The ESSnuSB Design Study: Overview and Future Prospects
<p>Dependence of <math display="inline"><semantics><msubsup><mi mathvariant="script">A</mi><mi>CP</mi><mrow><mi>μ</mi><mo>→</mo><mi>e</mi></mrow></msubsup></semantics></math> on ratio <math display="inline"><semantics><mrow><mi>L</mi><mo>/</mo><mi>E</mi></mrow></semantics></math>. The first maximum of the CPV amplitude is situated at L/E ≈ 585 km/GeV and the second at L/E ≈ 1534 km/GeV.</p> "> Figure 2
<p><math display="inline"><semantics><mrow><msub><mi>ν</mi><mi>μ</mi></msub><mo>→</mo><msub><mi>ν</mi><mi>e</mi></msub></mrow></semantics></math> and <math display="inline"><semantics><mrow><msub><mover><mi>ν</mi><mo>¯</mo></mover><mi>μ</mi></msub><mo>→</mo><msub><mover><mi>ν</mi><mo>¯</mo></mover><mi>e</mi></msub></mrow></semantics></math> oscillation probabilities as a function of neutrino energy at the fixed distance of 360 km. The oscillation probabilities are shown for <math display="inline"><semantics><mrow><msub><mi>δ</mi><mi>CP</mi></msub><mo>=</mo><mn>0</mn></mrow></semantics></math> and <math display="inline"><semantics><mrow><msub><mi>δ</mi><mi>CP</mi></msub><mo>=</mo><mo>−</mo><mi>π</mi><mo>/</mo><mn>2</mn></mrow></semantics></math>. Full lines correspond to oscillations in vacuum and dashed lines to oscillations in matter.</p> "> Figure 3
<p>Layout of the ESS accelerator including ESSnuSB modifications required for neutrino beam production and detection. The proposed modifications are show in color: the transfer line (blue), the accumulatior ring (red), the swithcyard (indigo), the neutrino target station (green), and the near detector hall (purple). Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 4
<p>The expected neutrino flux components and their energy distribution at the 100 km distance from the source, in absence of the neutrino oscillations. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 5
<p>Schematic view of the ESSnuSB near detector hall.</p> "> Figure 6
<p>Technical drawing of a single far detector cavern. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 7
<p>The efficiency to correctly select a neutrino flavor as a function of neutrino energy. Full lines correspond to different neutrino flavors. The dashed line is the efficiency of the fiducial cut. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 8
<p>The expected number of observed neutrino events as a function of reconstructed neutrino energy in the far detectors, shown for the signal channel and the most significant background channels. Each plot corresponds to 200 days (effective year) of data taking. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 9
<p>CPV discovery potential as a function of true <math display="inline"><semantics><msub><mi>δ</mi><mi>CP</mi></msub></semantics></math> value, assuming the baseline of 360 km (Zinkgruvan mine) and run-time of 5 y in <math display="inline"><semantics><mi>ν</mi></semantics></math> mode and 5 y in <math display="inline"><semantics><mover><mi>ν</mi><mo>¯</mo></mover></semantics></math> mode. Different lines correspond to different normalization uncertainty assumptions. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 10
<p>Coverage of the <math display="inline"><semantics><msub><mi>δ</mi><mi>CP</mi></msub></semantics></math> range for which the discovery potential is larger than 5 <math display="inline"><semantics><mi>σ</mi></semantics></math> as a function of run-time, assuming equal time in neutrino mode and antineutrino mode.</p> "> Figure 11
<p>The expected 1 <math display="inline"><semantics><mi>σ</mi></semantics></math> precision for the measurement of the CPV parameter <math display="inline"><semantics><msub><mi>δ</mi><mi>CP</mi></msub></semantics></math> as a function of the true value of <math display="inline"><semantics><msub><mi>δ</mi><mi>CP</mi></msub></semantics></math>, assuming the baseline of 360 km (Zinkgruvan mine) and run-time of 5 y in <math display="inline"><semantics><mi>ν</mi></semantics></math> mode and 5 y in <math display="inline"><semantics><mover><mi>ν</mi><mo>¯</mo></mover></semantics></math> mode. Different lines correspond to different bin-to-bin uncorrelated errors. A normalization error of 5% is applied on top of the bin-to-bin error. Reprinted from [<a href="#B25-universe-09-00347" class="html-bibr">25</a>,<a href="#B26-universe-09-00347" class="html-bibr">26</a>].</p> "> Figure 12
<p>Layout of the proposed upgrades to the ESS linear accelerator, including those from ESSnuSB and ESSnuSB+. The ESSnuSB+ upgrades include a special target station, a muon storage racetrack ring (LEnuSTORM), a low-energy monitored neutrino beam (LEMNB) line, and a new near detector to be used both for LEnuSTORM and LEMNB. The ESSnuSB near detector will be used as a far detector for LEnuSTORM and LEMNB. The image has been reprinted from the ESSnuSB+ proposal.</p> ">
Abstract
:1. Introduction
2. CP Violation Measurement at the Second Oscillation Maximum
2.1. Oscillations in Vacuum
2.2. Matter Effects
2.3. Summary
3. Neutrino Beam
4. Neutrino Detectors
4.1. Near Detectors
4.2. Far Detectors
5. Physics Reach
6. Future Developments
7. Conclusions
Funding
Data Availability Statement
Conflicts of Interest
Abbreviations
CPV | Charge-parity violation |
ESS | European spallation source |
ESSnuSB | European spallation source neutrino super beam |
PMNS | Pontecorvo–Maki–Nakagawa–Sakata |
NC | Neutral current |
CC | Charged current |
QCD | Quantum chromodynamics |
QES | Quasi-elastic scattering |
RES | Resonant scattering |
DIS | Deep-inelastic scattering |
MEC | Meson-exchange current |
SFGD | Super fine-grained detector |
CH | Hydrocarbons |
PMT | Photomultiplier tube |
R&D | Research and development |
LEnuSTORM | Low-energy neutrinos from stored muons |
LEMNB | Low-energy monitored neutrino beam |
WC | Water Cherenkov |
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Alekou, A.; Baussan, E.; Bhattacharyya, A.K.; Kraljevic, N.B.; Blennow, M.; Bogomilov, M.; Bolling, B.; Bouquerel, E.; Bramati, F.; Branca, A.; et al. The ESSnuSB Design Study: Overview and Future Prospects. Universe 2023, 9, 347. https://doi.org/10.3390/universe9080347
Alekou A, Baussan E, Bhattacharyya AK, Kraljevic NB, Blennow M, Bogomilov M, Bolling B, Bouquerel E, Bramati F, Branca A, et al. The ESSnuSB Design Study: Overview and Future Prospects. Universe. 2023; 9(8):347. https://doi.org/10.3390/universe9080347
Chicago/Turabian StyleAlekou, A., E. Baussan, A. K. Bhattacharyya, N. Blaskovic Kraljevic, M. Blennow, M. Bogomilov, B. Bolling, E. Bouquerel, F. Bramati, A. Branca, and et al. 2023. "The ESSnuSB Design Study: Overview and Future Prospects" Universe 9, no. 8: 347. https://doi.org/10.3390/universe9080347