Context : Dust and its emission is being increasingly used to constrain the evolutionary stage of galaxies .
A comprehensive characterization of dust , best achieved in nearby bright galaxies , is thus a highly useful resource .

Aims : We aim to characterize the relationship between dust properties ( mass , luminosity and temperature ) and their relationships with galaxy-wide properties ( stellar , atomic and molecular gas mass , and star formation mode ) .
We also aim to provide equations to estimate accurate dust properties from limited observational datasets .

Methods : We assemble a sample of 1,630 nearby ( z < 0.1 ) galaxies - over a large range of stellar masses ( M _ { * } ) , star formation rates ( SFR ) and specific star formation rates ( sSFR=SFR/M _ { * } ) - for which comprehensive and uniform multi-wavelength observations are available from WISE , IRAS , Planck and/or SCUBA .
the characterization of dust emission comes from spectral energy distribution ( SED ) fitting using Draine & Li dust models , which we parametrize using two components ( warm at 45 - 70 K and cold at 18 - 31 K ) .
The subsample of these galaxies with global measurements of CO and/or H { I } are used to explore the molecular and/or atomic gas content of the galaxies .

Results : The total infrared luminosity ( L _ { IR } ) , dust mass ( M _ { dust } ) and dust temperature of the cold component ( T _ { cold } ) form a plane that we refer to as the dust plane .
A galaxy ’ s sSFR drives its position on the dust plane : starburst ( high sSFR ) galaxies show higher L _ { IR } , M _ { dust } and T _ { cold } compared to Main Sequence ( typical sSFR ) and passive galaxies ( low sSFR ) .
Starburst galaxies also show higher specific dust masses ( M _ { dust } /M _ { * } ) and specific gas masses ( ~ { } M _ { gas } /M _ { * } ) .
We confirm earlier findings of an anti-correlation between the dust to stellar mass ratio and M _ { * } .
We also find different anti-correlations depending on sSFR ; the anti-correlation becomes stronger as the sSFR increases , with the spread due to different cold dust temperatures .
The dust mass is more closely correlated with the total gas mass ( atomic plus molecular ) than with the individual atomic and molecular gas masses .
Our comprehensive multi wavelength data allows us to define several equations to accurately estimate L _ { IR } , M _ { dust } and T _ { cold } from one or two monochromatic luminosities in the infrared and/or sub-millimeter .

Conclusions : It is possible to estimate the dust mass and infrared luminosity from a single monochromatic luminosity within the Rayleigh-Jeans tail of the dust emission , with errors of 0.12 and 0.20 dex , respectively .
These errors are reduced to 0.05 and 0.10 dex , respectively , if the dust temperature of the cold component is used .
The dust mass is better correlated with the total ISM mass ( ~ { } M _ { ISM } \propto M _ { dust } ^ { 0.7 } ) .
For galaxies with stellar masses 8.5 < log ( M _ { * } / ~ { } M _ { \odot } ) < 11.9 , the conversion factor between the single monochromatic luminosity at 850 ~ { } \hbox { $ \mu$m } and the total ISM mass ( \alpha _ { 850 ~ { } \hbox { $ \mu$m } } ) shows a large scatter ( rms = 0.29 dex ) and a weak correlation with the L _ { IR } .
The star formation mode of a galaxy shows a correlation with both the gas mass and dust mass : the dustiest ( high M _ { dust } /M _ { * } ) galaxies are gas-rich and show the highest SFRs .