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Project 1640: Conducting Remote Reconnaissances Of Other Solar
Systems
Ben R. Oppenheimer
Planets are complex
Vogt-Russell Theorem: “mass and chemical composition are sufficient to determine the structure, evolution and outward appearance of a star completely”
A few simple parameters are insufficient to
determine a planet’s salient features.
Our New Solar System
D. Jewi(
Jupiter
Trojans
Greeks
Hildas
M
M
V
E ¤
Our New Solar System
D. Jewi(
Direct Imaging Radial velocity -‐ blue TransiDng planets -‐ red Microlensing -‐ green Pulsar Dming -‐orange Solar system -‐ black Direct imaging -‐ purple Recent direct imaging -‐blue
Oppenheimer & Hinkley, Annual Reviews, 2009
Compara0ve Exoplanetary Science
• Observe individual planets in great detail – atmospheres, internal physics, geology and perhaps biology
• Observe as many planets as possible – At different ages, in different environments and with a broad range of parent stars (including pulsars and white dwarfs, giants and subgiants)
• A 0ny taste of what we might learn: – What do 50 different 1MJ planets have in common? – What does a young (or old) Earth mass planet look like? – What is a 5 Earth mass planet?
Toward a comprehensive theory of planet formation and evolution
WE NEED SPECTRA!
Contrast Needed Jupiter at various ages
DetecDon: 10-‐7 Study: 10-‐9 -‐ 10-‐10
Burrows et al. 2004
Gliese 229
Speckles
Project 1640 at Palomar: Through the Speckles
Four Instruments + 57,427 lines of Code • P3k AO system with 3388+241
actuator DMs (JPL/Caltech) • IFS covering λ = 0.98 -‐ 1.75µm,
3.8” FOV, 19-‐mas plate scale (AMNH/IoA)
• Apodized Pupil Lyot Coronagraph (AMNH)
• Wave Front CalibraDon Interferometer (JPL)
• Data extracDon pipeline (AMNH)
• Two Novel speckle suppression pipelines: KLIP (Pueyo) and S4 (Fergus)
Contrast: 10-‐7 at 1”
Palomar mountain crew: Bruce Baker, Mike Doyle, Carolyn Heffner, John Henning, Greg van Idsinga, Steve Kunsman, Dan McKenna, Jean Mueller, Kajsa Peffer, Kevin Rykowski, and Pam Thompson. This project would be impossible without the flexibility, responsiveness and dedicaDon of such an effecDve and moDvated staff.
Current Students: Eleanor Bacchus (IoA, Cambridge), Trevor David (Caltech) Aaron Veicht (AMNH/Columbia), Postdocs: Christoph Baranec (Caltech), Eric Cady (JPL), StaDa Cook (AMNH), JusDn R. Crepp (Caltech, now faculty at Notre Dame), Sasha Hinkley (AMNH student, now at Caltech), Ricky Nilsson (AMNH), Laurent Pueyo (Now faculty at STScI), Emily Rice (AMNH, now faculty at CUNY-‐SI) Neil Zimmerman (AMNH student, now at MPIA Heidelberg) Senior Research Scien0sts: Douglas Brenner (AMNH), David King (IoA/Cambridge), Rick Burruss (JPL), Lewis C. Roberts, Jr (JPL), Jennifer E. Roberts (JPL), Michael Shao (JPL), Anand Sivaramakrishnan (STScI), Richard Dekany (Caltech), Tuan Truong (JPL), Gautam Vasisht (JPL), Fred Vescelus (JPL), Chengxing Zhai(JPL), David Hale (Caltech), E. Robert Ligon (JPL), Tom Lockhart (JPL) Faculty: Charles Beichman (NExSci/Caltech), Rob Fergus (NYU), Ian R. Parry (IoA Cambridge), Lynne Hillenbrand (Caltech), David W. Hogg (NYU), Rémi Soummer (STScI)
Find out what they all did on our project website: www.amnh.org/project1640
The Team
No Adaptive Optics (AO) AO on, star unocculted, short exposure
AO on, star occulted, long exposure
AO on, star occulted, Calibration system on, long exposure
S4 Speckle Suppressed Sequence of exposures
N"
E" 0.5”"
b"
e"
d"
c"
S4"Algorithm"
Project 1640Toward Exploration of Other Worlds
Paco, the 1640 spokes-‐dog, apologizes for having a previous engagement
N"
E" 0.5”"
b"
e"
d"
c"
KLIP"Algorithm"
N"
E" 0.5”"
b"
e"
d"
c"
S4"Algorithm"
Two Independent Speckle Suppression Techniques:
Level of Speckle Suppression
Location of companion
Com
panio
n in
tensi
ty (
rel.%
)RMS Spectral Extraction Error
bcd
e
20 25 30 35 40 45 50
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
a Published values are from Marois et al. (2008), Marois et al. (2010b) and Skemmer et al. (2012).
The primary has MH = 2.30m (Cutri et al. 2003).
f λ
Fake Source Tests and Spectrum Fidelity
1000 1100 1200 1300 1400 1500 1600 17000
0.5
1
1.5
2
2.5
Wavelength (nm)
No
rma
lize
d f
! (
arb
. u
nits
)
Location of HR8799b
Ground TruthEstimated
1000 1100 1200 1300 1400 1500 1600 17000
0.5
1
1.5
2
2.5
3
Wavelength (nm)
No
rma
lize
d f
! (
arb
. u
nits
)
Location of HR8799c
Ground TruthEstimated
1000 1100 1200 1300 1400 1500 1600 17000
0.5
1
1.5
2
2.5
Wavelength (nm)
No
rma
lize
d f
! (
arb
. u
nits
)
Location of HR8799d
Ground TruthEstimated
1000 1100 1200 1300 1400 1500 1600 17000
0.5
1
1.5
2
2.5
3
3.5
Wavelength (nm)
No
rma
lize
d f
! (
arb
. u
nits
)
Location of HR8799e
Ground TruthEstimated
Barman et al. 2011a, ApJ 733, 65
b component
f λ
Conclusions Regarding HR8799 companions
We have now entered a new regime of diversity that physicists and astronomers are not accustomed to
Survey: 250 A0-F5V Stars • 99-‐night survey has begun for 1-‐100 MJ companions
• Observed roughly 20 of the target stars so far • EsDmated compleDon Dme: 3.5 years (end of 2015)
• Sample opDmized for youth and distance (Beichman et al 2010, PASP, 122, 162)
• EsDmate 5-‐25 new companions
• CollaboraDve agreement with GPI in place for overlapping region of sky (note: roughly 30% of the GPI team is also involved in P1640)
f λ
λ (µm)
B9IV 51.8 pc 2.8 M¤
72 L¤ ~185 Myr
κ Andromedae
Hinkley et al. (submitted)
A Hint at the Bigger Picture
• Are the terms “star,” “Brown dwarf” and “planet” meaningful categories?
• ExaminaDon of 2413 companions of stars • Require orbital parameters P, a, e, M1, M2
• Data gathered from ~180 sources in the literature and several compendia
1.E$06'
1.E$05'
1.E$04'
1.E$03'
1.E$02'
1.E$01'
1.E+00'
1.E+01'
0.001' 0.01' 0.1' 1' 10' 100' 1000' 10000'
Companion'Mass'
a'(AU)'
All Known Binaries with orbit determina0ons (M
¤)
Project 1640
“Stars”
“Brown Dwarfs”
“Planets”
1.E$06'
1.E$05'
1.E$04'
1.E$03'
1.E$02'
1.E$01'
1.E+00'
0.01' 0.1' 1' 10' 100'
q'
Primary'Mass' (M¤)
