Morphology, photometry and kinematics of N‐body bars – I. Three models with different halo central concentrations

By E. Athanassoula, A. Misiriotis. 2001

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We discuss the morphology, photometry and kinematics of the bars which have formed in three N-body simulations. These have initially the same disc and the same halo-to-disc mass ratio, but their haloes have very differentcentral concentrations. The third model includes a bulge. The bar in the model with the centrally concentrated halo (model MH) is much stronger, longer and thinner than the bar in the model with the less centrally concentrated halo (model MD). Its shape, when viewed side-on, evolves from boxy to peanut and then to 'X'-shaped, as opposed to that of model MD, which stays boxy. The projected density profiles obtained from cuts along the bar major axis, for both the face-on and the edge-on views, show a flat part, as opposed to those of model MD which are falling rapidly. A Fourier analysis of the face-on density distribution of model MH shows very large m = 2, 4, 6 and 8 components. Contrary to this, for model MD the components m = 6 and 8 are negligible. The velocity field of model MH shows strong deviations from axial symmetry, and in particular has wavy isovelocities near the end of the bar when viewed along the bar minor axis. When viewed edge-on, it shows cylindrical rotation, which the MD model does not. The properties of the bar of the model with a bulge and a non-centrally concentrated halo (MDB) are intermediate between those of the bars of the other two models. All three models exhibit a lot of inflow of the disc material during their evolution, so that by the end of the simulations the disc dominates over the halo in the inner parts, even for model MH, for which the halo and disc contributions were initially comparable in that region.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

OUR MILKY WAY AS A PURE-DISK GALAXY—A CHALLENGE FOR GALAXY FORMATION (2010, background): “A rigid halo also omits dynamical friction on the bar, but the central density of the cored halo we adopt is low enough so that friction will be very mild (e.g. Debattista & Sellwood 2000; Athanassoula & Misiriotis 2002).”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “In cosmological simulations, assembly of gas-rich small galaxies at z 2 results in “classical” bulges (e.g., Kobayashi & Nakasato 2011), whereas secular evolution could produce boxy bulges (e.g., Athanassoula & Misiriotis 2002) with cylindrical rotation (as observed by Howard et al. 2009).”
AINUR: Atlas of Images of NUclear Rings (2009, background): “Unfortunately, the bar measurement proceduresvary greatly from one paper to another (discussed by Athanassoula & Misiriotis 2002).”
The structure of the Milky Way's bar outside the bulge (2015, methodology): “Our threshold for Lprof is larger than the 5% used by Athanassoula & Misiriotis (2002) which we found gave spuriously large bar lengths for the densities considered here.”
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, methodology): “In this way we avoid the bias which would have been introduced had we sorted the particles with respect to distance from the centre, as initially pointed out by Athanassoula & Misiriotis (2002).”
Double-Barred Galaxies I. A Catalog of Barred Galaxies with Stellar Secondary Bars and Inner Disks (2003, background): “Despite the common use of aǫ, there is good evidence that it is usually an underestimate of the bar’s true length (e.g., Wozniak et al., 1995; Laurikainen et al., 2002; Athanassoula & Misiriotis, 2002; Erwin & Sparke, 2003); see Fig.”
Secular Evolution and the Formation of Pseudobulges in Disk Galaxies (2004, background): “…Illingworth 1982; Jarvis 1990; Shaw, Wilkinson, & Carter 1993a; Shaw 1993a; Bettoni & Galletta 1994; Fisher, Illingworth, & Franx 1994; D’Onofrio et al. 1999; and FalcónBarroso et al. 2004 for the observations and Combes et al. 1990; Sellwood 1993a; Athanassoula & Misiriotis 2002 for simulations).”
Bar Diagnostics in Edge-On Spiral Galaxies. III. N-Body Simulations of Disks (2004, methodology): “Athanassoula & Misiriotis (2002) and Athanassoula (2002, 2003a) also clearly showed that, even for highly concentrated and/or dominant halos, luminous matter can dominate the inner parts of the models at late times.”
HOW DO DISKS SURVIVE MERGERS? (2008, background): “…studies of isolated barred galaxies (e.g. Weinberg 1985; Hernquist & Weinberg 1992b; Friedli & Benz 1993; Friedli et al. 1994; Athanassoula 2002a; Athanassoula & Misiriotis 2002; Weinberg & Katz 2007; Kaufmann et al. 2007; Foyle et al. 2008) that a long-lived bar (regardless of whether the bar…”
Secular bar formation in galaxies with a significant amount of dark matter (2002, methodology): “Note that model MH of Athanassoula & Misiriotis (2002) has a surface density profile that reproduces very well the profiles of the S0 galaxies of the Aguerri et al. (2003) sample without mentioning the evolution of the bar pattern speed.”
Image decomposition of barred galaxies and AGN hosts (2007, background): “This is a very important parameter because it is strongly related with the strength of the bar, and can provide constraints for bar models, like those of, e.g., Athanassoula & Misiriotis (2002) and secular evolution scenarios (e.g., Gadotti & dos Anjos 2001).”
ARGOS – IV. The kinematics of the Milky Way bulge (2013, background): “The former leads to model with a submaximum disk, while in the latter the disc is maximum (for a discussion on the effects of maximum and sub-maximum disks on bar growth and evolution, see Athanassoula & Misiriotis (2002).”
Mapping the three-dimensional density of the galactic bulge with VVV red clump stars (2013, result): “The resultant three dimensional density of the bulge prominently displays a boxy/peanut-like structure, qualitatively very similar to that predicted by N-body simulations of the buckling instability (e.g. Athanassoula & Misiriotis 2002; Martinez-Valpuesta et al. 2006).”
The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, methodology): “…ellipticity (Martinet & Friedli 1997; Aguerri 1999; Whyte et al. 2002; Marinova & Jogee 2007), the maximum amplitude of the m = 2 Fourier mode (Athanassoula & Misiriotis 2002; Laurikainen et al. 2005), or integrating the m = 2 Fourier mode in the bar region (Ohta et al. 1990; Aguerri et al.…”
Evolution of galactic discs: multiple patterns, radial migration, and disc outskirts (2012, background): “Earlier works have related the formation of a bar and its strength to the halo concentration (e.g., Athanassoula and Misiriotis 2002; Bournaud et al. 2005), as well as its triaxiality (Machado and Athanassoula, 2010).”