from spectral fitting between 0.3 and 2.0 keV, for NGC 3221 and NGC 3877 disk only; Col. (10): total star formation rate, based on FIR and H$\alpha $ luminosities according to (Kennicutt 1998); Col. (11): SN energy input rates per unit area (Condon 1992; Dahlem et al. 1995) for $M>5~M_{\odot}$; Col. (12): the optical diameter of the 25th magnitude isophote (D25) was taken from RC3 (de Vaucouleurs 1991); Col. (13): baryonic masses were calculated according to Bell & de Jong (2001); Col. (14): to derive the H I gas mass, we used $M_{H {\sc i}}=4.78\times 10^5~d^2~S(H {\sc i})$, where $S(H {\sc i})$, the total H I flux in units of [Jy km s-1] has been taken from Huchtmeier & Richter (1989); Col. (15): dust masses were calculated following Hildebrand (1983).
References:     (a) Condon et al. (1996); (b) Condon et al. (1990); (c) Condon et al. (1998); (d) Dahlem et al. (1997); (e) Irwin et al. (1999); (f) Dahlem et al. (2001); (g) Dahlem et al. (1995); (h) Bell (2003); (i) Young et al. (1996); (j) Rossa & Dettmar (2000); (k) Strickland et al. (2004a); (l) Lehnert & Heckman (1996); (m) Ferguson et al. (1996); (n) Dahlem et al. (2003); (o) Kenney & Koopmann (1999); (p) Vogler et al. (1996); (q) Rand (priv. com.); (r) Tüllmann et al. (2006); (s) Schlegel et al. (1997); (t) Wang et al. (2003); (u) Rossa & Dettmar (2003); (v) Aldering (priv. com.).

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