4.7 Article

Peanuts at an angle: detecting and measuring the three-dimensional structure of bars in moderately inclined galaxies

Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 431, Issue 4, Pages 3060-3086

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt385

Keywords

galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: spiral; galaxies: structure

Funding

  1. Deutsche Forschungsgemeinschaft through Priority Programme 1177 'Galaxy Evolution'
  2. STFC Consolidated grant [ST/J001341/1]
  3. Alfred P. Sloan Foundation
  4. National Aeronautics and Space Administration
  5. National Science Foundation
  6. U.S. Department of Energy
  7. Japanese Monbukagakusho
  8. Max Planck Society
  9. Science and Technology Facilities Council [ST/J001341/1] Funding Source: researchfish
  10. STFC [ST/J001341/1] Funding Source: UKRI

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We show that direct detection and measurement of the vertically thickened parts of bars (so-called 'boxy' or 'peanut-shaped' bulges) are possible not only for edge-on galaxies but also for galaxies with moderate inclinations (i < 70 degrees), and that examples are relatively common in the nearby Universe. The analysis of a sample of 78 nearby, moderately inclined (i less than or similar to 65 degrees) early-type (S0-Sb) barred galaxies shows that the isophotal signature of the box/peanut can usually be detected for inclinations as low as i similar to 40 degrees - and in exceptional cases down to i similar to 30 degrees. In agreement with the predictions from N-body simulations, the signature is most easily detectable when the bar's position angle is within similar to 50 degrees of the galaxy major axis; in particular, galaxies where the bar lies very close to the minor axis do not show the signature clearly or at all. For galaxies with i = 40 degrees-65 degrees and relative angles < 45 degrees, we find evidence for the signature approximate to 2/3 of the time; the true frequency of box/peanut structures in bars may be higher. Comparison with N-body models also allows us to link observed photometric morphology with 3D physical structures, and thus estimate the relative sizes of box/peanut structures and bars. For our local sample, we find that box/peanut structures range in radial size (measured along the bar major axis) from 0.4 to 3.8 kpc (mean = 1.5 +/- 0.9 kpc) and span 0.26-0.58 of the bar length (mean of 0.38 +/- 0.08). This is a clear observational confirmation that when bars thicken, it is not the entire bar which does so, but only the inner part. This technique can also be used to identify galaxies with bars which have not vertically thickened. We suggest that NGC 3049 and IC 676 may be particularly good examples, and that the fraction of S0-Sb bars which lack box/peanut structures is at least similar to 13 per cent.

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