Japanese Research Plan for Exploring New Worlds with TMT. TMT 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
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Exploring New Worlds with TMT
Norio Narita (NAOJ)
on behalf of Japanese Science Working Group
Molecules in star-forming gas, IMF, High-mass star formation …
Detailed observations for jets, protoplanetary disks, debris disks…
Simulation of early phase of a protostar
Machida et al. (2006 – 2009)
Hashimoto et al. (2011)
Planet at R = 30 AU
← Subaru MIR spectroscopy for Pictoris (Okamoto et al. 2004)
Calculation of H2O distribution in disks
(Heinzeller, Nomura et al. submitted)
RV semi-amplitude of host stars by companions in HZ
At least ~1800 s exposure is
required to average out
stellar p-mode oscillation
down to <0.2 m/s level
(Mayor & Udry 2008)
Data from Lepine et al. (2005)
TMT has many target stars for which we can search for habitable earths.
One can probe atmospheres of transiting exoplanets by comparing spectra between during and out of transits.
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.
○：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 find many planets via this method
Only half of planets have
Need to resolve lens
star to measure lens
and planet’s mass!
Average relative proper motion of lens and source star: μ=6±4mas/yr
Required time to separate by 2×psf:
Condition for detection of
Earth-like (solid) and
Super-Earth planets (dotted)
● Matsuo’s Talk at 2:00 pm on 3rd day
Detection limits for future direct