CHANG-ES - VI. Probing Supernova energy deposition in spiral galaxies through multiwavelength relationships

16How a galaxy regulates its supernovae (SNe) energy into different interstellar/circumgalactic medium components strongly affects galaxy evolution. Based on the JVLA D-configuration C-(6 GHz) and L-band (1.6 GHz) continuum observations, we perform statistical analysis comparing multiwavelength properties of the Continuum Haloes in Nearby Galaxies - an EVLA Survey galaxies. The high-quality JVLA data and edge-on orientation enable us for the first time to include the halo into the energy budget for a complete radio-flux-limited sample. We find tight correlations of L-radio with the mid-IR-based star formation rate (SFR). The normalization of our I1.6 GHz/WHz-1-SFR relation is similar to 2-3times of those obtained for face-on galaxies, probably a result of enhanced IR extinction at high inclination. We also find tight correlations between L-radio and the SNe energy injection rate. (E)over dot(SN)(Ia+CC), indicating the energy loss via synchrotron radio continuum accounts for similar to 1 of. (E)over dot(SN), comparable to the energy contained in cosmic ray electrons. The integrated C-to-L-band spectral index is alpha similar to 0.5-1.1 for non-active galactic nucleus galaxies, indicating a dominance by the diffuse synchrotron component. The low-scatter L-radio-SFR/L-radio-. E SN(Ia+CC) relationships have superlinear logarithmic slopes at similar to 2 sigma in L band (1.132 +/- 0.067/1.175 +/- 0.102) while consistent with linear in C band (1.057 +/- 0.075/1.100 +/- 0.123). The superlinearity could be naturally reproduced with non-calorimeter models for galaxy discs. Using Chandra halo X-ray measurements, we find sublinear LX-L-radio relations. These results indicate that the observed radio halo of a starburst galaxy is close to electron calorimeter, and a galaxy with higher SFR tends to distribute an increased fraction of SNe energy into radio emission (than X-ray).reservedmixedLi JT; Beck R; Dettmar RJ; Heald G; Irwin J; Johnson M; Kepley AA; Krause M; Murphy EJ; Orlando E; Rand RJ; Strong AW; Vargas CJ; Walterbos R; Wang QD; Wiegert TLi, Jt; Beck, R; Dettmar, Rj; Heald, G; Irwin, J; Johnson, M; Kepley, Aa; Krause, M; Murphy, Ej; Orlando, E; Rand, Rj; Strong, Aw; Vargas, Cj; Walterbos, R; Wang, Qd; Wiegert,