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Japanese Research Plan forExploring New Worlds with TMTNorio Narita (NAOJ)on behalf of Japanese Science Working GroupTMT HERE!Science Group MembersStar/Planet FormationT. FujiyoshiM. FukagawaS. HiraharaM. HondaS. InutsukaT. MutoH. NomuraY. OasaT. PyoY. TakagiM. TakamiExoplanetsT. MatsuoN. NaritaB. SatoT. SumiT. Yamashita

Solar SystemY. KasabaT. SekiguchiT. Terai

Science Topics of Star FormationSearch for new interstellar molecules by high-dispersion Mid-IR spectroscopic observationInitial Mass Function (IMF), Masses and Ages of Young StarsThe Solution to The Angular Momentum Problem in Star Formation: Jets and Outflows from Young Stellar ObjectsHigh Mass Star FormationScience Topics of Planet FormationObservation of the Detailed Morphology of Circumstellar DisksObservations of the Spatial Distributions of Dust and Ice Grains in the Protoplanetary DiskMapping the magnetic field in the circumstellar disks by MIR polarimetryObservations of H2 Line Emission to Probe Gas Dispersal Mechanism of Protoplanetary DisksSpatial Distribution of Organic Molecules in Protoplanetary DisksScience Topics of ExoplanetsExoplanet Searches with Precise RV MethodHigh resolution spectroscopy of exoplanet biomarkers at transitsSearch for Biomarkers in Habitable Exoplanet Atmospheres by Multi-Object SpectroscopyHigh Dispersion Spectroscopy of Sodium Atmospheric Absorption in Exoplanet AtmospheresUncovering Migration Mechanisms of Earthlike Planets by the Rossiter-McLaughlin EffectDirect Imaging Survey of Terrestrial Planets in Habitable ZoneStudy of Exoplanet Distribution by Identifying the Host Stars of Planetary Gravitational Microlensing EventsDirect imaging and low resolution spectroscopy of exoplanets in the mid-infraredScience Topics of Solar SystemHigh Spatial Resolution Imaging for Small Solar System Bodies and Dwarf PlanetsHigh Spatial Resolution Imaging for Planets and SatellitesHigh Spectral Resolution Spectroscopy of Atmospheres of Planets and Satellites

Star formation:Molecules in star-forming gas, IMF, High-mass star formation Planet formation:Detailed observations for jets, protoplanetary disks, debris disksExploring Birthplace of PlanetsIMF S106,

Search for new interstellar molecules by high-dispersion Mid-IR spectroscopic observationInitial mass function, masses and ages of young starsThe solution to the angular momentum problem in star formation: Jets and outflows from young stellar objectsMassive star formationObservation of the detailed morphology of circumstellar disksObservations of the spatial distributions of dust and ice grains in the protoplanetary diskMapping the magnetic field in the circumstellar disks by MIR polarimetryObservations of H2 Line emission to probe gas dispersal mechanism of protoplanetary disksSpatial distribution of organic molecules in protoplanetary disks

7Jets from young starsAimsMake clear the origin of the launching mechanism of the young stellar outflows/jets.Understand the evolutional dependence of the characteristics of the outflows/jets from Class 0 to Class III (Time sequence).Probe the origin and difference of the outflows from massive stars to sub-stellar objects (Mass sequence)

MethodHigh-angular-resolution spectroscopy (R>10,000) using AO-fed NIR and MIR IFU

Simulation of early phase of a protostar Machida et al. (2006 2009)

TMT (Class 0, I, II, III)()

8Detailed Structure of Protoplanetary DisksAimsUnderstand planet formation processDirectly image forming planets in disks

ExampleAO imaging for AB Aurigae with SubaruSpatial resolution of 0.06 = 8 AUResolve the inner region, R > 22 AU (0.15)Non-axisymmetric, fine structure may be related to the presence of planets

Hashimoto et al. (2011)

0.06 22 AU 9Method High-angular-resolution imaging in NIR and MIR

PredictionsHydro-dynamical simulations for scattered light imaging at 1.6 mTMT can observeSpiral wake by a Saturn mass planetInner planet-forming regionstemporal change (rotation) of the structures

Planet at R = 30 AU

8.2-mTMTDetailed Structure of Protoplanetary Disks 8-m TMT TMT 0.2 TMT AB Aur 22 AU TMT

H1.65m 140 pc 10000 K 2.3 R 2.5 10-41Mo 10Evolution of dust grains

CenterSWNE

NASA APODAims Understand grain evolution: when, where, how?

MethodSpatially resolved spectroscopy in MIR

Example Subaru MIR spectroscopy for Pictoris (Okamoto et al. 2004)

TMT

Beta Pictoris /COMICS Beta Pic TMT

Okamoto et al. (2004) 0.1mm 2mm 11Evolution of gas in protoplanetary disksAimsUnderstand how gas dissipates from a disk, by measuring gas amount and temperature at each location Obtain spatial distribution of organic molecules in disks

MethodHigh dispersion spectroscopy or IFU observations in NIR and MIR

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

UV, X-rayphotoevaporationaccretionmoleculesH2O

TMT AU 12Exploring (Earth-like) ExoplanetsRV search for new low-mass planetsTransit follow-up studiesGravitational microlensing follow-up studiesDirect imaging studies

Exoplanet Searches with Precise RV MethodPrecise Radial Velocity MeasurementsHigh-dispersion spectrograph with very precise wavelength calibration is requiredUltimate precision depends on S/N of stellar spectrum

Huge aperture of TMT enables us toobserve faint stars with high S/NTargets: low-mass stars, stars in clusters, microlense objects, etc.observe relatively bright stars with ultra high S/N (ultra high precision)Targets: solar-type stars, giants and subgiants, early-type stars etc.14

Detecting Earth-mass Planets in HZM6M5M0K0G0F0Infrared preferredOptical preferred2ME1ME3ME5ME10MERV semi-amplitude of host stars by companions in HZred solidblue dashed15Detecting Earths around Solar-type Stars by Optical-RV Method: TargetsESO 3.6m+HARPS-type3800-6900, R=115,000, Simultaneous Th-Ar methodTexp=900s, =1m/s mv~10Subaru 8.2m+HDS-type5100-5700, R=100,000, Iodine CellTexp=900s, =1m/s mv~10

Texp=1800s, =0.1m/sESO(3.6m)+HARPS-type mv~5--6VLT(8m)+HARPS-type mv~7.5E-ELT(42m)+HARPS-type mv~11Subaru(8.2m)+HDS-type mv~5--6TMT(30m)+HDS-type mv~8.5At least ~1800 s exposure isrequired to average outstellar p-mode oscillationdown to