Cセミナー 2019

English

## 今後のセミナー

4月 | 5月 | 6月 | 7月 | 8月 | 9月 | 10月 | 11月 | 12月 | 1月 | 2月 | 3月

＊プレゼンテーションファイルは研究室内部ネットワークのみで閲覧可能です。

## 2月のセミナー

2月5日(水)13:00- @ES606

Non-linear effects during inflation can generate primordial non-Gaussianities(NG). Arkani-Hamed & Maldacena showed that an interaction between the inflaton and higher spin($s\geq2$) fields, which may be predicted in string theory, can generate angular dependent NG. As was argued by Schmidt et al., this anisotropy can be explored by observing galaxy alignments. In our previous work, we studied the closer to case massive spin-2 angular PNG. This result revealed that the imprint of PNG appears in small-scale. As our new idea, we propose higher moment of galaxy shape to probe PNG with higher spin. In particular, I will talk about the relation between the galaxy moment and the PNG from massive spin-4 particles.

## 1月のセミナー

1月22日(水)13:00- @ES606

At present, a widely used method for obtaining information of initial density fluctuation information from the analysis of large-scale structure is the calculation of two-point statistics of density fluctuation. Multi (three or more)-point statistics have additional cosmological information, but its calculation is very difficult. Therefore this study tried to obtain information from higher-order statistics using a convolutional neural network (CNN), a machine learning method. In this work, CNN is trained by using images generated from N-body simulation assuming cold dark matter (CDM) or warm dark matter (WDM), and CNN classifies images as CDM or WDM image. In this talk, we will discuss the details of the method and compare result of classification by CNN with by 2pt-correlation.

1月15日(水)11:00- @ES606

The growth of spike primordial curvature power spectrum leads to form the compact structure, ultracompact minihalos (UCMHs) after the matter-radiation equality. Since UCMHs’ abundance closely relate to the primordial power, if we constraint the UCMHs’ abundance using the observation, we obtain the constraint of the primordial power. Particularly, this method can give a powerful constraint from sub-Mpc scale to pc scale. In this seminar, we discuss the constraint of the primordial curvature power spectrum through the constraint of UCMHs’ abundance using the 21-cm line and CMB Lensing. If I have a time, we also report the future work.

1月15日(水)11:00- @ES606

Non-perturbative analysis of the QCD phase transition using lattice QCD reveals that the equation of state parameter and the sound speed change with time during the QCD phase transition. This changes the behavior of the gravitational potential. As a result, the secondary gravitational waves generated by the spatial fluctuation of the gravitational potential is also affected, so the trace of the QCD phase transition can be obtained. Therefore, in this study, we calculate the effect of changing the equation of state parameters on the secondary gravitational wave signal. This is expected to limit future observations and provide verification for the QCD phase transition. In this presentation, we will show that the traces of the QCD phase transition appear in the gravitational wave signal.

1月8日(水)13:00- @ES606

Galaxy clusters are important objects to search the universe. The relation between cluster mass and richness is predicted theoretically as a function of the cosmological model. Therefore, finding many clusters by observation and estimating their mass is very important because it can limit the cosmological model through the mass function. One of the methods to identify mass accurately is the weak gravity lens effect. In general, mass estimation using the weak-gravity lens effect uses a galaxy cluster as a background light source. On the other hand, using cosmic microwave background (CMB) from the final scattering surface as background light, the mass of high-z clusters can be estimated. In this presentation, I will introduce our previous research using the SDSS galaxy cluster catalog(z<0.6) and Planck lensing map.Next, the results of analysis using the HSC CAMIRA catalog (z <1.0), Planck map, and ACTpol are reported.

1月8日(水)13:00- @ES606

The effect of Cosmic Microwave Background (CMB) gravitational lensing is the phenomenon that primordial CMB is distorted by gravity between Last Scattering Surface and us. From the effect we can obtain information on matter distribution and primordial gravitational waves. The Quadratic Estimator method has been used to detect the lensing effect. Since the lensing effect produces the lensing B-mode from the primordial E-mode, planned B-mode experiments from ground and space, such as Simons Observatory and LiteBird, will significantly enhance the sensitivity of the lensing effect. In this talk, I will review the Quadratic Estimator method (Okamoto & Hu, PRD, 2003), and the combined analysis of the South Pole Telescope with Planck data (Omori et al., ApJ, 2017) as a reference for a future analysis using combined Simons Observatory and LiteBird data sets.

## 12月のセミナー

12月11日(水)13:00- @ES606

Indirect searches for dark matter (DM) annihilation signals have been traditionally carried out in a number of target regions such as the Galactic Center and Milky Way dwarf spheroidal galaxies (dSphs). Here, we propose low surface brightness galaxies (LSBGs) as novel targets for the indirect detection of DM emission. In particular, LSBGs are known to have very large DM contents and be less contaminated by extragalactic gamma-ray sources (e.g., blazars) compared to star forming galaxies or ordinally galaxies. In this analysis, we use eight LSBGs (detected by Subaru Hyper Suprime-Cam survey data) with known redshifts to conduct a search for gamma-ray emission at the positions of these new objects in Fermi Large Area Telescope data. We found no excesses of gamma-ray emission and set constraints on the dark matter annihilation cross-section. We provide a upper limit on the cross section to ~10^-23 [cm^3/s] at the 95\% C.L. for DM mass of 10 GeV for the b_b channel. Although, this constraint is fairly weaker than the ones reported in recent studies using other targets, we note that in the near future, the number of detections of new LSBGs will increase by a few orders of magnitude. We show that the constraint with LSBGs in future observations can be stronger three orders of magnitudes than one with our eight LSBGs.

## 11月のセミナー

11月27日(水)13:00- @ES606

To constrain the cosmological model from observations such as cosmic microwave background or the large-scale structure of the universe, the power spectrum or the two-point correlation function of the fluctuations have been frequently used to compare theoretical models to observations.
In this talk, I propose a novel method to constrain cosmological models using normality tests, under the assumption that the underlying density fluctuations are initially Gaussian distributed. My method is based on the D’Agostino’s K-squared tests, and enables us to estimate the growth factors and initial density fluctuations simultaneously. I demonstrate that the method can successfully recover the input growth factors using a simple random Gaussian field and N-body simulations.

11月27日(水)13:00- @ES606

Cosmological N-body simulations based on the Lambda-dominated, cold dark matter structure formation model predict that the large-scale structure of the Universe looks like “cosmic web” which consists of dark matter halos connected through the filamentary structure. The dark matter distribution within dark matter halos has been extensively studied by weak gravitational lensing, but lensing by filamentary structure is not explored enough yet.
In this seminar, I report the weak lensing measurement of filaments between pairs of SDSS BOSS galaxies to higher redshift (z~0.5) with the Subaru Hyper Supreme-Cam (HSC) Subaru Strategic Program (SSP) first year data. Also, we derive a theoretical prediction and covariance using mock catalogs based on full-sky ray-tracing simulations.
We will show the comparison to the measurement with the theoretical prediction by mock simulations.

11月20日(水)13:00- @ES606

Primordial black hole (PBH) is a black hole that is formed by the gravitational collapse of the overdensity region in the early universe. If PBHs exist, it is suggested that they play a lot of roles such as the candidate of dark matter or the source of the gravitational wave. However, they have not been observed yet. In this work, I focus on the Intergalactic Medium (IGM) gas around PBHs. The gas accreting on a PBH heats up by the release of the gravitational energy. As a result, the heated gas in the vicinity of the PBH emits the UV and X-ray photons. These photons can ionize the intergalactic medium (IGM) around the PBH. Assuming the simple model of these emitting photons, we compute the profiles of the IGM ionization fraction around a PBH by using the numerical calculation of the radiative transfer. Using this profile, we evaluate the extent of the thermal SZ effect and kinetic SZ effect created by the IGM gas around a PBH. Finally, we estimate the CMB temperature angular power spectrum due to the PBH SZ effect in our model. In this seminar, I discuss the resulting spectrum and the possibility to catch signals from them using Cosmic microwave background (CMB) anisotropic observation.

11月20日(水)13:00- @ES606

Axion is a plausible dark matter candidate, whose existence is originally required by the particle physics beyond the Standard Model. Moreover, axions are also predicted by the string theory. Recently, it was shown that axions can be a prominent source of gravitational wave by efficient growth of their fluctuation. In this seminar, we focus on self-interaction, which is one of the mechanism that enable fluctuation growth. First, we introduce a callable parameter q, which can be used to classify different types of parametric resonance described by the general Hill’s equation. We’ll also show that the flapping resonance instability, which takes place for q=O(1), typically leads to the most significant growth of the inhomogeneous mode among the self-resonance instabilities. Next, we focus on the QCD axion, which is one of the solutions of strong CP problem. We’ll show whether QCD axion can form clump in our Universe by the temperature dependence of axion or not.

## 10月のセミナー

10月23日(水)10:00- @ES606

In the early universe, cosmic string and cosmic superstring may have been generated. The former is from phase transition and the later is from one of the models of superstring theory. Kinks are formed on strings and propagate along strings. They produce a gravitational wave background at broad frequency range (Kawasaki et al. (2010), Matsui et al. (2016)).
Strings also generate a gravitational wave background by kink-kink collisions. In our work, for the first time, we calculate the number of kinks on cosmic superstring with Y-junction and estimate the gravitational wave background from kink-kink collisions. Finally, we discuss the observation probability of the gravitational wave background by the future instruments.

10月16日(水)13:00- @ES606

The Alcock Paczynski test is the one of the way to probe expansion history (or geometry) of the universe by observing the size of objects along the line of sight and angular directions. Previous studies have shown that stacked voids, the under dense region of the large scale structure, can be one of the candidate for the test, but there are some drawbacks coming from the number of voids in galaxy surveys. In order to overcome the difficulty, we propose a new way to detect voids in the HI intensity mapping survey which will observe a neutral hydrogen distribution along the large scale structure (or galaxy and dark matter distribution) so that we will obtain a sufficient number of voids. In this talk, we will present results of our analysis using hydrodynamical simulation data such that the shape of stacked HI voids are spherical in real space but contaminated in the redshift space due to the peculiar velocity around voids.

Johan Samsing (Princeton University)

10月15日(火)15:00- @ES606

Abstract
I will present recent results on how binary black holes (BBHs) merge in dense stellar systems through chaotic few-body interactions. By taking into account GR effects in the equation-of-motion, I will show that dense stellar systems are likely to produce non-circular (eccentric) mergers in both LISA and LIGO with rates that are 10-100 times larger than what have been computed over the last decades using Newtonian N-body codes. In particular, I will demonstrate using simple analytical arguments that 5-10% of all BBH mergers from classical globular clusters will be eccentric in LIGO. This makes eccentricity a promising parameter for distinguishing BBH merger channels from each other. I will further discuss new ideas related to how the BBH merger distribution indirectly can be mapped using interrupted stellar tidal disruptions.

10月9日(水)13:00-@ES606

Observations of large-scale structures (LSS) in the universe have been widely used to explore the origins of accelerated expansion of the universe, such as dark energy and modified gravity. Currently, 21-cm line emitted from neutral hydrogen (HI) is drawing attention as a probe of LSS. The 21-cm line intensity mapping can observe a wider and distant universe than conventional galaxy surveys. However, in the case of cosmological analysis by 21-cm survey, there is still no theoretical model to compare with observation, and it is necessary to construct it. Therefore it is necessary to understand the nature of the large-scale clustering of the HI. But since the complex physical processes such as UV background radiation and baryonic feedback from galaxies contribute to the ratio and spatial distribution of the HI , it is difficult to solve analytically.
Although it is necessary to model the HI power spectrum, cosmological hydrodynamical simulations with large box-size and large particle number are computationally expensive. In this study, we investigated better methods to reconstruct the HI distribution from the dark matter distribution obtained from N-body simulation.
After reionization, most of the HI is present inside the high-density regions such as dark matter halos, so a method of assigning HI on the dark matter halos has been done in several previous studies. However, we found that such a method underestimates the power spectrum. We will show the contribution to the power spectrum of HI present in the intergalactic medium (IGM) and discuss the modeling of HI in the halo and IGM.

10月2日(水)15:00- @ES606

In the present state of cosmology, it is believed that the accelerating expansion of the Universe called cosmic acceleration has occurred at least twice; inflation and late-time acceleration. As observations have shown, the accelerations we observed are well approximated by the de Sitter space, namely, the quasi-de Sitter phase.
The accountability for the cosmic acceleration is normally provided by a new scalar degree of freedom whose time evolution dynamically breaks the time translation symmetry of the de Sitter space. In the path of generalization of gravity theories, meanwhile, the break of the time translation symmetry is generally derived from the Effective Field Theory approach, or the analysis of the generic class of scalar-tensor theory, such as Horndeski, GLPV, and DHOST theories. In the last decade, the application of the EFT or scalar-tensor theories for cosmic acceleration has drawn the attention of the cosmological community as an alternative explanation for cosmic acceleration.
In this seminar, we shed the light to spot the nature of late time acceleration through the tests of scalar-tensor theories. We specifically argue how significantly the scalar-tensor theories are inspected by forthcoming observations such as galaxy surveys, cosmic shear, and gravitational wave observations. We show that the most promising cases enable us to reach the accuracy at 1% for testing any departure from the Lambda-CDM concordance cosmology.

## 7月のセミナー

6月24日(水)15:00-@ES606

We consider the constraints on Degenerate Higher-Order Scalar-Tensor (DHOST) theories with matter density fluctuations. The DHOST theory is one of the most interesting model of modified gravity which is an origin of the late-time acceleration. Its equations of motion has higher derivatives more than second order, but there is no ghost modes due to its degeneracy. These derivative interactions are imprinted on the growth of density fluctuations at both linear and non-linear levels. At a linear level, the effect of these interactions appears as the new friction term on the evolution equation of linear density fluctuations. Then, we derive the growth index of the linear growth rate in the DHOST theories and can constrain it from LSS observations. At a non-linear level, the second-order kernel is modified from that of GR and the shape dependence of matter bispectrum is peaked at the folded triangle in the DHOST theories.

6月24日(水)13:00- @ES606

21-cm線を用いた小スケールの初期パワースペクトルへの制限

ビッグバン理論の宇宙初期に関する諸問題の解決策としてインフレーション理論がある。インフレーションモデルは無数に存在するため、そのモデルを制限する必要がある。その方法の一つに初期パワースペクトルによる制限がある。初期パワースペクトルの制限は宇宙マイクロ波背景放射の観測などから得られてきたが、小スケール側 ($波数 k \ge 1Mpc^{－1}$) は不定性が大きい。近年注目されている Ultracompact minihalo (UCMH) という天体を用いることで小スケール側に制限を課せる可能性がある。 UCMH は、赤方偏移 z=1000 に形成される高密度天体であり、密度揺らぎの大きさが $10^{-3} \le \delta \le 0.3$ を 満たす時に構造形成されうる。高赤方偏移において形成される UCMH は、空間的にコンパクトであり、初期パワースペクトルの短波長側の波数範囲に制限をつけることが期待される。

6月24日(水)13:00- @ES606

Non Bunch-Davies真空における単一スカラー場インフレーションモデルの観測量の推定

インフレーション理論はビッグバン理論の抱える問題を解決するために生まれた理論であり、多様なモデルが存在する。その中でも最も単純なモデルとして、単一スカラー場インフレーションモデルがある。インフレーションモデルを特徴付ける観測量として、テンソル・スカラー比 r と非ガウス性パラメータ fNL に着目する。ここでテンソル・スカラー比とは、テンソル型の揺らぎ (初期重力波を生む時空の揺らぎ) とスカラー型の揺らぎ (曲率揺らぎと呼ばれる揺らぎで、密度揺らぎの起源となる) それぞれの二点相関関数の大きさの比に対応する量で、非ガウス性パラメータ fNL はインフレーション期につくられる初期揺らぎの三点相関の大きさを表す量である。このモデルでは r はスローロールパラメーター ε を用いて理論的に r = 16ε で表され、実際の CMB 観測では、その値は r < 0.07(⇒ ε < 0.07/16) に制限されている。また、fNL は無視できるほど小さな値となる。

6月17日(水)13:00- @ES606

クォーク・ハドロン相転移による背景重力波への影響

6月17日(水)13:00- @ES606

21cm線とCMB弱重力レンズ効果の相互相関による中性水素存在量の推定

HIは波長21cmの電磁波(21cm線)を放出する。従って21cm線を観測すば、HIの存在量の時間発展を得ることができる。しかし、21cm線のシグナルは前景放射によって汚染されてしまう。この問題を解決するために、21cm線と、大規模構造がCMBに及ぼす重力レンズ効果による収束場との相互相関をとるという手法を採用する。[Tanaka et al 2019]では、今後観測が始まる望遠鏡であるSKA(Square Kilometre Array)を想定した場合に、HIの存在量の推定精度をFisher解析により予測している。その結果、SKA観測による、相互相関を用いたHIの存在量の推定は、従来の望遠鏡による他の手法を用いた制限よりも、高赤方偏移まで精度よくHIの存在量を推定できる可能性を示している。

6月17日(水)13:00-@ES606

CMBレンジングを用いた銀河団の質量推

7月10日(水)13:00- @ES606

Based on the standard model of structure formation, the first stars have formed at around redshift 20-30 in mini-haloes. They play important roles in the history of the universe such as emitting ionizing photons and providing metals into intergalactic medium. Although resent theoretical studies remarkably improve our understanding on the stellar mass function (SMF) of the first stars, these studies have not reached consensus on the SMF. On the other hand, forthcoming 21-cm observation by SKA is expected to obtain 21-cm signal, originated from neutral hydrogen, from the first stars’ era, which would enables us to approach the SMF observationally. However, the relation between the SMF and cosmological 21-cm signal is poorly understood. Therefore, we model the relation focusing on the escape fraction of the ionizing photons for mini-haloes hosing the first stars. In this talk, I will explain, in detail, the model of escape fraction dependent on the SMF, background density, and redshift. Finally, I will show the results from test calculations of cosmological 21-cm signal with 21cmFAST in order to demonstrate how important the escape fraction is on the large scale 21-cm signal distribution.

7月3日(水)13:00- @ES606

The underdense regions of the Universe are called voids. While they are promising probe of gravity and cosmology on a larger scale than the galaxy, there is not enough agreement on what is the appropriate model for individual voids' evolution. It is known that the underdense region itself tends to grow to be spherical (V. Icke 1984), but the voids in cosmic web rather distort as it grows (e.g. E.G.P. Bos et al. 2012). Though there are some possibilities to cause this, here I follow the description that voids are distorted by the tidal field on their effective radii, and examine the correlation between time derivative of void shape and the tidal field. In this talk, I will first briefly introduce some previous works on the nature of void and related topics, and discuss the main cause of void shape evolution.

## 6月のセミナー

6月26日(水)13:00-@ES606

Large-scale structure (e.g., voids and galaxy clusters) is magnetized. The primordial magnetic fields (PMFs) are expected to explain the origin of these magnetic fields. If the PMFs exist, they possibly create remarkable effects on some cosmological observables, including the cosmic microwave background (CMB) anisotropy. PMFs create additional metric perturbations in the early universe, and induce the CMB temperature and polarization anisotropy. As these effects should include the information about the epoch or mechanisms of the primordial magnetogenesis, we can put a constraint on the PMF model parameters by analyzing the CMB data from Planck satellite and South Pole Telescope. In this seminar, I mainly review the effect of PMFs on the CMB anisotropy, and show the constraint on PMFs that we obtained.

Alexis Boudon

6月26日(水)13:00- @ES606

Quintessence, a canonical scalar tensor theory, is one of the simplest candidates to explain dark energy. During this presentation, we will look at the different changes that a non-minimally coupled theory of the quintessence can bring to the cosmological equation of state and to the gravitational "constant". In the first part, I will present the modifications on the Friedmann and Klein-Gordon equations as well as important formulas. In a second part, I will explain the approach used to build a code capable of numerically solving these equations according to different parameters. Finally, I will show that the equation of state and the gravitational "constant" depend a lot of these parameters but that within the limits of current observations, these differences are minimal.

6月19日(水)13:00- @ES606

As proposed by Hawking and Carr more than four decades ago, black holes can be formed even during the early radiation-dominated era in advance of the ordinary star formation, called “primordial black hole (PBH)”. The possible mass of PBHs covers a very wide range, and the extremely light one (~10^-12 M_\odot) attracts attention as a candidate of the main component of dark matters. Moreover recent LIGO/VIRGO’s gravitational wave detections have revealed the ubiquitous existence of slightly massive and less spinning BHs, which also can be explained by the primordial ones. I first briefly review such astrophysical motivations of PBHs and current constraints on those. Then I show that PBHs can be easily realized if inflation is not a single continuous phase but can be divided into multiple phases. Interestingly recently proposed “dS conjecture” in the context of string theory may also support such a multi-phase inflation scenario.

6月12日(水)13:00- @ES606

Where are metals originated in massive Population III stars?

Theoretical studies have shown that Population III stars are massive. Since massive metal-free stars are expected to eject metals with a characteristic pattern when the stars explode, detecting such a characteristic abundance pattern would be direct evidence for massive Pop III stars. In this study, by using numerical simulation data, we explore the distribution of metals ejected by Pop III stars, and compare it to that by Pop I (or II) galaxies. As a result, we find that metals originated in Pop III stars are dominant in low-density regions in the Universe. The absorption feature imprinted on QSO spectra could be detected by spectroscopic observations with Subaru PFS.

6月5日(水)13:00- @ES606

Photometric redshift (photo-z) is a method to measure the distance to galaxies. Although the photo-z measurement is a crude estimate, particularly for the photometric surveys where no spectrograph is available, the photo-z is the only tool to measure the distance. To alleviate the uncertainty of the photo-z, various approaches have been established. In this seminar, we will review the methods based on the traditional template fitting and empirical method including machine learning. Moreover, the image based analysis using deep neural network is recently proposed and approved by the practical data of BOSS survey. Finally, as an alternative approach, clustering redshift method is introduced where no photometric information is used. As an application of the clustering-z, we will also discuss how we quantify the effect of cosmic variance due to the limited region of the calibration sample, by use of Illustris TNG simulation with super survey modes.

## 5月のセミナー

5月29日(水)13:00- @ES606

We formulate two-point correlation function of primordial black holes (PBHs) at the formation, based on the functional integration approach which has been often used in the context of clustering of the halos. We found that the PBH clustering on large scales could be never induced in the case where the initial smoothed density fluctuations are Gaussian, while it can be enhanced by the so-called local-type trispectrum (4-point correlation function) of the primordial curvature perturbations.

Speaker
Hiroyuki Tashiro

Date/Place
13:00-, 22(Wed), May. @ES606

Title
Charge excess in the Universe

Abstract
It is widely accepted that the Universe is electrically neutral. So far, cosmological analysis are almost performed, based on the charge neutrality, and there are no observational results which is conflict with this assumption. However no one knows that the universe is perfectly neutral. In this seminar, we discuss the observational constraint on the charge excess in the Universe.

5月15日(水)13:00-@ES606

Although the CDM paradigm is consistent with a wide variety of existing observations, it has yet to be sufficiently tested on scales smaller than those of massive galaxies. Here we show that the future 21cm forest observations may offer a powerful test for various alternative dark matter models such as WDM, ULA and PBHs.

5月8日(水)13:00-@ES606

Weak gravitational lensing is one of the most powerful cosmological probes because of its direct sensitivity to dark matter distribution, and thus quite a few galaxy imaging surveys are carried out and being planned. In this talk, I will give a broad overview of ongoing and upcoming weak lensing surveys, including the Subaru Hyper Suprime-Cam survey, and major challenges towards high-precision weak lensing measurement. I will also present the current status of cosmological analysis I am recently working on, especially about the combined galaxy-galaxy clustering and lensing analysis.

## 4月のセミナー

4月24日(水)13:00-@ES606

Self Introduction

4月24日(水)13:00-@ES606

The cosmological principle is the Cosmology’s standard assumption. The cosmological principle is the idea that the Universe is isotropic and homogeneous. Isotropy of the universe is supported by some direct evidence. (CMB, Galaxy, etc. ). But homogeneity of the universe is NOT supported by any direct evidence. It is announced that distant Supernovae are darker than expected by matter dominated epoch in the universe under cosmological principle. The homogenous universe is necessary a dark energy to explain it. (Perlmutter(1998)) But the inhomogeneous universe causes it without a dark energy. I think the constrained (LTB) spacetime as the inhomogeneous universe. I verified that constrained LTB spacetime satisfied both SN-Ia and kinematic Sunyaev Zel’dovich effect, So the constrained LTB metric was excluded. I review the paper “Looking the void in the eyes – the kSZ effect in LTB models”(Garcia, Haugboelle(2008).

4月24日(水)13:00- @ES606

TiO2に担持されたPtナノ粒子触媒（以下Pt/TiO2と略記）は、CO酸化反応に高い活性を示し、COガスによって強い金属担体間相互作用（SMSI）を引き起こす。SMSIは、加熱処理や反応ガスの導入によって著しい活性の促進や劣化が起きる現象である。O2とCO導入におけるPt/TiO2のSMSI効果は報告されていないため、本研究では、Pt/TiO2触媒のCO,O2ガス導入による構造変化をTEMで観察した。その結果、O2ガス導入で、Pt/TiO2界面のピラー成長が見られた。

4月17日(水)13:00-@ES606

The analysis of large-scale structure is performed by calculating two-point correlation function, and most of the information on density fluctuations known to be approximately Gaussian can be obtained from the two-point correlation function. However, in order to further restrict the cosmological model, it is necessary to investigate non-Gaussianity contained in density fluctuation, and in order to extract this information, it is necessary to investigate the correlation of three or more points. The problem is that we need to increase the number of points in order to obtain sufficient information, but the information doesn’t increase greatly even if we increase the point which is calculated. On the other hand, it is difficult to calculate multi-point correlation. In this study, we focused on the analysis of the image of density distribution using machine learning. In the Convolutional Neural Network (CNN) method used in this research, the image is filtered and analyzed to extract the information of multi-point correlation at a small computational cost and classify the image. In this study, images of density distribution are created from simulations of the universe with cold dark matter (cdm), and with warm dark matter (wdm), and CNN is trained to use classification of cdm model and wdm model, or the estimation of mass of warm dark matter. In addition, the difference of results of the classification between when the value of density is converted and when it is not is examined. As a result of learning, the classifications of cdm and wdm of all the masses examined in this study can be correctly classified with probability of 80% or more, and the mass estimation of wdm is also much more accurate than randomly classifying.

4月17日(水)13:00-@ES606

In order to solve the problem of pure big bang theory, it is thought that inflation is necessary. In particular, slow-roll inflation (SR), which is one of the inflation models, is widely accepted. SR is characterized by the fact that initial perturbations, which are the seeds of large-scale structures, are preserved after horizon cross. However, in recent years, an inflation model with potential with an inflection point has been considered. Inflation with a flat potential is called ultra slow-roll inflation (USR). USR has the feature that the perturbation grows after the horizon cross. Therefore, it has recently been attracting attention as a theory for forming initial black holes. In this study, first, we explain the characteristics of the power spectrum in each model, and show that USR cannot end inflation. Next, we connect two models to solve this problem, and show the result of analytically investigating the influence of the connection on the power spectrum for the curvature perturbation.

4月17日(水)13:00-@ES606

New year's impression

New year's impression

4月15日(月)16:00-@ES606

In the standard cosmology, it is believed that the first self-evolving objects are born within the first billion years after the CMB is emitted in the bulk Universe. The objects have gravitationally and thermally grown over the past 10 billion years as the CMB has passed in the structures formed, during which local physical phenomena in the structures are imprinted on the CMB. One of the imprints created by the structures is the gravitational lensing of the CMB (CMB lensing).
In this talk, we report properties of CMB lensing presumably sourced by radio galaxies. We compute the angular cross power spectrum between radio galaxies in NRAO VLA Sky Survey (NVSS) and CMB measured by Planck. We estimate the redshift distribution of the radio galaxies in the lensing kernels via the galaxies in Kilo-Square Degree Survey (KiDS) catalog. To be precise, we use radio galaxies in CENSORS as a reference to the redshift distribution of radio galaxies in high precision.
The theoretical predictions via the Planck 2015 standard cosmological model with assuming the redshift distributions the estimation from KiDS and CENSORS, the angular auto power spectrum of radio galaxies is C_l = \cal O(10^{-3}), and the theories predict that the correlation coefficient is significantly high over 0.4 at l <= 300. The auto power of the radio galaxies is in good agreement with the first measurement in C.Blake et al 2004 at l <=100. Meanwhile, in our measurement of C_l at l>=100, the data is completely covered by shot noise, ending up underestimating the coefficient well down the theoretical predictions. This suggests that a more careful subtraction of the noise is necessary to test the cosmology and the formation history of radio galaxies.

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