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[Abridged] Tight correlations between supermassive black hole (SMBH) mass($M_{\rm BH}$) and the properties of the host galaxy have useful implicationsfor our understanding of the growth of SMBHs and evolution of galaxies. Here,we present newly observed correlations between $M_{\rm BH}$ and the host galaxytotal UV$-$ [3.6] color ($\mathcal{C_{\rm UV,tot}}$, Pearson's r = $0.6-0.7$)for a sample of 67 galaxies (20 early-type galaxies and 47 late-type galaxies)with directly measured $M_{\rm BH}$ in the GALEX/S$^{4}$G survey. The colorsare carefully measured in a homogeneous manner using the galaxies' FUV, NUV and3.6 $\micron$ magnitudes and their multi-component structural decompositions inthe literature. We find that more massive SMBHs are hosted by (early- andlate-type) galaxies with redder colors, but the $M_{\rm BH}- \mathcal{C_{\rmUV,tot}}$ relations for the two morphological types have slopes that differ at$\sim 2 \sigma$ level. Early-type galaxies define a red sequence in the $M_{\rmBH}- \mathcal{C_{\rm UV,tot}}$ diagrams, while late-type galaxies trace a bluesequence. Within the assumption that the specific star formation rate of agalaxy (sSFR) is well traced by $L_{\rm UV}/L_{\rm 3.6}$, it follows that theSMBH masses for late-type galaxies exhibit a steeper dependence on sSFR thanthose for early-type galaxies. The $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ and$M_{\rm BH}-L_{\rm 3.6,tot}$ relations for the sample galaxies reveal acomparable level of vertical scatter in the log $M_{\rm BH}$ direction, roughly$5\%-27\%$ more than the vertical scatter of the $M_{\rm BH}-\sigma$ relation.Our $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ relations suggest different channelsof SMBH growth for early- and late-type galaxies, consistent with theirdistinct formation and evolution scenarios.

The (black hole mass)-(color) relations for early- and late-type galaxies: red and blue sequences