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Date and Time of the Query: 2019-04-20 T05:59:08 PDT
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For refcode 2014AJ....148..111P:
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Copyright by American Astronomical Society. Reproduced by permission
2014AJ....148..111P The FUV to Near-IR Morphologies of Luminous Infrared Galaxies in the Goals Sample Petty, S. M.; Armus, L.; Charmandaris, V.; Evans, A. S.; Le Floc'h, E.; Bridge, C.; Diaz-Santos, T.; Howell, J. H.; Inami, H.; Psychogyios, A.; Stierwalt, S.; Surace, J. A. Abstract. We compare the morphologies of a sample of 20 luminous infrared galaxies (LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS) in the FUV, B, I, and H bands, using the Gini (G) and M_20_ parameters to quantitatively estimate the distribution and concentration of flux as a function of wavelength. Hubble Space Telescope (HST) images provide an average spatial resolution of ~ 80 pc. While our LIRGs can be reliably classified as mergers across the entire range of wavelengths studied here, there is a clear shift toward more negative M_20_ (more bulge-dominated) and a less significant decrease in G values at longer wavelengths. We find no correlation between the derived FUV G-M_20_ parameters and the global measures of the IR to FUV flux ratio (IRX). Given the fine resolution in our HST data, this suggests either that the UV morphology and IRX are correlated on very small scales, or that the regions emitting the bulk of the IR emission emit almost no FUV light. We use our multi-wavelength data to simulate how merging LIRGs would appear from z~ 0.5--3 in deep optical and near-infrared images such as the Hubble Ultra-Deep Field, and use these simulations to measure the G-M_20_ at these redshifts. Our simulations indicate a noticeable decrease in G, which flattens at z>=slant 2 by as much as 40%, resulting in mis-classifying our LIRGs as disk-like, even in the rest-frame FUV. The higher redshift values of M_20_ for the GOALS sources do not appear to change more than about 10% from the values at z~ 0. The change in G-M_20_ is caused by the surface brightness dimming of extended tidal features and asymmetries, and also the decreased spatial resolution which reduced the number of individual clumps identified. This effect, seen as early as z~ 0.5, could easily lead to an underestimate of the number of merging galaxies at high-redshift in the rest-frame FUV. Key words: galaxies: structure, infrared: galaxies, ultraviolet: galaxies
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