Defining the (Black Hole)-Spheroid Connection with the Discovery of Morphology-Dependent Substructure in the $M_{\mathrm{BH}}$--${\mathrm{n}}_{\mathrm{sph}}$ and $M_{\mathrm{BH}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$ Diagrams: New Tests for Advanced Theories and Realistic Simulations

Abstract

For 123 local galaxies with directly-measured black hole masses ($M_{\mathrm{BH}}$), we provide the host spheroid's Sérsic index (${\mathrm{n}}_{\mathrm{sph}}$), effective half-light radius (${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$), and effective surface brightness (${\mu }_e$), obtained from careful multi-component decompositions, and we use these to derive the morphology-dependent $M_{\mathrm{BH}}$--${\mathrm{n}}_{\mathrm{sph}}$ and $M_{\mathrm{BH}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$ relations. We additionally present the morphology-dependent $M_{\ast ,\mathrm{sph}}$--${\mathrm{n}}_{\mathrm{sph}}$ and $M_{\ast ,\mathrm{sph}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$ relations. We explored differences due to: early-type galaxies (ETGs) versus late-type galaxies (LTGs); Sérsic versus core-Sérsic galaxies; barred versus non-barred galaxies; and galaxies with and without a stellar disk. We detect two different $M_{\mathrm{BH}}$--${\mathrm{n}}_{\mathrm{sph}}$ relations due to ETGs and LTGs with power-law slopes $3.95\pm 0.34$ and $2.85\pm 0.31$. We additionally quantified the correlation between $M_{\mathrm{BH}}$ and the spheroid's central concentration index, which varies monotonically with the Sérsic index. Furthermore, we observe a single, near-linear $M_{\ast ,\mathrm{sph}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}^{1.08\pm 0.04}$ relation for ETGs and LTGs, which encompasses both classical and alleged pseudobulges. In contrast, ETGs and LTGs define two distinct $M_{\mathrm{BH}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$ relations with ${\Delta }_{rms|BH}\sim 0.60\mathrm{dex}$ (cf.\ $\sim$0.51~dex for the $M_{\mathrm{BH}}$--$\sigma$ relation and $\sim$0.58~dex for the $M_{\mathrm{BH}}$--$M_{\ast ,\mathrm{sph}}$ relation), and the ETGs alone define two steeper $M_{\mathrm{BH}}$--${\mathrm{R}}_{\mathrm{e},\mathrm{sph}}$ relations, offset by $\sim$1~dex in the $\log M_{\mathrm{BH}}$-direction, depending on whether they have a disk or not and explaining their similar offset in the $M_{\mathrm{BH}}$--$M_{\ast ,\mathrm{sph}}$ diagram. This trend holds using $10\%$, $50\%$, or $90\%$ radii.(Abridged)

arXiv comment30 pages, 14 figures

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