TY - JOUR
T1 - Advanced morphological galaxy classification: A comparison of observed and simulated galaxies
AU - Hambleton, K
AU - Gibson, Brad
AU - Brook, Chris
AU - Stinson, G
AU - Conselice, Christopher
AU - Bailin, J
AU - Couchman, H
AU - Wadsley, J
PY - 2011
Y1 - 2011
N2 - Encoded within the morphological structure of galaxies are clues related to their formation and evolutionary history. Recent advances pertaining to the statistics of galaxy morphology include sophisticated measures of concentration (C), asymmetry (A) and clumpiness (S). In this study, these three parameters (CAS) have been applied to a suite of simulated galaxies and compared with observational results inferred from a sample of nearby galaxies. The simulations span a range of late-type systems, with masses between a??1010 and a??1012 MaS?, and employ star formation density thresholds between 0.1 and 100cm-3. We have found that the simulated galaxies possess comparable concentrations to their observed counterparts. However, the results of the CAS analysis revealed that the simulated galaxies are generally more asymmetric, and that the range of clumpiness values extends beyond the range of those observed. Strong correlations were obtained between the three CAS parameters and colour (B-V), consistent with observed galaxies. Furthermore, the simulated galaxies possess strong links between their CAS parameters and Hubble type, mostly in-line with their observed counterparts.
AB - Encoded within the morphological structure of galaxies are clues related to their formation and evolutionary history. Recent advances pertaining to the statistics of galaxy morphology include sophisticated measures of concentration (C), asymmetry (A) and clumpiness (S). In this study, these three parameters (CAS) have been applied to a suite of simulated galaxies and compared with observational results inferred from a sample of nearby galaxies. The simulations span a range of late-type systems, with masses between a??1010 and a??1012 MaS?, and employ star formation density thresholds between 0.1 and 100cm-3. We have found that the simulated galaxies possess comparable concentrations to their observed counterparts. However, the results of the CAS analysis revealed that the simulated galaxies are generally more asymmetric, and that the range of clumpiness values extends beyond the range of those observed. Strong correlations were obtained between the three CAS parameters and colour (B-V), consistent with observed galaxies. Furthermore, the simulated galaxies possess strong links between their CAS parameters and Hubble type, mostly in-line with their observed counterparts.
UR - http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.19532.x/abstract
U2 - 10.1111/j.1365-2966.2011.19532.x
DO - 10.1111/j.1365-2966.2011.19532.x
M3 - Article
VL - 418
SP - 801
EP - 810
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -