Future Prospects Future Prospects Jacob Daughh Daughhetee etee - - PowerPoint PPT Presentation
COHE COHERENT: RENT: Recent Results a Recent Results and nd Future Prospects Future Prospects Jacob Daughh Daughhetee etee Unive University rsity of of Tenn Tenness essee Underg Un dergro round nd Nuc Nuclear ear and and Par
Jacob Daughh Daughhetee etee Unive University rsity of
Tenness essee
Un Underg dergro round nd Nuc Nuclear ear and and Par Particle e Sympo Symposium Marc March h 9th
th,
, 2019 2019
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satisfied ( 𝑟 ≤ ~ 𝑆−1)
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Weak Mixing Angle
targets with differing Z/N ratios
Non-Standard Interactions
neutrino mass ordering (NMO) determinations
enhancement CEνNS rate Sterile Searches
sterile ν
Nuclear Form Factors
measurements
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Irreducible Background for Direct Detection Dark Matter Experiments Monitoring Supernova Physics
Irene Tamborra, Bernhard Müller, Lorenz Hüdepohl, Hans-Thomas Janka, and Georg Raffelt Phys. Rev. D 86, 125031 (2012)
arXiv:1707.06277
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to WIMP detector technologies make this feasible!
will have higher rate of interactions (but lower energy recoils…)
incident neutrino)
ability to discriminate nuclear recoils from other events.
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Source (SNS) is the production of a large flux of neutrons for myriad physics studies.
during bombardment from accelerated protons.
60 Hz in 400 ns FWHM bunches.
power!
n flux is approximately 4.3x107 n cm-2 s-1 at 20 m
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Form Factor = 1
Assumed Form- Factor
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5s 2s 1s
SM prediction: 173 events Best fit: 134 ± 22
No CEnNS rejected at 6.7s
decommissioned.
approximately twice the amount of POT data (~14 GWhr).
quenching factor determination; new QF analysis will reduce this considerably.
28 m from SNS target (~2 x 107 ν / s )
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butadiene (TPB) as a wavelength shifter for VUV light
rate at CENNS-10 location
Beam-related neutrons in CENNS-10
acrylic cylinder replaced with set of 3 TPB coated Teflon cylinders (22.4 kg fiducial volume).
threshold reduced to ~ 20 keVnr.
environmental gamma backgrounds.
energy calibration at lower energies.
underway; will soon be opening the box!
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AmBe Calibration
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Spectroscopic Portal program (DHS).
for CEvNS
both low energy nuclear recoils and high energy CC signals to be
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energetic neutrons.
mimicking the CEvNS signal!
be observed, but this is a potential important background for COHERENT experiments.
this process and constrain the potential contribution to CEvNS signal.
supernova observatory.
LS Cell in CsI Shielding
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dramatically larger than CENNS-10…
made easier without this uncertainty
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detector element needed.
uncertainty and resolve conflict in existing data.
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port dewar that has already been procured.
signal-to-background ratio of 3.5 per year of SNS operation.
standard interactions, sterile oscillations, DM, etc.
The expected CEvNS signal in a 14.4kg PPC germanium detector array in 1 year of SNS operation.
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Precise measurement of CEvNS will require reduction in systematic uncertainties:
CC cross-section on deuterium known with approx. 2%
heavy water Cherenkov detector to normalize SNS neutrino flux.
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NSI Searches
cross-section and recoil spectrum for several targets.
perturbations.
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scattering (CEνNS), a long-predicted Standard Model interaction.
which will allow for precision measurement of the CEνNS process.
for physics beyond the Standard Model (NSI, sterile neutrinos, dark matter).