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Ben R. Oppenheimer, Sasha Hinkley, Anand Sivaramakrishnan, Remi Soummer, Douglas Brenner - PowerPoint PPT Presentation


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PROJECT 1640 AN ANCILLARY OF. Ben R. Oppenheimer, Sasha Hinkley, Anand Sivaramakrishnan, Remi Soummer, Douglas Brenner Ian Parry, David King, Steve Medlen http://lyot.org. Digital Universe: http://haydenplanetarium.org. Giants to scale. Planets are complex.

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slide1

PROJECT 1640

AN ANCILLARY OF

Ben R. Oppenheimer, Sasha Hinkley, Anand Sivaramakrishnan, Remi Soummer, Douglas Brenner

Ian Parry, David King, Steve Medlen

http://lyot.org

planets are complex

Giants to scale

Planets are complex

Vogt-Russell Theorem: “mass and chemical composition are sufficient to determine the structure, evolution and outward appearance of a star completely”

Planets have a diversity possibly unmatched in astronomy, and the theorem does not apply

The onset of complexity perhaps begins in the brown dwarf mass range where age is needed as well.

In coolest or lowest mass BDs, more complexity: The chemistry and SEDs are drastically affected by minor changes in composition, mass, age

Terrestrial Planets to scale

A few simple parameters are insufficient to determine a planet’s salient features.

slide4

3.6 m telescope atop Haleakela (Maui)

  • 941 actuator AO system
  • 80-90% Strehl at H-Band
  • Optimized, diffraction-limited coronagraph
  • 30 stars observed (1 candidate planet, 7 BDs, 3 disks)
  • Differential Polarimeter working
  • Integral Field Unit being built now
planet and brown dwarf sensitivity
Planet and Brown Dwarf Sensitivity

Lyot Project

Discovery Space

Known but

unseen

exoplanets

(Marcy et al.

2003)

some nearby star
Some Nearby Star

H-Band

S ~ 80-90%

H-Band

15 minute exp.

Oppenheimer et al. in prep.

Weird colors

(i, z, J, H, K)

Companionship

confirmed

Speckles are the bane of any exoplanet imager, even in space!

dynamic
Dynamic

Current

Performance

Dynamic

Range

Vega

Companion

Mass limits

Polarimetry

Speckle subtraction

Hinkley et al. 2006, astro-ph/0609337

hr4796
HR4796

Oppenheimer et al., in prep.

project 1640 integral field unit seeing through the speckles
Project 1640: Integral Field UnitSeeing through the speckles
  • Data Cube Movie
  • 10 nm Steps
  • S ~ 90%
  • = 1.6 m (1.0 at left)

Planet has flat spectrum

AO Performance

matched to current

AEOS performance

optics
Optics

R ~ 30-100 lenslet-based IFU

J-H band (1-1.85 µm)

4” FOV (200x200 spatial pixels)

First Light Jan 2008

Lenslet Array

HAWAII-II Array

Prism

~0.5 m

Dewar is Identical to PHARO’s

planet and brown dwarf sensitivity1
Planet and Brown Dwarf Sensitivity

PALM3000 + P1640

Discovery Space

Known but

unseen

exoplanets

(Marcy et al.

2003)

project 1640 passed cdr
Project 1640 Passed CDR

Design Review included 4 external people:

Jamie Lloyd (Cornell), James Larkin (UCLA), David Schiminovich (Columbia)

Russ Makidon (STScI)

Recommendation:

“collaboration with the Palomar

Observatory should be sought

immediatelyto put the team and

Palomar at the forefront of high

contrast science”

July at AMNH

Concept: Bring 1640 to 200”

put it and a small version of Lyot

behind the 3000 actuator AO system

Fully funded ($1.8M)

p1640 with palm3000
P1640 with PALM3000

Unique capability for years to come

Gemini Planet Imager and VLT’s SPHERE slated for late 2010

and both are in the south, and perhaps only marginally more sensitive

Hundreds of planets, circumstellar disk chemistry, disk evolution

PALAO (prior to upgrade): 1-2 magnitude improvement over AEOS

but much fainter stars are accessible

LGS: Galaxies

Solar System science (eg Kuiper belt moon spectroscopy)

Young stars

Debris disk science - spatially resolved chemistry

M-dwarf companions

Evolved star astrophysics

We have the money, the people and an instrument.

Palomar is the best place in the world suited to do this work

ten years of coronagraphy
Ten Years of CoronagraphyA Decade of Coronagraphy

Part of Palomar’s

Heritage is

Cutting-dege

Coronagraphy