MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on Angular Scales of 10[arcmin]–5°

Hanany, Shaul; Ade, Peter A. R.; Balbi, A.; Bock, J. J.; Borrill, J.; Boscaleri, A.; Bernardis, P. de; Ferreira, Pedro G.; Hristov, V. V.; Jaffe, A. H.; Lange, A. E.; Lee, A. T.; Mauskopf, Philip Daniel; Netterfield, C. B.; Oh, Sang-Yun; Pascale, Enzo; Rabii, B.; Richards, P. L.; Smoot, George F.; Stompor, R.; Winant, C. D.; Wu, Jian-Pin

doi:10.1086/317322

Cited by 1,157 publications

(654 citation statements)

References 30 publications

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“…This confluence of arguments favored the cosmological interpretation of the results over astrophysical explanations such as evolution of the supernova population or grey dust extinction that increased towards higher redshifts. Third, the supernova results were followed within a year by the results of balloon-borne CMB experiments that mapped the first acoustic peak and measured its angular location, providing strong evidence for spatial flatness (de Bernardis et al 2000;Hanany et al 2000; see Netterfield et al 1997 for earlier ground-based measurements hinting at the same result). On its own, the acoustic peak only implied Ω tot ≈ 1, not a non-zero Ω Λ , but it dovetailed perfectly with the estimates of Ω m and Ω Λ from large scale structure and supernovae.…”

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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Section: Historymentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…Here we take the latest bound from WMAP, Ωh 2 < .128 and also compare with the old limit (of 2001) from BOOMERANG [47], MAXIMA [48] and DASI [49] with Ωh 2 < 0.3. We will refer to this limit as pre-WMAP.…”

Section: Relic Density Of Neutralinosmentioning

confidence: 99%

Lower limit on the neutralino mass in the general MSSM

Bélanger¹,

Boudjema²,

Cottrant³

et al. 2004

J. High Energy Phys.

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We discuss constraints on SUSY models with non-unified gaugino masses and R P conservation. We derive a lower bound on the neutralino mass combining the direct limits from LEP, the indirect limits from (g − 2) µ , b → sγ, B s → µ + µ − and the relic density constraint from WMAP. The lightest neutralino mχ0 1 ≈ 6 GeV is found in models with a light pseudoscalar with M A < 200 GeV and a large value for tan β. Models with heavy pseudoscalars lead to mχ0 1 > 18(29) GeV for tan β = 50(10). We show that even a very conservative bound from the muon anomalous magnetic moment can increase the lower bound on the neutralino mass in models with µ < 0 and/or large values of tan β. We then examine the potential of the Tevatron and the direct detection experiments to probe the SUSY models with the lightest neutralinos allowed in the context of light pseudoscalars with high tan β. We also examine the potential of an e + e − collider of 500 GeV to produce SUSY particles in all models with neutralinos lighter than the W . In contrast to the mSUGRA models, observation of at least one sparticle is not always guaranteed.

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“…They originate during inflation as zero point oscillations of the quantum modes of various fields-the inflaton giving rise to scalar perturbations, the graviton to tensor perturbations-that are directly observable today as cosmic background anisotropy [8][9][10][11][12][13][14][15]. The field quanta in the original fluctuations convert to classical perturbations as they pass through the de Sitter-like event horizon; they are then parametrically amplified by an exponential factor during the many subsequent e-foldings of inflation, creating an enormous number of coherent quanta in phase with the original quantum seed perturbation; these in turn create large scale perturbations in the classical gravitational gauge-invariant potential φ m [16], leading to observable anisotropy and large scale structure.…”

Section: Introductionmentioning

confidence: 99%

Holographic discreteness of inflationary perturbations

Hogan

2002

Phys. Rev. D

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The cosmological holographic principle, which states that the total observable entropy of de Sitter space (including gravitational quanta) is bounded by S < π/H 2 , where H is the expansion rate, is used to estimate the magnitude of quantum-gravitational effects on inflationary perturbations. The constraint is shown to imply that the initial states of the vacua for perturbation modes are not independent, and that field theory is not a reliable tool to study transplanckian effects on mode amplitudes and phases. It is argued that holographic discreteness alters the continuous, random-phase gaussian distribution predicted by standard field theory for fluctuations in the inflaton field that lead to cosmic background anisotropy. A toy model, applied in the context of scalar inflaton perturbations produced during standard slow-roll inflation, and assuming that horizonscale perturbations "freeze out" in discrete steps separated by one bit of observable information, predicts discrete steps in anisotropy separated by ∆T ≈ 10 −10 K. It is conjectured that the Hilbert space of a typical observable perturbation is equivalent to that of no more than about 10 5 binary spins (approximately the inverse of the final scalar metric perturbation amplitude, independent of H and other parameters), and that some manifestations of this discreteness may be observable.

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MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on Angular Scales of 10[arcmin]–5°

Cited by 1,157 publications

References 30 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Lower limit on the neutralino mass in the general MSSM

Holographic discreteness of inflationary perturbations

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