SIMBAD references

In our first paper, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, M_BH, imaged at 3.6µm with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between M_BH and the host spheroid (and galaxy) luminosity, L_sph(and L_gal), and also stellar mass, M_*,sph. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have M_BH < 10⁷M_☉ and allows us to better investigate the poorly studied low-mass end of the M_BH-M_*,sph correlation. The bulges of early-type galaxies follow M_BH ∝ M_*,sph^1.04±0.10 and define a tight red sequence with intrinsic scatter ≡(M_BH/M_*,sph) = 0.43 ± 0.06 dex and a median M_BH/M_*, sph_ ratio of 0.68±0.04%, i.e., a ± 2 σ range of 0.1%-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with M_BH ∝ M_*,sph^2–3 and M_BH/M_*,sph equal to 0.02% at M_BH ≈ 10⁶ M_☉ We additionally report that (1) our Sérsic galaxy sample follows M_BH ∝ M_*,sph^1.48±0.20 a less steep sequence than previously reported; (2) bulges with Sérsic index n_sph < 2 argued by some to be pseudo-bulges, are not offset to lower M_BH from the correlation defined by the current bulge sample with n_sph > 2; and (3) L_sphand L_galcorrelate equally well with M_BH, in terms of intrinsic scatter, only for early-type galaxies–once reasonable numbers of spiral galaxies are included, the correlation with L_sphis better than that with L_gal.