原始銀河団環境における⼤質量銀河と超巨⼤ブラックホール
形成の研究
筑波⼤学

⽮島秀伸
計算科学研究センター

宇宙の歴史（138億年）
NASA/WMAP teamz~3: 古い銀河(t~3Gyr)z~15: 最初の星と銀河(t~300Myr)z~1: 銀河団
z~10: 宇宙再電離(t~6Gyr)(t~500Myr)z<1: 太陽系の形成
z~7: 超巨⼤ブラックホール z~3: 塵に覆われた銀河(t~3Gyr)(t~800Myr)

13.8 Gyr2

in the UV2,3,4. The detailed properties of these galaxies could be fied10 as a candmeasured from dust and cool gas emission at far-infrared wave- ble and Spitze
lengths if the galaxies have become sufficiently enriched in dust from photomet
andthe gala99.15
a metals. So far, however, the most distant UV-selectedb gal-9.17 9.3 by
axy detected in dust emission is only at z = 3.25, and recent1.5re- the gravitationa
47.0″
sults havecast doubt on whether dust and molecules can be galaxies know
found in typical galaxies at this early epoch6,7,8. Here we report several nights
time of 16 hour
thermal46.5″
dust emission from an archetypal early universe star1.0
The galaxy
forming galaxy, A1689-zD1. We detect its stellar continuum inspectroscopy and determine its redshift to be z = 7.5±0.2 from a spectrum (Fig.
46.0″
spectroscopic detection of the Lyα break. A1689-zD1 is repre- redshift, z = 7.
0.5 9,
sentative of the star-forming population during reionisation
known to date–1
at z > 7 wherewith a total
45.5″star-formation rate of about 12 M yr . The galaxy
is highly evolved: it has a large stellar mass, and is heavily en- stellar continuu
Fλ  λ–β, β = 2riched in45.0″
dust, with a dust-to-gas ratio close to that of the Milky
0.0
Way. Dusty, evolved galaxies are thus present among the fainter factor of ten instar-forming population at z > 7, in spite of the very short time out a different
44.5″
cluded to lensin
since theyfirst appeared.
dec. (J2000)

Hashimoto+18,
NatureFirst galaxies
First stars

Super-massive
Black holes

33.65 sProtoclusters
Dusty galaxies

33.60 s 33.55 s
RA (J2000)

Flux density (mJy)

初期宇宙での銀河形成

Darach Watson , Lise Christensen , Kirsten Kraiberg Knudsen , Johan Richard , AThis precisely determined redshift indicates that the red rest-frame telescope (HST), indicat
optical colour arises from a dominant stellar component that galaxy. The line has a lu
formed about 250
million years
thegalaxies
Big Bang,is the luminosity
As part ofofa
Candidates
for theaftermodestthatcorresponding
formed most of theL⊙stars
to a redshift of about
Our
results at
indicatethatpossiblevalue
X-shooterspeco
in the 15.
earlyuniverse,
redshifts
z >it7,may
havebebeen
found inadopt
large a fiducial
1
to detect such early
episodesof star formationin similarimaging
galaxies
candidate ih
numbers
with extremely
deep restframe-UV. Butmaximum
it has the(FWHM)
with future telescopes.
other high-z
galaxiegalaxy cluster,
proved difficult for existing spectrographs to characteriseinthem

33.50 s334

Fig. 1 | ALMA [O iii] contours and spectrum of MACS1149-JD1.
a, Magnification of an HST image (F160W), with the ALMA [O iii]
contours overlaid. Contours are drawn at −3σ (dashed line), 3σ, 4σ, 5σ
and 6σ, where σ = 17.5 mJy km s−1 per beam. The ellipse at the lower

3
Obser

left corner indicates the sascension and dec. denot
coordinates. b, The ALM
obtained with a resolutio

1

Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan. 2Nati
Department of Physics and Astronomy, University College London, London, UK. 4IRAP, Université de Toulouse, CNRS, UPS, CNES, To
Uppsala University, Uppsala, Sweden. 6Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA. 7Divisio
Science, Nagoya University, Nagoya, Japan. 8Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Univof Astrophysics (MAS), Santiago, Chile. 10Space Science Institute, Boulder, CO, USA. 11Institute for Cosmic Ray Research, The Univer
School of Science, The University of Tokyo, Tokyo, Japan. 13Institute of Astronomy, The University of Tokyo, Tokyo, Japan. 14European
15
Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), Tok
of Science, Hokakido University, Sapporo, Japan. 17Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Instit
Japan. 18Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Heidelberg, Germany. 19Theoretical A
University, Osaka, Japan. 20The Open University of Japan, Chiba, Japan. 21The Institute of Physical and Chemical Research (RIKEN),

CosmicWatson+15,
Naturereionization
How high-z galaxies form and evolve?
TMT
ALMA
What star formation history?
How radiation properties change with thegalaxy evolution?
How massive BHs form?
JWST
How reionization proceeds?
~2020s-2030s
3

3 9 2 | NAT U R E | VO L 5 5 7 | 1 7 M AY 2 0 1 8© 2018 Macmillan Publishers Limited, part of Springer Nature. All rights

Figure 1 | The gravitationally lensing galaxy cluster Abell 1689. The
colour image is composed with Hubble filters: F105W (blue), F125W(green), F160W (red). The zoomed box (4˝×4˝) shows A1689-zD1.
Contours indicate FIR dust emission detected by ALMA at 3, 4, and 5σ
local RMS (yellow, positive; white, negative). The ALMA beam

1

(1.36˝×1.15˝) isry-beam correcte
Slit positions formagenta (dashedwas used in the r

Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 32, København Ø, 2
3
University of Technology, Onsala Space Observatory, SE-439 92 Onsala, Sweden. Centre de Recherche Astr4nue Charles André, 69561 Saint Genis Laval Cedex, France. Istituto Nazionale di Astrofisica–Osservatorio As
Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinb

3

宇宙階層構造

SKA

⼤規模構造
Subaru

JWST

銀河
~Mpc

TMT

ALMA

~kpc

星団や
ブラックホール

Gas accretion, feedback, merger? ~pc

4

激しい形成期の銀河想像図(Tumlinson2017レビュー論⽂)

輻射流体力学
ダークマター重力多体力学
化学反応

重力 v.s.フィードバック&角運動量

原始銀河団とは？
The Astrophysical Journal Letters, 844:L23 (7pp), 2017 August 1

銀河団（現在）最終的に銀河団になりそうな初期宇宙の銀河密集領域

実際に発⾒されてきた原始銀河団
たち
RES EARCH | REPORTRESEARCH LETTER

es with Protoclusters at z ⇠ 67

z = 6.6

a –56° 37' 00.0"
5ume, allowing it to power star formation andblack-hole growth in active galaxy populations
at z ~3.
IRAC 3.6-μm background
LABOCA 870-μm contour
Sources A–N

b –56° 38' 10.0"

z=4.3
1.1-mm background

REFERENCES AND NOTES[C II] contours
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T. Saito, Lya view 35.0"
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RA (J2000)
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M.
Fumagalli
et
al.,
Mon.
Not.
R.
Astron.
Soc.
462,
1978–1988
Fig.
3.
Three-dimensional
picturesofLyafilaments.
(A)
Velocity
map
of
the
Lya
emissionobtainedd z = 6.6 (right). The black dots show the positions of the LAEs. The large(2016).
from its flux-weighted
centroid in the MUSE data. Image scale and plotting symbols are the same as thosedensity regions are indicated by the bluer colors, smoothedwith a Gaussian
17. L. D
Wisotzki et al., Nature 562,E229–232 (2018).
B (B) The 3D distribution
C
F
G
1.00
in Fig. 2. Coherent velocity trends can be seenalongAthe filament structures.
of18. D. K. Erb, M. Bogosavljević, C. C. Steidel, Astrophys. J. 740,
Lya filaments shown with blue [signal-to-noise0.7
ratio
(SNR)
>
2]
and
magenta(SNR>
5)
voxels.
The
locations
L31–L36 (2011).
5
19. C. Steidel et al., Astrophys. J. 492, 428–438 (1998).
of SMGs (without detectable x-ray AGNs, orange
0.5 0 circles), AGN-hosting SMGs (red diamonds), and
20. Y. Matsuda et al., Astrophys. J. 634, L125–L128 (2005).
x-ray–luminous AGNs without ALMA 1-mm detections (brown hexagons) are also displayed. The Lya
21. H. Umehata et al., Astrophys. J. 815, L8–L13 (2015).
0.25
filaments and SMGs and AGNs are colocated on megaparsec scales.
22. See supplementary materials.
0.00
23. C. C. Steidel et al., Astrophys. J. 532, 170–182 (2000).
C
24. Y. Matsuda et al., Astron. J. 128, 569–584 (2004).
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J
L
M
N
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Christopher Martin et al., Astrophys.
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1.00 H
26. M. Fumagalli et al., Mon. Not. R. Astron. Soc. 471, 3686–3698
at thisCO(4–3)
epoch (21). Such an overdensity of acGiven the large number of active galaxies in
0.7 5(2017).
tive populations is very rare (29), and there is
this region, the elevated photon flux required
27. B. D. Lehmer et al., Astrophys. J. 691, 687–695 (2009).
0.5
0little observational evidence regarding how
to power the filaments could be provided by
28. J. E. Geach et al., Astrophys. J. 700, 1–9 (2009).
0.2 our5
this intense activity is fueled and sustained.
the galaxy population identified within
29. C. M. Casey, Astrophys. J. 824, 36–51 (2016).
30. D. Narayanan et al., Nature 525, 496–499 (2015).
Cosmological simulations suggest that rapid
field. To test this hypothesis, we determined theDec. (J2000)

Dec. (J2000)

z66OD

Umehata
et al. (2019, Science) Miller et al. (2018, Nature)cIntensity (mJy beam–1)

130億年前の
原始銀河団

SMGs

Downloaded from http://science.sciencemag.org/ on October 6, 2019

z=3.1

Harikane et al. (2019)

1.
2.
3.
4.

原始銀河団の巨⼤フィラメント

0.00

爆発的星形成で構成される
原始銀河団

infall of gas from the cosmic web in protonumber of ionizing photons provided by x-ray–
AC KNOWLED GME NTS
0 1,000–1,0001,000 –1,000
0 1,000 –1,000
0 1,000 –1,000
0 1,000 –1,000
0 1,000 –1,000
0 1,000
clusters
may leadto the0 formationof SMGs
selected AGNs and SMGs (22). Under the–1,000
We thank the reviewers for their constructive comments, which(kmAlthough
s−1)
(30).
gas inflows are not directly
simple assumption that the ionizing sourcesVelocity
were very helpful in improving this paper. Our data are based on
observations collected at the European Organisation forobservable in our data, the location of SMGs
typically lie 250 kpc from filaments, the reAstronomical
Research wherein the Southern
Hemisphere.
We thank
all
Fig.
1
|
The
SPT2349-56
field
and
spectraoftheconstituent
galaxies.
showstheprimarybeam
is at 50% of its maximum. The filled
and AGNs within the filaments supports thequired photon flux corresponds to a photon
ESO staff who supported us in observation preparation and−1idea that large
reservoirsonof gasfunneled
emissionrate of contours
Qion ~1055 sof
toa,number
LABOCA
870-µmSPT2349-56,
overlaid
theareIRAC
ellipse
shows
the
0.4″
naturally
weightedsynthesized beam. c, CO(4execution. We thank the JAO and EA-ARC staffs for preparation,

7

ademic.oup.com/pasj/article/70/SP1/S31/4564193 by UNIV OF TSUKUBA user on 27 November 2020

原始銀河団で発⾒される珍しい銀河
⼤きく広がった銀河（ライマンアルファブロッブ）

塵に覆われた爆発的星形成銀河群

多重超巨⼤ブラックホール

The Astrophysical Journal, 856:72 (12pp), 2018 March 20

Figure 4. False-color image of the core of our protocluster at zspec = 4.002 ,obtained from our I-, KS-band and IRAC imaging. The positions of the 11 DRC
components are highlighted by white contours; 12CO(2–1) emission fromATCA is shown with green contours and the ALMA 12CO(4–3) emission isshown with red contours (note that this faint emission is on top of DRC-1). Alls in steps
1s . Most
components
contours
from 4s to 6areFig. 6. Local significance maps for seven z ∼ 1 pairs with >4σ overdensity within two arcminutes. The symbols
andruncontours
the ofsame
asDRC
figure1. are detected
in at least one optical/near-IR band and a variety of colors is seen, with thehavingintheJ020332−050944
reddest optical/near-IR colors.
brightest The
sourceswhite
at 2 mmstar
The first six panels show the BOSS binary fields and the bottom panel shows the one from Hennawi et al. (2006).

このような銀河がどのようにして形成されたのか分かっていない
and J020341−050739 field shows the companion quasar (SDSS J020320.47−050933.8) at z = 1.353. (Color online)

Component

Table 2
Line Properties of DRC Components

I[C I](1 - 0)
(mJy km s-1)

I12CO(6 - 5)
(mJy km s-1)

FWHM 12CO (6 - 5)

(km s-1)abeen spect
total obsc
zspec = 5.3
estimated f
at slightly
the protoc
Yamada etthe observ
adopting thconcentrat
SFR ~ 34
than DRC
high obscu
reported b
SFR was dour protoc
much lowe
As repoDSFGs. T
LABOCAis »106 m
DRC, the14,400 M:
are at its
redshifts m
2 photome
are require

The [C
tracer of th
CO lines i
and it has
population

研究課題
原始銀河団環境（宇宙⾼密度領域）では銀河や巨⼤ブラックホールはどのように形成するのか？
原始銀河団の理論や観測研究によって銀河研究のどのような側⾯が明らかになるのか？

理論的に調べるには
⼤規模な流体計算、輻射輸送計算などが必要

FOREVER22 simulation project(FORmation and EVolution of galaxies in Extremerly overdense
Regions motivated by SSA22)(Yajima et al. 2020 submitted)
z=3100 cMpc

100 kpc

2 cMpc理論
H. Yajima
M. AbeH. Fukushima
K. Nagamine
S. Arata
A. Inoue
S. Khochfar
C. Dalla Vecchia
Y. Li
観測
T. Kodama
M. OuchiN. Kashikawa
T. Hashimoto
Y. Matsuda
H. Umehata
M. Kubo
K. Mawatari10Forever 22 simulation run
PCR run (x10)VolumeL = 20 cMpc/h
mgas = 3x106 Msun
Mhalo ~ 1014 Msun
zend = 2

PC
R

BPCG run (x10)
L ~ 6 cMpc/h
mgas = 4x105 Msun
Mhalo ~ 1013 Msun
zend = 4

FIRST run (x2)
CG
P
B
T
S
F IR
Resolutiontime

L ~ 2 cMpc/h
mgas = 5000 Msun
Mhalo ~ 1011 Msun
zend = 911

宇宙論的流体計算

Cosmological SPH simulation with Gadget-3 (Springel 2005)+ FiBY models (Johnson+2013) + Eagle models (Schaye+2015)
PH fomulation+ Our original models (Yajima+ 2020)
Basic equationsd⇢+ ⇢r · v = 0
dt
dv
rP
=
r
dt
⇢
du
P
⇤(⇢, T )
=
r·v
dt
⇢
⇢
P =(
1) ⇢u

(43) matter
Dark
Star formation(44)
Feedback
Black holes(45)
Chemistry(46)

星からのフィードバック
輻射加熱
Photon conservation model (not RT)

⽔素分⼦破壊ダストへの輻射圧
Optically thin within a radius of tau<1

超新星爆発

H2
H(Johnson et al. 2013)

Stochastic thermal feedback(Dalla Vecchia & Schaye 2012)13

Protocluster formation
Gas structure

5 cMpc/h

17
18
19
20
21
22
Figure 3. Total SFR within 10 cMpc from the centre of mass considering massive haloe
23
Red thick solid line shows the PCR0 run. Blue and green lines represent PCR1-4 andtotal SFRs of protocluster candidates by Lacaille et al. (2019), Mitsuhashi (2020), Clem
24
Kubo et al. (2019). The lower and upper values at z = 5.7 assume that the fraction of a25
respectively, accounting for redshift uncertainty (Harikane et al. 2019). The open triangle
26
in Kubo et al. (2019).
27
実線：シミュレーション28
シンボル：観測29
Forever22 11
30
星形成率
31
32
星形成率
33
34
35
36
37
38
39
40
41
42
43
Figure 5. Cosmic
44
di↵erent lines is th45
observational data
46
ALMA ALPINE s
2020; Loiacono et
47
The black dashed
48
UV-selected galax49(2014).
e 3. Total SFR within 10 cMpc from the centre of mass considering massive haloes with Mh > 101250
M in each zoom-in region.
宇宙年齢
ick solid line shows the PCR0 run. Blue and green lines
represent PCR1-4 and PCR 5-9 runs. Open51 squares are the observed
FigureCumulative
SFR within a specific sky-area at z = 3.
FRs of protocluster candidates by Lacaille et al. (2019), Mitsuhashi (2020), Clements et al. (2016)52, Harikane
et al. 4.
(2019)
andThe meaning
the coloredsolid lines is the same as in Figure 3.
中⼼からの⾯積
While this mode
et al. (2019). The lower and upper values at z = 5.7 assume that the fraction of associated submillimeter galaxies
is 0.3 andof1.0,
53 AGN contribution
The black solidline is the total SFR in the MF run. Gray diively, accounting for redshift uncertainty (Harikane et al. 2019). The open triangle is the data without
derivedduce the observ
54
amonds are the observed total SFRs of protocluster candidateso et al. (2019).
violent disc insta
shown in figure 2 in Miller et al. (2018).
55
high sSFR is ind
15
56
forcing particles
57
resolution.

星形成史

平

均

場

?

活発さの度合い

星形成率

PCR runs at z =re 4. Black dashedr of 2.5. Open sym-

Forever2213

原始銀河団は重い銀河が多いが、質量に対する星形成率
は平均的な領域と変わらない？

質量

Figure 7. Star formation rates of galaxies as a function of stellar
mass. Di↵erent symbols represent each run: PC0 (filled red circles), PC1-4 (blue crosses), PC5-9 (green crosses), and MF (filled

16Inflow/Outflow to protoclusters(Harada, Yajima, et al. in prep.)

Rvir

AA55CH10-Tumlinson

ARI

3 August 2017

11:35

Tumlinson+17
Diffuse gas

SFR

as

g

15 kpcws
tflo

Annu. Rev. Astron. Astrophys. 2017.55:389-432. Downloaded from www.annualreviews.org
Access provided by Tsukuba University on 06/23/20. For personal use only.

g
tin
cre
c
A

Ou

z=3

g gas
clin
cy
Re

300 kpc
Figure 1
A diagram of the CGM. The galaxy’s red central bulge and blue gaseous disk are fed by filamentary accretion from the IGM (blue).
Outflows emerge from the disk in pink and orange, whereas gas that was previously ejected is recycling. The diffuse gas halo in varying
tones of purple includes gas that is likely contributed by all these sources and mixed together over time. Refer to Supplemental
Figure 1 for an alternate version of the figure, which illustrates the different observing techniques we discuss in Section 3.
Abbreviations: CGM, circumgalactic medium; IGM, intergalactic medium.

Most of outflow gas return into
the galaxy as fountain flow
Supplemental Material

time, τdep ∼ M gas / Ṁ sfr changes by only ∼2× over the factor of 30 between sub-L∗ and super-L∗
galaxies. More generally, sub-L∗ galaxies generally have extended bursty star-formation histories,
as opposed to the more continuous star formation found in more massive galaxies, suggesting
differences in how and when these galaxies acquire their star-forming fuel. As this fuel is from theCGM, we must explain how sub-L∗ and L∗ galaxies fuel star formation for longer than their τdep .

2.1.2. What quenches galaxies, and what keeps them that way? How galaxies become andremain passive is one of the largest unsolved problems in galaxy evolution (Figure 2b). Proposedsolutions to this problem involve controlling the gas supply, either by shutting off IGM accretionor keeping the CGM hot enough that it cannot cool and enter the ISM. Low-mass galaxies tend
to continue forming stars unless they are a satellite of or near a more massive galaxy (Geha et al.

17

392

Tumlinson·

Peeples

·

Werk

0

t =t

ds 00
, t =dst
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ct0 = t t0 =, t t00 = t, t00 t= t
t (59)cToymodel(M ) / M 2.35

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2.35

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(60)

ĖSN · tcoolĖSN · tcoolĖ · t
FSN ⇠ FSN ⇠ F ⇠ SN cool (61) (61)
Rcool SN
Rcool Rcool(61)

Supernova feedback

Momentum per 1 SN (Thornton+98)
✓
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⌘
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⌘
0.14
2/17
⇣
⌘
2/17
Z
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2/17
H
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n
5 1
Z
nH
H1
5
5
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=
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⇥
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km
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km=s 3 ⇥ 10 M 3 kms 3
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1Zcm 3 Z
Z
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(62)

✓

(62)

◆
✓
SF
✓2 1
◆ R SF R ◆
(63)
10
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FSN = PF1SN ⇥
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1SN

M 2 yr 1

GMhalofgas

2

(62)
(63)

18

FSN ⇠ ✓ ◆⌘ 2/17 Z
Rcool 0.14

⇣ n
H
5
1
= 3 ⇥ 10 M km s
1 cm 3(61)

Z⇣ n (62)⌘ 2/17 ✓ Z ◆ 0.14H
5
1
P1SN = 3 ⇥ 10 M km s✓
◆ 1 cm 3
Z
SF R
2
1
(62)
(63)
FSN = P1SN ⇥ 10 yr
Gravitation force M yr 1
✓
◆
SF R
2
2
1
(63)
Pf1SN
yr
FGM
gas ⇥ 10
SN =
halo
1
Fgrav =
(64)
M yr
2
Rvir
2
fgas
GMhalo✓◆4/3F✓(64)
grav = ◆2 ✓ 2 ◆
Mhalo
1+z
Rfvirgas
1
R > 25 M yr
Condition
for galactic outflow (FSN > Fgrav)
12
10 M
4
0.1
◆4/3
◆2 ✓
◆
0.14✓
⌘2/17 ✓ Z ◆
⇣ n ✓
Mhalo
1+z
fgas
H 1
SF R > 25⇥M yr 3
1 cm
1012MZ
40.1✓ ◆0.14⌘⇣ (65)
2/17
ZnH⇥
1 cm 3
Z(65) 19

Toy model

Outflow rate
SFR [Msun/yr]

Outflow rate/SFR

outflow

fountain

Halo mass [Msun]

Halo mass [Msun]
20

塵に覆われた爆発的星形成銀河群
の形成
251.5

Protocluster at z=6

251

fescUV < 10%, Z~0.1 Zsun
>0.1 mJy (850micron)

250.5

Radiative Transfer250
249.5

249

Massive galaxies (Mh>1012Msun)

248.5

248

100kpc

247.5

247
248

>2 mJy (850micron)
100kpc1Mpc(physical)

Clustering of SMGs along the filamentary structure!
21
248.5

249

249.5

250

250.5

251

251.5

252

252.5

Forever22

15

ar

⾃

急速

Slow

⼰

抑

制

成⻑

st

2x
10
-3
M
re
la
tio
n
Lo
ca
l

ブラックホール質量Black hole mass v.s. stellar mass

星質量

22

Massive disk formation?
Face-on100

Toomre-Q

10

z=7
5kpc

1
0.1

10kpc

edge-onR[kpc]

宇宙物理の計算技術を医療へ！
<赤外線CT技術の開拓>

Hillman (2007)より

生体ひかりイメージング
近赤外線の光を照射し、散乱光から
生体内の情報を取得する診断技術

DOTの臨床応用

1. 悪性腫瘍の検出利点

外因性トレーサーやプローブが不要
Fig. 1 Intrinsic chromophores and structures of the brain. !a" For small animal imaging, it is possible to use visible light to look at oxygenationdependent hemoglobin absorption !as well as exogenous absorbing and fluorescing dyes". The cortex can be exposed and imaged at highresolution, or imaged through the intact skull and scalp at lower resolution. !b" For human brain imaging, near-infrared light will penetrate more
readily through the scalp and skull to sample the brain thanks to lower scatter and absorption. The human brain has a more complex convoluted
structure compared to lower mammals. Spectra: major chromophores in brain are oxy- and deoxyhemoglobin and water !lipid is omitted here". For
generation of these spectra: water content is assumed to be 90% !quoted value in newborn brain, 71 to 85% in adult brain34". Hemoglobin
absorption is shown assuming 2-mM concentration of hemoglobin in blood and 3% content of blood in tissue !60 mM in tissue34" calculated fromspectra.257 HbR spectrum represents 3% fully deoxygenated blood in tissue. Scatter spectrum is approximate using: !!s = A"−b, where A = 1.14
# 10−7 m and b = 1.3.228

ゼロ被爆、非侵襲、ベッドサイド
低コスト、高時間分解能
新生児・乳児に適用可能

⾸の光輸送計算
NIR.
X線

乳がん

may be removed to provide a direct view of an area of thebrain’s surface. In mice, the brain can often be visualized
without even thinning the skull. Methods have been carefully
developed to ensure that normal brain function is not affectedby these approaches. Most often, the animal will remain anesthetized during measurements.23 In some cases, however, apermanent window can be surgically implanted and the animals can survive for over a year while an area of their brain isaccessible for repeated direct optical imaging.14,24
Imaging of pathologies requires only that the animal beanesthetized. Images during acute interventions, such as ad-

ministration of drugs or introduction of a stroke, must be carefully synchronized with image acquisition. While the brain’sfunctional response to stimulus is being studied, a carefully
controlled stimulus is presented during imaging. Such stimuli
may include visual !e.g., showing patterns or pictures", somatosensory !e.g., electrical or tactile stimulation of the whiskers
or forepaw", or auditory stimuli !different frequencies and amplitudes". Stimuli may be repeated in regular blocks, or presented in a randomized pattern.18,25 Data are usually shown as
the average response to multiple stimulus repetitions to obtain

乳癌

2. 新生児・乳幼児検査法

ただし、理論計算、ひかり計測ともに難しく、ほとんど実用にいたっていない（夢の技術）
Journal of Biomedical Optics

051402-3

September/October 2007!

新生Vol. 12!5"Phyµa = 0.019/mm, µs’ = 0.86/mm (800 nm), g = unknown, n =1.48

Simulation results(Yajima, Abe, Umemura in prep.)

S, 照射；D, 受光、最短SD間隔, 8 mm
計測平面：ファントム底面から、35 mm, 45
mm, 55 mm

Detection

Intensity

injection

simulation

Time[nano sec.]

25

まとめ
• ⾼精度な原始銀河団シミュレーションを⾏った• 原始銀河団では⼤きな星形成率を持つ⼤質量銀河が多数形成される• 原始銀河団銀河は⼤量のガスと塵に覆われて星の光のほとんどが隠される⾚外線で明るい銀河になる• フィラメント構造からのガス流⼊により原始銀河団環境では超巨⼤ブラックホールが形成される