TMT-AGE:
TMT
AGE:
Wide field of regard multi-object
adaptive optics forf TMT
Masayuki Akiyama (Tohoku Univ.)
Shin Oya (Subaru), Yoshito Ono (Subaru/Tohoku U.),
Hideki Takami (NAOJ), Shinobu Ozaki (NAOJ),
Yutaka Hayano (Subaru), Ikuru Iwata (Subaru),
K
Kazuhirohi HaneH(T h k U(TohokuU.),) TTong W
Wu (T(Tohokuh k UU.),)
Tomoyasu Yamamuro (Opt Craft),
Yuji Ikeda (Photocoding)TMT-AGE:
TMT Analyzer
Anal e fofor Galaxies
Gala ies in the Early
Ea l universe
ni e se• Multi-IFU NIR spectroscopy
ppy of ~20 objects
jscattered in wide(d=10ʼ) Field of Regard (FoR) assisted by MOAO correction

TMT-AGESCIENCE DRIVERSTMT-AGEThree Science Drivers

1. Revealing the history of establishment of the internal
structure of galaxies– By spatially-resolved spectroscopy of z=1-5 galaxies.
2. Revealing the violent star-formation process during theformation phase of galaxies– By integrated spectroscopy of z>5 galaxies.
3. Identifying galaxies in the early universe (z>8)– By follow-up
follow up spectroscopy of candidates picked up by
future wide-field IR surveys (Euclid, WFIRST, WISH,,,)
from space.
pTMT-AGE

1. Galaxy “establishment” history
Example: a massive galaxy at z=1.30.06” pixel map with FWHM=0.18” (HST H-bandFWHM) (FWHM=0.067”(FWHM 0.067 with JWST)
10h, SN=10, R=3,000 detection limit:
H-band continuum detection limit corresponds
to 6x109 Ms/kpc2
H-band unresolved line limit corresponds to 0.06
Ms/yr/kpc2
Star-formation rate distributionStellar mass distribution

2” FoV

100x100 = 6”x6”

Masuda 2014
Master Thesis

100x100 = 6”x6”

TMT-AGE

2. Understanding star-formation
in young galaxies

Average of rest-UV spectraof Z~3 star-forming galaxies• Rest-frame UV features of starforming galaxies– Low-ion IS abs line: Distribution and dynamics ofneutralt l gas– High-ion IS abs line: Distribution and dynamics ofionized gas– Stellar emission:
 High-mass star contents– Nebular emission:
Shapley et al. 2003

 Galaxy rest-frameTMT-AGE

3. Identify
y galaxies
gat z>8• Follow-up spectroscopy ofcandidates picked up
pbby ffuturet rewide-field (>10sq.deg) IR imaging
surveys (Euclid,(Euclid WFIRST,WFIRST WISH,,,)WISH )
from space.
www.wishmission.org

TMT-AGE

Diagnostic lines for high-z galaxies• Most of the redshifted diagnostic lines can be covered
within 7000-18000A.

TMT-AGE

Baseline Detection limits ‒ integrated J-band
J bandPoint source

Galaxies at z>5– Red (MOAO), blue (GLAO), green (seeing-limit) lines show thedetection 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”

TMT-AGE

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

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

TMT-AGE

Requirements

1. Spatially-resolved spectroscopy of z=1-5 galaxies.
– Highg spatial
pand spectral
presolution multi-IFUspectrograph within d=5ʼ FoR (IRMOS-like)– 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-up
p spectroscopyp
py of candidates of z>8 galaxies
g– High-sensitivity with moderate AO correction in short
NIR wavelength range within d=10ʼ FoR– 0.3x0.3” ‒ 0.5”x0.5” aperture integrated spectroscopy– R=3,000 (5A resolution, 2A/pix) forabsorption/emission lines with rest-frame EW of 1A.

TMT-AGE

MOAO PERFORMANCE FEASIBILITYWITHIN A WIDE FORTMT-AGE

AO performance simulation• We check AO performance feasibility within d=10ʼ FoR
with end-to-end AO simulator MAOS (Wang & Ellerbroek
2012) .
• We consider 6 LGS case and 8 LGS case with changing
th radius
thedi off th
the asterismt i(th(those are withinithi theth scope off
the TMT-LGSF specification [Subsystem RequirementsDocument]).
Document])

TMT-AGE

Ensquared E. Within 0.05x0.05”

6 LGS case (red arrows indicate the radius of LGS asterism)

8 LGS case (red arrows indicate the radii of LGS asterism)

LGS asterism in IRMOS

From top to bottom, K, H, J, 0.9um

TMT-AGE

Ensquared E. within 0.2”x0.2”

6 LGS case (red arrows indicate the radius of LGS asterism)

8 LGS case (red arrows indicate the radii of LGS asterism)

LGS asterism in IRMOS

From top to bottom, K, H, J, 0.9um

TMT-AGE

Good AO correction wide FoR• There is a possibility that good AO correction can be achieved
even within d=8ʼ-10ʼ FoR with a new tomography algorithm
utilizing wind profile (direction and speed) information

See poster by Y.Ono et al. 9148-258 on ThursdayTMT-AGESYSTEM CONSIDERATIONMOAO SYSTEM DESIGN AND REQUIREMENTS FOR DMSOPTICAL DESIGN FOR A COMMON DM SYSTEMTMT-AGE

Stroke Requirements for DMs• Th
Three configurations
fii
are considered
id d– A) One 60x60 DM for each science path– B) Small Woofer (30x30) and Tweeter (60x60) DMs foreach science path– C) Large
Lcommon (30x30)(30 30) DM andd 60x60
60 60 DM forf eachhscience path. Common DM corrects for common
turbulence with in the wide FoR,
FoR like Ground
Ground-Layer
Layer AO.
AO
30x30 DM
PV60x60 DM
IAAPV

IA

5.5 (10.0)

2.5 (4.0)B

5.5 (10.0)

2.5 (4.5)

1.0 (2.0)

1.0 (1.5)C

5.0 (8.0)

2.5 (3.5)

3.0 (5.5)

1.0 (2.0)

Zenith Distance with r0=0.156 (ZD=60 with r0=0.121)
Red: requirements larger than current MEMS DM

TMT-AGE

Optical designs
for the common DM system
yScience pick-off• At first, we consider
modified Offner system,s stem
following IRMOS-Tipi
design.
design• Extendig FoR to d=10ʼ.
• Modified Offner system byOptcraft (T.Y.)

TMT-AGE••

Performance

Wavefront at pickoff focal plane
For each FoR position••

Pupil image distortion at DM plane
For each pupil position

TMT-AGE

Optical designs
for the common DM systemDM• Three Mirror Arrayy designgwith free form curve
mirrors by Photocoding(Y I )(Y.I.)• O
Overallll system size
i iis
about half of the size ofthe modified Offnerdesign.

Science pick-off1.7m

TMT-AGESTATUS OF RELATED DEVELOPMENTSWFS FOR MOAO SYSTEMMEMS DMTOMOGRAPHY WITH GPU

LGS-WFS for MOAO system

TMT-AGE•Because off thB
the elongation
lti off th
the SHSH-WFSWFS spotst forf LGS,
LGS 0.4”
0 4” samplingli5” sub-sperture FoV is necessary. The FoV can cover the large spot
wondering for the open-loop MOAO system.

•We test centroiding with parallel calculation with GPGPU. Sufficiently
fast centroiding can be done for 60x60 WFS with 10x10 subaperture.
Reqquire time forCentroidding(ms))

0.20.10C2070
448 cores
1.15GHz•GTX Titan
2880 cores
0.93GHzK402880 cores
0.88 GHz

We tested data transfer between EM-CCD
EM CCD CCD60 (E2V) readout withNuvu camera CCCP electronics and GPGPU.

TMT-AGE•

MEMS DM with bimorph spring structure

P t tPrototype
withith 44x44 elementslt

W ett al.l 2013,Wu
2013
J.Micromech.Microeng, 23, 125003

TMT-AGE

Tomographic estimation with GPGPU

Solving Minimum Variance Reconstructer for 7 layer atmosphere with 860x60 LGS WFS system by Conjugate Gradient method (see Ono et al. 9148258 p
poster Thursday).
y)
We try two setups with Nvidia C2070 and GTX Titan. 300 iterations arerequiredqto converge
g the solution from zero initial gguess. The number canbe reduced to ~5 with using the solution from previous time-step as theintial guess.
Currently both boards are installed with PCIe2.0 bus, and data transfer time
can be reduced by 1.5 with using PCIe 3.0 setup.
C2070
Transfer data to GPU

0.2 ms

One iteration of C.G.

5.57 ms

Transfer data from GPU

0.4 msTotal with 300 iterations~1700 ms

GTX Titan

0.73 ms~200 ms

TMT-AGE

Summary

Moderate correction in wide FoR (d(d~10ʼ)
10 ) is important forhigh sensitivity spectroscopy of faint targets.
Such correction can be achieved with the current
tomography algorithm. Better correction can beachieved with a new algorithm with wind profile
information (see Y.Ono poster on Thu. 9148-258).
There are solutions for the common DM optical design FoRof d~10ʼ.
We will complete the concept proposal by end of FY 2015.

Requirements for 1<z<5 galaxies
High spatial and spectral resolution wide-wavelength
coverage• Velocity resolution of 30km/s R=10,000 (1A resolution,0 5A/pix) stellar dynamics in bulge/disk region
0.5A/pix)• 90009000-16000A
16000A coverage (14(14,000pix)
000pix) for z=1.4
z=1 4• 12000-22000A coverage (20,000pix) for z=2.4• 16000
16000-22000A
22000A coverage (12(12,000pix)
000pix) for z=3.4
z=3 4• 0.05”x0.05”
0.05 x0.05 aperture IFU spectroscopy• Size of FoV for each IFU : ~2” for the continuum
spectroscopy for the most massive galaxies.
• More extended region (~5”) can be detected by emission
line spectroscopyRequirements for z>5 galaxies
Moderate corrections in short NIR wavelength range.
• 0.3x0.3” ‒ 0.5”x0.5” aperture integrated spectroscopy• Size : re=0.1” : 2re diameter=0.4”• FoV 1” is sufficient• 7000-13500A coverage (3300pix) for z=5.0-6.0• 9000-18000A coverage (4500pix) for z=6.5-8.5• R=3,000 (5A resolution, 2A/pix) for absorption/emission
lines with rest-frame EW of 1A.

1. Galaxy “establishment” history• Revealing gas and stellar dynamics, internal metallicity
distribution byy spatially-resolved
pyspectroscopyp
py of z=1-4galaxies.
• Diagnostic lines = [NII]/Ha, [OIII]/Hb, 4000A break,Balmer break, [OII]• All of the features are observable at– zz~1
1.4
4 (9000(9000-16000)
16000)– z~2.4 (12000-22000)• Without [NII]/Ha– z~3.4 (16000-22000)• Without [[NII]/Ha,], [[OIII]]– z~5.0 (22000)

Baseline Detection limits ‒ spatially-resolved••

Detection limits in 0.05”x0.05” aperture
SN=10 in 10h integration with 22% throughput (atm-tel-inst-det) and 1eRoN•

R=3,000 flux density corresponds to– JAB= 27.64mag, HAB=27.74 mag, KAB= 26.68mag– H-band limit : stellar mass of ~1x108 Ms/pix ~ 6x108 Ms/kpc2 at z~1– HH-band
band limit : stellar mass of ~1x10
1x109 Ms/pix ~ 6x109 Ms/kpc2 at z~1z 1.33•

R=3,000 line flux corresponds to– SFR = 00.002
002 Ms/yr/pix
M / / i = 0.012
0 012 Ms/yr/kpc
M / /k 2 forf z=1.5
1 5 HaH emissioni i lineli– SFR = 0.01 Ms/yr = 0.06 Ms/yr/kpc2 for z=2.5 Ha emission line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

Maximum (20 objects 4Kx4K each)• 0.01”/pix with 0.02”/slice– 1x0.8” FoV = 100 pix/slice x 40 slices = 4000 pix• 0.02”/pix with 0.05”/slice– 2x2” FoV = 100pix/slice x 40 slices = 4000 pix• 0.05” / pix with
h 0.05”/slice
l– 5x2” FoV = 100pix/slice x 40 slices = 4000 pix• 0.1”/pix0 1”/ i with
ith 00.2”/slice2”/ li– 10x8” FoV = 100 pix/slice x 40 slices = 4000 pix• R=3,000 (5A resolution) with 2A/pix 8000A coverage =(J+H), (H+K)• R=5,000 (3A resolution) with 1A/pix 4000A coverage = (J),(H), (K)IFU sampling (20 objects 1Kx1K each)
For spatially-resolved spectroscopy of 1<z<5 galaxies• 0.05” / pix with 0.05”/slice– 2.5x1” FoV = 50pix/slice x 20 slices = 1000 pix
For integrated spectroscopy of z>5 galaxies• 0.1”/pix with 0.2”/slice– 1x2” FoV = 10 p
pix/slice x 10 slices = 100 ppix
– Dithering within the IFU FoV.

TMT-AGE:
TMT Analyzer for Galaxies in the Early universe• Put more emphasis on science cases for very high-redshift
galaxies (z>5)– The targets are faint– Low number density at the TMT detection limit• In order to maximize the efficiency of observation for
statistical number of targets, we consider FoR as wide asd 10
d=10ʼ
– Compared to previous MOAO concept studies for TMT((IRMOS-UF/HIA,, IRMOS-Tipi)p ) with d=5ʼ