Muon Collider Higgs Factory for Snowmass 2013
We propose the construction of, and describe in detail, a compact Muon Collider s-channel Higgs Factory.
hep-ph↗
arXiv subjects
David B. Cline
Publications and source records attributed to David B. Cline.
The Case for a Muon Collider Higgs Factory
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.
hep-ph↗
The status of the search for low mass WIMPs: 2012
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.
hep-ph↗
Recent results on the low mass dark matter WIMP controversy: 2011
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.
astro-ph.CO↗
Does Very Short Gamma Ray Bursts originate from Primordial Black Holes? Review
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 γ-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.
astro-ph.CO↗
The Search for Dark Matter (WIMPS) at Low Mass
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.
astro-ph.HE↗
Observational constraints on the nature of very short gamma-ray bursts
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.
astro-ph.HE↗
Evidence for Primordial Black Hole Final Evaporation: Swift, BATSE and KONUS and Comparisons of VSGRBs and Observations of VSB That Have PBH Time Signatures
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.
astro-ph.CO↗
Report on the Depth Requirements for a Massive Detector at Homestake
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.
hep-ex↗
LANNDD - A line of liquid argon TPC detectors scalable in mass from 200 Tons to 100 Ktons
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.
astro-ph↗
The Search for Dark Matter, Einstein's Cosmology and MOND
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.
astro-ph↗
A Unique Detector for Proton Decay and Neutrino Oscillations Study (LANNDD) for a Usa Dusel
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.
astro-ph↗
Direct Search for Dark Matter Particles With Very Large Detectors
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.
astro-ph↗
Status of the Search for Supersymmetric Dark Matter
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.
astro-ph↗
Mini-LANNDD T40: A detector to measure the neutrino-argon cross section and the electron-neutrino contamination in the off-axis NuMI beam
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 $\sin^2 2 θ_{13}$ in the future, and measuring the low energy neutrino-argon cross-section, an important piece of information for future long baseline experiments.
astro-ph↗
Study of the Backgrounds for the Search for Proton Decay to 10^35 Y at the WIPP Site with the LANNDD Detector
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.
astro-ph↗
Mini-LANNDD: A Very Sensitive Neutrino Detector To Measure sin sup 2(2 theta sub 13)
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.
astro-ph↗
ZEPLIN IV: A One Ton Ultimate WIMP Detector
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.
astro-ph↗