Constraints on small-scale cosmological fluctuations from SNe lensing dispersion

Ben-Dayan, Ido; Takahashi, Ryuichi

doi:10.1093/mnras/stv2356

Cited by 14 publications

(12 citation statements)

References 77 publications

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“…The running parameters are constrained also by supernovae lensing [73,74]. It involves nonlinear evolution and astrophysical uncertainties, so we do not adopt such bounds here.…”

Section: Inflation With Running Parametersmentioning

confidence: 99%

Primordial black hole dark matter and LIGO/Virgo merger rate from inflation with running spectral indices: formation in the matter- and/or radiation-dominated universe

Kohri¹,

Terada²

2018

Class. Quantum Grav.

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We study possibilities to explain the whole dark matter abundance by primordial black holes (PBHs) or to explain the merger rate of binary black holes estimated from the gravitational wave detections by LIGO/Virgo. We assume that the PBHs are originated in a radiation-or matter-dominated era from large primordial curvature perturbation generated by inflation. We take a simple model-independent approach considering inflation with large running spectral indices which are parametrized by n s , α s , and β s consistent with the observational bounds. The merger rate is fitted by PBHs with masses of O(10) M produced in the radiation-dominated era. Then the running of running should be β s ∼ 0.025, which can be tested by future observation. On the other hand, the whole abundance of dark matter is consistent with PBHs with masses of asteroids (O(10 −17 ) M ) produced in an early matter-dominated era if a set of running parameters are properly realized. arXiv:1802.06785v4 [astro-ph.CO] 5 Nov 2018 which we are interested [41][42][43][44][45][46][47][48][49][50]. In earlier works including Refs. [37,[51][52][53][54][55][56][57][58][59][60][61][62][63][64][65], the BH merger rate for LIGO/Virgo events and/or the DM abundance in inflationary scenarios have been discussed.Here we do not explicitly introduce features like double inflation [58,62] or additional fields like a curvaton [59, 61, 63] to explain DM or LIGO/Virgo events. It is remarkable and encouraging that such a simple inflationary power spectrum can account for the LIGO/Virgo BH merger rate or the whole DM. The former (latter) is explained by the PBHs of intermediate masses M ∼ O(10)M (asteroid masses M ∼ O(10 −17 )M ). Another feature of this paper is that we consider both cases of BH formation in the radiation-dominated (RD) era and in an early matter-dominated (MD) era. The latter is less extensively studied in the literature, but it is wellmotivated in the inflationary cosmology since e.g. the coherent oscillation phase of the inflaton before reheating behaves as a MD era. For the probability of PBH formations in a MD era, we take into account the effects of anisotropies [66-68] and angular momentum [22], which suppress the PBH formation compared to the case without these effects [66,69]. Differences of this paper from Ref. [59] include the facts that we also consider the running of running parameter β s , that we take into account the effects of angular momentum on the PBH formation rate in the MD era, and that we do not rely on a spectator field.

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“…The running parameters are constrained also by supernovae lensing [73,74]. It involves nonlinear evolution and astrophysical uncertainties, so we do not adopt such bounds here.…”

Section: Inflation With Running Parametersmentioning

confidence: 99%

Primordial black hole dark matter and LIGO/Virgo merger rate from inflation with running spectral indices: formation in the matter- and/or radiation-dominated universe

Kohri¹,

Terada²

2018

Class. Quantum Grav.

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“…Most studies focused on the magnitude probability distribution function (PDF) and some researchers have assumed a universal magnitude PDF and calibrated the coefficients, e.g., using N -body simulations, or considering a model of the universe and directly computing the magnitude PDF by ray-shooting simulations (Marra et al 2013, and references therein). Moreover, some authors have investigated, in particular, small-scale structure using the lensing effects for SNe Ia (Rauch 1991;Metcalf 1999;Metcalf & Silk 1999;Seljak & Holz 1999;Fedeli & Moscardini 2014;Castro & Quartin 2014;Ben-Dayan & Takahashi 2016).…”

Section: Introductionmentioning

confidence: 99%

CONSTRAINTS ON NEUTRINO MASSES FROM THE LENSING DISPERSION OF TYPE Ia SUPERNOVAE

Hada

Futamase

2016

ApJ

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We investigate how accurately the total mass of neutrinos is constrained from the magnitude dispersion of SNe Ia due to the effects of gravitational lensing. For this purpose, we use the propagation equation of light bundles in a realistic inhomogeneous universe and propose a sample selection for supernovae to avoid difficulties associated with small-scale effects such as strong lensing or shear effects. With a fitting formula for the nonlinear matter power spectrum taking account of the effects of massive neutrinos, we find that in our model it is possible to obtain the upper limit Σm ν ≃ 1.0[eV] for future optical imaging surveys with the Wide-Field InfraRed Survey Telescope and Large Synoptic Survey Telescope. Furthermore, we discuss how far we need to observe SNe Ia and to what extent we have to reduce the magnitude error except for lensing in order to realize the current tightest limit Σm ν < 0.2[eV].

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“…The reason we are justified in resorting to a first-order result after using second-order results up until this point is that r is already observationally constrained to be so small that even the leading order term has no significant effect on our constraints 7. We note that the supernova lensing dispersion can also probe the averaged value of the power spectrum on small scales, down to kmax 100Mpc −1 , but there is a degeneracy with the effect of baryons on the small-scale low-redshift power spectrum[31] 8. Note that this value is only important for including observational constraints in our plots.…”

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confidence: 67%

Can power spectrum observations rule out slow-roll inflation?

Vieira

Byrnes

Lewis

2018

J. Cosmol. Astropart. Phys.

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Abstract. The spectral index of scalar perturbations is an important observable that allows us to learn about inflationary physics. In particular, a detection of a significant deviation from a constant spectral index could enable us to rule out the simplest class of inflation models. We investigate whether future observations could rule out canonical single-field slowroll inflation given the parameters allowed by current observational constraints. We find that future measurements of a constant running (or running of the running) of the spectral index over currently available scales are unlikely to achieve this. However, there remains a large region of parameter space (especially when considering the running of the running) for falsifying the assumed class of slow-roll models if future observations accurately constrain a much wider range of scales.

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Constraints on small-scale cosmological fluctuations from SNe lensing dispersion

Cited by 14 publications

References 77 publications

Primordial black hole dark matter and LIGO/Virgo merger rate from inflation with running spectral indices: formation in the matter- and/or radiation-dominated universe

Primordial black hole dark matter and LIGO/Virgo merger rate from inflation with running spectral indices: formation in the matter- and/or radiation-dominated universe

CONSTRAINTS ON NEUTRINO MASSES FROM THE LENSING DISPERSION OF TYPE Ia SUPERNOVAE

Can power spectrum observations rule out slow-roll inflation?

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