Japanese Research Plan for

Exploring New Worlds with TMTTMT HERE!

Norio Narita (NAOJ)
on behalf of Japanese Science Working GroupScience Group Members
Star/Planet Formation• T. Fujiyoshi• M. Fukagawa• S. Hirahara• M. Honda• S. Inutsuka• T. Muto• H. Nomura• Y. Oasa• T. Pyo• Y. Takagi• M. Takami

Exoplanets• T. Matsuo• N. Narita• B. Sato• T. Sumi• T. Yamashita

Solar System• Y. Kasaba• T. Sekiguchi• T. Terai

Science Topics of Star Formation
1. Search for new interstellar molecules by high-dispersion Mid-IR

spectroscopic observation
2. Initial Mass Function (IMF), Masses and Ages of Young Stars
3. The Solution to The Angular Momentum Problem in Star Formation:

Jets and Outflows from Young Stellar Objects
4. High Mass Star Formation

Science Topics of Planet Formation
1. Observation of the Detailed Morphology of Circumstellar Disks

2. Observations of the Spatial Distributions of Dust and Ice Grains inthe Protoplanetary Disk
3. Mapping the magnetic field in the circumstellar disks by MIR

polarimetry
4. Observations of H2 Line Emission to Probe Gas Dispersal
Mechanism of Protoplanetary Disks
5. Spatial Distribution of Organic Molecules in Protoplanetary Disks

Science Topics of Exoplanets
1. Exoplanet Searches with Precise RV Method

2. High resolution spectroscopy of exoplanet biomarkers at transits
3. Search for Biomarkers in Habitable Exoplanet Atmospheres byMulti-Object Spectroscopy
4. High Dispersion Spectroscopy of Sodium Atmospheric Absorption inExoplanet Atmospheres
5. Uncovering Migration Mechanisms of Earth–like Planets by the
Rossiter-McLaughlin Effect

6. Direct Imaging Survey of Terrestrial Planets in Habitable Zone
7. Study of Exoplanet Distribution by Identifying the Host Stars ofPlanetary Gravitational Microlensing Events
8. Direct imaging and low resolution spectroscopy of exoplanets in themid-infrared

Science Topics of Solar System
1. High Spatial Resolution Imaging for Small Solar System Bodies andDwarf Planets
2. High Spatial Resolution Imaging for Planets and Satellites
3. High Spectral Resolution Spectroscopy of Atmospheres of Planetsand Satellites

Exploring Birthplace of Planets
Star formation:
Molecules in star-forminggas, IMF, High-mass starformation …

Planet formation:
Detailed observations forjets, protoplanetary disks,debris disks…

Jets from young starsAims• Make clear the origin of thelaunching mechanism of theyoung stellar outflows/jets.
• Understand the evolutional
dependence of thecharacteristics of theoutflows/jets from Class 0 toClass III (Time sequence).
• Probe the origin and difference ofthe outflows from massive stars
to sub-stellar objects (Masssequence)
Method• High-angular-resolution
spectroscopy (R>10,000) using
AO-fed NIR and MIR IFU

Simulation of early phase of aprotostar
Machida et al. (2006 – 2009)

Detailed Structure of Protoplanetary Disks
Aims• Understand planet
formation process• Directly image forming
planets in disks
Example• AO imaging for AB Aurigaewith Subaru• Spatial resolution of 0.”06= 8 AU• Resolve the inner region, R> 22 AU (0.”15)• Non-axisymmetric, finestructure may be related
to the presence of planets

Hashimoto et al. (2011)

Detailed Structure of Protoplanetary Disks
Planet at R = 30 AU

Method• High-angular-resolution
imaging in NIR and MIR
Predictions• Hydro-dynamical simulations
for scattered light imaging at
1.6 μm• TMT can observe…
– Spiral wake by a Saturnmass planet– Inner planet-forming
regions– temporal change (rotation)of the structures

8.2-m

TMT

Evolution ofdust grains
Aims
 Understand grain
evolution: when,where, how?

NASA APOD

NECenterSW

Method Spatially resolved
spectroscopy inMIR
Example← Subaru MIR
spectroscopy for 
Pictoris (Okamoto etal. 2004)

Evolution of gas in protoplanetary disks
Aims• Understand how gas
dissipates from a disk, bymeasuring gas amountand temperature at eachlocation• Obtain spatial distributionof organic molecules indisks
Method• High dispersion
spectroscopy or IFU
observations in NIR andMIRphotoevaporation
UV, X-rayaccretion
molecules

Calculation of H2O distribution in disks(Heinzeller, Nomura et al. submitted)

Exploring (Earth-like) Exoplanets• RV search for new low-mass planets• Transit follow-up studies• Gravitational microlensing follow-up studies• Direct imaging studies

Exoplanet Searches with Precise RV Method• Precise Radial Velocity Measurements– High-dispersion spectrograph with very precise wavelength
calibration is required– Ultimate precision depends on S/N of stellar spectrum• Huge aperture of TMT enables us to– observe faint stars with high S/N– Targets: low-mass stars, stars in clusters, microlense objects,etc.

– observe relatively bright stars with ultra high S/N (ultrahigh precision)– Targets: solar-type stars, giants and subgiants, early-typestars etc.

Detecting Earth-mass Planets in HZ
RV semi-amplitude of host stars by companions in HZ
Infrared preferred

red solid

Optical preferred

blue dashed

10ME
5ME
3ME
2ME
1ME

M6

M5

M0 K0

G0 F0

Detecting Earths around Solar-type Stars byOptical-RV Method: Targets• ESO 3.6m+HARPS-type– 3800-6900Å, R=115,000, Simultaneous Th-Ar method– Texp=900s, σ=1m/s  mv~10• Subaru 8.2m+HDS-type– 5100-5700Å, R=100,000, Iodine Cell
– Texp=900s, σ=1m/s  mv~10• Texp=1800s, σ=0.1m/s– ESO(3.6m)+HARPS-type  mv~5--6– VLT(8m)+HARPS-type  mv~7.5– E-ELT(42m)+HARPS-type  mv~11– Subaru(8.2m)+HDS-type  mv~5--6– TMT(30m)+HDS-type  mv~8.5

At least ~1800 s exposure isrequired to average out
stellar p-mode oscillationdown to <0.2 m/s level(Mayor & Udry 2008)

Searching for Habitable Earths around
M Stars by IR-RV Method: Targets
Data from Lepine et al. (2005)
400

350

Mv=130.3M 

3001630 stars

250

Subaru5<=J<10200
150

Mv=16
0.1M 

100
50
0350
Number of stars

Number of stars

4002871 stars

300
250

5<=J<12200150
100
50
08

910

111213

14

15

16

1718

1920

8

910

11

1213MV

15

16

1718

1920MV400

400

2534 stars

300
250

5<=J<11200150
100

250
150
100

001011121314MV

15

16

1718

19

205<=J<142005093039 stars

300

508TMT350
Number of stars

350
Number of stars

148910111213141516171819MV

TMT has many target stars for which we can search for habitable earths.

20Planetary Transit Follow-up• Transmission spectroscopy– method to observe exoplanetary atmospheres• high spectral resolution (HROS, NIRES, etc)
• MOS (WFOS/MOBIE, IRMOS etc)

• Rossiter effect– method to observe exoplanetary orbital tilts• precise RV measurements during transits

Transmission SpectroscopystarOne can probe atmospheres of transiting exoplanets bycomparing spectra between during and out of transits.

Targets and Methods• Target Stars: Earth-like planets in HZ– M stars: favorable– Solar-type stars: difficult• Target lines– molecule lines in NIR– oxygen A lines– sodium D lines• Methods– High Dispersion Spectroscopy– Multi-Object Spectroscopy

Rossiter effect of transiting planetsstar
planetplanet

the planet hides an approaching side
→ the star appears to be receding

the planet hides a receding side
→ the star appears to be approaching

One can measure the obliquity of the planetary orbit
relative to the stellar spin.

The obliquity can tell us orbital evolution mechanisms of exoplanets.

What we learned from the Rossiter effect For Jovian planets, tilted or retrograde planets are not so rare
(1/3 planets are tilted)
 How about low-mass planets?

Detectability of the Rossiter effectCurrentOpt. RVSubaru
IR RV

TMT IR(1m/s)TMT opt.
(0.1m/s)

F, G, K
Jupiter○○○○F, G, K
Neptune△△○○F, G, K
Earth×××○

M
Jupiter△○○○M
Neptune△○○○MEarth×△○△○：mostly possible, △：partially possible, ×：very difficult

Planetary Microlensing Follow-up

Ground-based surveys (e.g., OGLE,MOA) and future space-based
survey (e.g. WFIRST) will findmany planets via this method

Planet Distribution•RV•transit•Direct image•Microlensing：
Mass measurements
Mass by Bayesian

Only half of planets havemass measurements.
Need to resolve lensstar to measure lensand planet’s mass!

TMT can resolve source and lens star
Average relative proper motion of lens and source star: μ=6±4mas/yr
Resolution:•1.2x2.2μm/8.2m= 66mas(~80mass in VLT/NACO and Keck AO)•1.2x2.2μm/30m=18mass

Required time to separate by 2×psf:
8.2m: T8.2= 22+44-9 yr
30m: T30 = 6+12-2 yr

Direct Imaging• TMT/PFI can resolve outer side of planetary systems• Also, TMT may be able to detect a second Eartharound late-type stars

Second-Earth Imager for TMT (SEIT)- the first instrument for direct detection of “1” Earth-mass planets.
- A novel concept for high contrast imaging with ground-based telescopes- PFI has a general instrument for exoplanet and disk studies
 SEIT is complement with PFI (*NOT* competitive) 1.E-06● Matsuo’s Talk at 2:00 pm on 3rd day

Science Driver

Contrast
Inner working
Angle

PFI

Imaging of Earth-likeplanets

Imaging of reflected
gas giants
Imaging of finestructure of disks10-8 at 0”.010”.01(1.5l/D at 1.0µm)

10-8 at 0”.01
10-9 at 0”.10”.03(3l/D at1.6µm)

Contrast

SEIT

1.E-07

1.E-08Subaru/HiCIAO

Condition for detection ofEarth-like (solid) andSuper-Earth planets (dotted)
SEIT
TMT/PFI

1.E-09E-ELT/EPICS

1.E-100.01

0.1
Separation Angle (arcsec)

1Detection limits for future direct28
imaging projects

Exploring Our Solar System• High spatial resolution imaging for comets, small
solar system bodies, dwarf planets, planets andtheir satellites• High spectral resolution spectroscopy of coma ofcomets, atmospheres of planets and satellites

High Spatial Resolution Imaging for Small
Solar System Bodies and Dwarf Planets- Detection of binary systems  mass- Disk-resolved imaging
 size, shape, and spin density, albedo, and thermal inertia
Investigation of inner structure and compositions
22 Kalliope

Linus

9 MetisVLT + NACO

Keck + NIRC-2

Marchis et al. (2008)

Marchis et al. (2006)

TMT + IRIS + AO observations
Angular resolution: 0.015”

planetarysatellites

10000(2.2μm)- 800 main-belt asteroids
down to 20-km diameter1000

dwarfplanets

100

main belt

Disk-resolved imaging for

Diameter (km)Ceres

10- Satellites of the giant planets

Pluto
CharonEris
Haumea1- Most dwarf planets in theouter Solar system

110100

Heliocentric distance (AU)Expected production(i) Density and porosity
 Inner structure (monolith orrubble-pile)(ii) Irregular shape and craters
 History of impact excavationand disruption

Vesta

HST imageElevation

Thomas et al. (1997)

Geologic mapping of Vesta(iii) Surface inhomogeneity
 Exposure of subsurface material?
Rubble-pile structure?
Thermal metamorphism?
Zeller et al. (2005)

Summary• We have studied about 20 science cases and theirfeasibility for exploring new worlds, based on thecurrent performance handbook• One new instrument (SEIT) will be proposed from aJapanese team for exoplanet studies• We hope to make wide collaborations with other
TMT partners!!