Cosmology from MAXIMA-1, BOOMERANG, and COBE DMR Cosmic Microwave Background Observations

Jaffe, A. H.; Ade, Peter A. R.; Balbi, A.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; Bernardis, P. de; Farese, P.; Ferreira, Pedro G.; Ganga, K.; Giacometti, M.; Hanany, Shaul; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Lange, A. E.; Lee, A. T.; Martinis, L.; Masi, S.; Mauskopf, Philip Daniel; Melchiorri, A.; Montroy, T. E.; Netterfield, C. B.; Oh, Sang-Yun; Pascale, Enzo; Piacentini, F.; Pogosyan, D.; Prunet, S.; Rabii, B.; Rao, Sandhya M.; Richards, P. L.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Smoot, George F.; Stompor, R.; Winant, C. D.; Wu, Jiun-Huei Proty

doi:10.1103/physrevlett.86.3475

Cited by 476 publications

(377 citation statements)

References 26 publications

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“…However, the perfect fluid becomes negligible as the expansion proceeds and the universe subsequently enters a phase of power law, inflationary expansion driven by the exponential potential of a scalar field. For n = 3, the fluid is pressureless and current observations indicate that the universe is undergoing such a transition at the present epoch [4,5,6].…”

Section: Exact Cosmologies Sourced By Scalar Fields and Perfect Fluidsmentioning

confidence: 99%

“…High redshift observations of type Ia supernovae suggest that the universe is experiencing another phase of accelerated expansion at the present epoch [4]. This, combined with the CMB data, presents a picture of the universe dominated by a dark energy component [5,6]. One possible source of this dark energy is a scalar quintessence field that interacts with baryonic and non-baryonic matter in such a way that its potential energy is currently dominating the cosmic dynamics [7].…”

Section: Introductionmentioning

confidence: 99%

“…One possible source of this dark energy is a scalar quintessence field that interacts with baryonic and non-baryonic matter in such a way that its potential energy is currently dominating the cosmic dynamics [7]. The observations favour a model of structure formation where 70% of the energy density of the universe is presently in the form of quintessence [6]. The remaining fraction of the energy density is comprised of visible and cold dark matter which collectively act as a pressureless perfect fluid.…”

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confidence: 99%

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Ermakov-Pinney equation in scalar field cosmologies

2002

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It is shown that the dynamics of cosmologies sourced by a mixture of perfect fluids and self-interacting scalar fields are described by the non-linear, Ermakov-Pinney equation. The general solution of this equation can be expressed in terms of particular solutions to a related, linear differential equation. This characteristic is employed to derive exact cosmologies in the inflationary and quintessential scenarios. The relevance of the Ermakov-Pinney equation to the braneworld scenario is discussed. reviews, see, e.g., [3]). The simplest mechanism for inflation utilises the potential energy associated with the self-interaction of a scalar inflaton field to drive the accelerated expansion. High redshift observations of type Ia supernovae suggest that the universe is experiencing another phase of accelerated expansion at the present epoch [4]. This, combined with the CMB data, presents a picture of the universe dominated by a dark energy component [5,6]. One possible source of this dark energy is a scalar quintessence field that interacts with baryonic and non-baryonic matter in such a way that its potential energy is currently dominating the cosmic dynamics [7]. The observations favour a model of structure formation where 70% of the energy density of the universe is presently in the form of quintessence [6]. The remaining fraction of the energy density is comprised of visible and cold dark matter which collectively act as a pressureless perfect fluid.The ekpyrotic scenario has recently been proposed as an alternative to the standard inflationary cosmology [8]. In this scenario the big bang is interpreted as the collision of two domain walls or branes travelling through a fifth dimension. Before the collision, the effective dynamics on the four dimensional branes is described by Einstein's gravity minimally coupled to a self-interacting scalar field. The field parametrizes the separation between the branes and at early times slowly rolls down a negative potential. This results in an accelerated collapse of the universe and since the field is minimally coupled, its energy density is related to the Hubble parameter by the standard Friedmann equation. Thus, self-interacting scalar fields play a central role in modern cosmology and in view of the above developments, it is important to investigate cosmologies that contain both a scalar field and a perfect fluid.In this paper, we develop an analytical approach to models of this type by expressing the cosmological field equations in terms of an Ermakov system [9,10,11]. In general, an Ermakov system is a pair of coupled, second-order, non-linear ordinary differential equations (ODEs) [11] and such systems often arise in studies of nonlinear optics [12], nonlinear elasticity [13], molecular structures [14] and quantum cosmology [15]. (For further references, see, e.g., Refs. [16]). In the one-dimensional case, the two equations decouple and the system reduces to a single equation known as the Ermakov-Pinney equation [9,17]. This is given by 1

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Section: Exact Cosmologies Sourced By Scalar Fields and Perfect Fluidsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Ermakov-Pinney equation in scalar field cosmologies

2002

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“…Solving the dynamics of the inflaton during the inflation, we obtainΨ at the radiationdominated era [13] 17) where χ is the inflaton field. Using the slow-roll condition for χ, and also usingq H inf /2π, we obtain r q 9 4 18) where V inf is the inflaton potential and V inf is its derivative with respect to the inflaton field.…”

Section: )mentioning

confidence: 99%

Cosmic microwave background anisotropy with cosine-type quintessence

2001

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We study the Cosmic Microwave Background (CMB) anisotropies produced by cosine-type quintessence models. In our analysis, effects of the adiabatic and isocurvature fluctuations are both taken into account. For purely adiabatic fluctuations with scale invariant spectrum, we obtain a stringent constraint on the model parameters using the CMB data from COBE, BOOMERanG and MAXIMA. Furthermore, it is shown that isocurvature fluctuations have significant effects on the CMB angular power spectrum at low multipoles in some parameter space, which may be detectable in future satellite experiments. Such a signal may be used to test the cosine-type quintessence models.

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“…By the joint analysis of the Maxima-1, Boomerang and COBE cosmic microwave anisotropy results and the estimate of the systematic errors, the blue spectrum tilt should be in the region of 0 ≤ λ < 0.27 [29] 1 . In this case α ≃ 7.5.…”

Section: Termination Of Phantom Dominated Phasementioning

confidence: 99%

Avoidance of big rip in phantom cosmology by gravitational back reaction

Wu¹,

2005

Nuclear Physics B

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The effects of the gravitational back reaction of cosmological perturbations are investigated in a cosmological model where the universe is dominated by phantom energy. We assume a COBE normalized spectrum of cosmological fluctuations at the present time and calculate the effective energy-momentum tensor of the gravitational back-reactions of cosmological perturbations whose wavelengths at the time when the back-reactions are evaluated are larger than the Hubble radius.Our results reveal that the effects of gravitational back-reactions will counteract that of phantom energy sooner or later and can become large enough to terminate the phantom dominated phase before the big rip as the universe evolves. This arises because the phase space of infrared modes grows very rapidly as we come close to the big rip. 98.80.Cq

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Cosmology from MAXIMA-1, BOOMERANG, and COBE DMR Cosmic Microwave Background Observations

Abstract: Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE DMR, provide consistent and high signal-to-noise measurements of the cosmic microwave background power spectrum at spherical harmonic multipole bands over 2 Show more

Cited by 476 publications

References 26 publications

Ermakov-Pinney equation in scalar field cosmologies

Ermakov-Pinney equation in scalar field cosmologies

Cosmic microwave background anisotropy with cosine-type quintessence

Avoidance of big rip in phantom cosmology by gravitational back reaction

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