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: [email protected]
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.