Integral-field kinematics and stellar populations of early-type galaxies out to three half-light radii
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We observed twelve nearby HI -detected early-type galaxies (ETGs) of stellar mass ∼ 1010 M⊙ ≤ M* ≤1011 M⊙ with the Mitchell Integral-Field Spectrograph, reaching approximately three half-light radii in most cases. We extracted line-of-sight velocity distributions for the stellar and gaseous components. We find little evidence of transitions in the stellar kinematics of the galaxies in our sample beyond the central effective radius, with centrally fast-rotating galaxies remaining fast-rotating and centrally slow-rotating galaxies likewise remaining slow-rotating. This is consistent with these galaxies having not experienced late dry major mergers; however, several of our objects have ionised gas that is misaligned with respect to their stars,suggesting some kind of past interaction. We extract Lick index measurements of the commonly-used Hβ, Fe5015, Mg, b, Fe5270 and Fe5335 absorption features, and we find most galaxies to have flat Hβ gradients and negative Mg, b gradients. We measure gradients of age, metallicity and abundance ratio for our galaxies using spectral fitting, and for the majority of our galaxies find negative age and metallicity gradients. We also find the stellar mass-to-light ratios to decrease with radius for most of the galaxies in our sample. Our results are consistent with a view in which intermediate-mass ETGs experience mostly quiet evolutionary histories, but in which many have experienced some kind of gaseous interaction in recent times.
Boardman , N F , Weijmans , A-M , van den Bosch , R , Kuntschner , H , Emsellem , E , Cappellari , M , de Zeeuw , T , Falcón-Barroso , J , Krajnovic , D , McDermid , R , Naab , T , van de Ven , G & Yildirim , A 2017 , ' Integral-field kinematics and stellar populations of early-type galaxies out to three half-light radii ' Monthly Notices of the Royal Astronomical Society , vol 471 , no. 4 , pp. 4005-4026 . DOI: 10.1093/mnras/stx1835
Monthly Notices of the Royal Astronomical Society
© 2017, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at academic.oup.com / https://doi.org/10.1093/mnras/stx1835
DescriptionFunding: STFC grant ST/K502339/1 during the course of this work (NFB), Leverhulme Trust Early Career Fellowship (AW).
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