TMT-AGE:
TMT Analyzer
lf Galaxies
forl iin the Earlyy universe
TMT 広視野多天体分光器の可能性
Masayuki Akiyama (Tohoku Univ., Japan)
and TMT-AGE team

Requirements
1. Spatially-resolved spectroscopy of z=1-5 galaxies.
– Highg spatialpand spectralpresolution deployablep ymulti-IFU
spectrograph covering wide target field.
– 0.05x0.05” sampling IFUs with 2” FoV– R=10,000 spectroscopy for v~30km/s
2. Integrated spectroscopy of z>5 galaxies.
3. Follow-upp spectroscopy
ppy of candidates of z>8 ggalaxies– Wide-field high-sensitivity (moderate AO correction) multiobject spectrograph in short NIR wavelength range– 0.3x0.3” – 0.5”x0.5” aperture integrated spectroscopy– R=3,000 (5A resolution, 2A/pix) for absorption/emission
lines with rest-frame EW of 1A.

Early-lighty g 装置群と装置群との比較
比較• IRIS: 近赤外線での IFU (max 2.2”
2.2 x 4.554.55”)) と 34
34” 角の撮像装置。初期補償光学系 NFIRAOS で良く補償される領域をカバーする。
• IRMS: 近赤外線での多スリット分光装置。NFIRAOS で補償された 22ʼ x 0.60 6ʼ の視野をカバの視野をカバーするする。KeckKeck
MOSFIRE のクローン、ただし焦点距離の違いで視野は狭くなる。(分光は 2ʼ x 0.6ʼ, 撮像は 2ʼ x 2ʼ)• TMT-AGE: 近赤外線での multi-IFU (~20個)での多天体分
光装置 広視野 (直径 5ʼ-10ʼ光装置。広視野5ʼ 10ʼ の領域) の補償光学系を新しく設置する。視野を広げる分、IRIS よりも補償性能は劣る。

Three Science Drivers
1. How is the internal structure of local
galaxies established ?
2. What is going on in galaxies in the early
universe ?
3. Hunting for galaxies/AGNs at z>8

1. How is the internal structure oflocal galaxies established ?
Turbulent / High-density
disks at high-z
Typical galaxy seenin the local universe

Veryy compact
pgalaxies athigh-zgClumpy
pygalaxies athigh-zg

1. Galaxy “establishment” history
Example image of a massive galaxy at z=1.0
Even if we put this galaxy at zz=1.5,1.5, TMT IFU
spectroscopy can detect Ha-line / stellar continuum
from the colored regions shown below with 0.2”
resolution

Gas dynamics

Stellar dynamics

with 00.22” resolution

with 0.20 2” resolution

Stellar kinematics of z~2 quiescent massive galaxies•••Integratedgstellar kinematics of qquiescent massive ggalaxies at z~2.
X-shooter 0.9” slit with R=5100 @ 1.4um, 2hour integ.
Jap(1.75”)=21.09 and Jap(1.75”)=20.59 (Should be SN=15 with
J 21 09 aperture loss
J=21.09loff 0.50),0 50) SN=10
SN 10 withi h JJ=21.9)
21 9)

z=1.80J-bandSN~10? per 4A

z=1.46
Y-bandSande et al. 2013

低光度 AGN の探査
補償光学＋面分光観測により明らかになった銀河中心核領域のAGN活動性 Genzel et al.
al 2006
1.2nucleus(θ=1”)

Lyα

1.0flux

6CIV HeII

4CIII]

20normalised flux

81200

1400

1600

1800

[NII]
[SII]

0.6

0.4

0.2

b-0.2
6200

20006400

Hα1.0

[NII]

0.6

6800

disk (θ=0.3” &0 7”N
0.7
N of nucleus)

Hα0.8

normalised flux

normalised flux

0.8nucleus(θ=0.4”)

6600

rest wavelength

rest wavelength
1.0

Hα08
0.800
0.0

anucleus(θ=0.4”)

0.4

[NII]

[NII]

0.6

0.4

0.2

0.2
0.0
0.0

c

-3000

-2000

-0.2
-1000

01000

2000

velocity offset (km/s)

3000

-1000

d-500

0500

velocity offset (km/s)

1000

Targets
gof Multi-IFU Observations4000Ain J-band

Stellar mass
evolution ofmassive
ellipticals~10 objects in
d=10ʼ FoV

~10 objects in
d=5ʼ FoV

Morishita et al. 2015
Number density from MOIRCS Deep Survey results

Stellar mass
evolution ofMW analogs

2. What is going on in galaxies in theearlyl universei?
Average of rest-UV spectra ofz~3 star-forming galaxies• Rest-frame UV features of starforming galaxies– Low-ion IS abs line: Distribution and dynamics ofneutral gas– High-ion IS abs line: Distribution
Di t ib ti andd dynamics
di offionized gas– Stellar emission:
 High-mass star contents– Nebular emission:
Shapley et al. 2003

 Galaxy rest-frameDiagnostic lines for high-z galaxies• Most of the redshifted UV diagnostic lines fall within 7001800A for galaxies at z>5-9.

Sizes of high-z galaxies• z>5 galaxies are compact, but still extended comparedwith the diffraction-limit of TMT.

0.7 kpc
k = 0.13” @z=7-8

0.3 kpc = 0.07” @z=10

Ono et al. 2009

Baseline Detection limits ‒ integrated J-band
J bandPoint source

Galaxies at z>5– Red (MOAO), blue (GLAO), green (seeing-limit) lines show
the detection limits for each system with different aperture size.
– SN=10 for continuum with 10h integration– R=3,000
R=3 000 spectroscopy binned to R=500– Typical size of z>5 galaxies: effective radius of 0.1”

Number density• Red (MOAO), blue (GLAO), green (seeing-limit) lines show
the detection limits for each system.
• Number density of luminous z~6-7 LBGs is not so high.

Filled squares from Bouwens et al.
al 2014,2014
V-dropout for z~5, i-dropout for z~6, and Y-dropout for z~7

3. Hunting
g for ggalaxies/AGNs at z>8• Follow-up spectroscopy of candidates of high-z galaxies / AGNs
pickedi k d up byb wide-field
id fi ld IR surveys (Euclid,(E lid WFIRST,WFIRST SPICA,,,),SPICA )and wide-field X-ray surveys (Athena, STARX,,,) from space.

d~10ʼ~DEIMOSWFIRST 0.28 sq.deg
q g~Suprime-Cam

Nebular line emission
Estimated CIV,, CIII]] line flux for high-zggalaxies
gShimizu et al. 2015

BASELINE DESIGN広視野の補償光学系の実現が鍵• 地表層補償光学系：直径地表層補償光学系 直径 10 分角程度の視野内で、共通の大気揺らぎを補償して、近赤外線で FWHM = 0.2 秒角程度の補償を実現する。
• 多天体補償光学系：直径 5 分角程度の視野内で、それぞれの天体の方向に最適化した補償をして 近赤外線でれの天体の方向に最適化した補償をして、近赤外線でFWHM = 0.05 秒角程度の補償を実現する。
TMT の初期補償光学系 NFIRAOS は、、、
• 多層共役補償光学系：直径 30 秒角程度の視野内で、複数 高さ 大気揺らぎを補償し数の高さの大気揺らぎを補償して、近赤外線で近赤外線 FWHM= 0.02 秒角、TMT の回折限界の補償を実現する。

RAVEN: Subaru Multi-Object AO
engineering
ii andd scienceidemonstratordt t

RAVEN : MOAO demonstration• Simultaneous AO correction for two objects by tomography
estimation with three NGSs within d=3’ FoR.

Lardiere et al. 2014

Ground-layer AO optical design• d=10’ FoV AO optical design.

New Focal PlaneTMT Focal
Plane

Pupil distortion needs to be small to be
used as an AO system.

Pick-off Opt-mechanics
p
Mock-upp• Classical r-theta pick-off arm system.
• 20 pick-off
i k ff arms will
ill beb put aroundd theh correctedd focal
f l plane.
lOptical alignment test is underway

Integral Field Unit optical design• Optical design and prototyoing for the IFU by Yutaro Kitagawa.
Imageg Slicer

Input beamOutputSlit
ImageSlicer
Pupil Mirror

Output Slit

PupilMirror

Prototype of the image slicer optics
made bygriding + coating + ultra-fine polishing.
The unit will be used in TAO/SWIMS
instrument.

IFU spectrograph optical design(F8/F2 5)(F8/F2.5)• Optical design studies for F8/F2.5 spectrograph by Optcraft.
• F2.5 output and slit length of 194mm are achieved.

The camera system require
10 lenses including CaF2 lens with 295mm diameter.

ALTERNATIVE IDEAS

Idea 1: Pick-off arms as “multi-slits”• Pick-off arms can be used as object picker same as multi-slits toconduct multi-object spectroscopy.
• If we consider d=10’ FoV, TMT focal plane is large (d=1320mm).

VLT/KMOS

K k/MOSFIRE
Keck/MOSFIRE

Idea 2: GLAO optical design with
“ h i k d” ffocall plane“shrinked”l• GLAO corrected focal planeis smaller (d=300mm) withffasterF-ratioi (F3.5).
()•Imager / multi-slit MOS /fiber MOS can be put on the“shrunk”
shrunk focal plane.
planeIdea 3: IFU spectrographonl with
onlyith highhigh-resolution
resolution mode (F24/F7(F24/F7.6)
6)• Compared to F8/F2.5
F8/F2 5 spectrograph design,design the slow F
F-ratio
ratio
design is much simpler and more feasible.

Three alternative specificationsp
1. d=10d 10 arcmin multi
multi-pickoff-arm
pickoff arm MOS spectrograph with
GLAO correction (w/o imaging capability)
2. d=10 arcmin imager / MOS instrument with GLAOcorrection with shrunk focal plane
3. d=5 arcmin multi-IFU ((0.05” sampling)p g) spectrographpg p withGLAO+MOAO correction with optimized spectrograph for
high-spatial sampling mode.

Which configuration does your science prefer ?

ULTIMATE-Subaru• 地表層補償光学によるすばる望遠鏡で10分角程度の広視野補償光学系を実現するプロジェクト。TMTの広視野補償光学の開発にもつな広視野補償光学 開発 も ながる。
• 6/16-6/17 ULTIMATE-Subaru
Science workshop を国立天文台三鷹にて行います。詳しくはhttp://www.naoj.org/Projects/newdev/ngao/201606̲ULTIMATE̲WS/を参照ください。
を参照ください議論• z=1-3 の銀河内部構造を分解した分光探査から、どのような物理量を引き出すことが鍵になるか？
– 星の系の速度分散、回転速度？
– 中心核活動性 Seyfert
Seyfert-classclass ?
• z>5 の銀河の分光探査観測から、どんな物理量を引き出すことが鍵になるか？
– ガスの outflow / infall ?
– IMF ?
• TMT を用いた wide-field (d=10ʼ) narrow-bandsurveyery ?
• FoV:oV TMT (d(d=15ʼ-20ʼ)
5 0 ) vsvs. E-ELT (d(d=10ʼ)0 ) vsvs. G
GMT (d(d=20ʼ)0)