Comparison of Bar Strengths and Fractions of Bars in Active and Nonactive Galaxies

By E. Laurikainen, Heikki Salo, R. Buta. 2001

159 citations recorded by the source corpus.

Gravitational perturbation strengths and bar fractions in active and nonactive galaxies are compared using the Ohio State University Bright Galaxy Survey, which forms a statistically well defined sample of 180 disk galaxies. Bar fractions are studied using (1) the optical and near-IR classification of bars made by Eskridge and coworkers in 2002 and (2) our own bar classification based on Fourier decomposition of near-IR images (Fourier bars). The gravitational perturbation strengths are calculated using the bar torque method, taking the maximum ratio Qg of the tangential force to the mean background radial force as a measure of the nonaxisymmetric perturbation. In addition, two-dimensional bulge-disk-bar decomposition is used to study the properties of bulges of the sample galaxies. In the near-IR, Seyfert galaxies, LINERs, and H II/starburst galaxies were found to have a similar fraction, 72%, of Fourier bars (or SB-type bars), compared to 55% in the nonactive galaxies. However, if SAB-type bars are also included, practically all (95%) H II/starburst galaxies have bars. In addition, a large fraction (34%) of bars in LINERs are obscured by dust in the optical region. We find that bars in early-type galaxies are at the same time long and massive and have weak perturbation strengths. Weak perturbation strengths can be explained by dilution of the nonaxisymmetric forces by the massive bulges: for a bulge-to-disk mass ratio B/D ranging from 0 to 1, the dilution may reduce Qg from as high as 0.6 to as low as 0.1. On the other hand, bar length (relative to disk scale length) is not correlated with B/D, contrary to expectation. Seyfert- or LINER-type nuclear activity is present in most galaxies that have thin and thick planar bar components, whereas nuclear activity does not appear in those late-type galaxies that have extremely massive bars and strong perturbation strengths.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/893277fe36ef26da487aa71c1ee15213ed2cd6fc

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In Astronomy and Astrophysics

1. S. Jogee
2. J. Kormendy
3. P. Erwin
4. I. Marinova
5. S. Khochfar
6. Heikki Salo
7. E. Laurikainen
8. R. Buta

Citations in the corpus

• How Large Are the Bars in Barred Galaxies (2005, background): “More recent studies using CCDs or near-infrared images include those of Chapelon et al. (1999), Laine et al. (2002), and Laurikainen and collaborators (Laurikainen & Salo 2002; Laurikainen et al. 2002); these have, in general, supported the findings of Kormendy and EE85.”
• BULGE n AND B/T IN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS (2008, methodology): “This fraction is in excellent agreement with the H-band bar fraction of 60% reported by MJ07, based on ellipse fits of the same OSUBSGS sample, with a more conservative inclination cut (i ≤ 60◦).”
• Multicomponent decompositions for a sample of S0 galaxies (2005, methodology): “A three-component version (bulge/disc/bar) of this algorithm has been previously used in the studies by LSBV04, Laurikainen et al. (2004b) and Buta et al. (2004).”
• The EFIGI catalogue of 4458 nearby galaxies with detailed morphology (2011, background): “Another possible quantifier is bar elongation which is found to correlate strongly with bar torque in some samples (Block et al. 2001; Laurikainen et al. 2002).”
• Bars in Disk-dominated and Bulge-dominated Galaxies at z ~ 0: New Insights from ~3600 SDSS Galaxies (2007, background): “%) of bright disk galaxies are barred when observed in the near-infrared (Knapen 1999; Eskridge et al. 2000; Laurikainen et al. 2004; Menéndez-Delmestre et al. 2007; Marinova & Jogee 2007, hereafter MJ07), and a significant fraction of these ( 45”
• AINUR: Atlas of Images of NUclear Rings (2009, background): “For a givenǫb earlytype galaxies are found to have a slightly lowerQg, as found by Laurikainen et al. (2002).”
• Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, methodology): “Laurikainen et al. (2004) find a NIR bar fraction of 62% for galaxies with i < 60 .”
• Properties of Bars and Bulges in the Hubble Sequence (2007, methodology): “The decompositions for the individual galaxies discussed in this paper have been presented previously by Laurikainen, Salo & Buta (2004, 2005) and by Laurikainen et al. (2004, 2006).”
• Double-Barred Galaxies I. A Catalog of Barred Galaxies with Stellar Secondary Bars and Inner Disks (2003, methodology): “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.”