A Direct Empirical Proof of the Existence of Dark Matter

Clowe, Douglas; Bradač, Maruša; Gonzalez, Anthony H.; Markevitch, M.; Randall, Scott W.; Jones, Christine; Zaritsky, Dennis

doi:10.1086/508162

Cited by 2,008 publications

(2,305 citation statements)

References 30 publications

Supporting

Mentioning

2,187

Contrasting

Unclassified

Order By: Relevance

“…Markevitch et al 2002;Clowe et al 2006;Bradač et al 2006). In comparison, the observable signs of merging activity in XMMU J1230.3+1339 occur at smaller angular scales of < ∼ 1 and correspondingly shorter projected physical distances of < ∼ 500 kpc, which implies either a steeper viewing angle with respect to the plane-of-the sky or a merger event closer to cluster core passage.…”

Section: Central Merging Activitymentioning

confidence: 95%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

show abstract

Section: Central Merging Activitymentioning

confidence: 95%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…There is abundant evidence for a significant cold dark matter (CDM) component in the universe [1][2][3], and perhaps the bestmotivated candidate is the lightest neutralino from supersymmetric (SUSY) extensions to the Standard Model [4]. A neutralino is expected to be non-relativistic and stable, and is more generally classified as a weakly interacting massive particle (WIMP).…”

Section: Expected Signal In Xenon10mentioning

confidence: 99%

The scintillation and ionization yield of liquid xenon for nuclear recoils

Sørensen

Manzur

Dahl

et al. 2009

Nuclear Instruments and Methods in Physics Research Section A:

104

View full text Add to dashboard Cite

a b s t r a c t XENON10 is an experiment designed to directly detect particle dark matter. It is a dual phase (liquid/ gas) xenon time-projection chamber with 3D position imaging. Particle interactions generate a primary scintillation signal (S1) and ionization signal (S2), which are both functions of the deposited recoil energy and the incident particle type. We present a new precision measurement of the relative scintillation yield L eff and the absolute ionization yield Q y , for nuclear recoils in xenon. A dark matter particle is expected to deposit energy by scattering from a xenon nucleus. Knowledge of L eff is therefore crucial for establishing the energy threshold of the experiment; this in turn determines the sensitivity to particle dark matter. Our L eff measurement is in agreement with recent theoretical predictions above 15 keV nuclear recoil energy, and the energy threshold of the measurement is $4 keV.A knowledge of the ionization yield Q y is necessary to establish the trigger threshold of the experiment. The ionization yield Q y is measured in two ways, both in agreement with previous measurements and with a factor of 10 lower energy threshold.

show abstract

“…The imparted ellipticity is typically comparable to or smaller than that intrinsic to the galaxy, and thus the distortion is only measurable statistically with large numbers of background galaxies. To do this measurement, we detect faint galaxies on deep optical images and calculate an ellipticity from the second moment of their surface brightness distribution, correcting the ellipticity for smearing by the point spread function (corrections for both anisotropies and smearing are obtained using an implementation of the KSB technique (Kaiser et al 1995) discussed in Clowe et al (2006)). The corrected ellipticities are a direct, but noisy, measurement of the reduced shear g = γ /(1 − κ).…”

Section: Methodology and Datamentioning

confidence: 99%

“…The one exception is the single passband HST pointing of main cluster, for which we measure colors from the Magellan images. Because it is not feasible to measure redshifts for all galaxies in the field, we select likely background galaxies using magnitude and color cuts (m 814 > 22 and not in the rhombus defined by 0.5 < m 606 − m 814 < 1.5, the surface mass density of the gravitational lens, indicating that the majority of the mass is concentrated away for the regions of high plasma density [23].…”

Section: Methodology and Datamentioning

confidence: 99%

See 1 more Smart Citation

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

McCarthy¹

2013

View full text Add to dashboard Cite

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.

show abstract

A Direct Empirical Proof of the Existence of Dark Matter

Cited by 2,008 publications

References 30 publications

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

The scintillation and ionization yield of liquid xenon for nuclear recoils

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

Contact Info

Product

Resources

About