A Universal Density Profile for Dark and Luminous Matter?

Merritt, David; Navarro, Julio F.; Ludlow, Aaron D.; Jenkins, Adrian

doi:10.1086/430636

Cited by 228 publications

(301 citation statements)

References 26 publications

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“…We consider three DM halo profiles: the cored isothermal (ISO) and the cusped NFW, defined in Sec. 4.3.2, and the Einasto profile [113]. The ratio a/g is of order unity, larger for cuspy profiles compared with the cored one.…”

Section: B the Volume Factor For Antiproton Propagation: A Diffusion mentioning

confidence: 81%

Astrophysical implications of a visible dark matter sector from a custodially warped GUT

et al. 2010

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We explore, within the warped extra dimensional framework, the possibility of finding anti-matter signals in cosmic rays (CRs) from dark matter (DM) annihilation. We find that exchange of order 100 GeV radion, an integral part of this class of models, generically results in a sizable Sommerfeld enhancement of the annihilation rate for DM mass at the TeV scale. No ad-hoc dark sector is required to obtain boosted annihilation cross sections and hence signals. Such a mild hierarchy between the radion and DM masses can be natural due to the pseudo-Goldstone boson nature of the radion. We study the implications of a Sommerfeld enhancement specifically in warped grand unified theory (GUT) models, where proton stability implies a DM candidate. We show, via partially unified Pati-Salam group, how to incorporate a custodial symmetry for Z → bb into the GUT framework such that a few TeV Kaluza-Klein (KK) mass scale is allowed by electroweak precision tests. Among such models, the one with the smallest SO(10) (fully unified) representation, with SU (5) hypercharge normalization, allows us to decouple the DM from the electroweak gauge bosons. Thus, a correct DM relic density can be obtained and direct detection bounds are satisfied.Looking at robust CR observables, we find a possible future signal in thep/p flux ratio consistent with current constraints. Using a different choice of representations, we show how to embed in this GUT model a similar custodial symmetry for the right handed tau, allowing it to be strongly coupled to KK particles.Such a scenario might lead to observed signal in CR positrons; however, the DM candidate in this case can not constitute all of the DM in the universe. As an aside and independent of GUT or DM model, the strong coupling between KK particles and tau's can lead to striking LHC signals.

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Section: B the Volume Factor For Antiproton Propagation: A Diffusion mentioning

confidence: 81%

Astrophysical implications of a visible dark matter sector from a custodially warped GUT

et al. 2010

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“…While models with a power-law behaviour at small and large radii were preferred in earlier simulations (e.g. Navarro et al 1997;Moore et al 1999), other models seem to fit the mass density distribution of more recent (and higher resolution) simulations better (Navarro et al 2004(Navarro et al , 2010Merritt et al 2005Merritt et al , 2006Graham et al 2006;Aceves et al 2006;Gao et al 2008;Duffy et al 2008;Stadel et al 2009). Among these models, the Sérsic model (i.e., a model where the projected surface density is described by a Sérsic law) has also been proposed as a universal description for simulated 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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“…The use of a single (Sérsic) model to describe the full sample of galaxies also seems advisable in light of mounting evidence that, at least in terms of their structural parameters, the long-standing perception of a fundamental dichotomy between giant and dwarf ellipticals (e.g., Kormendy 1985) may be incorrect (see, e.g., Jerjen & Binggeli 1997;Graham & Guzmán 2003;Paper VI). From a theoretical perspective, the choice of equations (1) and (4) also seems reasonable given recent findings that the Sérsic law provides an accurate representation of the spatial and surface density profiles of dark matter halos in high-resolution ÃCDM simulations (Navarro et al 2004;Merritt et al 2005).…”

Section: Parameterization Of the Surface Brightness Profilesmentioning

confidence: 99%

The ACS Virgo Cluster Survey. VIII. The Nuclei of Early‐Type Galaxies

Côté

Piatek

Ferrarese

et al. 2006

ASTROPHYS J SUPPL S

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The ACS Virgo Cluster Survey is a Hubble Space Telescope program to obtain high-resolution imaging in widely separated bandpasses ( F475W % g and F850LP % z) for 100 early-type members of the Virgo Cluster, spanning a range of %460 in blue luminosity. We use this large, homogenous data set to examine the innermost structure of these galaxies and to characterize the properties of their compact central nuclei. We present a sharp upward revision in the frequency of nucleation in early-type galaxies brighter than M B % À15 (66% P f n P 82%) and show that groundbased surveys underestimated the number of nuclei due to surface brightness selection effects, limited sensitivity and poor spatial resolution. We speculate that previously reported claims that nucleated dwarfs are more concentrated toward the center of Virgo than their nonnucleated counterparts may be an artifact of these selection effects. There is no clear evidence from the properties of the nuclei, or from the overall incidence of nucleation, for a change at M B $ À17:6, the traditional dividing point between dwarf and giant galaxies. There does, however, appear to be a fundamental transition at M B $ À20:5, in the sense that the brighter, ''core-Sérsic'' galaxies lack resolved (stellar) nuclei. A search for nuclei that may be offset from the photocenters of their host galaxies reveals only five candidates with displacements of more than 0B5, all of which are in dwarf galaxies. In each case, however, the evidence suggests that these ''nuclei'' are, in fact, globular clusters projected close to the galaxy photocenter. Working from a sample of 51 galaxies with prominent nuclei, we find a median half-light radius of hr h i ¼ 4:2 pc, with the sizes of individual nuclei ranging from 62 pc down to 2 pc (i.e., unresolved in our images) in about a half-dozen cases. Excluding these unresolved objects, the nuclei sizes are found to depend on nuclear luminosity according to the relation r h / L 0:50AE0:03 . Because the large majority of nuclei are resolved, we can rule out low-level AGNs as an explanation for the central luminosity excess in almost all cases. On average, the nuclei are %3.5 mag brighter than a typical globular cluster. Based on their broadband colors, the nuclei appear to have old to intermediate age stellar populations. The colors of the nuclei in galaxies fainter than M B % À17:6 are tightly correlated with their luminosities, and less so with the luminosities of their host galaxies, suggesting that their chemical enrichment histories were governed by local or internal factors. Comparing the nuclei to the ''nuclear clusters'' found in late-type spiral galaxies reveals a close match in terms of size, luminosity, and overall frequency. A formation mechanism that is rather insensitive to the detailed properties of the host galaxy properties is required to explain this ubiquity and homogeneity. The mean of the frequency function for the nucleus-to-galaxy luminosity ratio in our nucleated galaxies, hlog i ¼ À2:49 AE 0:09 dex ( ¼ 0:59 AE 0:10), i...

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A Universal Density Profile for Dark and Luminous Matter?

Cited by 228 publications

References 26 publications

Astrophysical implications of a visible dark matter sector from a custodially warped GUT

Astrophysical implications of a visible dark matter sector from a custodially warped GUT

Analytical expressions for the deprojected Sérsic model

The ACS Virgo Cluster Survey. VIII. The Nuclei of Early‐Type Galaxies

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