Running-mass inflation model and WMAP

Covi, Laura; Lyth, David H.; Melchiorri, A.; Ödman, Carolina J.

doi:10.1103/physrevd.70.123521

Cited by 35 publications

(52 citation statements)

References 46 publications

(64 reference statements)

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“…If we neglect ǫ 1 (see below), then one recovers the formula already derived in [80,81,82], namely n S − 1 ≃ 2(s − c). The same route for the third slow-roll parameter gives…”

Section: Running-mass Inflationsupporting

confidence: 67%

“…As a result, integrating the equations of motion along 60 e-folds may require a computing accuracy much smaller than the quadruple precision computing bound 10 −32 . In order to satisfy this computing requirement, we have considered a rather limited range for the MCMC running mass parameters: an uniform prior has been chosen for log(κφ It may be convenient to compare this approach to the one used in the literature [82]. In that reference, when concerns with the leading order only, the slow-roll equations n S − 1 ≃ 2(s − c) and α S ≃ 2sc are assumed.…”

Section: Running Mass Modelsmentioning

confidence: 99%

See 1 more Smart Citation

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Martin

Ringeval

2006

J. Cosmol. Astropart. Phys.

241

374

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Abstract.The implications of the WMAP (Wilkinson Microwave Anisotropy Probe) third year data for inflation are investigated using both the slow-roll approximation and an exact numerical integration of the inflationary power spectra including a phenomenological modelling of the reheating era. At slow-roll leading order, the constraints ǫ 1 < 0.022 and −0.07 < ǫ 2 < 0.07 are obtained at 95% CL (Confidence Level) implying a tensor-to-scalar ratio r 10 < 0.21 and a Hubble parameter during inflation H/m Pl < 1.3 × 10 −5 . At next-to-leading order, a tendency for ǫ 3 > 0 is observed. With regards to the exact numerical integration, large field models, V (φ) ∝ φ p , with p > 3.1 are now excluded at 95% CL. Small field models, V (φ) ∝ 1 − (φ/µ) p , are still compatible with the data for all values of p. However, if µ/m Pl < 10 is assumed, then the case p = 2 is slightly disfavoured. In addition, mild constraints on the reheating temperature for an extreme equation of state w reh −1/3 are found, namely T reh > 2 TeV at 95% CL. Hybrid models are disfavoured by the data, the best fit model having ∆χ 2 ≃ +5 with two extra parameters in comparison with large field models. Running mass models remain compatible, but no prior independent constraints can be obtained. Finally, superimposed oscillations of trans-Planckian origin are studied. The vanilla slow-roll model is still the most probable one. However, the overall statistical weight in favour of superimposed oscillations has increased in comparison with the WMAP first year data, the amplitude of the oscillations satisfying 2|x|σ 0 < 0.76 at 95% CL. The best fit model leads to an improvement of ∆χ 2 ≃ −12 for 3 extra parameters. Moreover, compared to other oscillatory patterns, the logarithmic shape is favoured.

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“…If we neglect ǫ 1 (see below), then one recovers the formula already derived in [80,81,82], namely n S − 1 ≃ 2(s − c). The same route for the third slow-roll parameter gives…”

Section: Running-mass Inflationsupporting

confidence: 67%

Section: Running Mass Modelsmentioning

confidence: 99%

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Martin

Ringeval

2006

J. Cosmol. Astropart. Phys.

241

374

View full text Add to dashboard Cite

show abstract

“…From the theoretical point of view [77], H I can lie in the wide range of values from, say, H I ∼ 10 4 GeV for anomaly-mediation case to H I ∼ 10 −3 GeV for gauge-mediation. Assuming instant reheating at some value of the inflaton field, from the energy conservation condition we have:…”

Section: Constraints On the Running Mass Model From Pbhsmentioning

confidence: 99%

“…The running mass inflation model was proposed in [71,72] and further studied in many papers including [73,74,75,76,77]. The model predicts a rather strong scale dependence of the spectral index, possibly allowing large values of P R (k) at small scales, which can lead to PBH production [ [78], [79], [31]].…”

Section: Constraints On the Running Mass Model From Pbhsmentioning

confidence: 99%

Constraints on amplitudes of curvature perturbations from primordial black holes

Bugaev

Klimai

2009

Phys. Rev. D

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We calculate the primordial black hole (PBH) mass spectrum produced from a collapse of the primordial density fluctuations in the early Universe using, as an input, several theoretical models giving the curvature perturbation power spectra PR(k) with large (∼ 10 −2 ÷ 10 −1 ) values at some scale of comoving wave numbers k. In the calculation we take into account the explicit dependence of gravitational (Bardeen) potential on time. Using the PBH mass spectra, we further calculate the neutrino and photon energy spectra in extragalactic space from evaporation of light PBHs, and the energy density fraction contained in PBHs today (for heavier PBHs). We obtain the constraints on the model parameters using available experimental data (including data on neutrino and photon cosmic backgrounds). We briefly discuss the possibility that the observed 511 keV line from the Galactic center is produced by annihilation of positrons evaporated by PBHs.

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“…However the shape of potential does appear in a more theoretically motivated setup, the running mass model [44,60,61,62,63,64,65,66,67] which has the potential:…”

Section: The Running Mass Modelmentioning

confidence: 99%

Generating primordial black holes via hilltop-type inflation models

Alabidi

Kohri

2009

Phys. Rev. D

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It has been shown that black holes would have formed in the early Universe if, on any given scale, the spectral amplitude of the Cosmic Microwave Background (CMB) exceeds P ζ ∼ 10 −4 . This value is within the bounds allowed by astrophysical phenomena for the small scale spectrum of the CMB, corresponding to scales which exit the horizon at the end of slow-roll inflation. Previous work by Kohri et. al. (2007) showed that for black holes to form from a single field model of inflation, the slope of the potential at the end of inflation must be flatter than it was at horizon exit. In this work we show that a phenomenological Hilltop model of inflation, satisfying the Kohri et. al. criteria, could lead to the production of black holes, if the power of the inflaton self-interaction is less than or equal to 3, with a reasonable number or e−folds. We extend our analysis to the running mass model, and confirm that this model results in the production of black holes, and by using the latest WMAP year 5 bounds on the running of the spectral index, and the black hole constraint we update the results of Leach et. al. (2000) excluding more of parameter space.

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Running-mass inflation model and WMAP

Cited by 35 publications

References 46 publications

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Constraints on amplitudes of curvature perturbations from primordial black holes

Generating primordial black holes via hilltop-type inflation models

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