The cores of dwarf galaxy haloes

Navarro, Julio F.; Eke, V. R.; Frenk, Carlos S.

doi:10.1093/mnras/283.3.l72

Cited by 610 publications

(637 citation statements)

References 18 publications

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“…Dissipationless collapses in existing dark matter haloes were invoked by Nipoti et al (2006) as a possible mechanism for forming depleted cores. Another suggested alternative was the adiabatic expansion of the core region driven by the rapid mass loss from the effects of supernova and AGN feedback (Navarro et al 1996;Read & Gilmore 2005;Peirani, Kay & Silk 2008;Martizzi et al , 2013 and Krajnović et al (2013) pointed out that this scenario is compatible with the properties of "core slow rotators". In addition, Goerdt et al (2010) proposed that the energy transferred from sinking massive objects would produce cores that are as large as 3 kpc in size.…”

Section: Alternative Core Formation Scenariosmentioning

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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Section: Alternative Core Formation Scenariosmentioning

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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“…non adiabatically) transfer energy into collisionless particles, thus generating a dark matter core (see also Ogiya & Mori 2014 for a detailed analysis of the effect of resonances between DM particles and the density wave excited by the oscillating potential). These strong gas outflows are triggered by stellar (and AGN) feedback (Navarro, Eke & Frenk 1996;Read & Gilmore 2005;Mashehenko, Couchman & Wadsley 2006;Pontzen & Governato 2014;Martizzi et al 2013).…”

Section: Introductionmentioning

confidence: 99%

NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time

Tollet

Macciò

Dutton

et al. 2016

Mon. Not. R. Astron. Soc.

276

349

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We use the NIHAO (Numerical Investigation of Hundred Astrophysical Objects) cosmological simulations to investigate the effects of baryonic physics on the time evolution of Dark Matter central density profiles. The sample is made of ≈ 70 independent high resolution hydrodynamical simulations of galaxy formation and covers a wide mass range:, from dwarfs to L ⋆ . We confirm previous results on the dependence of the inner dark matter density slope, α, on the ratio between stellar-to-halo mass, M star /M halo . We show that this relation holds approximately at all redshifts (with an intrinsic scatter of ∼ 0.18 in α measured between 1 − 2% of the virial radius). This implies that in practically all haloes the shape of their inner density profile changes quite substantially over cosmic time, as they grow in stellar and total mass. Thus, depending on their final M star /M halo ratio, haloes can either form and keep a substantial density core (R core ∼ 1 kpc), or form and then destroy the core and re-contract the halo, going back to a cuspy profile, which is even steeper than CDM predictions for massive galaxies (10 12 M ⊙ ). We show that results from the NIHAO suite are in good agreement with recent observational measurements of α in dwarf galaxies. Overall our results suggest that the notion of a universal density profile for dark matter haloes is no longer valid in the presence of galaxy formation.

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“…Stellar feedback could produce rapid variations of the gravitational potential through substantial gas mass outflows from the central region. This would flatten the inner density profile of the dark matter halo (Navarro et al 1996b;Gnedin & Zhao 2002;Read & Gilmore 2005;Mashchenko et al 2006Mashchenko et al , 2008Ogiya & Mori 2011, 2014Governato et al 2012;Macciò et al 2012;Teyssier et al 2013;Oñorbe et al 2015;Chan et al 2015;El-Zant et al 2016;Del Popolo & Pace 2016). On the other hand, dark matter can also be gravitationally "heated" by baryons through dynamical friction caused either by selfgravitating gas clouds orbiting near the center of the galaxy (El-Zant et al 2001, El-Zant et al 2004Jardel & Sellwood 2009;Lackner & Ostriker 2010;Cole et al 2011, Del Popolo & Pace 2016 by the presence of a stellar bar (Weinberg & Katz 2002;Holley-Bockelmann et al 2005;Sellwood 2008), by the radiation recoil from coalescing black holes (Merritt et al 2004), or by processes which transfer of angular momentum from baryonic to dark matter (Tonini et al 2006, Del Popolo 2009, 2012, 2014.…”

Section: Introductionmentioning

confidence: 99%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

143

141

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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The cores of dwarf galaxy haloes

Cited by 610 publications

References 18 publications

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

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

NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

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