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Galaxy And Mass Assembly (GAMA): the wavelength dependence of galaxy structure versus redshift and luminosity

Kennedy, R, Bamford, SP, Baldry, IK, Häußler, B, Holwerda, BW, Hopkins, AM, Kelvin, LS, Lange, R, Moffett, AJ, Popescu, CC, Taylor, EN, Tuffs, RJ, Vika, M and Vulcani, B (2015) Galaxy And Mass Assembly (GAMA): the wavelength dependence of galaxy structure versus redshift and luminosity. Monthly Notices of the Royal Astronomical Society, 454 (1). pp. 806-817. ISSN 0035-8711

1509.06756v3.pdf - Accepted Version

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We study how the sizes and radial profiles of galaxies vary with wavelength, by fitting Sersic functions simultaneously to imaging in nine optical and near-infrared bands. To quantify the wavelength dependence of effective radius we use the ratio, $\mathcal{R}$, of measurements in two restframe bands. The dependence of Sersic index on wavelength, $\mathcal{N}$, is computed correspondingly. Vulcani et al. (2014) have demonstrated that different galaxy populations present sharply contrasting behaviour in terms of $\mathcal{R}$ and $\mathcal{N}$. Here we study the luminosity dependence of this result. We find that at higher luminosities, early-type galaxies display a more substantial decrease in effective radius with wavelength, whereas late-types present a more pronounced increase in Sersic index. The structural contrast between types thus increases with luminosity. By considering samples at different redshifts, we demonstrate that lower data quality reduces the apparent difference between the main galaxy populations. However, our conclusions remain robust to this effect. We show that accounting for different redshift and luminosity selections partly reconciles the size variation measured by Vulcani et al. with the weaker trends found by other recent studies. Dividing galaxies by visual morphology confirms the behaviour inferred using morphological proxies, although the sample size is greatly reduced. Finally, we demonstrate that varying dust opacity and disc inclination can account for features of the joint distribution of $\mathcal{R}$ and $\mathcal{N}$ for late-type galaxies. However, dust does not appear to explain the highest values of $\mathcal{R}$ and $\mathcal{N}$. The bulge-disc nature of galaxies must also contribute to the wavelength-dependence of their structure.

Item Type: Article
Additional Information: This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Galaxy And Mass Assembly (GAMA): the wavelength dependence of galaxy structure versus redshift and luminosity is available online at: http://dx.doi.org/doi:10.1093/mnras/stv2032
Uncontrolled Keywords: astro-ph.GA; astro-ph.GA
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Related URLs:
Date Deposited: 05 Oct 2015 09:29
Last Modified: 04 Sep 2021 13:55
URI: https://researchonline.ljmu.ac.uk/id/eprint/2118
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