Dark Matter Substructure within Galactic Halos

Moore, Ben; Ghigna, Sebastiano; Governato, Fabio; Lake, George; Quinn, Thomas; Stadel, Joachim; Tozzi, P.

doi:10.1086/312287

Cited by 2,909 publications

(3,220 citation statements)

References 37 publications

(53 reference statements)

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“…ρ(r) ∼ r −α int , where α int is close to unity. To this respect a number of discrepancies have been found α int < 1 (e.g., Subramanian et al, 2000;Taylor and Navarro, 2001;Ricotti, 2003), and α int = 1.5 (e.g., Fukushige andMakino, 1997, 2001;Moore et al, 1998Moore et al, , 1999. On the other hand, Hayashi et al (2004); Navarro et al (2004);Power et al (2003), concluded, by using a suite of high resolution simulations, that α int = 1 remains consistent with simulated halo shapes (they found mean values α int = [1.1;1.2;1.35] respectively), while they claim that cusps as steep as α int = 1.5 are ruled out (Spekkens et al, 2005).…”

Section: The Cusp/core Problemmentioning

confidence: 99%

Toward understanding the origin of the fundamental plane for early-type galaxies

D’Onofrio

Valentinuzzi

Secco

et al. 2006

New Astronomy Reviews

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We present a panoramic review of several observational and theoretical aspects of the modern astrophysical research about the origin of the Fundamental Plane (FP) relation for Early-Type Galaxies (ETGs). The discussion is focused on the problem of the tilt and the tightness of the FP, and on the attempts to derive the luminosity evolution of ETGs with redshift. Finally, a number of observed features in the FP are interpreted from the standpoint of a new theoretical approach based on the two-component tensor virial theorem.

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Section: The Cusp/core Problemmentioning

confidence: 99%

Toward understanding the origin of the fundamental plane for early-type galaxies

D’Onofrio

Valentinuzzi

Secco

et al. 2006

New Astronomy Reviews

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“…Moore et al (1999) argue that the number of dark matter subhalos is 10 − 100 times larger than the number of satellites observed around the Milky Way (Kravtsov 2010). The so-called "missing satellite problem" has been revisited in a somewhat quantitative context (Boylan-Kolchin et al 2011;Lovell et al 2012;Boylan-Kolchin et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

Kamada

Yoshida

Kohri

et al. 2013

J. Cosmol. Astropart. Phys.

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We study the formation of non-linear structures in Warm Dark Matter (WDM) models and in a Long-Lived Charged Massive Particle (CHAMP) model. CHAMPs with a decay lifetime of about 1 yr induce characteristic suppression in the matter power spectrum at subgalactic scales through acoustic oscillations in the thermal background. We explore structure formation in such a model. We also study three WDM models, where the dark matter particles are produced through the following mechanisms: i) WDM particles are produced in the thermal background and then kinematically decoupled; ii) WDM particles are fermions produced by the decay of thermal heavy bosons; and iii) WDM particles are produced by the decay of non-relativistic heavy particles. We show that the linear matter power spectra for the three models are all characterised by the comoving Jeans scale at the matter-radiation equality. Furthermore, we can also describe the linear matter power spectrum for the Long-Lived CHAMP model in terms of a suitably defined characteristic cut-off scale k Ch , similarly to the WDM models. We perform large cosmological N -body simulations to study the non-linear growth of structures in these four models. We compare the halo mass functions, the subhalo mass functions, and the radial distributions of subhalos in simulated Milky Way-size halos. For the characteristic cut-off scale k cut = 51 h Mpc −1 , the subhalo abundance -2 -(∼ 10 9 M sun ) is suppressed by a factor of ∼ 10 compared with the standard ΛCDM model. We then study the models with k cut ≃ 51, 410, 820 h Mpc −1 , and confirm that the halo and the subhalo abundances and the radial distributions of subhalos are indeed similar between the different WDM models and the Long-Lived CHAMP model. The result suggests that the cut-off scale k cut not only characterises the linear power spectra but also can be used to predict the non-linear clustering properties. The radial distribution of subhalos in Milky Way-size halos is consistent with the observed distribution for k cut ∼ 50 − 800 h Mpc −1 ; such models resolve the so-called "missing satellite problem".

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“…Alternative DM scenarios have been proposed in response to the discrepancy between observations and CDM numerical simulations on small scales (which notably predict cuspy haloes [6]). The most "robust" one, the Warm Dark Matter scenario (WDM), involves non-annihilating particles and a very narrow range for the DM mass [7], obtained by requiring that the freestreaming length be of the order of the smallest primordial scale one wants to be compatible with.…”

Section: Introductionmentioning

confidence: 99%