Structural and Stellar Population Properties vs. Bulge Types in Sloan Digital Sky Survey Central Galaxies

Abstract

This paper studies pseudo-bulges (P-bulges) and classical bulges (C-bulges) in Sloan Digital Sky Survey central galaxies using the new bulge indicator $\Delta {\Sigma }_1$, which measures relative central stellar-mass surface density within 1 kpc. We compare $\Delta {\Sigma }_1$ to the established bulge-type indicator $\Delta ⟨{\mu }_e⟩$ from Gadotti (2009) and show that classifying by $\Delta {\Sigma }_1$ agrees well with $\Delta ⟨{\mu }_e⟩$. $\Delta {\Sigma }_1$ requires no bulge-disk decomposition and can be measured on SDSS images out to $z=0.07$. Bulge types using it are mapped onto twenty different structural and stellar-population properties for 12,000 SDSS central galaxies with masses 10.0 < log $M_{\ast }$/$M_{\odot }$ < 10.4. New trends emerge from this large sample. Structural parameters show fairly linear log-log relations vs. $\Delta {\Sigma }_1$ and $\Delta ⟨{\mu }_e⟩$ with only moderate scatter, while stellar-population parameters show a highly non-linear "elbow" in which specific star-formation rate remains roughly flat with increasing central density and then falls rapidly at the elbow, where galaxies begin to quench. P-bulges occupy the low-density end of the horizontal arm of the elbow and are universally star-forming, while C-bulges occupy the elbow and the vertical branch and exhibit a wide range of star-formation rates at fixed density. The non-linear relation between central density and star-formation rate has been seen before, but this mapping onto bulge class is new. The wide range of star-formation rates in C-bulges helps to explain why bulge classifications using different parameters have sometimes disagreed in the past. The elbow-shaped relation between density and stellar indices suggests that central structure and stellar-populations evolve at different rates as galaxies begin to quench.

23 pages, 17 figures, published in MNRAS

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