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Curriculum Vitæ Jocelyn Monroe
CURRICULUM VITÆ JOCELYN MONROE ! ADDRESS: CONTACT: Royal Holloway University of London Phone: +44 1784 443513 Department of Physics, W255 Email: [email protected] Egham, Surrey Web: http://www.pp.rhul.ac.uk/~jmonroe EDUCATION: 2006: Ph.D. (Physics) Columbia University Dissertation Title: “A Combined "µ and "e Oscillation Search at MiniBooNE,” Advisor: Prof. Michael Shaevitz 2002: M.A. (Physics) Columbia University 2002: M.Phil. (Physics) Columbia University 1999: B.A. (Astrophysics) Columbia University EMPLOYMENT: May 2013-: Professor of Physics, Royal Holloway University of London 2011-2013: Senior Lecturer, Royal Holloway University of London 2009-2014: Assistant Professor, Massachusetts Institute of Technology 2006-2009: Pappalardo Fellow, Massachusetts Institute of Technology 2000-2006: Research Assistant, Columbia University 1999-2000: Engineering Physicist, Beams Division, Fermi National Accelerator Laboratory 1997: DOE REU Summer Program, Particle Physics Division, Fermi National Accelerator Laboratory COLLABORATION MEMBERSHIPS: 2017-: DarkSide-20k Collaboration, UK P.I. (LNGS, IT), Deputy Spokesperson (2021-) 2019-: The PlomBox Project, P.I. (https://plombox.org/) 2008-: DEAP-3600 (SNOLab, Canada), Executive Board Chair (2014-15) 2006-2016: DMTPC (WIPP, USA), Spokesperson (2011-2016) 2006-2009: SNO (SNOLab, Canada) 1999-2008: MiniBooNE (FNAL, USA) 1999-2000: Neutrino Factory (FNAL, USA) AWARDS AND HONORS: 2016 Breakthrough Prize in Fundamental Physics Laureate 2012 Kavli Frontiers of Science Fellow, U.S. National Academy -
Head of the River
the brithe newsletter for keblec alumni • ik ss u e 6 6 • trinity term 2 0 1 8 • www.keble.ox.ac.uk Head of the River likely last the whole 1300m course and that the crucial bump might occur even later in the week. However, nothing could have been further from the truth; we gained on Christ Church from the outset and bumped in an unprecedented distance about halfway down the course. The rest of the week was nothing but smooth open water, holding off Christ Church, then Oriel. Headship was ours. This historic achievement for the College was celebrated by carrying Mr Mac (a boat with significant history at Keble) through town past the College. I was held aloft, riding the boat, crowds surging and chanting out Keble’s victory. The most surreal experience of my athletic career, and what a way to finish! Ana Arce Ana Arce Michael Hobley Sitting on the bunglines at the start of Summer Eights was pure anticipation. 2014 Engineering Science KCBC President and M1 Cox I was silent – waiting for the cannon to go, to be slammed into the back of the coxing seat by eight athletes. We were working towards the goal of Top left: Keble M1. Bottom right: Headship. For the first time in 41 years, we were going to achieve it. Michael Hobley celebrating with KCBC. A unique aspect of ‘bumps rowing’, a style This year, the athletes had a wide range of of racing primarily conducted at Oxbridge, histories, both at KCBC and in the broader is the importance of previous crews. -
Monday 22 June
Monday 22 June 7:00 AM US CDT Opening 7:00 AM 10 Welcome Steve Brice Fermilab 7:10 AM 5 Update on IUPAP neutrino panel Nigel Smith SNOLab 7:15 AM 5 The Snowmass process for neutrinos Kate Scholberg Duke University 7:20 AM 35+5 Neutrinos in the era of multi-messenger astronomy Francis Halzen University of Wisconsin, Madison 8:00 AM US CDT 10 Break 8:10 AM 25+5 A review of progress in R&D for neutrino detectors David Nygren University of Texas, Arlington 8:40 AM 17+3 Neutrino oscillation measurements with IceCube Summer Blot DESY/Zeuthen 9:00 AM US CDT 10 Break 9:10 AM US CDT Direct Neutrino Mass Measurements 9:10 AM 17+3 Mass meaurements with Ho-163 Maurits Haverkort University of Heidelberg 9:30 AM 20+5 Project 8 Noah Oblath Pacific Northwest National Laboratory 9:55 AM 20+5 KATRIN: first results and future perspectives Susanne Mertens Technical University Munich and Max Planck Institute for Physics 10:20 AM US CDT 10 Break 10:30 AM 60 Poster Session 11:30 AM US CDT End of Day Tuesday 23 June 7:00 AM US CDT Neutrino Interactions 7:00 AM 25+5 Historical Review and Future program of neutrino cross section measurements and calculations Noemi Rocco Argonne National Laboratory and Fermilab 7:30 AM 17+3 Connections between neutrino and electron scattering Adi Ashkenazi MIT 7:50 AM US CDT 10 Break 8:00 AM 20+5 The Neutrino's View of the Nucleus: New Results from MINERvA Deepika Jena Fermilab 8:25 AM 20+5 Neutrino Interaction Measurements on Argon Kirsty Duffy Fermilab 8:50 AM 20+5 Cross-section measurements with NOvA Linda Cremonesi University -
Understanding the Universe from Deep Underground
Understanding the Universe from Deep Underground Sudbury Neutrino Observatory Art McDonald, Professor Emeritus Queen’s University, Kingston, Ontario, Canada With our laboratory deep underground we have created a very low radioactivity location where we study some of the most basic scientific questions: • How do stars like our Sun burn and create the elements from which we are made? • What are the basic Laws of Physics for the smallest fundamental particles? • What is the composition of our Universe and how has it evolved to the present ? How do you make measurements that can provide answers to enormous questions like these? Answers: 1: Measure elusive particles called NEUTRINOS that come from the deepest reaches of the Sun where the energy is generated and from cosmic rays interacting in the atmosphere. 2: Measure fundamental particles (DARK MATTER) that are left over from the original formation of the Universe. 3. Measure rare forms of radioactivity (DOUBLE BETA DECAY) that can tell us more about fundamental laws of physics. Neutrinos from the Sun The middle of the sun is so hot that the centers of the atoms (nuclei) fuse together, giving off lots of energy and neutrinos. The neutrinos penetrate easily through the dense material in the Sun and reach the earth. Neutrino facts: • Neutrinos, along with electrons and quarks, are basic particles of nature that we do not know how to sub-divide further. • Neutrinos come in three “flavours” (electron, mu, tau) as described in The Standard Model of Elementary Particles, a fundamental theory of microscopic particle physics. •They only stop if they hit the nucleus of an atom or an electron head-on and can pass through a million billion kilometers of lead without stopping. -
Jocelyn Monroe
CURRICULUM VITÆ JOCELYN MONROE ADDRESS: CONTACT: Massachusetts Institute of Technology Phone: (617) 253 2332 77 Massachusetts Avenue, 26-561 Email: [email protected] Cambridge, MA 02139 Web: http://molasses.lns.mit.edu/jocelyn EDUCATION: 2006: Ph.D. (Physics) Columbia University Dissertation Title: “A Combined νµ and νe Oscillation Search at MiniBooNE,” Advisor: Prof. Michael Shaevitz 2002: M.A. (Physics) Columbia University 2002: M.Phil. (Physics) Columbia University 1999: B.A. (Astrophysics) Columbia University EMPLOYMENT: July 2009-: Assistant Professor, Massachusetts Institute of Technology 2006-2009: Pappalardo Fellow, Massachusetts Institute of Technology 2000-2006: Research Assistant, Columbia University 1999-2000: Engineering Physicist, Beams Division, Fermi National Accelerator Laboratory 1997: DOE REU Summer Program, Particle Physics Division, Fermi National Accelerator Laboratory COLLABORATION MEMBERSHIPS: 2008-: CLEAN/DEAP Collaboration (SNOLab, Canada) 2006-: DMTPC Collaboration (MIT, USA) 2006-: SNO Collaboration (SNOLab, Canada) 1999-: MiniBooNE Collaboration (FNAL, USA) 1999-2000: Neutrino Factory Collaboration (FNAL, USA) COMMITTEES: SNO Physics Interpretation Review Committee Chair (2006-present) SNO Low Energy Threshold Analysis Review Committee Member (2006-2009) Conference Organizer, 2nd CYGNUS Directional Dark Matter Workshop (2009) SNO Collaboration Executive Board Junior Member (2007-2008) Conference Organizer, 5th International Workshop on Neutrino Factories (2003) Jocelyn Monroe 1 of 11 OUTREACH: 2009 MIT Physics -
Recent Progress from the DEAP-3600 Dark Matter Direct Detection Experiment
Recent Progress from the DEAP-3600 Dark Matter Direct Detection Experiment Jocelyn Monroe, Royal Holloway University of London IPA2014 August 22, 2014 Outline 1. DEAP-3600 Detector 2. Experimental Technique 3. Status and Outlook RHUL Jocelyn Monroe December 12, 2012 The Low-Background Frontier: Status of SI Searches 1 event/ kg/day 1 event/ 100kg/day 1 event/ 100 kg/ 100 days RHUL Jocelyn Monroe August 22, 2014 The Low-Background Frontier: Status of SI Searches 1 event/ kg/day 1 event/ 100kg/day 1 event/ 100 kg/ 100 days Scalability of Detector Technology Scalability of Detector RHUL Jocelyn Monroe August 22, 2014 The Low-Background Frontier: Status of SI Searches 1 event/ kg/day 1 event/ 100kg/day 1 event/ 100 kg/ 100 days New Techniques for Backgrounds Techniques New Scalability of Detector Technology Scalability of Detector RHUL Jocelyn Monroe August 22, 2014 The Low-Background Frontier: Status of SI Searches 1 event/ kg/day 1 event/ 100kg/day 1 event/ 100 kg/ 100 days New Techniques for Backgrounds Techniques New Scalability of Detector Technology Scalability of Detector Complementary with High-Energy Frontier RHUL Jocelyn Monroe August 22, 2014 The Low-Background Frontier: Prospects under construction proposed so far: <1 event at 1E-45 cm2, therefore need minimum 2 1E-47 cm sensitivity for 100 events to measure MX,σ RHUL Jocelyn Monroe August 22, 2014 cross section (cm2) detector mass (ktonnes) Neutrino Lesson: key to scalability is large, open volume 10-45 100 simple detector design 30 DEAP/CLEAN Strategy: Super-K draw on design successes of 10-44 (55 kt) large neutrino experiments 10 DEAP/CLEAN Kamland (3 kt) 10-43 3 1 10-42 SNO (1 kt) MiniBooNE 10-39 0.1 (0.8 kt) RHUL Jocelyn Monroe August 22, 2014 Single Phase a la Neutrinos high light yield and self-shielding of target background discrimination from prompt scintillation timing.. -
Can Tonne-Scale Direct Detection Experiments Discover Nuclear Dark Matter?
Prepared for submission to JHEP Can Tonne-Scale Direct Detection Experiments Discover Nuclear Dark Matter? Alistair Butcher, Russell Kirk, Jocelyn Monroe and Stephen M. West Dept. of Physics, Royal Holloway University of London, Egham, Surrey, TW20 0EX, U.K. E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: Models of nuclear dark matter propose that the dark sector contains large composite states consisting of dark nucleons in analogy to Standard Model nuclei. We examine the direct detection phenomenology of a particular class of nuclear dark mat- ter model at the current generation of tonne-scale liquid noble experiments, in particular DEAP-3600 and XENON1T. In our chosen nuclear dark matter scenario distinctive fea- tures arise in the recoil energy spectra due to the non-point-like nature of the composite dark matter state. We calculate the number of events required to distinguish these spectra from those of a standard point-like WIMP state with a decaying exponential recoil spec- trum. In the most favourable regions of nuclear dark matter parameter space, we find that a few tens of events are needed to distinguish nuclear dark matter from WIMPs at the 3 σ level in a single experiment. Given the total exposure time of DEAP-3600 and XENON1T we find that at best a 2 σ distinction is possible by these experiments individually, while 3 σ sensitivity is reached for a range of parameters by the combination of the two experiments. We show that future upgrades of these experiments have potential to distinguish a large range of nuclear dark matter models from that of a WIMP at greater than 3 σ. -
Dark Matter Direct Detection
Dark Matter Direct Detection Jocelyn Monroe, Royal Holloway University of London PPAP Community Meeting University of Birmingham September 18, 2012 Outline 1. Dark Matter Direct Detection Overview • What are the top scientific challenges in Particle Physics to be solved in the next 20-30 years? 2. Current and Future UK Efforts 3. DMUK Collaboration Input to PPAP • What current and future facilities will be needed for the UK to make significant contributions to these areas? • What are the technology needs for each key priority? • What is the appropriate programmatic balance between construction, operations, exploitation, and R&D? 4. Conclusions (my opinions) The Standard Model of Cosmology E. Komatsu et al., Astrophys. J. Suppl 192 (2011) 18 evidence from CMB, galaxy clusters, large scale structure, supernova data, distance measurements, gravitational lensing Dark Matter is ~25% of the universe. RHUL Jocelyn Monroe Sept. 18, 2012 We only understand 4% of the universe! E. Komatsu et al., Astrophys. J. Suppl 192 (2011) 18 No good Standard Model dark matter particle candidates... new physics ? required. ?? (NASA) Dark matter is globally acknowledged to be one of the top scientific challenges in Particle Physics to be solved in the next 20-30 years, perhaps the top challenge. RHUL Jocelyn Monroe Sept. 18, 2012 Direct Dark Matter Detection χ Signal: χN ➙χN’ Scintillation χ Heat Ionization Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’ RHUL Jocelyn Monroe Sept. 18, 2012 Around the World KIMS NEWAGE XMASS, PANDA-X DEAP/CLEAN Picasso COUPP DRIFT LUX CDMS Xenon100 DAMA CRESST DMTPC DarkSide DM-ICE Confirmation of EDELWEISS signal from multiple SIMPLE, ANAIS technologies required. -
Dosimetry and Calorimetry Performance of a Scientific CMOS
sensors Article Dosimetry and Calorimetry Performance of a Scientific CMOS Camera for Environmental Monitoring Alexis Aguilar-Arevalo 1 , Xavier Bertou 2 , Carles Canet 3 , Miguel Angel Cruz-Pérez 4 , Alexander Deisting 5,* , Adriana Dias 5 , Juan Carlos D’Olivo 1, Francisco Favela-Pérez 1,2, Estela A. Garcés 6 , Adiv González Muñoz 6, Jaime Octavio Guerra-Pulido 1 , Javier Mancera-Alejandrez 7, Daniel José Marín-Lámbarri 6 , Mauricio Martinez Montero 1, Jocelyn Monroe 5 , Sean Paling 8, Simon J. M. Peeters 9 , Paul Scovell 8, Cenk Türko˘glu 10 , Eric Vázquez-Jáuregui 6 and Joseph Walding 5 1 Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de Mexico, A. P. 70-543, Mexico 04510, Mexico; [email protected] (A.A.-A.); [email protected] (J.C.D.); [email protected] (F.F.-P.); [email protected] (J.O.G.-P.); [email protected] (M.M.M.) 2 Centro Atómico Bariloche, CNEA/CONICET/IB, Bariloche 8400, Argentina; [email protected] 3 Centro de Ciencias de la Atmósfera, Universidad Nacional Autónoma de México, Mexico 04110, Mexico; [email protected] 4 Programa de Posgrado en Ciencias de la Tierra, Universidad Nacional Autónoma de Mexico, Ciudad Universitaria, Coyoacán 04510, Mexico; [email protected] 5 Royal Holloway, University of London, Egham Hill TW20 0EX, UK; [email protected] (A.D.); [email protected] (J.M.); [email protected] (J.W.) 6 Instituto de Física, Universidad Nacional Autónoma de México, A. P. 20-364, Mexico 01000, -
Slide from Marco Martini) a New Concept to Measure, and Report Neutrino Cross Section Data, Now the Standard of the Community
1. MiniBooNE 2. Beam Observation of a Significant Excess of Electron-Like Events3. Detector 4. Oscillation in the MiniBooNE Short-Baseline Neutrino Experiment5. Discussion arXiv:1805.12028 outline 1. MiniBooNE neutrino experiment 2. Booster Neutrino Beamline (BNB) 3. MiniBooNE Detector 4. Oscillation canDiDate search 5. Discussion Teppei Katori for the MiniBooNE collaboration Queen Mary University of London HEP seminar, UCL, UK, June 14, 2018 13/06/18 1 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion 1. MiniBooNE neutrino experiment 2. Booster Neutrino Beamline (BNB) 3. MiniBooNE Detector 4. Oscillation canDidate search 5. Discussion 13/06/18 2 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion 13/06/18 3 PHYSICAL REVIEW LETTERS 120, 141802 (2018) signature of dark matter annihilation in the Sun [5,6]. 1. MiniBooNE Despite the importance of the KDAR neutrino, it has never MiniBooNE 2. Beam been isolated and identified. 3. Detector 86 m 4. Oscillation In the charged current (CC) interaction of a 236 MeV νμ background KDAR 12 − NuMI 5. Discussion (νμ C → μ X), the muon kinetic energy (Tμ) and closely beam decay pipe related neutrino-nucleus energy transfer (ω E − E ) horns ν μ target distributions are of particular interest for benchmarking¼ absorber neutrino interaction models and generators, which report widely varying predictions for kinematics at these tran- 5 m 675 m sition-region energies [7–14]. Traditionally, experiments 40 m are only sensitive, at best, to total visible hadronic energy FIG. 1. The NuMI beamline and various sources of neutrinos since invisible neutrons and model-dependent nucleon that reach MiniBooNE (dashed lines). -
Annual Report 2017 Foundation Trustees
Victoria University of Wellington Foundation Annual Report 2017 Foundation trustees Craig Stevens, Chair Leo Lonergan, Rick Christie Bernadette Courtney Steven Fyfe Professor Deputy Chair Grant Guilford Sir Neville Jordan, Brent Manning Kerry Prendergast, Dr Farib Sos, Sir Maarten Wevers, Rory Lenihan-Ikan KNZM, DistFIPENZ CNZM MNZM KNZM (VUWSA representative) 2017 snapshot $4.3 million raised $7.2 million earned $4.2 million in donations on investments distributed 308 members 83 members of of Victoria Victoria Legacy Club Benefactors’ Circle Contents From the Chair 2 From the Vice-Chancellor 3 Our year 4 Victoria Benefactors' Circle 12 Victoria Legacy Club 15 U.K. and U.S. Friends 15 Donations received 16 Disbursements 20 Summary annual report 22 You can help 28 Cover image: This 3D illustration is of T cells attacking a cancer cell. A $500,000 donation from Breast Cancer Foundation New Zealand will help Victoria’s Ferrier Research Institute progress a vaccine-based immunotherapy treatment for breast cancer (see page 5). ISSN 2230-3723 (Print) ISSN 2230-3731 (Online) © Victoria University of Wellington, 2018 From the Chair Responsible investing means more than what we do with our funds. It’s about the investment we are making in the education of young New Zealanders and the future of our country. Every year, our First-in-Family Scholarships are an example of the many meaningful and impactful projects the Foundation supports. In 2017, in addition to these scholarships, the Foundation was able to almost double the number of Achiever Scholarships Victoria offered school leavers who might otherwise not have been in a position to attend university. -
Dark Matter Direct Detection Status and Prospects
Dark Matter Direct Detection Status and Prospects Jocelyn Monroe, Royal Holloway, University of London 2019 International Workshop on Baryon and Lepton Number Violation Institute for Theoretical Physics, Madrid, ES October 24, 2019 Big Questions for the Dark Sector (a la European Strategy for Particle Physics Update 2019) 1) How do we search for dark matter, depending on its properties? 2) What are the highlights and challenges of the experimental programs, current or near-future, that address different regions of parameter space? 3) How can dark matter detection experiments inform/guide energy and intensity frontier experiments, and vice versa? Jocelyn Monroe Oct. 24, 2019 / p.2 Big Questions for the Dark Sector (a la European Strategy for Particle Physics Update 2019) 1) How do we search for dark matter, depending on its properties? 2) What are the highlights and challenges of the experimental programs, current or near-future, that address different regions of parameter space? 3) How can dark matter detection experiments inform/guide energy and intensity frontier experiments, and vice versa? Jocelyn Monroe Oct. 24, 2019 / p.2 χ χ Gravitational Detection Indirect Detection ? e-,ν,γ e+,p,D Direct Detection Accelerator Production χ χ jet p p N N’ χ χ Jocelyn Monroe Oct. 24, 2019 / p.3 Dark Matter Direct Detection Signal:χN ➙χN χ χ Backgrounds: γ e- ➙ γ e- n N ➙ n N N ➙ N’ + α, e- ν N ➙ ν N experimental requirements: particle ID for recoil N, e-, alpha, n (multiple)γ final states γ Jocelyn Monroe Oct. 24, 2019 / p.4 1 E = m v2 WIMP Scattering χ D 2 D χ kinematics: v/c ~ 8E-4! q2 = 2m E recoil angle strongly correlated T recoil 4mDmT with incoming WIMP direction r = 2 (mD + mT ) N N (1 cosq) E = E r − recoil D 2 Spin Independent: χscatters coherently off of the entire nucleus A: σ~A2 D.