Galaxy Formation and Evolution Explored with Subaru, ALMA ... · • Suprime-Cam (34’×27’)...

Tadayuki Kodama (NAOJ)

NGC2403 (Subaru/Suprime-Cam)

Galaxy Formation and Evolution

Explored with Subaru, ALMA, and TMT

Subaru Autumn School (2014/9/24-26)

E-mail: t.kodama@nao.ac.jp

M63 (Subaru Telescope)

Our Galaxy contains hundres of billions of stars like the sun. The size of

disk is about 30K light years, and the sun is located at 25K light years away

from the galaxy center.

solar system

Milky Way is the edge-on view of our Galaxy !

image

What are galaxies?

Disk

Bulge

Present-day galaxies

Elliptical galaxies

Lenticular galaxies

Spiral galaxies

There are ~100 billion galaxies in the Universe.

Andromeda (M31)

NGC3115

M87

“Hubble sequence” of galaxies

pure bulge

Bulge dominated

Disk dminated

Clusters of galaxies

CL0024 cluster (4.2 Gyr), Subaru TelescopeAbell1689 cluster (2.2Gyr), Hubble Telescope

radius ~ 3M l.y. – 10M l.y.

A cluster of galaxies consists of 100s -1000s of galaxies.

Mass ~ 1014-15 M☉

ＣfA Survey（Gellar & Huchra 1986）

VIRGO simulation（C.Frenk etc）

Real Universe Computers

Super-Clusters (Large Scale Structures)

StarsGalaxiesClustersSuper-

clusters

Hierarchical Universe

Clusters are also connected to form even larger structures in the Universe.

From Uniformity to Complexity

400,000yr (z=1100)

(recombination era)

Very uniform

Δρ/ρ=10-5

Present-day (z=0)

Lots of structures

Δρ/ρ=1~1000

？

How did the present-day complex (non-uniform) Universe

come from the extremely uniform early Universe?

13.7 Gyrs

WMAP (cosmic microwave background)

Subaru Telescope (cluster)

z = 3

Nature? (intrinsic)

earlier galaxy formation and evolution in high density regions

Nurture? (external)

galaxy-galaxy interaction/mergers, gas-stripping

SpiralsLenticulars

Ellipticals

Star-forming

(young)No/little SF

(old)

Morphology- (SFR-) density relation(Dressler 1980)

z~0

log surface density (Mpc-2)

Origin of the cosmic habitat segregation

10 Gyrs ago

Present-day

Hierarchical structure formation (Theory)

z = 0

z = 1

z = 0.5

z = 3

z = 2

z = 25Galaxy scale

Hayagi et al.

Small objects form first, they drag each other by gravity, merge together,

and grow to more massive objects with cosmic times

Cluster scale12.5 Gyrs ago

Saito et al.

http://4d2u.nao.ac.jp/

movie movie

Time-Machine takes you to the past

Galaxy evolution

Galaxy formaiton

Dark age

Big Bang

The further away in distance you see, the farther away in the past you look into.

Astronomy is the Ultimate Archeology!

7 Gyrs ago

10 Gyrs ago

13.5 Gyrs ago

13.7 Gyrs ago

Subaru Telescope (Optical-NIR)(Mauna kea, Big island, Hawaii; 4200m)

Observation bldg.

Keck (USA)

Gemini(USA, Canada, Australia)CFHT

(Canada, France, Hawaii))

UKIRT (UK)

Subaru (Japan) JCMT (UK)

SMA (USA)

Subaru Telescope(hight: 22.2m, diameter: 8.2m)

Mauna Kea Observatories

CSO (USA)

UH88 (USA)

Elevation: 4200m (~60% oxygen)

ALMA (Submm-Radio)(Atacama, Chile; 5000m）

Gigantic interferometer with 66 antenas in total, consisting of 50 antenas of 12m

diameter and Morita Array (ATC; 4 antenas of 12 m and 12 antenas of 7m) .

International collaboration among Japan-USA-Europe

High sensitivity and

high spatial resolution

(0.01-0.1”)

Thirty Meter Telescope (TMT; optical-NIR)

(Mauna kea, Hawaii; 4200m)

First light expected in 2021

A large international collaborations among USA, Japan, Canada, India, and China

Subaru (optical, NIR)

Hawaii, D=8.2m

resolution: 0.1-1.0”

ALMA (Submm, radio)

Chile, D=12m x 54, 7m x 12

resolution: 0.01-0.1”

The three big projects that NAOJ pursuits

TMT (optical, NIR)

Hawaii, D=30m

resolution：0.015”

galaxies（stars）

© Subaru Telescope

clusters（stars）

© Subaru Telescope

Star forming galaxies

（emission lines from ionized gas）

What Subaru and TMT can see in the optical-NIR regime

© Subaru Telescope

NGC2403

CL0024 (z=0.4)

Kodama et al. (2004)

Matsuda et al. (2007)

Stars (a major component of galaxies) and Ionized gas (HII region) with emission lines.

Star bursting

galaxiesMolecular gas

NIR 電波

Mergers

optical

Submm

Dust

©ALMA/HST/Hibbard

©ALMA/VISTA/Emerson

Internal kinematic structures

Wang et al. (2013)

What ALMA can see in the Submm-radio regime

©ALMA

(z=6) [CII]158μm

velocity map

Molecular gas (from which stars form) and Dust (ejected from young stars)

Subaru’s Unique Wide-Field Imaging Capability

Subaru (30arcmin=Full moon) HST (3arcmin)

Digital camera

with 84M pixels

Subaru’s Field of View (area of sky

observed at once) is 100 times bigger!

HUDF

Subaru Deep Field (SDF)

Subaru Prime-Focus

Camera

(Suprime-Cam)

Subaru’s new gigantic cameraHyper Suprime-Cam

Field of view is 7 times larger than Suprime-Cam.

870M pixels, 3 tons

Hangs on there!

Subaru’s unique wide-field instruments will map

out the distant Universe,

as well as discover rare objects.

• Suprime-Cam (34’×27’) optical imaging

• Hyper Suprime-Cam (1.5°Φ) optical imaging

• MOIRCS (7’×4’) NIR imaging and spectroscopy

• FMOS (30’Φ) NIR spectroscopy

• PFS (1.5°Φ) optical and NIR spectroscopy

Panoramic Universe explored by Subaru

z = 30 z = 5

z = 2

z = 3

z = 0z = 1

MOIRCS

(NIR)

MOIRCS (NIR)

Suprime-Cam (optical)

34’×27’

4’×7’

4’×7’

Subaru’s powerful wide-field instruments

Final cluster with M=6×1014 M☉ , 20×20Mpc2 (co-moving) (Yahagi et al. 2005; νGC)

Panoramic Views of Distant Clusters

Subaru/Suprime-Cam view of CL0939 cluster at z=0.41 (4.3Gyrs ago)

30’ corresponds

to 30M light yrs at

the cluster distance.

Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru (PISCES)

『うお座』、『魚』

Kodama et al. (2001)

Dominant central body and surrounding filamentary structures

along which many groups of galaxies are aligned.

Resemble to numerical simulations

Panoramic Views of Cluster Assembly（4.3 Gyrs ago, z=0.41）

30 M

lig

ht

yrs

Kodama et al. (2001)

CL0016 cluster (z=0.55)

Millenium Simulation

(Springel et al. 2005)

Dots: red sequence galaxies in V-I

Red: spectroscopically confirmed members

Blue: spectroscopically confirmed non-members

~1200 secure redshifts!

Hyper Suprime-Cam

(HSC)

A Huge Cosmic Web at z=0.55 over 50 Mpc

(80’x80’ by 7 S-Cam ptgs.)

Tanaka, M. et al.

(2009b)

Cosmic Star Formation History

Peak epoch of galaxy formation and AGN activities in the Universe

Cosmic Noon: 1<z<3 (6>T(Gyr)>2)(in analogy to cosmic dawn at z>6)

Fan et al. (2006)

AGN activities (QSO number density)

Hopkins and Beacom (2006)

This also coincides with the appearance of the Hubble sequence of galaxies.

The most important epoch for galaxy formation

when the grand design of galaxies are established.

How can we sample forming galaxies?

Kinney et al.

(1996)

[OII][OIII]

[Hα]

[SII][Hβ]

[SIII]

It consists of blue stellar continuum and many emission lines from ionized gas.

A typical spectrum of star forming galaxy

(SFRHα > 0.3M☉/yr)

Hα (6563A)@z=0.4

NB921z’

Flux ratio between

narrow-band (NB921) and

broad-band (z’)

Koyama et al. (2011)

Magnitudes in NB

Narrow-band imaging survey will efficientlysample star forming galaxies at high-z

4 narrow-band filters 7 narrow-band filters

FWHMs correspond

to ±1500-2000km/s

Subaru Wide-Field Survey of Narrow-Band Emitters ([OII], [OIII] and Hα) at 0.4<z<2.5

MOIRCS FoV

7’x4’Cluster N-body+SAM simulation

(Yahagi et al. 2005; νGC)

z = 2

Suprime-Cam (optical; 34’x27’) MOIRCS (NIR; 7’x4’)

20×20 Mpc2 box (co-moving)

18 nights for imaging, >15 nights for spectroscopy

“MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru

Unique sample of NB-selected SF galaxies across environments and cosmic times

z>2

clusters

z>2

field

z~1.5

clusters

z<1

clusters

Koyama+’14

status

radio galaxyNB2315

dense clump

Hayashi et al. (2012)

Ks

A Prominent Star-Bursting Proto-Cluster at z~2.5

Hα imagingwith MOIRCS/NB2315

~20x denser than the general field.Mean separation between galaxies is ~150kpc (in 3D).

1.5Mpc away

from the RG

USS1558-003 (z=2.53)

68 Hα emitters detected.~40 are spec. confirmed.

Ks

NB2315 (Hα)

5”=40kpc

Outflow?

radio galaxy

Hayashi et al. (2012)

Red Hα emitters (dusty starbursts?) tend to favor higher density regions!(=key populations under the influence of environmental effects)

Koyama et al. (2013)

Spatial distributions of HAEs in two proto-clusters at z>2

★

★

★ RG

Blue HAE

Red HAE

clumps

~10M

pc o

n a

sid

e (

co-m

ovin

g)

filaments

Proto-clusters are filamentary/clumpy, in the mid of vigorous assembly!

(Hα emitters)

Spatial distribution of star-forming galaxies in clusters

Hα emitters at z=0.81 (RXJ1716) [OII] emitters at z=1.46 (XCS2215)

Koyama, et al. (2011) Hayashi, et al. (2010)

□ □

● phot-z members

Lx=2.7×1044 erg/s Lx=4.4×1044 erg/s

0.5 x R200 0.5 x R200

Clusters Grow Inside-Out !

Dynamical masses and Integrated SFRs in cluster cores

Shimakawa et al. (2014a)

Identification of the progenitors of rich clusters and member galaxies in rapid formation at z> 2 5

F i g u r e 3 . (a) I ntegrated SFR s in the cluster cores, ΣSFR , nor-malized w ith the cluster dynam ical m asses (upper panel) and (b)

cluster dynam ical m asses ( lower panel) are plotted as a func-

tion of redshift. T he open diamonds show the measurements for

the M ahalo-Subaru cluster sample including this work , calculated

w ithin R 200 of each cluster (K oyama et al . 2010, 2011; H ayashi et

al . 2011; Tadak i et al . 2012) . T he fi l led diamonds indicate the val-ues w ithin 0.5×R 200 to match the defi nition with other prev ious

measurements for a direct comparison. T he previous works for 8

clusters at z= 0.1–0.9 are shown by squares (F inn et al . 2005) .

T he grey and open squares separate those clusters according to

their dynam ical m asses as shown in the lower panel. N ote that

SFR s are measured from Hα l ine strengths for al l the clustersexcept for the z= 1.46 and z= 1.62 clusters which are based on

[O i i ] l ines. N ote also that R 200 is not ful ly covered for the z= 0.81

cluster. T he cluster mass of J0218 cluster at z= 1.62 is adopted

from Tanaka et al . (2010) . T he red dotted curve shows a relation

as a function of redshift scaling as (1+ z)6 . I n the lower panel , the

red line and the pink zone show the typical m ass growth historyof massive cluster haloes w ith 1–2×1015M predicted by theo-

retical models (Shim izu et al . 2012; Chiang et al . 2013) . T he pink

zone corresponds to ±1σ scatter around the median values.

red line and the pink zone show the mass growth history ofmassive cluster haloes predicted by cosmological simulations(Shim izu et al. 2012; Chiang et al. 2013). T he data pointsshow the measurements of dynamical masses of real clustersused for comparison. I t turns out that our proto-clustersat z> 2 have large enough masses to be consistent with theprogenitors of the most massive class of clusters like Coma.T he lower-z clusters shown with fi l led squares also followthe same mass growth curve. T herefore we argue that weare comparing the right ancestors with right descendants,and the redshift variation of the mass-normalized SFRs seenin the upper panel can be seen as the intrinsic cosm ic SFhistory of the most massive class of clusters.

I n this Letter, we have presented the kinematical struc-tures of the two richest proto-clusters at z> 2, and extendedthe cosmic evolution of ΣSFR/M cl back to z> 2 or 11 Gyrsago, based on the intensive multi-ob ject N IR spectroscopyof the NB selected star-form ing galaxies. I n our forthcom-ing Paper II ( in preparation) , we wil l discuss the physicalproperties of these galaxies (such as gaseous metal l icities,ionizing states, and dust extinction) using the multi em is-

sion line diagnostics, and compare them with those in thegeneral field at sim ilar redshifts.

A C K N OW LE D G M E N T S

W e thank Prof. T . Yamada at Tohoku Univ. for allowing usto use their VPH-K grism on MOIRCS. W e also acknowledgeDr. K . Aoki at Subaru Telescope for useful discussion. T hiswork is financially supported in part by a Grant-in-A id forthe Scientific Research (Nos. 21340045 and 24244015) by theJapanese M inistry of Education, Culture, Sports, Scienceand Technology. W e are grateful to the anonymous refereefor useful comments.

R E F E R E N C E S

Caril l i C. L . , Harris D . E . , Pentericci L . , R ottgering H . J.A . , M iley G . K . , Bremer M . N ., 1998, ApJ, 494, L143Chiang Y .-K ., Overzier R ., Gebhardt K . , 2013, ApJ, 779,127Croft S. , K urk J. D . , van Breugel W ., Stanford S. A ., deVries W ., Pentericci L . , R ottgering H . J. A . , 2005, AJ,130, 867Doherty M ., et al. , 2010, A& A , 509, 83Ebizuka N . et al. , 2011, PASJ, 63, 605F inn R . A . et al. , 2005, ApJ, 630, 206Garn T ., Best P. N . , 2010, M NRAS, 409, 421Hayashi M ., K odama T ., K oyama Y ., Tadaki K .-i. , TanakaI . , 2011, M NRAS, 415, 2670Hayashi M ., K odama T ., Tadaki K .-i. , K oyama Y ., TanakaI . , 2012, ApJ, 757, 15Ichikawa T . et al. , 2006, SPIE , 6269, 38K aj isawa M ., K odama T ., Tanaka I . , Yamada T ., BowerR ., 2006, M NRAS, 371, 577K ennicutt R . C., Jr. , 1998, ARA& A , 36, 189K odama T . et al. 2007, M NRAS, 377, 1717K odama T ., Hayashi M ., K oyama Y ., Tadaki K .-i. , TanakaI . , Shimakawa R ., 2013, Proceedings of the IAU , 295, 74K oyama Y ., K odama T ., Shimasaku K ., Hayashi M ., Oka-mura S., Tanaka I . , Tokoku C., 2010, M NRAS, 403, 1611K oyama Y ., K odama T ., Nakata F ., Shimasaku K ., Oka-mura S. , 2011, ApJ, 734, 66K oyama Y ., K odama T ., Tadaki K .-i. , Hayashi M ., TanakaM ., Smail I . , Tanaka I . , K urk J. , 2013, M NRAS, 428, 1551K riss G ., 1994, adass, 3, 437K urk J. D . , et al. , 2000, A& A , 358, L1K urk J. D . , Penterici L . , Overzier R . A . , R ottgering H . J.A ., M iley G . K ., 2004, A& A , 428, 817Pentericci L . K urk J. D . , Cari l l i C. L . , Harris D . E . , M ileyD . K . , R ottgering, H . J. A . , 2002, A& A , 396, 109Shim izu I . Yoshida N ., Okamoto T ., 2012, M NRAS, 427,2866Suzuki R . et al . , 2008, PASJ, 60, 1347Tadaki K .-i. et al. , 2012, M NRAS, 423, 2617Tanaka M ., F inoguenov A ., Ueda, Y . , 2010, ApJ, 716, L152Venemans B. P. et al. , 2010, A& A , 461, 823Yoshikawa T . et al. , 2010, ApJ, 718, 112

This paper has been typeset from a TEX / LATEX fi le preparedby the author.

c 2014 RAS, M NRAS 000 , 1–5

Rapid increase of

integrated SFR

per unit cluster mass

with increasing z

Numerical simulations

suggest that

these proto-clusters will

grow to ~1015M◉ clusters

by the present-day

Inside-out growth of galaxy clusters as revealed

by MAHALO-Subaru project

: passive red galaxy

: normal SF galaxy

: dusty SF / AGN

z = 0

z ~ 0.5

z ~ 1

z ~ 2

Illustrated by Yusei Koyama

Dusty starbursts (red HAEs/IR galaxies)should hold the key to understanding

the environmental effects !

Shimakawa et al. (2014a)

MOIRCS multi-object spectroscopy of two proto-clusters at z>2

27 new

members

(totally 49

members)

36 members

40-50 spectroscopically

confirmed members in each cluster!

Dynamical mass of the cluster

core is ~ 1-2 × 1014 M◉

(assuming local virialization)

Shimakawa et al. (2014a)

3-D Views of Proto-Clusters at z>2

velocity

gradient

PKS1138

low mass

PKS1138

high mass

USS1558

low mass

USS1558

high mass

Stacked spectra

Individual spectra (examples)[OIII] strong

galaxies in

proto-clusters

at z>2

Kewley’s model (2013) suggests:

low metallicity and/or

large sSFR and/or

large density?

Shimakawa et al. (2014b)

HST images (V606,I814,H160) from the CANDELS survey

less massive clumpy galaxies

（Mstar<1010

M◉）

0.9

0.80.6

0.5

0.8

0.7

0.9

0.6

0.5

0.6 0.4

0.4

2.2

1.2

1.7

1.4

1.1

0.2

1.7

0.9

1.62.0

1.9

1.0

1.8

1.3

1.0

0.7

2.0

0.9

massive clumpy galaxies

（Mstar=1010-11

M◉）

Tadaki et al. (2013b)

Clumpy structures are common (~40%) in HAEs at z~2 (Field)

colours (I814-H160) of individual clumps are shown with red numbers

Massive clumpy galaxies tend to have a red clump,and they tend to be detected with MIPS 24μm.

The red clumps may be the site of nucleated dusty starburst to form a bulge!We need to spatially resolve star forming activities within galaxies.

3”

3” (~25kpc)

Dekel et al.

(2009, Nature)

Goerdt et al.

(2010)

320 kpc

10 kpc

Efficient gas supply to form a massive

galaxy on a short time scale at high-z.

Rapid gas accretion forms a gas rich disk which

becomes gravitationally unstable and fragmented.

“Cold Streams” along filaments

(Inflow)

cooling radiation of Lyα 37

Bournaud et al. (2013)

Massive gas infall

↓

Gas rich disk

↓

Fragment to clumps

↓

Migrate towards center

↓

Formation of a bulge

Numerical simulations

(N-body+SPH)

reproduce the

clumpy nature of star

forming galaxies and

the bulge formation

180Myr 300Myr

420Myr

640Myr 760Myr

540Myr

Mdyn = 3.5 × 1010 M◉diskbulge

Hypothesis

(UV) (optical)

Spatially resolved Hα line emission in clumpy galaxies

Tadaki et al. (2013b) Contours: Hα images

Hα emission tends to be

stronger in red clumps,

suggesting a dusty

starburst occuring there

Some extended HAEs are resolved with natural seeing, but for the majority,

we require better resolutions with AO+NB imaging, IFU and ALMA.

Seeing-limited images

High-z Galaxy Anatomy

IFU (3D spectroscopy) w/AO

Genzel et al. (2011)

Rotation of gas-rich clumpy disk of a SFG at z=2.4

resolved with IFU (SINFONI) on VLT

Galaxy Anatomy with 3D spectroscopy （Integral Field Unit）

VLT(UT4) / SINFONI

VLT/SINFONI

32 slices x 64 pixels

Keck/OSIRIS

Gemini/NIFS

No such NIR instrument

on Subaru unfortunately!

41

Foerster-Schreiber et al. (2009)z~2 UV selected galaxies; VLT/SINFONI w/o AO; Vc/σ~2-4

SINS Survey

42

K-band (continuum)Narrow-band (Hα)

Stellar mass distributionStar formation distribution

“GANBA-Subaru” Galaxy Anatomy with Narrow-Band A0-imaging with Subaru

A star forming galaxy at z~2

Ganba!

Narrow-band Hα imaging with IRCS + AO188

Struggling with terrible weather at MK :<

(0.1-0.15” seeing)

Ultra-wide-field Laser Tomographic Imager and MOS with AO for

Transcendent Exploration by SUBARU telescope.

Future key instruments of Subaru Telescope

HSC(opt)PFS

(opt)ULTIMATE

(NIR)

鼎（tripod pot）

“ULTIMATE-Subaru”: GLAO + Wide-Field NIR Instr.

High resolution (0.2”~1.5kpc) and Wide-field (13.5’)

NIR: Narrow-band imaging and Multi-object IFU / MOS

Lyα emitters at z=8-10

and

spatially resolved

Hα, [OIII] emitters at 1<z<3.5

NB imaging in between OH sky lines is

competitive to JWST (wins by 20x FoV !)

Ultra-wide Laser Tomographic Imager and MOS with AO for Transcendent Exploration

JWSTSubaru

GLAO

NB imaging

L: SFR>100M☉/yr

M: > 50 M☉/yr

S: < 50 M☉/yr

( Mgas／Mgas+Mstar )

ALMA

Band-3

FoVMol. Gas fraction

SF efficiency ( SFR／Mgas )

spatial resolution (<0.1”), velocity resolusion (~50km/s)

USS1558 proto-cluster (z=2.53)“Mahalo-Subaru”

MApping HAlpha andLines of Oxygen with Subaru

“Gracias-ALMA” GRAphing CO IntensityAnd Submm with ALMA

Mol. Gas. CO(32) @100GHz gas mass (Mgas)

Dust cont. @450 μm–1.1 mm hidden SFR

Spatial distribution and Kinematics｛Proto-clusters are excellent targets for ALMA

“GRACIAS-ALMA” GRAphing CO Intensity And Submm with ALMA

Mapping/resolving molecular gas and dust contents of high-z SF galaxies

CO line @ Band-3 (~100GHz) SFR~50M☉/yr (2.7hrs, 5σ)

Dust continuum@ Band-6-9 (450 μm–1.1 mm)

cycle-2 sensitivities

Spatial resolution: 0.01-0.1” ( 0.1-1kpc) (0.18-0.4” in cycle-2)

SFR~15M☉/yr (50min, 5σ)@1<z<3

f(gas) and SFE(=SFR/Mgas) are essential quantities to characterize the mode of SF.

Relations between red clumps ~ dusty starbursts ~ bulge formation ~ environment

We can spatiall resolve dusty star formation directly within galaxies.

Band-6 (dust)

Band-3 (CO)

Clusters are efficient targets for ALMA

especially at Band-3 as multiple targets

can be observed by a single pointing (1’).

USS1558 proto-cluster (z=2.53)

Chandra 100ks X-ray data (Martini et al.)

have just been taken.

(AGN fraction, distribution)

HST images (Hayashi et al.)

are being taken NOW!

(Clumpy fraction, size evolution)

Unique targets to test the effects of environment on galaxy formation

ALMA Takes Off

Riechers et al. (2014)

A detection of nebular emission line from a distant, heavily obscured galaxy

at z=5.3 in a protocluster.

Now expecting molecular gas observations (CO) from those systems.

Velocity gradient!

Merger remnant or Outflow?

“ALOHA-TMT” Anatomy with Lines of Oxygen and Hydrogen with AO on TMT

Resolving internal structures/kinematics within galaxies under construction

Huge light collecting power (13×Subaru), and

High spatial resolution (0.015”@2μm with AO)

~3 mag deeper (x 15) for point sources and

~1.5 mag deeper (x 4) for extended sources

compared to Subaru (8.2m diameter)

0.015”@2μm ⇔ ~0.1kpc @z>1

TMT can resolve stars and ionized gas with high resolution

which is comparable to ALMA (molecular gas and dust)!

• Location of SF activities and its propagation

Central starbursts or normal/secular SF in disks?

• Gas motions

Inflows (accretion to galaxies) and outflows (ejection from galaxies?

• AGN activities

co-activation of SB and AGNs?

gaseous outflow by AGN

• Morphologies

merger rates and its impact on galaxy size/morphology evolution

Central concepts of galaxy formation are yet to be explored.

Bright future but hard competition!

Witnessing and resolving the physical mechanisms of

galaxy formation in action!

Physics of galaxy formation

to be explored by Subaru, ALMA, and TMT

• HSC hybrid blind cluster survey (0.4-1.0μm: z<1.7)

• SWIMS-18 (0.9-2.5μm: z<5)

• WISH-7 (1-5μm; z<8)

More Future Surveys ofthe Cosmic Noon and Beyond

HSC Hybrid Blind Cluster Survey to z~1.5-1.7

HSC

NB

filters

“red sequence” survey (passive galaxies)“blue sequence” survey (SF galaxies)

phot-z (or color-color) survey to z~1.5 NB [OII] emitter survey to z~1.7

Large-scale (~20Mpc) structures at z~1.5unveiled by [OII]l3727 emitter survey with S-Cam

Tadaki et al. (2012)

Hayashi et al. (2011)

●

(Hilton+09)

(Papovich+10)

XCS2215(z=1.46)

ClGJ0218(z=1.62)

NB973

NB912

Subaru-HSC Legacy Surveys

survey area cluster number (dn/dz)

HSC-Deep 27 deg2 200 (>1014 M◉) at z=1

6 (>1014.5M◉) at z=1

HSC-Wide 1400 deg2 10,000 (>1014 M◉) at z=1

300 (>1014.5M◉) at z=1

SWIMS-18 Survey

Unique, comprehensive imaging survey of the Cosmic Noon

Simultaneous observations of blue (<1.4μm) and red (>1.4μm) channels !

18 filters (6 NBs, 9 MBs, and 3 BBs) will be available !

SWIMS is the new wide-field NIR camera and spectrograph to be installed on

TAO 6.5m telescope in Chile, and will be mounted on Subaru for 2015-2017.

Blue Red

SWIMS-18 Medium-Band Filters (9)

van Dokkum et al. (2009)

NEWFIRM survey (KPNO)

with 5 MBs + Ks

Great improvement

in phot-z such as

⊿z/(1+z) < 0.02

Will open a new window to 3.5<z<5 with K1,K2,K3 !

M*-limited sample of galaxies up to z~4ー5

SWIMS-18 Narrow-Band Filters (6)

Dual Emitters ([OIII] and Hα) Survey

with Pair NB filters (4 pairs)

※ HST F126N 1.259 0.015

SFR-limited sample of star forming galaxies at 0.9<z<3.3

Survey Design for SWIMS-18 (imaging)

Requires 0.7-1.5 yrs of observing time at TAO1/10-1/30 of the survey will be done with Subaru as a pilot study

when SWIMS is mounted on Subaru for 3 yrs (2015-2017)

SFR-limited sample (HAEs) : 7.5 × 105 Mpc3 at each redshift

M*-limited sample: 1.2 × 107 Mpc3 (Δz=1)

NB

Filter

Wavelength

(μm)Redshift

(Hα, OIII)

SFR

(Msun/yr)

Number /

FoV

NB217(same as SWIMS-18)

2.17 2.3, 3.3 7 ~1500

NB284 2.84 3.3, 4.7 20 ~200

NB335 3.35 4.1, 5.7 30 ~150

NB441 4.41 5.7, 7.8 90 ~20

NB497 4.97 6.6, 8.9 250 ??

6hrs exp. (5σ), 1mag extinction of Hα

NB filters at 2.5 ~ 5 μm will be the key for WISH !

Pair filters ([OIII], Hα) to z~6 !

WISH Space Telescope

WISH is a planned 1.5m diameter space telescope

mission for 1-5μm (NIR) with a FoV of 0.24 sq. deg.

Proposing NB filters for WISH

PI: T. Yamada (Tohoku Univ.)

WISH-7 Survey

• 「7」 sq. deg.

~7×107 Mpc3 / (Δz=1)

~10 progenitors of Coma class clusters at every z

NB: 3.5-7×106 Mpc3 / (Δz=0.05-0.1)

~ 1 progenitor of Coma class cluster per filter

30 WISH pointings (0.24 sq. deg. / FoV)

• Exposure times needed

BB: 1 hrs × 6 filters x 30 p = 180 hrs

NB: 6 hrs × 4 filters x 30 p = 720 hrs

900 hrs in total (or 1200 hrs including overheads)

for 1.5<z<8

Summary• Mahalo-Subaru has been mapping out star formation activities

across cosmic times (0.4<z<3) and environments.

• Clusters grow inside-out, and the SF activity in cluster cores drops rapidly as (1+z)6. Dusty starbursts are more prevalent in proto-clusters, and the key populations under the influence of environmental effects.

• Clumpy nature of SFGs at z~2 (in particular, red dusty clumps) maybe closely related to a bulge formation.

• Galaxy Anatomy with NB+AO (Ganba-Subaru), Gracias-ALMAand ULTIMATE-Subaru will reveal the physical processes of galaxy formation.

• HSC will make a large, statistical sample of clusters to z~1.7. SWIMS-18 will be sensitive up to z~5, and WISH will extend the frontier of SFR- and Mass-limited samples to z~6-8.