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The Cores of Dark Matter Dominated Galaxies: theory vs. observations
Astrophysics · Submitted 19 Aug 1997
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We further show that the observed shape of the rotation curves is well matched by the density profiles of DM halos formed in very high resolution simulations of the CDM, LCDM, and CHDM models of structure formation.
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The abstract, sentence by sentence
We use the rotation curves of a sample of dark matter dominated dwarf and low-surface brightness (LSB) late-type galaxies to study their radial mass distributions. We find that the shape of the rotation curves is remarkably similar for all (both dwarf and LSB) galaxies in the sample, suggesting a self-similar density distribution of their dark matter (DM) halos. This shape can be reproduced well by a density profile with a shallow central cusp (rho(r)\propto 1/r^gamma, gamma\approx 0.2-0.4), corresponding to a steeply rising velocity curve (v(r)\propto r^g, g\approx 0.9-0.8). We further show that the observed shape of the rotation curves is well matched by the density profiles of DM halos formed in very high resolution simulations of the CDM, LCDM, and CHDM models of structure formation. This is surprising in light of several previous studies which suggested that the structure of simulated DM halos is inconsistent with the dynamics of dwarf galaxies. We discuss possible explanations for this discrepancy. We show that although the mass distribution in the hierarchically formed halos is on average consistent with the shape of rotation curves of dark matter dominated galaxies, the scatter of the individual profiles around the average is substantial and should not be neglected in comparisons with the data. Finally, we show that the DM halos in our hierarchical simulations and the real galaxies in our sample exhibit a similar decrease in their characteristic densities with increasing characteristic radial scales, and increase in their maximum rotation velocities with increasing radii at which their maximum velocity occurs. (Abridged)
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We use the rotation curves of a sample of dark matter dominated dwarf and low-surface brightness (LSB) late-type galaxies to study their radial mass distributions. | method 0.70 | 0.96 | 0.03 | asserted 0.82 |
| s1 | We find that the shape of the rotation curves is remarkably similar for all (both dwarf and LSB) galaxies in the sample, suggesting a self-similar density distribution of their dark matter (DM) halos. | result 0.94 | 0.97 | 0.38 | asserted 0.70 |
| s2 | This shape can be reproduced well by a density profile with a shallow central cusp (rho(r)\propto 1/r^gamma, gamma\approx 0.2-0.4), corresponding to a steeply rising velocity curve (v(r)\propto r^g, g\approx 0.9-0.8). | result 0.98 | 0.87 | 0.30 | asserted 0.99 |
| s3 | We further show that the observed shape of the rotation curves is well matched by the density profiles of DM halos formed in very high resolution simulations of the CDM, LCDM, and CHDM models of structure formation. | result 0.97 | 0.82 | 0.24 | asserted 1.00 |
| s4 | This is surprising in light of several previous studies which suggested that the structure of simulated DM halos is inconsistent with the dynamics of dwarf galaxies. | interpretation 0.73 | 0.26 | 0.10 | asserted 0.91 |
| s5 | We discuss possible explanations for this discrepancy. | contribution 0.45 | 0.39 | 0.03 | unclear 0.95 |
| s6 | We show that although the mass distribution in the hierarchically formed halos is on average consistent with the shape of rotation curves of dark matter dominated galaxies, the scatter of the individual profiles around the average is substantial and should not be neglected in comparisons with the data. | result 0.90 | 0.94 | 0.17 | asserted 1.00 |
| s7 | Finally, we show that the DM halos in our hierarchical simulations and the real galaxies in our sample exhibit a similar decrease in their characteristic densities with increasing characteristic radial scales, and increase in their maximum rotation velocities with increasing radii at which their maximum velocity occurs. (Abridged) | result 1.00 | 0.94 | 0.24 | asserted 1.00 |
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The paper
Original abstract
We use the rotation curves of a sample of dark matter dominated dwarf and low-surface brightness (LSB) late-type galaxies to study their radial mass distributions. We find that the shape of the rotation curves is remarkably similar for all (both dwarf and LSB) galaxies in the sample, suggesting a self-similar density distribution of their dark matter (DM) halos. This shape can be reproduced well by a density profile with a shallow central cusp (rho(r)\propto 1/r^gamma, gamma\approx 0.2-0.4), corresponding to a steeply rising velocity curve (v(r)\propto r^g, g\approx 0.9-0.8). We further show that the observed shape of the rotation curves is well matched by the density profiles of DM halos formed in very high resolution simulations of the CDM, LCDM, and CHDM models of structure formation. This is surprising in light of several previous studies which suggested that the structure of simulated DM halos is inconsistent with the dynamics of dwarf galaxies. We discuss possible explanations for this discrepancy. We show that although the mass distribution in the hierarchically formed halos is on average consistent with the shape of rotation curves of dark matter dominated galaxies, the scatter of the individual profiles around the average is substantial and should not be neglected in comparisons with the data. Finally, we show that the DM halos in our hierarchical simulations and the real galaxies in our sample exhibit a similar decrease in their characteristic densities with increasing characteristic radial scales, and increase in their maximum rotation velocities with increasing radii at which their maximum velocity occurs. (Abridged)
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References
How the literature uses it
37 arXiv papers cite this in 46 sentences
Papers whose main result relates to this one's
States a conflicting result 1 paper
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We show that the derived rotation curves comply best with cored DM density profiles, whereas the signatures of the central cusps invariably predicted by LCDM simulations are not seen.
Papers citing it · 36 sentences without a confident label
Contests it 1 paper
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At the initial time the subhalo is assumed to be spherically symmetric and has a density profile described by [ref] : [equation] To enforce that the subhalo has a finite total mass, we truncate the subhalo density profile at $r>r_vir$ following [ref] : [equation] where $c=r_vir/r_s$ is the halo concentration and [equation] We take $r_decay/r_vir=0.1$, with which the total mass of subhalo is $1.02-1.2 M_vir,sub$ depending on the parameters $(α,β,γ)$.
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Implications of Sgr A$^\ast$ on the $\gamma$-rays searches of Bino Dark Matter with $(g-2)_\mu$ · Photon spectra of Neutralino dark matter in the presence of the Milky Way’s supermassive black hole · 0.98
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Cold dark matter (CDM) can account for structures on length scales larger than $∼10$ Mpc [ref] (reviews include [ref] .) However, problems have been noted with fits to observational data on shorter length scales of $∼1-100$ kpc using early CDM simulations without baryon feedback [ref] .
Fitting a Self-Interacting Dark Matter Model to Data Ranging From Satellite Galaxies to Galaxy Clusters · Introduction · 0.80
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Commonly used profiles [ref] (see also Ref. [ref] ) can differ considerably in the inner part of the galaxy.
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