Observation of Low-Lying Isomeric States in 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Cs</mml:mi></mml:mrow><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>136</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math>
: A New Avenue for Dark Matter and Solar Neutrino Detection in Xenon Detectors

Haselschwardt, S. J.; Lenardo, B. G.; Daniels, T.; Finch, S. W.; Friesen, F. Q. L.; Howell, C. R.; Malone, C. R.; Mancil, E.; Tornow, W.

doi:10.1103/physrevlett.131.052502

Cited by 6 publications

(2 citation statements)

References 45 publications

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“…The signal generated in the detector is the combination of the outgoing electron and any γ rays or conversion electrons emitted as the Cs nucleus relaxes to its ground state. Recently, many new low-lying states in 136 Cs have been identified, several of which are isomeric and potentially can be used in filtering events [60]. As the reaction threshold Q of 136 Xe is low enough (lowest among all naturally occurring isotope of xenon), this reaction can be used to search for neutrinos from the solar carbon-nitrogen-oxygen (CNO) cycle [61,62], and can also provide a unique measurement of 7 Be neutrinos, which may enable novel measurements of temperature of the solar core With the mass excess of 136 Cs from our measurements combined with the mass value of 136 Xe measured at FSU Penning trap [33,52,64], we refined the Q value to be 79.1 (5) keV.…”

Section: Resultsmentioning

confidence: 99%

β− decay Q -value measurement of Cs136 and its implications for neutrino studies

Ge,

Eronen,

de Roubin

et al. 2023

Phys. Rev. C

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The β − decay Q value of 136 Cs (J π = 5 + , t 1/2 ≈ 13 d) was measured with the JYFLTRAP Penning trap setup at the Ion Guide Isotope Separator On-Line facility of the University of Jyväskylä, Finland. The monoisotopic samples required in the measurements were prepared with a new scheme utilized for the cleaning, based on the coupling of dipolar excitation with Ramsey's method of time-separated oscillatory fields and the phase-imaging ion-cyclotron-resonance technique. The Q value is determined to be 2536.83(45) keV, which is ≈4 times more precise and 11.4(20) keV (≈6σ ) smaller than the adopted value in the most recent Atomic Mass Evaluation AME2020. The daughter, 136 Ba, has a 4 + state at 2544.481(24) keV and a 3 − state at 2532.653(23) keV, both of which can potentially be ultralow Q-value end states for the 136 Cs decay. With our new ground-to-ground state Q value, the decay energies to these two states become −7.65(45) keV and 4.18(45) keV, respectively. The former is confirmed to be negative at the level of ≈17σ , which verifies that this transition is not a suitable candidate for neutrino mass determination. On the other hand, the slightly negative Q value makes this transition an interesting candidate for the study of virtual β-γ transitions. The decay to the 3 − state is validated to have a positive low Q value which makes it a viable candidate for neutrino mass determination. For this transition, we obtained a shell-model-based half-life estimate of 2.1 +1.6 −0.8 × 10 12 yr. Furthermore, the newly determined low reaction threshold of 79.08(54) keV for the charged-current ν e + 136 Xe (0 + ) → 136 Cs * + e − neutrino capture process is used to update the cross sections for a set of neutrino energies relevant to solar 7 Be, pep, and CNO neutrinos. Based on our shell-model calculations, the new lower threshold shows event rates of 2-4 percent higher than the old threshold for several final states reached by the different species of solar neutrinos.

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Section: Resultsmentioning

confidence: 99%

β− decay Q -value measurement of Cs136 and its implications for neutrino studies

Ge,

Eronen,

de Roubin

et al. 2023

Phys. Rev. C

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“…𝜈 e (or dark matter : 𝜒) + 136 Xe → e − + 136 Cs * (XeCC) is an available reaction channel at xenonbased experiments whose observables are recoil electrons and de-excitation 𝛾-rays from the excited state of 136 Cs [1]. Recentry, the low-lying isomeric states in 136 Cs * with lifetimes on the order of 100 ns were observed [2,3]. Therefore, one can conduct delayed-coincidence tagging of multiple time-correlated de-excitation 𝛾-rays using a ns-response detector like liquid scintillator.…”

Section: Introductionmentioning

confidence: 99%

A New Method for Detecting Charged-Current Neutrino Interactions on $^{136}$Xe in KamLAND-Zen: Implications for Solar Neutrino Measurements and Fermionic Dark Matter Searches

Tachibana

2024

Proceedings of XVIII International Conference on Topics in Astroparticle and Underground Physics — PoS(TAUP2023)

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A 136 Xe nuclei capture electron neutrinos through charged-current (CC) interaction. This lead to an excited state of 136 Cs : 𝜈 e + 136 Xe → e − + 136 Cs (1 + ). This reaction can be used for low energy solar neutrino measurements and MeV scale mass fermionic dark matter searches. The recent observation of low-lying isomeric states in 136 Cs with lifetimes on the order of 100 ns implies that the CC interaction can be identified by a delayed-coincidence measurement in liquid scintillator detector. This technique involves detecting a prompt signal conposed of the electron and most of the de-excitation 𝛾-rays, followed by a delayed signal consisting of the remaining de-excitation 𝛾-rays with energies below 140 keV. KamLAND-Zen is an experiment designed to search for neutrinoless double-beta decay of 136 Xe. KamLAND-Zen uses organic liquid scintillators dissolving 750 kg of xenon (91% enriched in 136 Xe) and has the world's largest exposure to the CC reaction. We conducted a feasibility study of identifying the CC interaction in KamLAND-Zen.

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Supernova electron-neutrino interactions with xenon in the nEXO detector

Hedges,

Al Kharusi,

Angelico

et al. 2024

Phys. Rev. D

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Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-β decay detector (∼5 metric ton, 90% Xe136, 10% Xe134) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement between MARLEY’s predictions and existing theoretical calculations of the inclusive cross sections at supernova neutrino energies. The interactions modeled by MARLEY were simulated within the nEXO simulation framework and were run through an example reconstruction algorithm to determine the detector’s efficiency for reconstructing these events. The simulated data, incorporating the detector response, were used to study the ability of nEXO to reconstruct the incident electron-neutrino spectrum and these results were extended to a larger xenon detector of the same isotope enrichment. We estimate that nEXO will be able to observe electron-neutrino interactions with xenon from supernovae as far as 5–8 kpc from Earth, while the ability to reconstruct incident electron-neutrino spectrum parameters from observed interactions in nEXO is limited to closer supernovae. Published by the American Physical Society 2024

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Observation of Low-Lying Isomeric States in Cs136 : A New Avenue for Dark Matter and Solar Neutrino Detection in Xenon Detectors

Cited by 6 publications

References 45 publications

β− decay Q -value measurement of Cs136 and its implications for neutrino studies

β− decay Q -value measurement of Cs136 and its implications for neutrino studies

A New Method for Detecting Charged-Current Neutrino Interactions on $^{136}$Xe in KamLAND-Zen: Implications for Solar Neutrino Measurements and Fermionic Dark Matter Searches

Supernova electron-neutrino interactions with xenon in the nEXO detector

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