Search

We study the details of the DAMA/LIBRA results and compare those with the recent published DM Ice results of ICE Cube. In various recent papers, it was shown that the 40K peak on DAMA/LIBRA data leaves no room for a Dark Matter signal in the bulk of the data. Using Information Theory for the different types of detection environments, we show that annual variation calculations and the DM Ice data reinforce the claims that the DAMA/LIBRA detector is not observing Dark Matter WIMPs., Comment: 8 pages

Recently, in February 2014, we held a comprehensive meeting at UCLA on the Search for Dark Matter. 190 scientists came to the meeting, many of the leaders in the field of WIMP Dark Matter searches. We first review the data from LUX that excludes the low-mass WIMP region and slightly lowers the XENON100 limits. We provide a brief review of the problems with the claimed low-mass signals. We discuss the current expectations for SUSY-WIMP Dark Matter and show why very massive detectors like Darwin may be required. We discuss some theoretical predictions from the meeting., Comment: arXiv admin note: substantial text overlap with arXiv:1308.3477

Using information from a recent dark matter symposium at Marina del Rey and from various publications in 2012 and 2013, we discuss the most recent evidence and constraints on low mass WIMPs. There are now five separate experimental limits on such WIMPs, including a new paper on the XENON100 225 day exposure. There are very different experimental methods with different backgrounds that comprise this limit. We speculate on the possible sources of the reported low mass WIMP signals and background. We present recent arguments concerning DAMA that show the possible DM claims are likely misleading. We discuss the new CDMS claims for a signal and question the very low ionization in these events. We also discuss an analysis of XENON 100 data that uses information theory that further excludes the CDMS results., Comment: 11 pages, 10 figures. arXiv admin note: substantial text overlap with arXiv:1209.4037

We propose the construction of, and describe in detail, a compact Muon Collider s-channel Higgs Factory., Comment: 43 pages, 20 figures, 10 tables

The preponderance of matter over antimatter in the early Universe, the dynamics of the supernova bursts that produced the heavy elements necessary for life and whether protons eventually decay --- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our Universe, its current state and its eventual fate. The Long-Baseline Neutrino Experiment (LBNE) represents an extensively developed plan for a world-class experiment dedicated to addressing these questions. LBNE is conceived around three central components: (1) a new, high-intensity neutrino source generated from a megawatt-class proton accelerator at Fermi National Accelerator Laboratory, (2) a near neutrino detector just downstream of the source, and (3) a massive liquid argon time-projection chamber deployed as a far detector deep underground at the Sanford Underground Research Facility. This facility, located at the site of the former Homestake Mine in Lead, South Dakota, is approximately 1,300 km from the neutrino source at Fermilab -- a distance (baseline) that delivers optimal sensitivity to neutrino charge-parity symmetry violation and mass ordering effects. This ambitious yet cost-effective design incorporates scalability and flexibility and can accommodate a variety of upgrades and contributions. With its exceptional combination of experimental configuration, technical capabilities, and potential for transformative discoveries, LBNE promises to be a vital facility for the field of particle physics worldwide, providing physicists from around the globe with opportunities to collaborate in a twenty to thirty year program of exciting science. In this document we provide a comprehensive overview of LBNE's scientific objectives, its place in the landscape of neutrino physics worldwide, the technologies it will incorporate and the capabilities it will possess., Comment: Major update of previous version. This is the reference document for LBNE science program and current status. Chapters 1, 3, and 9 provide a comprehensive overview of LBNE's scientific objectives, its place in the landscape of neutrino physics worldwide, the technologies it will incorporate and the capabilities it will possess. 288 pages, 116 figures

We propose the construction of a compact Muon Collider Higgs Factory. Such a machine can produce up to \sim 14,000 at 8\times 10^{31} cm^-2 sec^-1 clean Higgs events per year, enabling the most precise possible measurement of the mass, width and Higgs-Yukawa coupling constants., Comment: Supporting letter for the document: "Muon Collider Higgs Factory for Smowmass 2013", A White Paper submitted to the 2013 U.S. Community Summer Study of the Division of Particles and Fields of the American Physical Society, Y. Alexahin, et. al, FERMILAB-CONF-13-245-T (July, 2013)

Using information from a recent dark matter symposium at Marina del Rey, we discuss the most recent evidence and constraints on low mass WIMPs. There are now five separate experimental limits on such WIMPs, including a new paper on the XENON100 225 day exposure. There are very different experimental methods with different backgrounds that comprise this limit. We speculate on the possible sources of the reported low mass WIMP signals and background., Comment: 8 pages, 6 figures

We review the confused situation concerning evidence for low-mass WIMPs. In the past one half year there have been new results concerning the existence of WIMPs at low mass including the new XENON 100, 100-day data, additional CDMS results, the publication of annual variation data from LVD and Borexino and new CoGeNT data. Along with the S2 analyses of the XENON 10 data we provide an overview of this situation. We discuss new results from 2011 here. We also discuss the origin of annual variations of signals in underground laboratories. This article is meant to be an update of recent experimental results. It is not a critical comparison of the claims of various experimental groups. Such critiques are made in public conferences and meetings. There is currently an intense discussion being carried out about the low mass WIMP region with many different viewpoints. We have little to say about this situation except that the scientific method usually insures the correct results will eventually surface., Comment: 15 pages, 13 figures

We present the state of current research of Very Short Gamma Ray Bursts (VSGRBs) from seven GRB detectors. We found that VSGRBs form distinct class of GRBs, which in our opinion, in most cases can originate from the evaporating Primordial Black Holes (PBHs). Arguments supporting our opinion: 1. GRBs with time duration (T90) < 100 ms form distinct class: VSGRBs. 2. We observe significant anisotropy in the galactic angular distribution of BATSE VSGRB events. 3. V/Vmax distribution for BATSE VSGRB events indicates the local distance production. 4. VSGBBs have more energetic {\gamma}-ray burst than other GRBs with longer duration (KONUS). 5. We observe small number of afterglows in SWIFT VSGRB sample (25%), in contrast with the noticeable afterglow frequency in SGRB sample (78%). 6. Time profile of rising part BATSE VSGRBs is in agreement with the evaporation PBH model., Comment: 12 pages, 10 figures

We briefly review the constraints on the search for low mass wimps (< 15 GeV) and the various experimental methods. These experiments depend on the response of detectors to low energy signals (less than 15 KeV equivalent energy). We then describe recent fits to the data and attempt to determine Leff, the energy response at low energy. We find that the use of a liquid Xenon 2-phase detector that employs the S_2 data near threshold is the most sensitive current study of the low mass region. We rely on some talks at Dark Matter 2010., Comment: 11 pages, 9 figures

We discuss a very peculiar subgroup of gamma-ray bursts among the BATSE sources. These bursts are very short ($T_{90} \le $0.1 s), hard, and came predominantly from a restricted direction of the sky (close to the Galactic anti-center). We analyze their arrival times and possible correlations, as well as the profiles of individual bursts. We find no peculiarities in the arrival times of Very Short Bursts (VSBs) despite their highly non-uniform spatial distribution. There is no dependence in the burst shapes on location. Bursts coming both from the burst-enhancement Galactic Anticenter region and from all other directions show considerable dispersion in their rise and fall times. Significant fraction of VSBs have multiple peaks despite their extremely short duration. Burst time properties are most likely to be consistent with two origin mechanisms: either with binary NS-NS mergers with low total masses passing through a phase of hypermassive neutron star, or with evaporation of the primordial black holes in the scenario of no photosphere formation., Comment: 25 pages, 14 figures; accepted to New Astronomy

More than a decade ago we identified a class of VSGRB (T90 < 100 ms) as having unusual properties: (1) galactic position asymmetry, (2) very hard gamma spectrum, (3) possible evidence for galactic origin of these events. We now study the recent Swift data and show that a VSGRB enhancement consistent BATSE and KONUS exists. We estimate that this is now a total 4.5sigma observation. We then study the VSB for evidence of the time structure expected for PBH evaporation. Several of the events show the general time structure expected for PBH evaporation. If correct, then PBH must exist in this galaxy. Since even large detectors like BATSE record only a few VSB per year the density of PBH can still be very small and it is hard to predict a rate for the Fermi spacecraft LAT., Comment: 11 pages, 7 figures

This report provides the technical justification for locating a large detector underground in a US based Deep Underground Science and Engineering Laboratory. A large detector with a fiducial mass in the mega-ton scale will most likely be a multipurpose facility. The main physics justification for such a device is detection of accelerator generated neutrinos, nucleon decay, and natural sources of neutrinos such as solar, atmospheric and supernova neutrinos. In addition to the physics justification there are practical issues regarding the existing infrastructure at Homestake, and the stress characteristics of the Homestake rock formations. The depth requirements associated with the various physics processes are reported for water Cherenkov and liquid argon detector technologies. While some of these physics processes can be adequately studied at shallower depths, none of them require a depth greater than 4300 mwe which corresponds to the 4850 ft level at Homestake. It is very important to note that the scale of the planned detector is such that even for accelerator neutrino detection (which allows one to use the accelerator duty factor to eliminate cosmics) a minimum depth is needed to reduce risk of contamination from cosmic rays. After consideration of the science and the practical issues regarding the Homestake site, we strongly recommend that the geotechnical studies be commenced at the 4850ft level in a timely manner., Comment: 64 pages, prepared to be part of the DUSEL design reviews 8/9/2009 corrected author list, removed extra file

A scalable line of liquid argon TPC detectors is described, based on a three dimensional cubic frame array immersed on a common liquid argon volume. The paper describes general lines, main construction criteria, crucial points, parameters and required preliminary R&D activities for the construction of detectors with active mass ranging from 200 ton to 100 kTon. Such detectors appear as unique for supernova detection, proton decay, LBL neutrino physics and other astropaticle physics applications., Comment: PDF, 13 pages with 19 JPEG figures and 1 table

The discovery of dark matter particles would conclusively reject the MOND theory. MOND may violate Einstein's Strong Equivalence principle. However, as we show, there is already evidence that MOND is likely not required. MOND was invented to explain the rotation velocities of stars far into the galactic halos. Dark Matter also explains this same effect. These both use a gravity probe of the I/R^2 law. We show that non gravity probes determine the same value for the amount of dark matter that does not involve modifications of gravity. Using Occam's Razor this coincidence is best explained by the existence of dark matter., Comment: 7 pages; prepared for 2005 Paris/Einstein conference

We discuss the major scientific issues of the search for proton decay to $10^{35}$ years lifetime and search for CP violation with a VLBL superbeam (~2000 km distance). The 100 kT LANNDD liquid Argon TPC is well matched to these goals. We describe the progress in the R&D program for the detector as well as the possible location in an underground laboratory in the USA called DUSEL., Comment: 13 pages, 6 figures, invited talk at the XI Neutrino Telescope Conference, February 2005, Venice, Italy

We briefly discuss the expected level of supersymmetric dark matter cross-sections as a reference for dark matter detectors. We then discuss the current ZEPLIN II program as a prototype of large liquid Xenon detectors. Cryoarray is a possible cryogenic detector. Finally we discuss ZEPLIN IV and other one ton liquid Xenon detectors and the limiting backgrounds for such detectors., Comment: 10 pages, 8 figures, paper presented at Beyond 03 Conference; corrected summary for Reference 4

We assume the supersymmetric model for dark matter in the universe and our galaxy, and direct methods to distinguish these kinds of dark matter are described. We then focus on the current and future experiment search for SUSY-WIMPS. Theoretical models suggest that a new generation of at least one ton detectors may be required to observe this form of dark matter. We concentrate on Liquid Xenon detectors because they can be scaled to large mass., Comment: 10 pages, 8 figures, invited talk at the SUGRA 20 Meeting, Boston, MA 2003

We describe a preliminary study of a 40-ton liquid argon TPC based on the ICARUS method to use in the NuMI near region in line with the LANNDD project. This reduced-scale detector, called ``Mini-LANNDD T40'', is designed for R&D purposes and systematic measures on its response. Safety concerns are a key issue, which will be discussed as well as a preliminary design of the detector. Adapted as a near or vertex detector in a neutrino beam, the Mini-LANNDD T40 is capable of observing the electron-neutrino flux in the off-axis beam, a key to use for measuring $\sin^2 2 \theta_{13}$ in the future, and measuring the low energy neutrino-argon cross-section, an important piece of information for future long baseline experiments., Comment: 4 pages, 5 figures, 2 tables

We briefly describe the LANNDD 70-kT liquid argon TPC proposal for the WIPP underground facility at Carlsbad, New Mexico. We, then, identify the key backgrounds for the search for p -> K+ nu_bar to 10^35 years lifetime. The most serious non-neutrino background is due to high-energy neutrons producing strange particles in the detector. We show that this can be reduced to an acceptable level by appropriate fiducial volume cuts., Comment: 7 pages, 5 figures

The ICARUS Detector at the LGNS will carry out a sensitive search for a sin sup 2(2 theta sub 13). We describe a small version for the LANNDD proton decay detector (70kT Liquid Argon) to measure nu sub mu -> nu sub e in a low energy or off-axis neutrino beam. We find an optimal detector size is 5 kT and at a distance of about 700 km from a high-energy neutrino source. This detector uses the ICARUS method., Comment: Talk given by D. Cline at the New Initiative Workshop, FNAL, May 2002

We describe the research and development program carried out by the UCLA - Torino group leading to the ZEPLIN II detector under construction for the Boulby Laboratory. Knowledge of ZEPLIN II performance will help in the design and construction of ZEPLIN IV. This detector could be located at a U.S. underground laboratory (WIPP site or others) or elsewhere. We show that a detector of this size is required to observe SUSY WIMPS., Comment: 6 pages, 7 figures

We present a concept of a one ton two-phase liquid Xenon detector based on the concept of the ZEPLIN II detector currently under construction by a UCLA/Torino/UKDM team. The ZEPLIN II detector may be installed in the Boulby laboratory early in 2002. The one ton detector design will benefit from the initial operations of ZEPLIN II., Comment: 4 pages, 6 figures

We describe a possible Liquid Argon Neutrino and Nuclear Decay Detector (LANNDD) that consists of a 70kt magnetized liquid argon tracking detector. The detector is being designed for the Carlsbad Underground Laboratory., Comment: 8 pages, 5 figures; for the Neutrino Facory Meeting at KEK-NUFACT '01

While most gamma-ray bursts (GRBs) are now believed to be from cosmological distances, the origin of very short-time GRBs is still not known. In the past, we have shown that GRBs with time duration (T90) less than 100 ms may form a separate class of GRBs based on the hardness and time distribution of these events. We have also shown that the ln N ln S distribution is consistent with the expectation of quasi-Euclidean distribution of sources. In this paper, we report the study of the angular location of these GRBs showing a strong deviation from isotropy within the Galactic coordinates of plus 180 degrees < longitude < 90 degrees and -30 degrees < latitude < 30 degrees. We have studied the rest of the GRBs and do not find a similar deviation. This further indicates that the very-short GRBs likely form a separate class of GRBs, most probably from sources of Galactic or near solar origin.

We review some of the expectations for Primordial Black Hole evaporation and we review the properties of short Gamma Ray Bursts. It is plausible that these GRB come from PBH evaporation. We then show that the angular distribution asymmetry recently observed by us could be due to a concentration of PBH in the Galactic Arms like the Orion arm.

We describe the Neutrino Spectrum and detection for SN II sources. We discuss the effects of neutrino mixing in the SN II. A new analysis of SN1987A is described. We discuss the possible detection of the diffuse relic SN II flux. Finally we discuss a new detection concept, OMNIS, for Nu sub mu and Nu sub tau and detection and compare with other present and future SN detectors.

The development of new supernova neutrino detectors relies on the expected hard energy spectrum of the nu_mu and nu_tau emitted in the supernova. We show that SN1987A was sensitive to the large mixing angle (LMA) and "just so" solution to the solar neutrino problem. We review the previous analysis of the SN1987A data and propose a new analysis. The results of this analysis strongly disfavor the LMA solution, provided the nu_mu and nu_tau are hard as predicted, Comment: 4 pages; 6 figures. Presented at the Europhysics Neutrino Oscillation Workshop, NOW 2000 (EPS, Lecce, Italy, Sept. 9-16, 2000) and to be published in Nucl. Phys. B (PS) (North Holland, Amsterdam, 2001)

We describe the research and development efforts of the UCLA Torino group to develop a large, powerful, discriminating WIMP detector. We also discuss the possible amplifications of the WIMP signal. The first real detector, ZEPLIN II, is being prepared for the UKDMC Boulby Mine Laboratory., Comment: 5 pages, including 6 figures; Presented at the Conference on Cosmology and Particle Physics, CAPP-2000 (Verbier, Switzerland, July 17-28, 2000) and to be published in the Proceedings by AIP

A neutrino factory storage ring can provide beams to various locations. We discuss the ICANOE detector (at LNGS) at one such site. We then describe the prospects for the use of the underground location at Carlsbad, NM for a neutrino factory detector. A brief discussion is given of a simple magnetized Fe detector of 10 50 kT for this site., Comment: 8 pages, including 4 figures; Presented at NuFact'00 (Monterey, CA, May 2000) and to be published in the Proceedings by NIMPR-A

We describe the current situation concerning methods to search for relic neutrinos from the Big Bang and from all past supernovae (SNs). The most promising method for Big Bang neutrinos is by the interaction of ultra-high- energy (UHE) neutrinos. For supernova neutrinos, both Super Kamiokande- and ICARUS-type detectors will be important to study both nubar_{e} and nu_{e} fluxes. We also discuss a dedicated supernova burst observatory (OMNIS) being planned for three sites in the world. We also describe the possible analysis of the supernova type-II (SNII) neutrinos, including flavor mixing, that might be carried out in the future., Comment: 12 pages with 11 figures, 5 tables; for Proceedings of VIII Int'l Wksp. on Neutrino Telescopes (Venice, Italy, Feb. 23-26, 1999

We describe the liquid-xenon dark-matter detector program of the UCLA-Torino team. A two-phase detector, ZEPLIN II, for the Boulby Mine is a good match for the current search for WIMP dark matter., Comment: 3 pages with 4 figures; for Proceedings, Sixth Int'l Wksp. On Topics in Astroparticle and Underground Physics, TAUP99 (College de France, Paris, Sept. 6-10, 1999), to be published in Nucl. Phys. B(PS)

We discuss the prospects for detecting nu_{mu,tau} and nu_{tau}neutrinos from Type II supernovas using the novel detector at the Supernova Burst Observatory (SNBO) or OMNIS that is being designed for an underground laboratory in the USA. This detector would collect ~2000 flavor selected events from a Galactic supernova and could probe neutrino mass down to a few eV, as well as the dynamics of the supernova process. We believe this is essential to further our understanding of the neutrino section of elementary particle physics., Comment: 4 pages containing 5 figures, 4 tables; workshop on Next Generation Nucleon Decay and Neutrino Detectors, NNN99 (SUNY at Stony Brook, NY, Sept. 23-25, 1999), and to be published by the American institute of Physics

We have carried out a detailed study of the morphology of gamma-ray bursts (GRBs) with time duration less than 100 ms that includes: (1) a fast-Fourier spectrum analysis, (2) a comparison with the Stern analysis of longer bursts, (3) an inner comparison of the properties of the short bursts, and (4) a comparison of the short burst properties with the bulk of the GRBs from the Burst and Transient Source Experiment (BATSE) 4B catalogue. We have used the time tagged event (TTE) BATSE 3B data, which is available to the public, for part of the analysis. We show that these bursts are very different from the rest of the GRB events. The short bursts appear to be nearly identical, suggesting a separate class of GRBs. We also show that the short bursts have a Euclidean space-time distribution, in sharp contrast to the longer bursts with $\tau_{duration} >$ 100 ms that implies that these sources are likely local. Finally we compare the bursts with a model of primordial black hole (PBH) evaporation at the quark-gluon (Q-G) phase transition temperature and other shock wave models., Comment: Text and 9 figures

Three-neutrino mixing schemes suggested by Cardall & Fuller and Acker & Pakvasa are compared and contrasted. Both of these schemes seek to solve the solar and atmospheric neutrino problems and to account for the possible neutrino oscillation signal in the LSND experiment. These neutrino oscillation schemes have different atmospheric and solar neutrino signatures that will be discriminated by Super-Kamiokande and SNO. They will also have different signatures in proposed long-baseline accelerator and reactor experiments. In particular, both of these schemes would give dramatic (and dramatically different) signals in an ``intermediate baseline'' experiment, such as the proposed ICARUS detector in the Jura mountains 17 km from CERN., Comment: 12 pages, latex; uses elsart.sty, elsart12.sty, and epsf.sty

Using a case study approach, this study focuses on a physical science teacher's method of pacing instruction and the use of target students. This report includes an examination of: (1) the teacher's perceptions of the target students in the science class; (2) possible reasons for certain students being target students; and (3) types of questions that students received. With the intention of obtaining information on the basic management of the classroom, the investigation centered on what patterns of turn taking exist in a ninth-grade physical science classroom. Also reviewed are the views of the observed teacher and an analysis of the teacher's behavior based on observational data and the perceptions of the teachers. Implications for instruction and research are discussed. (ML)