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Rediscovering the disc origin of the Milky Way bulge

Published online by Cambridge University Press:  02 August 2018

F. Fragkoudi ,
P. Di Matteo ,
M. Haywood ,
A. Gómez ,
S. Khoperskov ,
D. Katz ,
M. Schultheis ,
F. Combes  and
B. Semelin
F. Fragkoudi
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
P. Di Matteo
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
M. Haywood
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
A. Gómez
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
S. Khoperskov
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
D. Katz
Affiliation:
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, 92195, Meudon, France
M. Schultheis
Affiliation:
Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Bd de l’Observatoire, 06304 Nice, France
F. Combes
Affiliation:
Observatoire de Paris, LERMA, CNRS, PSL Univ., UPMC, Sorbonne Univ., F-75014, Paris, France College de France, 11 Place Marcelin Berthelot, 75005, Paris, France
B. Semelin
Affiliation:
Observatoire de Paris, LERMA, CNRS, PSL Univ., UPMC, Sorbonne Univ., F-75014, Paris, France
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Abstract

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We explore morphological, kinematic and chemical trends of boxy/peanut (b/p) bulges of Milky Way (MW)-type galaxies, to better understand the formation history of the MW’s bulge. We show, using N-body simulations with both a kinematically cold and a kinematically hot disc, that colder populations develop a more prominent bar and X-shaped peanut as compared to their hotter counterpart. Colder discs also exhibit lower line-of-sight velocities (when viewed edge-on) at the edges of the b/p compared to hot discs, in agreement with what is seen for the MW bulge. Furthermore, we explore an N-body model which has three co-spatial discs with metallicities which correspond to the stellar populations of the inner Milky Way, where the α-enhanced thick disc populations are massive and centrally concentrated. The metallicity trends seen in observations of the Bulge can be reproduced in the model without the need of adding any additional components, which hints to the disc origin of the MW’s bulge.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 288 - 289
Copyright
Copyright © International Astronomical Union 2018 

References

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