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Date and Time of the Query: 2019-04-20 T00:10:08 PDT
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For refcode 2014ApJ...781...12H:
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Copyright by American Astronomical Society. Reproduced by permission
2014ApJ...781...12H Morphological Parameters of a Spitzer Survey of Stellar Structure in Galaxies Holwerda, B. W.; Munoz-Mateos, J.-C.; Comeron, S.; Meidt, S.; Sheth, K.; Laine, S.; Hinz, J. L.; Regan, M. W.; Gil de Paz, A.; Menendez-Delmestre, K.; Seibert, M.; Kim, T.; Mizusawa, T.; Laurikainen, E.; Salo, H.; Laine, J.; Gadotti, D. A.; Zaritsky, D.; Erroz-Ferrer, S.; Ho, L. C.; Knapen, J. H.; Athanassoula, E.; Bosma, A.; Pirzkal, N. Abstract. The morphology of galaxies can be quantified to some degree using a set of scale-invariant parameters. Concentration (C), asymmetry (A), smoothness (S), the Gini index (G), the relative contribution of the brightest pixels to the second-order moment of the flux (M_20_), ellipticity (E), and the Gini index of the second-order moment (G_M_) have all been applied to morphologically classify galaxies at various wavelengths. Here, we present a catalog of these parameters for the Spitzer Survey of stellar structure in Galaxies, a volume-limited, near-infrared (NIR) imaging survey of nearby galaxies using the 3.6 and 4.5 micron channels of the Infrared Array Camera on board the Spitzer Space Telescope. Our goal is to provide a reference catalog of NIR quantified morphology for high-redshift studies and galaxy evolution models with enough detail to resolve stellar mass morphology. We explore where normal, non-interacting galaxies---those typically found on the Hubble tuning fork---lie in this parameter space and show that there is a tight relation between concentration (C_82_) and M_20_ for normal galaxies. M_20_ can be used to classify galaxies into earlier and later types (i.e., to separate spirals from irregulars). Several criteria using these parameters exist to select systems with a disturbed morphology, i.e., those that appear to be undergoing a tidal interaction. We examine the applicability of these criteria to Spitzer NIR imaging. We find that four relations, based on the parameters A and S, G and M_20_, G_M_, C, and M_20_, respectively, select outliers in morphological parameter space, but each selects different subsets of galaxies. Two criteria (G_M_ > 0.6, G > --0.115 x M_20_ + 0.384) seem most appropriate to identify possible mergers and the merger fraction in NIR surveys. We find no strong relation between lopsidedness and most of these morphological parameters, except for a weak dependence of lopsidedness on concentration and M_20_. Key words: galaxies: elliptical and lenticular, cD, galaxies: general, galaxies: irregular, galaxies: spiral, galaxies: statistics, galaxies: stellar content, galaxies: structure
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