K-band observations of boxy bulges. I. Morphology and surface brightness profiles
Identifieur interne : 001E05 ( PascalFrancis/Curation ); précédent : 001E04; suivant : 001E06K-band observations of boxy bulges. I. Morphology and surface brightness profiles
Auteurs : M. Bureau [Royaume-Uni] ; G. Aronica [Allemagne, France] ; E. Athanassoula [France] ; R.-J. Dettmar [Allemagne] ; A. Bosma [France] ; K. C. Freeman [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006.
Descripteurs français
- Pascal (Inist)
- Morphologie, Brillance surface, Galaxies spirales, Structure spirale, Simulation numérique, Système n corps, Orbite, Transfert moment cinétique, Variation rapide, Résonance, Instabilité, Modèle, Couplage fort, Formation galaxies, Galaxies disques, Cinématique stellaire, Corrélation, Photométrie, Bulbe galaxies, Evolution galaxies, Structure galaxies.
English descriptors
- KwdEn :
- Angular momentum transfer, Correlations, Digital simulation, Disk galaxies, Fast variation, Galaxy bulge, Galaxy evolution, Galaxy formation, Galaxy structure, Instability, Models, Morphology, N body system, Orbits, Photometry, Resonance, Spiral galaxies, Spiral structure, Stellar kinematics, Strong coupling, Surface brightness.
Abstract
In this first paper of a series on the structure of boxy and peanut-shaped (B/PS) bulges, Kn-band observations of a sample of 30 edge-on spiral galaxies are described and discussed. Kn-band observations best trace the dominant luminous galactic mass and are minimally affected by dust. Images, unsharp-masked images, as well as major-axis and vertically summed surface brightness profiles are presented and discussed. Galaxies with a B/PS bulge tend to have a more complex morphology than galaxies with other bulge types, more often showing centred or off-centred X structures, secondary maxima along the major-axis and spiral-like structures. While probably not uniquely related to bars, those features are observed in three-dimensional 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, typically containing three or more clearly separated regions, including a shallow or flat intermediate region (Freeman Type II profiles). The breaks in the profiles offer evidence for bar-driven transfer of angular momentum and radial redistribution of material. The profiles further suggest a rapid variation of the scaleheight of the disc material, contrary to conventional wisdom but again as expected from the vertical resonances and instabilities present in barred discs. Interestingly, 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 intermediate region of the profiles. The steep inner region is also much more prominent along the major-axis than in the vertically summed profiles. Similarly to other recent work but contrary to the standard 'bulge + disc' model (where the bulge is both thick and steep), 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 likely formed secularly through bar-driven processes and is responsible for the steep inner region of the surface brightness profiles, traditionally associated with a classic bulge, while the bar is responsible for the flat intermediate region of the surface brightness profiles and the thick complex morphological structures observed. Those components are strongly coupled dynamically and are formed mostly of the same (disc) material, shaped by the weak but relentless action of the bar resonances. Any competing formation scenario for galaxies with a B/PS bulge, which represent at least 45 per cent of the local disc galaxy population, must explain equally well and self-consistently the above morphological and photometric properties, the complex gas and stellar kinematics observed, and the correlations between them.
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<front><div type="abstract" xml:lang="en">In this first paper of a series on the structure of boxy and peanut-shaped (B/PS) bulges, Kn-band observations of a sample of 30 edge-on spiral galaxies are described and discussed. Kn-band observations best trace the dominant luminous galactic mass and are minimally affected by dust. Images, unsharp-masked images, as well as major-axis and vertically summed surface brightness profiles are presented and discussed. Galaxies with a B/PS bulge tend to have a more complex morphology than galaxies with other bulge types, more often showing centred or off-centred X structures, secondary maxima along the major-axis and spiral-like structures. While probably not uniquely related to bars, those features are observed in three-dimensional 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, typically containing three or more clearly separated regions, including a shallow or flat intermediate region (Freeman Type II profiles). The breaks in the profiles offer evidence for bar-driven transfer of angular momentum and radial redistribution of material. The profiles further suggest a rapid variation of the scaleheight of the disc material, contrary to conventional wisdom but again as expected from the vertical resonances and instabilities present in barred discs. Interestingly, 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 intermediate region of the profiles. The steep inner region is also much more prominent along the major-axis than in the vertically summed profiles. Similarly to other recent work but contrary to the standard 'bulge + disc' model (where the bulge is both thick and steep), 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 likely formed secularly through bar-driven processes and is responsible for the steep inner region of the surface brightness profiles, traditionally associated with a classic bulge, while the bar is responsible for the flat intermediate region of the surface brightness profiles and the thick complex morphological structures observed. Those components are strongly coupled dynamically and are formed mostly of the same (disc) material, shaped by the weak but relentless action of the bar resonances. Any competing formation scenario for galaxies with a B/PS bulge, which represent at least 45 per cent of the local disc galaxy population, must explain equally well and self-consistently the above morphological and photometric properties, the complex gas and stellar kinematics observed, and the correlations between them.</div>
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<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Couplage fort</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Strong coupling</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Acoplamiento fuerte</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="3" l="FRE"><s0>Formation galaxies</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="3" l="ENG"><s0>Galaxy formation</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="3" l="FRE"><s0>Galaxies disques</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Disk galaxies</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE"><s0>Cinématique stellaire</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>Stellar kinematics</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA"><s0>Cinematica estelar</s0>
<s5>41</s5>
</fC03>
<fC03 i1="17" i2="3" l="FRE"><s0>Corrélation</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="3" l="ENG"><s0>Correlations</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="3" l="FRE"><s0>Photométrie</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="3" l="ENG"><s0>Photometry</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Bulbe galaxies</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Galaxy bulge</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="19" i2="3" l="SPA"><s0>Bulbo galaxias</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="20" i2="3" l="FRE"><s0>Evolution galaxies</s0>
<s4>CD</s4>
<s5>97</s5>
</fC03>
<fC03 i1="20" i2="3" l="ENG"><s0>Galaxy evolution</s0>
<s4>CD</s4>
<s5>97</s5>
</fC03>
<fC03 i1="20" i2="3" l="SPA"><s0>Evolución galaxias</s0>
<s4>CD</s4>
<s5>97</s5>
</fC03>
<fC03 i1="21" i2="3" l="FRE"><s0>Structure galaxies</s0>
<s4>CD</s4>
<s5>98</s5>
</fC03>
<fC03 i1="21" i2="3" l="ENG"><s0>Galaxy structure</s0>
<s4>CD</s4>
<s5>98</s5>
</fC03>
<fC03 i1="21" i2="3" l="SPA"><s0>Estructura galaxias</s0>
<s4>CD</s4>
<s5>98</s5>
</fC03>
<fN21><s1>233</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>
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