Relic Neutrinos (and other Holy Grails) Institute for Nuclear Theory February 2010 J. A. Formaggio MIT
New New Frontiers Connections • With the launch of the Planck satellite, the connection between neutrino physics and cosmology becomes even stronger. • A strong verification of the existence of the relic neutrino background (via direct detection) may provide strong validation of our current cosmological model(s), • Can direct detection of relic neutrinos be accomplished?
The Triumph of Cosmology Microwave Background 400 kyr z =1100 Nucleosynthesis • The combination of the standard model 3-30 min of particle physics and general relativity z = 5 × 10 8 allows us to relate events taking place at different epochs together. Relic Neutrinos 0.18 s • Observation of the cosmological z = 1 × 10 10 neutrinos would then provide a window into the 1 st second of creation
Signal Properties 1 f i ( p, T ) = Ei ( p ) − µi +1 e T • Cosmological neutrinos (or the C ν B) are inherently connected to the photon microwave background. However, there are significant differences between the two. Bose-Einstein Fermi-Dirac ( γ ‘s) ( ν ‘s) • Some characteristics: Temperature 2.725 K 1.945 K (Now) ζ { 3 } ζ { 3 } 3 Number • The C ν B temperature is related to the π 2 gT 3 π 2 gT 3 density photon temperature (including reheating). γ ν 4 π 2 π 2 7 Energy 30 gT 4 30 gT 4 Density γ ν 8 • The C ν B is inherently a gas of spin 1/2 particles: obey Fermi-Dirac statistics rather than Bose-Einstein). From CMB, the neutrino density is ~110 ν ’s/cm 3 per flavor. • The C ν B density is predicted directly from the photon density. (neutrino and anti-neutrino)
Local Enhancement • Because neutrinos have a small (but non-zero) mass, they feel the force of gravity and are thereby affected by it. • Given the present-day cosmological neutrinos are non-relativistic, one could expect a local enhancement of the density of neutrinos in our galaxy.
We have a good track record... Neutrinos from supernovae. Neutrinos from reactors. Detected (1980s) Detected (1950s) Neutrinos from the Earth. Neutrinos from the sun. Detected (2000s) Detected (1960s) Neutrinos from the atmosphere. Neutrinos from galactic sources. Detected (1960s) Not yet (but close!) Neutrinos from accelerators. Neutrinos from the Big Bang. Created & detected (1960s) Not even close...
Why is it so hard??? • Cosmological neutrinos comprise the most intense natural source of neutrinos available to us from nature. • The cosmological photon background has been measured incredibly well. The noise from the early big bang still rings today. So?? What’s the problem?!
Why is it so hard? • Actually, the problem is THRESHOLD. “Choice. The problem is choice.” • Consider, for example, ordinary inverse beta decay. ν e + p → e + + n ¯ E ν + m p ≥ m e + m n • Since energy is conserved, you need the neutrino to have enough energy • But here the kinetic energy from relics to initiate the process. is very small. • For most nuclei, you just do not < K > = 6 . 5 T 2 ν /m ν or 3 . 15 T ν have enough energy. You need a threshold-less process.
Some quotes.... “About every neutrino physicist goes through a phase in his or her career and asks ‘There’s got to be a way to measure the relic neutrino background...’” P. Fisher
Coherent Scattering k 2 • Consider the scattering of a σ = G 2 F m 2 L (scattering) macroscopic object against the neutrino wind . ν π • This wind is actually the motion of the earth with respect to the neutrinos (similar to moving through a dark matter halo). • Consider the coherent scattering of d � p neutrinos against an object (spheres) (mom. trans. ) dt = F ν σ ∆ p and look at the force imposed by the neutrino wind.
Coherent Elastic Scattering • Effect takes advantage of a macroscopic de Broglie wavelength (for these momenta). • Equivalent to measuring a small Eot-Wash acceleration on a macroscopic object. Pendulum • Currently can measure accelerations down to 10 -13 cm/s 2 . Can push this down to 10 -23 cm/s 2 in the future. a t ≃ (10 − 46 − 10 − 54 ) A 100 cm s − 2
ULHC??? High Energy Scattering : Beams • Take advantage of cross-section growth with energy, using very high energy isotopes as probes. • Two possible sources: high energy accelerators & cosmic rays. • Most parameters necessary for relic neutrino detection beyond scope of conventional machines. A 2 R ν = 2 × 10 − 9 · m ν E n L I A[yr − 1 ] eV 10TeV km Z
= m 2 High Energy E res Z ν 2 m ν Scattering : Cosmic Rays • Conversely, one can use cosmic rays as the high energy source. • One can look at absorption of extremely high energy neutrinos near the Z- resonance, or for emission features above the natural GZK cutoff. Resonance Dips Z-bursts
Neutrino Capture 3 H ➟ 3 He + + e - + ν e Instead of beta decay...
Neutrino Capture 3 H ➟ 3 He + + e - + ν e 3 H + ν e ➟ 3 He + + e - References ...look for neutrino A. Cocco, G. Mangano, and M. Messina, hep-ph/0703075 (2007). capture S. Weinberg, Phys. Rev. 128, 1457 (1962). T. W. Donnell and J. D. Walecka, Ann. Rev. Nucl. Sci. 25, 329 (1975). The process is energetically allowed even at zero momentum. This threshold-less reaction allows for relic neutrino detection
Detecting the Impossible... • The rate is determined by the neutrino density σ ν · v · f ( p ν )( dp � 2 π ) 3 λ ν = in our galaxy ( n ν ) and the cross-section for the process to occur. Neutrino Capture Rate σ ν · v c = (7 . 84 ± 0 . 03) × 10 − 45 cm 2 • Cross-section can be calculated from the Tritium Cross-Section ordinary beta-decay matrix elements. • Because neutrino temperature is small (1.9 K), the energy distribution is also narrow and near 2m ν zero. • This results in a unique signature: a mono- energetic electron removed from the endpoint energy of beta decay.
The Targets • The half-life of the beta-decay isotope essentially determines the rate at which the neutrino capture reaction occurs. • Rate (for nominal neutrino density) can therefore be computed. • Tritium emerges as the one isotope adaptable for relic neutrino detection. Bottom Line: 100 g of 3 H provides ~10 events/year
Intense Tritium Sources KATRIN: ~100 μ g (target) ITER: Exit Signs: ~3 kg (initial) ~1 μ g Intense tritium sources (order ~100 g) are obtainable
The Need for Resolution... • Resolution is a key ingredient in the tagging of this process. • As in neutrinoless double beta decay, one must separate the (more abundant) beta decay rate from the (rare) neutrino capture signal. R. Lazauskas, P. Vogel, C. Volpe arXiv:0710.5312 • The only separation stems from the energy difference (i.e. 2m ν ). In general, we want Δ ≤ m ν • Even if achieved, the background in the signal region must be < 1 event/year.
Some More Quotes.... “About every neutrino physicist goes through a phase in his or her career and asks ‘There’s got to be a way to measure the relic neutrino background...’” P. Fisher “... In all fairness, this method [neutrino capture] appears to have survived the longest.” P. Fisher “Anyone who can measure relic neutrinos via neutrino capture will have made an amazing neutrino mass measurement...” G. Drexlin “If it were easy, we’d be done by now...” my translation
• The KATRIN experiment uses magnetic The KATRIN Experiment adiabatic collimation with electrostatic filtering to achieve its energy resolution. • Target activity is approximately 4.7 Ci. Energy resolution from spectrometer is 0.93 eV. Detector T 2 Source Spectrometer
KATRIN = Liouville’s • Electrons from tritium decay need to Theorem + Jackson problem overcome a known potential Φ in order to be counted to the detector. Measures an integrated spectrum. • Problem: decays are isotropic, but filter acts on cos( θ ). • Solution: adiabatically rearrange their phase space. Detector Spectrometer T 2 Source
KATRIN = Liouville’s Δ x is the Theorem + Jackson problem size of the vacuum tank Source area ΔθΔ x determines amount of T 2 Δθ determines the energy x x resolution x x θ θ θ θ Detector Spectrometer T 2 Source
Can KATRIN be Scaled? Source Strength Size Final States There are three main obstacles for improving KATRIN to a better neutrino mass or relic neutrino measurement:
Scaling KATRIN: • Therefore, scaling the source strength requires Source Strength either scaling the area of the source or its column density ( ρ d). • Here, the source and the detector are distinct. • Increasing the column density does not help in For a fixed resolution, the luminosity of this case, since inelastic cross-section limits the KATRIN is dictated by the flux of opacity of the source. electrons created from the source. Minimum Ratio of effective versus energy loss free column density T 2 elastic scattering
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