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Title:
Galaxy And Mass Assembly (GAMA): understanding the wavelength dependence of galaxy structure with bulge-disc decompositions
Authors:
Kennedy, Rebecca; Bamford, Steven P.; Häußler, Boris; Baldry, Ivan; Bremer, Malcolm; Brough, Sarah; Brown, Michael J. I.; Driver, Simon; Duncan, Kenneth; Graham, Alister W.; Holwerda, Benne W.; Hopkins, Andrew M.; Kelvin, Lee S.; Lange, Rebecca; Phillipps, Steven; Vika, Marina; Vulcani, Benedetta
Affiliation:
AA(School of Physics and Astronomy, The University of Nottingham, University Park, Nottingham NG7 2RD, UK ), AB(School of Physics and Astronomy, The University of Nottingham, University Park, Nottingham NG7 2RD, UK), AC(University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, Oxon OX1 3RH, UK; University of Hertfordshire, Hatfield, Hertfordshire AL10 9AB, UK; European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile), AD(ARI, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), AE(School of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol BS8 1TL, UK), AF(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), AG(School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia), AH(ICRAR, The University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia; SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AI(School of Physics and Astronomy, The University of Nottingham, University Park, Nottingham NG7 2RD, UK; Leiden Observatory, Leiden University, NL-2300 RA Leiden, the Netherlands), AJ(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, VIC 3122, Australia), AK(Leiden Observatory, Leiden University, NL-2300 RA Leiden, the Netherlands), AL(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), AM(ARI, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), AN(ICRAR, The University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia), AO(School of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol BS8 1TL, UK), AP(IAASARS, National Observatory of Athens, GR-15236 Penteli, Greece), AQ(Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, the University of Tokyo, Kashiwa 277-8582, Japan)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 460, Issue 4, p.3458-3471 (MNRAS Homepage)
Publication Date:
08/2016
Origin:
CROSSREF; OUP
Astronomy Keywords:
galaxies: formation, galaxies: fundamental parameters, galaxies: general, galaxies: structure
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stw1176
Bibliographic Code:
2016MNRAS.460.3458K

Abstract

With a large sample of bright, low-redshift galaxies with optical-near-IR imaging from the GAMA survey we use bulge-disc decompositions to understand the wavelength-dependent behaviour of single-Sérsic structural measurements. We denote the variation in single-Sérsic index with wavelength as {N}, likewise for effective radius we use {R}. We find that most galaxies with a substantial disc, even those with no discernable bulge, display a high value of {N}. The increase in Sérsic index to longer wavelengths is therefore intrinsic to discs, apparently resulting from radial variations in stellar population and/or dust reddening. Similarly, low values of {R} (< 1) are found to be ubiquitous, implying an element of universality in galaxy colour gradients. We also study how bulge and disc colour distributions vary with galaxy type. We find that, rather than all bulges being red and all discs being blue in absolute terms, both components become redder for galaxies with redder total colours. We even observe that bulges in bluer galaxies are typically bluer than discs in red galaxies, and that bulges and discs are closer in colour for fainter galaxies. Trends in total colour are therefore not solely due to the colour or flux dominance of the bulge or disc.
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