project 8: a radiofrequency approach to the neutrino mass ben monreal, uc santa barbara

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neutrino mass neutrino mass Ben Monreal, UC Santa Barbara Ben Monreal, UC Santa Barbara

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Page 1: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Project 8: a Project 8: a radiofrequency approach radiofrequency approach

to the neutrino massto the neutrino massBen Monreal, UC Santa BarbaraBen Monreal, UC Santa Barbara

Project 8: a Project 8: a radiofrequency approach radiofrequency approach

to the neutrino massto the neutrino massBen Monreal, UC Santa BarbaraBen Monreal, UC Santa Barbara

Page 2: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Project 8 collaboration

• UCSB: Ben Monreal

• MIT: Joe Formaggio, Asher Kaboth, Daniel Furse

• University of Washington: Hamish Robertson, Peter Doe, Leslie Rosenberg, Michael Miller, Gray Rybka, Brent Vandevender, Adam Cox, Michelle Leber, Laura Bodine

• NRAO: Rich BradleyBM & JF, arxiv:0904.2860, shortly in PRD

Page 3: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Neutrino massKurie, Richardson, & Paxton 1936

Page 4: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Neutrino mass

Page 5: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Liouville’s theorem

x

θ x

θ

x

θ

x

θSource area ΔθΔx

determines amount of T2

Δθ determines

energyresolution

Δx is the size of your

vacuum tank

The volume of phase space is conserved

for any system obeying T symmetry

Page 6: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Nondestructive measurement

•Maxwell’s Demon

• Stochastic cooling

Page 7: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Cyclotron motion

Pitch angle = 90

Pitch angle = 45

Page 8: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Cyclotron radiation• accelerating charge = EM

radiation

• Coherent, narrowband

• High power per electron

• Electron energy contributes to velocity v, power P, frequency ω

• Can we detect this radiation, measure v, P, ω, and determine E ± 1 eV?

Page 9: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Complications

• Frequency resolution?

•Doppler shift?

•Huge fluxes!

• Available power

Systematics?

Page 10: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Frequency• Schawlow: “Never

measure anything but frequency”

• f ∙ΔE/E ~ Δf = 1/Δt

• 1 eV energy resolution

• Δf /f = 2x10-6 (easy!)

• Δt = 20µs (hard!)

• βc∙Δt = 1400 meters

Page 11: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Radiative losses• E changes during

measurement (cyclotron radiation)

•Decay rate ΔE/Δt α B2

• Fourier limit ΔE Δt α B-1

•Prevents high-res experiment at high B

•~1 Tesla works for 0.5 eV

Page 12: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Complications

• Frequency resolution?

•Doppler shift?

•Huge fluxes!

• Available power

store > 106 cycles

Page 13: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

redshift

ω0(1-βcosθ)

blueshift

ω0(1-βcosθ)

ω0 (no shift)

Doppler shift

Page 14: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

ω0

(no shift)Multiple

small antennae

= synthetic large

antenna

Doppler shift

Page 15: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

ω0

(no shift)Multiple

small antennae

= synthetic large

antenna

Doppler shiftElectron moves in and out

of antenna sensitivit

y= periodic change in amplitude

(AM modulation)

Page 16: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

In frequency space

Frequency

ωcenter = qB/γmωside = ωcenter /(1±βcosθ)

Page 17: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Complications

• Frequency resolution?

•Doppler shift?

•Huge fluxes!

• Available power

store > 106 cycles

ω0 still obtainable

Page 18: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

The experiment

Page 19: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Endpoint signalsFrequency ROI

noDoppler

e-energy

Page 20: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Endpoint signalsFrequency ROI

withDopplere-

energy

Page 21: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Endpoint signalwith

Dopplere-energy

Frequency ROI

Page 22: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

many overlappinglow-energy electrons

many overlappinglow-energy electrons

rare high-energyelectrons

rare high-energyelectrons

100,000 tritium electrons

Page 23: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara
Page 24: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Complications

• Frequency resolution?

•Doppler shift?

•Huge fluxes!

• Available power

store > 106 cycles

ω0 still obtainable

do not fake signal in ROI

Page 25: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Power• At 1T, 18 keV electron emits 10-

15 W

• A 1-eV-resolution experiment will see this power in a 50kHz band

• noise power = 6x10-19 W/K

• noise RMS = 6x10-21 W/K

•4K experiment seems possible

how much detected?

divided amonghow many channels?

Keep an eye on signal width: many

broadening sources may appear

Page 26: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Complications

• Frequency resolution?

•Doppler shift?

•Huge fluxes!

• Available power

store > 106 cycles

ω0 still obtainable

do not fake signal in ROI

needs detailed RF design

Systematics?

Page 27: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Systematics•Magnet inhomogeneity

and drift: should respond well to source calibrations

• e-T and e-wall scattering

a)Run at low densityb)Each scattering

event shifts/broadens the cyclotron frequency

c)fiducialize?

• Full differential spectrum; no first-order correction for source strength

•No electrostatics; source is grounded

• T2 molecular final state = irreducible 0.3 eV (+/- 0.01 eV?) blurring of endpoint

Page 28: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Real-world designs

•Gray Rybka, UW: two-wire antenna

•Rich Bradley, NRAO: microwave receivers from radio astronomy

Page 29: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Alternatives• Toroidal magnetic

field?

•Magnetic bottle?

•Ramsey spectroscopy?

• Bucket spectroscopy?

Measuring frequency in one pass: Δf = Δt-1

N passes of Δt each: Δf = (Δt√N)-1

Page 30: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Bucket spectroscopy

• Shoot microwave beam (at ROI frequency) into magnet.

• Electron cyclotron in microwave field = electron bunch in synchrotron RF bucket

•Use “bucket” to grab and store ROI electrons, later accelerate to make detectable

•Decouples time constraints from detection constraints

Page 31: Project 8: a radiofrequency approach to the neutrino mass Ben Monreal, UC Santa Barbara

Conclusions

• UCSB: Ben Monreal

• MIT: Joe Formaggio, Asher Kaboth

• University of Washington: Hamish Robertson, Peter Doe, Leslie Rosenberg, Michael Miller, Gray Rybka, Brent Vandevender, Adam Cox, Michelle Leber, Laura Bodine

• NRAO: Rich BradleyBM & JF, arxiv:0904.2860, shortly in PRD