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Black holes and rotation: Internal kinematics of star clusters with MUSE

Published online by Cambridge University Press:  11 March 2020

Sebastian Kamann Open the ORCID record for Sebastian Kamann [Opens in a new window]
Sebastian Kamann*
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, GB-L3 5RF, Liverpool, United Kingdom email: [email protected]
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Abstract

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Over the last decade, our abilities to observe the internal kinematics of star clusters have drastically increased. Where a few years back only small numbers of bright stars with radial velocity measurements were available, we can nowadays study the three-dimensional motions of large stellar samples, thanks to the combined datasets gathered by state-of-art spectrographs and astrometric satellites. In this work, I summarise the contribution of integral-field spectrographs, in particular MUSE, to this paradigm change. Using dedicated software tools, we were able to overcome a fundamental limitation of spectroscopy and advance to the crowded cluster centres. This allowed us to study the central kinematics in unprecedented detail and to start uncovering the populations of black holes that reside in massive star clusters.

Keywords

globular clustersbinaries: generalstars: black holesstars: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 384 - 388
Copyright
© International Astronomical Union 2020

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