SIMBAD references

We continue to explore the relationship between the total number of globular clusters (GCs), N_GC, and the central black hole mass, M_•, in spiral galaxies. We present here results for the Sab galaxies NGC 3368, NGC 4736 (M94), and NGC 4826 (M64), and the Sm galaxy NGC 4395. The GC candidate selection is based on the (u* - $i^{\prime} $) versus ($i^{\prime} $ - K_s) color-color diagram, and $i^{\prime} $-band shape parameters. We determine the M_• versus N_GC correlation for these spirals, plus NGC 4258, NGC 253, M104, M81, M31, and the Milky Way. We also redetermine the correlation for the elliptical sample in Harris et al., with updated galaxy types from Sahu et al. Additionally, we derive the total stellar galaxy mass, M_*, from its two-slope correlation with N_GC, and fit M_• versus M_* for both spirals and ellipticals. We obtain log M_• ∝ (1.01 ± 0.13) log N_GC for ellipticals, and log M_• ∝ (1.64 ± 0.24) log N_GC for late-type galaxies (LTGs). The linear M_• versus N_GC correlation in ellipticals could be due to statistical convergence through mergers, unlike the much steeper correlation for LTGs. However, in the M_• versus total stellar mass (M_*) parameter space, with M_* derived from its correlation with N_GC, M_• ∝ (1.48 ± 0.18) log M_* for ellipticals, and M_• ∝ (1.21 ± 0.16) log M_* for LTGs. The observed agreement between ellipticals and LTGs in this parameter space may imply that black holes and galaxies coevolve through calm accretion, active galactic nuclei feedback, and other secular processes.