[보고서]우주거대구조를 이용한 암흑우주 연구

송용선

우주거대구조를 이용한 암흑우주 연구
Research on dark universe using large scale structure of the universe 원문보기

보고서 정보
주관연구기관	한국천문연구원 Korea Astronomy Observatory
연구책임자	송용선
참여연구자	Arman Shafieloo , David Parkinson , 공진욱 , BenJamin L’Huillier , Feng Shi , Ryan Keeley , Jacobo Asorey , Srivatsan Sridhar , 구한울 , 한인우 , Jurgen Mifsud , Satadru Bag
보고서유형	2단계보고서
발행국가	대한민국
언어	대한민국
발행년월	2019-12
과제시작연도	2019
주관부처	과학기술정보통신부 Ministry of Science and ICT
등록번호	TRKO202000008054
과제고유번호	1711101090
사업명	한국천문연구원연구운영비지원(R&D)(주요사업비)
DB 구축일자	2020-07-29
키워드	우주가속팽창.암흑에너지.암흑물질.우주거대구조.우주초기급팽창.Cosmic acceleration.Dark energy.Dark matter.Large scale structure of the Universe.Inflation.

초록 ▼

우주거대구조의 형성과 진화의 이해를 위해 상대론적 우주거대구조를 연구를 통해서, 우주초기, 암흑물질 및 암흑에너지 본질규명 등의 중요한 문제들을 해결하고자 함. 우주를 이해한다는 기관의 고유 연구 활동과 매우 밀접하게 연관되어 있음.

지구상에서 알려져 있는 기초과학으로 설명할 수 없는 우주론적인 난제들, 1) 입자표준모형의 범주를 넘어서는 우주초기조건 규명, 2) 보이지 않는 암흑물질의 검출, 그리고 3) 단순한 우주상수 모형에 기반 한 아인슈타인의 중력이론으로 설명할 수 없는 암흑 에너지 등의 정체를 규명하는 데 공헌

Abstract ▼

Chapter 1 Probing the Universe
Section 1 The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights

We develop a new method, which is based on the optimal redshift weighting scheme, to extract the maximal tomographic information of baryonic acoustic oscillations (BAO) and redshift space distortions (RSD) from the extended Baryon Oscillation Spectroscopic Survey(eBOSS) Data Release 14 quasar (DR14Q) survey. We validate our method using the Extended Zel’dovich mocks, and apply our pipeline to the eBOSS DR14Q sample in the redshift range of 0.8 < z < 2.2. We report a joint measurement of fσ8 and two-dimensional BAO parameters DA and H at four effective redshifts of zeff = 0.98, 1.23, 1.52, and 1.94, and provide the full data covariance matrix. Using our measurement combined with BOSS DR12, Main GalaxySample (MGS), and 6 degree Field Galaxy Survey (6dFGS) BAO measurements, we find that the existence of dark energy is supported by observations at a 7.4σ significance level.
Combining our measurement with BOSS DR12 and Planck observations, we constrain the gravitational growth index to be γ = 0.580 ± 0.082, which is fully consistent with the prediction of general relativity. This paper is part of a set that analyses the eBOSS DR14 quasar sample.

(출처 : 본문 Chapter 1 Probing the Universe 6p)

목차 Contents

COVER ... 1
제 출 문 ... 2
보고서 요약서 ... 3
요 약 문 ... 4
목차 ... 5
Chapter 1 Probing the Universe ... 6
Section 1 The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights ... 6
Section 2 DASH: Deep Learning for the Automated Spectral Classification of Supernovae and Their Hosts ... 7
Section 3 Cosmic distance determination from photometric redshift samples using BAO peaks only ... 8
Section 4 First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant ... 9
Section 5 Study on the mapping of halo clustering from real space to redshift space ... 10
Chapter 2 Test of Standard model of the Universe ... 11
Section 1 Revisiting Metastable Dark Energy and Tensions in the Estimation of Cosmological Parameters ... 11
Section 2 Implications of a transition in the dark energy equation of state for the H0 and σ8 tensions ... 12
Section 3 A Model-independent Determination of the Hubble Constant from Lensed Quasars and Supernovae Using Gaussian Process Regression ... 13
Section 4 A Simple Phenomenological Emergent Dark Energy Model can Resolve the Hubble Tension ... 14
Section 5 Superluminous supernovae from the Dark Energy Survey ... 15
Section 5 Model independent expansion history from supernovae: Cosmology versus systematics ... 16
Chapter 3 Understanding inflation ... 17
Section 1 Abundance of primordial black holes with local non-Gaussianity in peak theory ... 17
Section 2 Quantum non-linear evolution of inflationary tensor perturbations ... 18
Chapter 4 연구 외 활동 ... 19
Section 1 WBS 연구관리 도입 ... 19
Section 2 국제워크숍 개최 (CosKASI Conference III: The Correlated Universe) ... 32
Section 3 논문발표 목록 ... 33
End of Page ... 34

표/그림 (12)

표 The 68 percent and 95 percent CL contour plots between fσ8 and FAP(left-handpanel), and between fσ8 and DV(right). Ineachpanel, the contours from left to right are for measurements at four effective redshifts, as illustrated in the legend. The filled bands show the mean, and 68 per cent CL constraint on fσ 8 , derived from Planck 2015 observations, combined with external data sets in a CDM Universe
표 Distribution of the final data set used to train the machine learning model. The numbers of spectra for each subtype (rows) and each corresponding age in days since maximum (columns) are listed. The color bar ranges from 0 to 50 spectra
표 The two-dimensional correlation function for the spectroscopic sample (top left), σ0 = 0.01 photometric sample (top right), σ0 = 0.02 photometric sample (bottom left) and σ0 = 0.03 photometric sample (bottom right) given by the coloured contours. The BAO feature which is clearly visible in the spectroscopic sample (∼ 100 h−1 Mpc) is smoothed out in the photometric samples (the smoothing becomes greater with increasing photometric uncertainty). The function plotted in the colour bar is sinh−1(300)ξ(σ, π), which is linear near zero, but logarithmic for high values of ξ(σ, π)
표 Here we illustrate the inverse distance ladder method. The white data points are the BAO distance measurements, and the black data points are the SNe Ia data. The DES-SN3YR sample comprises the higher redshift DES SNe (illustrated with hexagonal points), and the Low-z SNe (illustrated with triangular points). The red line shows our best-fitting cosmographical model, and the shaded region is the 68 per cent confidence region. The blue dashed line and shaded region illustrates the equivalent constraints from just the BAO data, without any supernovae. The blue, BAO-only region is very large at z > 0.7 because we fit only for rs, and not the absolute distance scale at the CMB
표 we incorporate the full bias model into the halo mapping formula. We calculate real space Pδh δh , Pδh θ and higher order terms using bias models in the fitting procedure
표 Observed constraints on standard ΛCDM. Left plot gives the 1D likelihood for Wm,0h2 and right plots shows the 1σ and 2σ contours for Wm,0 vs. H0
표 The same case are the posteriors for the derived parameters including DH(z∗), rdrag, and ρDE(z)/ρcrit,0, for redshifts z = 0,0.5,2 (blue, green, violet). This plots is useful to show how the TDE model with rdrag scaling linearly with DH(z∗) predicts values for ωm, DH(z∗) and rdrag different than the ΛCDM values, while showing no strong preference for a transition in the dark energy density
표 Probability distribution functions (PDFs) of H0 in the cases of flat and non-flat universes. Note that the solid curves labeled "(this work)" indicate results from our model-independent method while the dashed curves assumed ΛCDM using strong lensing only
표 2D regions and 1D marginalized distributions with 1σ and 2σ contours for the ΛCDM model from different observations. From left to right, we use no H0 prior, 2σ hard-cut H0 prior, and 1σ hard-cut H0 prior from Riess et al. (2019), respectively. The black curves/contours denote for the constraints from Pantheon +BAO, and the blue ones are derived with Pantheon+BAO+Lyα+CMB data combination
표 The stacked r-band imaging of the DESSLSN hosts. All images are 10 arcsec×10 arscec. Red crosses mark the location of the SN, and circles mark the locations of fainter host galaxies where they fall within the limits of our imaging (but are still clearly detected within SEXTRACTOR). We identify six events in the sample as being hostless down to the limits of our imaging: DES14C1rhg, DES14E2slp, DES14S2qri, DES14X2byo, DES15X3hm, and DES16C3cv
표 Top left: residuals with respect to the□CDM bestfit. The data points with error bars are the residuals of the SNIa measurements (with orange points including the high-redshift correction), and the coloured lines are the smooth reconstructions from dark blue (first iteration) to yellow (last iteration), using the corrected data. Top right: dimensionless Hubble parameter. Bottom left: Om diagnostic. Bottom right: equation of state of dark energy for the best-fitting
표 A flow chart of our procedure

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우주거대구조를 이용한 암흑우주 연구
Research on dark universe using large scale structure of the universe 원문보기