筑波大学 宇宙史研究センター

Tomonaga Center for the History of the Universe

https://tchou.tomonaga.tsukuba.ac.jp/eng

About the Tomonaga Center
Tomonaga Center for the History of the Universe (TCHoU) was founded in2017 as a research center at the University of Tsukuba to clarify the genesis of theUniverse as well as the origin of matter and life through construction of an
integrated view of the History of the Universe.
Why our Universe was bone and how it developed into the present state? Since
its birth by the Big Bang, the Universe has experienced various drastic events.
Because the Universe is not a stable object, we have to understand and explain thepresent state as a consequence of dynamical processes the Universe hasexperienced. Though many events in the History of the Universe have been clarified,still many pieces are missing to understand our Universe today.
At Tsukuba, five experimental projects in the area of astrophysics, particle physics,
and nuclear physics were selected in the Master Plan 2017 of the Science Council ofJapan as scientifically important projects to be pushed by the whole community, i.e.,"Search for the decay from the cosmic neutrino background", "Study of the quarkgluon plasma phase by high-energy heavy ion collision experiment", "Antarctic
Astrotelescope Project", "Heavy-elements science through improvement of RI BeamFactory", and "Particle experiments by the high-luminosity Large Hadron Collider(HL-LHC)". Based on close collaborations with the Center for Computational
Science (CCS) that pushes forward the "Cosmo-Simulator Project -From the genesisof the Universe to the creation of life-", TCHoU connects these five projects to casta new light on the missing pieces in the History of the Universe.

Towards Clarification of the History of Universe: Projects at Tsukubagib`bfHg_HeZjjgib`bfHg_H_gi\^Higgs
and the originof masses

Unstablenuclei and theorigin of heavy
elementsdb`akH^d^e^fkj]ZicH`ZdZob^jdZi`^Ij\Zd^H\gjeb\Hjkil\kli^ja^ZmpH^d^e^fkj

Simulation
"%#
ofthe universe,matter & life

MrLgib`bfHg_H
jhZ\^Ikbe^`ignbf`H_dl\klZkbgfjHg_HNTj^^]jHg_H_dl\klZkbgfj

WlZicHQdlgfHVdZjeZjlhhi^jjbgfHg_H_dl\klZkbgfjH[pHr[Zipgfb\H_dl\klZkbgfj？？？

QGP andthe origin ofhadrons
Cosmic νbackground？？？

     

VdZf\cHYTKVi^IbgfbqZkbgfHg_Hka^Hlfbm^ij^_bijkHjkZijHJH_bijkH`ZdZob^j

Antarctic
Observatory ofAstronomy
Rare-RI Ring

稀少RIリング宇宙史研究センター

Tomonaga Center for the History of the Universe
南極天文学研究部門

運営協議会

Div. of Antarctic Astronomy

Steering Committeeセンター長・副センター長

素粒子構造研究部門

運営委員会

Div. of Elementary Particles

Administration Committee

Director /Codirector

クォーク・核物質研究部門

構成員会議

Div. of Quark Nuclear Matters

Research Member Meeting

光量子計測器開発部門

融合研究企画調整室
Office for Integrated Researches

Div. of Photon and Particle Detectors

計算科学研究センター (CCS)
数理物質系 数理科学研究コア (RCMS)
エネルギー物質科学研究センター (TREMS)

Tomonaga Centerfor the History of the Universegib`bfHg_HeZjj
gib`bfHg_H_gi\^Unstablenuclei and theorigin of heavy
elements

Higgs
and the originof massesdb`akH^d^e^fkj]ZicH`ZdZob^jdZi`^Ij\Zd^H\gjeb\Hjkil\kli^ja^ZmpH^d^e^fkj

Simulation
"%#
of the universe,matter & lifeMrL
gib`bfHg_H
jhZ\^Ikbe^`ignbf`H_dl\klZkbgfjHg_HNTj^^]jHg_H_dl\klZkbgfj

jlhhi^jjbgfHg_H_dl\klZkbgfjH[pHrWlZicHQdlgfHVdZjeZ[Zipgfb\H_dl\klZkbgfj

？ ？ ？

？？？

・Detection of cosmic
neutrino background by
COBAND experiment

・Theory of quantum gravity
and superstrings

i^IbgfbqZkbgfHg_Hka^Hlfbm^ij^

Cosmic νbackground・Higgs precision study by
ATLAS experiment    

VdZf\cHYTKVQGP andthe origin ofhadrons

Division of
素粒子構造研究
Elementary部門
Particles

Center for
ComputationalSciences_bijkHjkZijHJH_bijkH`ZdZob^jAntarctic
Observatory ofAstronomy

Division ofクォーク・核物
Quark質Nuclear
Matters
研究部門

・QGP study by ALICE andSTAR experiments
・Study of unstable nuclei
by RI-beam factory

・QCD simulations towards
QGP and nuclear matters

Division ofAntarctic
Astrophysics

・Construction of Antarctic
Observatory of Astronomy
towards dark galaxies

Division ofPhoton andParticle
Detectors

・Development of PPD by
superconducting and SOI
technologies

・Simulation of universeand galaxies

Tsukuba Research Center
for Energy Materials Science
TIA-ACCELERATE, . . .
稀少RIリング

Members, Associates, Research Fellows
Director: Prof. F. Ukegawa

Codirector: Prof. N. Kuno

Div. of Antarctic Astronomy
Chair: Prof. N. Kuno
Member: Assi.Prof. T. Hashimoto, Assi.Prof. S. Honda,
Associate: Prof. K. Sorai (Hokkaido U.), Prof. N. Nakai (Kwansei Gakuin U.), Prof. M. Seta (Kwansei Gakuin U.),
Prof.Y. Kasai† (NICT), Asso.Prof. T. Nishibori† (JAXA), Asso.Prof.Y. Watanabe (Shibaura Inst. Tech.),Asso.Prof. H.Yajima (CCS), Asso.Prof. H. Matsuo (NAOJ)
Div. of Elementary Particles
Chair: Asso.Prof. Y. Takeuchi
Member: Prof. N. Ishibashi, Prof. F. Ukegawa, Asso.Prof. G. Ishiki, Assi.Prof. K. Sato, Assi.Prof. T. Iida,Assi.Prof. S. Hirose, Assi.Prof.Y. Asano, Prof. S. Kim††
Associate: Prof. S. Matsuura† (Kwansei Gakuin U.), Asso.Prof.Y. Ikegami† (KEK), Asso.Prof.Y. Satoh (Fukui U.)
Div. of Quark Nuclear Matters
Chair: Prof. S. Esumi
Member: Prof. A. Ozawa, Assi.Prof. T. Chujo, Assi.Prof. T. Niida, Assi.Prof. T. Nonaka, Prof.Y. Miake††,Prof. K. Kanaya††, Prof. Th. Peitzmann* (PI: Utrecht U.), Prof. M. van Leeuwen* (PI: Utrecht U.),
Assi.Prof. J. Park* (Utrecht U.)Associate: Prof.Y. Kuramashi, Asso.Prof. K. Sasa, Assi.Prof. T. Moriguchi, Prof. T. Sugitate†† (Hiroshima U.),
Prof.Y. Akiba† (RIKEN), Prof. M. Wakasugi† (Kyoto U.), Prof. S. Nagamiya (RIKEN),
Asso.Prof. T. Gunji (U. Tokyo), Prof. K. Shigaki (Hiroshima U.), Prof. H. Sako (CA JAEA),
Prof. T. Saito† (RIKEN), Asso.Prof.Y.Yamaguchi† (RIKEN), Asso.Prof. T.Yamaguchi† (Saitama U.),
Asso.Prof. K. Ozawa† (KEK), Asso.Prof. M. Inaba† (Tsukuba U. of Tech.)
Res.Fellow: S. SakaiDiv. of Photon and Particle Detectors
Chair: Prof. A. Ozawa
Member: Prof. S. Esumi, Asso.Prof.Y. Takeuchi, Assi.Prof. T. Chujo, Assi.Prof. S. Hirose, Assi.Prof. S. Honda,
Prof. S. Kim††
Associate: Prof. E. Nishibori, Asso.Prof. S. Tomita, Asso.Prof. T. Kondo, Assi.Prof. K. Nakamura (KEK),
Assi.Prof. M.Yamada (Tokyo Metropolitan Col. of Ind. Tech.)†) Visiting (Asso.) Prof.,††)

Specially Appointed Prof., *) Research unit under IERL Program.

2024/04

The name of the "Tomonaga Center" is from Dr.
Sin-Itiro Tomonaga, the second Nobel Laureate
from Japan, who made fundamental contributions
in constructing relativistic quantum field theories,
the renormalization theory, theory of collective
motions, etc. and also a founder of the physics
institute at Tsukuba.

Sin-Itiro Tomonaga

1906 – 1979
(Tomonaga Memorial Room, Univ. Tsukuba)Exploration of Cosmic Neutrino BackgroundFew seconds after Big Bang → Cosmic Neutrino Background (CνB)
CMB

300,000 years after BB → Cosmic Microwave Background (CMB）
Discovery of CνB means the first direct observation of the cosmic
era before CMB, => clarification of the initial condition for theformation of galaxies and large-scale structures of the Universe.
A large amount of CνB of about 100/cm3 is expected.
This enables us a high precision observation of the neutrino decay,
and thus provides us with the only way to directly measure theabsolute value of neutrino masses, which play an essential role in thedevelopment of cosmic fluctuations together with the effects of dark
matter and dark energy.

COBAND Project: exploration of CνB by rocket and satellite experimentsCνB!"!$!#!"!#!#!$Precision measurements of far IR photons from neutrino decays.

Step 1: Rocket experiment : take data for 5 min. at 200 km high.

!#!$!#%%!"



Far IR telescope

Determine the life of the neutrino if it is shorter than 1014 years.
(cf. current lower bound = 3×1012 years.)

Step 2: Satellite experiment
Determine the life of the neutrino if it is shorter than 1017 years.

Development of SOI-STJ detectors.
Operation at extreme low temperatures confirmed.
(Nagata et al., 2009).

Antarctic Observatory of Astronomy
Present Universe is in an ionized plasma state. On the other hand, it
was neutral 0.3 Bi. years ago as the CMB is observable.
<= Ionization due to UV radiation from the stars.
Existing telescopes could identify only 30% of required stars/galaxies.
Remaining 70% -- "dark galaxies" -- should be found in the deepspace.
To understand the formation of galaxies, stars, and life, it isindispensable to clarify the ionization mechanism.

Dark Galaxies

CMB？？？

existingtelescopes

Antarctic
Observatory ofAstronomy

Deep-space exploration by THz Telescope at Antarctica
Step 1: 10m THz Telescope
Due to the expansion of the Universe, lights from the deep-space are in the THz range,
which are dumped by the water vapor in the atmosphere.

=> Antarctica with its extremely low humidity is the only place on the Earthwhere THz waves are observable.
Wide angle survey up to 12.6 Bi. years ago by 10m telescope. Recommendation by SCAR
(2010). Combining with the IR observation by the rocket/satellite experiment of the cosmic
neutrino background project, we clarify the whole spectrum to determine the characterand distance of dark galaxies.
galaxies in thedeep space
Planned site: New Dome Fuji (3800m, Japan)
日本経済新聞２０１２年５月２０日

near galaxies

Step 2: 30m THz Telescope
Survey up to 13.6-13.7 Bi. years ago.

=> Direct observation of first stars and galaxies.
Based on the experience of 10m telescope.
Planned site: New Dome Fuji (3800m, Japan)

THz
NHK-BS コズミックフロント 2012 年 6 月 14, 18, 19 日「モンスターブラックホール」研究を紹介

IRClarification of Quark and Nuclear Matters10-4 sec after Big Bang: phase transition from quark matter(quark-gluon plasma: QGP) to ordinary matter of hadrons/nucleons

QGP

It is the most recent particle-level phase transition of our Universe.

=> Initial condition for the evolution of ordinary elements.

High-energy heavy-ion collision experiments
Create QGP on the earth by mankind ("Little Bang").

QGP andthe origin ofhadrons=> Clarify the nature of the phase transition and the quark
nuclear matters (fluctuations, expansion, transition temperature,viscosity, etc.) around the transition temperature.

BeSc am E
annat ergy
RHIC

1st order phase transition
beyond the critical end point
towards high density region

The Univ. of Tsukuba ispushing forward the RHICexperiment at BNL and theALICE experiment at CERN.
hadrons

hadronproduction

photons
jets

expansion in theQGP phasejet quenching
primary scattering
initial fluctuations

Study of Higgs Particle and Search for New Particles
10-10 sec after Big Bang: Higgs phase transition, particles get masses.
Clarification of the nature of the Higgs particle(s): the number of Higgs
particles, decay to dark matter particles, self-coupling

Higgs
particle

Unstablenuclei=> Origin of mass, direct search for the dark mattertowards physics beyond the standard model, critical test of the principles ofparticle physics (gauge symmetry, renormalizability).
Exploration of super-symmetric particles, extra dimensions, etc.

=> Origin of force, origin of space-time

ATLAS experiment at CERN/LHC
Development of high-resolution detectors by the silicon micro strip sensor.
Abundance of elements in the Solar System
612 U

N~

100
陽子数 （Z）

80
6082



061



041001

0

8

流壊タ崩

ベー


084



6020

40202

1001

Rプロセス仮説を検証

r-process

001

吸収性子

的中爆発

11

安定核
不安定核（RI）

0206

Origin of heavy elements in the Universe:

1N~

150

Fe N~

鉄比在存素元の宙宇

40010-21010Study of Unstable Nuclei

0020
80

20

4060

中性子数（N）

80

100

120

140

160

Super-nova explosions after the formation of first stars and galaxies around 13Bi. years ago, merger of neutron stats, etc.
Important to understand the reaction processes of unstable nuclei (r-process,s-process).

Study of unstable nuclei using heavy-ion accelerators
稀少RIリングǙǐǒǌǕƸǙǐǉǍMeasure masses and lifetimes of unstable nuclei by Rare RI-Ring at the RI Beam
Factory (RIBF) of RIKEN, and obtain the reaction rates for the r-process.

1st step: Study the reason for the peak at N≈50;
2nd step: N≈82; 3rd step: N≈126

Theoretical investigations of Universe, Matter, and Life
Large-scale simulation of Universe and Matter
Under a close collaboration with the Center for
Computational Science (CCS), carry out simulations
on the Universe, matter, and life to clarify the origin of
their generation and structure formation. Combine thelatest results of theoretical and experimental studies.

large-scalesimulations

Determination of fundamental parameter of NaturePhase structure and equation of state of QCD at
finite temperature and density=> Genesis of matter at 10-6 sec, inner structure of neutron stars, dark matter
Nucrear reactions
Unstable nuclei
r-process=> Light andheavy elementsin the Universe

Dark Matter, large-scale structure of the Universe
Formation and collision of galaxies
Black hole and gravitational wave
Chemical evolution of the Universeman plas=> Origin of structures of the Universe,
origin of organic molecules and lifegluoquarkeg forc

stronoundbackgr ionradiat

creation ofmatterstar formation

hadrons

metry ?

supersym

electromagnetic force
BIGnucleus
BANG superstrings weak force?
grandgra unificvity ation ? CP vio
dark matterlationSuper-string and super-gravity theories

Investigations of the string theory towards quantum theory of gravity
and unified theory of particles.

great wall

dark energymatte

r-antim

atter

asym

=> Origin of the space-time, origin of particles and forces.

metry

galaxy

AGE
[sec]

-43

10-30

10-20

10-10

10-6

10 1 sec

1 yearformation

PRESENT
14 Bi. yearsDivision for Development of Photon and Particle Detectors
Advanced detectors enabling new physics measurements
Advanced detectors based on new technologies promote and enable measurements in various physics area beyond the current
limitations. The Division supports R&D of new detectors for the projects of TCHoU and develops innovative detectors in theframework of TIA activities.
COBAND

Development of PPDs in close
linkage with other TCHoU
divisions
Developments of silicon semiconductor
devices for ATLAS and ALICE detector
upgrades, STJs for COBAND project,and detectors for other TCHoU projects
are pushed forward by the Division withexchanging knowledge and expertise.
(For details, visit corresponding projectpages.)microstrip

LGAD

FoCal Si/W

pixel sensor

HL-LHC ATLAS

Innovative detectors in TIA

Rad-harddetector R&D
3D stacking enhances
the sensor capability,e.g, for ILC experiment

SOI monolithic detector

LHC ALICE

TIA (Tsukuba Innovation Arena) brings together thepotentials and resources of ﬁve organizations in the
Tsukuba area. The Sensor & Imaging Square of TIA isorganized for developments of advanced detectors tocreate new scientiﬁc ﬁelds and industries.

World-best spatial
resolution 0.65mm
achieved in 2017

VLSI design

STJ

Innovative monolithic pixel detectors are being
realized by the SOI technology. Design and fabricationof VLSI are made in collaboration with KEK and VDEC
(U Tokyo). 3D stacking using μ-bumps enables
further enhancement of the sensor capability.
The projects for STJs and imaging of massive objects(muon-radiography) are also included in the Square.

Tomonaga Centerfor the History of the Universe
Faculty of Pure and Applied Sciences
University of Tsukuba
Tsukuba, Ibaraki 305-3571
Japanhttps://tchou.tomonaga.tsukuba.ac.jp/eng
phone: +81-29-853-3724, 6305(fax)email: TCHoU@tchou.tomonaga.tsukuba.ac.jp2024/04