Structural properties of dwarf ellipticals and the connection with (ordinary) elliptical galaxies

Graham, Alister W.

doi:10.1017/s1743921305003960

Cited by 3 publications

(1 citation statement)

References 33 publications

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“…Graham and Guzmán (2003) find continuity in the plot of µ 0 (or µ e ) against M B : figure 5 shows that µ 0 first increases from low luminosity, then transitions smoothly near M B ∼ −20.5 to decrease with further increasing luminosity. They show that a Sérsic profile fits very well throughout the galaxy for all lower luminosity Egs; Graham (2005) presents the case that Egs form a single family in their photometric profiles. Only at higher masses must it be modified in the inner regions to avoid over-predicting SB, and Graham and Guzmán (2003) argue that more massive Egs harbour a central supermassive black-hole, which Valluri and Merritt (1998) among others have shown may make orbits near the centre chaotic, thereby lower the central stellar mass density.…”

Section: Global Scaling Parametersmentioning

confidence: 88%

Constraints on galaxy structure and evolution from the light of nearby systems

Cecil¹,

Rose

2007

Rep. Prog. Phys.

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Abstract. We review knowledge of galaxy structures obtained by their emitted light and in the local universe where they can be studied in great detail. We discuss the shapes of, and stellar motions within, galaxies, compositional clues derived from their spectra, and what luminous matter implies about their dark matter content. Implications on the current theory of hierarchical galaxy formation are explored.

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Section: Global Scaling Parametersmentioning

confidence: 88%

Constraints on galaxy structure and evolution from the light of nearby systems

Cecil¹,

Rose

2007

Rep. Prog. Phys.

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The Structure of Galaxies: II. Fitting Functions and Scaling Relations for Ellipticals

Schombert

2013

Publ. Astron. Soc. Aust.

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Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the Sérsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the Sérsic r 1/n model produces good fits to the core regions of ellipticals (r < r half ), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the Sérsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of Sérsic parameters that will equally describe the shape of the outer profile, degrading the Sérsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than M J < −23 the following structural relations are found: L Ý r 0.8±0.1 , L Ý −0.5±0.1 , and Ý r −1.5±0.1 .

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The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) Survey: Scaling Relations and the Stellar-to-total Mass Relation

Ouellette

Courteau

Holtzman

et al. 2017

ApJ

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We present parameter distributions and fundamental scaling relations for 190 Virgo cluster galaxies in the SHIVir survey. The distribution of galaxy velocities is bimodal about V circ ∼ 125 km s −1 , hinting at the existence of dynamically unstable modes in the inner regions of galaxies. An analysis of the Tully-Fisher relation (TFR) of late-type galaxies (LTGs) and fundamental plane (FP) of earlytype galaxies (ETGs) is presented, yielding a compendium of galaxy scaling relations. The slope and zero-point of the Virgo TFR match those of field galaxies, while scatter differences likely reflect distinct evolutionary histories. The velocities minimizing scatter for the TFR and FP are measured at large apertures where the baryonic fraction becomes subdominant. While TFR residuals remain independent of any galaxy parameters, FP residuals (i.e. the FP "tilt") correlate strongly with the dynamical-to-stellar mass ratio, yielding stringent galaxy formation constraints. We construct a stellar-to-total mass relation (STMR) for ETGs and LTGs and find linear but distinct trends over the range M * = 10 8−11 M . Stellar-to-halo mass relations (SHMRs), which probe the extended dark matter halo, can be scaled down to masses estimated within the optical radius, showing a tight match with the Virgo STMR at low masses; possibly inadequate halo abundance matching prescriptions and broad radial scalings complicate this comparison at all masses. While ETGs appear to be more compact than LTGs of the same stellar mass in projected space, their mass-size relations in physical space are identical. The trends reported here may soon be validated through well-resolved numerical simulations.

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Structural properties of dwarf ellipticals and the connection with (ordinary) elliptical galaxies

Cited by 3 publications

References 33 publications

Constraints on galaxy structure and evolution from the light of nearby systems

Constraints on galaxy structure and evolution from the light of nearby systems

The Structure of Galaxies: II. Fitting Functions and Scaling Relations for Ellipticals

The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) Survey: Scaling Relations and the Stellar-to-total Mass Relation

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