Abstract
Bars have a complex three-dimensional shape. In particular their inner part is vertically much thicker than the parts further out. Viewed edge-on, the thick part of the bar is what is commonly known as a boxy-, peanut-, or X- bulge and viewed face-on it is referred to as a barlens. These components are due to disc and bar instabilities and are composed of disc material. I review here their formation, evolution and dynamics, using simulations, orbital structure theory and comparisons to observations.
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Notes
- 1.
For certain potentials there is also the z3.1s family whose morphology resembles that of the x 1 v 4 family, but it is not related to the x 1 tree . Another potentially useful family is the x1mul2 (Patsis and Katsanikas 2014a).
- 2.
In the end-on view the galaxy is observed edge-on with the line of sight along the bar major axis.
- 3.
In the side-on view the galaxy is observed edge-on with the line of sight perpendicular to the bar major axis.
- 4.
Unsharp masking, also called median filtering, consists in replacing the value of each pixel by the difference between it and the median of all pixel values within a circular aperture centered on the pixel. This highlights sharp features.
- 5.
Peanut formation without buckling has also been found in simulations with no gas (Quillen et al. 2014).
- 6.
Since here I concentrate on the structure of the inner parts, I do not discuss outer breaks and the discs beyond them.
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Acknowledgements
I thank Albert Bosma for many stimulating discussions and the editors for inviting me to write this review. Figures 14.4 and 14.5 were made using glnemo2 (http://projets.lam.fr/-projects/glnemo2). I acknowledge financial support from the People Programme (Marie Curie Actions) of the European Union’s Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313 to the DAGAL network. I also acknowledge financial support from the CNES (Center National d’Etudes Spatiales – France) and from the “Programme National de Cosmologie et Galaxies” (PNCG) of CNRS/INSU, France, and HPC resources from GENCI- TGCC/CINES (Grants x2013047098 and x2014047098) and from the Mesocentre of Aix-Marseille Université (program DIFOMER).
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Athanassoula, E. (2016). Boxy/Peanut/X Bulges, Barlenses and the Thick Part of Galactic Bars: What Are They and How Did They Form?. In: Laurikainen, E., Peletier, R., Gadotti, D. (eds) Galactic Bulges. Astrophysics and Space Science Library, vol 418. Springer, Cham. https://doi.org/10.1007/978-3-319-19378-6_14
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