D. Markoff - North Carolina Central University

D. Markoff
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Name
D. Markoff
Affiliation
North Carolina Central University
City
Durham
Country
United States

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High Energy Physics - Experiment (16)
 
Nuclear Experiment (11)
 
Physics - Instrumentation and Detectors (8)
 
High Energy Astrophysical Phenomena (3)
 
High Energy Physics - Phenomenology (2)
 
Solar and Stellar Astrophysics (2)

Publications Authored By D. Markoff

We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and the luminosity of the astrophysical sources. Read More

The COHERENT collaboration's primary objective is to measure coherent elastic neutrino-nucleus scattering (CEvNS) using the unique, high-quality source of tens-of-MeV neutrinos provided by the Spallation Neutron Source (SNS) at Oak Ridge National Laboratory (ORNL). In spite of its large cross section, the CEvNS process has never been observed, due to tiny energies of the resulting nuclear recoils which are out of reach for standard neutrino detectors. The measurement of CEvNS has now become feasible, thanks to the development of ultra-sensitive technology for rare decay and weakly-interacting massive particle (dark matter) searches. Read More

A search for double-beta decays of 136Xe to excited states of 136Ba has been performed with the first phase data set of the KamLAND-Zen experiment. The 0+1, 2+1 and 2+2 transitions of 0{\nu}\{beta}\{beta} decay were evaluated in an exposure of 89.5kg-yr of 136Xe, while the same transitions of 2{\nu}\{beta}\{beta} decay were evaluated in an exposure of 61. Read More

In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. Read More

2015Mar
Authors: C. Adams, J. R. Alonso, A. M. Ankowski, J. A. Asaadi, J. Ashenfelter, S. N. Axani, K. Babu, C. Backhouse, H. R. Band, P. S. Barbeau, N. Barros, A. Bernstein, M. Betancourt, M. Bishai, E. Blucher, J. Bouffard, N. Bowden, S. Brice, C. Bryan, L. Camilleri, J. Cao, J. Carlson, R. E. Carr, A. Chatterjee, M. Chen, S. Chen, M. Chiu, E. D. Church, J. I. Collar, G. Collin, J. M. Conrad, M. R. Convery, R. L. Cooper, D. Cowen, H. Davoudiasl, A. De Gouvea, D. J. Dean, G. Deichert, F. Descamps, T. DeYoung, M. V. Diwan, Z. Djurcic, M. J. Dolinski, J. Dolph, B. Donnelly, D. A. Dwyer, S. Dytman, Y. Efremenko, L. L. Everett, A. Fava, E. Figueroa-Feliciano, B. Fleming, A. Friedland, B. K. Fujikawa, T. K. Gaisser, M. Galeazzi, D. C. Galehouse, A. Galindo-Uribarri, G. T. Garvey, S. Gautam, K. E. Gilje, M. Gonzalez-Garcia, M. C. Goodman, H. Gordon, E. Gramellini, M. P. Green, A. Guglielmi, R. W. Hackenburg, A. Hackenburg, F. Halzen, K. Han, S. Hans, D. Harris, K. M. Heeger, M. Herman, R. Hill, A. Holin, P. Huber, D. E. Jaffe, R. A. Johnson, J. Joshi, G. Karagiorgi, L. J. Kaufman, B. Kayser, S. H. Kettell, B. J. Kirby, J. R. Klein, Yu. G. Kolomensky, R. M. Kriske, C. E. Lane, T. J. Langford, A. Lankford, K. Lau, J. G. Learned, J. Ling, J. M. Link, D. Lissauer, L. Littenberg, B. R. Littlejohn, S. Lockwitz, M. Lokajicek, W. C. Louis, K. Luk, J. Lykken, W. J. Marciano, J. Maricic, D. M. Markoff, D. A. Martinez Caicedo, C. Mauger, K. Mavrokoridis, E. McCluskey, D. McKeen, R. McKeown, G. Mills, I. Mocioiu, B. Monreal, M. R. Mooney, J. G. Morfin, P. Mumm, J. Napolitano, R. Neilson, J. K. Nelson, M. Nessi, D. Norcini, F. Nova, D. R. Nygren, G. D. Orebi Gann, O. Palamara, Z. Parsa, R. Patterson, P. Paul, A. Pocar, X. Qian, J. L. Raaf, R. Rameika, G. Ranucci, H. Ray, D. Reyna, G. C. Rich, P. Rodrigues, E. Romero Romero, R. Rosero, S. D. Rountree, B. Rybolt, M. C. Sanchez, G. Santucci, D. Schmitz, K. Scholberg, D. Seckel, M. Shaevitz, R. Shrock, M. B. Smy, M. Soderberg, A. Sonzogni, A. B. Sousa, J. Spitz, J. M. St. John, J. Stewart, J. B. Strait, G. Sullivan, R. Svoboda, A. M. Szelc, R. Tayloe, M. A. Thomson, M. Toups, A. Vacheret, M. Vagins, R. G. Van de Water, R. B. Vogelaar, M. Weber, W. Weng, M. Wetstein, C. White, B. R. White, L. Whitehead, D. W. Whittington, M. J. Wilking, R. J. Wilson, P. Wilson, D. Winklehner, D. R. Winn, E. Worcester, L. Yang, M. Yeh, Z. W. Yokley, J. Yoo, B. Yu, J. Yu, C. Zhang

The US neutrino community gathered at the Workshop on the Intermediate Neutrino Program (WINP) at Brookhaven National Laboratory February 4-6, 2015 to explore opportunities in neutrino physics over the next five to ten years. Scientists from particle, astroparticle and nuclear physics participated in the workshop. The workshop examined promising opportunities for neutrino physics in the intermediate term, including possible new small to mid-scale experiments, US contributions to large experiments, upgrades to existing experiments, R&D plans and theory. Read More

We search for electron anti-neutrinos ($\overline{\nu}_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline{\nu}_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between $\overline{\nu}_e$ luminosity and effective temperature. Read More

We describe a new detector, called NuLat, to study electron anti-neutrinos a few meters from a nuclear reactor, and search for anomalous neutrino oscillations. Such oscillations could be caused by sterile neutrinos, and might explain the "Reactor Antineutrino Anomaly". NuLat, is made possible by a natural synergy between the miniTimeCube and mini-LENS programs described in this paper. Read More

We describe a compact, ultra-clean device used to deploy radioactive sources along the vertical axis of the KamLAND liquid-scintillator neutrino detector for purposes of calibration. The device worked by paying out and reeling in precise lengths of a hanging, small-gauge wire rope (cable); an assortment of interchangeable radioactive sources could be attached to a weight at the end of the cable. All components exposed to the radiopure liquid scintillator were made of chemically compatible UHV-cleaned materials, primarily stainless steel, in order to avoid contaminating or degrading the scintillator. Read More

2014May
Affiliations: 1The KamLAND Collaboration, 2The KamLAND Collaboration, 3The KamLAND Collaboration, 4The KamLAND Collaboration, 5The KamLAND Collaboration, 6The KamLAND Collaboration, 7The KamLAND Collaboration, 8The KamLAND Collaboration, 9The KamLAND Collaboration, 10The KamLAND Collaboration, 11The KamLAND Collaboration, 12The KamLAND Collaboration, 13The KamLAND Collaboration, 14The KamLAND Collaboration, 15The KamLAND Collaboration, 16The KamLAND Collaboration, 17The KamLAND Collaboration, 18The KamLAND Collaboration, 19The KamLAND Collaboration, 20The KamLAND Collaboration, 21The KamLAND Collaboration, 22The KamLAND Collaboration, 23The KamLAND Collaboration, 24The KamLAND Collaboration, 25The KamLAND Collaboration, 26The KamLAND Collaboration, 27The KamLAND Collaboration, 28The KamLAND Collaboration, 29The KamLAND Collaboration, 30The KamLAND Collaboration, 31The KamLAND Collaboration, 32The KamLAND Collaboration, 33The KamLAND Collaboration, 34The KamLAND Collaboration, 35The KamLAND Collaboration, 36The KamLAND Collaboration, 37The KamLAND Collaboration, 38The KamLAND Collaboration, 39The KamLAND Collaboration, 40The KamLAND Collaboration, 41The KamLAND Collaboration, 42The KamLAND Collaboration, 43The KamLAND Collaboration, 44The KamLAND Collaboration, 45The KamLAND Collaboration, 46The KamLAND Collaboration, 47The KamLAND Collaboration, 48The KamLAND Collaboration, 49The KamLAND Collaboration, 50The KamLAND Collaboration, 51The KamLAND Collaboration, 52The KamLAND Collaboration, 53The KamLAND Collaboration, 54The KamLAND Collaboration, 55The KamLAND Collaboration, 56The KamLAND Collaboration, 57The KamLAND Collaboration, 58The KamLAND Collaboration, 59The KamLAND Collaboration, 60The KamLAND Collaboration, 61The KamLAND Collaboration, 62The KamLAND Collaboration, 63The KamLAND Collaboration, 64The KamLAND Collaboration, 65The KamLAND Collaboration, 66The KamLAND Collaboration, 67The KamLAND Collaboration, 68The KamLAND Collaboration, 69The KamLAND Collaboration, 70The KamLAND Collaboration, 71The KamLAND Collaboration

We report a measurement of the neutrino-electron elastic scattering rate of 862 keV 7Be solar neutrinos based on a 165.4 kton-day exposure of KamLAND. The observed rate is 582 +/- 90 (kton-day)^-1, which corresponds to a 862 keV 7Be solar neutrino flux of (3. Read More

2013Dec
Affiliations: 1Tohoku University, 2Tohoku University, 3Tohoku University, 4Tohoku University, 5Tohoku University, 6Tohoku University, 7Tohoku University, 8Tohoku University, 9Tohoku University, 10Tohoku University, 11Tohoku University, 12Tohoku University, 13Tohoku University, 14Tohoku University, 15Tohoku University, 16Tohoku University, 17Tohoku University, 18Tohoku University, 19Tohoku University, 20Tohoku University, 21Tohoku University, 22Tohoku University, 23Tohoku University, 24Tohoku University, 25Tohoku University, 26Tohoku University, 27Tohoku University, 28CEA-Saclay, 29CEA-Saclay, 30CEA-Saclay, 31CEA-Saclay, 32CEA-Saclay, 33CEA-Saclay, 34CEA-Saclay, 35CEA-Saclay, 36CEA-Saclay, 37CEA-Saclay, 38CEA-Saclay, 39CEA-Saclay, 40CEA-Saclay, 41CEA-Saclay, 42CEA-Saclay, 43Colorado State University, 44Colorado State University, 45University of Tokyo, 46Lawrence Berkeley National Laboratory and Berkeley University, 47Lawrence Berkeley National Laboratory and Berkeley University, 48Lawrence Berkeley National Laboratory and Berkeley University, 49Lawrence Berkeley National Laboratory and Berkeley University, 50Lawrence Berkeley National Laboratory and Berkeley University, 51Lawrence Berkeley National Laboratory and Berkeley University, 52Lawrence Berkeley National Laboratory and Berkeley University, 53Nikhef and the University of Amsterdam, 54North Carolina Central University, 55Osaka University, 56ITEP/INR RAS, 57IPCE RAS, 58Mephi, 59University of Hawaii, 60University of Hawaii, 61University of Hawaii, 62University of Hawaii, 63University of North Carolina, 64University of Tennessee, 65University of Washington, 66University of Washington

The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND) as early as 2015. KamLAND's 13 m diameter target volume provides a suitable environment to measure the energy and position dependence of the detected neutrino flux. Read More

The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this white paper, we describe how the SNS source can be used for a measurement of coherent elastic neutrino-nucleus scattering (CENNS), and the physics reach of different phases of such an experimental program (CSI: Coherent Scattering Investigations at the SNS). Read More

We propose to test for short baseline neutrino oscillations, implied by the recent reevaluation of the reactor antineutrino flux and by anomalous results from the gallium solar neutrino detectors. The test will consist of producing a 75 kCi 144Ce - 144Pr antineutrino source to be deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND's 13m diameter target volume provides a suitable environment to measure energy and position dependence of the detected neutrino flux. Read More

The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this document, the product of a workshop at the SNS in May 2012, we describe this free, high-quality stopped-pion neutrino source and outline various physics that could be done using it. We describe without prioritization some specific experimental configurations that could address these physics topics. Read More

The Spallation Neutron Source in Oak Ridge, Tennessee, is designed to produce intense pulsed neutrons for various science and engineering applications. Copious neutrinos are a free by-product. When it reaches full power, the SNS will be the world's brightest source of neutrinos in the few tens of MeV range. Read More

A liquid helium target system was designed and built to perform a precision measurement of the parity-violating neutron spin rotation in helium due to the nucleon-nucleon weak interaction. The measurement employed a beam of low energy neutrons that passed through a crossed neutron polarizer--analyzer pair with the liquid helium target system located between them. Changes between the target states generated differences in the beam transmission through the polarizer--analyzer pair. Read More