Imagining the Future: Gravitational Wave AstronomyBCBAct/talks04/GW... · 28-Oct-04 Imaging the...
Transcript of Imagining the Future: Gravitational Wave AstronomyBCBAct/talks04/GW... · 28-Oct-04 Imaging the...
Imagining the Future: Gravitational Wave Astronomy
Barry BarishCaltech
28-Oct-04
“What infrastructure will contribute to facilitating broad participation, community growth, and the best possible science?”
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A Roadmap for the FutureFrontier Pathway
Scenic and Historic BywayA "roadmap" is an extended look at the future of a chosen field of inquiry composed from the collective knowledge and imagination of the brightest drivers ofchange in that field.
R GalvinMotorola
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Creating a Roadmap for the FutureGravitational Wave Astronomy
• What have we accomplished?
• Where are we now?
• Where are we going?
• What are the paths to get there?
• What tools do we need to reach our goals?
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Comparing the Evolutionof Two Fields
Neutrino Physicsand Astronomy
Gravitational WaveAstronomy
Solar Neutrinos Binary Black Hole Merger
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Wolfgang Pauli
Pauli's letter of the 4th of December 1930
Dear Radioactive Ladies and Gentlemen,
As the bearer of these lines, to whom I graciously ask you to listen, will explain to you in more detail, how because of the "wrong" statistics of the N and Li6 nuclei and the continuous beta spectrum, I have hit upon a deseperateremedy to save the "exchange theorem" of statistics and the law of conservation of energy. Namely, the possibility that there could exist in the nuclei electrically neutral particles, that I wish to call neutrons, which have spin 1/2 and obey the exclusion principle and which further differ from light quanta in that they do not travel with the velocity of light. The mass of the neutrons should be of the same order of magnitude as the electron mass and in any event not larger than 0.01 proton masses> The continuous beta spectrum would then become understandable by the assumption that in beta decay a neutron is emitted in addition to the electron such that the sum of the energies of the neutron and the electron is constant...
I agree that my remedy could seem incredible because one should have seen those neutrons very earlier if they really exist. But only the one who dare can win and the difficult situation, due to the continuous structure of the beta spectrum, is lighted by a remark of my honoured predecessor, Mr Debye, who told me recently in Bruxelles: "Oh, It's well better not to think to this at all, like new taxes". From now on, every solution to the issue must be discussed. Thus, dear radioactive people, look and judge.
Unfortunately, I cannot appear in Tubingen personally since I am indispensable here in Zurich because of a ball on the night of 6/7 December. With my best regards to you, and also to Mr Back.
Your humble servant
. W. Pauli
Neutrinos: the birth of the idea
1930
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Neutrinos a glitch
1932
Chadwick discovered the neutron, but neutrons are heavy and do not correspond to the particle imagined by Pauli.
Pauli responds …. J Chadwick
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1933Neutrinos
Pauli responds at Solvang, in October 1933
“... their mass can not be very much more than the electron mass. In order to distinguish them from heavy neutrons, mister Fermi has proposed to name them "neutrinos". It is possible that the proper mass of neutrinos be zero... It seems to me plausible that neutrinos have a spin 1/2... We know nothing about the interaction of neutrinos with the other particles of matter and with photons: the hypothesis that they have a magnetic moment seems to me not founded at all." E Fermi
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1916Gravitational Wavesthe birth of the idea
Newton’s Theory“instantaneous action at a
distance”
Einstein’s Theoryinformation carried
by gravitational radiation at the speed
of light
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Gravitational Wavesa glitch
Early claims of gravitational wave detection were not confirmed.
J. Weber
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Developing the Theoryrefining the predictions"Since I first embarked on my
study of general relativity, gravitational collapse has been for me the most compelling implication of the theory - indeed the most compelling idea in all of physics . . . It teaches us that space can be crumpled like a piece of paper into an infinitesimal dot, that time can be extinguished like a blown-out flame, and that the laws of physics that we regard as 'sacred,' as immutable, are anything but.”
– John A. Wheeler in Geons, Black Holes and Quantum Foam
John Wheeler
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Neutrinosdirect detection 1953
Reines and CowanThe target is made of about 400 liters of water mixed with cadmium chloride
The anti-neutrino coming from the nuclear reactor interacts with a proton of the target, giving a positron and a neutron. The positron annihilates with an electron of target and gives two simultaneous photons. The neutron slows down before being eventually captured by a cadmium nucleus, that gives the emission of photonsabout one 15 microseconds after those of the positron. All those photons are detected and the 15 microseconds identify the "neutrino" interaction.
Fred Reines
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“Indirect”evidence
for gravitational waves
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Direct Detectionstill waiting …..
Detectors in space
LISA
Gravitational Wave Astrophysical Source
Terrestrial detectorsLIGO, TAMA, Virgo, AIGO
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The Birth of a FieldThe evolving ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physics
Reines-Cowandirect ν detection
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The Birth of a FieldThe evolving ‘roadmap’ for gravitational-wave astrophysics
GW Observed
GW Properties ImprovedSensitivity
astrophysicsphysics
LIGO et al (soon ??)direct grav. wave detection
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Neutrinos the properties 1960
In 1960, Lee and Yang are realized that if a reaction like
µ- → e- + γ
is not observed, this is because two types of neutrinos exist νµ and νe
Lee and Yang
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Neutrinos Beams1960
Mel Schwartz realized the possibility to produce an intense neutrino beam from the decay of pions, that are particles produced from the collision of a proton beam produced in accelerators
P + N → Nucleons +nπ’s
π → µ + νMel Schwartz
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Two Neutrinos
1962
Schwartz Lederman SteinbergerAGS Proton Beam
Neutrinos fromµ-decay onlyproduce muons (not electrons) when they interact in matter
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Neutrinos the modern era 1970’s
High energy neutrino beams at CERN and Fermilab
15 footBubble Chamber
At Fermilab
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Neutrino Physicsweak neutral current
Gargamelle Bubble ChamberCERN
First evidence for weak neutral current
νµ + e → νµ + e
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Neutrino Physicsneutrino scattering CCFR – Fermilab
νµ + N → µ + X
• Quark Structure• QCD
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Neutrino Astrophysicssolar neutrinos
Solar Neutrino Detection600 tons of chlorine.
• Detected neutrinos of energy > 1 MeV
• Detection verifies fusion process in the sun
• The rate of solar neutrinos detected is three times less than predicted
Ray DavisHomestake Detector
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The Development of the FieldThe evolving ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physics
solar ν’s
weak neutral currentquark structure
QCD
νµ & νeSchwartz-BNLHE CERN/Fermilab
Reines-Cowandirect ν detection
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gamma ray b
urst
Properties of Gravitational Waves
If gamma ray burst (GRB) and gravitational waves arrive at same time to within ~ 1 sec
Then, speeds are the same to ~1 second / 2 billion yrs
~1 part in 1017
The Speed
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Properties of Gravitational Waves
The Polarizationof Gravitational Waves
gµν = ηµν + hµν (r r , t)
h+ = ε+ h ei(r k ⋅
r r −ωt )
h× = ε× h e i(r k ⋅
r r −ωt )
TAMA 300
LIGO
LIGO
GEO 600
Virgo
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Advanced LIGOimproved subsystems
Active Seismic
Multiple SuspensionsSapphire Optics
Higher Power Laser
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Advanced LIGOCubic Law for “Window” on the Universe
Initial LIGO
Advanced LIGO
Improve amplitude sensitivity by a factor of 10x…
…number of sources goes up 1000x! Virgo cluster
Today
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Event Localization With a Network
LIGO+VIRGO+GEO Transient Event Localization LIGO+VIRGO+GEO+TAMA Transient Event Localization
LIGO Transient Event Localization LIGO+VIRGO Transient Event Localization
SOURCE SOURCE
SOURCE SOURCE
LIGOLivingston
LIGOHanford
TAMA GEO
VIRGO
θ∆L = δt
/c
cosθ = δt / (c D12)∆θ ~ 0.5 deg
1 2
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Advanced LIGO2007 +
Enhanced Systems• laser• suspension• seismic isolation• test mass
RateImprovement
~ 104
+narrow band
optical configuration
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The Development of a FieldThe evolving ‘roadmap’ for gravitational-wave astrophysics
GW Observed
GW Properties ImprovedSensitivity
astrophysicsphysics
Binary InspiralPulsars
StrongField GR
GW NetworksAdv Detectors
SpeedPolarization
LIGO et al (soon ??)direct grav. wave detection
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ν Oscillation Probability
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ν Oscillation Phenomena
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The Status of the FieldThe evolving ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physics
solar ν’srate?
weak neutral currentquark structure
QCD
νµ & νe
3 ν typesν oscillations
Schwartz-BNLHE CERN/Fermilab
Reines-Cowandirect ν detection
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Roadmap for the Futureof Two Fields
Neutrino Physicsand Astronomy
Gravitational WaveAstronomy
High Energy Neutrino Astonomy LISA – Low Frequency Grav Waves
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Goals: Dirac or Majorana particle?
Majorana : The neutrino is its own antiparticle
Ettore Majorana
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Acceleratorsneutrino factory – neutrinos from muon collider
muon collider
Example7400 km baseline
Fermilab → Gran Sasso“world project”
neutrino beamsselect νµ’s or anti νµ’s
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Future Long Term Goals for the FieldThe future ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physics
Dirac vs Majorana
ν osc parametersCP violation
Neutrino Factories
Superbeams
the long term
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Future Long Term Goals for the FieldThe future ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physicsWIMPDark matter
cosmic rays
High energySolarSupernovaeGRBs
Dirac vs Majorana
ν osc parameters
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Future Long term Goals for the FieldThe evolving ‘roadmap’ for gravitational-wave astrophysics
GW Observed
GW Properties ImprovedSensitivity
astrophysicsphysics
New Phenomena
New Physics
SpeedPolarization ?????????
LIGO et al (soon ??)direct grav. wave detection
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Multi-messenger Astronomysupernova
neutrinos
gravitational waves
electromagnetic radiation
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Emerging Detector Technologies
• Cryogenic suspensions (LCGT Japan)• Broadband (white light) interferometers
(Hannover, UF)• All-reflective interferometers (Stanford)• Reshaped laser beam profiles (Caltech)• Quantum non-demolition
– Evade measurement back-action by measuring of an observable that does not effect a later measurement
• Speed meters (Caltech, Moscow, ANU)• Optical bars (Moscow)
– Correlations between the SN and RPN quadratures
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Sub-quantum-limited interferometer
101
102
103
104
10−24
10−23
10−22
10−21
f (Hz)
h(f)
(1/
Hz1/
2 )
Standard config.Broadband config. with squeezingBroadband config. without squeezing
Quantum correlations(Buonanno and Chen)
X+
X−
Input squeezing
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Ultimate Goal for the FieldThe future ‘roadmap’ for neutrino physics
ν interactions
ν properties ν beams
astrophysicsparticle physicsQCDWIMPS
High energySolarSupernovaeGRBs
Dirac vs Majorana
ν osc parameters
ν cosmology
relic ν’s
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Ultimate Goal for the FieldThe evolving ‘roadmap’ for gravitational-wave astrophysics
GW Observed
GW Properties ImprovedSensitivity
astrophysicsphysics
?????????
New Phenomena
New Physics
SpeedPolarization
gw cosmology
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Neutrino Signals from the Early Universe
Cosmic microwave background
• Neutrinos decoupled just prior to big bang nucleosynthesis, when the age of the universe was around 1s and the temperature around 1 MeV. • Their momentum distribution subsequently redshifted to an effective temperature Tν ~ 1.9 K, and they have an average density of ~ 300/cm3. • The direct detection of such low-energy neutrinos remains an ultimate challenge.
the ultimate goal
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Gravitational Waves from the Early Universe
Cosmic microwave background
the ultimate goal
Maybe a Special New ExperimantA. Vecchio
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Ultimate GW Stochastic Probes
-6 -5 -4 -3 -2 -1 0 1 2 3 log f
log Omega(f)
-11
-12
-13
-14
-15
-16
LISA sensitivity limit (1yr)
3rd generation sensitivity limit (1yr)
WD-WD
NS-NS
BH-MBH
NS
?CLEAN
CORRUPTED
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Future experiments in the “gap” (?)
Unresolved Binaries
MBH-MBHcoalescences
LISA
LISA II
LIGOSN
NS
10-18
10-20
10-26
10-24
10-22
10-3 10-1 101 10310-7 10-5
Frequency [Hz]
h
Sun
Earth
60°
50 000 km
90°
90°
A. Vecchio
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Imagining the FutureReaching our Goals
The morale of my story: “Comparing roadmaps for neutrinos & gravitational waves
The key to the future will be investing enough resourcesin technological development and new detectors