A New Nonparametric Approach to Galaxy Morphological Classification

We present two new non-parametric methods for quantifying galaxy morphology:the relative distribution of the galaxy pixel flux values (the Gini coefficientor G) and the second-order moment of the brightest 20% of the galaxy's flux(M20). We test the robustness of G and M20 to decreasing signal-to-noise andspatial resolution, and find that both measures are reliable to within 10% ataverage signal-to-noise per pixel greater than 3 and resolutions better than1000 pc and 500 pc, respectively. We have measured G and M20, as well asconcentration (C), asymmetry (A), and clumpiness (S) in the rest-framenear-ultraviolet/optical wavelengths for 150 bright local "normal" Hubble typegalaxies (E-Sd) galaxies and 104 0.05 < z < 0.25 ultra-luminous infraredgalaxies (ULIRGs).We find that most local galaxies follow a tight sequence inG-M20-C, where early-types have high G and C and low M20 and late-type spiralshave lower G and C and higher M20. The majority of ULIRGs lie above the normalgalaxy G-M20 sequence, due to their high G and M20 values. Their high Ginicoefficients arise from very bright nuclei, while the high second-order momentsare produced by multiple nuclei and bright tidal tails. All of these featuresare signatures of recent and on-going mergers and interactions. We also findthat in combination with A and S, G is more effective than C at distinguishingULIRGs from the "normal" Hubble-types. Finally, we measure the morphologies of45 1.7 < z < 3.8 galaxies from HST NICMOS observations of the Hubble Deep FieldNorth. We find that many of the z $\sim$ 2 galaxies possess G and A higher thanexpected from degraded images of local elliptical and spiral galaxies, and havemorphologies more like low-redshift single nucleus ULIRGs.Comment: 48 pages, 9 tables and 17 figures, accepted to the Astronomical Journal with minor revision