Recurring Planetary Debris Transits and Circumstellar Gas ...
Abstract The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) is a precursor...
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Abstract The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) is a precursor science and technology pathfinder to the Pupil mapping Exoplanet Coronagraphic Observer, designed to fit within a SMEX mission cost cap. EXCEDE will directly image starlight-scattering circumstellar material in the planet- forming regions of stars exhibiting thermal infrared emission above their stellar photospheric levels (a signpost of planetary systems in formation). EXCEDE will provide contrast-limited scattered-light detection sensitivities ~ 10 2—3 times more sensitive than the HST and JWST coronagraphs at a smaller inner working angle, enabling the exploration and characterization of exoplanetary circumstellar disk systems in currently inaccessible observational domains. Utilizing a laboratory-demonstrated high- performance Phase Induced Amplitude Apodized Coronagraph (PIAA-C), integrated with a 50 cm diameter unobscured aperture visible-light telescope, EXCEDE will provide an unrivaled disk-to-star imaging contrast of < 10 -7 at a 1 /D inner working angle of 0.2" with 0.2" spatial resolution at 0.4 microns. Such unprecedented spatially-resolved circumstellar disk images, polarimetrically analyzed at two wavelengths, will enable determinations of disk characteristics (mass, geometry, surface brightness, grain properties) for stars over a wide range of stellar mass and age, providing a unique and comprehensive dataset to understand the formation and evolution of extrasolar planetary systems. Concomitantly, EXCEDE will provide unparalleled imagery of those rare debris disks previously resolved with inferior capabilities. These "Rosetta stones" are the basis of our current understanding of planetary disk systems and EXCEDE observations will overcome current limitations that thus- far have resulted in significant model degeneracies. EXCEDE will also directly image and characterize extrasolar giant planets with orbital distances as small as 1.5 AU and disk sub-structures influenced by co-orbiting planets - for the first time within the terrestrial planet zone (< 5 AU) around the nearest stars - while providing future missions well-honed targets sets for follow-on and multi-wavelength investigations. SCIENCE with EXCEDE Diagnosing Disks with Multiband Imaging Polarimetry Monte-Carlo Scattering Models: (top) Example total intensity images for a circumstellar disk with a surface density ~ 1/r. Larger grains show a stronger forward vs. backward scattering asymmetry, which is greater at shorter wavelengths. (bottom) Percentage polarization maps of the same disks (linear stretched black = 0%, white = 100%). In both spectral bands, larger grains produce higher linear polarization, but large grains polarize light much more efficiently than smaller grains. Thus two-band imaging polarimetry provides a powerful diagnostic to constrain grain Simulated PSF-subtracted EXCEDE images of hypothetical 100 “zodi” SB(r) ~ r -2.4 zodiacal debris systems about nearby sun- like stars. With polarimetric “speckle nulling”, EXCEDE’s reach will further extend to 10- 20 zodi debris systems with strongly polarizing dust. Imaging Circumstellar Disks with EXCEDE EXCEDE will reveal the inner regions of circumstellar debris disks otherwise lost in the glare of the central stars. E.g., HD 107146: r < 60 AU (gray circle) unseen with HST/ACS (left; Ardila et al 2004). Cen HD 82328 Left: EXCEDE will stabilize the WFE to < 10%, resulting in highly repeatable coronagraphic PSFs (top) yielding photon limited azimuthally medianed contrasts < 10 -8 at > 2 /D (middle) revealing detailed structures in low SB disks (e.g., bottom). Right: Simulated images of 1" and 2" radius ring- like disks with 10 -7 per resolution element disk:star contrast at 2 /D. 3AU P(max) = 75% P(max) = 35% 0.8m 0.4m P(max) = 45% P(max) = 50% ISM-like Dust a ≥ 3m grains ISM-like Dust a ≥ 3m grains Polarimetric analysis of the protoplanetary disk around the T Tauri star GM Aur (Schneider et al. 2007), analogously enabled with EXCEDE’s two Wollaston polarimeter for much more contrast-challenging sources, provides complete spatially resolved polarimetric state vector information while fully recovering physical flux density measurements (Hines et. al 2000) – crucial in constraining disk models to elucidate grain properties. PIAA M1 PIAA M2 Mask optics OAP 1 Mask Inverse PIAA 1 Beam Reducer Pupil Relay Pupil WHEEL Camera Mirror Passive corrector Mask optics OAP 2 Beam Reducer Pupil Relay Inverse PIAA 2 Fold Mirror LOWFS (out of plane ) 1024x1024 (21 m) pixel CCD Sensor Prism + Focus – Focus PIAA-C, RELAY, and CAMERA OPTICS LOW ORDER WAVEFRONT SENSOR (LOWFS) CONFIGURATION Pegasus XL Fairing Launch Telescope & Optics focus 80x80 pixel e2v CCD39-02 phase diversity images EXCEDE TELESCOPE & INSTRUMENT e 45° o 45° e 0° o 0° CCD ACROMATIC WOLLASTON -1.00 1.00 .0300 -.0300 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 No. (microns) 1. 0.4000 2. 0.3600 3. 0.4400 -.075000 .075000 .075000 -.075000 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 33 33 33 33 33 33 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WAVEFRONT CONTROL & CONTRAST pixel 0.4 m resolution element + /33 – /33 † At all radii > 2/D Peak speckle contrast ≤ 10 -6 Fold Mirrors Mask Triplet Focal plane mask used to feed LOWFS in Subaru PIAA testbed opaque reflective transparent Fold Mirror O-Ray E-Ray 31.35° MgF2 0.65° Calcite 40” Beam Footprint FPA SPECTRAL ELEMENTS The Exoplanetary Circumstellar Environments And Disk Explorer A Science and Technology Pathfinder for the Pupil mapping Exoplanet Coronagraphic Observer Glenn Schneider and the EXCEDE Science and Mission Team Science Objectives Discovery Science: Obtain a compendium of scattered light images of solar systems in formation Probe dust-scattered starlight within the inner (terrestrial) habitable zones of exoplanetary systems Reveal the presence of previously undetected planets by measuring asymmetries in disk structures Characterization Science: Determine physical and geometrical properties of dust grains within circumstellar environments over a range of stellar ages Assess the growth of primordial dust grains into planetesimals by comparing dust properties of young planet-forming CS environments over the epoch of planet formation Directly image Jupiter-like planets in nearby exoplanetary systems (to IWA limit of 0.2”) Relevance to NASA Science Programs Strategic Plan subgoal 3b: “conduct advanced telescopic searches for Earth-like planets and habitable environments around other stars” Science Plan – Strategic Goals and Decadal Outcomes: “understand … the formation of planetary systems” and “create a census of extrasolar planets and measure their properties” Science Plan – Targeted Outcomes: “study the birth of … planetary systems,” and “determine what properties of a star… are most strongly correlated with the presence of habitable Earth- like planets EXCEDE Science Team Glenn Schneider (PI, University of Arizona): [email protected] Olivier Guyon (PS, University of Arizona) Mark Kuchner (NASA/GSFC) Dean Hines (dPI, Space Science Institute) Alycia Weinberger (Carnegie Inst Wash.) Roger Angel (University of Arizona) Carol Grady (Eureka Scientific) Laird Close (University of Arizona) Mark Wyatt (Cambridge University) Michael Meyer (University of Arizona) Paul Kalas (Univ. Ca., Berkeley Ed Prather (University of Arizona) Barbara Whitney (Space Science Institute) Science Payload 50 cm diameter unobscured aperture off-axis telescope Passive optic for wavefront error correction Phase Induced Amplitude Apodized Coronagraph 1 /D image plane masks Two-band polarimetric imager Instrument Characteristics Spectral passbands: 0.4, 0.8 m (20% FWHM) Coronagraph inner working angle: 0.2” at 0.4 m, 0.4” at 0.8 m Raw/augmented IWA image contrast: point-source: 10 -6 , azimuthal median: 10 -7 Spatial resolution: 200 mas at 0.4m Linear Polarimetry with Wollaston prisms Coronagraphic Polarimetry IWA contrast: down to 10 -9 for strongly polarizing dust around bright unpolarized stars Full Polarimetric Field of View: 40” x 40” Image scale: 83 mas pixel -1 (PSF critically sampled at 0.4 m) Image data format: 2 x (512 x 512) pixels Science detector: low noise, high QE, high dynamic range CCD Guiding array: low noise CCD to produce target derived optical FES with NEA < 2 mas to PCS Spacecraft Mass (SC + Payload): 149 kg Power (SC + Payload): 214 W Pointing Control: 3-axis stabilized Pointing authority: 2 mas using closed-loop optically derived fine error signal from instrument using target star Raw Science Data Downlink 512x512 16-bit images 280 images per day 312 Mbytes/day 2 data dumps/day High Level Data Products 0.4 m & 0.8 m surface brightness maps 0.4 m & 0.8 m flux density limits Polarimetric Stokes u, q images 2D Polarization state vector maps (polarization fraction, orientation) Polarized and total intensity images Quantitative estimation on all products Mission Timeline (dates w.r.t. launch) Launch Readiness: Phase A start + 3 years Initial On-Orbit Checkout: L + 30 days Baseline Mission: IOC + 2 years Science Extension Option: Baseline + 1 year Mission Objectives Enable high spatial resolution optical imaging in the planet-forming zones of circumstellar environments with unprecedented < 10 -7 contrast Survey selected stars with IR excesses indicative of thermally emissive orbiting dust from a > 300 high priority target pool to image circumstellar protoplanetary, transitional, and debris disks and disk sub-structures with an anticipated yield of approximately 100% Survey selected stars nearest Earth with radial velocity detected giant planets to directly image EGPs into terrestrial planet zones Provide two-band optical polarimetry, a key diagnostic tool for disk grain properties, also enhancing instrumental sensitivity to dust (or planet) scattered starlight by an additional factor of > 100 (i.e. 10 -9 inner working angle contrast) 2 year survey of ~ 250 high priority target Mission Characteristics Type: Small Explorer/Astrophysics Launch Vehicle: Pegasus XL or similar Launch Date: Unconstrained Orbit: Sun-synchronous, 950 km, e = 0, i = 99°, Low Earth Orbit Duration: 2 yr after IOC + 1 yr SEOs Identifying New Planets Via Dynamical Influence on Circumstellar Disks Embedded Planets Influencing Circumstellar Material: Scattered light surface brightness distributions for debris disks under the dynamical influence of a co-orbiting planet. Left: Type I (Kuchner & Holmes 2003) debris disk model with a one earth-mass planet orbiting at 1 AU (Kuchner et al. 2007). Right: Type IV debris disk model for the Vega system, an archetype for EXCEDE exoplanetary debris disk targets. The clumpy structure in Vega's debris disk has been used to infer the presence of a Neptune mass planet at 65 AU that migrated outward from 40 AU over ~50 Myr Fomalhaut: One of the very few debris systems resolved with both Spitzer/MIPS (left; Stapelfeldt et al. 2004) and HST/ACS (right; Kalas et al. 2005). The 70 m thermal emission and scattered optical light trace an inclined dust belt ~140 AU distant, but de- centering from, the central star indicative of the presence of an unseen massive planet. EXCEDE will image the inner hot debris that is detected (but unresolved) by Spitzer at 24 m, Surveying Stellar Environments for Scattered Light Disks Removing Model Degeneracies with Scattered-Light Imaging (right): Disk geometries and morphologies cannot be determined by thermal IR excess alone. Small grains radiate less efficiently than large grains. Therefore, at a given equilibrium temperature, small grains reside farther from their central stars than large grains. E.g., IR-excesses measured by IRAS (squares) and Spitzer (dots) for the dominant grain populations around HD 181327 (top) and HD 61005 (right) indicate similar temperatures, but drastically different disk morphologies as revealed with scattered light imaging (HST/NICMOS; Schneider et al 2006, Hines et al 2007). Reaching into Stellar Habitable Zones (left): (adapted from Kasting et al. 1993) EXCEDE will survey nearby stars to image debris structures within their planetary systems. The 0.2" inner working angle at 0.4 m for our sample in AU is shown (red dots). For ~10% of the sample, EXCEDE will probe into the stellar “habitable zones” (red dots in green region), where temperatures allow for the existence of liquid water in the circumstellar environment. NASA Center Partnership & Management NASA Ames Research Center Lead Industrial Partner Lockheed-Martin Data Archive and Distribution Center Multimission Archive at STScI Utilizing A Phase Induced Amplitude Apodized Coronagraphic Telescope For High Contrast Imaging Of Circumstellar Planet-forming Environments EXCEDE PIAA-C/Optics Packaging Articulati ng SM 50 cm dia. unobscured ULE PM
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Transcript of Abstract The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) is a precursor...
AbstractThe EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) is a precursor science and technology pathfinder to the Pupil mapping Exoplanet Coronagraphic Observer, designed to fit within a SMEX mission cost cap. EXCEDE will directly image starlight-scattering circumstellar material in the planet-forming regions of stars exhibiting thermal infrared emission above their stellar photospheric levels (a signpost of planetary systems in formation). EXCEDE will provide contrast-limited scattered-light detection sensitivities ~ 102—3 times more sensitive than the HST and JWST coronagraphs at a smaller inner working angle, enabling the exploration and characterization of exoplanetary circumstellar disk systems in currently inaccessible observational domains. Utilizing a laboratory-demonstrated high-performance Phase Induced Amplitude Apodized Coronagraph (PIAA-C), integrated with a 50 cm diameter unobscured aperture visible-light telescope, EXCEDE will provide an unrivaled disk-to-star imaging contrast of < 10-7 at a 1 /D inner working angle of 0.2" with 0.2" spatial resolution at 0.4 microns. Such unprecedented spatially-resolved circumstellar disk images, polarimetrically analyzed at two wavelengths, will enable determinations of disk characteristics (mass, geometry, surface brightness, grain properties) for stars over a wide range of stellar mass and age, providing a unique and comprehensive dataset to understand the formation and evolution of extrasolar planetary systems. Concomitantly, EXCEDE will provide unparalleled imagery of those rare debris disks previously resolved with inferior capabilities. These "Rosetta stones" are the basis of our current understanding of planetary disk systems and EXCEDE observations will overcome current limitations that thus-far have resulted in significant model degeneracies. EXCEDE will also directly image and characterize extrasolar giant planets with orbital distances as small as 1.5 AU and disk sub-structures influenced by co-orbiting planets - for the first time within the terrestrial planet zone (< 5 AU) around the nearest stars - while providing future missions well-honed targets sets for follow-on and multi-wavelength investigations.
SCIENCE with EXCEDE
Diagnosing Disks with Multiband Imaging Polarimetry
Monte-Carlo Scattering Models: (top) Example total intensity images for a circumstellar disk with a surface density ~ 1/r. Larger grains show a stronger forward vs. backward scattering asymmetry, which is greater at shorter wavelengths. (bottom) Percentage polarization maps of the same disks (linear stretched black = 0%, white = 100%). In both spectral bands, larger grains produce higher linear polarization, but large grains polarize light much more efficiently than smaller grains. Thus two-band imaging polarimetry provides a powerful diagnostic to constrain grain size distributions.
Simulated PSF-subtracted EXCEDE images of hypothetical 100 “zodi” SB(r) ~ r-2.4 zodiacal debris systems about nearby sun-like stars. With polarimetric “speckle nulling”, EXCEDE’s reach will further extend to 10-20 zodi debris systems with strongly polarizing dust.
Imaging Circumstellar Disks with EXCEDE
EXCEDE will reveal the inner regions of circumstellar debris disks otherwise lost in the glare of the central stars. E.g., HD 107146: r < 60 AU (gray circle) unseen with HST/ACS (left; Ardila et al 2004).
CenHD 82328
Left: EXCEDE will stabilize the WFE to < 10%, resulting in highly repeatable coronagraphic PSFs (top) yielding photon limited azimuthally medianed contrasts < 10-8 at > 2 /D (middle) revealing detailed structures in low SB disks (e.g., bottom). Right: Simulated images of 1" and 2" radius ring-like disks with 10-7 per resolution element disk:star contrast at 2 /D.
3AU
P(max) = 75%P(max) = 35%
0.8m0.4m
P(max) = 45% P(max) = 50%
ISM-like Dust a ≥ 3m grains ISM-like Dust a ≥ 3m grains
Polarimetric analysis of the protoplanetary disk around the T Tauri star GM Aur (Schneider et al. 2007), analogously enabled with EXCEDE’s two Wollaston polarimeter for much more contrast-challenging sources, provides complete spatially resolved polarimetric state vector information while fully recovering physical flux density measurements (Hines et. al 2000) – crucial in constraining disk models to elucidate grain properties.
PIAAM1
PIAA M2
Mask optics OAP 1
Mask
Inverse PIAA 1
Beam ReducerPupil Relay
Pupil WHEEL
Camera Mirror
Passive corrector
Mask optics OAP 2
Beam Reducer
Pupil Relay
Inverse PIAA 2
Fold Mirror
LOWFS (out of plane )
1024x1024(21 m) pixel
CCD Sensor
Prism
+ Focus
– Focus
PIAA-C, RELAY, and CAMERA OPTICS
LOW ORDER WAVEFRONT SENSOR (LOWFS)
CONFIGURATION
Pe
ga
su
s X
L F
air
ing
Launch Telescope & Optics
focus
80x80 pixel e2v CCD39-02
phase diversity images
EXCEDE TELESCOPE & INSTRUMENT
e45°
o45°
e0°
o0°
CCDACROMATIC WOLLASTON
-1.00 1.00
.0300
-.0300
11
11
11
11
11
11
11
11
11
11
11
1
1
1
1
2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2
3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3
YFAN - WAVELENGTH(S) 1, 2, 3OPD-WV VS. FRC
f/105 40asec AchroWollaston MgF2/Calcite & imager CFG 1FOB (X,Y,Z) 0.00000 0.00000 0.00000X-SCALE = 0.20000Y-SCALE = 0.00600 Lockheed Martin Adv. Tech. Center
1030 HRS 28 Nov 07R.D. Sigler, x43592
No. (microns)1.0.40002.0.36003.0.4400
-.075000 .075000
.075000
-.075000
1111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 11 111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111 11 11 11 11 11 11 11 11 11 11 11 11 11 12222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222222 22 22 22 22 22 22 22 22 22 22 22 22 22 23333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333 33 33 33 33 33 33 33 33 33 33 33 33 33 33 33 33 33 333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333333 33 33 33 33 33 33 33 33 33 33 33 33 33 3
f/105 40asec AchroWollaston MgF2/Calcite & imager CFG 1FOB (X,Y,Z) 0.00000 0.00000 0.00000Focus shift 0.00000 Coll. surf. 11Chief ray (X,Y) 0.00000 5.50000Origin shift (X,Y) 0.00000 0.00000Scale is linearX-SCALE = 0.01500 MMY-SCALE = 0.01500 MM
Lockheed Martin Adv. Tech. Center1034 HRS 28 Nov 07R.D. Sigler, x43592
Wavefront ErrorO-Ray (~ constant over fov)
ChromaticSpot Size
SCIENCE CAMERA
Contrast: < 10-6 everywhere in focal plane
(0.4mm, 2.1 pixel per l/D)
Passive Corrector ion-beam figuring*PUPIL WAVEFRONT ERROR
BEFORE: 2.5 nm RMS AFTER: 1.0 nm RMS
Contrast: ≤10-7 azimuthal median†
(0.4m, 2.1 pixel per /D)
Wavefront Error (nm) PSF Contrast
*Ion beam size = 1/40 pupil diameter15% measurement+figuring calibration error
WAVEFRONT CONTROL & CONTRAST
pixel
0.4 mresolutionelement
+ /33
– /33
†At all radii > 2/DPeak speckle contrast ≤ 10-6
Fold Mirrors
Mask
Triplet
Focal plane mask used to feedLOWFS in Subaru PIAA testbed
opaquereflective transparentFold Mirror
O-Ray
E-Ray
31.35° MgF2 0.65° Calcite 40” Beam Footprint
FPA
SPECTRAL ELEMENTS
The Exoplanetary Circumstellar Environments And Disk ExplorerA Science and Technology Pathfinder for the Pupil mapping Exoplanet Coronagraphic Observer
Glenn Schneider and the EXCEDE Science and Mission Team
Science ObjectivesDiscovery Science: Obtain a compendium of scattered light images of solar systems in formation Probe dust-scattered starlight within the inner (terrestrial) habitable zones of exoplanetary systems Reveal the presence of previously undetected planets by measuring asymmetries in disk structures
Characterization Science: Determine physical and geometrical properties of dust grains within circumstellar environments over a range of stellar ages Assess the growth of primordial dust grains into planetesimals by comparing dust properties of young planet-forming CS environments over the epoch of planet formation Directly image Jupiter-like planets in nearby exoplanetary systems (to IWA limit of 0.2”)
Relevance to NASA Science Programs
Strategic Plan subgoal 3b: “conduct advanced telescopic searches for Earth-like planets and habitable environments around other stars”
Science Plan – Strategic Goals and Decadal Outcomes: “understand … the formation of planetary systems” and “create a census of extrasolar planets and measure their properties”
Science Plan – Targeted Outcomes: “study the birth of … planetary systems,” and “determine what properties of a star… are most strongly correlated with the presence of habitable Earth- like planets
EXCEDE Science Team Glenn Schneider (PI, University of Arizona): [email protected] Olivier Guyon (PS, University of Arizona) Mark Kuchner (NASA/GSFC) Dean Hines (dPI, Space Science Institute) Alycia Weinberger (Carnegie Inst Wash.) Roger Angel (University of Arizona) Carol Grady (Eureka Scientific) Laird Close (University of Arizona) Mark Wyatt (Cambridge University) Michael Meyer (University of Arizona) Paul Kalas (Univ. Ca., Berkeley Ed Prather (University of Arizona) Barbara Whitney (Space Science Institute)
Science Payload50 cm diameter unobscured aperture off-axis telescopePassive optic for wavefront error correction Phase Induced Amplitude Apodized Coronagraph 1 /D image plane masks Two-band polarimetric imager
Instrument CharacteristicsSpectral passbands: 0.4, 0.8 m (20% FWHM)Coronagraph inner working angle: 0.2” at 0.4 m, 0.4” at 0.8 mRaw/augmented IWA image contrast: point-source: 10-6, azimuthal median: 10-7
Spatial resolution: 200 mas at 0.4mLinear Polarimetry with Wollaston prismsCoronagraphic Polarimetry IWA contrast: down to 10-9 for strongly polarizing dust around bright unpolarized starsFull Polarimetric Field of View: 40” x 40”Image scale: 83 mas pixel-1 (PSF critically sampled at 0.4 m)Image data format: 2 x (512 x 512) pixelsScience detector: low noise, high QE, high dynamic range CCDGuiding array: low noise CCD to produce target derived optical FES with NEA < 2 mas to PCS
SpacecraftMass (SC + Payload): 149 kgPower (SC + Payload): 214 W Pointing Control: 3-axis stabilized Pointing authority: 2 mas using closed-loop optically derived fine error signal from instrument using target star
Raw Science Data Downlink512x512 16-bit images 280 images per day312 Mbytes/day 2 data dumps/day
High Level Data Products0.4 m & 0.8 m surface brightness maps0.4 m & 0.8 m flux density limitsPolarimetric Stokes u, q images2D Polarization state vector maps (polarization fraction, orientation)Polarized and total intensity imagesQuantitative estimation on all products
Mission Timeline (dates w.r.t. launch)Launch Readiness: Phase A start + 3 yearsInitial On-Orbit Checkout: L + 30 daysBaseline Mission: IOC + 2 years Science Extension Option: Baseline + 1 year
Mission ObjectivesEnable high spatial resolution optical imaging in the planet-forming zones of circumstellar environments with unprecedented < 10-7 contrastSurvey selected stars with IR excesses indicative of thermally emissive orbiting dust from a > 300 high priority target pool to image circumstellar protoplanetary, transitional, and debris disks and disk sub-structures with an anticipated yield of approximately 100%Survey selected stars nearest Earth with radial velocity detected giant planets to directly image EGPs into terrestrial planet zones Provide two-band optical polarimetry, a key diagnostic tool for disk grain properties, also enhancing instrumental sensitivity to dust (or planet) scattered starlight by an additional factor of > 100 (i.e. 10-9 inner working angle contrast)2 year survey of ~ 250 high priority target
Mission CharacteristicsType: Small Explorer/AstrophysicsLaunch Vehicle: Pegasus XL or similarLaunch Date: UnconstrainedOrbit: Sun-synchronous, 950 km, e = 0, i = 99°, Low Earth OrbitDuration: 2 yr after IOC + 1 yr SEOs
Identifying New Planets Via Dynamical Influence on Circumstellar Disks
Embedded Planets Influencing Circumstellar Material: Scattered light surface brightness distributions for debris disks under the dynamical influence of a co-orbiting planet. Left: Type I (Kuchner & Holmes 2003) debris disk model with a one earth-mass planet orbiting at 1 AU (Kuchner et al. 2007). Right: Type IV debris disk model for the Vega system, an archetype for EXCEDE exoplanetary debris disk targets. The clumpy structure in Vega's debris disk has been used to infer the presence of a Neptune mass planet at 65 AU that migrated outward from 40 AU over ~50 Myr (Wyatt 2003).
Fomalhaut: One of the very few debris systems resolved with both Spitzer/MIPS (left; Stapelfeldt et al. 2004) and HST/ACS (right; Kalas et al. 2005). The 70 m thermal emission and scattered optical light trace an inclined dust belt ~140 AU distant, but de-centering from, the central star indicative of the presence of an unseen massive planet. EXCEDE will image the inner hot debris that is detected (but unresolved) by Spitzer at 24 m, but is un-observable with HST.
Surveying Stellar Environments for Scattered Light Disks
Removing Model Degeneracies with Scattered-Light Imaging (right): Disk geometries and morphologies cannot be determined by thermal IR excess alone. Small grains radiate less efficiently than large grains. Therefore, at a given equilibrium temperature, small grains reside farther from their central stars than large grains. E.g., IR-excesses measured by IRAS (squares) and Spitzer (dots) for the dominant grain populations around HD 181327 (top) and HD 61005 (right) indicate similar temperatures, but drastically different disk morphologies as revealed with scattered light imaging (HST/NICMOS; Schneider et al 2006, Hines et al 2007).
Reaching into Stellar Habitable Zones (left): (adapted from Kasting et al. 1993) EXCEDE will survey nearby stars to image debris structures within their planetary systems. The 0.2" inner working angle at 0.4 m for our sample in AU is shown (red dots). For ~10% of the sample, EXCEDE will probe into the stellar “habitable zones” (red dots in green region), where temperatures allow for the existence of liquid water in the circumstellar environment.
NASA Center Partnership & Management NASA Ames Research Center Lead Industrial Partner Lockheed-MartinData Archive and Distribution Center Multimission Archive at STScI
Utilizing A Phase Induced Amplitude Apodized Coronagraphic Telescope For High Contrast Imaging Of Circumstellar Planet-forming Environments
EXCEDE
PIAA-C/Optics Packaging
Articulating SM
50 cm dia. unobscured ULE PM
