SCIENCE with SPICA

(SPace Infrared Telescope for Cosmology and Astrophysics]

SCIENCE with SPICA

(SPace Infrared Telescope for Cosmology and Astrophysics]

M. Tamura (NAOJ)

SPICA Science Working Group

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

summary

Today’s talk

Enya, Keigo ISAS/JAXAHasegawa, Naoshi ISAS/JAXAKaneda, Hidehiro ISAS/JAXAKataza, Hirokazu ISAS/JAXAKitamura, Yoshimi ISAS/JAXAMatsuhara, Hideo ISAS/JAXAMatsumoto, Toshio ISAS/JAXANakagawa, Takao ISAS/JAXAYamamura, Issei ISAS/JAXAHayashi, Masahiko NAOJ/NINSImanishi, Masatoshi NAOJ/NINSIzumiura, Hideyuki NAOJ/NINSKodama, Tadayuki NAOJ/NINSKokubo, Ei-ichiro NAOJ/NINSNakajima, Tadashi NAOJ/NINSOmukai, Kazuyuki NAOJ/NINSPyo, T. S. NAOJ/NINSSekiguchi, Tomohiko NAOJ/NINSTamura, Motohide NAOJ/NINSWatanabe, Jun-ichi NAOJ/NINSYamada, Tohru NAOJ/NINS

Current SWG MemberNishi, Ryo-ichi Niigata UniversityOkamoto, Yoshiko Tsukuba University Fukagawa, Misato The University of TokyoHonda, Mitsuhiko The University of TokyoMiyata, Takashi The University of TokyoOnaka, Takashi The University of TokyoUeno, Munetaka The University of Tokyo Ida, Shigeru Tokyo Inst. of TechnologySusa, Hajime Rikkyo UniversityHirao, Takanori Nagoya UniversityOtsubo, Takafumi Nagoya UniversitySugitani, Kohji Nagoya City CollegeInutsuka, Syuichiro Kyoto UniversityKamaya, Fumihide Kyoto UniversityNagata, Tetsuya Kyoto University Aikawa, Yuri Kobe UniversityKawabata, Kohji Hiroshima UniversityKawakita, Hideo Gunma Observatory

~40 people fromISAS/NAOJ/Universitiesas of 2004.10.12(not complete; sorry)

2.1. Galaxy Formation and Evolution2.1.1. Current Status of Extragalactic Researches2.1.2. First Object and Reionization

2.1.2.1. Cooling by Molecular Hydrogen2.1.2.2. Development of Reionization traced by Hα

2.1.3. Dusty Forming Galaxies2.1.3.1. Internal Kinematics and Physics2.1.3.2. First Star Formation and Chemistry

2.1.4. Basic Structure of Galaxies2.1.4.1. Appearance and Development of Morphology2.1.4.2. Mass Assembly and Star Formation History

2.1.5. Cosmic Large Scale Structure2.1.6. Cosmic Background Radiation

(Nishi, Susa, Kodama, Yamada, Matsuhara, Yoshida, Omukai, etc.)

2.2. Active Galactic Nuclei(Imanishi, Nakagawa, etc.)

Cosmic History

This topic to be covered by Matsuhara, Imanishi, Yamada.

2.3. Star Formation and Evolution2.3.1. Star Formation in Our Galaxy

2.3.1.1. Low-mass Star Formation2.3.1.2. Outflows2.3.1.3. High- and Intermediate-mass Star Formation2.3.1.4. Triggered Star Formation2.3.1.5. Star Formation in the Galactic Center2.1.1.6. Cluster Formation2.1.1.7. Interstellar Matter

2.3.2. Star Formation in Nearby Galaxies and Super Star Clusters2.3.3. IMF and Stellar Populations2.3.4. Interstellar Chemistry

(Tamura, Hayashi, Pyo, Okamoto, Sugitani, Nagata, Inutsuka,Imanishi, Kamaya, Aikawa)

Star Formation and Evolution

2.4. Very Low-Mass Stars and Star Death2.4.1. Very Low-Mass Stars

2.4.1.1. Brown Dwarfs2.4.1.2. Sub-Brown Dwarfs

(Nakajima, Tamura)

2.4.2. Star Death2.4.2.1. Low-Mass Stars2.4.2.2. Mass Outflows2.4.2.3. High-Mass Stars2.4.2.4. Recycles of Dust

(Izumiura, Yamamura, Onaka, Miyata, Kawabata)

Very Low-Mass Stars &Star Death

2.5. Planet Formation and Evolution2.5.1. Protoplanetary Disks2.5.2. Debris Disks2.5.3. Extrasolar Planets

(Tamura, Ida, Fukagawa, Hirao, Honda, Kokubo)

Planet Formation and Evolution

2.6. Solar System2.6.1. Comets2.6.2. Minor Planets2.6.3. Interplanetary Dust2.6.4. Small Icy Objects

2.6.5. Minor Bodies(Watanabe, Hasegawa, Kawakita, Furusyo, S

ato, Sekiguchi, Kasuga, Otsubo)

Solar System

Several Possible Key

SciencesExtra-Solar PlanetsAstro-MineralogyAstro-Organic-Chemistry

Extrasolar Planets

High sensitivityHigh Spatial ResolutionHigh contrast

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.

0.1 1 10 100 micron 1M 10M 100M 1G 10Gyr

FLUX LUMINOSITY

stars

browndwarfs

planets

Sun

JE

SPICA will target direct observations of self-luminous planets at r>a few to ~20 AU of nearby (<10pc) stars. The detectable planets depend on their mass, ages, and separation. If we assume the inner working distance of 3λ/D, then:

Extrasolar Planets

Wavelength Detectable Planets at 10pc=5 micron 1 Gyr – 2 M(Jupiter) , r9AU

~30 G-M target stars

=20 micron 5 Gyr – 2 M(Jupiter), r36AU~150 G-M target stars

SPICA Sensitivity in a perfect coronagraph mode.

Cold BD Gl229B 1 Jupiter mass obj

ect of 10Myr, 100Myr, and 1 Gyr at d=10pc.

Comparison with Subaru 8.2m NIR and MIR sensitivity.

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.

Extrasolar Planets

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.

Extrasolar Planets: Free-Floaters

Natta and Testi 20010 5 10 15 μm

SPICAR~1000

BD flared disk w/ silicate feat.

Natta & Testi 2001

Mohanty, RayJay, Tamura et al. 2004

Astromineralogy

& Astroorganic chemistry

High Spatial ResolutionHigh Sensitivity

From Disks to

Planets:Continuous Studies

with SPICAPassive Disk

Planetesimal

Protoplanetary Disk

Planetary Systems and Exozodi

Cloud

10 km

0.1μm10 K

160K(5AU)1000K(1AU)

160K(3AU)300K(1AU)

Ice

Minerals

Dust

Accretion Disk

Core Envelope

Yamamoto

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.

Astro-mineralogy

Silicate features

Dominant forms of astronomical silicates olivine (Mg2XFe2-2XSiO4) pyroxene (MgXFe1-XSiO3) forsterite (Mg2SiO4) enstatite (MgSiO3)

Thermal (?) processing: ISM: <5% crystalline silicate HAEBE disks: crys. Si found; som

e in evolved disks T Tauri disks: crys. Si found in ve

ry few sources comets and IPDs: 0-30% cry. Si Meteorites: 100%, but not primor

dial 8-10m class ground-based teles

cope progresses, too! ⇒ crystallization occurring during

disk phase?

Silicate Features

Forrest et al. 2004

Silicate Features: ground-based

Subaru/COMICS

TTS

Vega-likestar

Evolution from Mg-pure silicate to Fe-Mg silicate?Honda et al. 2004

How and when the thermal processing are occurring?

Connection with comets (low temperature dust)? FIR obs. of low temp. co

mponent is essential! Spatially resolved silicat

e mineralogy! 2D spectrometer resolution=0.3-12”

Silicate Features w/ SPICA

Forrest et al. 2004

H2O

PAH

Forsterite

Case Study: beta Pic

Hirao report

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 (>5μm), 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”

Astro-Organic-Chemistry

SST

Numerousicy molecules!some probably produced“hot core” regionaround protostarsfor various molecules

But not spatially resolved.

B5 IRS 1andHH 46 IRS(Class Iprotostar)

Boogert et al. 2004

IRAS04016+2610Tamura et al.

HL Tau Tamura et al.

GM Aur & AB Aur　 (Schneider03; Fukagawa04)

ClassⅠ(protostars)

ClassⅠ～Ⅱ

ClassⅡ(CTTS)

1000AU

=7”

Ice Evolution from Protostars to TTS

original from Ishii

extended envelope

less extended envelopemostly disk only

HerbigAe/Be

all images are2.2 or 1.7 micron

OtherTopics

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

Solar System : Comet Dust

ISO spectra of HD 100546, a Herbig

Ae/Be star.

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.

Solar System : Icy small objects

SED of minor bodies in the solar system.

Direct observations are only for three comet nuclei.

All icy minor bodies ate very small (<<1”).

Why the albedo of icy minor bodies are so diverse? (0.02-1.0)

Only a dozen or so of data so far.

Solar System : Icy small objects

Albedo diversity of icy minor bodies.

Object Albedo (average)

5 TNOs 0.051

4 Centaurs

0.088

3 Unusual asteroids

0.027

Pluto 0.5—0.7

Charon 0.3—0.4

Enceradus 1.0

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 R=105 spectroscopy.

Warm Molecular Hydrogen

S(0) (v=0－ 0 J=2→0; 28.218μm)S(1) (v=0－ 0 J=3→1; 17.035μm)…J= 10→8: 5.05 µm, etc.

Possible sequential star formation (radiation induced) in massive SFRs.

Several excellent sites for detailed studies. High spatial resolution is essential.

Triggered Star Formation

optical-HST (0.1”) NIR-SIRIUS (1”) MIR-ISO (3”)

from Sugitani

MIR 2D spectroscopy (λ/Δλ<1000). FIR 2D spectroscopy (λ/Δλ<1000). MIR coronagraph imaging and spectroscopy (λ/

Δλ<a few 100). Some request λ/Δλ=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.

Instrument Requirements Summary