|X CO||Variable||Samplea||c||d||ρ b||σ c||N.obj.|
|Constant||log[πr24.5(g)2]||all||0.75 ± 0.11||7.02 ± 0.26||0.51||0.34||96|
|Lum.dep.||all||0.43 ± 0.10||7.74 ± 0.23||0.37||0.35||96|
|Constant||logMstar||all||0.81 ± 0.07||0.84 ± 0.73||0.69||0.27||95|
|Lum.dep.||all||0.49 ± 0.07||3.95 ± 0.71||0.52||0.31||95|
|Constant||logMstar||Kuno||1.01 ± 0.37||−0.76 ± 3.79||0.69||0.14||8|
|Lum.dep.||Kuno||0.80 ± 0.32||1.24 ± 3.29||0.62||0.13||8|
Notes. Linear fit.
The sample used to fit the M(H2) vs. Variable relations is composed of all spiral galaxies (all) with molecular gas (considering CO non-detections as detections) with and Hi deficiency parameter Hi − def≤ 0.4 (black filled dots and triangles in Figs. 1 and 2). The sample Kuno indicates the subsample of galaxies with integarted CO data from Kuno et al. (2007). For this subsample, the galaxies used to fit the relation are all those with Hi − def≤ 0.4 (red filled squares in Fig. 3).
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