記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1103/PhysRevD.106.042007

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

In this work, we have performed numerical simulations of primordial black hole (PBH) formation in the Friedman-Lemaître-Robertson-Walker universe filled by radiation fluid, introducing the local-type non-Gaussianity to the primordial curvature fluctuation. We have compared the numerical results from simulations with previous analytical estimations on the threshold value for PBH formation done in the previous paper [1], particularly for negative values of the non-linearity parameter f NL. Our numerical results show the existence of PBH formation of (the so-called) type I also in the case f NL ≤2-0.336, which was not found in the previous analytical expectations using the critical averaged compaction function. In particular, although the universal value for the averaged critical compaction function ō o = 2/5 found previously in the literature is not satisfied for all the profiles considered in this work, an alternative direct analytical estimate has been found to be roughly accurate to estimate the thresholds, which gives the value of the critical averaged density with a few % deviation from the numerical one for f NL ≤3-1.

DOI： 10.1088/1475-7516/2022/05/012

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記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Galaxies  

The DECi-hertz Interferometer Gravitational-Wave Observatory (DECIGO) is a space gravitational wave (GW) detector. DECIGO was originally designed to be sensitive enough to observe primordial GW background (PGW). However, due to the lowered upper limit of the PGW by the Planck observation, further improvement of the target sensitivity of DECIGO is required. In the previous studies, DECIGO’s parameters were optimized to maximize the signal-to-noise ratio (SNR) of the PGW to quantum noise including the effect of diffraction loss. To simulate the SNR more realistically, we optimize DECIGO’s parameters considering the GWs from double white dwarfs (DWDs) and the thermal noise of test masses. We consider two cases of the cutoff frequency of GWs from DWDs. In addition, we consider two kinds of thermal noise: thermal noise in a residual gas and internal thermal noise. To investigate how the mirror geometry affects the sensitivity, we calculate it by changing the mirror mass, keeping the mirror thickness, and vice versa. As a result, we obtained the optimums for the parameters that maximize the SNR that depends on the mirror radius. This result shows that a thick mirror with a large radius gives a good SNR and enables us to optimize the design of DECIGO based on the feasibility study of the mirror size in the future.

DOI： 10.3390/galaxies10010025

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出版者・発行元：Proceedings of the 20th Workshop on General Relativity and Gravitation in Japan, JGRG 2010  

Modulated reheating scenario is one of the most attractive models that predict possible detections of primordial non-Gaussianity through future CMB observations such as the Planck satellite. We study the baryonic-isocurvature fluctuations in the Affleck- Dine baryogenesis with the modulated reheating scenario. We show that the simple Affleck-Dine baryogenesis would be incompatible with the modulated reheating scenario with respect to the current observational constraint on the baryonic-isocurvature fluctuations, like a gravitino dark matter scenario.

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Progress of Theoretical and Experimental Physics  

Since the discovery of the accelerated expansion of the present universe, significant theoretical developments have been made in the area of modified gravity. In the meantime, cosmological observations have been providing more high-quality data, allowing us to explore gravity on cosmological scales. To bridge the recent theoretical developments and observations, we present an overview of a variety of modified theories of gravity and the cosmological observables in the cosmic microwave background and large-scale structure, supplemented with a summary of predictions for cosmological observables derived from cosmological perturbations and sophisticated numerical studies. We specifically consider scalar-tensor theories in the Horndeski and DHOST family, massive gravity/bigravity, vector-tensor theories, metric-affine gravity, and cuscuton/minimally modified gravity, and discuss the current status of those theories with emphasis on their physical motivations, validity, appealing features, the level of maturity, and calculability. We conclude that the Horndeski theory is one of the most well-developed theories of modified gravity, although several remaining issues are left for future observations. The paper aims to help to develop strategies for testing gravity with ongoing and forthcoming cosmological observations.

DOI： 10.1093/ptep/ptad052

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掲載種別：研究論文（学術雑誌）   出版者・発行元：Publications of the Astronomical Society of Japan  

In the most distant reaches of the Universe, the 21 cm hyperfine transition in neutral hydrogen provides one of the only available tracers of large-scale structure. A number of instruments have been working or are planned to measure the 21 cm line signals, and in particular, the Experiment to Detect the Global EoR Signature (EDGES) has recently reported the first detection of an absorption signal, which corresponds to the 21 cm line global signal at the epoch of reionization (EoR). The future large radio telescope, the Square Kilometre Array (SKA) will be able to deliver the high-precision measurement of the 21 cmline emission/absorption signals. In this paper, we review the current status for the 21 cmline global and fluctuation signals from EoR to the dark ages, and then summarize the recent studies of how we probe the primordial Universe particularly motivated by the recent EDGES result and future observations by SKA. We focus on two applications for constraining cosmology with the EDGES result: constraints on the primordial magnetic fields and those on the primordial power spectrum.We also discuss the potential of future SKA for probing the inflationary Universe, by discussing expected constraints on the primordial power spectrum, its adiabaticity, and primordial non-Gaussianities from future observations of 21cm fluctuations.

DOI： 10.1093/pasj/psac015

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Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

Motivated by the result of Planck+BICEP/Keck recently released, we investigate the consistency of the multi-field inflation models in terms of the spectral index ns and the tensor-to-scalar ratio r. In this study, we focus on double-inflaton models with and without a spectator field. We find that inflaton with a quadratic potential can become viable when three fields with a specific hierarchical mass spectrum are realized such that two fields act as inflatons and the other one is the spectator. We also discuss the conditions to avoid the fine-tuning, by careful study of how the prediction depends on the background trajectory in the inflaton-field space.

DOI： 10.1088/1475-7516/2022/07/042

DOI： 10.1088/1475-7516/2022/07/042

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その他リンク： https://iopscience.iop.org/article/10.1088/1475-7516/2022/07/042/pdf

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

In this paper, we update the peak theory for the estimation of the primordial black hole (PBH) abundance, particularly by implementing the critical behavior in the estimation of the PBH mass and employing the averaged compaction function for the PBH formation criterion to relax the profile dependence. We apply our peak theory to a specific non-Gaussian feature called the exponential tail, which is characteristic in ultra slow-roll models of inflation. With this type of non-Gaussianity, the probability of a large perturbation is not suppressed by the Gaussian factor but decays only exponentially, so the PBH abundance is expected to be much enhanced. Not only do we confirm this enhancement even compared to the case of the corresponding nonlinearity parameter f NL = 5/2, but also we find that the resultant PBH mass spectrum has a characteristic maximal mass which is not seen in the simple Press-Schechter approach.

DOI： 10.1088/1475-7516/2021/10/053

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その他リンク： https://iopscience.iop.org/article/10.1088/1475-7516/2021/10/053/pdf

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

We motivate a minimal realization of slow-roll k-inflation by incorporating the local conformal symmetry and the broken global SO(1,1) symmetry in the metric-affine geometry. With use of the metric-affine geometry where both the metric and the affine connection are treated as independent variables, the local conformal symmetry can be preserved in each term of the Lagrangian and thus higher derivatives of scalar fields can be easily added in a conformally invariant way. Predictions of this minimal slow-roll k-inflation, ns∼0.96, r∼0.005, and cs∼0.03, are not only consistent with current observational data but also have a prospect to be tested by forthcoming observations.

DOI： 10.1103/PhysRevD.103.L101303

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その他リンク： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.103.L101303/fulltext

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We develop a possibility of generating tensor non-Gaussianity in a kind of anisotropic inflation, where a U(1) gauge field is kinetically coupled to a spectator scalar field. Owing to this coupling, the coherent mode of the electric field appears and softly breaks the isotropy of the Universe. We compute the bispectrum of linearly-polarized tensor perturbations sourced by the gauge field and find that it is strongly red-tilted and has distinctive statistical anisotropies including higher-order multipole moments. Interestingly, the tensor bispectra with the specific combinations of linear polarization modes are dominant, and their amplitudes depend on the different sets of multipole moments. This new type of statistically-anisotropic tensor non-Gaussianity can be potentially testable with the upcoming cosmic microwave background B-mode polarization experiments.

DOI： 10.1088/1475-7516/2021/03/047

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その他リンク： https://iopscience.iop.org/article/10.1088/1475-7516/2021/03/047/pdf

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2021/01/071

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その他リンク： https://iopscience.iop.org/article/10.1088/1475-7516/2021/01/071

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

We study matter density perturbations up to third order and the one-loop matter power spectrum in degenerate higher-order scalar-tensor (DHOST) theories beyond Horndeski. We systematically solve gravitational field equations and fluid equations order by order and find three novel shape functions characterizing the third-order solution in DHOST theories. A complete form of the one-loop matter power spectrum is then obtained using the resultant second- and third-order solutions. We confirm the previous result that the convergence condition of the loop integrals in the infrared limit becomes more stringent than that of the standard one in general relativity. We show that also in the ultraviolet limit the convergence condition becomes more stringent and the one-loop matter power spectrum is thus sensitive to the short-wavelength behavior of the linear power spectrum.

DOI： 10.1103/PhysRevD.102.103505

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その他リンク： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.102.103505/fulltext

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：EPL  

DOI： 10.1209/0295-5075/132/39001

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その他リンク： https://iopscience.iop.org/article/10.1209/0295-5075/132/39001/pdf

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

We show that a nonminimal coupling to gravity can not only make some inflationary models consistent with cosmological data, similar to the case of Higgs inflation, but can also invoke slow-roll violation to realize a graceful exit from inflation. In particular, this is the case in models where a destabilizing mechanism that ends inflation should be assumed when the model is minimally coupled to gravity. As explicit examples, we consider the power-law and inverse monomial inflation models with a nonminimal coupling to gravity. While these models are excluded in the minimally coupled case, we show that they can become viable again in nonminimally coupled scenarios. In most scenario we considered, reheating can be naturally realized via gravitational particle production but this depends on the underlying theory of gravity in a nontrivial way reheating can be naturally realized via gravitational particle production but that this depends on the underlying theory of gravity in a nontrivial way.

DOI： 10.1103/PhysRevD.102.043524

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その他リンク： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.102.043524/fulltext

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

Primordial magnetic field (PMF) is one of the feasible candidates to explain observed large-scale magnetic fields, for example, intergalactic magnetic fields. We present a new mechanism that brings us information about PMFs on small scales based on the abundance of primordial black holes (PBHs). The anisotropic stress of the PMFs can act as a source of the super-horizon curvature perturbation in the early universe. If the amplitude of PMFs is sufficiently large, the resultant density perturbation also has a large amplitude, and thereby, the PBH abundance is enhanced. Since the anisotropic stress of the PMFs is consist of the square of the magnetic fields, the statistics of the density perturbation follows the non-Gaussian distribution. {Assuming Gaussian distributions and delta-function type power spectrum for PMFs, based on a Monte-Carlo method, we obtain an approximate probability density function of the density perturbation, and it is an important piece to relate the amplitude of PMFs with the abundance of PBHs.} Finally, we place the strongest constraint on the amplitude of PMFs as a few hundred nano-Gauss on 102 Mpc-1 k 1018 Mpc-1 where the typical cosmological observations never reach.

DOI： 10.1088/1475-7516/2020/05/039

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arXiv

その他リンク： https://iopscience.iop.org/article/10.1088/1475-7516/2020/05/039

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Progress of Theoretical and Experimental Physics  

DOI： 10.1093/ptep/ptaa011

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出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.100.123544

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arXiv

Computations of the primordial black hole (PBH) mass function discussed in
the literature have conceptual issues. They stem from that the mass function is
a differential quantity and the standard criterion of the PBH formation from
the seed primordial fluctuations cannot be directly applied to the computation
of the differential quantities. We propose a new criterion of the PBH formation
which is an addition of one extra condition to the existing one. By doing this,
we derive a formal expression of the PBH mass function without introducing any
ambiguous interpretations which exist in the previous studies. Once the
underlying primordial fluctuations are specified, the PBH mass function can be
in principle determined by the new formula. As a demonstration of our
formulation, we compute the PBH mass function analytically for the case where
the perturbations are Gaussian and the space is one dimension.

arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Monthly Notices of the Royal Astronomical Society  

Spatially fluctuating primordial magnetic fields (PMFs) inhomogeneously reheat the Universe when they dissipate deep inside the horizon before recombination. Such an energy injection turns into an additional photon temperature perturbation. We investigate secondary cosmic microwave background (CMB) temperature anisotropies originated from this mechanism, which we call inhomogeneous magnetic reheating. We find that it can bring us information about non-linear coupling between PMFs and primordial curvature perturbations parametrized by bNL, which should be important for probing the generation mechanism of PMFs. In fact, by using current CMB observations, we obtain an upper bound on the non-linear parameter as log (bNL(Bλ/nG)2) ≲− 36.5nB − 94.0 with Bλ and nB being a magnetic field amplitude smoothed over λ = 1 Mpc scale and a spectral index of the PMF power spectrum, respectively. Our constraints are far stronger than a previous forecast based on the future CMB spectral distortion anisotropy measurements because inhomogeneous magnetic reheating covers a much wider range of scales, i.e. 1 Mpc−1 ≲ k ≲ 1015 Mpc−1

DOI： 10.1093/mnras/stz2882

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arXiv

出版者・発行元：Progress of Theoretical and Experimental Physics  

DOI： 10.1093/ptep/ptz105

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arXiv

その他リンク： http://arxiv.org/pdf/1906.04958v2

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

In this paper, we fully investigate cosmological scenarios in which dark matter is non-minimally coupled to an extra scalar degree of freedom. The interaction is realized by means of conformal and disformal terms in the transformed gravitational metric. Considering linear perturbation theory, we show that the growth rate of dark matter differs from the uncoupled case and that the well-known Kaiser formula undergoes modification. As a result, redshift space distortion measurements cease to be a direct probe of the linear growth rate of total matter, since the distortion factor has an extra, coupling-dependent term. We study the effect of the coupling in three cosmological models, two conformally and one disformally coupled, and forecast the constraints on the coupling, and other cosmological parameters, from future galaxy surveys.

DOI： 10.1088/1475-7516/2019/10/049

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arXiv

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2019/09/033

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arXiv

DOI： 10.1103/PhysRevD.100.023537

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arXiv

出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.99.104051

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arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）  

掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.99.083503

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arXiv

その他リンク： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.99.083503/fulltext

掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We investigate future constraints on primordial local-type non-Gaussianity from 21 cm angular power spectrum from minihalos. We particularly focus on the trispectrum of primordial curvature perturbations which are characterized by the non-linearity parametersτ NL and g NL . We show that future measurements of minihalo 21 cm angular power spectrum can probe these non-linearity parameters with an unprecedented precision of τ NL ∼ 30 and g NL ∼ 2 × 10 3 for Square Kilometre Array (SKA) and τ NL ∼ 0.6 and g NL ∼ 8 × 10 2 for Fast Fourier Transform Telescope (FFTT). These levels of sensitivity would give significant implications for models of the inflationary Universe and the origin of cosmic density fluctuations.

DOI： 10.1088/1475-7516/2019/02/033

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arXiv

出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.98.083522

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arXiv

その他リンク： http://arxiv.org/pdf/1808.08044v1

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

Primordial magnetic fields (PMFs) can source gravitational wave background (GWB). In this paper, we investigate the possible constraints on small-scale PMF considering the ongoing and forthcoming direct detection observations of GWB. In contrast to the conventional cosmological probes, e.g., cosmic microwave background anisotropies, which are useful to investigate large-scale PMFs (>1 Mpc), the direct detection experiments of GWB can explore small-scale PMFs whose scales correspond to the observed frequencies of GWB. We show that future ground-based or space-based interferometric gravitational wave detectors give a strong constraint of about 102 nG on much smaller scales of about k≈1012 Mpc-1. We also demonstrate that pulsar timing arrays have a potential to strongly constrain PMFs. The current limits on GWB from pulsar timing arrays can put the tight constraint on the amplitude of the PMFs of about 30 nG whose coherent length is about k≈106 Mpc-1. The future experiments for the direct detection of GWB by the Square Kilometre Array could give much tighter constraints on the amplitude of PMFs of about 5 nG on k≈106 Mpc-1, on which scales it is difficult to reach by using the cosmological observations.

DOI： 10.1103/PhysRevD.98.083518

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その他リンク： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.98.083518/fulltext

DOI： 10.1103/PhysRevLett.121.059901

PubMed

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D  

The Horndeski scalar-tensor theory and its recent extensions allow nonlinear derivative interactions of the scalar degree of freedom. We study the matter bispectrum of large scale structure as a probe of these modified gravity theories, focusing in particular on the effect of the terms that newly appear in the so-called "beyond Horndeski" theories. We derive the second-order solution for the matter density perturbations and find that the interactions beyond Horndeski lead to a new time-dependent coefficient in the second-order kernel which differs in general from the standard value of general relativity and the Horndeski theory. This can deform the matter bispectrum at the folded triangle configurations (k1+k2=k3), while it is never possible within the Horndeski theory.

DOI： 10.1103/PhysRevD.97.103517

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arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Institute of Physics Publishing  

It has been proposed that primordial black holes (PBHs) form binaries in the radiation dominated era. Once formed, some fraction of them may merge within the age of the universe by gravitational radiation reaction. We investigate the merger rate of the PBH binaries when the PBHs have a distribution of masses around O(10)M, which is a generalization of the previous studies where the PBHs are assumed to have the same mass. After deriving a formula for the merger time probability distribution in the PBH mass plane, we evaluate it under two different approximations. We identify a quantity constructed from the mass distribution of the merger rate density per unit cosmic time and comoving volume R(m1, m2), α = -(m1+ m2)2∂2 In R/∂m1∂m2, which universally satisfies 0.97≲α≲ 1.05 for all binary masses independently of the PBH mass function. This result suggests that the measurement of this quantity is useful for testing the PBH scenario.

DOI： 10.3847/1538-4357/aaa7f4

Scopus

arXiv

記述言語：英語   出版者・発行元：Institute of Physics Publishing  

This article reviews current understanding of primordial black holes (PBHs), with particular focus on those massive examples (≳1015 g) which remain at the present epoch, not having evaporated through Hawking radiation. With the detection of gravitational waves by LIGO, we have gained a completely novel observational tool to search for PBHs, complementary to those using electromagnetic waves. Taking the perspective that gravitational-wave astronomy will make significant progress in the coming decades, the purpose of this article is to give a comprehensive review covering a wide range of topics on PBHs. After discussing PBH formation, as well as several inflation models leading to PBH production, we summarize various existing and future observational constraints. We then present topics on formation of PBH binaries, gravitational waves from PBH binaries, and various observational tests of PBHs using gravitational waves.

DOI： 10.1088/1361-6382/aaa7b4

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arXiv

掲載種別：研究論文（学術雑誌）   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2018/02/053

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arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Monthly Notices of the Royal Astronomical Society: Letters  

We provide a new bound on the amplitude of primordial magnetic fields (PMFs) by using a novel mechanism, magnetic reheating. The damping of the magnetohydrodynamics fluid motions in a primordial plasma brings the dissipation of the PMFs. In the early Universe with z ≳ 2 × 106, cosmic microwave background (CMB) photons are quickly thermalized with the dissipated energy and shift to a different Planck distribution with a new temperature. In other words, the PMF dissipation changes the baryon-to-photon number ratio, and we name such a process magnetic reheating. From the current baryon-to-photon number ratio obtained from the big bang nucleosynthesis and CMB observations, we put the strongest constraint on the PMFs on small scales which CMB observations cannot access, B0 ≲ 1.0 μG at the scales 104 < k < 108 h Mpc-1.Moreover, when the PMF spectrum is given in a blue power-law type, the magnetic reheating puts a quite strong constraint, for example, B0 ≲ 10-17, 10-23, and 10-29 nG at 1 comoving Mpc for nB = 1.0, 2.0, and 3.0, respectively. This constraint would give an impact on generation mechanisms of PMFs in the early Universe.

DOI： 10.1093/mnrasl/slx195

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arXiv

掲載種別：研究論文（学術雑誌）   出版者・発行元：IOP Publishing  

We consider the inflationary universe with a spectator scalar field coupled
to a $U(1)$ gauge field and calculate curvature perturbation and gravitational
waves (GWs). We find that the sourced GWs can be larger than the one from
vacuum fluctuation and they are statistically anisotropic as well as linearly
polarized. The GW power spectrum acquires higher multipole moments as
$\mathcal{P}_h \propto (1-\cos^2\theta+\cos^4\theta-\cos^6\theta)$ irrespective
of the model parameters.

DOI： 10.1088/1475-7516/2018/07/023

arXiv

その他リンク： http://arxiv.org/pdf/1801.02778v1

出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.96.123516

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arXiv

その他リンク： http://arxiv.org/pdf/1709.03243v1

記述言語：英語   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We revisit the generation of dark matter isocurvature perturbations in the curvaton model in greater detail, both analytically and numerically. As concrete examples, we investigate the cases of thermally decoupled dark matter and axionic dark matter. We show that the radiation produced by the decay of the curvaton, which has not been taken into account in previous analytical studies, can significantly affect the amplitude of isocurvature perturbations. In particular, we find that they are drastically suppressed even when the dark matter freeze-out (or the onset of the axion oscillations for axionic dark matter) occurs before the curvaton decays, provided the freeze-out takes place deep in the curvaton-dominated Universe. As a consequence, we show that the current observational isocurvature constraints on the curvaton parameters are not as severe as usually thought.

DOI： 10.1088/1475-7516/2017/12/042

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arXiv

We present an impact of coupling between dark matter and a scalar field,
which might be responsible for dark energy, on measurements of redshift-space
distortions. We point out that, in the presence of conformal and/or disformal
coupling, linearized continuity and Euler equations for total matter fluid
significantly deviate from the standard ones even in the sub-horizon scales. In
such a case, a peculiar velocity of total matter field is determined not only
by a logarithmic time derivative of its density perturbation but also by
density perturbations for both dark matter and baryon, leading to a large
modification of the physical interpretation of observed data obtained by
measurements of redshift-space distortions. We reformulate galaxy two-point
correlation function in the redshift space based on the modified continuity and
Euler equations. We conclude from the resultant formula that the true value of
the linear growth rate of large-scale structure cannot be necessarily
constrained by single-redshift measurements of the redshift-space distortions,
unless one observes the actual time-evolution of structure.

DOI： 10.1093/pasj/psy083

arXiv

出版者・発行元：Monthly Notices of the Royal Astronomical Society  

DOI： 10.1093/mnras/stx530

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arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：OXFORD UNIV PRESS INC  

We estimate the spin distribution of primordial black holes based on the
recent study of the critical phenomena in the gravitational collapse of a
rotating radiation fluid. We find that primordial black holes are mostly slowly
rotating.

DOI： 10.1093/ptep/ptx087

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arXiv

その他リンク： http://arxiv.org/pdf/1704.06573v2

出版者・発行元：Publications of the Astronomical Society of Japan  

DOI： 10.1093/pasj/psw098

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arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：AMER PHYSICAL SOC  

We explore the use of galaxy bispectra with multitracer technique as a
possible probe of primordial non-Gaussianities. We forecast future constraints
on non-linearity parameters, $f_{\rm NL}^{\rm eq}$ and $f_{\rm NL}^{\rm orth}$,
which respectively characterize the equilateral- and orthogonal-types
primordial bispectra, and show that the multitracer analysis would be effective
with reducing the cosmic-variance noise if the number density of galaxies is
high enough. We find that the measurement of galaxy bispectrum by future galaxy
surveys can reach the constraints on the non-local type primordial
non-Gaussianities to the level severer than current one which has been obtained
by cosmic microwave background observations.

DOI： 10.1103/PhysRevD.95.063530

Web of Science

arXiv

出版者・発行元：Physical Review D  

DOI： 10.1103/PhysRevD.93.103537

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：AMER PHYSICAL SOC  

We investigate expected constraints on equilateral-type primordial
non-Gaussianities from future/ongoing imaging surveys, making use of the fact
that they enhance the halo/galaxy bispectrum on large scales. As model
parameters to be constrained, in addition to $f_{\rm NL}^{\rm equil}$, which is
related to the primordial bispectrum, we consider $g_{\rm NL}^{(\partial
\sigma)^4}$, which is related to the primordial trispectrum that appeared in
the effective field theory of inflation. After calculating the angular
bispectra of the halo/galaxy clustering and weak gravitational lensing based on
the integrated perturbation theory, we perform Fisher matrix analysis for three
representative surveys. We find that among the three surveys, the tightest
constraints come from Large Synoptic Survey Telescope ; its expected $1\sigma$
errors on $f_{\rm NL}^{\rm equil}$ and $g_{\rm NL}^{(\partial \sigma)^4}$ are
respectively given by $7.0 \times 10^2$ and $4.9 \times 10^7$. Although this
constraint is somewhat looser than the one from the current cosmic microwave
background observation, since we obtain it independently, we can use this
constraint as a cross check. We also evaluate the uncertainty with our results
caused by using several approximations and discuss the possibility to obtain
tighter constraint on $f_{\rm NL}^{\rm equil}$ and $g_{\rm NL}^{(\partial
\sigma)^4}$.

DOI： 10.1103/PhysRevD.94.043532

Web of Science

arXiv

出版者・発行元：Monthly Notices of the Royal Astronomical Society  

DOI： 10.1093/mnras/stw482

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：AMER PHYSICAL SOC  

The conventional slow-roll approximation is broken in the so-called "ultra
slow-roll" models of inflation, for which the inflaton potential is exactly (or
extremely) flat. The interesting nature of (canonical) ultra slow-roll
inflation is that the curvature perturbation grows on superhorizon scales, but
has a scale-invariant power spectrum. We study the ultra slow-roll inflationary
dynamics in the presence of non-canonical kinetic terms of the scalar field,
namely ultra slow-roll G-inflation. We compute the evolution of the curvature
perturbation and show that the primordial power spectrum follows a broken power
law with an oscillation feature. It is demonstrated that this could explain the
lack of large-scale power in the cosmic microwave background temperature
anisotropies. We also point out that the violation of the null energy condition
is prohibited in ultra slow-roll G-inflation and hence a blue tensor tilt is
impossible as long as inflation is driven by the potential. This statement is,
however, not true if the energy density is dominated by the kinetic energy of
the scalar field.

DOI： 10.1103/PhysRevD.94.103515

Web of Science

arXiv

記述言語：英語  

DOI： 10.1103/PhysRevLett.117.061101

Web of Science

PubMed

arXiv

記述言語：英語   出版者・発行元：Monthly Notices of the Royal Astronomical Society  

The redshifted 21cm line signal from neutral hydrogens is a promising tool to probe the cosmic dawn and the epoch of reionization. Ongoing and future low-frequency radio experiments are expected to detect its fluctuations, especially through the power spectrum. In this paper, we give a physical interpretation of the time evolution of the power spectrum of the 21cm brightness temperature fluctuations, which can be decomposed into dark matter density, spin temperature and neutral fraction of hydrogen fluctuations. From the one-point statistics of the fluctuations, such as variance and skewness, we find that the peaks and dips in the time evolution are deeply related to X-ray heating of the intergalactic gas, which controls the spin temperature. We suggest the skewness of the brightness temperature distribution is a key observable to identify the onset of X-ray heating.

DOI： 10.1093/mnras/stv965

Web of Science

Scopus

arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Physical Society  

Primordial black holes (PBHs) are theoretical black holes which can be formed during the radiation dominant era through the gravitational collapse of radiational overdensities. It has been well known that in the context of the structure formation in our Universe such collapsed objects, e.g., halos/galaxies, could be considered as bias tracers of underlying matter fluctuations and the halo/galaxy bias has been studied well. Applying such a biased tracer picture to PBHs, we investigate the large scale clustering of PBHs and obtain an almost mass-independent constraint to the scenario that the dark matter (DM) consists of PBHs. We focus on the case where the statistics of the primordial curvature perturbations is almost Gaussian, but with small local-type non-Gaussianity. If PBHs account for the DM abundance, such a large scale clustering of PBHs behaves as nothing but the matter isocurvature perturbation which is strictly constrained by the observations of cosmic microwave backgrounds (CMBs). From this constraint, we show that, in the case where a certain single field causes both CMB temperature perturbations and PBH formation, the PBH-DM scenario is excluded even with quite small local-type non-Gaussianity, |fNL|∼O(0.01).

DOI： 10.1103/PhysRevD.91.123534

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Physical Society  

We investigate the effect of equilateral-type primordial trispectrum on the halo/galaxy bispectrum. We consider three types of equilateral primordial trispectra which are generated by quartic operators naturally appearing in the effective field theory of inflation and can be characterized by three nonlinearity parameters, gNLσ4, gNLσ2(∂σ)2, and gNL(∂σ)4. Recently, constraints on these parameters have been investigated from Cosmic Microwave Background (CMB) observations by using WMAP9 data. In order to consider the halo/galaxy bispectrum with the equilateral-type primordial trispectra, we adopt the integrated perturbation theory in which the effects of primordial non-Gaussianity are wholly encapsulated in the linear primordial polyspectrum for the evaluation of the biased polyspectrum. We show the shapes of the halo/galaxy bispectrum with the equilateral-type primordial trispectra and find that the primordial trispectrum characterized by gNLσ4 provides the same scale dependence as the gravity-induced halo/galaxy bispectrum. Hence, it would be difficult to obtain the constraint on gNLσ4 from the observations of the halo/galaxy bispectrum. On the other hand, the primordial trispectra characterized by gNLσ2(∂σ)2 and gNL(∂σ)4 provide the common scale dependence which is different from that of the gravity-induced halo/galaxy bispectrum on large scales. Hence, future observations of the halo/galaxy bispectrum would give constraints on the nonlinearity parameters, gNLσ2(∂σ)2 and gNL(∂σ)4 independently from CMB observations.

DOI： 10.1103/PhysRevD.91.123521

Scopus

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We calculate the CMB $\mu$-distortion and the angular power spectrum of its
cross-correlation with the temperature anisotropy in the presence of the
non-Gaussian neutrino isocurvature density (NID) mode. While the pure Gaussian
NID perturbations give merely subdominant contribution to $<\mu>$ and vanishing
$< \mu T>$, the latter quantity can be large enough to be detected in the
future when the NID perturbations $\mathcal S(\mathbf x)$ are proportional to
the square of a Gaussian field $g(\mathbf x)$, i.e. $\mathcal S({\mathbf
x})\propto g^2({\mathbf x})$. In particular, large $< \mu T>$ can be realized
since Gaussian-squared perturbations can yield a relatively large bispectrum,
satisfying the constraints from the power spectrum of CMB anisotropies, i.e.
$\mathcal{P}_\mathcal{SS}(k_0) \sim\mathcal{P}_g^2(k_0)\lesssim10^{-10}$ at
$k_0=0.05$ Mpc$^{-1}$. We also forecast constraints from the CMB temperature
and E-mode polarisation bispectra, and show that
$\mathcal{P}_g(k_0)\lesssim10^{-5}$ would be allowed from Planck data. We find
that $< \mu >$ and $|l(l+1)C^{\mu T}_l|$ can respectively be as large as
$10^{-9}$ and $10^{-14}$ with uncorrelated scale-invariant NID perturbations
for $\mathcal{P}_g(k_0)=10^{-5}$. When the spectrum of the Gaussian field is
blue-tilted (with spectral index $n_g \simeq 1.5$), $< \mu T>$ can be enhanced
by an order of magnitude.

DOI： 10.1088/1475-7516/2015/03/013

Web of Science

arXiv

記述言語：英語   出版者・発行元：OXFORD UNIV PRESS INC  

We consider the possibility of enhancing the inflationary tensor mode by
introducing a spectator scalar field with a small sound speed which induces
gravitational waves as a second order effect. We analytically obtain the power
spectra of gravitational waves and curvature perturbation induced by the
spectator scalar field. We found that the small sound speed amplifies the
curvature perturbation much more than the tensor mode and the current
observational constraint forces the induced gravitational waves to be
negligible compared with those from the vacuum fluctuation during inflation.

DOI： 10.1093/ptep/ptv037

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/1411.3658v1

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

Although the cosmological paradigm based on cold dark matter and adiabatic, nearly scale-invariant primordial fluctuations is consistent with a wide variety of existing observations, it has yet to be sufficiently tested on scales smaller than those of massive galaxies, and various alternatives have been proposed that differ significantly in the consequent small-scale power spectrum (SSPS) of large-scale structure. Here we show that a powerful probe of the SSPS at k≳10Mpc-1 can be provided by the 21 cm forest, that is, systems of narrow absorption lines due to intervening, cold neutral hydrogen in the spectra of high-redshift background radio sources in the cosmic reionization epoch. Such features are expected to be caused predominantly by collapsed gas in starless minihalos, whose mass function can be very sensitive to the SSPS. As specific examples, we consider the effects of neutrino mass, running spectral index (RSI) and warm dark matter (WDM) on the SSPS, and evaluate the expected distribution in optical depth of 21 cm absorbers out to different redshifts. Within the current constraints on quantities such as the sum of neutrino masses -mν, running of the primordial spectral index dns/dlnk and WDM particle mass mWDM, the statistics of the 21 cm forest manifest observationally significant differences that become larger at higher redshifts. In particular, it may be possible to probe the range of mWDM≳10keV that may otherwise be difficult to access. Future observations of the 21 cm forest by the Square Kilometer Array may offer a unique and valuable probe of the SSPS, as long as radio sources such as quasars or Population III gamma-ray bursts with sufficient brightness and number exist at redshifts of z≳10-20, and the astrophysical effects of reionization and heating can be discriminated.

DOI： 10.1103/PhysRevD.90.083003

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

Matter isocurvature perturbations are strictly constrained from cosmic
microwave background observations. We study a sneutrino curvaton model where
both cold dark matter (CDM)/baryon isocurvature perturbations are generated. In
our model, total matter isocurvature perturbations are reduced since the
CDM/baryon isocurvature perturbations compensate for each other. We show that
this model can not only avoid the stringent observational constraints but also
suppress temperature anisotropies on large scales, which leads to improved
agreement with observations.

DOI： 10.1088/1475-7516/2014/10/068

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/1409.1669v1

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We study the impact of a temperature-dependent curvaton decay rate on the
primordial curvature perturbation generated in the curvaton scenario. Using the
familiar sudden decay approximation, we obtain an analytical expression for the
curvature perturbation after the decay of the curvaton. We then investigate
numerically the evolution of the background and of the perturbations during the
decay. We first show that the instantaneous transfer coefficient, related to
the curvaton energy fraction at the decay, can be extended into a more general
parameter, which depends on the net transfer of the curvaton energy into
radiation energy or, equivalently, on the total entropy ratio after the
complete curvaton decay. We then compute the curvature perturbation and compare
this result with the sudden decay approximation prediction.

DOI： 10.1088/1475-7516/2014/10/032

Web of Science

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We investigate constraints on the spectral index of primordial gravitational
waves (GWs), paying particular attention to a blue-tilted spectrum. Such
constraints can be used to test a certain class of models of the early
Universe. We investigate observational bounds from LIGO+Virgo, pulsar timing
and big bang nucleosynthesis, taking into account the suppression of the
amplitude at high frequencies due to reheating after inflation and also
late-time entropy production. Constraints on the spectral index are presented
by changing values of parameters such as reheating temperatures and the amount
of entropy produced at late time. We also consider constraints under the
general modeling approach which can approximately describe various scenarios of
the early Universe. We show that the constraints on the blue spectral tilt
strongly depend on the underlying assumption and, in some cases, a highly
blue-tilted spectrum can still be allowed.

DOI： 10.1088/1475-7516/2015/02/003

Web of Science

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We investigate the degeneracy of the isocurvature perturbations and the
primordial gravitational waves, by using recent observations of the cosmic
microwave background (CMB) reported by Planck and BICEP2 collaborations. We
show that the tension in the bound on the tensor-to-scalar ratio $r$ between
Planck and BICEP2 can be resolved by introducing the anti-correlated
isocurvature perturbations. Quantitatively, we find that with the
anti-correlated isocurvature perturbations the constraints on $r$ from Planck
alone and BICEP2 results can be consistent at 68 % C.L.

DOI： 10.1088/1475-7516/2014/08/043

Web of Science

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We comprehensively explore the quadratic curvaton models in the chaotic
inflation. In the light of the BICEP2 result $r \approx 0.2$, all model
parameters and relevant observables are computed. It is found the curvaton
field value is constrained into a narrow range, $\sigma_* =
\mathcal{O}(10^{-2}$-$10^{-1})$ and the running of the spectral index is $n_s'
\gtrsim -10^{-3}$. We show that if the curvaton is added, the models are
heavily degenerated on the $n_s$ - $r$ plane. However, introducing a new plane,
the degeneracy can be resolved. To distinguish the curvaton models, precise
measurements of not only $r$ but also $n_s'$ and the tensor tilt $n_T$ are
required.

DOI： 10.1088/1475-7516/2014/09/015

Web of Science

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

Recently, BICEP2 has reported the large tensor-to-scalar ratio
$r=0.2^{+0.07}_{-0.05}$ from the observation of the cosmic microwave background
(CMB) B-mode at degree-scales. Since tensor modes induce not only CMB B-mode
but also the temperature fluctuations on large scales, to realize the
consistent temperature fluctuations with the Planck result we should consider
suppression of scalar perturbations on corresponding large scales. To realize
such a suppression, we consider anti-correlated iso-curvature perturbations
which could be realized in the simple curvaton model.

DOI： 10.1088/1475-7516/2014/05/046

Web of Science

arXiv

出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.89.063508

Web of Science

Scopus

arXiv

出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.89.043524

Scopus

DOI： 10.1103/PhysRevD.89.043524

Web of Science

記述言語：英語   掲載種別：研究論文（学術雑誌）  

We derive a formula for the halo/galaxy bispectrum on the basis of the integrated perturbation theory (iPT). In addition to the gravity-induced non-Gaussianity, we consider the non-Gaussianity of the primordial curvature perturbations and investigate in detail the effect of such primordial non-Gaussianity on the large-scale halo/galaxy bispectrum. In iPT, the effects of primordial non-Gaussianity are wholly encapsulated in the linear (primordial) polyspectra, and we systematically calculate the contributions to the large-scale behaviors arising from the three types of primordial bispectrum (local, equilateral, and orthogonal types), and primordial trispectrum of the local-type non-Gaussianity. We find that the equilateral- and orthogonal-type non-Gaussianities show distinct scale-dependent behaviors which can dominate the gravity-induced non-Gaussianity at very large scales. For the local-type non-Gaussianity, higher-order loop corrections are found to give a significantly large contribution to the halo/galaxy bispectrum of the squeezed shape and eventually dominate over the other contributions on large scales. A diagrammatic approach based on the iPT helps us to systematically investigate an impact of such higher-order contributions to the large-scale halo/galaxy bispectrum. © 2014 American Physical Society.

DOI： 10.1103/PhysRevD.89.043524

Scopus

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

Recently, there are several reports that the cosmic magnetic fields on Mpc
scale in void region is larger than $\sim 10^{-15}$G with an uncertainty of a
few orders from the current blazar observations. On the other hand, in
inflationary magnetogenesis models, additional primordial curvature
perturbations are inevitably produced from iso-curvature perturbations due to
generated electromagnetic fields. We explore such induced curvature
perturbations in a model independent way and obtained a severe upper bound for
the energy scale of inflation from the observed cosmic magnetic fields and the
observed amplitude of the curvature perturbation, as $\rho_{\rm inf}^{1/4} <
30{\rm GeV} \times (B_{\rm obs}/10^{-15}{\rm G})^{-1}$ where $B_{\rm obs}$ is
the strength of the magnetic field at present. Therefore, without a dedicated
low energy inflation model or an additional amplification of magnetic fields
after inflation, inflationary magnetogenesis on Mpc scale is generally
incompatible with CMB observations.

DOI： 10.1088/1475-7516/2014/03/013

Web of Science

arXiv

掲載種別：研究論文（国際会議プロシーディングス）   出版者・発行元：Journal of Physics: Conference Series  

DOI： 10.1088/1742-6596/485/1/012023

Web of Science

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Institute of Physics Publishing  

DOI： 10.1088/1475-7516/2014/05/E02

Scopus

記述言語：英語   出版者・発行元：AMER PHYSICAL SOC  

We derive a formula for the halo/galaxy bispectrum on the basis of the
integrated Perturbation Theory (iPT). In addition to the gravity-induced
non-Gaussianity, we consider the non-Gaussianity of the primordial curvature
perturbations, and investigate in detail the effect of such primordial
non-Gaussianity on the large-scale halo/galaxy bispectrum. In iPT, the effects
of primordial non-Gaussianity are wholly encapsulated in the linear
(primordial) polyspectra, and we systematically calculate the contributions to
the large-scale behaviors arising from the three types of primordial bispectrum
(local-, equilateral-, and orthogonal-types), and primordial trispectrum of the
local-type non-Gaussianity. We find that the equilateral- and orthogonal-type
non-Gaussianities show distinct scale-dependent behaviors which can dominate
the gravity-induced non-Gaussianity at very large scales. For the local-type
non-Gaussianity, higher-order loop corrections are found to give a
significantly large contribution to the halo/galaxy bispectrum of the squeezed
shape, and eventually dominate over the other contributions on large scales. A
diagrammatic approach based on the iPT helps us to systematically investigate
an impact of such higher-order contributions to the large-scale halo/galaxy
bispectrum.

DOI： 10.1103/PhysRevD.89.043524

Web of Science

arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）  

We compute the power spectrum ζ and non-linear parameters fNL and τNL of the curvature perturbation induced during inflation by the electromagnetic fields in the kinetic coupling model (IFF model). By using the observational result of ζ,fNL and τNL reported by the Planck collaboration, we study the constraint on the model comprehensively. Interestingly, if the single slow-rolling inflaton is responsible for the observed ζ, the constraint from τNL is most stringent. We also find a general relationship between fNL and τNL generated in this model. Even if fNL ∼ (1), a detectable τNL can be produced. © 2013 IOP Publishing Ltd and Sissa Medialab srl.

DOI： 10.1088/1475-7516/2013/09/009

Scopus

arXiv

出版者・発行元：Monthly Notices of the Royal Astronomical Society  

Anisotropic stress perturbations induced by primordial Gaussian vector fields create non- Gaussianity in curvature perturbations.We found that such non-Gaussianity closely resembles the local-type non-Gaussianity parametrized by fNL, and generates scale-dependent bias in large-scale structures. We also found a simple relationship between the scale-dependent bias and the power spectrum of the vector fields.When the vector fields are interpreted as primordial magnetic fields, the effective fNL is shown to be always negative. The scale-dependent bias provides a new approach to probing primordial vector fields. © 2013 The Author. Published by Oxford University Press on behalf of the Royal Astronomical Society.

DOI： 10.1093/mnras/stt594

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We investigate the gravitational wave background induced by the first order
scalar perturbations in the curvaton models. We consider the quadratic and
axion-like curvaton potential which can generate the blue-tilted power spectrum
of curvature perturbations on small scales and derive the maximal amount of
gravitational wave background today. We find the power spectrum of the induced
gravitational wave background has a characteristic peak at the frequency
corresponding to the scale reentering the horizon at the curvaton decay, in the
case where the curvaton does not dominate the energy density of the Universe.
We also find the enhancement of the amount of the gravitational waves in the
case where the curvaton dominates the energy density of the Universe. Such
induced gravitational waves would be detectable by the future space-based
gravitational wave detectors or pulsar timing observations.

DOI： 10.1088/1475-7516/2013/08/042

Web of Science

arXiv

出版者・発行元：Progress of Theoretical and Experimental Physics  

DOI： 10.1093/ptep/ptt031

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We discuss implications of Planck results for models with local type
non-Gaussianity. In light of the recent results of the Planck satellite, we
constrain model parameters of several representative models and give the
prediction of trispectrum, in particular, gNL. We also consider interesting
possibilities that trispectrum appears as the first signature of the
non-Gaussianities of the curvature perturbations, that is, fNL is small while
gNL can be significantly large.

DOI： 10.1088/1475-7516/2013/06/012

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/1303.5374v3

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We provide a general formula for calculating correlators of arbitrary
function of a Gaussian field. This work extends the standard leading-order
approximation based on the delta N formalism to the case where truncation of
the delta N at some low order does not yield the correct answer. As an
application of this formula, we investigate 2, 3 and 4-point functions of the
primordial curvature perturbation generated in the massless preheating model by
approximating the mapping between the curvature perturbation and the Gaussian
field as a sum of the many spiky normal distribution functions as suggested by
lattice calculations. We also discuss observational consequences of this case
and show that trispectrum would be a key observable to search signature of
preheating in the CMB map. It is found the forms of the curvature correlation
functions for any delta N, at the leading order in the correlator of the
Gaussian field, coincide with the standard local type ones. Within this
approximation, it is also found that the standard formula for the non-linearity
parameters given by the product of the derivatives of the e-folding number
still holds after we replace the bare e-folding number appearing in the
original delta N expansion with the one smoothed in the field space with a
Gaussian window function.

DOI： 10.1088/1475-7516/2013/06/018

Web of Science

arXiv

記述言語：英語   出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

We analytically derive a more accurate formula for the power spectrum of the biased objects with the primordial non-Gaussianity parametrized not only by the nonlinearity parameter fNL, but also by gNL and τNL which characterize the trispectrum of the primordial curvature perturbations. We adopt the integrated perturbation theory which was constructed in Matsubara. We discuss an inequality between fNL and τNL in the context of the scale-dependent bias, by introducing a stochasticity parameter. We also mention higher order loop corrections in the scale dependency of the bias parameter. © 2013 American Physical Society.

DOI： 10.1103/PhysRevD.87.023525

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1210.2495v1

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2012/11/046

Web of Science

Scopus

arXiv

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We investigate bounds on the strength of the primordial magnetic field (PMF) from the cosmic microwave background (CMB) bispectra of the intensity (temperature) modes induced from the auto- and cross-correlated bispectra of the scalar and tensor components of the PMF anisotropic stress. At first, we construct a general formula for the CMB intensity and polarization bispectra from PMFs composed of any type of perturbation. Then we derive an approximate expression which traces the exact shape of the CMB bispectrum in order to reduce the computation time with respect to a large number of the multipole configurations, and also show that the non-Gaussian structure coming from PMFs is classified as the local-type configuration. Computing the signal-to-noise ratio on the basis of the approximate formula with the information of the instrumental noises and resolutions, we find expected upper bounds on the magnetic field strength, when the magnetic spectrum is nearly scale invariant (nB = -2.9), smoothed on 1Mpc scale at 95% confidence level from the WMAP and PLANCK experiments as B1Mpc < 4.0-6.7nG and 3.8-6.5nG, respectively, depending on the energy scale of the magnetic field production from 1014GeV to 103GeV. Our new consequences imply slight overestimations by the previous rough discussions.©2012 IOP Publishing Ltd and Sissa Medialab srl.

DOI： 10.1088/1475-7516/2012/03/041

Web of Science

Scopus

arXiv

記述言語：英語  

出版者・発行元：Progress of Theoretical Physics Supplement  

We discuss generation of non-Gaussianity in primordial density perturbation through the super-horizon evolution during inflation by using the so-called δN formalism. In order to discuss the difficulties of generating large local-type non-Gaussianity during inflation, we discuss Kadota-Stewart model. This model gives an example in which we have to choose rather unnatural initial conditions even if large non-Gaussianity can be generated.

Scopus

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2011/12/008

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We investigate the halo bias in the case where the primordial curvature fluctuations, Φ, are sourced from both a Gaussian random field and a Gaussian-squared field, as Φ(x) = φ(x)+ψ(x)2-ψ(x) 2ngle, so-called "ungaussiton model". We employ the peak-background split formula and find a new scale-dependence in the halo bias induced from the Gaussian-squared field. © 2011 IOP Publishing Ltd and SISSA.

DOI： 10.1088/1475-7516/2011/11/001

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1108.5569v1

Web of Science

Web of Science

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Progress of Theoretical Physics  

We investigate the cosmic microwave background (CMB) bispectra of the intensity (temperature) and polarization modes induced by the graviton non-Gaussianities, which arise from the parity-conserving and parity-violating Weyl cubic terms with time-dependent coupling. By considering the time-dependent coupling, we find that even in the exact de Sitter space time, the parity violation still appears in the three-point function of the primordial gravitational waves and could become large. Through the estimation of the CMB bispectra, we demonstrate that the signals generated from the parity-conserving and parity-violating terms appear in completely different configurations of multipoles. For example, the parity-conserving non-Gaussianity induces the nonzero CMB temperature bispectrum in the configuration with Σ_<n=1>^3l_n=even and, while due to the parity-violating non-Gaussianity, the CMB temperature bispectrum also appears for Σ_<n=1>^3l_n=odd. This signal is just good evidence of the parity violation in the non-Gaussianity of primordial gravitational waves. We find that the shape of this non-Gaussianity is similar to the so-called equilateral one and the amplitudes of these spectra at large scale are roughly estimated as |b_<lll>|～l^<-4>×3.2×10^<-2>(GeV/Λ)^2 (r/0.1)^4, where Λ is an energy scale that sets the magnitude of the Weyl cubic terms (higher derivative corrections) and r is a tensor-to-scalar ratio. Taking the limit for the nonlinearity parameter of the equilateral type as f_<NL>^<eq><300, we can obtain a bound as Λ&gsum;3×10^6GeV, assuming r=0.1.

DOI： 10.1143/PTP.126.937

Scopus

arXiv

出版者・発行元：Publication Office, Progress of Theoretical Physics  

We discuss generation of non-Gaussianity in primordial density perturbation through the super-horizon evolution during inflation by using the so-called δN formalism. In order to discuss the difficulties of generating large local-type non-Gaussianity during inflation, we discuss Kadota-Stewart model. This model gives an example in which we have to choose rather unnatural initial conditions even if large non-Gaussianity can be generated.

DOI： 10.1143/PTPS.190.135

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Monthly Notices of the Royal Astronomical Society: Letters  

We study the scale-dependent bias of the halo power spectrum arising from primordial non-Gaussianity. We present an analytic result of the halo bias including up to the trispectrum contributions. We find that the scale-dependent bias opens a new possibility of probing the relation between the non-linearity parametersfNL and τNL. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

DOI： 10.1111/j.1745-3933.2011.01124.x

Web of Science

Scopus

記述言語：英語   出版者・発行元：Monthly Notices of the Royal Astronomical Society  

We study the halo mass function in the presence of a kurtosis type of primordial non-Gaussianity. The kurtosis corresponds to the trispectrum as defined in Fourier space. The primordial trispectrum is commonly characterized by two parameters, τNL and gNL. We focus on τNL which is an important parameter to test the physics of multifield inflation models. As applications of the derived non-Gaussian mass function, we consider the effects on the abundance of void structure, on early star formation and on formation of the most massive objects at high redshift. We show that by comparing the effects of primordial non-Gaussianity on cluster abundance with that on void abundance, we can distinguish between the skewness and the kurtosis types of primordial non-Gaussianity. As for early star formation, we show that the kurtosis type of primordial non-Gaussianity seems on the average not to affect the reionization history of the Universe. However, at high redshifts (up to z≃ 20) such non-Gaussianity does somewhat affect the early stages of reionization. © 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS.

DOI： 10.1111/j.1365-2966.2011.19323.x

Web of Science

Scopus

arXiv

出版者・発行元：Progress of Theoretical Physics  

We investigate a statistical anisotropy on the Cosmic Microwave Background (CMB) bispectrum, which can be generated from the primordial non-Gaussianity induced by quantum fluctuations of a vector field. We find new configurations in the multipole space of the CMB bispectrum given by l_1=l_2+l_3+2,|l_2-l_3|-2 and their permutations, which violate the rotational invariance, such as an off-diagonal configuration in the CMB power spectrum. We also find that in a model presented by Yokoyama and Soda (2008), the amplitude of the statistically anisotropic bispectrum in the above configurations becomes as large as that in other configurations such as l_1=l_2+l_3. As a result, it might be possible to detect these contributions in future experiments, which would give us novel information about the physics of the early Universe.

DOI： 10.1143/PTP.126.923

Web of Science

Scopus

arXiv

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2011/07/033

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1105.5851v2

出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.83.123523

Web of Science

Scopus

arXiv

掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.83.123003

Web of Science

Scopus

arXiv

Web of Science

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2011/01/027

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1008.1450v2

Web of Science

記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1103/PHYSREVD.83.029901

Web of Science

記述言語：英語  

出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.82.121302

Web of Science

Scopus

出版者・発行元：Progress of Theoretical Physics  

We present an all-sky formalism for the Cosmic Microwave Background (CMB) bispectrum induced by the primordial non-Gaussianities not only in scalar but also in vector and tensor fluctuations. We find that the bispectrum can be formed in an explicitly rationally invariant way by taking into account the angular and polarization dependences of the vector and tensor modes. To demonstrate this and present how to use our formalism, we consider a specific example of the correlation between two scalars and a graviton as the source of non-Gaussianity. As a result, we show that the CMB reduced bispectrum of the intensity anisotropies is evaluated as a function of the multipole and the coupling constant between two scalars and a graviton denoted by g_<tss>; |b_<lll>|～l^<-4>×8×10^<-18>|g_<tss>|. By estimating the signal-to-noise ratio, we find that the constraint as |g_<tss>|<6 will be expected from the PLANCK experiment.

DOI： 10.1143/PTP.125.795

Web of Science

Scopus

arXiv

出版者・発行元：Proceedings of the 20th Workshop on General Relativity and Gravitation in Japan, JGRG 2010  

Scopus

記述言語：英語   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We classify models generating large local-type non-Gaussianity into some categories by using some "consistency relations" among the non-linearity parameters fnllocalτnLlocal and gNLlocal, which characterize the size of bispectrum for the former and trispectrum for the latter two. Then we discuss how one can discriminate models of large local-type non-Gaussianity with such relations. We first classify the models by using the ratio of T NLlocal/(6fNLlocal/5)2, which is unity for "single-source" models and deviates from unity for "multi-source" ones. We can make a further classification of models in each category by utilizing the relation between fNLlocal and Gnllocal. Our classification suggests that observations of trispectrum would be very helpful to distinguish models of large non-Gaussianity and may reveal the generation mechanism of primordial fluctuations. © 2010 IOP Publishing Ltd and SISSA.

DOI： 10.1088/1475-7516/2010/12/030

Web of Science

Scopus

arXiv

出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

DOI： 10.1103/PhysRevD.82.103505

Web of Science

Scopus

arXiv

出版者・発行元：Physical Review Letters  

DOI： 10.1103/PhysRevLett.105.121301

Web of Science

Scopus

PubMed

arXiv

記述言語：英語  

DOI： 10.1088/0264-9381/27/12/124003

Web of Science

arXiv

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2010/05/007

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：Journal of Physics: Conference Series  

In this talk, we have shown that current cosmic acceleration can be explained by an almost massless scalar field experiencing quantum fluctuations during primordial inflation. Provided its mass does not exceed the Hubble parameter today, this field has been frozen during the cosmological ages to start dominating the universe only recently. By using supernovae data, completed with baryonic acoustic oscillations from galaxy surveys and cosmic microwave background anisotropies, we infer the energy scale of primordial inflation to be around a few TeV, which implies a negligible tensor-to-scalar ratio of the primordial fluctuations. Moreover, our model suggests that inflation lasted for an extremely long period. Dark energy could therefore be a natural consequence of cosmic inflation close to the electroweak energy scale. © 2010 IOP Publishing Ltd.

DOI： 10.1088/1742-6596/259/1/012082

Web of Science

Scopus

掲載種別：研究論文（国際会議プロシーディングス）  

We calculate CMB bispectrum of vector modes induced from primordial magnetic fields. We take into account the full angular dependence of the bispectrum and discuss the amplitude and also the shape of the bispectrum. In the squeezed limit, we estimate a typical values of the normalized reduced bispectrum as ℓ11(ℓ1+1) ℓ3(ℓ 3+1) |bℓ1ℓ2ℓ3|∼2 × 10 -19, for the strength of the primordial magnetic field smoothed on 1Mpc scale B1Mpc = 4.7nG assuming nearly scale-invariant spectrum of magnetic fields. We find that a new constraint on the magnetic field strength will be placed as B1Mpc < 10nG if PLANCK will place a limit on the nonlinearity parameter of local-type configuration as |flocalNL | < 5.

Scopus

出版者・発行元：Proceedings of the 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009  

Scopus

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2009/12/012

Web of Science

Scopus

arXiv

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Physical Review D - Particles, Fields, Gravitation and Cosmology  

We investigate primordial non-Gaussianity and dark matter isocurvature fluctuations in the modulated reheating and the curvaton scenarios. In these scenarios, a large non-Gaussianity can be generated; on the other hand, depending on how dark matter is produced, too large isocurvature fluctuations can also arise, which is inconsistent with current observations. In this paper, we study this issue in a mixed scenario where the curvature fluctuations can also be produced from the inflaton fluctuations as well as those from a light scalar field such as the modulus and the curvaton. We show that primordial fluctuations can be highly non-Gaussian without conflicting with the current constraint on isocurvature fluctuations for such mixed scenarios. However, if the constraint on isocurvature fluctuations becomes severer as expected by the Planck satellite, fNL, a nonlinearity parameter for adiabatic fluctuations, should be very small as fNL3, which would give interesting implications for the generation mechanism of dark matter. Non-Gaussianity from isocurvature fluctuations is also discussed in these scenarios. © 2009 The American Physical Society.

DOI： 10.1103/PhysRevD.80.063524

Web of Science

Scopus

記述言語：英語   出版者・発行元：Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics  

We show that, assuming the dispersion relation proposed recently by Hořava in the context of quantum gravity, radiation energy density exhibits a peculiar dependence on the scale factor; the radiation energy density decreases proportional to a-6. This simple scaling can have an impact on cosmology. As an example, we show that the resultant baryon asymmetry as well as the stochastic gravity waves can be enhanced. We also discuss current observational constraint on the dispersion relation. © 2009 Elsevier B.V. All rights reserved.

DOI： 10.1016/j.physletb.2009.07.005

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/0905.0055v2

出版者・発行元：Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics  

DOI： 10.1016/j.physletb.2009.06.007

Web of Science

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/0905.0240v2

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2009/05/004

Web of Science

Scopus

arXiv

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2009/02/012

Web of Science

Scopus

arXiv

出版者・発行元：Proceedings of the 18th Workshop on General Relativity and Gravitation in Japan, JGRG 2008  

Scopus

出版者・発行元：Journal of Cosmology and Astroparticle Physics  

DOI： 10.1088/1475-7516/2008/08/034

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：Journal of Cosmology and Astroparticle Physics  

We present a new mechanism for generating primordial statistical anisotropy of curvature perturbations. We introduce a vector field which has a non-minimal kinetic term and couples with a waterfall field in a hybrid inflation model. In such a system, the vector field gives fluctuations of the end of inflation and hence induces a subcomponent of curvature perturbations. Since the vector has a preferred direction, the statistical anisotropy could appear in the fluctuations. We present the explicit formula for the statistical anisotropy in the primordial power spectrum and the bispectrum of curvature perturbations. Interestingly, there is the possibility that the statistical anisotropy does not appear in the power spectrum but does appear in the bispectrum. We also find that the statistical anisotropy provides the shape dependence to the bispectrum. © 2008 IOP Publishing Ltd. and SISSA.

DOI： 10.1088/1475-7516/2008/08/005

Web of Science

Scopus

arXiv

記述言語：英語   出版者・発行元：AMER PHYSICAL SOC  

We give a concise formula for the non-Gaussianity of the primordial curvature
perturbation generated on super-horizon scales in multi-scalar inflation model
without assuming slow-roll conditions. This is an extension of our previous
work. Using this formula, we study the generation of non-Gaussianity for the
double inflation models in which the slow-roll conditions are temporarily
violated after horizon exit, and we show that the non-linear parameter $f_{NL}$
for such models is suppressed by the slow-roll parameters evaluated at the time
of horizon exit.

DOI： 10.1103/PhysRevD.77.083511

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/0711.2920v3

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We analyze the non-Gaussianity for primordial curvature perturbations
generated in multi-scalar slow-roll inflation model including the model with
non-separable potential by making use of $\delta N$ formalism. Many authors
have investigated the possibility of large non-Gaussianity for the models with
separable potential, and they have found that the non-linear parameter,
$f_{NL}$, is suppressed by the slow-roll parameters. We show that for the
non-separable models $f_{NL}$ is given by the product of a factor which is
suppressed by the slow-roll parameters and a possible enhancement factor which
is given by exponentials of quantities of O(1).

DOI： 10.1088/1475-7516/2007/07/013

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/0705.3178v1

記述言語：英語  

We show that the primordial curvature perturbations may originate not from
the quantum fluctuations of inflaton during inflation but from isocurvature
perturbations which are amplified during preheating after inflation. We
consider a simple preheating model, whose potential is given by $V(\phi,
\chi)={1/4}\lambda \phi^4+{1/2}g^2 \phi^2 \chi^2$ with $g^2/\lambda=2$, as a
possible realization of generating curvature perturbations during preheating.
We make use of the $\delta N$ formalism which requires only knowledge of the
homogeneous background solutions in order to evaluate the evolution of
curvature perturbations on super-horizon scales. We solve the background
equations numerically and find that the amplitude and the spectral index of
curvature perturbations originating from preheating can be tuned to the
observed values if the isocurvature perturbations at the end of inflation is
not suppressed on super-horizon scales. We also point out that the tensor to
scalar ratio in ${1/4}\lambda \phi^4$ inflation model can be significantly
lowered, hence letting the ${1/4}\lambda \phi^4$ model, which is ruled out by
the Wilkinson Microwave Anisotropy Probe (WMAP) data combined with SDSS data,
get back into the observationally allowed region.

DOI： 10.1088/0264-9381/24/6/015

arXiv

その他リンク： http://arxiv.org/pdf/astro-ph/0606228v2

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

We present a new formulation for the evaluation of the primordial spectrum of
curvature perturbations generated during inflation, using the fact that the
Wronskian of the scalar field perturbation equation is constant. In the
literature, there are many works on the same issue focusing on a few specific
aspects or effects. Here we deal with the general multi-component scalar field,
and show that our new formalism gives a method to evaluate the final amplitude
of the curvature perturbation systematically and economically. The advantage of
the new method is that one only has to solve a single mode of the scalar field
perturbation equation backward in time from the end of inflation to the stage
at which the perturbation is within the Hubble horizon, at which the initial
values of the scalar field perturbations are given. We also clarify the
relation of the new method with the new delta N formalism recently developed in
Lee et al.(2005).

DOI： 10.1088/1475-7516/2006/06/020

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/astro-ph/0605021v2

記述言語：英語   出版者・発行元：IOP PUBLISHING LTD  

The delta N formula that relates the final curvature perturbation on comoving
slices to the inflaton perturbation on flat slices after horizon crossing is a
powerful and intuitive tool to compute the curvature perturbation spectrum from
inflation. However, it is customarily assumed further that the conventional
slow-roll condition is satisfied, and satisfied by all components, during
horizon crossing. In this paper, we develop a new delta N formalism for
multi-component inflation that can be applied in the most general situations.
This allows us to generalize the idea of general slow-roll inflation to the
multi-component case, in particular only applying the general slow-roll
condition to the relevant component. We compute the power spectrum of the
curvature perturbation in multi-component general slow-roll inflation, and find
that under quite general conditions it is invertible.

DOI： 10.1088/1475-7516/2005/10/004

Web of Science

arXiv

その他リンク： http://arxiv.org/pdf/astro-ph/0506262v2

開催年月日： 2020年11月

記述言語：英語   会議種別：ポスター発表  

国名：日本国