On the shape of the light profiles of early-type galaxies

Caon, N.; Capaccioli, M.; D’Onofrio, M.

doi:10.1093/mnras/265.4.1013

Cited by 661 publications

(1,005 citation statements)

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“…where μ e is the surface brightness at the effective radius R e that encloses half of the total light from the model [43,44]. The constant b n is defined in terms of the parameter n, which described the overall shape of the light profile.…”

Section: The Baryonic Contributionmentioning

confidence: 99%

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

Seigar

2011

ISRN Astronomy and Astrophysics

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We investigate the dark matter halo density profile of M33. We find that the HÁ rotation curve of M33 is best described by an NFW dark matter halo density profile model, with a halo concentration of c vir = 4.0±1.0 and a virial mass of M vir = (2.2±0.1)×10 11 M . We go on to use the NFW concentration (c vir ) of M33, along with the values derived for other galaxies (as found in the literature), to show that c vir correlates with both spiral arm pitch angle and supermassive black hole mass.

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Section: The Baryonic Contributionmentioning

confidence: 99%

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

Seigar

2011

ISRN Astronomy and Astrophysics

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“…with c n = 2.5(0.868n − 0.142) (valid for 0.5 < n < 16.5; Caon et al 1993). The fit was made from that particular radius, chosen by eye, where the, sometimes visible, inner plateau, will not disturb the fit.…”

Section: Global Parametersmentioning

confidence: 99%

HST/ACS observations of shell galaxies: inner shells, shell colours and dust

Sikkema

Carter²,

Peletier

et al. 2007

A&A

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Context. Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence for a merger event. Accurate photometry at high spatial resolution is needed to learn on presence of inner shells, population properties of shells, and dust in shell galaxies. Aims. Learn more about the origin of shells and dust in early type galaxies. Methods. V − I colours of shells and underlying galaxies are derived, using HST Advanced Camera for Surveys (ACS) data. A galaxy model is made locally in wedges and subtracted to determine shell profiles and colours. We applied Voronoi binning to our data to get smoothed colour maps of the galaxies. Comparison with N-body simulations from the literature gives more insight to the origin of the shell features. Shell positions and dust characteristics are inferred from model galaxy subtracted images. Results. The ACS images reveal shells well within the effective radius in some galaxies (at 0.24 r e = 1.7 kpc in the case of NGC 5982). In some cases, strong nuclear dust patches prevent detection of inner shells. Most shells have colours which are similar to the underlying galaxy. Some inner shells are redder than the galaxy. All six shell galaxies show out of dynamical equilibrium dust features, like lanes or patches, in their central regions. Our detection rate for dust in the shell ellipticals is greater than that found from HST archive data for a sample of normal early-type galaxies, at the 95% confidence level.Conclusions. The merger model describes better the shell distributions and morphologies than the interaction model. Red shell colours are most likely due to the presence of dust and/or older stellar populations. The high prevalence and out of dynamical equilibrium morphologies of the central dust features point towards external influences being responsible for visible dust features in early type shell galaxies. Inner shells are able to manifest themselves in relatively old shell systems.

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“…This seemed a sensible approach a few decades ago, when the technique was used to quantify the sizes of elliptical galaxies, which were thought to be all well described by homologous R 1/4 de Vaucouleurs (1948) surface-brightness profiles. But we now know that ETGs are best represented by Sersic (1968) profiles, with concentration that systematically increases with galaxy mass (Caon et al 1993). Moreover the ATLAS 3D volume-limited (M > 6×10 9 M ) survey of nearby ETGs (Cappellari et al 2011a) has revealed that the majority of the systems are more closely related to spiral galaxies than to genuine spheroidal ellipticals (Cappellari et al 2011b).…”

Section: Uncertainties Of Galaxy Sizesmentioning

confidence: 99%

Dynamical masses of early-type galaxies at z ~ 2

Cappellari¹

2012

Proc. IAU

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Abstract. The evolution of masses and sizes of passive (early-type) galaxies with redshift provides ideal constraints to galaxy formation models. These parameters can in principle be obtained for large galaxy samples from multi-band photometry alone. However the accuracy of photometric masses is limited by the non-universality of the IMF. Galaxy sizes can be biased at high redshift due to the inferior quality of the imaging data. Both problems can be avoided using galaxy dynamics, and in particular by measuring the galaxies stellar velocity dispersion. Here we provide an overview of the efforts in this direction.

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On the shape of the light profiles of early-type galaxies

Cited by 661 publications

References 0 publications

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

HST/ACS observations of shell galaxies: inner shells, shell colours and dust

Dynamical masses of early-type galaxies at z ~ 2

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