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Cited by 294

The DOI matches its Crossref record; 71 of the 71 references it cites were found in a registry or an index.

Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology

Open access
Lange, Rebecca, Driver, Simon P., Robotham, Aaron S. G., Kelvin, Lee S., Graham, Alister W., Alpaslan, Mehmet, Andrews, Stephen K., Baldry, Ivan K., Bamford, Steven, Bland-Hawthorn, Joss, Brough, Sarah, Cluver, Michelle E., Conselice, Christopher J., Davies, Luke J. M., Haeussler, Boris, Konstantopoulos, Iraklis S., Loveday, Jon, Moffett, Amanda J., Norberg, Peder, Phillipps, Steven, Taylor, Edward N., López-Sánchez, Ángel R., Wilkins, Stephen M.·2015·Monthly Notices of the Royal Astronomical Society
DOI 10.1093/mnras/stu2467
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Abstract

We use data from the Galaxy And Mass Assembly (GAMA) survey in the redshift range 0.01 < z < 0.1 (8399 galaxies in g to K s bands) to derive the stellar mass-half-light radius relations for various divisions of 'early'-and 'late'-type samples.We find that the choice of division between early and late (i.e.colour, shape, morphology) is not particularly critical; however, the adopted mass limits and sample selections (i.e. the careful rejection of outliers and use of robust fitting methods) are important.In particular, we note that for samples extending to low stellar mass limits (<10 10 M ) the Sérsic index bimodality, evident for high-mass systems, becomes less distinct and no-longer acts as a reliable separator of earlyand late-type systems.The final set of stellar mass-half-light radius relations are reported for a variety of galaxy population subsets in 10 bands (ugrizZY JHK s ) and are intended to provide a comprehensive low-z benchmark for the many ongoing high-z studies.Exploring the variation of the stellar mass-half-light radius relations with wavelength, we confirm earlier findings that galaxies appear more compact at longer wavelengths albeit at a smaller level than previously noted: at 10 10 M both spiral systems and ellipticals show a decrease in size of 13 per cent from g to K s (which is near linear in log wavelength).Finally, we note that the sizes used in this work are derived from 2D Sérsic light profile fitting (using GALFIT3), i.e. elliptical semimajor half-light radii, improving on earlier low-z benchmarks based on circular apertures.

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Metadata

Authors
Lange, R., Driver, S. P., Robotham, A. S. G., Kelvin, L. S., Graham, A. W., Alpaslan, M., Andrews, S. K., Baldry, I. K., Bamford, S., Bland-Hawthorn, J., Brough, S., Cluver, M. E., Conselice, C. J., Davies, L. J. M., Haeussler, B., Konstantopoulos, I. S., Loveday, J., Moffett, A. J., Norberg, P., Phillipps, S., Taylor, E. N., López-Sánchez, Á. R., & Wilkins, S. M.
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2015-01-10
Volume
447
Issue
3
Pages
2603-2630
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1093/mnras/stu2467
OpenAlex
W2150586900
Cited by
294
References
71
FWCI
14.08
Type
journal article
Language
en
Open access
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CoChat. (2026). Citation check: Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology. https://app.cochat.ai/papers/10.1093/mnras/stu2467
The paper
Lange, R., Driver, S. P., Robotham, A. S. G., Kelvin, L. S., Graham, A. W., Alpaslan, M., Andrews, S. K., Baldry, I. K., Bamford, S., Bland-Hawthorn, J., Brough, S., Cluver, M. E., Conselice, C. J., Davies, L. J. M., Haeussler, B., Konstantopoulos, I. S., Loveday, J., Moffett, A. J., Norberg, P., . . . Wilkins, S. M. (2015). Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology. Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/stu2467

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.