Low surface brightness galaxies in the Fornax Cluster: automated galaxy surface photometry - III

Davies, Jonathan Ivor; Phillipps, Steven; Cawson, M. G. M.; Disney, M. J.; Kibblewhite, E. J.

doi:10.1093/mnras/232.2.239

Cited by 114 publications

(119 citation statements)

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“…In the recent literature, pseudo-and classical bulges have frequently been divided at the Sérsic index n 2 sph = (e.g., Sani et al 2011;Beifiori et al 2012), although, from a selection of hundreds of disk galaxies imaged in the Kband, Graham & Worley (2008) observed no bimodality in the bulge Sérsic indices about n 2 sph = or any other value. While pseudo-bulges are expected to have exponential-like surface brightness profiles (n 1 sph  ), being disky components that formed from their surrounding exponential disks (e.g., Bardeen 1975;Hohl 1975;Combes & Sanders 1981;Combes et al 1990;Pfenniger & Friedli 1991), it has been shown that mergers can create bulges with n 2 sph < (e.g., Eliche-Moral et al 2011;Scannapieco et al 2011;Querejeta et al 2015), just as low-luminosity elliptical galaxies (not built from the secular evolution of a disk) are also well known to have n 2 sph < and even n 1 sph < (e.g., Davies et al 1988;Young & Currie 1994;Jerjen et al 2000). The use of the Sérsic index (in addition to rotation) to identify pseudo-bulges is thus a dangerous practice.…”

Section: Pseudo-versus Classical Bulgesmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

130

181

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In our first paper, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, M BH , imaged at 3.6 m m with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between M BH and the host spheroid (and galaxy) luminosity, L sph (and L gal ), and also stellar mass, M .,sph * While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have M M 10 , argued by some to be pseudo-bulges, are not offset to lower M BH from the correlation defined by the current bulge sample with n 2; sph > and (3)L sph and L gal correlate equally well with M BH , in terms of intrinsic scatter, only for early-type galaxies-once reasonable numbers of spiral galaxies are included, the correlation with L sph is better than that with L gal .

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Section: Pseudo-versus Classical Bulgesmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

130

181

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“…Over the past two decades, the Sérsic model has become the standard for describing the surface brightness profiles of early-type galaxies and bulges of spiral galaxies (e.g. Davies et al 1988;Caon et al 1993;D'Onofrio et al 1994;Cellone et al 1994;Andredakis et al 1995;Prugniel & Simien 1997;Möllenhoff & Heidt 2001;Graham & Guzmán 2003;Allen et al 2006;Méndez-Abreu et al 2008;Gadotti 2009). In the past few years, Sérsic-like models have also gained popularity as a model to describe the spherically averaged profiles for dark matter haloes.…”

Section: I(r)mentioning

confidence: 99%

Analytical expressions for the deprojected Sérsic model

Baes

Gentile

2010

A&A

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The Sérsic model has become the standard for parametrizing the surface brightness distribution of early-type galaxies and bulges of spiral galaxies. A major problem is that the deprojection of the Sérsic surface brightness profile to a luminosity density cannot be executed analytically for general values of the Sérsic index. We use Mellin integral transforms to derive an analytical expressions for the luminosity density in terms of the Fox H function for all values of the Sérsic index. We derive simplified expressions for the luminosity density, cumulative luminosity, and gravitational potential in terms of the Meijer G function for all rational values of the Sérsic index, and we investigate their asymptotic behaviour at small and large radii. As implementations of the Meijer G function are currently available both in symbolic computer algebra packages and as high-performance computing code, our results open up the possibility to calculate the density of the Sérsic models to arbitrary precision.

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“…One of these is the Einasto (1965) profile, a three-dimensional version of the two-dimensional Sérsic (1968) profile used to describe the surface brightness of earlytype galaxies and the bulges of spiral galaxies (e.g. Davies et al 1988;Caon et al 1993;D'Onofrio et al 1994;Cellone et al 1994;Andredakis et al 1995;Prugniel & Simien 1997;Möllenhoff & Heidt 2001;Graham & Guzmán 2003;Graham et al 2006;Gadotti 2009). The Sérsic profile can be written as:…”

Section: Introductionmentioning

confidence: 99%

Analytical properties of Einasto dark matter haloes

Retana-Montenegro

Hese

Gentile

et al. 2012

A&A

110

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Recent high-resolution N-body CDM simulations indicate that nonsingular three-parameter models such as the Einasto profile perform better than the singular two-parameter models, e.g. the Navarro, Frenk and White, in fitting a wide range of dark matter haloes. While many of the basic properties of the Einasto profile have been discussed in previous studies, a number of analytical properties are still not investigated. In particular, a general analytical formula for the surface density, an important quantity that defines the lensing properties of a dark matter halo, is still lacking to date. To this aim, we used a Mellin integral transform formalism to derive a closed expression for the Einasto surface density and related properties in terms of the Fox H and Meijer G functions, which can be written as series expansions. This enables arbitrary-precision calculations of the surface density and the lensing properties of realistic dark matter halo models. Furthermore, we compared the Sérsic and Einasto surface mass densities and found differences between them, which implies that the lensing properties for both profiles differ.

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Low surface brightness galaxies in the Fornax Cluster: automated galaxy surface photometry - III

Cited by 114 publications

References 0 publications

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Analytical expressions for the deprojected Sérsic model

Analytical properties of Einasto dark matter haloes

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Low surface brightness galaxies in the Fornax Cluster: automated galaxy surface photometry - III

Cited by 114 publications

References 0 publications

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

Analytical expressions for the deprojected Sérsic model

Analytical properties of Einasto dark matter haloes

Contact Info

Product

Resources

About

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM