some bright cirrus filament or a bright galaxy. Our manual fine-tuning avoids such background problem.

FIR and radio continuum emission in local volume galaxies {#sec:emission}
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FIR-radio correlation {#subsec:frc}
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As in @2001ApJ...554..803Y, we define the FIR-to-radio ratio $q$ as:

$$q \equiv \log(\frac{F_\mathrm{FIR}}{3.75\times10^{12}{\ensuremath{\,\mathrm{W\,m^{-2}}}}}) - \log(\frac{F_\mathrm{1.4\,GHz}}{10^{26}{\ensuremath{\,\mathrm{Jy}}}}).$$

Here the total FIR flux density is calculated from 60[$\,\mathrm{\mu m}$]{} and 100[$\,\mathrm{\mu m}$]{} flux densities as below [@1988ApJS...68..151H]:

$$F_{\mathrm{FIR}} = 1.26 \times 10^{-14} \times (2.58 \times \frac{f_\nu(60{\ensuremath{\,\mathrm{\mu m}}})}{1{\ensuremath{\,\mathrm{Jy}}}} + \frac{f_\nu(100{\ensuremath{\,\mathrm{\mu m}}})}{1{\ensuremath{\,\mathrm{Jy}}}}){\ensuremath{\,\mathrm{W\,m^{-2}}}}.$$

Figure \[fig:frc\] shows the distribution of LVHIS galaxies on the FIR-radio plane. There are totally 30 galaxies detected in both wavelengths (3 of them are potentially contaminated by nuclear emission). We confirm strong correlation between FIR and radio continuum flux densities, for full sample, massive galaxies and dwarf galaxies, respectively, by using the Spearman rank correlation coefficient (see Table \[tab:stats\]).

![image](fig/frc.pdf){width="16cm"}

. \[fig:frc\]

The data are fit with power law model ($\log(y)=a\log(x)+b$) by using orthogonal distance regression method in log-log space (throughout this paper, “linear” refers $a=1$). In order to properly estimate the uncertainty of the fitting results, bootstrapping method is used. 10000 random runs are performed to resample the galaxies. The flux density of each simulated source is the observed value added 