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Table 1

Basic data for the group-dominant galaxies.

Galaxy z DL (1–0) Beam log LB a log D25 a log Mdust c log M(HI)b log LFIR c log M∗ d M(H2)e F(1.4 GHz)f
[Mpc] [kpc] [L⊙] [kpc] [L⊙] [L⊙] [L⊙] [ M⊙] [108 M⊙] [mJy]
Newly observed systems
NGC 193 0.014723 63.8 6.99 10.24 1.58 – – – 10.92 <1.35 1710
NGC 677 0.017012 73.9 8.08 10.52 1.58 – – – 10.91 <2.25 21
NGC 777 0.016728 72.6 7.94 11.03 1.78 3.60 – 7.91 11.32 <2.08 7
NGC 940 0.017075 74.2 8.11 10.81 1.53 6.71 – 10.06 10.94 61.0 8
NGC 1060 0.017312 75.2 8.22 11.09 1.71 6.49 – 10.51 11.42 <0.76 9
NGC 1167i 0.016495 71.6 7.83 10.88 1.72 7.23 10.01g 9.59 11.23 3.3 1840
NGC 1587 0.012322 53.3 5.85 10.64 1.48 – 9.40 – 11.01 2.3 131
NGC 2768i 0.004580 19.7 2.18 10.28 1.50 4.36 7.81h 8.66 10.76 0.18 15
NGC 5846 0.005717 24.6 2.72 10.71 1.48 4.60 8.65 7.83 10.53 <0.20 21
NGC 5982 0.010064 43.5 4.78 10.75 1.60 5.48 – 7.87 10.91 <0.25 <2.5
NGC 7619 0.012549 54.3 5.96 10.93 1.62 – – – 11.21 <0.33 20
CO detected by previous studies
NGC 315 0.016485 71.6 7.83 10.87 1.79 5.87 – 9.56 11.49 0.74 6630
NGC 524 0.008016 34.6 3.81 10.57 1.55 6.06 – 9.39 11.17 1.9 3
NGC 3665 0.006901 29.7 3.28 10.18 1.54 6.68 – 9.74 10.72 6.0 133
NGC 5044 0.009280 40.1 4.41 10.61 1.67 4.57 – 8.66 11.08 0.5 36
NGC 5127 0.016218 70.4 7.70 10.25 1.64 – – – 10.84 0.77 1980
NGC 7252 0.015984 69.4 7.59 10.55 1.57 7.02 9.61 10.67 10.92 58.0 25
Upper limits on CO from previous studies
NGC 1407 0.005934 25.5 2.82 10.56 1.67 5.46 – 8.49 11.09 <0.34 89
NGC 3613 0.006841 29.5 3.25 10.17 1.48 – – – 10.60 <0.46 <1.3
NGC 4261i 0.007378 31.8 3.51 10.41 1.60 5.20 – 8.34 11.07 <0.48 19 500
NGC 4697 0.004140 17.8 1.97 10.36 1.57 5.40 – 8.63 10.93 <0.07 0.4
NGC 5322 0.005937 25.6 2.82 10.33 1.62 7.53 – 9.53 10.93 <0.58 78
NGC 5353 0.007755 33.4 3.69 10.18 1.35 6.20 – 9.19 10.99 <1.32 41

Notes.

(a)

Computed from HYPERLEDA (http://leda.univ-lyon1.fr/).

(b)

These quantities are from NED (http://nedwww.ipac.caltech.edu/).

(c)

The derivation of LFIR and dust masses Mdust is described in Sect. 4.3.

(d)

Stellar masses were obtained through SED fitting with SDSS and/or 2MASS fluxes.

(e)

Molecular gas masses and upper limits either derived from our data (see Sects. 4.1 and 4.2) or drawn from previous observations (Dupraz et al. 1990; Sage et al. 2007; Ocaña Flaquer et al. 2010; Young et al. 2011; David et al. 2014).

(f)

1.4 GHz continuum fluxes are drawn from the NRAO VLA Sky Survey (NVSS, Condon et al. 1998, 2002)  except in the cases of NGC 940 and NGC 4697, where we extrapolate from measurements at 2.4 GHz (Dressel & Condon 1978) and 8.5 GHz (Wrobel et al. 2008) respectively, assuming a spectral index of 0.8. The two upper limits are taken from (Brown et al. 2011).

(i)

The CO content of these systems is discussed individually in Appendix A.

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