ダークバリオン探査計画「Super DIOS」の現状~コズミックネットワークを巡るエネルギーと物質の探査~(2020年2月よりISAS/JAXAのRGとして承認)

佐藤浩介 (PI, 埼玉大学)
大橋隆哉、石崎欣尚、江副祐一郎、山田真也 (首都大学東京)
山崎典子、満田和久、石田学、前田良知、中島裕貴 (ISAS/JAXA)
三石郁之、田原譲 (名古屋大学)、河合誠之 (東京工業大学)
松下恭子 (東京理科大学)、藤田裕 (大阪大学)、永井大輔 (米 Yale大学)
吉川耕司 (筑波大学)、大里健 (仏 ソルボンヌ大学)
藤本龍一 (金沢大学)、鶴剛 (京都大学)、太田直美 (奈良女子大学)
一戸悠人 (立教大学)、内田悠介 (広島大学)
2020年3月3日 高宇連研究会＠zoom

1ダークバリオン探査

The Astrophysical Journal, 759:23 (15pp), 2012 November 1

Shull, Smith, & Danforth(2008), Tilton et al. (2012), and the systematic uncertainties• “ミッシング”バリオン問題の解決
discussed in Section 3.2.
of intergalac2. WHIM (O vi-traced). Previous FUSE surveys
-5 cm
-3 程度
• 温度数百万度,
密度10
tic O vi absorbers (Danforth & Shull 2005; Tripp et al. 2006)
found lower limits of 5% and 7%, respectively for the conの希薄なガスの観測
tribution of this gas to the baryon inventory. These surveys
assumed metallicity Z = 0.1 Z⊙ and ionization fraction
fO vi = 0.2. In 2008, three O vi surveys with HST/STIS• 様々なスケールにおけるバリオンの(Danforth & Shull 2008; Tripp et al. 2008; Thom & Chen
2008) probed to lower O vi column densities. Based on the
直接観測と定量化
survey of 83 O vi absorbers (Danforth & Shull 2008) andour more recent analysis of 111 O vi absorbers (Tilton et al.
vi)✓銀河周辺物質2012), we adopt a baryon(CGM)
fraction Ω(O= 17% ± 4%.
b
The factor-of-two increase arises primarily from our re✓銀河群/銀河団とその周辺部
vised corrections, (Z/Z⊙ )fO vi = 0.01, for metallicity andO vi ionization fraction (see Section 3.1). There may besome, as yet undetermined, overlap of photoionized O vi
✓宇宙の大規模構造に付随するガスwith the Lyα forest.
3.(WHIM)
WHIM (BLA-traced). BLAs were proposed (Richter et al.
2004, 2006; Lehner et al. 2006, 2007) as repositories of

Shull+12

Planck Collaboration: Planck early results. VIII.

Figure 10. Compilation of current observational measurements of the lowIllustris-TNG
a substantial
fractionof theor candidates
low-redshift
baryons.
sampleof 189 SZ clusters
detected over
the whole BLAs
redshift baryon census (Section 3.3). Slices of the pie chart show baryons in
Planck collaboration+11
from the first ten months of the Planck survey of the sky.
collapsed form, in the circumgalactic medium (CGM) and intercluster medium
are definedskyas
Lyα absorbers with Doppler parameters
The present article details the process by which Planck ESZ−1(ICM), and in cold gas (H i and He i). Primary baryon reservoirs include diffuse
b ! 40 km
s was, constructed
corresponding
temperatures
sampleand validated. to
The Planck
data and the T =© NASA
photoionized
Lyα forest and WHIM traced by O vi and broad Lyα absorbers.
specific
SZ
extraction
methodsusedtodetectthe
SZ
candidates
2
2
4
(m
b
/2k)
=
(9.69
×
10
K)b
for
pure
thermalH
arepresented
inSects.
2
and3.
Planck’smeasurements
provide broad40
Blended colors (BLAs and O vi) have a combined total of 25% ± 8%, smaller−1
the integrated
parameter,Y, ofde- abunening with anb estimate= (40ofkms )b40Compton. Owing
to thelarge
than their direct sum (17% plus 14%) owing to corrections for double-counting
tected SZ cluster “candidates”. A subsequent validation process
dance of hydrogen,a smallneutralfraction(H i) remainsof WHIM at 105 –106 K with detectable metal ions (Section 4.1). Collapsed
is needed to identify
which among
the candidates
are previously
6
known
clusters,
programme ishighrephases (galaxies, CGM, ICM, cold neutral gas) total 18% ± 4%. Formally,
detectable in
Lyα
up andto anTadditional∼ 10follow-up
K, although
S/N
quired to scientifically exploit Planck cluster data. This includes
29% ± 13% of the baryons remain unaccounted for. Our simulations (Figure 3)
confirmation the(catalogue
validation)and the measurement
is required cluster
to measurebroad,
shallowabsorption. As
suggest that an additional 15% reside in X-ray-absorbing gas at T ! 106.3 K.
of relevant physical parameters. These diﬀerent steps of the ESZ
a result, theconstruction
surveysandofvalidation
BLAs
are differ
presented considerably.
in Sect. 4 and the sub-In theirAdditional baryons may be found in weaker lines of low-column-density O vi
sequent active
results aregalactic
given in Sect.nucleus
5. Finally, Sects.
6–8 present
survey of seven(AGN)
sight lines,
and Lyα absorbers. Deeper spectroscopic UV and X-ray surveys are desirable.
the general properties of the ESZ cluster sample. Planck early
Lehner et al.
(2007)
founda BLA
frequencydN
results
on clustersof galaxies
are presented
here and inofa setof /dz =(A color version of this figure is available in the online journal.)
02:00.0

58:00.0

13:00:00.0

12:56:00.0

27:59:59.9

29:59.9

銀河団 ~1Mpc

26:59:59.9

銀河 ~10 kpc

宇宙の大規模構造
articlesCollaboration
30 ± 4 for accompanying
absorberswith(Planck
40 km
s−1 "2011e,f,g,h).
b " 150 km s−1
Throughout the article, and in all the above cited Planck SZ~100Mpc
and log NHearlyclaimed model
thatis a20%
result 13.2.
papers, theThey
adopted cosmologicalΛCDM of thei !

cosmology with Hubble constant, H0 = 70 km s− 1 Mpc− 1 , mationization corrections, metallicity, and geometricfactors (cloudbaryonsin parameter
BLAs.ΩA
more recent survey (Danforth
Fig. 1. Planck y-map of Coma on a ∼3 × 3 patch with
the ROSAT-resideter densitym = 0.3 and dark energy density paramPSPC
iso-luminosity
contours
overlaid.
size). It is possible that the baryon inventory could change aseterΩ
Thedifferent
quantity E(z)isthe ratio of the Hubble
Λ = 0.7.to
2020年3月3日
高宇連研究会＠zoom
et al. 2010)
came
conclusions.
Surveying
constant at redshift z to its present value, H0 , i.e., E 2 (z) =a result of better determinations of these parameters. However,
3
◦

◦

2

ダークバリオン探査~10 kpc ̶ ~100 Mpc のスケール•宇宙の大規模構造✓宇宙全体でのバリオンフラクションの解明と定量化✓大規模構造の中での銀河と銀河団の進化の解明✓バリオン効果によるダークマターへの制限•銀河群/銀河団及びその周辺部✓大規模構造から銀河団へのガスの降着とエネルギーの流れの解明✓ダークマターハロー分布と質量の評価、電波/可視光観測との比較✓銀河団~大規模構造に至る元素循環の解明•銀河周辺部✓銀河周辺物質(CGM)の分布の解明と定量化✓銀河のハロー内外でのガスの流れとフィードバック効果✓銀河の星生成率のウエンチングとCGMの相関

各階層での宇宙のバリオン分布を定量的に観測し、宇宙の進化におけるエネ
ルギーと物質の循環、さらにはダークマター分布との相関の解明を目指す
2020年3月3日 高宇連研究会＠zoom

3国内外の情勢ダークバリオン観測は世界的にも2040-50年代に実現されるべき大型ミッションとして提案• NASAʼs Decadal Survey (Walker et al., AAS, 2019)
Astro2020 Science White Paper• ESAʼs Voyage 2050
(Simionescu et al. arXiv:19080177)
Unveiling the Galaxy Cluster – Cosmic Web
Astro2020
White
Paper
ConnectionScience
with X-ray
observationsin theNext Decade
Unveiling the Galaxy Cluster – Cosmic Web
Thematic Areas:⇤ Planetary Systems ⇤ Star and Planet Formation
3 Cosmology and Fundamental
Connection
with
X-ray
in the Physics⇤ Formation and Evolutionof Compact
Objects observations⇤⇤ Stars and Stellar Evolution ⇤ Resolved Stellar Populations and their Environments
3 Galaxy Evolution
Next
Decade ⇤ Multi-Messenger Astronomy and Astrophysics⇤
Principal Authors:
Thematic
Areas:A. Walker1 , Daisuke⇤ Planetary
Name: Stephen
Nagai2Systems ⇤ Star and Planet Formation
3 Cosmology and Fundamental Physics⇤Institution:
Formation1)and
EvolutionofCompact
Objects⇤
NASA GSFC, 2) Yale University,⇤Email:Stars andStellar Evolution ⇤ Resolved
Stellar Populations and their Environments
stephen.a.walker@nasa.gov;
daisuke.nagai@yale.edu
3⇤
Galaxy+1Evolution
Multi-Messenger
Astronomy and Astrophysics
Phone:(301) 286-9882; +1⇤(203)432-5370

Principal
Authors:
Co-authors:
A. Simionescu (SRON), M. Markevitch (NASA GSFC), H. Akamatsu (SRON), M.
1
2
Name:
NagaiM.
ArnaudStephen(CEA),A.
C.Walker
Avestruz, Daisuke(U.Chicago),
Bautz (MIT), V. Biffi (CfA), S. Borgani
Institution:1) NASAGSFC,
2) YaleUniversity,(MPA), K. Dolag (USM/MPA), D. Eckert (MPE),(UniTS/INAF),
E. Bulbul(CfA),
E. Churazov
Email:
stephen.a.walker@nasa.gov;
daisuke.nagai@yale.edu
S. Ettori(INAF), Y. Fujita (Osaka), M.
Gaspari (Princeton), V. Ghirardini (CfA), R. Kraft (CfA),
Phone:+1 (Miami),(301) 286-9882;+1(Stanford),(203) 432-5370
E. T. Lau
A. Mantz
K. Matsushita (TUS), M. McDonald (MIT), E. Miller(MIT), T. Mroczkowski (ESO), P. Nulsen (CfA), N. Okabe (Hiroshima), N. Ota (Nara), E.
Co-authors:
A.(IRAP),
Simionescu(SRON),(NASA
GSFC),
H. Akamatsu(SRON),
M.
Pointecouteau
G. Pratt(CEA),M.K.Markevitch
Sato (Saitama),
X. Shi(SWIFAR),
G. Tremblay(CfA),
Arnaud(CEA),
C. Avestruz(U.Chicago),
Bautz (MIT),
V. Biffi (CfA),
S. Borgani
M. Tremmel(Yale),
F. Vazza(Bologna), I.M.
Zhuravleva(U.Chicago),
E. Zinger(Heidelberg), J.
(UniTS/INAF),
ZuHone (CfA) E. Bulbul (CfA), E. Churazov (MPA), K. Dolag (USM/MPA), D. Eckert (MPE),
S. Ettori (INAF), Y. Fujita (Osaka), M. Gaspari (Princeton), V. Ghirardini (CfA), R. Kraft (CfA),
E. T. Lau (Miami), A. Mantz (Stanford), K. Matsushita (TUS), M. McDonald (MIT), E. Miller
Abstract:
In recent years,
the outskirtsof(CfA),galaxy N.
clusters
emerged asN.one
the newE.frontiers(MIT),
T. Mroczkowski(ESO),
P. Nulsen
Okabehave(Hiroshima),
Otaof(Nara),
anduniquelaboratories
forstudyingthegrowth
of
large
scale
structure
intheuniverse.
Pointecouteau (IRAP), G. Pratt (CEA), K. Sato (Saitama), X. Shi (SWIFAR), G. TremblayModern(CfA),
cosmologicalhydrodynamical
simulations
make firm (U.Chicago),
and testable E.
predictionsof the thermodyM.
Tremmel (Yale),
F. Vazza (Bologna),
I. Zhuravleva
Zinger (Heidelberg),
J.
namic andchemical evolution of the X-ray emitting intracluster medium. However, recent X-ray
ZuHone(CfA)
and Sunyaev-Zeldovich effect observations have revealed enigmatic disagreements with theoreticalpredictions, which have motivated deeper investigations of a plethora of astrophysical processes
operating In
in recentthe virialization
region inofthecluster
outskirts.
of thephysics
clusteroutAbstract:
years, the outskirts
galaxyclusters
haveMuchemergedas oneof theofnew
frontiers
skirtsis fundamentally
fromthethatgrowthof cluster
cores,scale
whichstructure
has beeninthe
focus of
X-ray
anduniquelaboratories different
for studyingof large
themainuniverse.
Moderncluster science
over the past several
decades.
A next-generation
telescope,equippedwithcosmologicalhydrodynamical
simulations
makefirm and testableX-ray
predictionsof thethermodysub-arcsecond
spatialresolution
a largeemitting
field of viewalong witha low However,and stable recent
instrumental
namic
and chemical
evolutionof overthe X-rayintracluster
medium.
X-ray
background,is requiredeffectin orderto reveal havethe fullstory enigmaticof the growthof galaxy clusters
and theandSunyaev-Zeldovich
observations
revealed
disagreementswith theoreticalcosmic webwhich
and their
applications
cosmology.
predictions,have
motivated fordeeperinvestigations of a plethora of astrophysical processes
operating in the virialization region in the cluster outskirts. Much of the physics of cluster out1
skirts is fundamentally different from that of cluster
cores, which has been the main focus of X-ray
cluster science over the past several decades. A next-generation X-ray telescope, equipped with
sub-arcsecond spatial resolution over a large field of view along with a low and stable instrumental
background, is required in order to reveal the full story of the growth of galaxy clusters and the

世界に先駆け2030年代にダークバリオン探査「Super DIOS」の検討を開始し、2020年2月にISAS/JAXAのRGとして承認
2020年3月3日 高宇連研究会＠zoom

4バリオン探査衛星計画• XRISM計画により旧DIOS計画はキャンセルとなったが、宇宙のバリオン
探査は宇宙物理学に残された重要課題• XRISM/Athenaの観測を補完し、宇宙の広い領域でバリオンを定量的に観測するには、広視野/高空間撮像分解能力/高エネルギー分光能力が必要
Year

Detector

FOV

Ang. Resol.

Aera
(cm2)

Grasp
(cm2 deg2)

1500

1500

eROSITA2019

pn-CCD

1 deg.

16-28
arcsec

XRISM

2022

CAL/CCD3ʼ/38ʼ

2 arcmin

~350

1/90

Athena2031

TES/CCD5ʼ/40ʼ

5 arcsec>15000100/6500

HUBS

2030ʼsTES

1 deg.

~1 arcmin

~1000

~1000

Super DIOS 2030ʼs

TES

0.5-1 deg.

~10 arcsec>1000

300-1000

2020年3月3日 高宇連研究会＠zoom

5Baseline plan of Super DIOS
Super DIOS performance
Weight2000-3000 kg

RocketH2-H3

Area at 0.6 keV> 1000 cm2

Focal length

about 3-4 m

Angular resolution ~10 arcsec
Energy resolution< 2 eV @ 1 keV

TES pixels~30000Field of view

0.5 - 1 deg.

Instruments (TBD for detail after
feasibility study based on simulations):✓1 TES array with 30,000 pixels, cooled
by a cryogen-free cooling system✓Microwave SQUID multiplexer (MUX)
TES readout system✓1 XRT, covering 0.5-1 deg. FOV with~10” angular resolution and eﬀective
area > 1000 cm2 @0.6 keV✓1 Gamma-ray burst detector with fast
repointing system
Launch:✓Satellite mass will be 2000-3000 kg✓Launch year will be >2030
Study team:✓International study team with Japan,
US, and Europe(TBD)
2020年3月3日 高宇連研究会＠zoom

6国内外の協力体制•科学目標設定の検討のため宇宙論的シミュレーションを用いた議論を開始しており、国内外の理論/シミュレーションの専門家がチームメンバーとして新たに加入•ハードウエアの開発は、これまでのX線衛星の開発を担ってきたJAXA及び各大学機関だけでなく、産業技術総合研究所など地上実験で高度な技術を持つ機関や、民間企業とも協力•米国 NASAゴダード宇宙飛行センター(GSFC)のRichard L.
Kelly 博士のグループとは今後のバリオン探査ミッションにおいて協力することで合意•オランダ SRONからも協力に前向きな回答
2020年3月3日 高宇連研究会＠zoom

7

OVII surface brightness in z=0, 0.5 and 1

IllustriousTNG100-3
75 MpcIl

Feasibility study with “Illustris-TNG”(Pillepich+18)

Pr

elim

ina

ry

S-DIOS detection limit?

IllustriousTNG100-3

tion は下がっているものの、密度が高いため、Based on simulations✓Quantifying what fraction of “dark baryon”✓Fractions of X-ray signals arising from ICM,
CGM, and WHIM components✓Feasibility study with mock X-ray spectra with
detector responses to determine requirements
for detector performances
Simulation meeting @ISAS/JAXA, Jan. 6th, 2020

Works in progress by Y. Ichinohe & Y. Uchida
2020年3月3日 高宇連研究会＠zoom

8

Cros

GND via

2.5 μm
1.5 μm

400 nm

15 mm

15 mm

Resonator

Z0 ~ 50 Ω

micrograph of a SQUID, and Fig.
TESof readout(Microwave SQUID MUX)
drawing
the SQUID onsystemwhich
are formed. We provided a hole on
beginning and the end of
input coil. Pixels
Detector
ΔE
Readout
Input coil
Modulation coil
30 μm
Hole
Ground pla
ce of input coil, Z1 , on the SQUID
AthenaTES< 2.5 eV
FDM/TDM
oughly 30 Ω, while that on
the hole 3,840
due to theSuperabsentDIOS
screening
currents ~30,000
TES< 2 eV
Microwave SQUID MUX
us, the input coil can be regarded as (c)(d)
中島博士論文, 2020, 東京大永吉/中島講演n line.
Feedlinew that the schematic representationSRON
n input
coil TES
through Min . A standTurn Number
: 1
2
10
11
of Input Coilh of 2linput /m can occur on the
RF-SQUID
n integer. The input-coil length isLSesponds to an input-coil resonanceInsulator (SiO ): 400 nmMin
GHz. The SQUID-loop length is
Input coil
Washer, SQUID loop (Nb) : 300 nm≈ Opends to a washer resonance frequency ≈ OpenInsulator (SiO ): 300 nmCurrent
asher resonance can not occur in Voltage
Ground Plane (Nb)
: 300 nm19 mmof that being higher
than 4–8 GHz
linput-Mux. Note that those resonance
38画素同時読み出し(配線数6!)でed on the basis of the assumption Fig. 1. (a) Micrograph of a SQUID, which acts as a parallel two-loop (fir
3.3gradiometer,eV, 最高: coupled
2.8 eV)
to an 11-turn input coil on each loop. (b) Desiof SiO2 insulator, and高い分解能(中央:the magnetic order)
drawingof SQUID, on which
inputMUX
and modulation
are formed. A h
are39working
developmentsof Microwave
SQUID
readoutcoils
systemere We4, andnm [?], on
respectively.
on ground-plane yields characteristic-impedance gaps between the input crosswith
sectionof one of the SQUID onUniv
JAXA/AIST/TMU/Saitama
and
SRON.
and off
the hole.
The length of input coil is determined by that between
9
2020年3月3日
高宇連研究会＠zoom
hole in this paper.
(c) Schematic representati
in Fig. ?? (b). The coils with a start from and the end of the2

Z1 ~ 30 Ω

2

高結像性能・大有効面積電鋳光学系開発の現状 (名大)要求仕様が大幅に変わり、設計や開発体制の構築から着手→独自の国産次世代高結像性能電鋳光学系の開発をスタート

要求
Wolter 型マンドレル (上左) とその放物面 slope error プロファイル(上右) およびニッケル電鋳ミラー (下) 夏目光学 & 東京大学三村グループ提供✦ <~10 秒角 (要検討)
200 mm2✦ >1000 cm @0.6 keV➡ Wolter 型大有効面積光学系が必須
Slope error [arcsec]
04080

放物面の形状誤差
rms: 0.66 µm, PV: 1.53 µm~11 秒角の形状誤差→境界を除くと ~6 秒角‣ 一昨年度から国産の高性能電鋳光学系の開発に着手

0境界からの距離 [mm]100

小口径サンプル鏡設計・試作・形状評価まで完遂‣ 周方向の形状精度は本手法世界最高レベル (<1 秒角)
基準円筒
境界部を除き ~6 秒角を達成
模擬反射鏡‣ X 線評価@SPring-8 予定 (PI: 三石で採択済み, 2020/6E)
TOP リング‣ ハウジングシステムの設計・試作まで完遂
200 mm‣ 単体鏡での動径調整に成功 (<1 µm)‣ 複数枚調整方法の確立を目指す
BOTTOM リング
国際協力‣
試作ハウジングシステム外観‣ 三石が cosine 社訪問やイタリアグループと議論し、サンプル提供を含めポジティブなレスポンスをもらっている
要求性能は上がったものの、国産光学系も視野に入れ開発を進めていく‣Summary & future work
✓Our project was accepted for establishing the research group in
ISAS/JAXA✓Super DIOS will enable us to resolve not only dark baryons but
also “low X-ray surface brightness diﬀuse” objects such as cluster
outskirts, galaxies, and their halos over several scales✓We have started discussions to quantify what fraction of “darkbaryons” based on cosmological simulations✓The ﬁrst simulation paper on the scientiﬁc feasibility study for
Super DIOS based on simulations will be submitted soon
✓Instrumental performance requirements will be determined basedon the feasibility study with mock X-ray spectra taking into accountdetector responses in future work
✓Developments of TES readout system and X-ray mirror candidates
are ongoing✓Synergy with other missions should be discussed
2020年3月3日 高宇連研究会＠zoom

11