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From Greek Philosophers ...
“There are infinite worlds both like and unlike this world of ours...We must believe that in all worlds there are living creatures and plants and other things we see in this world.”--- Epicurus (c. 300 B.C)
…to Medieval Scholars...
“I [regard]… as false and damnable the view of those who would put inhabitants on Jupiter, Venus, and Saturn, and the moon, meaning by ‘inhabitants’ animals like ours and men in particular.”
…and Medieval Martyrs...
"There are countless suns and countless earths all rotating around their suns in exactly the same way as the seven planets of our system. We see only the suns because they are the largest bodies and are luminous, but their planets remain invisible to us because they are smaller and non-luminous. The countless worlds in the universe are no worse and no less inhabited than our Earth”Giordano Bruno (1584) in De L'infinito Universo E Mondi
…To Hollywood Producers…Klaatu Borada Nikto
“Your choice is simple. Join us and live in peace or pursue your present course and face obliteration. We shall be waiting for your answer. The decision rests with you.”
NASA’s Origins Theme Has Two Defining Questions
Are We Alone?
Search for Life Outside the Solar system
• Remote detection of the signposts of biological activities on extra- solar planets
Where Did We Come From?
Tracing Our Cosmic Roots• Formation of galaxies, stars, heavy elements, planetary systems and ….. life on the Early Earth
NASA Origins Science GoalsNASA Origins Science Goals
Understand How Stars
and Planetary Systems
Form and Evolve2
Determine Whether Habitable
or Life-bearing Planets Exist Around Nearby Stars
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1
Understand How Galaxies Formed in the
Early Universe
Some Fundamental Scientific Facts To Remember
• The necessary ingredients of life are widespread – Observation reveals uniformity of physical and chemical laws – Origin of the elements and their dispersal is well understood
• Life on Earth can inhabit harsh environments– Micro- and environmental biology reveal life in extremes of
temperature, chemistry, humidity
• Life affects a planetary environment in a detectable way– Our own atmosphere reflects the presence of primitive through
advanced life
• Planets are a common outcome of star formation– Modern theory of star formation makes planet formation likely
IR, submm, mm spectra reveal gas phase, ices, mineralogical signatures of many species, incl:H2O, CO2, CH3OH, CO, CH4, formic acid (HCOOH) and formaldehyde (H2CO), etc.
…Star Forming
Regions…
…and distant galaxies
• Polycyclic Armomatic Hydrocarbons (PAHs)– Complex 2-D carbon
molecules (>25 carbon atoms)
– Found in many active galaxies
Pierre et al 2001
z=1.5??
Barthel 2001
PAH
• Perhaps in distant quasar at z~1.5 (wait for SIRTF)
• CO detected in a very distant quasar (z=4.1!)– Found with more complex species in
more nearby objects
Life is Hardy
• Life needs water, a source of energy, and cosmically abundant elements
•Extremophiles can live in hot (~120 C!) acid lakes, near undersea volcanic vents, in underground aquifers, and within rocks in Antarctica
Star Formation & Protoplanetary Disks• The formation of planets is an integral part of our theory of how stars
form– Hundreds of planetary masses of gaseous and solid material in the protostellar
disk
• Solar System-scale dust disks found around nearby stars
Fomalhaut
Debris DisksFrom the Ground
• Sub-millimeter (SCUBA/JCMT) observations of disks reveal evacuated cavities the size of our solar system as well as clumps that may be structures associated with planets
• Many groups searching for planets using AO
Beta Pic
Eps Eri
SIRTF Observations of Disks• NASA’s next Great Observatory will map disks, survey 100s stars
– single, binary–with, w/o planets–ages from 1 million to 5 billion yr
• SIRTF launches April 18 after 25 years!
Finding Planets Indirectly
• Gravitational Effects on Parent Star– Radial Velocity Changes– Positional Wobble
(Astrometry)
• Effect of Planet on Star’s Brightness– Transits of edge-on systems– Gravitational micro-Lensing
Gas Giant Planets
• Over 100 planets found using radial velocity wobble
– ~10% of stars have planets – Most orbits < 2-3 AU– Half may be multiple systems
???
Marcy et al.
• Planets on longer periods starting to be identified
– 55 Cancri is solar system analog
• Radial velocity technique not sensitive to terrestrial planets
The Royal Society sent Captain Cook along with Joseph Banks to Tahiti to observe a transit of Venus on June 3, 1769 to set the scale of the Solar System
Planetary Transits: Then and Now
Fundraising: Cook, Joesph Banks, and Lord Sandwich.
Transit Determines Planet’s Properties
• Transits of HD 209458 determine properties of another Solar System– Confirmation of planet interpretation – Inclination= 85.9– Mass= 0.69 ± 0.07 Mjup
– Radius =1.35 ± 0.06 Rjup
– Density= 0.35 g/cc <Saturn
• Active ground based efforts using 10 cm to 10 m telescopes
• COROT, Kepler and Eddington will find fewhundreds of Earths, thousands of Jupiters
• Spectroscopy probes atmosphere– Cloud heights, heavy-element abundances, temperature
and vertical temperature stratification, and wind velocities
Astrometric Search for Planets
• Astrometry measures positional wobble due to planets
• Interferometry enables measurements at the micro-arcsecond level
• Result of new observing systems will be a census of planets down to a few Mearth
over the next 10-20 years
Interferometery Is One Key to Planet Detection
• Enables precision astrometry, high resolution imaging, starlight nulling
• Make astrometric census of planets • Detect “Hot Jupiter’s” • Detect exo-zodiacal dust clouds• Image protostellar disks
• Break link between diameter, baseline
Space Interferometer Mission (SIM) Will Make Definitive Planet Census
A Deep Search for Earths• Are there Earth-like (rocky)
planets orbiting the nearest stars?
• Focus on ~250 stars like the Sun (F, G, K) within 10 pc
• Sensitivity limit of ~3 Me at 10 pc requires 1 µas accuracy
A Broad Survey for Planets • Is our solar system unusual?• What is the range of planetary system architectures?• Sample 2000 stars within ~25 pc at 4 µas accuracy
Evolution of Planets• How do systems evolve?• Is the evolution conducive to the
formation of Earth-like planets in stable orbits?
• Do multiple Jupiters form and only a few (or none) survive?
What We Don’t Know• Are planetary systems like our own common?• What is the distribution of planetary masses?
– Only astrometry measures planet masses unambiguously
• Are there low-mass planets in ‘habitable zone’ ?
But What is a Habitable Planet?
• Not too big– Avoid accreting
material to become gas giant
• Not too small– Lose atmosphere
• Not too hot or too cold– No liquid water
• Not too close to star– Avoid tidal lock
Finding Terrestrial Planets• Detecting light from planets
beyond solar system is hard:– Planet signal is weak but
detectable (few photons/sec/m2)
– Star emits million to billion more than planet
– Planet within 1 AU of star– Dust in target solar system
300 brighter than planet
• Finding a firefly next to a searchlight on a foggy night
>109>106
Four Hard Things About TPF • Sensitivity (relatively easy)
– Detection in hours spectroscopy in days. – Integration time (distance/diameter)4
– Need 12 m2 of collecting area (>4 m) for star at ~10 pc
• Angular resolution (hard)– 100 mas is enough to see ~25 stars, but requires >4 m coronagraph or >20 m
interferometer– Baseline/aperture distance
• Starlight suppression (hard to very hard)– 10-4 to 10-6 in the mid-IR– 10-8 to 10-10 in the visible/near-IR
• Solar neighborhood is sparsely populated– Fraction of stars with Earths (in habitable zone) unknown– Unknown how far we need to look to ensure success– Surveying substantial number of stars means looking to ~15 pc
Signatures of Life• Oxygen or its proxy ozone is most reliable biomarker
– Ozone easier to detect at low Oxygen concentrations but is a poor indicator of quantity of Oxygen
• Liquid water on a planet’s surface is considered essential to life.
• Carbon dioxide indicates an atmosphere and oxidation state typical of terrestrial planet.
• Abundant Methane can have a biological source– Non-biological sources might be confusing
• Find an atmosphere out of equilibrium• Expect the unexpected
Mars Odyssey Looks Back at Earth
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Christensen and Pearl 1997
Goals for Terrestrial Planet Finder• Primary Goal: Direct detection of emitted or reflected radiation
from Earth-like planets located in the habitable zones of nearby solar type stars. – Determine orbital and physical properties – Characterize atmospheres and search for bio-markers– Search a statistically meaningful sample of stars (30-150)
• The Broader Scientific Context: Comparative Planetology– Understand properties of all planetary system constituents, e.g. gas giant
planets, terrestrial planets and debris disks.
• Astrophysics: An observatory with the power to detect an Earth orbiting a nearby star will be able to collect important new data on many targets of general astrophysical interest.
TPF Candidate Architectures• Visible Coronagraph
– System concept is relatively simple, 4-10 m mirror on a single spacecraft
– Components are complex• Build adequately large mirror of
appropriate quality (/300)• Hold (/3000) stability during
observation with deformable mirror
• IR Interferometer− Components are simple: 3-4 m mirrors of average quality−System is complex: 30 m boom or separated spacecraft
The Challenge of Angular Resolution
+
• Coronagraphs at >3/D• Interferometers at > 1 /B
10 mm, 28 mCoronagraph
Cost ($$), L
aun
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• How many stars to avoid mission failure (Np = 0)• How many stars to ensure enough planets (Np >5) # Stars Dist(Aperture, Baseline)CostSchedule
How Many Planets Are Enough ?
Visible Light Planet Detection• A simple coronagraph on NGST could detect
Jupiters around the closest stars as well as newly formed Jupiters around young stars
• Advanced coronagraph/apodized aperture telescope– 2~4 m telescope (Jupiters and nearest Earths) – 8~10 m telescope (full TPF goals)
• Presence and Properties of Planets– Planet(s) location and sizereflectivity– Atmospheric or surface composition– Rotation surface variability– Radial and azimuthal structure of disks
Simulated NGST coronagraphic image of a planet around Lalande 21185 (M2Vat 2.5pc) at 4.6 mm
Control of Star Light
• Control diffracted light with various apodizing pupil and/or image plane (coronagraph) masks– Square masks– Graded aperture– Multiple Gaussian masks– Band limited masks
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• Control scattered light with deformable mirror
−10,000 actuators for final l/3000 wavefront (<1 Å)
Coronagraph Status• Current contrast limited to 10-5 due to DM
imperfections and lab seeing−New DM due from Xinetics in March
• Kodak selected to provide large (1.8m), high precision (<5 nm) Mirror
− Very similar to SNAP mirror!• Innovative ideas to improve angular
resolution by combining interferometer and coronagraph ideas
5 Airy rings
10-5
IR Interferometer
• Interferometer with cooled two to four 3~4 m mirrors – 30 m boom – 75-1000 m baseline using formation flying
• Operate at 1 AU for 5 years to survey 150 stars
Goal Earth at 10 pc TimePlanet? R=3/SNR=5 2.0 hourAtmosphere? R=20/SNR=10 2.3 day CO2, H2O Habitable? R=20/SNR=25 15.1 day O3, CH4
Interferometer Detects and
Characterizes Planetary Systems
• TPF produces image of planetary system
– Orbital location– Temperature and radius
• TPF produces spectrum to search for biomarkers• 1-2 m telescopes to find Jupiters, nearest Earths•3-4 m telescopes for full TPF goals
IR Nulling • JPL Modified Mach-Zender (Serabyn et al)– 1.4 10-6 null laser null @ 10.6 um – Aim for 10-6 null target broadband
• Add spatial filter• Active pathlength stabilization
Nulling with two detectors- only low end detector shown, ignore initial spikes
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• UofA group (Hinz et al) demonstrated nulling with BLINC instrument on MMT
Pre-TPF Study Will Span Wavelengths, Techniques, Years, Ground and Space,
Theory and Observation
Hale Bopp
Planet Finding Is A Decades-Long
Undertaking• Like cosmology, the search
for planets and life will motivate broad research areas and utilize many telescopes for decades to come
• NASA’s program for planet finding will be broad and rich, with results emerging on many time scales, from the immediate to the long-term
• There are exciting, mid-term ways to detect giant planets and the nearest Earths
Collaboration on TPF/Darwin• Strong ESA/NASA interest in
joint planet-finding mission– Collaborative architecture studies– Discussions on technology
planning and development• Joint project leading to launch
~2015– Scientific and/or technological
precursors as required and feasible
The NASA Vision– To improve life here– To extend life to there– To find life beyond
The Science Vision“Search for Life outside of earth and, if it is found, determine its nature and its distribution in the galaxy…[This] is so challenging and of such importance that it could occupy astronomers for the foreseeable future” --- NAS/NRC Report