Properties of Bars and Bulges in the Hubble Sequence

By E. Laurikainen, Heikki Salo, R. Buta, Johan H. Knapen. 2007

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Properties of bars and bulges in the Hubble sequence are discussed, based on the analysis of 216 disk galaxies (S0s and spirals from NIRS0S and OSUBGS surveys, respectively). For that purpose we have collected together, and completed when necessary, the various analysis we have previously made separately for early and late types. We find strong photometric and kinematic evidence of pseudobulges in the S0-S0/a galaxies: their bulges are on average fairly exponential, inner disks are common (in 56%), and in many of the galaxies the bulges are rotationally supported. This would be difficult to understand in such gas poor galaxies as in S0s, i f these pseudobulge candidates were formed by star formation in the disk in a a similar manner as in spirals. A more likely explanation is that pseudobulges in the early-type galaxies are bar-related structures, connected to the evolution of bars, which interpretation is supported by our Fourier analysis and structural decompositions. Bars in the early-type galaxies are found to have many characteristics of evolved systems: (1) they have flat-top/double peaked Fourier amplitude profiles, (2) bars have typically sharp outer cut-offs, (3) the higher Fourier modes appear in the amplitude profiles, and (4) many bars have also ansae-type morphologies. We show the distributions of bar strength in different Hubble type bins using four bar strength indicators, Qg, A2, fbar and the bar length, which are expected to give important clues for understanding the mechanism of how bars evolve.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/95193ed861e8b406210e9fe2346a66755bf4fe87

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A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “…1979; Kent 1985; Byun & Freeman 1995; Scorza & Bender 1995; Baggett et al. 1998; GIM2D: Simard et al. 2002; GALFIT: Peng et al. 2002; BUDA: de Souza et al. 2004; Laurikainen et al. 2005, 2007; Courteau et al. 2007; GASP2D: Méndez-Abreu et al. 2008; Fisher & Drory 2008; Weinzirl et al. 2009).”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, methodology): “We take results on (v/σ) and ǫ from Laurikainen et al. (2007), Morelli et al. (2008), and MacArthur et al. (2009), and plot them in Figure 10.”
Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: a Sloan Digital Sky Survey perspective (2008, background): “…to be able to measure how relevant is the bulge component within a given galaxy in an objective and quantitative fashion, even if there is some scatter in the relation between measured bulge prominence and visually determined Hubble type (e.g. Laurikainen et al. 2007; Graham & Worley 2008).”
Photometric scaling relations of lenticular and spiral galaxies (2010, background): “However, in contrast to bars, they have lower ellipticities, b/a > 0.85 (Kormendy & Kennicutt 2004), and therefore lack significant Fourier terms higher than m = 2 (Laurikainen et al. 2007).”
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◦).”
The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, methodology): “The bars of the lenticular galaxies were found to be weaker than those in spirals, as found by Laurikainen et al. (2007) too.”
THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES (2012, background): “…photometric bulge mass of barred galaxies is less than that of non-barred disc galaxies of similar total galaxy stellar mass (Aguerri et al. 2005; Laurikainen et al. 2007; Coelho & Gadotti 2011, but see Laurikainen et al. 2010), and that the bulge-to-total flux ratio is smaller in barred…”
The black hole mass–stellar velocity dispersion correlation: bulges versus pseudo-bulges (2008, background): “…and is the characteristic ellipticity in the region interior to the radius of Vm. Bulges of different types (especially the boxy/peanut and discy bulges) often coexist in the same galaxy (Athanassoula 2005), the pseudobulges are found in all types (S0-Sm) of disk galaxies (Laurikainen et al. 2007).”
Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, background): “This can happen when using a (signalto-noise)-weighted bulge + disc fitting routine on a galaxy which has additional nuclear components and, as noted by Laurikainen et al. (2007) and Weinzirl et al. (2008), when significant bars are present.”
The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall (2008, background): “Recent work on higher quality data also suggests that the concentration differences between spirals and S0s are not as large as once claimed (Laurikainen et al. 2007; Weinzirl et al. 2008).”
Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, methodology): “This parameter was defined by Abraham & Merrifield (2000) and it is correlated with the most widely used parameter Qg, defined by Buta & Block (2001; Laurikainen et al. 2007).”
Physical properties and environments of nearby galaxies (2009, background): “At minimum they must include a general Sérsic profile bulge (they are only rarely exactly de Vaucouleurs profiles; Graham 2001; de Jong et al. 2004; Laurikainen et al. 2007).”