# Presentation: 090506

## Ground-Based Exoplanet Searches

- Princeton University
- Radial Velocity
- Astrometry
- Transits
- Lensing
- Pulsation Timing
- Disks
- Direct Detection

## Timing:

- Pulsars + White Dwarfs

- t = z / c

- Time Stamp on Each Pulse gives you
- More Information than Doppler Shift

## Pulsar planet interactions

- 4.3, 3.9 M
- Konacki & Wolszczan 2003

- Mukadam et al. 2003

## Microlensing  

- Einstein Ring

- background star

- Paczynski 1996

- Microlensing
- Mao & Paczynski 1991

## Probing Lensing Anomalies NETwork (PLANET)

- V

- days

## caustic

- Planet near RE around
- lensing star.
- Lensing Stars/yr
- OGLE-III: 500
- MOA: 60

## If 3/4 of lenses had

- 43 events from PLANET.   Gaudi et al. 2003

- Projected Separation
- units of RE

- mostly M stars
- halfway to galactic
- center
-  RE~ 2.5 AU

- planets above this
- line, they would
- have been detected.

- 1/4

- 3/4

## Direct Detection: Optical

- Boo:   A < 0.39
-       at i = 36R=1.2 RJ
-            (Leigh et al. 2003)
-  And: similar (Cameron et al. 2002)

- star

- star + planet

## Direct Detection:

- Nulling (Mid+Near IR)

## Slide 10

## Slide 11

## Slide 12

## Keck Interferometer

## Slide 14

## Inside Quadratic Null:

- star and planet are spectrally
- degenerate ()
- planet  and flux are degenerate

## VLTI:

**VLTI:**
**Ground-based European Nulling Interferometer Experiment (GENIE****)**

## Direct Detection:

- Differential Phase
- (near IR)

## center of light

- Burrows 2000

## 2 m

- 2 m

- 5 m

- Serabyn 2002

## Slide 20

## Large Binocular Telescope (LBT)

**Large Binocular Telescope (LBT)**

## Antarctica: 

- Cold, Dry, and No High-Altitude
- Turbulence
- Nulling, AO, Differential Phase,
- Astrometry
- Antarctic Planet Interferometer (API)

## Astrometry

- perturbation
- magnified 30x  !!

- 15 MJ
- e=0.2 a=0.6 AU
- d=50 pc =50 mas/yr
- Perryman 2000

- Stellar Planet Survey
- (STEPS)
- 30 M stars
- Astrometric Search for Planets Encircling Nearby Stars (ASPENS)
- 100 stars
-  2 mas: 10 MJ in 4 years
- 1 MJ in 15 years

## Direct Detection:

- Near Infrared

## Simulated 15 minute H-band image 
5 MJ planet/solar-type star

4096 actuators 

Extreme Adaptive Optics
Planet Imager (XAOPI)
Bruce Macintosh, James
Graham et al.

- Simulated 15 minute H-band image
- 5 MJ planet/solar-type star
- 4096 actuators
- Extreme Adaptive Optics
- Planet Imager (XAOPI)
- Bruce Macintosh, James
- Graham et al.

- 1.6 arcseconds

## Kuchner &

- Traub 2002

## Slide 27

## Direct

- Detection:
- Radio

- cyclotron maser

*[Kraus, RadioAstronomy, 1966]*

## Radio Bode's Law

*Radio Bode's Law*

- •

*•*

*Zarka et al. 2001*

## Farrell, Desch & Zarka 1999

- VLA
- Green Bank Telescope
- Nancay Decametric Array
- Arecibo

- LOFAR : Farrell et al. 2003

## ALMA

- Hot Young
- Jupiter at 160 pc~10 mJy at 850 m

## Disks

##  Eridani 15, 20 and 40 m

-  Eridani 15, 20 and 40 m

- Moran, Kuchner & Holman 2003

## Timing

- Direct Infrared

- Astrometry and Lensing

- Radial Velocity and Transits

## log “Q”: 

- log “Q”:
-  0
- -2
-        Transits
- -4
- -6
- -   Radial Velocity, Astrometry & Microlensing

- Nulling          Coronagraphy

-  spectral signal from hot Jupiter

- residual stellar signal

- Differential Phase

- Doppler Tomography

## Slide 36