SCIENCE with SPICA SPace Infrared Telescope for Cosmology and Astrophysics

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SCIENCE with SPICA (SPace Infrared Telescope for
Cosmology and Astrophysics
M. Tamura (NAOJ) SPICA Science Working Group
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Todays talk

• - SPICA Science working
• - Science Proposal
• - Possible Key Sciences
• - Several other topics
• - Instrument requirement summary

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Current SWG Member

• Enya, Keigo ISAS/JAXA
• Hasegawa, Naoshi ISAS/JAXA
• Kaneda, Hidehiro ISAS/JAXA
• Kataza, Hirokazu ISAS/JAXA
• Kitamura, Yoshimi ISAS/JAXA
• Matsuhara, Hideo ISAS/JAXA
• Matsumoto, Toshio ISAS/JAXA
• Nakagawa, Takao ISAS/JAXA
• Yamamura, Issei ISAS/JAXA
• Hayashi, Masahiko NAOJ/NINS
• Imanishi, Masatoshi NAOJ/NINS
• Izumiura, Hideyuki NAOJ/NINS
• Kodama, Tadayuki NAOJ/NINS
• Kokubo, Ei-ichiro NAOJ/NINS
• Nakajima, Tadashi NAOJ/NINS
• Omukai, Kazuyuki NAOJ/NINS
• Pyo, T. S. NAOJ/NINS
• Sekiguchi, Tomohiko NAOJ/NINS
• Tamura, Motohide NAOJ/NINS

Nishi, Ryo-ichi Niigata University Okamoto,
Yoshiko Tsukuba University Fukagawa, Misato The
University of Tokyo Honda, Mitsuhiko The
University of Tokyo Miyata, Takashi The
University of Tokyo Onaka, Takashi The University
of Tokyo Ueno, Munetaka The University of Tokyo
Ida, Shigeru Tokyo Inst. of Technology Susa,
Hajime Rikkyo University Hirao, Takanori Nagoya
University Otsubo, Takafumi Nagoya
University Sugitani, Kohji Nagoya City
College Inutsuka, Syuichiro Kyoto
University Kamaya, Fumihide Kyoto
University Nagata, Tetsuya Kyoto University
Aikawa, Yuri Kobe University Kawabata,
Kohji Hiroshima University Kawakita, Hideo Gunma
Observatory
40 people from ISAS/NAOJ/Universities as of
2004.10.12 (not complete sorry)
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Cosmic History

• 2.1. Galaxy Formation and Evolution
• 2.1.1. Current Status of Extragalactic
  Researches
• 2.1.2. First Object and Reionization
• 2.1.2.1. Cooling by Molecular Hydrogen
• 2.1.2.2. Development of Reionization traced by
  Ha
• 2.1.3. Dusty Forming Galaxies
• 2.1.3.1. Internal Kinematics and Physics
• 2.1.3.2. First Star Formation and Chemistry
• 2.1.4. Basic Structure of Galaxies
• 2.1.4.1. Appearance and Development of
  Morphology
• 2.1.4.2. Mass Assembly and Star Formation
  History
• 2.1.5. Cosmic Large Scale Structure
• 2.1.6. Cosmic Background Radiation
• (Nishi, Susa, Kodama, Yamada, Matsuhara, Yoshida,
  Omukai, etc.)
• 2.2. Active Galactic Nuclei
• (Imanishi, Nakagawa, etc.)

This topic to be covered by Matsuhara, Imanishi,
Yamada.
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Star Formation and Evolution

• 2.3. Star Formation and Evolution
• 2.3.1. Star Formation in Our Galaxy
• 2.3.1.1. Low-mass Star Formation
• 2.3.1.2. Outflows
• 2.3.1.3. High- and Intermediate-mass Star
  Formation
• 2.3.1.4. Triggered Star Formation
• 2.3.1.5. Star Formation in the Galactic Center
• 2.1.1.6. Cluster Formation
• 2.1.1.7. Interstellar Matter
• 2.3.2. Star Formation in Nearby Galaxies and
  Super Star Clusters
• 2.3.3. IMF and Stellar Populations
• 2.3.4. Interstellar Chemistry
• (Tamura, Hayashi, Pyo, Okamoto, Sugitani, Nagata,
  Inutsuka,
• Imanishi, Kamaya, Aikawa)

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Very Low-Mass Stars Star Death

• 2.4. Very Low-Mass Stars and Star Death
• 2.4.1. Very Low-Mass Stars
• 2.4.1.1. Brown Dwarfs
• 2.4.1.2. Sub-Brown Dwarfs
• (Nakajima, Tamura)
• 2.4.2. Star Death
• 2.4.2.1. Low-Mass Stars
• 2.4.2.2. Mass Outflows
• 2.4.2.3. High-Mass Stars
• 2.4.2.4. Recycles of Dust
• (Izumiura, Yamamura, Onaka, Miyata, Kawabata)

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Planet Formation and Evolution

• 2.5. Planet Formation and Evolution
• 2.5.1. Protoplanetary Disks
• 2.5.2. Debris Disks
• 2.5.3. Extrasolar Planets
• (Tamura, Ida, Fukagawa, Hirao, Honda, Kokubo)

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Solar System

• 2.6. Solar System
• 2.6.1. Comets
• 2.6.2. Minor Planets
• 2.6.3. Interplanetary Dust
• 2.6.4. Small Icy Objects
• 2.6.5. Minor Bodies
• (Watanabe, Hasegawa, Kawakita, Furusyo, Sato,
  Sekiguchi, Kasuga, Otsubo)

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Several Possible Key Sciences
Extra-Solar Planets Astro-Mineralogy Astro-Organic
-Chemistry
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Extrasolar Planets
High sensitivity High Spatial Resolution High
contrast
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Direct Detection

• Next milestone in extrasolar planet researches.
• The younger, the better (brighter and less
  contrast).
• Very young giant planets will be detected from
  ground.
• SPICA has an enough sensitivity for more
  general planets, but resolution/contrast needs
  to be overcome by technically or target selection.

FLUX
LUMINOSITY
stars
Sun
brown dwarfs
planets
J
E
0.1 1 10 100 micron 1M 10M
100M 1G 10Gyr
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Extrasolar Planets

• SPICA will target direct observations of
  self-luminous planets at rgta few to 20 AU of
  nearby (lt10pc) stars. The detectable planets
  depend on their mass, ages, and separation. If we
  assume the inner working distance of 3?/D, then

Wavelength Detectable Planets at 10pc ?5
micron 1 Gyr 2 M(Jupiter) , r?9AU 30 G-M
target stars ?20 micron 5 Gyr 2 M(Jupiter),
r?36AU 150 G-M target stars
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Extrasolar Planets

• SPICA Sensitivity in a perfect coronagraph mode.
• Cold BD Gl229B
• 1 Jupiter mass object of 10Myr, 100Myr, and 1 Gyr
  at d10pc.
• Comparison with Subaru 8.2m NIR and MIR
  sensitivity.

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Extrasolar Planets

• Young planets and sub-brown dwarfs in nearby star
  forming regions and cold brown dwarfs are also
  good targets.
• cf. Voyager/IRIS a Fourier spectrometer with a
  wavelength coverage from 4 to 56 micron and a
  spectral resolution of 40-600.
• While IRIS played an important role for revealing
  the atmospheric compositions of the four giant
  planets of our solar system (Jupiter, Saturn,
  Uranus, Neptune Hanel et al. 1979, 1981, 1982,
  1986 Conrath et al. 1989), the coronagraph
  spectrometer of SPICA will be an important tool
  for a study of extrasolar planets.

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Extrasolar Planets Free-Floaters
Natta Testi 2001

• Young FF planets or sub-brown dwarfs or planemos
  in nearby star forming regions and cold brown
  dwarfs are also good targets.
• SPICA is necessary for ?1M(Jupiter) FF-planets,
  if any.
• Astromineralogy including FF-planet disks.

BD flared disk w/ silicate feat.
Natta and Testi 2001
Mohanty, RayJay, Tamura et al. 2004
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Astromineralogy Astroorganic chemistry
High Spatial Resolution High Sensitivity
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From Disks to PlanetsContinuous Studies with
SPICA
Dust
Minerals
Cloud
Ice
0.1µm
10 K
Core ? Envelope
Protoplanetary Disk
160K(5AU)
1000K(1AU)
Accretion Disk
160K(3AU)
300K(1AU)
Passive Disk
Planetary Systems and Exozodi
Planetesimal
10 km
Yamamoto
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Astro-mineralogy

• Rapidly developing field, especially with ISO,
  SST, and probably ASTRO-F.
• 8-10m class ground-based telescope progresses,
  too!
• Ground-based 10 micron window is not enough to
  fully exploit this field.
• Too much unmatching of spatial resolution
  between space and ground at present and near
  future.
• SPICA can mitigate this unmatching.
• Key Word Origin of Earth-like Planets
• Examples in Solar Sys. and YSOs shown later.

Silicate features
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Silicate Features

• Dominant forms of astronomical silicates
• olivine (Mg2XFe2-2XSiO4)
• pyroxene (MgXFe1-XSiO3)
• forsterite (Mg2SiO4)
• enstatite (MgSiO3)
• Thermal (?) processing
• ISM lt5 crystalline silicate
• HAEBE disks crys. Si found some in evolved
  disks
• T Tauri disks crys. Si found in very few sources
• comets and IPDs 0-30 cry. Si
• Meteorites 100, but not primordial
• 8-10m class ground-based telescope progresses,
  too!
• ? crystallization occurring during disk phase?

Forrest et al. 2004
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Silicate Features ground-basedSubaru/COMICS
TTS
Vega- like star
Evolution from Mg-pure silicate to Fe-Mg
silicate? Honda et al. 2004
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Silicate Features w/ SPICA

• How and when the thermal processing are
  occurring?
• Connection with comets (low temperature dust)?
• FIR obs. of low temp. component is essential!
• Spatially resolved silicate mineralogy!
• 2D spectrometer
• resolution0.3-12

Forsterite
H2O
PAH
Forrest et al. 2004
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Case Study beta Pic
Hirao report
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Astro-Organic-Chemistry

• Dust surface chemistry is extremely important,
  although 80 of the known interstellar molecules
  are explained by ion-molecule reactions.
• Also rapidly developing field, especially with
  ISO, SST (gt5µm), and ASTRO-F (incl. 2-5µm). 8-10m
  class ground-based telescopes, too.
• Ground-based L-band and M-band windows are not
  enough to develop this field.
• Searches for amino-acid such as glycine (the
  simplest one).
• Key Word Origin of Life

B5 IRS 1 and HH 46 IRS (Class I protostar)
SST Numerous icy molecules! some probably
produced hot core region around protostars for
various molecules But not spatially resolved.
Boogert et al. 2004
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Ice Evolution from Protostars to TTS
all images are 2.2 or 1.7 micron
Class? (protostars)
extended envelope
1000AU7
IRAS040162610 Tamura et al.
Class? (CTTS)
Class??
HL Tau Tamura et al.
Herbig Ae/Be
GM Aur AB Aur (Schneider03 Fukagawa04)
less extended envelope
original from Ishii
mostly disk only
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OtherTopics
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Solar System Comet Dust

• Mineralogy Ice
• Recent progresses on YSO disks and cloud (core)
• But very few data on comets
• How crystalline silicates are included in comet
  nuclei?
• Various ice features and those ice conditions
  (crystalline or amorphous?) as a function of
  distance from the sun
• 65micron H2O only in crystalline ice

ISO spectra of HD 100546, a Herbig Ae/Be star.
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Solar System Icy small objects

• EKBOs, Centaurus, icy satellites, other minor
  bodies
• Origin of planetesimals
• Derivation of Albedo and Size, combined with
  ground-based optical observations.
• Good matches w/ new targets from 8-m class
  telescopes for next several years.

SED of minor bodies in the solar system.
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Solar System Icy small objects

• Direct observations are only for three comet
  nuclei.
• All icy minor bodies ate very small (ltlt1).
• Why the albedo of icy minor bodies are so
  diverse? (0.02-1.0)
• Only a dozen or so of data so far.

Albedo diversity of icy minor bodies.
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Warm Molecular Hydrogen

• Will be exploited with SST.
• Spatial resolution is essential for the next
  step.
• Spatially resolved spectroscopy of circumstellar
  structure around various YSOs.
• Another challenging but unique idea H2 line
  dynamics with R105 spectroscopy.

S(0) (v0-0 J2?0 28.218µm) S(1) (v0-0 J3?1
17.035µm) J 10?8 5.05 µm, etc.
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Triggered Star Formation

• Possible sequential star formation (radiation
  induced) in massive SFRs.
• Several excellent sites for detailed studies.
• High spatial resolution is essential.

from Sugitani
optical-HST (0.1)
NIR-SIRIUS (1)
MIR-ISO (3)
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Instrument Requirements Summary

• MIR 2D spectroscopy (?/??lt1000).
• FIR 2D spectroscopy (?/??lt1000).
• MIR coronagraph imaging and spectroscopy (?/??lta
  few 100).
• Some request ?/??105 spectroscopy at MIR. This
  is challenging but unique (vs. JWST, HSO, ALMA).
• Comets chemistry (Watanabe)
• H2 line dynamics (Kitamura, Tamura)
• Stellar physics (Yamamura)
• Spatial resolution is not important in this mode.