TMT Science & Instrument Workshop (Victoria, 2011/3/28-3/30)“Sharp” Views of Galaxy Formation and Evolution with TMTTadayuki Kodama (Subaru, NAOJ)“Shadow of Mauna Kea” (12/01/2007)

Japanese Science Report for TMT has just been issued!
(392 pages! written in Japanese, but all the abstracts have English translations.)

TMT science working group in Japanconsists of 51 members,
and the report is written by 73 people.
－Chiefs and Speakers in this WS－+Cosmology and Early Universe:
N. Yoshida (IPMU, Tokyo)
 M. Ouchi (ICRR, Tokyo)+Galaxy: K. Motohara (IoA, Tokyo)
 T. Kodama (Subaru)+AGN:
T. Nagao (Ehime)  M. Akiyama (Tohoku)+Stars/Local group:
W. Aoki (NAOJ)  K. Kawabata (Hiroshima)+SF/Planets/Solar systems: N. Narita (NAOJ)

Key Performances of TMT (30m)
Huge light collecting power (13×Subaru), andHigh 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 this resolution
which is comparable to ALMA (molecular gas and dust)!

AO assisted IFU is the key instrument at the TMT era, whichresolves the internal kinematical structures of high-z galaxies

VLT/SINFONI
32 slices x 64 pixels

VLT(UT4) / SINFONITMT will have IRIS as an
early-light-instrument
and IRMOS (multi-IFU)
is planned as a firstgeneration-instrument

Rotation of a star-forming galaxy at z=2.4
SINFONI (IFU) + AO  0.15” resolution (~1.2kpc@z=2.38)

z=2.38, Ks=19.2, Mdyn=1.13×1011M☉ (Vc=230km/s),
Mstars=7.7×1011M☉, Re=4.5kpc , Mgas(Hα)=4.3×1010M☉
Genzel et al. (2006, Nature)

Vc/σ~2-4

See also Foerster-Schreiber et al. (2006)

Properties

Key Scientific Goals

mass (m)(Galaxy working group)
time (t)environment (ρ )“Sharp Views of Galaxy Formation and Evolution”• SF and MA histories as a function of environment and mass
Relative contributions of SF and MA? How is AGN activity related?

• Emergence/establishment of galaxy morphologies/types
Visual shapes, Internal kinematics of stars and gas (V/σ), Mergers• Internal structures and kinematics of forming galaxies
Population/chemical structure (inside-out), Gas dynamics (inflow/outflow)

The peak epoch of the Universe: 1<z<3 (6>Tcos(Gyr)>2)
Star formation

AGN (QSO)

Fan et al. (2006)
Hopkins and Beacom (2006)※ Hα ([OII]) can be observed from the ground (<2.5μm) up to z=2.8 (5.7),
Lyα can be observed from the ground (>0.35μm) from z=2.

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

Narrow-band survey of line emitters (Hα, [OII]) at 0.4<z<2.5 (primarily z>1.5)

Fieldsclusters

down to 2 M☉/yr at z=1.5, and 10 M☉yr at z=2.5

Inside-out propagation/truncation of starformation activities in clusters□ Hα emitters at z=0.81 (RXJ1716)●□ [OII] emitters at z=1.46 (XCS2215)

phot-z members

0.5 x R200

0.5 x R200

Lx=2.7×1044 erg/s
Koyama, et al. (2010)

Lx=4.4×1044 erg/s
Hayashi, et al. (2010)

Star forming activity in the core is much higher in the higher redshift cluster!

Do
we eventually
see the reversalInside-Out
Propagation
ofof the SFR-density relation atStar Formation Activityz>1.5 as a result of galaxy
and its Truncation?
formationbias?

z~0.8z~1.5?

z=0Illustrated by Yusei Koyama: passive red galaxy: normal SF galaxy: dusty starburst

Two recently found, confirmed clusters at z~1.6
ClG J0218.3-0510 (z=1.62) in SXDF

CL0332-2742 (z=1.61) in GOODS-S[OII] from
z=1.61-1.62

Suprime-Cam

9 spec-z members, σ=540km/s
X-ray detection (4.5σ)(Papovich et al. 2010; Tanaka et al. 2010)42 spec-z members, σ=500km/s
Kurk et al. (2009)

Hα Emitters in a Proto-Cluster 4C23.56 at z=2.48
Subaru/MOIRCS
NB2288(Hα) / Ks
Radio Galaxy(4C23.56)

Spatially extended (Hα Blobs!)
Offset?
SFR=100~1000 M☉/yr !

3arcmin = 1.3Mpc
Tanaka, I., et al. (2011)

“Mahalo-plot” (in analogy to “Madau-plot”)〈SSFR〉vs. z and environment for emitters

Emitters Only!
Highly uncertain yet !

incompletenesscosmic variance…

“What are the physical mechanisms behind this diagram?”
Tadaki et al. (2011), in press

IRIS (IFU: imaging spectroscopy)
FoV=2” (IFU),0.015”@2μm ⇔ ~0.1kpc @z>1

 Spatially resolved star formation (Hα) and chemicalevolution ([NII]/Hα, R23)
・Nucleated starburst (merger-driven)?
or wide-spread star formation over disk (secular evolution)?
・Propagation of star formation/chemical evolution (inside-out)?

 Internal gas kinematics (Hα, [OII], Lyα…)
・Establishment of kinematical morphology?
(rotation or random motion or disordered merger?)・Inflow (cold streams) and Outflow (feedback)?

 AGN activity (BPT diagram at galactic center)
・AGN contribution at center? Is it accompanied by starbursts?

IRMOS (Multi-IFU) will be efficient especially for high density regions.

Can we see cold streams in forming galaxies?
Lyα (1216Å)

1Mpc

100kpcSmoothed (0.5”)

320kpcDekel et al. (2009)“Cold Streams”

HeII (1640Å)

A model for z=3 Yang et al. (2006)

An excellent mechanism of efficient gas supply along filaments to form massive
galaxies at high-z.

Lyα Blobs in a high density region SSA22 at z=3.1
Progenitors of massive galaxies in their early formation phase?
Lyα emission is extended due to photo ionization and/or resonant scatteringof the surrounding gas trapped in a massive halo.

40 arcsec= 300kpc

Can we see cold streams (as Lyα filaments) if we go much deeper with TMT?
Matsuda et al. (2011)

Lyα profile

Velocity structure of neutral gas in Lyα blob at z=3

Wilman et al. (2005)

Wavelength (Å)

absorbers = associated HI gas along the line of sight line-of-sight velocity as a function of location  gas inflow/outflow?Resolved Gas-Phase Chemical Evolution
2D map of line ratios(metallicity indicators)
such as[OIII]/Hβ and [NII]/Hα

VLT/SINFONICresci et al. (2010)see also
Jones et al (2010)
With Keck2/OSIRIS

Lower metallicity at the center  Dilution by (almost) metal-free cold streams?

IRIS (IFU: imaging spectroscopy)
FoV=2” (IFU),0.015”@2μm ⇔ ~0.1kpc @z>1

 Spatially resolved star formation (Hα) and chemicalevolution ([NII]/Hα, R23)
・Nucleated starburst (merger-driven)?
or wide-spread star formation over disk (secular evolution)?
・Propagation of star formation/chemical evolution (inside-out)?

 Internal gas kinematics (Hα, [OII], Lyα…)
・Establishment of kinematical morphology?
(rotation or random motion or disordered merger?)・Inflow (cold streams) and Outflow (feedback)?

 AGN activity (BPT diagram at galactic center)
・AGN contribution at center? Is it accompanied by starbursts?

IRMOS (Multi-IFU) will be efficient especially for high density regions.

Emergence of the red sequence (massive-end) at 2<z<3Confirmed proto-clusters (in terms of associated Lyα emitters) around radio galaxies

PKS1138 (z=2.16)

USS0943 (z=2.93)● r-JHK ● b-JHK● DRG(J-K>2.3)

1011 M☉

RG

1011 M☉

Ancestors of massive galaxies in clusters are just vigorously forming between 2<z<3.
Subaru/MOIRCS, Kodama et al. (2007)

Continuum (Balmer/4000Åbreak)redshifts for DRG Kriek et al. (2008)
z=2.3

MUSYC survey, K<19.7(~M*－0.5)
 K~21.5 (Vega, M*-1) with TMTGNIRS on Gemini-S, R=1000, 2-3hrs each
R=1000  SED: R=40-50 (smoothing)⊿z/(1+z) < 0.019 (~6000km/s)

Ultra-Deep Continuum Spectrum of a DRG at z=2.2Hβλ4861Mg
λ5172

Spectrum and HST images of 1255-0 at z = 2.186.
van Dokkum et al. Nature 460, 717-719 (2009)

GNIRS on Gemini-S, 29 hrs
K=19.26 (Vega)
M*=2×1011M☉
 2hrs exposure with TMT !

SED fitting see colored contours

Balmer/4000Å break, Mg2 feature  luminosity weighted age, Av, SFR…
Kriek et al. (2006)

Establishment of Hubble types at 1<z<3?
Observed galaxies at z=3

Simulated galaxies at z=3
based on z=0.4~0.7 galaxies

spheroiddisk

Sersic index

LBG
DRG

effective radius [kpc]Subaru + AO
Spheroidal galaxies are much scarcer at high-z (~3).

Akiyama et al. (2008)

Massive, compact, spheroidal galaxies at z>2

Median stellar mass: 1.7×1011M☉
Median effective radius: 0.9 kpc
Sizes are x5 smaller, and densities are
2 orders higher than nearby ellipticals!

HST/NIC2
Keck/LGS-AO
van Dokkum et al. (2008)

How well can we determine galaxy morphology at high-z?
Sa galaxy at z~0 (SDSS)
Minowa et al. (2004)

g’u’i’

z=1.4

1.9

3.6

5.2r’Conclusionsz<3: ground 20mz>3: space 3.5mz’

2.50.03” = 240pc

Ground-based 20m + AO (K-band)

z=2.9

3.6

6.4

9.0

4.7

0.21” = 1.6kpc

Space 3.5m (L-band)

IRMS (multi-slit spectroscopy)
Imaging: 2’×2’

Spectroscopy: 2’×0.6’, 46 slits

 Morphology and Size Evolution
AO imaging (~0.1kpc) of less massive galaxies (M*<1011M☉)
 merger rate, bulge/disk ratio, size evolution

 Resolving Star Formation History in Finer Time Scale
Hα＋ Balmer absorption ＋ SED ＋ dust correction
107 yr108-9 yr>109 yr(Hα/Hβ)Starburst? Truncation timescale?  Physical mechanisms

 Chemical Evolution of Interstellar Gas[NII]/Hα and ([OII]+[OIII])/Hβ  Metallicity in HII regions

 Co-appearance of AGN with Active Galaxies
BPT diagram  Conditions for AGN (environment and time)Properties

Key Scientific Goals

mass (m)(Galaxy working group)
time (t)environment (ρ )“Sharp Views of Galaxy Formation and Evolution”• SF and MA histories as a function of environment and mass
Relative contributions of SF and MA? How is AGN activity related?

• Emergence/establishment of galaxy morphologies/types
Visual shapes, Internal kinematics of stars and gas (V/σ), Mergers• Internal structures and kinematics of forming galaxies
Population/chemical structure (inside-out), Gas dynamics (inflow/outflow)