TMT-AGE:
TMT Analyzer for
Galaxies in the Early universe
AO-assisted wide-field multi-object
NIR spectrograph concept
Masayuki Akiyama (Tohoku U.)
Yosuke Minowa,Yoshito Ono, Shin Oya (NAOJ)
Kentaro Motohara (Tokyo U.)
Tadayuki Kodama (Tohoku U.),Yusei Koyama (NAOJ)

Three Science Drivers for TMT-AGE
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>6AGN

1. How is the internal structure oflocal galaxies established ?
Turbulent / high surface-density
disks at high-z
Typical galaxy seen in thelocal universe

Very compact
galaxies at high-z

Clumpy galaxies athigh-z

1. How is the internal structure of
local galaxies established ?
Missing information :“stellar dynamics” and its cosmological evolution.
TMT can measure the local stellar dynamics of galaxies at z>1.

Targets of Multi-IFU Observations

2. What is going on in galaxies in the early
universe ?
• TMT observations of rest-frame
UV features of star-forming
galaxies can reveal :– Low-ion IS abs line: Distribution and dynamics ofneutral gas– High-ion IS abs line: Distribution and dynamics ofionized gas– Stellar emission:
 High-mass star contents
Average of rest-UV spectra ofz~3 star-forming galaxies– Nebular emission:
 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.

3. Hunting for galaxies/AGNs
in the early universe• Follow-up spectroscopy of candidates of high-z galaxies / AGNs
picked up by wide-field IR surveys (Euclid, WFIRST, SPICA,,,), andwide-field X-ray surveys (Athena, LYNX,,,) from space.

High-z galaxy survey parameter space• FoV, apparent magnitudes, and continuum spectroscopy limits.

Highly accreting SMBHs
Obscured AGNs at z>6• Depth of >10 sq.deg wide-field surveys in late 2020s X-ray /NIR / FIR compared to the obscured QSO SED.

System Requirements
1. Spatially-resolved spectroscopy of z=1-5 galaxies.
– High spatial and spectral resolution deployable multi-IFU
spectrograph covering (moderately) wide target field.
– 0.05x0.05” sampling IFUs with 2” FoV– R=10,000 spectroscopy for v~30km/s– >10 objects in 5 arcmin diameter FoV
2. Integrated spectroscopy of z>5 galaxies.
3. Follow-up spectroscopy of candidates of z>8 galaxies– Wide-field high-sensitivity (moderate AO correction)
multi-object 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.
– >10 objects in 10 arcmin diameter FoV

Wide-field AO development path
• We kicked-off laser tomography AO experiments with a JSPS
funding as the first step of the wide-field AO systems.

1. Tomography AO correction with 3 NGSs : RAVEN 2. Laser Tomography AO experiment with 4 LGSs : Install 4 LGSs + WFSunitULTIMATE-START
3. Laser Tomography AO correction
 Installing high-order DM

4. Ground-layer AO system : ULTIMATE-Subaru
 Installing adaptive 2ndry

5. Wide-field multi-AO system : TMT-AGE

– 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 spectroscopy binned to R=500– Typical size of z>5 galaxies: effective radius of 0.1”

• 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. 2014,
V-dropout for z~5, i-dropout for z~6, and Y-dropout for z~7