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27 April 2024 |
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Beyond Spheroids and Discs: Classifications of CANDELS Galaxy Structure at 1.4 < z < 2 via Principal Component Analysis | | Michael A. Peth
; Jennifer M. Lotz
; Peter E. Freeman
; Conor McPartland
; S. Alireza Mortazavi
; Gregory F. Snyder
; Norman A. Grogin
; Yicheng Guo
; Shoubaneh Hemati
; Jeyhan S. Karteltepe
; Dale D. Kocevski
; Anton M. Koekemoer
; Daniel H. McIntosh
; Hooshang Nayyeri
; Casey Papovich
; Joel R. Primack
; Raymond C. Simons
; Arjen van der Wel
; | | Date: |
7 Apr 2015 | | Abstract: | To understand the processes driving galaxy morphology and star formation, we
need a robust method to classify the structural elements of galaxies. Important
but rare and subtle features may be missed by traditional spiral, elliptical,
irregular or S’ersic bulge/disc classifications. To overcome this limitation,
we use a principal component analysis of non-parametric morphological
indicators (concentration, asymmetry, Gini coefficient, $M_{20}$, multi-mode,
intensity and deviation) measured at rest-frame $B$-band (corresponding to
HST/WFC3 F125W at 1.4 $< z <$ 2) to trace the natural distribution of massive
($>10^{10} M_{odot}$) galaxy morphologies. Principal component analysis (PCA)
quantifies the correlations between these morphological indicators and
determines the relative importance of each. The first three principal
components (PCs) capture $sim$75 per cent of the variance inherent to our
sample. We interpret the first principal component (PC) as bulge strength, the
second PC as dominated by concentration and the third PC as dominated by
asymmetry. Both PC1 and PC2 correlate with the visual appearance of a central
bulge and predict galaxy quiescence. We divide the PCA results into 10 groups
using an agglomerative hierarchical clustering method. Unlike S’ersic, this
classification scheme separates quenched compact galaxies from larger, smooth
proto-elliptical systems, and star-forming disc-dominated clumpy galaxies from
star-forming bulge-dominated asymmetric galaxies. Distinguishing between these
galaxy structural types in a quantitative manner is an important step towards
understanding the connections between morphology, galaxy assembly and
star-formation. | | Source: | arXiv, 1504.1751 | | Services: | Forum | Review | PDF | Favorites | |
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