Glenn Schneider

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High Contrast Imaging and The Disk/Planet
Connection
Glenn Schneider Steward Observatory, University
of Arizona (NICMOS/IDT)
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Direct (Scattered Light) Imaging of Dusty Debris
Asymmetries (radial azimuthal) May implicate
low-mass perturbers (planets) from
Rings, Central Holes, Gaps, Clumps, Arcs,
Arclets Help Elucidate the scattering
physical properties of the grains.
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The HUBBLE Legacy Breaking the Low Contrast
Paradigm
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TODAY HST Provides a Unique Venue for High
Contrast Imaging
Diffraction Limited Imaging in Optical/Near-IR
gt 98 Strehl Ratios _at_ all ls
Highly STABLE PSF
Coronagraphy NICMOS STIS, ACS
NIR High Dynamic Range Sampling NICMOS/MA
Dmag19.4 (6 x 4m)
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Planet-Building Timeline
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Pressure 10
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Scientific Areas of Investigation Enabled With
Todays Capabilities on HST via PSF-Subtracted
Coronagraphic Imaging
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Moving Beyond HST into the Super-High Contrast
Regime
OPTICAL CONFIGURATIONS Coronagraphy Polarimetric
Nulling Nulling Interferometry Wavefront
Correction Station-Keeping Occulters Interferome
tric Arrays
TECHNOLOGICAL CHALLENGES               Micro-Roug
hness of Optical Surfaces Particulate/Contaminati
on Control Stray Light Management
Control Pupil Apodization (and
Shaping) Metrological Tolerancing
Stability Wavefront/Mirror Sensing Control
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The Dusty Disk/Planet Connection
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lt 1Myr Proplyds in Orion
and Substellar Objets to 10 Mjup
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HH30 Obscured GM AUR Unembedded
Coronagraph PSF Subtraction
Direct Image
1 few Myr
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Coronagraph PSF Subtraction
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Planet-Building Timeline
HH 30
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Planet-Building Timeline
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Planet-Building Timeline
141569A
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Planet-Building Timeline
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Primary Dust (
m) Secondary Dust (
m)
m
m
b
e
l
t
?
Locked to Gas Collisional erosion
Clearing Timescales P-R drag few 10
6
4
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Pressure 10
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Examples of Dusty Disks with Radial and
Hemispheric Brightness Anisotropies and Complex
Morphologies, Possibly Indicative of Dynamical
Interactions with Unseen Planetary Mass
Companions, Spatially Resolved and Imaged Around
Young (lt 10 Myr) Stars by HST.
17
Examples of Dusty Disks with Radial and
Hemispheric Brightness Anisotropies and Complex
Morphologies, Possibly Indicative of Dynamical
Interactions with Unseen Planetary Mass
Companions, Spatially Resolved and Imaged Around
Young (lt 10 Myr) Stars by HST.
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Examples of Dusty Disks with Radial and
Hemispheric Brightness Anisotropies and Complex
Morphologies, Possibly Indicative of Dynamical
Interactions with Unseen Planetary Mass
Companions, Spatially Resolved and Imaged Around
Young (lt 10 Myr) Stars by HST.
19
Examples of Dusty Disks with Radial and
Hemispheric Brightness Anisotropies and Complex
Morphologies, Possibly Indicative of Dynamical
Interactions with Unseen Planetary Mass
Companions, Spatially Resolved and Imaged Around
Young (lt 10 Myr) Stars by HST.
TW Hya (K7) Old PMS Star
Pole-on circularly symmetric disk with a break in
its surface brightness profile at 120 AU (2).
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HR 4796A
1.1mm 0.58mm
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HR 4796A RING GEOMETRY
(Least-Squares Isophotal Ellipse Fit)
Ansal Separation (Peaks) 2.107
0.0045 Major Axis of BFE
2.114 0.0055" P.A. of Major Axis (E of N)
27.06 0.18 MajorMinor Axial Length
(3.9658 0.034) 1 Inclination of Pole
to LOS 75.73 0.12 Photocentric
Offset from BFE(Y) -0.0159"
0.0048" Photocentric Offset from BFE(X)
0.0031" 0.0028"
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HR 4796A Circumstellar Debris Ring - WIDTH
WIDTH AT NE ANSA
FWHM 12.30.7AU 8.7 Dring
1-e-1 17.710.1AU 12.5 Dring
Brightness (Normalized to NE Ansa)
Measured 0.197
PSF point source 0.070
FWHM ring 0.184
1-e-1 0.265
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RING GEOMETRY - Least-Squares Isophotal Ellipse
Fit
Ansal Separation (Peaks) 2.107
0.0045 Major Axis of BFE
2.114 0.0055" P.A. of Major Axis (E of N)
27.06 0.18 MajorMinor Axial Length
(3.9658 0.034) 1 Inclination of Pole
to LOS 75.73 0.12 Photocentric
Offset from BFE(Y) -0.0159"
0.0048" Photocentric Offset from BFE(X)
0.0031" 0.0028"
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FACE-ON PROJECTION - With Flux Conservation
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Spatially Resolved Relative PHOTOMETRY of the Ring
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NWSE Surface Brightness Anisotropy
N-Sigma Brightness Ratio (Percent)
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FrontBack Surface Brightness Anisotropy
N-Sigma Brightness Ratio (Percent)
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Broad Colors of the HR 4796A Debris Ring
Intrinsically red grains Consistent with
collisionally evolved population of particle
sizes gt few microns Not primordial ISM
grains Similar intrinsic colors to TNOs in our
solar system V-J1.07 Consistent with
laboratory irradiation experiments on a
variety of organics to study reddening of D P
type asteroids with distance From Sun. Barucci
et al (1993) Andronico et al (1987)
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.
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Cooling Curves for Substellar Objects
0
Evolution of M Dwarf Stars, Brown Dwarfs
and Giant Planets
(from Adam Burrows)
-2
200M
jup
80M
jup
-4
L/Lsum
10
Log
sun
-6
14M
jup
-8
STARS (Hydrogen burning)
BROWN DWARFS (Deuterium burning)
JUPITER
PLANETS
SATURN
-10
6
10
9
8
7
Log
Age (years)
10
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CORONAGRAPHIC COMPANION DETECTION (Multiaccum)
Imaging at two S/C orientations (in a single HST
visability period). Background objects rotate
about occulted Target. PSF structures and
optical artifacts do not.
TWA6. Two Integrations Median of 3
Multiaccum Each D Roll 30 D Time 20
minutes
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H companion 20.1 DH 13.2, r2.5 At
r2.5 background brightness is reduced by an
ADDITIONAL factor of 50 over raw coronagraphic
gain (of appx 4). Each independent image of
TWA6B is S/N 20 in difference frame.
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Imperfections in PSF-subtractions result in
residuals expected from pure photon
noise. Systematics OTA Breathing Target
Re-centration Coron. Edge Effects Mechanical
Stability
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Detectability and Spatial Completeness (r,q)
Dependence via Model PSF Implantation
Observed Model Nulled
Implant
TinyTim 5.0 HSTNICMOS Optical Model - Krist
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Detectability (r,q) Dependence via Model PSF
Implantation
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.
Photometric Efficacy Statistical Significance
2
5
2
0
1
6
S/N (Positive Implant Only)
Recovered Flux
1
2
8
4
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Detectability (1,q) Dependence via Model PSF
Implantation
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NICMOS
Camera 2 (0.076"/pixel)
F160W
Coronagraph (0.3" radius)
25 OCT 1998
Integration Time 1280s
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H-Band (F160W) Point-Source Detectability Limits
Two-Roll Coronagraphic PSF Subtraction 22m Total
Integration DH(5s) 7.14 3.15r - 0.286r 2
MK Stars
.
.
Photon Noise Dominated
Read Noise Dominated
H6.9
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TW Hya Assn K7primary, D 55pc Age 10
Myr r2.54, 140AU DH 13.2 (LB/A)H5
x10-6 Habs 16.6 Implies Mass 2Jupiter
Teff 800K IF Companion...
TWA 6A/B
S/NTWA6B 35
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Confirmation (or Rejection) by Common Proper
Motion
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Anomaly or Bias? A Jovian Planet _at_ gt 140 AU?
RV Surveys suggest 5 MS s have 0.88 Mjup
companions _at_ d lt 3AU from their primaries.
NOT Where Giant Planets are found in our own
Solar System WHY ARE THEY THERE? Posited
Mutual interactions within a disk can perturb one
young planet to move into a lt 1AU
eccentric orbit (as inferred from
RV surveys), and the other
Ejected (but bound) to very large separations, gt
100AU Cannot be observationally tested with
HST-like capabilities, requires Super-High
contrast imaging. e,g., Lin Ida (ApJ, 1997)
Boss (2001, IAU Symp 202)
43
Inner Regions of Evolved Disks
Cannot yet be probed in scattered light. Yet, as
inferred from mid-IR
What evolutionary and dynamical interactions may
be going on between unseen planets and unseen
dust which will shape these systems?
Requires Super-High contrast and resolution.
44
.
.
HST Has Sampled Only the Low-Hanging Fruit in
the Disk/Planet Orchard.
0
GL577B/C
HR 7329B
GL 503.2B
CD -33 7795B
-2
200M
jup
80M
jup
-4
TWA6B ?
L/Lsum
10
Log
sun
-6
14M
jup
-8
STARS (Hydrogen burning)
BROWN DWARFS (Deuterium burning)
JUPITER
PLANETS
SATURN
-10
6
10
8
9
7
Log
Age (years)
10
45
Anomaly or Bias? A Jovian Planet _at_ gt 140 AU?
RV Surveys suggest 5 MS s have 0.88 Mjup
companions _at_ d lt 3AU from their primaries.
NOT Where Giant Planets are found in our own
Solar System WHY ARE THEY THERE? Posited
Mutual interactions within a disk can perturb one
young planet to move into a lt 1AU
eccentric orbit (as inferred from
RV surveys), and the other
Ejected (but bound) to very large separations, gt
100AU e,g., Lin Ida (ApJ, 1997) Boss (2001,
IAU Symp 202)
46
UV/Optical imaging and spectroscopy of
collisionally evolved circumstellar debris and
co-orbital bodies will play a pivotal role in
furthering our understanding of the formation and
evolution of exosolar planetary systems. To
study physical processes acting over sub-AU
spatial scales and time scales comparable to the
age of our solar system will require a 34 order
of magnitude improvement in instrumental stray
light rejection over the performance obtainable
with HST.
GLENN SCHNEIDER NICMOS Project Steward
Observatory 933 N. Cherry Avenue University of
Arizona Tucson, Arizona 85721
Phone [phone]
FAX [phone] e-mail
gschneider_at_as.arizona.edu http//nicmosis.as.arizo
na.edu8000/
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Is it, or Isnt It?
Undetected in NICMOS 0.9mm Followup Observation
I-H gt 3 Marginally Detected in 6-Orbit
Binned STIS G750L Spectrum Colors Consistent
with 2 Mjup, 10 Myr, Hot Giant Planet
Instrument Band Bandpass Mag   NICMOS/C2
F160W 1.401.80 20.1 NICMOS/C2 F090M
0.801.00 gt23.1 STIS/G750L I extract
0.810.99 25.4 STIS/G750L R extract 0.630.77
gt27.2
If NOT a hot young planet, it must be a Highly
exotic object!
50
Is it, or Isnt It?
Undetected in NICMOS 0.9mm Followup Observation
I-H gt 3 Marginally Detected in 6-Orbit
Binned STIS G750L Spectrum Colors Consistent
with 2 Mjup, 10 Myr, Hot Giant Planet
Sudarsky et al., 2000
Spectrum from A. Burrows
Keck/AO Astrometric (PM) Follow-up Thus-Far
Inconclusive
51
Is it, or Isnt It?
A differential proper motion measure will be
obtained with NICMOS. If common proper motions
are confirmed we will request time for NICMOS
grism spectrophotometry to obtain a near-IR
spectrum.