SIMBAD references

We present a catalog of 422 galaxies with published measurements of their globular cluster (GC) populations. Of these, 248 are E galaxies, 93 are S0 galaxies, and 81 are spirals or irregulars. Among various correlations of the total number of GCs with other global galaxy properties, we find that N_GC correlates well though nonlinearly with the dynamical mass of the galaxy bulge M_dyn = 4σ_e²R_e/G, where σ_e is the central velocity dispersion and R_e the effective radius of the galaxy light profile. We also present updated versions of the GC specific frequency S_N and specific mass S_Mversus host galaxy luminosity and baryonic mass. These graphs exhibit the previously known U-shape: highest S_N or S_Mvalues occur for either dwarfs or supergiants, but in the midrange of galaxy size (10⁹-10¹⁰ L_☉) the GC numbers fall along a well-defined baseline value of S_N≃ 1 or S_M= 0.1, similar among all galaxy types. Along with other recent discussions, we suggest that this trend may represent the effects of feedback, which systematically inhibited early star formation at either very low or very high galaxy mass, but which had its minimum effect for intermediate masses. Our results strongly reinforce recent proposals that GC formation efficiency appears to be most nearly proportional to the galaxy halo mass M_halo. The mean "absolute" efficiency ratio for GC formation that we derive from the catalog data is M_GCS/M_halo= 6 x10^–5. We suggest that the galaxy-to-galaxy scatter around this mean value may arise in part because of differences in the relative timing of GC formation versus field-star formation. Finally, we find that an excellent empirical predictor of total GC population for galaxies of all luminosities is N_GC ∼ (R_eσ_e)^1.3, a result consistent with fundamental plane scaling relations.