The role of young and evolved stars in the heating of dust in local galaxies

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Table 4.

Correlation coefficients and p-values for each sample galaxy.

Galaxy	r_{T_dust − Σ_SFR}	r_{T_dust − Σ_{M_*}}	p_{T_dust − Σ_dust}
NGC 300	0.79	0.61	0.008
NGC 2403	0.77	0.63	0.016
IC 342	0.36	0.71	0.963
NGC 7793	0.88	0.63	0.001
NGC 3031 (M 81)	0.64	0.66	0.297
NGC 6946	0.57	0.79	0.994
NGC 4736 (M 94)	0.70	0.73	0.995
NGC 5236 (M 83)	0.50	0.52	0.981
NGC 3621	0.81	0.60	0.014
NGC 5457 (M 101)	0.68	0.18	0.159
NGC 5194 (M 51)	0.67	0.70	1.000
NGC 925	0.83	0.37	0.012
NGC 628 (M 74)	0.85	0.70	0.254
NGC 5055 (M 63)	0.87	0.77	1.000
NGC 4725	0.80	0.76	0.239
NGC 3521	0.79	0.69	0.996
NGC 1097	0.59	0.71	0.193
NGC 1365	0.40	0.62	1.000

Notes. Weighted Pearson correlation coefficients of the T_dust − Σ_SFR (r_{T_dust − Σ_SFR}) and T_dust − Σ_{M_*} (r_{T_dust − Σ_{M_*}}) correlations (see Sect. 3.3.1) and p-value of the χ² fit for the T_dust − Σ_dust correlation for each sample galaxy (see Sect. 3.3.2).

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