ar X iv : a st ro - p h / 05 08 61 6 v 1 2 9 A ug 2 00 5 THREE - DIMENSIONAL BAR STRUCTURE AND DISC / BULGE SECULAR EVOLUTION

Kn-band imaging of a sample of 30 edge-on spiral galaxies with a boxy or peanut-shaped (B/PS) bulge is discussed. Galaxies with a B/PS bulge tend to have a more complex morphology than galaxies with other bulge types, unsharp-masked images revealing structures that trace the major orbit families of three-dimensional bars. Their surface brightness profiles are also more complex, typically containing 3 or more clearly separated regions, including a shallow or flat intermediate region (Free-man Type II profiles), suggestive of bar-driven transfer of angular momentum and radial redistribution of material. The data also suggest abrupt variations of the discs' scaleheights, as expected from the vertical resonances and instabilities present in barred discs but contrary to conventional wisdom. Counter 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), itself contained within a thin outer disc. The inner disc most likely formed through bar-driven processes while the thick bar arises from buckling instabilities. Both are strongly coupled dynamically and are formed mostly of the same (disc) material. 1. Introduction Bulges are traditionally viewed as low-luminosity elliptical galaxies, suggesting a rapid formation dominated either by mergers/accretion (e.g. Searle & Zinn 1978) or possibly by dissipative gravitational collapse (e.g. Eggen et al. 1962). Those ideas have come under increasing criticism, however, and competing models where bulges grow secularly (i.e. over a long timescale and in relative isolation) are now widely discussed, many of them bar-driven (e.