Yusei Koyama (NAOJ)

From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of

distant galaxies across environment

T. Kodama (NAOJ), K.I. Tadaki (NAOJ), M. Hayashi (Tokyo), I. Tanaka (Subaru), R. Shimakawa

(Sokendai), andMAHALO-Subaru collaboration

TMT science workshop @ Asahi-seimei building, 16/10/2013

Outline

- MAHALO-Subaru quick overview

- Prospects for TMT era (ALOHA-TMT)

- Summary & Conclusions

Thank you !

Hello !

Galaxy properties vs. Environment

ES0

Spiral

High-density

“ Morphology–Density Relation”

red, old, low SF activity

blue, young, high SF activity

Low-density

(Dressler 1980)

MAHALO-Subaru project

Narrow-band Ha/[OII] emission-line survey for 0.4<z<2.5

MApping H-Alpha and Lines of Oxygen with Subaru

Collaborators: T.Kodama (PI), M.Hayashi, K.Tadaki, I.Tanaka, R.Shimakawa

Tadaki+’12Koyama+’13a

Hayashi+’12

z = 30 z = 5

z = 2

z = 3

z = 0z = 1

Subaru: big advantage with wide FoV

Yahagi et al. (2005)M=6×10^14 Msun, 20Mpc×20Mpc (co-moving)

MOIRCS(4’ x 7’)

MOIRCS

Suprime-Cam (34’ x 27’)

High-z structures revealed by MAHALO

(Koyama+11)

(Koyama+10)

(Hayashi+10, 11)

(Tadaki+12)

(Koyama+13)

(Hayashi+12)

z=0.4

z=0.8

z=1.5

z=1.6

z=2.2

z=2.5

Many strong emitters

in z>1.5 cluster cores

SF main sequence is independent of environment out to z~2 (as far as we rely on Ha-based SFR).

(Koyama et al. 2013b, MNRAS, 434, 423)

From rest-frame R-band

photometry+ M/L correction

Fro

m L

(Ha)

+ M

★-

dep

en

den

t d

ust

co

rrect

ion

Beyond the SF Main Sequence(two important caveats)

Dust extinction depends on environment

Cluster SF galaxies tend to be dustier – different SF mode?

z=0.4 HAE sampleA(Ha) from

SFR(IR)/SFR(Ha)

A(Ha) fromA(Ha)-M* relation(calibrated at z=0)

(Koyama et al. 2013b, MNRAS, 434, 423)

“Mass segregation” in z>2 proto-cluster

(Koyama et al. 2013a, MNRAS, 428, 1551)

SF galaxies in z>2 proto-cluster show redder colours and

higher M* (>1011M)

compared to general field

galaxies.

: 24um-source

■ ： red HAE (dusty SF)　　 (J-KAB>1.4, DRG)■ ： green HAE 　 (0.8<J-KAB<1.4) ■ ： blue HAE (J-KAB<0.8)

Towards the TMT era

ALOHA-TMTAnatomy with Lines of Oxygen

and Hydrogen with AO on TMT

cluster phenomena !

HST/i-band snapshots (4”x4”=30 kpc for each)

z=2.2 HAEs in PKS1138

M: 24um source X: X-ray source

(Koyama et al. 2013a)

HST morphologies of Ha emitters at z=2

z~2 proto-cluster galaxies (rest-UV)

rest-UVHa

Ha

(seeing)

(seeing)

Ha emitters at z=2.5 in SXDF/CANDELS from Tadaki et al. (2013)

red clum

p rest-UV

HST image(ACS+WFC

3)

HST image(ACS+WFC

3)

Deep TMT+IFU observation will allow us to map Ha/Hb ratio (i.e. extinction map)

over the galaxies.

ALOHA [1]: (Dust-corrected) Ha mapping

Ha-strong (but UV-faint)

dusty red clumps.

Responsible for major SF activity

in these galaxies?

ALOHA [2]: Spatially-resolved line ratios

Pixel-by-pixel BPT diagram from SINFONI+AO observation (Newman et al. 2013)

Mapping multiple emission-lines over the galaxies allow us to unveil central AGN, metallicity gradient, excitation state… etc. AGN in the central

regionPurely star-forming

Redder symbols show galaxy central pixels

Recent discovery: high-z clumpy (field) galaxies are disk-rotating.

ALOHA [3] : Galaxy dynamics with IFU

Shapiro et al. (2008)

Disk/merger classification

with “kinemetry”

merger

disk

Genzel et al. (2006)

Forster-Schreiber et al. (2011)

Is it really true for high-z “cluster” galaxies as well?

Proto-cluster (z=2)

General Field (z=2)

rest-UV (ACS) rest-UV (ACS)

Tadaki et al. (2013) Koyama et al. (2013)

ALOHA-TMT will give us a direct answer !!

ALOHA [3] : Galaxy dynamics with IFU

(and for more normal, low-mass galaxies?)

Summary

(2) Using MAHALO sample, we find that SF main sequence is independent of environment at any time in the history of the universe since z~2 (as far as we rely on the Ha-based SFRs).

(4) SF galaxies in z~2 proto-cluster environments tend to be more massive (and have higher SFR) than the field counterparts.(5) High-z galaxies are clumpy (both in clusters and fields). ALOHA-TMT will reveal the environmental impacts on the internal physics of high-z galaxies with deep IFU observation.

(1) MAHALO-Subaru unveiled large-scale structures at z>>1 with wide-field emission-line galaxy survey with Subaru.

(3) SF galaxies in cluster environments may be more highly obscured by dust – implying a different mode of SF activity from general field galaxies.