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Table 1.

Basic data for the newly observed or processed group-dominant galaxies.

Galaxy z DL (Mpc) Beama (kpc) log LBb (L) D25b (kpc) log Mdustd (L) log M(HI)c (M) log LFIRd (L) log M*e (M) M(H2)f (108 M) F1.4 GHzg (mJy)
IRAM 30 m CLoGS survey observations
NGC 128 0.014146 58.54 6.22 10.66 53.73 6.48 8.65 9.84 ± 0.03 11.09 1.76 ± 0.18h 1.5
NGC 252 0.016471 71.65 7.63 10.56 33.72 6.97 9.56 9.84 ± 0.05 11.06 6.29 ± 0.79 2.5
NGC 410 0.017659 76.67 8.17 10.95 52.77 11.37 <1.17 5.8
NGC 584 0.006011 18.71 1.97 10.20 20.60 6.06 8.08 8.15 ± 0.06 10.62 <0.11 0.6
NGC 924 0.014880 63.61 6.76 10.30 37.61 7.30 9.96 9.50 ± 0.23 10.76 0.52 ± 0.10 0.9
NGC 978 0.015794 68.66 7.30 10.56 36.60 5.49 8.96 ± 0.08 11.08 <0.70 0.7
NGC 1106 0.014467 63.26 6.72 10.33 33.56 6.19 10.03 ± 0.06 10.87 6.81 ± 0.33 132
NGC 1453 0.012962 53.54 5.68 10.61 38.32 7.15 9.01 9.10 ± 0.06 11.16 <0.78 28
NGC 1550 0.012389 52.13 5.53 10.36 26.17 10.88 <0.47 17
NGC 2563 0.014944 64.39 6.84 10.47 37.89 <8.73 11.02 <0.93 0.7
NGC 2911 0.010617 45.84 4.85 10.43 46.13 5.13 9.31 8.83 ± 0.07 10.82 2.66 ± 0.31 56
NGC 3325 0.018873 79.67 8.50 10.40 29.24 9.18 4.10 ± 0.01 10.88 <1.57
NGC 4008 0.012075 53.96 5.72 10.47 32.57 4.62 <8.49 8.87 ± 0.20 10.90 <0.73 11
NGC 4169 0.012622 56.67 6.01 10.44 27.04 7.48 10.03 10.46 ± 0.01 10.89 1.44 ± 0.34 1.1
NGC 4261 0.007378 29.38 3.10 10.65 36.29 5.04 <8.69 8.30 ± 0.11 11.05 <0.37 19700
NGC 4956 0.015844 70.90 7.54 10.58 32.16 5.87 9.05 9.54 ± 0.09 10.91 <0.75
NGC 5353 0.007755 35.43 3.74 10.49 24.44 3.91 9.72 8.74 ± 0.04 11.05 1.90 ± 0.25 40
NGC 5444 0.013169 60.46 6.42 10.64 43.67 <8.79 11.04 <0.64 660
NGC 5490 0.016195 71.94 7.66 10.68 34.73 11.15 <0.64 1300
NGC 5629 0.015004 67.73 7.20 10.58 33.61 10.95 <0.91 4.6
NGC 6658 0.014243 63.97 6.79 10.66 27.84 10.76 <0.71
IRAM 30 m deep observations
NGC 4636 0.003129 13.61 1.43 10.44 24.98 5.07 8.84i 7.94 ± 0.03 10.51 0.010 ± 0.003 78
NGC 5813 0.006525 29.92 3.15 10.53 36.28 4.55 <7.94 8.09 ± 0.06 10.89 <0.11 15
NGC 5846 0.005711 23.12 2.44 10.48 28.69 3.99 8.48i 8.05 ± 0.06 10.83 0.14 ± 0.06 21
NGC 7619 0.012549 54.30 5.76 10.82 39.68 6.98 7.41i 9.17 ± 0.12 11.21 <0.29 20
APEX CLoGS survey observations
ESO 507-25 0.010788 45.21 6.00 10.45 34.67 6.50 10.50 9.46 ± 0.05 10.95 4.23 ± 0.56 24
NGC 1779 0.011051 44.44 5.90 10.27 34.47 6.53 9.26 9.73 ± 0.08 10.75 4.57 ± 0.60 5.4
NGC 2292 0.006791 29.57 3.91 10.40 37.29 6.84 9.35 9.26 ± 0.03 10.79 <0.47
NGC 3923 0.005801 21.28 2.81 10.54 42.63 3.63 <8.41 7.38 ± 0.08 11.03 <0.29 1.0
NGC 5061 0.006945 28.26 3.73 10.61 30.82 2.65 <8.66 7.40 ± 0.10 10.96 <0.43 <1.0
NGC 5153 0.014413 60.54 8.06 10.59 43.03 10.89 <1.75
NGC 5903 0.008556 31.48 4.17 10.30 27.46 9.48 10.73 <0.58 320
NGC 7377 0.011138 46.73 6.20 10.69 53.25 6.70 9.47 ± 0.05 11.04 4.74 ± 0.44 3.1
APEX archival observations
NGC 1395 0.005727 22.39 2.95 10.65 31.39 5.64 <8.45 8.12 ± 0.08 10.91 <0.27 1.1
NGC 3078 0.008606 32.66 4.32 10.39 28.89 <8.78 10.84 <0.23 310
NGC 5084 0.005741 24.09 3.18 10.31 69.59 5.74 10.18 8.87 ± 0.05 10.91 <0.16 46
(a)

FWHM CO(1-0)beam for IRAM observations, CO(2-1) beam for APEX observations.

(b)

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

(d)

The derivation of LFIR and dust masses Mdust is described in Sect. 5.2.

(e)

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

(f)

Molecular gas masses and upper limits either derived from our data or drawn from previous observations (see Sect. 3). Where CO(1-0) and CO(2-1) estimates are available, the larger mass or upper limit is reported here.

(g)

1.4 GHz continuum fluxes are drawn from the NRAO VLA Sky Survey (NVSS, Condon et al. 1998, 2002), the Faint Images of the Radio Sky at Twenty Centimeters survey (FIRST, Becker et al. 1995), or from Brown et al. (2011) except in the cases of NGC 924, NGC 978 and NGC 2563, where we extrapolate from the 610 MHz flux (Kolokythas et al. 2018) assuming a spectral index α = 0.8, and NGC 5903 where use the measured flux from O’Sullivan et al. (2018).

(h)

Mass estimated from offset pointing, see NGC 128-HI in Table 2.

(i)

Conflicting H I measurements, see text for discussion.

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