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The correlation between black hole mass and the stellar mass of the bulge ofthe host galaxy has attracted much attention ever since its discovery. Whiletraditional investigations of this correlation have treated elliptical galaxiesas single, monolithic spheroids, the recent realization that massive ellipticalgalaxies have undergone significant late-time ($z \lesssim 2$) dissipationlessassembly since their initially dense "red nugget" phase strongly suggests thatblack holes in present-day ellipticals should be associated only with theircores and not with their extended envelopes. We perform two-dimensional imagedecomposition of Two Micron All Sky Survey $K_s$-band images to derive thestellar mass of the cores of 35 nearby ellipticals with reliably measured blackhole masses. We revisit the relation between black hole mass and bulge stellarmass by combining classical bulges with the cores of ellipticals. The newrelation exhibits nearly identical slope ($M_{\bullet} \proptoM_{\text{core}}^{1.2}$) as the conventional relation but a factor of $\sim2$higher normalization and moderately larger intrinsic scatter (0.4 dex). At acore mass of $10^{11}\,M_{\odot}$, $M_{\bullet}/M_{\text{core}} = 0.9\%$, butit rises to $M_{\bullet}/M_{\text{core}}=1.5\%$ for the most massive cores withmass $10^{12}\,M_{\odot}$. Fast and slow rotator ellipticals follow the samecorrelation. The $M_{\bullet}-M_{\text{core}}$ relation provides a revisedbenchmark for studies of black hole-galaxy coevolution in the high-redshiftUniverse.

The Correlation between Black Hole Mass and Stellar Mass for Classical Bulges and the Cores of Ellipticals