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Spotting a counter-rotating galaxy

Published online by Cambridge University Press:  14 May 2020

Michela Rubino Open the ORCID record for Michela Rubino [Opens in a new window] ,
Alessandro Pizzella  and
Lorenzo Morelli
Michela Rubino
Affiliation:
Dipartimento di Fisica e Astronomia “G. Galilei”, Università degli Studi di Padova, vicolo dell’Osservatorio 3, I-35122, Padova, Italy
Alessandro Pizzella
Affiliation:
INAF-Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy
Lorenzo Morelli
Affiliation:
Instituto de Astronomia y Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiapó, Chile email: [email protected]
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Abstract

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The presence of counter-rotating (CR) components in galaxies is not that rare but their origin is still unclear. Important clues to the formation and evolution of CR galaxies are provided by galaxy kinematics, such as the mass distribution and the shape of the gravitational potential. In order to better understand the origin and incidence of CR galaxies, we aim at modeling CR stellar disks, as they would be observed with Integral Field Units (IFU) instruments, and measuring the kinematics of these peculiar astrophysical objects to reveal the CR signatures. In the bi-dimensional maps of analysed models, the double sigma signature is the best diagnostic to spot the presence of a CR disk component.

Keywords

Galaxy: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 231 - 232
Copyright
© International Astronomical Union 2020

References

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