A Measurement of Excess Antenna Temperature at 4080 Mc/s.

Penzias, A. A.; Wilson, R. W.

doi:10.1086/148307

Cited by 2,135 publications

(1,318 citation statements)

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“…As a result, the higher-Tc side had higher phonon noise (σ ∼ 250 eV) than the other (σ ∼ 130 eV). Future devices will have matched Tc's near 80 mK and be optimized to avoid TES phase separation [5]. The measured charge noise was σ ∼ 300 eV for the inner channels, near the resolution achieved in our standard detectors [4], and in agreement with the calculated 98 pF capacitance.…”

Section: Detector Designsupporting

confidence: 75%

“…5. The two MISS rejection/identification cuts proposed in this chapter were unable to remove a subset of ∼10% of the MISS events, which occupied a region of the timing parameter space shared by both surface ERs and bulk NRs.…”

Section: Resultsmentioning

confidence: 91%

“…Penzias and Robert Wilson [5] in 1965, though earlier studies are now known to have accurately measured the CMB temperature through its effects on absorption lines [6] and directly through radio astronomy [7,8]. The existence of the CMB and its strong degree of homogeneity even at the largest scales is among the strongest evidence for Big Bang cosmology (along with the cosmological redshift and the abundances of the light elements).…”

Section: Cosmic Microwave Backgroundmentioning

confidence: 99%

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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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Section: Detector Designsupporting

confidence: 75%

Section: Resultsmentioning

confidence: 91%

Section: Cosmic Microwave Backgroundmentioning

confidence: 99%

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

McCarthy¹

2013

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“…In 1929, Hubble discovered direct evidence for the expansion of the universe (Hubble, 1929), thus removing the original motivation for the Λ term. 1 In 1965, the discovery and interpretation of the cosmic microwave background (CMB; Penzias and Wilson 1965;Dicke et al 1965) provided the pivotal evidence for a hot big bang origin of the cosmos.…”

Section: Historymentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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“…The discovery of the cosmic microwave background (CMB) by Penzias & Wilson (1965) in the mid sixties set the stage for a quantitative exploitation of the Big Bang nucleosynthesis theory. In their pioneer studies, Peebles (1966) and Wagoner et al (1967) demonstrated that D, 3 He and 4 He could well have been produced in solar-system abundances in the 'primordial fireball'.…”

Section: Introductionmentioning

confidence: 99%

Galactic evolution of D, ³He and ⁴He

Romano

2009

Proc. IAU

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Abstract. The uncertainties which still plague our understanding of the evolution of the light nuclides D, 3 He and 4 He in the Galaxy are described. Measurements of the local abundance of deuterium range over a factor of 3. The observed dispersion can be reconciled with the predictions on deuterium evolution from standard Galactic chemical evolution models, if the true local abundance of deuterium proves to be high, but not too high, and lower observed values are due to depletion onto dust grains. The nearly constancy of the 3 He abundance with both time and position within the Galaxy implies a negligible production of this element in stars, at variance with predictions from standard stellar models which, however, do agree with the (few) measurements of 3 He in planetary nebulae. Thermohaline mixing, inhibited by magnetic fields in a small fraction of low-mass stars, could in principle explain the complexity of the overall scenario. However, complete grids of stellar yields taking this mechanism into account are not available for use in chemical evolution models yet. Much effort has been devoted to unravel the origin of the extreme helium-rich stars which seem to inhabit the most massive Galactic globular clusters. Yet, the issue of 4 He evolution is far from being fully settled even in the disc of the Milky Way.

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A Measurement of Excess Antenna Temperature at 4080 Mc/s.

Cited by 2,135 publications

References 0 publications

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

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

Observational probes of cosmic acceleration

Galactic evolution of D, ³He and ⁴He

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A Measurement of Excess Antenna Temperature at 4080 Mc/s.

Cited by 2,135 publications

References 0 publications

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

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

Observational probes of cosmic acceleration

Galactic evolution of D, 3He and 4He

Contact Info

Product

Resources

About

Galactic evolution of D, ³He and ⁴He