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We present an improved study of the relation between supermassive black holegrowth and their host galaxy properties in the local Universe (z < 0.33). Tothis end, we build an extensive sample combining spectroscopic measurements ofstar-formation rate (SFR) and stellar mass from Sloan Digital Sky Survey, withspecific Black Hole accretion rate (sBHAR, $\lambda_{\mathrm{sBHAR}} \proptoL_{\mathrm{X}}/\mathcal{M}_{\ast}$) derived from the XMM-Newton SerendipitousSource Catalogue (3XMM-DR8) and the Chandra Source Catalogue (CSC 2.0). We findthat the sBHAR probability distribution for both star-forming and quiescentgalaxies has a power-law shape peaking at $\log\lambda_{\mathrm{sBHAR}}\sim-3.5$ and declining toward lower sBHAR in all stellar mass ranges. This findingconfirms the decrease of AGN activity in the local Universe compared to higherredshifts. We observe a significant correlation between$\log\,\lambda_{\mathrm{sBHAR}}$ and $\log\,{\mathrm{SFR}}$ in almost allstellar mass ranges, but the relation is shallower compared to higherredshifts, indicating a reduced availability of accreting material in the localUniverse. At the same time, the BHAR-to-SFR ratio for star-forming galaxiesstrongly correlates with stellar mass, supporting the scenario where both AGNactivity and stellar formation primarily depend on the stellar mass viafuelling by a common gas reservoir. Conversely, this ratio remains constant forquiescent galaxies, possibly indicating the existence of the different physicalmechanisms responsible for AGN fuelling or different accretion mode inquiescent galaxies.

Probing supermassive black hole growth and its dependence on stellar mass and star-formation rate in low-redshift galaxies