The Rotation Velocity Attributable to Dark Matter at Intermediate Radii in Disk Galaxies

McGaugh, Stacy S.; Blok, W. J. G. de; Schombert, James M.; Naray, Rachel Kuzio de; Kim, Ji Hoon

doi:10.1086/511807

Cited by 103 publications

(148 citation statements)

References 144 publications

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“…This implies a dark matter halo consistent with the near-universal halo found by McGaugh et al (2007) and Walker et al (2010). Unfortunately, this empirical dark matter halo is not consistent with ΛCDM (McGaugh et al 2007), though presumably it can be accommodated by invoking feedback or some other mechanism.…”

Section: Ret II Hor I and Hyd Iimentioning

confidence: 71%

“…This is done with the scaling relations of McGaugh et al (2007) and Walker et al (2009), the results of which are tabulated in Table 5. Walker et al (2010) showed that the distinct relations of McGaugh et al (2007) and Walker σ Newton : Predicted velocity dispersion assuming M/L = 2 and that the objects are dark-matter-free.…”

Section: Scaling Relationsmentioning

confidence: 99%

“…The results depend strongly on which dynamical model (Newtonian dynamics or Modified Newtonian Dynamics, MOND, Milgrom 1983) or which dark matter halo scaling relation is assumed (McGaugh et al 2007;Walker et al 2009). We will provide predictions for all these different cases.…”

Section: Introductionmentioning

confidence: 99%

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The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

Pawlowski

McGaugh

Jerjen

2015

Mon. Not. R. Astron. Soc.

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The evidence that stellar systems surrounding the Milky Way (MW) are distributed in a Vast Polar Structure (VPOS) may be observationally biased by satellites detected in surveys of the northern sky. The recent discoveries of more than a dozen new systems in the southern hemisphere thus constitute a critical test of the VPOS phenomenon. We report that the new objects are located close to the original VPOS, with half of the sample having offsets less than 20 kpc. The positions of the new satellite galaxy candidates are so well aligned that the orientation of the revised best-fitting VPOS structure is preserved to within 9 degrees and the VPOS flattening is almost unchanged (31 kpc height). Interestingly, the shortest distance of the VPOS plane from the MW center is now only 2.5 kpc, indicating that the new discoveries balance out the VPOS at the Galactic center. The vast majority of the MW satellites are thus consistent with sharing a similar orbital plane as the Magellanic Clouds, confirming a hypothesis proposed by Kunkel & Demers and Lynden-Bell almost 40 years ago. We predict the absolute proper motions of the new objects assuming they orbit within the VPOS. Independent of the VPOS results we also predict the velocity dispersions of the new systems under three distinct assumptions: that they (i) are dark-matter-free star clusters obeying Newtonian dynamics, (ii) are dwarf satellites lying on empirical scaling relations of galaxies in dark matter halos, and (iii) obey MOND.

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Section: Ret II Hor I and Hyd Iimentioning

confidence: 71%

Section: Scaling Relationsmentioning

confidence: 99%

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The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

Pawlowski

McGaugh

Jerjen

2015

Mon. Not. R. Astron. Soc.

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“…It has already been conclusively demonstrated that spiral galaxy rotation curves are well recovered in MOND purely by the baryon distribution without any parameter adjustments (Sanders & McGaugh 2002;McGaugh 2004McGaugh , 2005aSanders & Noordermeer 2007), and MOG is reported to also do well on this account (Brownstein & Moffat 2006). In contrast, the DM approach can only poorly reproduce the vast variety of rotation curves, and cannot explain the amazing regularities found in them (McGaugh 2004;McGaugh et al 2007;Gentile et al 2009;Milgrom 2009a). Notably, the realisation (Gentile et al 2009;Milgrom 2009a) that the ratio of DM mass to baryonic mass within the DM core radius is constant despite the large variation in the DMto-baryonic-matter ratio globally within galaxies cannot be understood within the DM hypothesis.…”

Section: Non-newtonian Weak-field Gravitymentioning

confidence: 99%

Local-Group tests of dark-matter concordance cosmology

Kroupa

Famaey

Boer

et al. 2010

A&A

221

298

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Predictions of the concordance cosmological model (CCM) of the structures in the environment of large spiral galaxies are compared with observed properties of Local Group galaxies. Five new, most probably irreconcilable problems are uncovered: 1) A wide variety of published CCM models consistently predict some form of relation between dark-matter-mass and luminosity for the Milky Way (MW) satellite galaxies, but none is observed.2) The mass function of luminous sub-haloes predicted by the CCM contains too few satellites with dark matter (DM) mass ≈10 7 M within their innermost 300 pc than in the case of the MW satellites.3) The Local Group galaxies and data from extragalactic surveys indicate there is a correlation between bulge-mass and the number of luminous satellites that is not predicted by the CCM. 4) The 13 new ultra-faint MW satellites define a disc-of-satellites (DoS) that is virtually identical to the DoS previously found for the 11 classical MW satellites, implying that most of the 24 MW satellites are correlated in phase-space. 5) The occurrence of two MW-type DM halo masses hosting MW-like galaxies is unlikely in the CCM. However, the properties of the Local Group galaxies provide information leading to a solution of the above problems. The DoS and bulge-satellite correlation suggest that dissipational events forming bulges are related to the processes forming phase-space correlated satellite populations. These events are well known to occur since in galaxy encounters energy and angular momentum are expelled in the form of tidal tails, which can fragment to form populations of tidal-dwarf galaxies (TDGs) and associated star clusters. If Local Group satellite galaxies are to be interpreted as TDGs then the substructure predictions of the CCM are internally in conflict. All findings thus suggest that the CCM does not account for the Local Group observations and that therefore existing as well as new viable alternatives have to be further explored. These are discussed and natural solutions for the above problems emerge.

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“…The Cuspy Halo Problem refers to the discrepancy between the galactic dark matter halo density profiles predicted by ΛCDM galaxy formation simulations and the density profiles inferred from galactic rotation curves [29,30]. Galaxies are believed to form through a process of hierarchical clustering [31], in which large galaxies are formed via mergers of many smaller objects, with the initial density fluctuations arising during the Big Bang.…”

Section: The Cuspy Halo Problemmentioning

confidence: 99%

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

McCarthy¹

2013

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Astrophysical and cosmological measurements on the scales of galaxies, galaxy clusters, and the universe indicate that ∼85% of the matter in the universe is composed of dark matter, made up of non-baryonic particles that interact with cross-sections on the weak scale or lower. Hypothetical Weakly Interacting Massive Particles, or WIMPs, represent a potential solution to the dark matter problem, and naturally arise in certain Standard Model extensions.The Cryogenic Dark Matter Search (CDMS) collaboration aims to detect the scattering of WIMP particles from nuclei in terrestrial detectors. Germanium and silicon particle detectors are deployed in the Soudan Underground Laboratory in Minnesota. These detectors are instrumented with phonon and ionization sensors, which allows for discrimination against electromagnetic backgrounds, which strike the detector at rates orders of magnitude higher than the expected WIMP signal.This dissertation presents the development of numerical models of the physics of the CDMS detectors, implemented in a computational package collectively known as the CDMS Detector Monte Carlo (DMC). After substantial validation of the models against data, the DMC is used to investigate potential backgrounds to the next iteration of the CDMS experiment, known as SuperCDMS. Finally, an investigation of using the DMC in a reverse Monte Carlo analysis of WIMP search data is presented.140.23 kg-days of WIMP search data from the silicon detectors in the CDMSII experiment is also analyzed. The resulting upper limits on the WIMP-nucleon crosssection are higher than those published by other experiments at all WIMP masses, and the lowest limit on the WIMP-nucleon cross-section is 1.07*10 −42 cm 2 at a mass 3 of 60 GeV/c 2 . These results do provide new and interesting constraints at WIMP masses ≤40 GeV/c 2 and cross sections from 10 −42 -10 −39 cm 2 , a region in which some WIMP search experiments have claimed evidence for a WIMP signal, which other experiments claim to have ruled out.

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The Rotation Velocity Attributable to Dark Matter at Intermediate Radii in Disk Galaxies

Cited by 103 publications

References 144 publications

The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

Local-Group tests of dark-matter concordance cosmology

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

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