K-Band Observations of Boxy Bulges. I. Morphology and Surface Brightness Profiles

Details K-Band Observations of Boxy Bulges. I. Morphology and Surface Brightness Profiles K-Band Observations of Boxy Bulges. I. Morphology and Surface Brightness Profiles

2006-06-02

arxiv.org/abs/astro-ph/0606056v1

Mon.Not.Roy.Astron.Soc.370:753-772,2006

Astronomy and Astrophysics

Astrophysics

23 pages, 34 figures. Accepted for publication in MNRAS. A version with full resolution figures is available at http://www-a

Scientific paper

10.1111/j.1365-2966.2006.10471.x

Kn-band images, unsharp-masked images, as well as major-axis and vertically- summed surface brightness profiles are presented for 30 edge-on spiral galaxies, most with a boxy or peanut-shaped (B/PS) bulge. Such galaxies have more complex morphologies than galaxies of other bulge types, more often showing (off-)centered X structures, secondary major-axis maxima and spiral-like structures. Those features are also observed in N-body simulations of barred discs and may trace the main bar orbit families. The surface brightness profiles of galaxies with a B/PS bulge are also more complex, with typically 3 or more clearly separated regions, including a flat intermediate region (Freeman Type II profiles). Those radial breaks offer evidence for bar-driven transfer of angular momentum and radial redistribution of material. The profiles also suggest a rapid variation of the scaleheight of the disc material, contrary to conventional wisdom but again as expected from vertical resonances and instabilities in barred discs. The steep inner region of the surface brightness profiles is often shorter than the isophotally thick part of the galaxies, itself always shorter than the flat region of the profiles. Contrary to the standard `bulge + disc' model, we thus propose that galaxies with a B/PS bulge are composed of a thin concentrated disc (a disc-like bulge) contained within a partially thick bar (the B/PS bulge) and a thin outer disc. The inner disc likely formed secularly through bar-driven processes and is responsible for the steep inner region of the surface brightness profiles, while the bar is responsible for the flat region and the thick complex morphological structures observed. Those components are strongly coupled dynamically and are formed mostly of the same (disc) material. [Abridged]

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