Dissipationless galaxy formation and the r1/4 law

Vanalbada, Ts

doi:10.1093/mnras/201.4.939

Cited by 359 publications

(200 citation statements)

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“…This result is of course consistent with those found in the classical literature, where reasonably strong indications are found that "clumpy" and "cold" initial conditions are fundamental for the formation of objects similar to ellipticals (e.g. van Albada 1982;May & van Albada 1984;Merritt & Aguilar 1985;Aguilar & Merritt 1990;Londrillo et al 1991).…”

Section: Discussionsupporting

confidence: 91%

“…Shier & Fischer 1998;Bender & Saglia 1999 and references therein). On the other hand, theoretical and numerical investigations on pure dissipationless collapses of stellar systems have historically beenof special interest (Polyachenko & Shukhman 1981;Hénon 1973;van Albada 1982;McGlynn 1984;Villumsen 1984;May & van Albada 1984;Merritt & Aguilar 1985;Aguilar & Merritt 1990;Londrillo et al 1991;Katz 1991;Carpintero & Muzzio 1995). In particular, the role of gravitational instabilities in a model evolving towards equilibrium is still an open field of investigation (Palmer 1994), and may be a key feature for understanding the basics of the dynamics that play a role in the formation of galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Dissipationless collapse of spherical protogalaxies and the fundamental plane

Dantas

Capelato

Carvalho

et al. 2002

A&A

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Abstract. Following on from the numerical work of Capelato et al. (1995Capelato et al. ( , 1997, where dissipationless merger simulations were shown to reproduce the "Fundamental Plane" (FP) of elliptical galaxies, we investigate whether the end products of pure, spherically symmetric, one-component dissipationless collapses could also reproduce the FP. Past numerical work on collisionless collapses have addressed important issues on the dynamical/structural characteristics of collapsed equilibrium systems. However, the study of collisionless collapse in the context of the nature of the FP has not been satisfactorily addressed yet. Our aim in this paper is to focus our attention on the resulting collapse of simple one-component spherical models with a range of different initial virial coefficients. We find that the characteristic correlations of the models are compatible with virialized, centrally homologous systems. Our results strengthen the idea that merging may be a fundamental ingredient in forming non-homologous objects.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Dissipationless collapse of spherical protogalaxies and the fundamental plane

Dantas

Capelato

Carvalho

et al. 2002

A&A

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“…Basically, it is the time-varying gravitational field during galaxy formation that leads to the equipartition of velocity among stars (why velocity instead energy is evident from the fact that mass drops out from the equations of motion, thanks to the equality of inertial and gravitational mass) [34]. Actually, numerical simulations of this process have shown that the resulting surface brightness has the form I lum ∝ R 1/4 , where R is the projected galactocentric distance, which is in very good agreement with observations (see below) [35].…”

Section: Elliptical Galaxiessupporting

confidence: 83%

Observational Evidence for Dark Matter and Dark Energy

Roncadelli¹

2016

Proceedings of XVI International Workshop on Neutrino Telescopes — PoS(NEUTEL2015)

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“…Second, the higher luminosity (core-Sérsic) elliptical galaxies have a central deficit of light rather than an excess, and are thought to be formed from dry merger events (e.g., Faber et al 1997). The violent relaxation simulations yield n ≈ 2 − 4 (e.g., van Albada 1982;McGlynn 1984) and therefore cannot account for luminous elliptical galaxies with n > ∼ 4 built from dry mergers. In addition, they do not explain how low-luminosity elliptical galaxies with n < ∼ 2 are made, nor why these galaxies follow the same L − n relation as the massive ellipticals with n > ∼ 4.…”

Section: Multi-component Model Fits For Core-sérsic Galaxiesmentioning

confidence: 99%

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

147

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New surface brightness profiles from 26 early-type galaxies with suspected partially depleted cores have been extracted from the full radial extent of Hubble Space Telescope images. We have carefully quantified the radial stellar distributions of the elliptical galaxies using the core-Sérsic model whereas for the lenticular galaxies a core-Sérsic bulge plus an exponential disc model gives the best representation. We additionally caution about the use of excessive multiple Sérsic functions for decomposing galaxies and compare with past fits in the literature. The structural parameters obtained from our fitted models are in general, in good agreement with our initial study using radially limited (R < ∼ 10 ′′ ) profiles, and are used here to update several "central" as well as "global" galaxy scaling relations. We find near-linear relations between the break radius R b and the spheroid luminosity L such that R b ∝ L 1.13±0.13 , and with the supermassive black hole mass. This is internally consistent with the notion that major, dry mergers add the stellar and black hole mass in equal proportion, i.e., M BH ∝ L. In addition, we observe a linear relation R b ∝ R 0.98±0.15 e for the core-Sérsic elliptical galaxies-where R e is the galaxies' effective half light radii-which is collectively consistent with the approximately-linear, bright-end of the curved L − R e relation. Finally, we measure accurate stellar mass deficits M def that are in general 0.5−4 M BH , and we identify two galaxies (NGC 1399, NGC 5061) that, due to their high M def /M BH ratio, may have experienced oscillatory core-passage by a (gravitational radiation)-kicked black hole. The galaxy scaling relations and stellar mass deficits favor core-Sérsic galaxy formation through a few "dry" major merger events involving supermassive black holes such that M def ∝ M 3.70±0.76 BH , for M BH > ∼ 2 × 10 8 M ⊙ .

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Dissipationless galaxy formation and the r1/4 law

Cited by 359 publications

References 0 publications

Dissipationless collapse of spherical protogalaxies and the fundamental plane

Dissipationless collapse of spherical protogalaxies and the fundamental plane

Observational Evidence for Dark Matter and Dark Energy

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

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