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J/MNRAS/458/963     CANDELS galaxy structure classification       (Peth+, 2016)

Beyond spheroids and discs: classifications of CANDELS galaxy structure at 1.4 < z < 2 via principal component analysis. Peth M.A., Lotz J.M., Freeman P.E., McPartland C., Mortazavi S.A., Snyder G.F., Barro G., Grogin N.A., Guo Y., Hemmati S., Kartaltepe J.S., Kocevski D.D., Koekemoer A.M., McIntosh D.H., Nayyeri H., Papovich C., Primack J.R., Simons R.C. <Mon. Not. R. Astron. Soc., 458, 963-987 (2016)> =2016MNRAS.458..963P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Redshifts ; Morphology Keywords: methods: statistical - catalogues - galaxies: evolution - galaxies: structure Abstract: Important but rare and subtle processes driving galaxy morphology and star formation may be missed by traditional spiral, elliptical, irregular or Sersic bulge/disc classifications. To overcome this limitation, we use a principal component analysis (PCA) of non-parametric morphological indicators (concentration, asymmetry, Gini coefficient, M20, multimode, 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 (>1010M) galaxy morphologies. PCA quantifies the correlations between these morphological indicators and determines the relative importance of each. The first three principal components (PCs) capture ∼75 per cent of the variance inherent to our sample. We interpret the first 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. PC1 is a better predictor of quenching than stellar mass, as good as other structural indicators (Sersic-n or compactness). We divide the PCA results into groups using an agglomerative hierarchical clustering method. Unlike Sersic, this classification scheme separates compact galaxies from larger, smooth protoelliptical 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. Description: We use the CANDELS H-band (F160W) selected multiwavelength catalogues (UDS, Galametz et al. 2013, Cat. J/ApJS/206/10; GOODS-S, Guo et al. 2013, Cat. J/ApJS/207/24; COSMOS, Nayyeri et al. in preparation), photometric redshifts (Dahlen et al., 2013ApJ...775...93D), non-parametric morphologies (this work), Sersic parameters (van der Wel et al., 2012, Cat. J/ApJS/203/24), visual classifications (Kartaltepe et al., 2015, Cat. J/ApJS/221/11), rest-frame photometry, and stellar masses (this work). The limiting magnitude for HST/WFC3 F125W and F160W are 27.35 and 27.45, respectively, with full width half-maximum (FWHM) of ∼0.135arcsec and ∼0.15arcsec, respectively. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 232 1244 Non-parametric morphology statistics and PC values for CANDELS (UDS/GOODS-S/COSMOS) galaxies
See also: J/ApJS/207/24 : GOODS-S CANDELS multiwavelength catalog (Guo+, 2013) J/ApJS/206/10 : CANDELS multiwavelength catalog (Galametz+, 2013) J/ApJS/203/24 : CANDELS galaxies structural parameters (van der Wel+, 2012) J/ApJS/221/11 : CANDELS visual classifications for GOODS-S (Kartaltepe+, 2015) J/ApJ/801/97 : GOODS-S+UDS stellar mass catalogs from CANDELS (Santini+, 2015) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 5 I5 --- ID Galaxy identification number, from Galametz et al., Cat. J/ApJS/206/10 7- 16 F10.6 deg RAdeg ?=-99 Rigth ascension (J2000) 18- 27 F10.6 deg DEdeg ?=-99 Declination (J2000) 29- 36 F8.6 --- CJ Concentration index (1) 38- 46 F9.6 --- AsymJ Asymmetry (1) 48- 56 F9.6 --- M20J M2, second order moment of the brightest regions of a galaxy (1) 58- 65 F8.6 --- GINIJ Gini coefficient (1) 67- 76 F10.6 --- MJ ?=-99 Multimode statistic (ratio, in pixels, of the two brightest regions of a galaxy) (1) 78- 85 F8.6 --- IJ Intensity (ratio, in flux, of the two brightest regions) (1) 87- 94 F8.6 --- DJ Deviation (distance between the intensity centroid of a galaxy and the center of the brightest region) (1) 96-104 F9.6 [Msun] logMass Mass 106-113 F8.6 --- zphot Photometric redshift 115-116 I2 --- Group Group number 118-126 F9.6 --- PC1 Principal component 1 (bulge strength indicator) 128-136 F9.6 --- PC2 Principal component 2 (dominated by concentration) 138-147 F10.6 --- PC3 Principal component 3 (dominated by asymmetry) 149-157 F9.6 --- PC4 Principal component 4 159-167 F9.6 --- PC5 Principal component 5 169-177 F9.6 --- PC6 Principal component 6 179-187 F9.6 --- PC7 Principal component 7 189-192 F4.2 --- pGoutlier Probability of a galaxy being outlier 194-197 F4.2 --- pG0 Probability of a galaxy being in group 0 199-202 F4.2 --- pG1 Probability of a galaxy being in group 1 204-207 F4.2 --- pG2 Probability of a galaxy being in group 2 209-212 F4.2 --- pG4 Probability of a galaxy being in group 4 214-217 F4.2 --- pG5 Probability of a galaxy being in group 5 219-222 F4.2 --- pG6 Probability of a galaxy being in group 6 224-227 F4.2 --- pG8 Probability of a galaxy being in group 8 229-232 F4.2 --- pG9 Probability of a galaxy being in group 9
Note (1): measured at rest-frame J-band.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 26-May-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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