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Stellar angular momentum distribution linked to galaxy morphology

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Burkert,  Andreas
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Citation

Sweet, S. M., Glazebrook, K., Obreschkow, D., Fisher, D. B., Burkert, A., Lagos, C. D. P., et al. (2020). Stellar angular momentum distribution linked to galaxy morphology. Monthly Notices of the Royal Astronomical Society, 494(4), 5421-5438. doi:10.1093/mnras/staa1050.


Cite as: http://hdl.handle.net/21.11116/0000-0006-ED16-7
Abstract
We study the spatially resolved stellar specific angular momentum j* in a high-quality sample of 24 Calar Alto Legacy Integral Field Area galaxies covering a broad range of visual morphology, accounting for stellar velocity and velocity dispersion. The shape of the spaxelwise probability density function of normalized s = j*/j*mean, PDF(s), deviates significantly from the near-universal initial distribution expected of baryons in a dark matter halo and can be explained by the expected baryonic effects in galaxy formation that remove and redistribute angular momentum. Further we find that the observed shape of the PDF(s) correlates significantly with photometric morphology, where late-type galaxies have a PDF(s) that is similar to a normal distribution, whereas early types have a strongly skewed PDF(s) resulting from an excess of low-angular momentum material. Galaxies that are known to host pseudo-bulges (bulge Sérsic index nb < 2.2) tend to have less skewed bulge PDF(s), with skewness (b1rb) ≲ 0.8. The PDF(s) encodes both kinematic and photometric information and appears to be a robust tracer of morphology. Its use is motivated by the desire to move away from traditional component-based classifications which are subject to observer bias, to classification on a galaxy’s fundamental (stellar mass and angular momentum) properties. In future, PDF(s) may also be useful as a kinematic decomposition tool.