The Tully-Fisher relation for S0 galaxies

Monthly Notices of the Royal Astronomical Society (Impact Factor: 5.11). 09/2006; 373(3). DOI: 10.1111/j.1365-2966.2006.11031.x
Source: arXiv


We present a study of the local B- and Ks-band Tully–Fisher relation (TFR) between absolute magnitude and maximum circular speed in S0 galaxies. To make this study, we have combined kinematic data, including a new high-quality spectral data set from the Fornax cluster, with homogeneous photometry from the Third Reference Catalogue of Bright Galaxies and Two Micron All Sky Survey catalogues, to construct the largest sample of S0 galaxies ever used in a study of the TFR. Independent of environment, S0 galaxies are found to lie systematically below the TFR for nearby spirals in both optical and infrared bands. This offset can be crudely interpreted as arising from the luminosity evolution of spiral galaxies that have faded since ceasing star formation.
However, we also find a large scatter in the TFR. We show that most of this scatter is intrinsic, not due to the observational uncertainties. The presence of such a large scatter means that the population of S0 galaxies cannot have formed exclusively by the above simple fading mechanism after all transforming at a single epoch. To better understand the complexity of the transformation mechanism, we have searched for correlations between the offset from the TFR and other properties of the galaxies such as their structural properties, central velocity dispersions and ages (as estimated from line indices). For the Fornax cluster data, the offset from the TFR correlates with the estimated age of the stars in the individual galaxies, in the sense and of the magnitude expected if S0 galaxies had passively faded since being converted from spirals. This correlation implies that a significant part of the scatter in the TFR arises from the different times at which galaxies began their transformation.

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    ABSTRACT: Spectroscopic observations of three lenticular (S0) galaxies (NGC 1167, NGC 4150, and NGC 6340) and one SBa galaxy (NGC 2273) have been taken with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences aimed to study the structure and kinematic properties of early-type disk galaxies. The radial profiles of the stellar radial velocities and the velocity dispersion are measured. N-body simulations are used to construct dynamical models of galaxies containing a stellar disk, bulge, and halo. The masses of individual components are estimated formaximum-mass disk models. A comparison of models with estimated rotational velocities and the stellar velocity dispersion suggests that the stellar disks in lenticular galaxies are “overheated”; i.e., there is a significant excess velocity dispersion over the minimum level required to maintain the stability of the disk. This supports the hypothesis that the stellar disks of S0 galaxies were subject to strong gravitational perturbations. The relative thickness of the stellar disks in the S0 galaxies considered substantially exceed the typical disk thickness of spiral galaxies. PACS numbers98.52.Lp–98.52.Nr–98.62.Ck–98.62.Dm–98.62.Hr
    Full-text · Article · Feb 2011 · Astronomy Reports
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    ABSTRACT: The Tully-Fisher Relation (TFR) links two fundamental properties of disk galaxies: their luminosity and their rotation velocity (mass). The pioneering work of Vogt et al. in the 1990's showed that it is possible to study the TFR for spiral galaxies at considerable look-back-times, and use it as a powerful probe of their evolution. In recent years, several groups have studied the TFR for galaxies in different environments reaching redshifts beyond one. In this brief review I summarise the main results of some of these studies and their consequences for our understanding of the formation and evolution of disk galaxies. Particular emphasis is placed on the possible environment-driven differences in the behaviour of the TFR for field and cluster galaxies.
    Preview · Article · Nov 2006 · Proceedings of the International Astronomical Union
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    ABSTRACT: We explore the dependence of the ratio of a galaxy's maximum circular velocity, Vc, to its central velocity dispersion, sigma0, on morphology or, equivalently, total light concentration. Such a dependence is expected if light traces the mass. Over the full range of galaxy types, masses, and brightnesses, and assuming that the gas velocity traces the circular velocity, we find that galaxies obey the relation log(Vc/sigma0)=0.63-0.11C28, where C28=5log(r80/r20) and the radii are measured at 80% and 20% of the total light. Massive galaxies scatter about the Vc=sqrt(2)sigma0 line for isothermal stellar systems. For pure disks, C28~2.8 and Vc~=2sigma0. Self-consistent equilibrium galaxy models from Widrow & Dubinski constrained to match the size-luminosity and velocity-luminosity relations of disk galaxies fail to match the observed Vc/sigma0 distribution. Furthermore, the matching of dynamical models for Vc(r)/sigma(r) with observations of dwarf and elliptical galaxies suffers from limited radial coverage and relatively large error bars; for dwarf systems, however, kinematical measurements at the galaxy center and optical edge suggest Vc(Rmax)>~2sigma0 [in contrast with past assumptions that Vc(Rmax)=sqrt(2)sigma0 for dwarfs]. The Vc-sigma0-C28 relation has direct implications for galaxy formation and dynamical models, galaxy scaling relations, the mass function of galaxies, and the links between the formation and evolution processes of a galaxy's central massive object, bulge, and dark matter halo.
    Preview · Article · Jan 2007 · The Astrophysical Journal
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