Debris Disks

Amaya Moro-Martín Center for Astrobiology-CSIC (Spain) and Princeton University Outline Outline Neptune

Part I What is a debris disks Part II Why are debris disks interesting Part III Future prospects in debris disks studies (of particular relevance to the Japanese community) What is a Debris disks main properties

Disks of dust around mature (0.01-10 Gyr) main sequence (generally K2-A, i.e. 0.8-3 Msun)

Sizes: 10s-100s AU (Solar System size)

Low gas-to-dust ratio (primordial gas dissipates in < 10 Myr)

There are ~300 known debris disks, mostly detected by IRAS and Spitzer from their IR excesses; some also detected in scattered light Mostly spatially unresolved Debris disks main properties Neptune

HD 105

IRAS ISO Spitzer

Minor(Meyer Centeret al. 2004) Debris disks main properties

Disks are generally spatially unresolved. 24 μm 70 μm 450 μm Can constrain dust location from SED. Near IR Mid IR Far IR sub mm

Distance 0.1 1 10 100 Holland et al. (2003) (AU) Stapelfeldt et al. (2004)

Disk SED

24μm 33μm 70μm

Distribución Espectral

Log[F(mJy)] de Energía

Log[λ(μm)] (Moro-Martin, Wolf & Malhotra 2005) (Meyer et al. 2004) Debris disks main properties

Disks are generally spatially unresolved. 24 μm 70 μm 450 μm Can constrain dust location from SED. Far IR sub mm

Distance 10 100 Holland et al. (2003) (AU) Stapelfeldt et al. (2004)

Disk SED

24μm 33μm 70μm

Distribución Espectral

Log[F(mJy)] de Energía

Log[λ(μm)] (Moro-Martin, Wolf & Malhotra 2005) (Meyer et al. 2004) Debris disks main properties

Frequency of debris disks from Spitzer surveys:

- FEPS Legacy survey: 328 FGK stars (0.7-1.4Msun) >3 Myr.; 5-70 μm. Detection rates: 15% at 24 μm (<300 Myr), 3% at 24 μm (>300 Myr), 7% at 70 μm. - FGK GTO Survey: 150 FGK stars; 8-70 μm. Detection rates: 13+/-3% at 70 μm. - MIPS GTO Binary Survey: 69 A3-F8 binaries. Detection rates: 9+/-4% at 24 μm and 40+/-7% at 70μm (1/2 circumbinary and 1/3 circumstellar) - MIPS GTO A- Survey: 160 A stars, 5-850 Myr. Detection rates: 32+/-5% at 24 μm and 33+/-5 at 70μm. -5 -7 -6 Surveys limited to Ldust/L* ~ 10 : Ldust/L* ~ 10 -10 -8 -7 Asteroid Belt: Ldust/L* ~ 10 -10 22 spatially resolved; showing a complex morphology (warps , spirals, offsets, brightness asymmetries, cumply rings, sharp inner edges...) Image gallery of dusty debris disks 8/15/08 5:34 PM

The Circumstellar Disk Learning Site

INTRODUCTION IMAGE GALLERY LIBRARY THE OTHER SITES GLOSSARY – 38 – Gallery of spatially resolved debris disks Neptune Image Gallery of Circumstellar Dust Disks

μ μ μ μ μ 0.50.5 microns m 11-2-2 microns m 10-2010-20 microns m 70-45070-450 microns m 850 microns m 1-31-3 mm

Above are the most recent debris Epsilon disk images appearing in the Eri eps Eri scientific literature.

On the left is HD 15745 discovered by and collaborators with the . Fomalhaut On the right is HD 61006 also discovered with Hubble by Dean Fomalhaut Hines and collaborators. Both debris disks have unusual morphologies. HD 15745 has been nicknamed "the fan", whereas HD Vega Fig. 1.— Images of ! Eri in the three Spitzer MIPS channels. N is up and E to the left in 61005 looks like a "moth". Vega all the panels; 10!! = 32 AU at ! Eri’s distance. A cross marks the stellar position at the

of each observation, taking into account ! Eri’s of ∼ 1!! per . Dark To the right you will find a current (Minor Planet Center) Minor Planet Center is positive. Circles indicate FWHM beam sizes. The left column shows 24 µm images gallery of resolved debris disks in log stretch. These have been reconstructed from multiple dithered exposures and are sorted by increasing wavelength See individual referencesoversa inmp http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#led by a factor of four. Panel (a) is the direct image, dominated by the stellar PSF. horizontally, and by heliocentric Panel (d) shows this image after subtracting a PSF reference star scaled to the photospheric AU Mic distance vertically (the closest flux density. The remaining excess (18% of the total 24 µm emission) appears largely as an unresolved point source. The middle column shows 70 µm images in linear stretch. Panel debris disks begin at the top). (b) is the default pixel-scale image used for photometric measurements, and panel (e) shows the fine pixel-scale image. The right column shows 160 µm images in linear stretch. Panel Clicking on any image will open a (c) is the direct image, and panel (f) shows this image after subtraction of the ghost image new browser window with higher arising from the spectral leak. resolution images and more HD information about each debris disk 207129 and star.

HD 10647

HD 139664

HD 109085

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 1 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

The Circumstellar Disk Learning Site

INTRODUCTION IMAGE GALLERY LIBRARY THE ASTRONOMERS OTHER SITES GLOSSARY

Image Gallery of Circumstellar Dust Disks

0.5 microns 1-2 microns 10-20 microns 70-450 microns 850 microns 1-3 mm

Above are the most recent debris Epsilon disk images appearing in the Eri scientific literature.

On the left is HD 15745 discovered by Paul Kalas and collaborators with the Hubble Space Telescope. Fomalhaut On the right is HD 61006 also discovered with Hubble by Dean Hines and collaborators. Both debris disks have unusual Gallery of spatially resolved debris disks morphologies. HD 15745 has been Neptune nicknamed "the fan", whereas HD Vega 61005 looks like a "moth".

To the right you will find a current 0.5 μm 1-2 μm 10-20 μm 70-450 μm 850 μm 1-3 mm gallery of resolved debris disks sorted by increasing wavelength horizontally, and by heliocentric AU Mic distance vertically (the closest AU Mic debris disks begin at the top).

Clicking on any image will open a new browser window with higher resolution images and more HD information about each debris disk 207129 and star. HD 207129

HD 10647 HD 10647 (Minor Planet Center) Minor Planet Center

See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# HD 139664

HD 109085

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 1 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

The Circumstellar Disk Learning Site

INTRODUCTION IMAGE GALLERY LIBRARY THE ASTRONOMERS OTHER SITES GLOSSARY

Image Gallery of Circumstellar Dust Disks

0.5 microns 1-2 microns 10-20 microns 70-450 microns 850 microns 1-3 mm

Above are the most recent debris Epsilon disk images appearing in the Eri scientific literature.

On the left is HD 15745 discovered by Paul Kalas and collaborators with the Hubble Space Telescope. Fomalhaut On the right is HD 61006 also discovered with Hubble by Dean Hines and collaborators. Both debris disks have unusual morphologies. HD 15745 has been nicknamed "the fan", whereas HD Vega 61005 looks like a "moth".

To the right you will find a current gallery of resolved debris disks sorted by increasing wavelength horizontally, and by heliocentric AU Mic distance vertically (the closest debris disks begin at the top).

Clicking on any image will open a new browser window with higher resolution images and more HD information about each debris disk 207129 and star.

Gallery of spatially resolved debris disks Neptune HD 10647

0.5 μm 1-2 μm 10-20 μm 70-450 μm 850 μm 1-3 mm

HD 139664 HD 139664

HD 109085 Image gallery of dusty debris disks 8/15/08 5:34 PM HD 109085

HD 53143

HD 53143 (Minor Planet Center) Minor Planet Center http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#Page 1 of 3 Beta Pictoris

HD 92945

HD 107146

HD 61005

HD 15115

HD 202917

HD 181327

49 Cet

HD 15745

HR 4796A

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 2 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

The Circumstellar Disk Learning Site

Image gallery of dusty debris disks 8/15/08 5:34 PM INTRODUCTION IMAGE GALLERY LIBRARY THE ASTRONOMERS OTHER SITES GLOSSARY Gallery of spatially resolved debris disks Neptune HD 53143 Image Gallery of Circumstellar Dust Disks

μ μ μ μ μ 0.50.5 microns m 11-2-2 microns m 10-2010-20 microns m 70-45070-450 microns m 850 microns m 1-31-3 mm

Above are the most recent debris EpsilonBeta Pictoris disk images appearing in the Eri beta Pic scientific literature.

On the left is HD 15745 discovered by Paul Kalas and collaborators with the Hubble Space Telescope. FomalhautHD 92945 On the right is HD 61006 also discovered with Hubble by Dean HD 92945 Hines and collaborators. Both debris disks have unusual morphologies. HD 15745 has been nicknamed "the fan", whereas HD VegaHD 61005 looks like a "moth". 107146

Minor Planet Center To the right you will find a current HD 107146 (Minor Planet Center) gallery of resolved debris disks sorted by increasing wavelength See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# horizontally, and by heliocentric AU Mic distance vertically (the closest HD 61005 debris disks begin at the top).

Clicking on any image will open a new browser window with higher resolution images and more HD information about each debris disk 207129HD 15115 and star.

HD 10647 202917

HD 139664HD 181327

HD 109085 49 Cet

HD 15745

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 1 of 3

HR 4796A

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 2 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

HD 53143

Image gallery of dusty debris disks 8/15/08 5:34 PM Beta Pictoris

The Circumstellar Disk Learning Site HD 92945

INTRODUCTION IMAGE GALLERY LIBRARY THE ASTRONOMERS OTHER SITES GLOSSARY Gallery of spatially resolved debris disks

HD Neptune 107146 Image Gallery of Circumstellar Dust Disks

μ μ μ μ μ 0.50.5 microns m 11-2-2 microns m 10-2010-20 microns m 70-45070-450 microns m 850 microns m 1-31-3 mm

Above are the most recent debris Epsilon HD 61005 disk images appearing in the Eri

scientific literature. HD 61005

On the left is HD 15745 discovered by Paul Kalas and collaborators with the Hubble Space Telescope. Fomalhaut On the right is HD 61006 also HD 15115 discovered with Hubble by Dean HD 15115 Hines and collaborators. Both debris disks have unusual morphologies. HD 15745 has been nicknamed "the fan", whereas HD VegaHD 61005 looks like a "moth". 202917

Minor Planet Center To the right you will find a current HD 202917 (Minor Planet Center) gallery of resolved debris disks sorted by increasing wavelength See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# horizontally, and by heliocentric AUHD Mic distance vertically (the closest 181327 debris disks begin at the top).

Clicking on any image will open a new browser window with higher resolution images and more HD 207129 information about each debris disk 49 Cet and star.

HD 10647 HD 15745

HD 139664 HR 4796A

HD 109085 http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 2 of 3

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 1 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

HD 53143

Beta Pictoris

HD 92945

HD 107146

Image gallery of dusty debris disks 8/15/08 5:34 PM HD 61005

The Circumstellar Disk Learning Site HD 15115

INTRODUCTION IMAGE GALLERY LIBRARY THE ASTRONOMERS OTHER SITES GLOSSARY Gallery of spatially resolved debris disks

HD Neptune 202917 Image Gallery of Circumstellar Dust Disks

μ μ μ μ μ 0.50.5 microns m 11-2-2 microns m 10-2010-20 microns m 70-45070-450 microns m 850 microns m 1-31-3 mm

Above are the most recent debris HDEpsilon 181327 disk images appearing in the Eri

scientific literature. HD 181327

On the left is HD 15745 discovered by Paul Kalas and collaborators with the Hubble Space Telescope. 49Fomalhaut Cet On the right is HD 61006 also discovered with Hubble by Dean 49 Cet Hines and collaborators. Both debris disks have unusual morphologies. HD 15745 has been nicknamed "the fan", whereas HD HDVega 15745 61005 looks like a "moth".

Minor Planet Center To the right you will find a current HD 15745 (Minor Planet Center) gallery of resolved debris disks sorted by increasing wavelength See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# horizontally, and by heliocentric AU Mic distance vertically (the closest HR 4796A debris disks begin at the top).

Clicking on any image will open a new browser window with higher resolution images and more HD http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#information about each debris disk 207129 Page 2 of 3 and star.

HD 10647

HD 139664

HD 109085

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 1 of 3 Image gallery of dusty debris disks 8/15/08 5:34 PM

HD 53143

Beta Pictoris

HD 92945

HD 107146

HD 61005

HD 15115

HD 202917

HD 181327

49 Cet

Gallery of spatially resolved debris disks Neptune HD 15745

0.5 μm 1-2 μm 10-20 μm 70-450 μm 850 μm 1-3 mm

HR 4796A Image gallery of dusty debris disks 8/15/08 5:34 PM HR 4796A

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#HD Page 2 of 3 141569 HD 141569

HD 32297

Minor Planet Center HD 32297 (Minor Planet Center)

See individual references in http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html#

BD +31 643

0.5 microns 1-2 microns 10-20 microns 850 microns

http://astro.berkeley.edu/~kalas/disksite/pages/gallery.html# Page 3 of 3 Why are debris disks interesting Debris disks are evidence of the presence of planetesimals

Dust Removal Time Scales < 104-106 yr Stellar age << > 107 yrs Poynting-Robertson: Grain-grain collisions: Radiation Pressure:

Dust is not primordial but is replenished by planetesimals (like asteroids, comets and KBOs). Indirect evidence that the first steps of planet formation have taken place.

Debris disks are planetary systems. Alligators are cold-blooded. They cannot generate their own heat. Instead, they take on the temperature of their environment. Notice in the infrared images, how the alligator is cool compared to the warm-blooded human holding it. The alligator's temperature is close to room temperature. Notice also how cold the alligator's eyes are. In the wild, alligators will adjust their body temperature by entering water to cool off, or by basking in sunlight to warm up.

Interplanetary Dust Particle (15 µm) 24 µm

Fomalhaut

Fomalhaut 70 µm

Fomalhaut 450 µm

Fomalhaut 0.8 µm

1.63 µm AU

50

AU AU Mic 20 0.2-1 µm

-Pic ! The study of debris disks AU can shed light on the 100 diversity of planetary -Eri 850 µm ! systems, helping us place our Solar System into context

AU

Alligators are40 cold-blooded. They cannot generate their own heat. Instead, they take on the temperature of their environment. Notice in the infrared images, how the alligator is cool compared to the warm-blooded human holding it. The alligator's temperature is close to room temperature. Notice also how cold the alligator's eyes are. In the wild, alligators will adjust their body temperature by entering water to cool off, or by basking in sunlight to warm up.

AU HD 32297 1.1 µm 70

-5 Surveys limited to Ldust/L* ~ 10 -7 -6 For comparison: Ldust/L* ~ 10 -10 for the KB -8 -7 Ldust/L* ~ 10 -10 for the AB Frequency and timing of planetesimal formation in the terrestrial planet region Frequency and timing of planetesimal formation in the terrestrial planet region 3 (Meyer et al. 2008) 2 0.

If epoch of 24 μm m Excess Emission

μ excess emission lasts

1 0. < x10 the age bins, at least 32% of sun- like stars exhibit evidence of planetesimal formation in Sensitive to ~100-1000 times the the terrestrial planet 0 0. amount of dust in the Solar System region.

Frequency of MIPS 24 If epoch lasts < age bins, 6 7 8 9 frequency is > 60%. Age (Myr) Occurrence of other major evolutionary events Occurrence of other major evolutionary events

...e.g. the Late Heavy Bombardment in the early Solar system - Narrow period of time (3.8-4.1 Gya) - Large number of impact crater created in the Moon and the terrestrial

(Dcrater ~ 100 km Dimpactor ~ 10 km). - Source of impactors: main asteroid belt. - Triggered by orbital migration of giant planets; sweeping of secular resonances through AB; ejection of asteroids into planet-crossing orbits. - Unique event in Solar system’s history - High rate of asteroid collisions and dust production - Large spike in the warm dust of the young Solar System well after the planets were formed. Occurrence of other major evolutionary events m) µ

Large variability at a given age indicate stochastic collisional events may be common

t-1 as planetesimals erode Excess Ratio (over - at 24 (Siegler et al. 2006) Age (Myr) Occurrence of other major HD 69830 (K0V, 0.8Msun, 0.45Lsun, 2 Gyr)

3 Neptune-like planets: ≥ 10.2 M⊕ at evolutionary events

0.0785 AU, ≥ 11.8 M⊕ at 0.186 AU and ≥

18.1 M⊕ at 0.63 AU (Lovis et al. 2006) Spitzer shows a strong 24 µm excess (warm dust) but no 70 µm excess (no cold dust) (Beichman et al. 2005) Possibly a transient event, because... - The observed levels of dust production is too high to be sustained for the star’s lifetime. - There are strong emission features implying small grains with short lifetimes. Could be an AB at ~ 1 AU (~2:1 and 5:2 MMRs of outermost planet - Lisse et al. 2007) ...or it could be a LBH-type of event where icy planetesimals are scattered into the inner system (Wyatt et al. 2006)

Figure 3 - Emissivity spectrum for HD69830 excess, as measured by the Spitzer IRS. The data and model shown are for the smallest photospheric subtraction, demonstrating the upper limits to the abundance of PAHs, amorphous carbon, and sulfides in the system. Error bars are ±2!. Black : SST excess spectrum, divided by a 400K blackbody. Orange dashed line: best fit model spectrum. Colored curves: emission spectra for the constituent species, scaled by the ratio B"(Tdust(a)i)/B"(Tcontinuum), with Tcontinuum = 400K. The best-fit model individual species curves have been scaled by a factor of two versus the data for emphasis. Purples - amorphous silicates of pyroxene or olivine composition. Light blues - crystalline pyroxenes: ferrosilite, diopside, and orthoenstatite, in order of 20 !m amplitude. Dark blues - crystalline olivines, forsterite and fayalite, in order of 20 !m amplitude. Red - amorphous carbon. Deep orange - water ice. Light orange - water gas. Yellow - PAHs. Bright greens - carbonates: siderite and magnesite, by order of 7 !m emissivity amplitude. Olive green - sulfides.

Figure 4 - Spectrum after subtraction of the best-fit silicate components, the dominant species in the emission. Scale, color and labels are the same as in Figure 3. The sinusoidal features at 15 - 20 !m are artifacts ('fringes') of the IRS instrument. The true signal is near the average of the excursions.

19 Substantially different from abundances found for comet 9P/ Tempel 1 or comet Hale-Bopp (Lisse et al. 2007).

Similar to P- or D-type asteroidal body. Analogous to the fragmentation material that accompanied the formation of the Karin and Veritas families in the Solar system. Characterizing planetesimal belts Characterizing planetesimal belts

Kuiper Belt Asteroid Belt

Jupiter Saturn Mars

Uranus

Jupiter Neptune

Frequency of cold debris disks (KB-type): ~10% But results are sensitivity limited to (Bryden et al. 2006, Hillenbrand et al. 2008, Carpenter et al. 2008.) > 100x KB dust. Debris disks at the Frequency of giant planets (<20 AU): ~12% Solar System level may be common (extrapolating from RV surveys; Marcy et al. 2005). Presence and location of planets Presence and location of planets

High resolution observations show complex morphology that could result from gravitational perturbations by planets via: - Gravitational scattering - Resonant perturbations β-Pic AU-Mic - Secular perturbations TW PresenceHD and 141569 location of planets far from the star Fomalhaut ε-Eri

HR4796 HD 32297 Fomalhaut 0.03 0.1 0.3 1 3 10 % of ejected particles

Planet mass (MJup) (Moro-Martin & Malhotra 2005) AU-Mic Kuiper Belt Vega ε-Eri Fomalhaut β-Pic Presence and location of planets

High resolution observations show complex morphology that could result from gravitational perturbations by planets via: - Gravitational scattering - Resonant perturbations β-Pic AU-Mic - Secular perturbations TW Hydra

HD 141569 Presence and location of Kuiper Belt Dust Disk planets far from the star Fomalhaut ε-Eri Log[Number]

a (AU) (Moro-Martin & Malhotra 2002)

HR4796 HD 32297 Fomalhaut

AU-Mic Kuiper Belt Vega ε-Eri Fomalhaut β-Pic Presence1MJup and location of planets particle size at 1AU 135 µm 33 µm 9 µm 2 µm m 1MJup 0.7 µ at 5AU

1MJup at Log[Number] 30AU

Solar System (Moro-Martin & Malhotra, 2002; Moro-Martin, Wolf in prep.)

Semimajor Axis (AU) Presence and location of planets

High resolution observations show complex morphology that could result from gravitational perturbations by planets via: - Gravitational scattering - Resonant perturbations β-Pic AU-Mic - Secular perturbations TW Hydra

HD 141569

Presence and location of 0.8 MJup 0.13 AU e=0.25 planets far from the star 12.2 MJup 3.74 AU e=0.35 Secular Fomalhaut ε-Eri perturb. are long ranged max. eccentricity HR4796 HD 32297 Fomalhaut

a (AU) (Moro-Martin et al. 2007) AU-Mic Kuiper Belt Vega ε-Eri Fomalhaut β-Pic Presence and location of planets

High resolution observations show complex morphology that could result from gravitational perturbations by planets via: - Gravitational scattering - Resonant perturbations β-Pic AU-Mic - Secular perturbations TW Hydra PresenceHD and 141569 location of The study0.8 MJup of 0.13 debris AU e=0.25 disk planets far from the star 12.2 MJup 3.74 AU e=0.35 structureSecular could be a Fomalhaut ε-Eri perturb. are potentiallong rangedplanet detection technique sensitive to

HR4796 HD 32297 Fomalhaut long period planets.

AU-Mic Kuiper Belt Vega ε-Eri Fomalhaut β-Pic Future prospects in debris disks studies (of particular relevance to the Japanese astronomical community) SUBARU 2009-2014 Neptune Subaru Strategic Exploration of and Disks with HiCIAO/AO188 Goal: To address the following key issues in /disk science

The detection and census of exoplanets in the outer circumstellar regions around solar-mass stars and massive stars (test for planet formation models).

The evolution of protoplanetary and debris disks including their morphological diversity.

The direct link between exoplanets and circumstellar disks from a few AU to 10s of AU. SUBARU 2009-2014

1st Subaru Legacy Survey. 1st project under the newly approved N-PAC 120 nights awarded for 5 . 500 targets (focus on solar-mass) (including ~100 debris disks targets) Most extensive imaging survey so far. 3 years ahead of other next generation 8-m instruments Gemini Planet Imager (GPI) Spectro-Polarimetric High-contrast Exoplanet Reseach (SPHERE - VLT) Search for protoplanetary and debris disks and for young self- luminous planets >1 MJup from few AU to 10s of AU Only imaging. Spectroscopy should follow Observations start late 2009. Proprietary time: 18 months. SUBARU 2009-2014 Members and Students Neptune

! 21 institutes 83 members (18 foreigners). " !"#$%#&'()*$+,-.#/'.0")1!*23)456789:;<=> " ?0@!*3)A4BC89:;<=>DEFGH89:;<=> " ?0@*3)89:;<=> IJKDLMNODP4QRDA4BCDA4@ST UVWDXYZ[D\]^D_(#+#,")`ab0$DcdeGfgDhijkDlT mnDEopqDEFGHDr4sfDt(,u'$v,")w'+"0+D4567Dx4 yDzX{D|}~DT•€•Dw',@‚00 !b0Dƒ„JFD5…qCD†}‡ fDˆ‰Š‹)8Œ•Ž••‘’•‘>“T”•D–—˜D™š{D›„œ‹) 8•ž•‘>Ÿ ¡¢‹)8£Ÿ¤•‘>¥¦§¨‹)8©£•‘>£5VS ªD„4«‹)8¬••‘>®šVWD¯°±²‹)8©³•‘>…}±´Dµ ¶·•D¸4¹e‹)8©³“º•‘>M4»DST<¼‹)8½¾¿‘Ž•š >ÀÁÂÃDÄÅyfDÆXÇÈ‹)8\ÉX•‘>š4ÊË‹)8ÌÍΕ ‘>•ÏÇäÁåæ‹)8³ç •‘>è–éfgD²TêëDìíî‹)8\ï•‘>ðTsfD•ñòV WD*$/"#v)ó'$$Dôõ”ö‹)8÷9 øùúûüú•‘>ý,",þb)ÿ'-v#$D ý#(()ÿ$'&&Dó#%!',()ó%"(#'#$Dtþ'b' ó0"0@ó'".#$D$'+#v)‚&,"/,(D"v) wa"$,"D%0&,".)''$v,"&,#‹)8÷9 ()*•‘>ÿ('a-)+0v'&&‹)8÷9 ý!,>`,$,)‚,"'&b$‹)8=- Æ.Ž•’;•™23D EF¤4Dý,$$#5,")ÿ'""‹)86*7 89:ûø;ú:Ž•1>0(5/'$/)?"'$v$,"Dw!0þ'-)+,$$#$/Dó'"@a-)ý'$-0$Dý0-,&!)?'"-0$‹) 8A;úû BCû•‘>,ba t&,‹)8*Dùû (CüAEC6FGC•‘> w#þ)`(,v!#((Dý'þ,-)+0a/!D!!#(#&),a%'-

!"#$%#&'()*$'*&+,&-$./0$&12&3(/&$0#&1)*#0#%*#4&1), SUBARU 2009-2014

HiCIAO can obtain spatially resolved observations at high resolution with unexplored dynamical range and inner working angle. HiCIAO can obtain polarimetry observations useful to study dust grain properties (size and composition). HiCIAO can substantially expand the sample of spatially resolved debris disks and in favorable cases do a simultaneous search for long-period planets (same spatial scale as the dust). What is the connection between debris disks and planets? SUBARU 2009-2014 Neptune SUBARU 2009-2014

Spectral Differential Imaging (SDI) mode: FOV : 5” x 5”

Filters : CH4, [FeII], H2 Four images are generated simultaneously with different narrowband filters Enhance contrast for self-luminous gas planets Contrast : 104 @ 0.”1 separation, 105.5 @ 1” separation Direct Imaging (DI) mode: FOV: 20’’x20’’

Filters: Y, J, H, Ks Polarimetric Differential Imaging (PDI) mode: FOV : 20” x 10” Filters : Y, J, H, Ks Two images (o-ray/eo-ray) are generated simultaneously Enhance contrast for proto-planetary/debris disks SUBARU 2009-2014 Nasmyth pllatform HiCIAO ConceptNeptune

Warm Off-axis distance (λ/D) Cold

t t h h s s p p a

HiCIAO inner working angle = 0.08’’ a r a r a e e t r t r l l e e HST/ACS inner working angle = 0.9’’ e l e l n n g u g u n n Relative magnitude ( ∆ m) ) u + u + o o p e p a d e Module a d Module o l o l 10 d d n n o o o o u u C C o m o m o o c c d d h M r h M r s s M M m m o o o g o g i i e e o o l l C M C M H H Optics Optics Optics Optics e C e C IR Camera IR Camera AO AO T T Relative Intensity (log

188 actuators Coronagraph Differential optics Hawaii 2-RRGG AO Focal masks (Wollaston prisms) 2k ! 2k array Future: Pupil stoOff-axisps distance (arcsec) ASICS Sidecar Controller Complementary MEM DM (32!32) Filters Common+Differential !"#$%"

&'((")*'+,-%.)# SUBARU Proposed Observations in SEEDS 2009-2014 brighter and less-contrast when young ! To conduct a Subaru- 0 HiCIAO-AO188 imaging survey in 5 years, -2 stars searching for giant -4 ) brown planets (~1-13 MJ) andSun dwarfs protoplanetary/debris -6

Log (L/L planets disks around ~500 -8 nearby solar-type SEEDS age span -10 young stars. 1 Myr 10 Myr 100 Myr 1 Gyr 10 Gyr !"#########!$"########!$$"########!%########!$%&' ! Direct imaging is Age (log scale) indispensable for the SEEDS (Based on Burrows et al. 2003) detection of such contrast "young", self-luminous planets, especially planets in outer circumstellar regions (~a few AU-10s AU). !"#$%&'()$*&"+&',--"./)&0"*$12 3,#&)#411&54+$&.4#6&7(-1$8/)&0"*$19 Proposed Observations in SEEDS brighter and less-contrast when young ! To conduct a Subaru- HiCIAO-AO188 imaging survey in 5 years, stars searching for giant planets (~1-13 MJ) and brown protoplanetary/debris dwarfs disks around ~500 planets SUBARUSEEDS age span nearby solar-type 2009-2014 young stars. Direct imaging of young, self-luminous planets from few-10s of AU !"#########!$"########!$$"########!%########!$%&' ! Direct imaging is indispensable for the SEEDS detection of such 10 contrast "young", self-luminous Planets are 15 planets, especially brighter and have less planets in outer ∆ m contrast circumstellar regions 20 when young (~a few AU-10s AU). (Based on Burrows et al. 2003) !"#$%&'()$*&"+&',--"./)&0"*$12 25

3,#&)#411&54+$&.4#6&7(-1$8/)&0"*$19 Wavelength (μm) SUBARU 2009-2014

Hot start models: (Baraffe et al. 2003; Burrows et al. 2003) SEEDS at 0.5 arcsec

SEEDS at 1.5 arcsec

Low-entropy core accretion: (Marley et al. 2007; Fortney et al. 2008)

Uncertain < 100 Myr (uncertain mass estimates)

10 MJ 8 MJ 6 MJ 4MJ 2 MJ 1MJ SUBARU 2009-2014

Hot start models: (Baraffe et al. 2003; Burrows et al. 2003) SEEDS at 0.5 arcsec

SEEDS at 1.5 arcsec

Low-entropy core accretion: Estimated(Marley et al. 2007; Planet Fortney et al. 2008) Detectability

•Comparison with YSOs and OCs category Uncertain luminosities < 100 Myr (uncertain mass estimates) Distance Category Expected Planet Detection Performance

< 200 pc YSOs >2 MJ for >15 AU >0.5 MJ for >100 AU

125 pc Open Clusters >5 MJ for >12 AU >3 MJ for >30 AU 10 MJ 8 MJ 6 MJ 4MJ 2 MJ 1MJ < 30 pc Nearby Stars >10 MJ for a few AU >1 MJ for >25 AU

7 Detection limit diagram (NS) (YSOs and OCs) Figure made by Matsuo, T. ALMA 2012 Neptune

High sensitivity: large unbiased surveys sensitive the level of dust found in the Solar System. Improve statistics. - Are KB-like disks common? The presence of icy planetesimals can shed light on the possiblity of water delivery in the terrestrial planet region. ALMA 2012 Neptune

Unprecedented spatially resolution (a few milliarcseconds for the longest baselines and highest frequencies - better than HST in the optical) In some cases, ALMA will spatially resolve the debris disks.

Spatially resolved observations of debris disks around stars with planets will help us understand how planets affect the disk structure.

Because debris disk structure is sensitive to long period planets, its study could be used as a planet detection technique complementary to and transit surveys (preferentially sensitive to planets close to the star), and to direct imaging (preferentially sensitive to young planets). SPICA ~ 2018 ? Neptune

3.5 meter telescope (similar to Herschel) but cooled to < 5K. Sensitivity in FIR is 100 times better than Herschel.

Monolithic mirror (unlike the segmented JWST) will deliver diffraction limited performance at 5μm with a clean point spread function.

SAFARI instrument: FIR imaging spectrometer from 30-120 μm with a large field-of-view of 2′x2′ and angular resolutions from 2′′ to 15′′ (or 20 to 150AU at 10 pc). SPICA ~ 2018 ?

SPICA’s high-photometric sensitivity would be able to detect dust at 90 K down to a dust mass of 0.01 MMoon around Solar-type stars out to 180 pc (compared to 18 pc for Herschel), increasing the number of detections to 105 (compared to 102) and allowing for better statistics of disk frequencies and properties as a function of stellar type, age and environment. - Are LHB-type of events common? This can set constraints on the frequency of planet migration and have consequences for the habitability of these systems. SPICA ~ 2018 ?

For distant systems, SPICA’s spectroscopy would be able to study the mineralogy or 100s of spatially unresolved debris disks and the coronograph would allow to image and take spectra of the inner disks.

For nearby systems, SPICA’ spectroscopy would be able trace the variation in dust mineral content and grain size distribution as a function of radius; compare to composition of asteroids and KBOs, also studied by SPICA (the large FOV would allow for KBO detections that could be fully characterized with SPICA). November 20, 2008 Time: 06:58am t1-v1.4 SPICA 84 ~ 2018 ? D. Jewitt et al.

01 Vega 24 µm

02 In nearby systems, SPICA03 would be 04 Vega 70 µm able to spatially resolved05 the disks allowing to study their structure;06 Vega has taught 07 us that multi-λ’s studies0 8 are critical for the correct interpretation09 of the systems. 10

11 Vega 160 µm

SPICA’s coronography12 would allow to search for planets and dust13 on similar 14 spatial scales, shedding 1light5 on the planet-

16 disk interaction. Vega 850 µm 17

18

19 200 AU 20

21

22

23

24 Fig. 3.18 Spatially resolved images of Vega from Spitzer/MIPS at 24, 70, 160 ␮m (Su et al. 2005) 25 and from JCMT/SCUBA at 850 ␮m (Holland et al. 1998). All images are in the same scale. The 26 instrument beam sizes (shown in white circles) indicate that the wide radial extent of the MIPS disk 27 images compared to the SCUBA disk image is not a consequence of the instrumental PSF but due

28 to a different spatial location of the particles traced by the two instruments. The sub-mm emission is thought to arise from large dust particles originating from a planetesimal belt analogous to the KB, 29 while the MIPS emission is though to correspond to smaller particles with β < 0.5 (may be due to 30 porosity), produced by collisions in the planetesimal belt traced by the sub-mm observations, and 31 that are blown away by radiation pressure to distances much larger than the location of the parent 32 bodies (Su et al. 2005). This scenario would explain not only the wider extent of the MIPS disk but

33 also its uniform distribution, in contrast with the clumply and more compact sub-mm disk

34

35 36 transient studies, and therefore the study of debris disk structure can help us learn 37 about the diversity of planetary systems. In this context, high resolution debris disk 38 observations over a wide wavelength range are of critical importance, like those to 39 be obtained with Herschel, JWST and ALMA. 40

41 42 3.8.1.3 Spectral EnerUNCORRECTEDgy Distributions PROOF 43

44 As we mentioned above, most of the debris disks observations are spatially un- 45 resolved and are limited to the study of the SED of the star+disk system. Even