High Contrast Imaging with Coronagraphy and Integral Field Spectroscopy

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High Contrast Imaging with Coronagraphy and
Integral Field Spectroscopy
Sasha Hinkley Sagan Fellow, Caltech Berkeley AO
Seminar, Oct. 20th 2009
Ben R Oppenheimer Doug Brenner Remi Soummer
(STScI) Anand Sivaramakrishnan Neil Zimmerman
Lynne Hillenbrand Justin Crepp Rich
Dekany Antonin Bouchez
Photo by Scott Kardel
Lewis Roberts Mike Shao Gautam Vasisht Rick
Burruss Jenny Roberts Chas Beichman
Ian Parry Stephanie Hunt
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The Known Planets
less sensitivity
Marcy et al. 2005
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Transits Radial Velocity
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Transits Radial Velocity
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Transits Radial Velocity Direct Imaging
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Direct Imaging
Images with help from Remi Soummer
Radial velocity - blue Transiting planets -
red Microlensing - green Pulsar timing
-orange Solar system - black Direct imaging -
purple Recent direct imaging -blue

• Frequency of planets around host stars as a
  function of . . .
• Host star type
• Host star metallicity

Oppenheimer Hinkley, ARAA, 2009
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Recent Direct Imaging
Oppenheimer Hinkley ARAA Vol. 47

• Fomalhaut b
• 119 AU
• Few MJup

• HR 8799 b, c, d
• 68, 38, 24 AU
• 7, 10, 10 MJup
• 60 Myr system

Kalas et al. (2008)
Marois et al. (2008)
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Recent Direct Imaging
Get Spectra
Oppenheimer Hinkley ARAA Vol. 47

• Fomalhaut b
• 119 AU
• Few MJup

• HR 8799 b, c, d
• 68, 38, 24 AU
• 7, 10, 10 MJup
• 60 Myr system

Kalas et al. (2008)
Marois et al. (2008)
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The Lyot Project (AEOS)

• Optimized, diffraction limited classical Lyot
  Coronagraph.
• Deployed at 3.63m AEOS alt-az telescope on
  Heleakala. 941 actuator, Shack-Hartmann AO
  system.

• Survey in J, H, and Ks bands. Dual-channel
  imaging polarimetric observations to access Q,U,
  and V stokes images.

• Precursor project to our
• current Palomar project

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Correlated Speckle Noise Limits Sensitivity
Coronagraphically-occulted (AO on!) H-band
sequence of images (40 min) from the star Vega
from the AEOS 3.63m telescope.
Correlated speckle noise is the greatest
hindrance to ground-based exoplanet detection.
Hinkley et al. (2007)
Averaging does not work
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Speckle Lifetimes

• Autocorrelation was calculated for each pixel.
  Similar to Fitzgerald Graham (2006)
• Two distinct timescales evident.
• ??short rapid decorrelation of speckles, slight
  increase in dynamic range.
• ?long measure of quasi-static speckle
  lifetimes.

Hinkley et al. ApJ 654, 633 (2007)
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Dynamic Range Evolution
Hinkley et al. ApJ 654, 633 (2007)
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Method 1 Speckle Subtraction

• Subtraction of purely static, rotating spider
  speckles in telescope pupil frame gives
  significant improvement.
• Similar to Marois (2006)

Subsequent subtraction of speckle pattern due to
DM and AO optics gives even more improvement.
Hinkley et al. ApJ 654, 633 (2007)
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Dynamic Range Improvement (Method 1)
Hinkley et al. ApJ 654, 633 (2007)
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Method 2 Speckle Suppression Through Polarimetry
Hinkley et al. ApJ (2009)
See also Perrin, Duchêne, Kalas, Graham
(2006) Oppenheimer et al. (2008)
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Polarimetric Dynamic Range
Traditional Dynamic range
Dynamic range after polarimetric speckle
suppression
Residual deviation from Gaussian-likeBehavior
200-300 mmag.
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Hinkley et al. ApJ (2009)
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The Lyot Project Polarimetry Results
HR 4796A
Models
Thanks to James Graham for providing models!
Hinkley et al. ApJ (2009)

• Lower limit fractional polarization 29
• Scattering Asymmetry parameter
• g ltcos(?)gt 0.20 /- 0.7

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Method 3 Speckle Suppression Through Chromaticity
BLUE (1.0 ?m)
RED (1.8 ?m)
Plan Utilize the chromatic nature of speckles
with a IFS.
Automatically provides spectra of any companions.
Enables differentiation between speckles and
companions
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Simulation courtesy of Remi Soummer James Lloyd
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Project 1640 IFUCoronagraph at Palomar

• Science Camera IFU covering
  ?? 1.05 - 1.75µm (J to H bands)
• Diffraction-limited Apodized Pupil Lyot
  Coronagraph (APLC)
• Separate (2nd Stage) IR fine guidance system
• Designed to interface with the Palomar
  AO system (PalAO)
• Only project like it in the Northern Hemisphere.

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Integral Field Spectrograph

• Microlens based design (a la OSIRIS)
• No moving internal parts
• Entirely cold optics
• JH filter permits observation
• over 1.05-1.75 µm at once

JH prism
Collimating optics
Lenslet array
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Project 1640 Spectrograph Internals

• Array of 270 x 270 microlenses each with
• 75?m pitch. Two
• powered faces.
• Rockwell Hawaii-II 2048x2048 pixel HgCdTe array

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Coronagraph APLC
Fold
Focal Plane Mask
OAP2
Lyot Stop
OAP3
Fold
Final Sphere (above plate)
Atmospheric Dispersion Prisms
Infrasil Window
OAP1
Apodizer
AO Input Beam
Fast Steering Mirror
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Coronagraph Masks
FPM 5.37?/D at 1.65 ?m, .37 arcsec on
sky hole diameter 1332 microns Lyot stop
2 downsized from primary Beam size at
stop 3.8mm
Apodizing mask Chromium microdots
(1?m) on glass IR Tip/Tilt system using
Hamamatsu InGaAs quad cell. 1kHz update
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Integrated System
Project 1640 and Palomar 5-m AO System
IFU
AO System
Coronagraph
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Initial Data
Monochromatic 1330nm light source
Broadband white light source
Photo by Scott Kardel
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Data
Data cube spans 1.05 - 1.75 ?m.
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Stellar Companion to a Nearby A-star

• Photometry suggests
• 0.16 M_solar.
• Mass ratio q 0.07

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1.25?m
1.58?m
1.73?m

• Isocrones
• 600 Myr (black)
• 200 Myr (red)

Hinkley et al. (2009) in prep
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Stellar Companion to a Nearby A-star

• Photometry
• Astrometry
• CPM
• Orbital motion
• Spectrum

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1.25?m
1.58?m
1.73?m
Hinkley et al. (2009) in prep
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Stellar Companion to a different Nearby A-star

• Golub (1983), Schmitt (1985) suggest unseen
  M-dwarf companions may be the source of
  anomolously high X-ray counts.

• Common parallax obtained
• Anomolously high
• ROSAT brightness
• M3-M4 companion

Zimmerman et al. (2009) in prep
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Stellar Companion to a different Nearby A-star
Data cube spans 1.05 - 1.75 ?m.
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Titan
Data cube spans 1.05 - 1.75 ?m.
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Speckle Suppression with LOCI (Locally Optimized
Combination of Images)
See LaFrenière et al. (2007)
Images courtesy of Laurent Pueyo
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Performance
Still some sensitivity issues. Speckle
suppression Seems to gain about 4
magnitudes. Contrast not dependent on
telescope aperture (see Keck/Palomar curves
in black.
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SPHERE (VLT)
Gemini Planet Imager
MEMS Extreme-AO apodized pupil coronagraph
IFS (1-2.4 ?m), R45, 2.8"x2.8" FOV Dual
channel polarimetry Wave front calibration
system
Beuzit et al (2008)
First light 2011
(south)
Extreme-AO (41x41 actuator)
coronagraph Differential imaging (Y, J, H,
Ks) IFS (0.95-1.65 mm) R30, 1.8" x
1,8"FOV Visible Imaging Polarimeter
Macintosh et al (2008) Graham et al (2007) ExoPTF
white paper
First light 2011
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The Future

• PALM3K upgrade(2010)
• New 3000 actuator Xinetics deformable mirror
• High-order Wave Front Sensor (62 x 62
  Shack-Hartmann)
• Low-order WFS (visible/IR pyramid sensor)

Wave Front Calibration system (2009 -10)

• Interferometer nearly identical to GPI
• Designed to achieve 1nm RMS wave front error
  measurement at 1Hz
• Dynamic Control of wave front errors

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Ongoing P1640 Observations

• Opportunities planet searches, binary star
  studies, and planetary science.
• Data cubes obtained for at least 100 stars.
• Data cube extraction pipeline is mature.
• At least 500 GB of data.

Observing Plan

• Initial survey with current PalAO system (2008-9)
  Magnitude limit 13th
• Key Project Survey with PALM3000 and Calibration
  system (2010-12).
• Magnitude limit 8th

1.34?m
1.55?m
1.67?m
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