The Nova Neutrino Experiment and Its Astrophysics Program
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Icecube Searches for Neutrinos from Dark Matter Annihilations in the Sun and Cosmic Accelerators
UNIVERSITE´ DE GENEVE` FACULTE´ DES SCIENCES Section de physique Professeur Teresa Montaruli D´epartement de physique nucl´eaireet corpusculaire IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. THESE` pr´esent´ee`ala Facult´edes sciences de l'Universit´ede Gen`eve pour obtenir le grade de Docteur `essciences, mention physique par M. Rameez de Kozhikode, Kerala (India) Th`eseN◦ 4923 GENEVE` 2016 i Declaration of Authorship I, Mohamed Rameez, declare that this thesis titled, 'IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.' and the work presented in it are my own. I confirm that: This work was done wholly or mainly while in candidature for a research degree at this University. Where any part of this thesis has previously been submitted for a degree or any other qualifica- tion at this University or any other institution, this has been clearly stated. Where I have consulted the published work of others, this is always clearly attributed. Where I have quoted from the work of others, the source is always given. With the exception of such quotations, this thesis is entirely my own work. I have acknowledged all main sources of help. Where the thesis is based on work done by myself jointly with others, I have made clear exactly what was done by others and what I have contributed myself. Signed: Date: 27 April 2016 ii UNIVERSITE´ DE GENEVE` Abstract Section de Physique D´epartement de physique nucl´eaireet corpusculaire Doctor of Philosophy IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. -
Supernova Neutrinos in the Proto-Neutron Star Cooling Phase and Nuclear Matter
TAUP 2019 IOP Publishing Journal of Physics: Conference Series 1468 (2020) 012089 doi:10.1088/1742-6596/1468/1/012089 Supernova neutrinos in the proto-neutron star cooling phase and nuclear matter Ken’ichiro Nakazato1 and Hideyuki Suzuki2 1 Faculty of Arts and Science, Kyushu University, 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan 2 Faculty of Science & Technology, Tokyo University of Science, 2641 Yamazaki, Noda, Chiba 278-8510, Japan E-mail: [email protected] Abstract. A proto-neutron star (PNS) is a newly formed compact object in a core collapse supernova. Using a series of phenomenological equations of state (EOS), we have systematically investigated the neutrino emission from the cooling phase of a PNS. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. As a result, the cooling timescale evaluated from the neutrino light curve is found to be long for the EOS models with small neutron star radius and large effective mass of nucleons. It implies that extracting properties of a PNS (such as mass and radius) and the nuclear EOS is possible by a future supernova neutrino observation. 1. Introduction Core collapse supernovae, which are the spectacular death of massive stars, emit an enormous amount of neutrinos. In the case of SN1987A, a few tens of events were actually detected [1, 2, 3] and contributed to confirm the standard scenario for supernova neutrino emission. Although the neutron star formed in SN1987A has not yet been observed, its mass estimations had been attempted by using the neutrino event number [4, 5]. -
Measurement of the + ̅ Charged Current Inclusive Cross Section
Measurement of the �! + �!̅ Charged Current Inclusive Cross Section on Argon in MicroBooNE Krishan Mistry on behalf of the MicroBooNE Collaboration 15 March 2021 New Directions in Neutrino-Nucleus Scattering (NDNN) NuSTEC Workshop ICARUS T600 MicroBooNE SBND Importance of the �!-Ar cross section • MicroBooNE + SBN Program + DUNE ⇥ Employ Liquid Argon Time Projection Chambers (LArTPCs) arXiv:1503.01520 [physics.ins-det] • Primary signal channel for these experiments is �!– Ar CC interactions arXiv:2002.03005 [hep-ex] 15 March 2021 K Mistry 2 Building a Picture of �! Interactions ArgoNeuT is the first A handful of measurements measurement made on on other nuclei in the argon hundred MeV to GeV range ⇥ Sample of 13 selected events Nuclear Physics B 133, 205 – 219 (1978) Phys. Rev. D 102, 011101(R) (2020) ⇥ Gargamelle Phys. Rev. Lett. 113, 241803 (2014) ⇥ Phys. Rev. D 91, 112010 (2015) T2K J. High Energ. Phys. 2020, 114 (2020) ⇥ MINER�A Phys. Rev. Lett. 116, 081802 (2016) !! " !! " Argon Other 15 March 2021 K Mistry 3 What are we measuring? ! /!̅ " # • Total �!+ �!̅ Charged Current (CC) ! ! $ /$ inclusive cross section • Signature: the neutrino event ? contains at least one electron-liKe shower Ar ⇥ No requirements on the presence (or absence) of any additional particle ⇥ Do not differentiate between �! and �!̅ Inclusive channel is the most straightforward channel to compare to predictions 15 March 2021 K Mistry 4 MicroBooNE • Measurement is performed • Features of a LArTPC using the MicroBooNE detector: LArTPC ⇥ Precise calorimetry ⇥ 4� -
Neutrinos from Core-Collapse Supernovae and Binary Neutron Star Mergers
Neutrinos from core-collapse supernovae and binary neutron star mergers Maria Cristina Volpe Astroparticules et Cosmologie (APC), Paris, France Sun core-collapse Supernovae McLaughlin Perego et al, 2014 accretion disks around black holes or neutron star mergers remnants Solar neutrino observations Vacuum averaged oscillations pep MSW solution 7Be 8B ν Survival Probability e Borexino, Nature 512 (2014) ν Neutrino Energy (MeV) Vacuum-averaged oscillations versus MSW suppression of high energy 8B neutrinos. Energy production of low mass main sequence stars confirmed — pp reaction chain. Future measurement of CNO neutrinos - main energy production in massive main sequence stars. The Mikheev-Smirnov-Wolfenstein effect Neutrinos interact with matter and undergo resonant adiabatic flavor conversion. Wolfenstein PRD (1978) Mikheev, Smirnov(1985) hmat = p2GF ⇢e mean-field approximation matter basis flavour basis ~ ν2 =νe ν , ν ν ν ~ ν2 µ τ e 2 ~ ν 1 =νµ ν~ 1 Effective mass Effective vacuum ν1 MSW resonance DENSITY 2 ∆m˜ /4E i✓˙M h⌫ = − − neutrino hamiltonian in the matter basis i✓˙ ∆m˜ 2/4E ✓ M ◆ ✓˙M Resonance condition : Adiabaticity : γ = | 2 | << 1 h h 0 ∆m˜ /4E ⌫,11 − ⌫,22 ⇡ Also in supernovae, in accretion disks around compact objects, in the Earth and in the Early Universe (BBN epoch) Heavy elements nucleosynthesis Two main mechanisms at the origin of elements heavier than iron : s-process (s-slow) and r-process (r-rapid). Double peak structures at the first A=90, the second A=130 and third A=190 peaks due to both the s-process and the r-process. The r-process sites : a longstanding question The r-process : neutron-capture is fast compared to half-lives of neutron-rich unstable nuclei. -
First MINOS Results from the Numi Beam Nathaniel Tagg, for the MINOS Collaboration Tufts University, 4 Colby Street, Medford, MA, USA 02155 FERMILAB-CONF-06-130-E
First MINOS Results from the NuMI Beam Nathaniel Tagg, for the MINOS Collaboration Tufts University, 4 Colby Street, Medford, MA, USA 02155 FERMILAB-CONF-06-130-E As of December 2005, the MINOS long-baseline neutrino oscillation experiment collected data with an exposure of 0.93 × 1020 protons on target. Preliminary analysis of these data reveals a result inconsistent with a no- oscillation hypothesis at level of 5.8 sigma. The data are consistent with neutrino oscillations reported by m2 . +0.60 × − 2 θ . +0.12 Super-Kamiokande and K2K, with best fit parameters of ∆ 23 = 3 05−0.55 10 3 and sin 2 23 = 0 88−0.15. 1. Introduction end of the run period in March 2006, the maximum in- tensity delivered to the target was in excess of 25 1012 × The MINOS long-baseline neutrino oscillation ex- protons per pulse, with a maximum target power of periment [1] was designed to accurately measure neu- 250 kW. trino oscillation parameters by looking for νµ disap- pearance. MINOS will improve the measurements of ∆m223 first performed by the Super-Kamiokande 3. The MINOS Detectors [2, 3] and K2K experiments [4]. In addition, MINOS is capable of searching for sub-dominant νµ νe os- The MINOS Near and Far detectors are constructed cillations, can look for CPT-violating modes→ by com- to have nearly identical composition and cross-section. paring νµ toν ¯µ oscillations, and is used to observe The detectors consist of sandwiches of 2.54 cm thick atmospheric neutrinos [5]. steel and 1 cm thick plastic scintillator, hung verti- The MINOS experiment uses a beam of νµ created cally. -
Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using Hpge Detectors
Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using HPGe Detectors Robert A. Johnson A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Washington 2010 Program Authorized to Offer Degree: Physics University of Washington Graduate School This is to certify that I have examined this copy of a doctoral dissertation by Robert A. Johnson and have found that it is complete and satisfactory in all respects, and that any and all revisions required by the final examining committee have been made. Chair of the Supervisory Committee: John F. Wilkerson Reading Committee: Steven R. Elliott Nikolai R. Tolich John F. Wilkerson Date: In presenting this dissertation in partial fulfillment of the requirements for the doctoral degree at the University of Washington, I agree that the Library shall make its copies freely available for inspection. I further agree that extensive copying of this dissertation is allowable only for scholarly purposes, consistent with “fair use” as prescribed in the U.S. Copyright Law. Requests for copying or reproduction of this dissertation may be referred to Proquest Information and Learning, 300 North Zeeb Road, Ann Arbor, MI 48106-1346, 1-800-521-0600, to whom the author has granted “the right to reproduce and sell (a) copies of the manuscript in microform and/or (b) printed copies of the manuscript made from microform.” Signature Date University of Washington Abstract Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using HPGe Detectors Robert A. Johnson Chair of the Supervisory Committee: Professor John F. -
![INO/ICAL/PHY/NOTE/2015-01 Arxiv:1505.07380 [Physics.Ins-Det]](https://docslib.b-cdn.net/cover/2862/ino-ical-phy-note-2015-01-arxiv-1505-07380-physics-ins-det-842862.webp)
INO/ICAL/PHY/NOTE/2015-01 Arxiv:1505.07380 [Physics.Ins-Det]
INO/ICAL/PHY/NOTE/2015-01 ArXiv:1505.07380 [physics.ins-det] Pramana - J Phys (2017) 88 : 79 doi:10.1007/s12043-017-1373-4 Physics Potential of the ICAL detector at the India-based Neutrino Observatory (INO) The ICAL Collaboration arXiv:1505.07380v2 [physics.ins-det] 9 May 2017 Physics Potential of ICAL at INO [The ICAL Collaboration] Shakeel Ahmed, M. Sajjad Athar, Rashid Hasan, Mohammad Salim, S. K. Singh Aligarh Muslim University, Aligarh 202001, India S. S. R. Inbanathan The American College, Madurai 625002, India Venktesh Singh, V. S. Subrahmanyam Banaras Hindu University, Varanasi 221005, India Shiba Prasad BeheraHB, Vinay B. Chandratre, Nitali DashHB, Vivek M. DatarVD, V. K. S. KashyapHB, Ajit K. Mohanty, Lalit M. Pant Bhabha Atomic Research Centre, Trombay, Mumbai 400085, India Animesh ChatterjeeAC;HB, Sandhya Choubey, Raj Gandhi, Anushree GhoshAG;HB, Deepak TiwariHB Harish Chandra Research Institute, Jhunsi, Allahabad 211019, India Ali AjmiHB, S. Uma Sankar Indian Institute of Technology Bombay, Powai, Mumbai 400076, India Prafulla Behera, Aleena Chacko, Sadiq Jafer, James Libby, K. RaveendrababuHB, K. R. Rebin Indian Institute of Technology Madras, Chennai 600036, India D. Indumathi, K. MeghnaHB, S. M. LakshmiHB, M. V. N. Murthy, Sumanta PalSP;HB, G. RajasekaranGR, Nita Sinha Institute of Mathematical Sciences, Taramani, Chennai 600113, India Sanjib Kumar Agarwalla, Amina KhatunHB Institute of Physics, Sachivalaya Marg, Bhubaneswar 751005, India Poonam Mehta Jawaharlal Nehru University, New Delhi 110067, India Vipin Bhatnagar, R. Kanishka, A. Kumar, J. S. Shahi, J. B. Singh Panjab University, Chandigarh 160014, India Monojit GhoshMG, Pomita GhoshalPG, Srubabati Goswami, Chandan GuptaHB, Sushant RautSR Physical Research Laboratory, Navrangpura, Ahmedabad 380009, India Sudeb Bhattacharya, Suvendu Bose, Ambar Ghosal, Abhik JashHB, Kamalesh Kar, Debasish Majumdar, Nayana Majumdar, Supratik Mukhopadhyay, Satyajit Saha Saha Institute of Nuclear Physics, Bidhannagar, Kolkata 700064, India B. -
MINOS+: Running the MINOS Detectors in the Numi-Nova Beam
MINOS+: Running the MINOS Detectors in the Numi-NOvA Beam (FNAL P-1016) Presented by Alexander Radovic of University College London on behalf of the MINOS Collaboration. The Proposal: The Physics Reach: By continuing to the run the MINOS detectors during the NOvA Era Not only could MINOS+ augment the sin22ϴ and Δm2 we would hope to not only help NOvA improve on its measurement measurements of NOvA, it could also represent an opportunity of the oscillation parameters but also to probe new and interesting to probe some interesting areas of new physics. Such as: areas of physics, as well as improve our understanding of the neutrino beam flux. The Study of High Energy Neutrinos. Until now most neutrino oscillation experiments have focused on the lower The diagram on the right energies where the PMNS scenario tells us oscillations will shows the approximate occur. The MINOS detectors however would see the high energy regime that the MINOS energy tail of the NOvA beam, allowing for investigation MINOS detectors will be beyond the PMNS model of oscillations. sensitive to. Clearly very different to the spectrum The Search for seen at the NOvA Sterile Neutrinos. detectors it would give a NOvA The MINOS detectors window into a completely will see a large νμ flux different physical domain. from the NOvA beam which is perfect for With the MINOS detectors searching for a sterile we have a unique neutrino with opportunity to secure 2 2 2 m 4-m 3=O(1eV ) as Fermilab's position as a it would cause the world leader in Neutrino disappearance of research. -
Upgrade of the Minos+ Experiment Data Acquisition for the High Energy Numi Beam Run
FERMILAB-CONF-14-503-ND (accepted) Upgrade of the Minos+ Experiment Data Acquisition for the High Energy NuMI Beam Run William Badgett, Steve R. Hahn, Donatella Torretta, Jerry Meier, Jeffrey Gunderson, Denise Osterholm, David Saranen Abstract–The Minos+ experiment is an extension of the Minos Minos was designed a number of years before data taking experiment at a higher energy and more intense neutrino beam, commenced; by dint of technical progress, some of the with the data collection having begun in the fall of 2013. The electronics technology involved has become obsolete. The neutrino beam is provided by the Neutrinos from the Main Minos+ experiment was approved to extend the Minos data set Injector (NuMI) beam-line at Fermi National Accelerator Laboratory (Fermilab). The detector apparatus consists of two in the Noνa [2] NuMI beam era [3] with a higher energy and main detectors, one underground at Fermilab and the other in more intense neutrino beam. Both improved beam features Soudan, Minnesota with the purpose of studying neutrino result in higher signal occupancies in the Minos detector, and oscillations at a base line of 735 km. The original data especially so at the near detector located at Fermilab. The acquisition system has been running for several years collecting near detector is situated at 371 meters from the decay pipe, data from NuMI, but with the extended run from 2013, parts of while the far detector is 735 km away. At the peak beam the system needed to be replaced due to obsolescence, reliability problems, and data throughput limitations. Specifically, we have intensities of the high-energy run, we expect twenty neutrino replaced the front-end readout controllers, event builder, and interactions at the near detector per spill of ten micro-seconds data acquisition computing and trigger processing farms with duration at the near detector, compared to a maximum of three modern, modular and reliable devices with few single points of in the run ending in 2011. -
The Minerνa Detector Construction Database
The MINERνA detector construction database Moureen Kemei Mount Holyoke College Physics Department South Hadley, MA, 01075 Supervisor: Dave J Boehnlein Particle Physics Department MINERνA Experiment Fermi National Accelerator Laboratory Batavia, IL, 60510 2009 Summer Internship in Science and Technology(SIST) Program Abstract We describe the construction database for the MINERν-A detector. MINERν- A is a low mass fully active neutrino detector that is designed to study low-energy neutrino interactions. The detector database keeps track of all detector components, illustrates the relationship between different compo- nents, simplifies future data entry and record maintenance. The database is written in Structured Query Language (MySQL). A Python graphical user interface for the detector has been developed. Contents 0.1 Introduction . 2 0.2 Background . 3 0.2.1 The NuMI Beam . 3 0.2.2 The Minerva Detector . 4 0.2.3 Event Reconstruction and Particle Identification . 7 0.3 The Construction Database . 8 0.3.1 Module Table . 9 0.3.2 Outer Detector Table . 10 0.3.3 Plane Table . 11 0.3.4 Outer Detector Channel Table . 12 0.3.5 Outer ECAL Table . 12 0.3.6 Graphical User Interface (GUI) for the database . 12 0.4 Summary and Conclusions . 13 0.5 Acknowledgements . 13 1 0.1 Introduction The Main INjector Experiment for ν-A (MINERνA) is a neutrino scattering experiment that will study low energy ν-nucleus interactions to high preci- sion. The NuMI (neutrino's from the main injector) beamline at Fermilab provides an intense ν(neutrino) beam for the MINERνA detector. Neutrinos outnumber protons, electrons and neutrons yet they are the most difficult particles to observe because they are weakly interacting, have a very small mass and possess no electric charge. -
Gigantic Japanese Detector Seeks Supernova Neutrinos Tracing the History of Exploding Stars Is a Goal of the Revamped Super-Kamiokande
NEWS IN FOCUS ASAHI SHIMBUN/GETTY Observations by the Super-Kamiokande neutrino detector have forced theorists to amend the standard model of particle physics. PHYSICS Gigantic Japanese detector seeks supernova neutrinos Tracing the history of exploding stars is a goal of the revamped Super-Kamiokande. BY DAVIDE CASTELVECCHI weight. These data will help astronomers to detector much better at distinguishing between better understand the history of supernovae different types, or ‘flavours’, of neutrino, as well leven thousand giant orange eyes in the Universe — but the neutrinos that the as their antiparticles, antineutrinos. confront the lucky few who have explosions emit have been difficult to detect. In 1987, the Kamiokande detector, Super-K’s entered the Super-Kamiokande under- “Every 2–3 seconds, a supernova goes off smaller predecessor, detected the first neutri- Eground neutrino observatory in Japan — by somewhere in the Universe, and it produces nos from a supernova. The dozen neutrinos far the largest neutrino detector of its kind in 1058 neutrinos,” says Masayuki Nakahata, came from Supernova 1987A, which occurred the world. A chance to see these light sensors who heads the Super-K, an international col- in the Large Magellanic Cloud, a small galaxy is rare because they are usually submerged in laboration led by Japan and the United States. that orbits the Milky Way. Head experimenter 50,000 tonnes of purified water. But a major With the upgrade, the detector should be able Masatoshi Koshiba shared the 2002 Nobel revamp of Super-K that was completed in to count a few of these ‘relic’ neutrinos every physics prize partly for that discovery. -
Component Study of the Numi Neutrino Beam for Noνa Experiment at Fermilab D
Proceedings of the DAE Symp. on Nucl. Phys. 58 (2013) 822 Component study of the NuMI neutrino beam for NOνA experiment at Fermilab D. Grover1,* B. Mercurio2, K. K. Maan3, S. R. Mishra2 and V. Singh1 1Department of Physics, Banaras Hindu University, Varanasi - 221005, INDIA 2Deptartment of Physics and Astronomy, University of South Carolina, Columbia, SC 229208, USA 3Department of Physics, Panjab University, Chandigarh, INDIA * email:[email protected] 1. Introduction axis beam aids in rejecting backgrounds to the The neutrino beam, NuMI, from Fermilab’s electron neutrino appearance search. Fig. 1 shows Main Injector accelerator is the most intense the effect on neutrino energy spectrum for neutrino beam in the world. The experiment NOνA progressively larger off-axis angles. On-axis, the will use this neutrino beam to study neutrino beam produces a neutrino flux peaked at 7 GeV oscillation where neutrino of a given flavor [2]. oscillates into another flavor. The oscillation is parameterized by the PMNS mixing-matrix and the mass squared differences between the three masses. Thus, there are six variables that affect neutrino oscillation: the three mixing angles θ12, θ23 and θ13, a CP-violating phase δ, and two mass-differences. The angles θ12 and θ23 have been measured to be non zero by several experiments. In 2012, the last angle, θ13, was measured at Daya Bay/Reno to be non zero to a statistical significance of 5.2σ [1]. No measurement of the CP-violating phase, δ has been made. Furthermore, whereas the absolute values of two mass square differences are known, the ordering of the masses has not been determined.