2019@, 11/11-13, 2019

原始銀河団領域における銀河と巨大ブラックホールの形成Recent wide-survey of galaxy observation has
discovered a lot of candidates of protoclusters

Publications of the Astronomical Society of Japan (2018), VAL.
Overzier+08 OVERZIER ETMiller+18,
Natureb
z=4.1
z=4.3

156

7' 00.0"

IRAC 3.6-μm background
LABOCA 870-μm contour
Sources A–N–56° 38' 10.0"

1.1-mm background[C II] contours
CO(4–3) contours

15.0"

8' 00.0"

radio gal.

Dec. (J2000)

30.0"

K20.0"AN

25.0"

BFGCHEL
I

30.0"

J20"

2"35.0"

9' 00.0"
48.00 s44.00 s40.00 s23 h 49 m 36.00 s

44.00 s43.00 s42.00 s23 h 49 m 41.00 s

How galaxies form and evolve in protoclusters?
Can supermassive black holes form?
Can protoclusters make giant HII bubbles at the reionization epoch?
RA (J2000)

ALBGs

SMGs D

M

30.0"

1.00

Toshikawa+18
z~4Vol. 673

BRA (J2000)

CD

Fig. 14.— Object map of the g475 -dropout candidates (circles), TN J1338!
0.7 5 1942 (square), LAEs (stars), and the detection catalog (points). The g475 -dropouts
detected in Ks are indicated by filled circles. Larger circles indicate brighter ob0.5 0 jects in z . The contours represent density fluctuations ! $ ( " ! ")/¯ "¯ of !1,850
0.25 !0.5, !0.1 (dashed contours) and +0.1, +0.5, +1, +1.5 (solid contours), achievedby smoothing the object map with a Gaussian of width 3600 , or 250 kpc ( FWHM ),0.00 using equal weights. LAEs that are not in the g -dropout sample were not in475
cluded in the density contours. [See the electronic edition of the Journal for a color
H of this fi[CIJKII]
gure.]
1.00 version
CO(4–3)EFG

Fig. 5. Examples of the protocluster candidates. The points indig-dropout galaxies. Individual protocluster candidates exhibit uni
shapes, and some are accompanied by several other overdense reg(e.g., bottom-left and top-right panels).
CL

M

N

2

-- -(Yajima, Abe et al. in prep.)
500 cMpc/h

Halo mass
1000

500

Galaxy cluster

450
450

PC2400
400
350
350

900

MF

300
300

PC3PC1PC2850

250
250

PC1

Milky Way-like-260

200200800

255150150250

100100245

PC3505000

950

240
240005050100150200250

10Mpc/h245300250350

255

400

750
Gadget-3+ FiBY options + Eagle options+ our original options
700= 3 x 106 MmSPH
4 x 105 Msun
sun ,Lzoom = 20 Mpc/h (Large), 10 Mpc/h(small)
L 650= 500 Mpc/h
500 box3260

450

100 150 200 250 300 350 400 450

Stellar feedback
Photoionization heating
Photon conservation model (not RT)

Radiation pressure on dust
Optically thin within a radius of tau<1(Abe, Yajima, et al. in prep.)

Lyman-WernerSupernovaeH2H(Johnson et al. 2013)

Stochastic thermal feedback(Dalla Vecchia & Schaye 2012)
4Black hole feedback
SeedingAccretion
MBH=105 Msun
Mhalo=5x1010 MsunFeedback

Bondi-Hoyle-Littleton model+ suppression term by angularmomentum (Schaye+15)
Super-Eddington acc. OK(fedd,max=3)
Stochastic thermal feedback
Neighbor gas particles are heated up
to 109 K+
Jet feedback (turn off)Gas structure
SFR density
ProtoNorm

5 cMpc/hclustera l f ield6)1)11251.5

Protocluster at z=6251

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

250.5

Radiative Transfer250
249.5

249

Massive galaxies (Mh>1012Msun)

248.5

248100kpc

1>2 mJy (850micron)

-()1

247
248100kpc)1!

247.5- 1)

248.5

249249.5)

250

250.5

251

251.5

252

7252.5

Stellar mass function
protocluster
Mean density

Z/ZsunMetallicity

τ>1

Mhalo [1010 Msun]

Growth of 10 BHs
fEdd

10^8suppress

io n

Su

10^7pedr-Ed.

BH[Msun]

10^910^610^56

789Redshift1011

MBH-Mstar relation( 0 ca l.2 g% alx M axist esar)

Lo

BH [Msun]

108z=6107
106
105 8
10Super-Eddington OKEddington limited

1091010

 [Msun]⊙(86)

!

ṀBH
SFR
249
SFR× c ∼ 4×10 erg/yr
ĖAGN ∼ frfe×
SFR
1 M⊙ yr−1(87)"

Simple spherical shell model

Efb ∼ fkinfEddLEddtcool∼ 2.5 × 10

58erg fEdd!

fkin0.5"!

GMh2fgas
Egrav ∼Rvir∼ 1.0 × 10

critfEdd∼ 0.4!

MBH
106 M⊙"!

"tcool10 Myr(88)T~10^9K,n~10/cc,free-free1658erg!

"−1 !

fkin
0.5!
×Mh
1011 M⊙"5/3 !

"−1 !

MBH
106 M⊙"5/3 !

Mh
1011 M⊙

1+z
11"!
"−1"

fgas
0.16
(89)

tcool
10 Myr"!
" (90)
1+z
fgas
110.16

BHs and Halos growth rate

Eddington ratio

Major merger helps the growth

Major merger
Halo growth rate [ΔMh/Δt/Mh]

Massive disk formation?
Face-on100

z=75kpc

Toomre-Q

10
1

10kpc

0.1

edge-onR[kpc]

Cold stream feeds a BH
10^5
[K] 10^4

Cold stream?
10^31
Specific ang.
mom.
0.1
0.01
0.01

r / Rvir

0.1

1.0Model dependence
10^9

BH mass[Msun]

fedd,max=1, Region0
10^8fiducial

10^7
10^6 fedd,max=1fedd,max=1, MBH0=106Msun
fedd,max=1, Mhalo=1010Msun

10^5redshift! !!      




z=3

!

10 Mpc20

Log NH/cm2

23-4

Log <Z/Zsun>

0
! -23

Log SB-17

17 $Why cosmic web?
logSBLya[erg/s/cm2/arcsec2]

     "    #  " ! ! #18

Summary• We study galaxy formation in protocluster(PC) regions
by cosmological simulations• Star formation proceeds efficiently• Massive galaxies are obscured and become
submillimeter galaxies with S850 >~ 1mJy
• BHs grow with cycles of super-Eddington and subEddington• Giant Lyman-alpha nebulae forms along filaments withthe size of ~100kpc (S>~10^-19erg/s/cm2/arcsec2)