The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores

Cintio, Arianna Di; Brook, Chris; Macciò, Andrea V.; Stinson, Greg; Knebe, Alexander; Dutton, Aaron A.; Wadsley, James

doi:10.1093/mnras/stt1891

Cited by 459 publications

(554 citation statements)

References 71 publications

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“…It requires a heavy stellar disk at the limit of the range allowed by our mass maps. The presence of a dark cuspy core in M 33, as predicted by structure formation in a ΛCDM hierarchical universe, is in agreement with numerical simulation of baryonic feedback effects on the density profile of dark matter (Di Cintio et al 2014b). For our best fit halo mass, energy from stellar feedback is insufficient to significantly alter the inner dark matter density, and the galaxy retains a cuspy profile.…”

Section: Discussionsupporting

confidence: 83%

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Corbelli

Thilker

Zibetti

et al. 2014

A&A

153

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Aims. We determine the mass distribution of stars, gas, and dark matter in M 33 to test cosmological models of galaxy formation and evolution. Methods. We map the neutral atomic gas content of M 33 using high resolution Very Large Array and Green Bank Telescope observations of the 21 cm HI line emission. A tilted ring model is fitted to the HI datacube to determine the varying spatial orientation of the extended gaseous disk and the rotation curve. We derive the stellar mass surface density map of M 33's optical disk via pixel-SED fitting methods based on population synthesis models that allow for positional changes in star formation history. Stellar and gas maps are used in the dynamical analysis of the rotation curve to constrain the dark halo properties. Results. The disk of M 33 warps from 8 kpc outward without substantial change of its inclination with respect to the line of sight; the line of nodes rotates clockwise toward the direction of M 31. Rotational velocities rise steeply with radius in the inner disk, reaching 100 km s −1 in 4 kpc, then the rotation curve becomes more perturbed and flatter with velocities as high as 120-130 km s −1 out to 2.7 R 25 . The stellar surface density map highlights a star-forming disk with a varying mass-to-light ratio. At larger radii, a dynamically relevant fraction of the baryons are in gaseous form. A dark matter halo with a Navarro-Frenk-White density profile, as predicted by hierarchical clustering and structure formation in a ΛCDM cosmology, provides the best fits to the rotation curve. Dark matter is relevant at all radii in shaping the rotation curve and the most likely dark halo has a concentration C 9.5 and a total mass of 4.3(±1.0) × 10 11 M . This imples a baryonic fraction of order 0.02 and the evolutionary history of this galaxy should therefore account for loss of a large fraction of its original baryonic content.

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Section: Discussionsupporting

confidence: 83%

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Corbelli

Thilker

Zibetti

et al. 2014

A&A

153

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“…As we discussed [8], these limits are subject to large astrophysical uncertainties, and a sufficiently large, > 1 kpc, core can be invoked to reconcile the wino with experiment. However, we see that the situation is qualitatively unchanged from our earlier result, and saving the wino requires a profile in tension with current results from simulation [14][15][16].…”

Section: Jhep03(2016)213contrasting

confidence: 74%

“…We found the overall correction from resummed double logs to be modest, with a few percent reduction in the cross section at the relic density mass of 3 TeV relative to tree level (+ Sommerfeld enhancement). Thus, the factor of ∼ 15 exclusion by HESS remained, unless one invoked a profile with coring 1.5 kpc, in tension with recent simulations [14][15][16].…”

Section: Jhep03(2016)213mentioning

confidence: 81%

Semi-inclusive wino and higgsino annihilation to LL′

Baumgart¹,

Vaidya²

2016

J. High Energ. Phys.

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We systematically compute the annihilation rate for winos and higgsinos into the final state relevant for indirect detection experiments, γ + X. The radiative corrections to this process receive enhancement from the large Bloch-Nordsieck-Violating Sudakov logarithm, log(2M χ /M W ). We resum the double logs and include single logs to fixed order using a formalism that combines nonrelativistic and soft-collinear effective field theories. For the wino case, we update an earlier exclusion adapting results of the HESS experiment. At the thermal relic mass of 3 TeV, LL corrections result in a ∼30% reduction in rate relative to LL. Nonetheless, single logs do not save the wino, and it is still excluded by an order of magnitude. Experimental cuts produce an endpoint region which, our results show, significantly effects the higgsino rate at its thermal-relic mass near 1 TeV and is deserving of further study.

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“…Di Cintio et al (2014a) found that the inner dark matter density slope, α, was more strongly correlated with ǫSF, than galaxy or halo mass. At very low efficiencies, there is no change with α ≈ 1.2 as would be expected.…”

Section: Introductionmentioning

confidence: 99%

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

Dutton

Macciò

Dekel³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

118

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We use ∼ 100 cosmological galaxy formation 'zoom-in' simulations using the smoothed particle hydrodynamics code gasoline to study the effect of baryonic processes on the mass profiles of cold dark matter haloes. The haloes in our study range from dwarf (M 200 ∼ 10 10 M ⊙ ) to Milky Way (M 200 ∼ 10 12 M ⊙ ) masses. Our simulations exhibit a wide range of halo responses, primarily varying with mass, from expansion to contraction, with up to factor ∼ 10 changes in the enclosed dark matter mass at 1 per cent of the virial radius. Confirming previous studies, the halo response is correlated with the integrated efficiency of star formation:In addition, we report a new correlation with the compactness of the stellar system: ǫ R ≡ r 1/2 /R 200 . We provide an analytic formula depending on ǫ SF and ǫ R for the response of cold dark matter haloes to baryonic processes. An observationally testable prediction is that, at fixed mass, larger galaxies experience more halo expansion, while the smaller galaxies more halo contraction. This diversity of dark halo response is captured by a toy model consisting of cycles of adiabatic inflow (causing contraction) and impulsive gas outflow (causing expansion). For net outflow, or equal inflow and outflow fractions, f , the overall effect is expansion, with more expansion with larger f . For net inflow, contraction occurs for small f (large radii), while expansion occurs for large f (small radii), recovering the phenomenology seen in our simulations. These regularities in the galaxy formation process provide a step towards a fully predictive model for the structure of cold dark matter haloes.

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The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores

Cited by 459 publications

References 71 publications

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Semi-inclusive wino and higgsino annihilation to LL′

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

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