Search

Radial velocity (RV) and light curve (LC) data for the overcontact binary V563 Lyr have been obtained and analysed with the 2003 version of the WilsonDevinney (WD) code with results K1 = 147.4 ± 2.1 km/s, K2 = 247.2 ± 1.1 km/s, RVγ = 22.5 ± 1.5 km/s, qsp = 0.596 ± 0.008, M1 = 2.49(4)M☉, M2 = 1.45(4)M☉, R1 = 2.23(2)R☉, R2 = 1.81(2)R☉. A third component was identified, with radial velocity RV3 = 18.8 ± 6.7 km/s. Inserting the derived parameters of the eclipsing pair into a Log (L)-Log (Teff) plot for each star using data from Yakut and Eggleton (2005) suggested that both stars are over-luminous and evolved to, and perhaps past, the terminal age main sequence (TAMS). The companion (star 3) has a spectral type of A0 ± 1 spectral subclass but cannot be gravitationally bound to the eclipsing pair, as its flux would dominate that of the pair, which was not observed. The companion must lie at some other distance.

Precise multi-color CCD-derived photometric data were obtained from EH Cnc at two sites during 2010, 2014 and 2018 wherein each epoch used a different instrument. This has provided a unique opportunity to investigate parameter uncertainty following Roche modeling of light curves optimized by differential corrections using the Wilson–Devinney code. Furthermore, new radial velocity data from EH Cnc presented in this study for the first time has produced absolute physical and geometric parameters for this A-subtype W UMa-type variable. Analysis of eclipse timing data confirms the presence of sinusoidal-like excursions in the eclipse timing residuals. We address whether these are due to magnetic activity cycles, the so-called “Applegate effect”, or related to a light-time effect (LiTE) resulting from the presence of a third gravitationally bound cool low mass white dwarf. A model using the PAdova & TRieste Stellar Evolution Code (PARSEC) has provided valuable insight about the evolutionary history of EH Cnc as a trinary system.

Radial velocity data and photometric light curves (in the B. V, and Ic passbands) for the detached eclipsing binary AG Leo Minoris were acquired–apparently for the first time–and are reported here. Roche modelling using the 2003 version of the Wilson-Devinney code was completed, yielding the basic parameters. The period appears to be constant, but further monitoring is highly desirable. Reference to zero age main sequence values in Cox (2000) indicates that both stars are evolved. Tables from Schaller et al. (1992) suggest an age of 3.17 Gy.

The first reliable radial velocity curves for RZ Tau have been obtained. Combined with new light curve (LC) data, simultaneous Roche-based light curve analyses have been carried out using the 2003 version of the Wilson-Devinney code. New values for the masses and radii have been obtained: M1 = 1.53 (4) Mʘ, M2 = 0.57 (2) Mʘ, and R1 = 1.50 (4) Rʘ, R2 = 0.99 (2) Rʘ. Although there is a multitude of spectral classifications listed in the literature, the classification of F0 from Struve et al. (1950) is shown to be the most reliable. On the basis of the latter, the most likely luminosities are L1 = 4.97 (44) Lʘ and L2 = 2.11 (19) Lʘ. Additional modelling was carried out using the same RV data, but with LC data (binned and unbinned) from Binnendijk (1963); the results were substantially the same except that they favoured slightly later spectral sub-classes.

New radial velocity and photometric data for TW CrB have been obtained, and Roche-based simultaneous analysis of RV and light curve data for the system has been accomplished for the first time, using the 2003 version of the Wilson-Devinney code. Values for the masses and radii have been obtained: M1 = 1.31 (6) Mʘ, M2 = 1.22 (4) Mʘ, and R1 = 1.50 (1) Rʘ, R2 = 1.42 (1) Rʘ. For the luminosities the most likely values are L1 = 2.78 (5) Lʘ and L2 = 2.01 (4) Lʘ. Both stars are likely unevolved. There is general agreement with earlier photometric values for Zhang and Zhang (2003) with the exception of their masses and mass ratio. Because the values in this paper for the latter quantities are based on radial velocities, they are to be preferred.

New radial velocity and photometric data for BO Ari have been obtained, and Roche-based simultaneous analysis of RV and light curve data for the system has been accomplished using the 2003 version of the Wilson-Devinney code. Values for the masses and radii have been obtained: M1 = 1.34 (2) Mʘ, M2 = 0.26 (1) Mʘ, and R1 = 1.25 (2) Rʘ, R2 = 0.61 (2) Rʘ. For the luminosities the most likely values are L1 = 1.67 (15) Lʘ and L2 = 0.42 (4) Lʘ, each the mean of two values. There is poor agreement with earlier values by Gurol et al. (2015). During the light curve modelling, solutions were found with a small third light contribution, but the existence of the latter cannot be established unambiguously owing to the very close residuals of the different solutions. A third component was not found in the RV data within detection limits.

In an effort to resolve the discrepancy between two earlier studies, new radial velocity and photometric data have been obtained and analyzed by Roche modelling for AB Andromedae, an overcontact W-subtype eclipsing binary. The new values for the basic data, m1 = 0.60 (3) Mʘ, m2 = 1.14 (3) Mʘ, R1 = 0.81 (1) Rʘ, R2 = 1.08 (1) Rʘ, L1 = 0.73 (6) Lʘ, and L2 = 1.02 (7) Lʘ, mostly lie close to a given set of previously reported values, but in some cases show small but significant differences. The latter may reflect the real errors in derived quantities, as opposed to estimated errors (quoted here and elsewhere), the latter of which sometimes underestimate the true values. A distance estimate of r = 116 (8) pc was obtained, in poor agreement with the Gaia value of 85.24 (26) pc. In addition, a new period analysis is presented using updated eclipse times, resulting in a new light time effect (LiTE) fit. Magnetic cycles, due to the Applegate effect, are likely present.

New radial velocity and photometric data for DU Leonis have been obtained, and Roche-based simultaneous analysis of RV and light curve data for DU Leo has been accomplished for the first time, using the 2003 and 2015 versions of the Wilson-Devinney code. Values for the masses and radii have been obtained: M1 = 0.937 (5) Mʘ, M2 = 0.921 (5) Mʘ, and R1 = 1.25 (1) Rʘ, R2 = 1.21 (1) Rʘ. For the luminosities the most likely values are L1 = 1.66 (3) Lʘ and L2 = 1.50 (3) Lʘ. Both stars are at or near the end of hydrogen-burning in the cores, and are moving toward the red giant phase.

A search for instability of nucleons bound in Xe136 nuclei is reported with 223 kg·yr exposure of Xe136 in the EXO-200 experiment. Lifetime limits of 3.3×1023 and 1.9×1023 yr are established for nucleon decay to Sb133 and Te133, respectively. These are the most stringent to date, exceeding the prior decay limits by a factor of 9 and 7, respectively.

An updated period analysis for the overcontact eclipsing binary ER Orionis is presented. Featured is animproved derivation of parameters for the light time effect (LTE) due to the third star (in actuality, a pairof stars) utilising the latest set of eclipse timings. The very good fit between the eclipse timing differences(ETD) plot (otherwise known as an O–C diagram) and the theoretical ETD curve makes possible animproved determination of the rate of mass interchange between the binary pair, dm 1 /dt = +1.83(6) 10 7 M ( /year. In addition, the mass of the companion system (in actuality, m 3 sini) andthe elements of its orbit were computed. A suggestion is made for a method of future determinationof the inclination of the orbit of the companion system. 2014 Elsevier B.V. All rights reserved. 1. IntroductionER Ori (= BD 8 1050 = TYC 5330-784-1 = HIP 24156; RA = 05 h11 m 14.505 s, Dec 08 33 0 24.70 00 , J2000) was discovered to bevariable by Hoffmeister (1929) who supplied coordinates and amagnitude range, and labelled the system as Algol-type. It was firstcorrectly recognised, from visual observations, as a W UrsaeMajoris system by Florja (1931), who also supplied a period.Photographic observations were made by Alexander (1940) whilephotoelectric light curves were obtained by Huruhata et al.(1957). Struve (1944) obtained spectroscopic observations, deriv-ing radial velocity (RV) curves; he also classified the system asspectral type G0-2. The first period study was by Kwee (1958),who noticed, from an ETD plot, that the period was fairly constantuntil about 1952, after which it increased ‘‘very strongly’’ from0.4233955 to 0.42340620 days. Binnendijk (1962) also madenumerous photoelectric observations (over six successive seasons)and noted that Min I and Min II should be reversed. He alsosupplied new orbital elements and updated the ETD plot.In the intervening years, additional light curve and RV analyseswere undertaken. Russo et al. (1982) re-analysed Binnendijk’sobservations with the Wilson–Devinney (WD) code (Wilson andDevinney, 1971) and determined fundamental parameters suchas stellar mass, radius and luminosity. They also indicated the sys-tem to be a W-type (smaller star is the hotter) and hinted that EROri is evolved from the zero age main sequence (ZAMS). Rovithisand Rovithis-Livaniou (1986) obtained B and V photoelectricobservations and performed a light curve analysis using frequencydomain techniques. Liu et al. (1988) obtained additional B and Vphotoelectric observations and performed an analysis using theWD code. Goecking et al. (1994) obtained photoelectric andspectroscopic observations, deriving RV curves from the cross-correlation technique; they also used the latter to establish theexistence of a third body (first suggested by Abhyankar andPanchatsaram, 1982). They went on to say that ‘‘High-resolutionspeckle masking observations show that this companion has a sep-aration of 0.19’’ from the W UMa system, is about 2.3 magnitudesfainter than the binary at maximum light, and is very likely phys-ically connected to the system’’. They also calculated a new valuefor the mass ratio, and deduced that the system is slightly evolvedand is of spectral type F8. They also asserted that, contrary to the

Searches for double beta decay of ^(134)Xe were performed with EXO-200, a single-phase liquid xenon detector designed to search for neutrinoless double beta decay of ^(136)Xe. Using an exposure of 29.6 kg⋅yr, the lower limits of T^(2νββ_+(1/2) > 8.7×10^(20) yr and T^(0νββ)_(1/2) > 1.1×10^(23) yr at 90% confidence level were derived, with corresponding half-life sensitivities of 1.2×10^(21) yr and 1.9×10^(23) yr. These limits exceed those in the literature for ^(134)Xe, improving by factors of nearly 105 and 2 for the two antineutrino and neutrinoless modes, respectively.

Results from a search for neutrinoless double-beta decay $0\nu\beta\beta$ of $^{136}$Xe are presented using the first year of data taken with the upgraded EXO-200 detector. Relative to previous searches by EXO-200, the energy resolution of the detector has been improved to $\sigma/E$=1.23%, the electric field in the drift region has been raised by 50%, and a system to suppress radon in the volume between the cryostat and lead shielding has been implemented. In addition, analysis techniques that improve topological discrimination between $0\nu\beta\beta$ and background events have been developed. Incorporating these hardware and analysis improvements, the median 90% confidence level $0\nu\beta\beta$ half-life sensitivity after combining with the full data set acquired before the upgrade has increased 2-fold to $3.7 \times 10^{25}$ yr. No statistically significant evidence for $0\nu\beta\beta$ is observed, leading to a lower limit on the $0\nu\beta\beta$ half-life of $1.8\times10^{25}$ yr at the 90% confidence level., Comment: 6 pages, 4 figures, final version submitted to PRL

We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in the high-frequency domain both in the ground-based data and in Kepler observations. In the longer-period domain, the Lomb–Scargle periodogram revealed several peaks above the 99% significance level. The longest one—about 95 days—corresponds to the innermost stable circular orbit (ISCO) period of the more massive black hole. The 43-day period could be an alias, or it can be attributed to accretion in the form of a two-armed spiral wave.

We analyse the light curve in the R-band gathered during the 2015/16 observing season of OJ287. We did a search for QPOs using several methods in wide time domain. No statistically significant periods were found in the high frequency domain both in the ground data and also in K2 observations. In the longer periods domain the Lomb-Scargle periodogram revealed several peaks above the 99\% significance level. The longest one, about 95-day, corresponds to the ISCO period of the more massive SMBH. The 43-day period could be an alias or can be attributed to accretion in the form of two armed spiral wave.

EXO-200 is a single phase liquid xenon detector designed to search for neutrinoless ββ decay of ^(136)Xe to the ground state of ^(136)Ba. We report here on a search for the two-neutrino ββ decay of 136Xe to the first 0+ excited state, 0^+_1, of ^(136)Ba based on a 100 kg yr exposure of ^(136)Xe. Using a specialized analysis employing a machine learning algorithm, we obtain a 90% CL half-life sensitivity of 1.7 × 10^(24) yr. We find no statistically significant evidence for the 2νββ decay to the excited state resulting in a lower limit of T^(2ν)_(1/2)(0^+ → 0^+_1) > 6.9 ×10^(23) yr at 90% CL. This observed limit is consistent with the estimated half-life of 2.5 × 10^(25) yr.

The energy resolution of the EXO-200 detector is limited by electronics noise in the measurement of the scintillation response. Here we present a new technique to extract optimal scintillation energy measurements for signals split across multiple channels in the presence of correlated noise. The implementation of these techniques improves the energy resolution of the detector at the neutrinoless double beta decay Q-value from $\left[1.9641\pm 0.0039\right]\%$ to $\left[1.5820\pm 0.0044\right]\%$., Comment: 21 pages, 8 figures, 1 table

In this paper we present a combined photometric, spectroscopic and orbital period study of three early-type eclipsing binary systems: XZ Aql, UX Her, and AT Peg. As a result, we have derived the absolute parameters of their components and, on that basis, we discuss their evolutionary states. Furthermore, we compare their parameters with those of other binary systems and with the theoretical models. An analysis of all available up-to-date times of minima indicated that all three systems studied here show cyclic orbital changes, their origin is discussed in detail. Finally, we performed a frequency analysis for possible pulsational behavior and as a result we suggest that XZ Aql hosts a {\delta} Scuti component., Comment: 40 pages, 16 figures

We aim to discover the accuracy of photometric mass ratios (qph) determined for eclipsing binary stars, in the case of the system having at least one ‘flat bottom’ as a minimum profile, as well as the accuracy of data used in that sense. Within this context, we present the results of two-dimensional grid search (q – i) for some W UMa-type eclipsing binaries showing total eclipses, based on the high precision photometric data provided by the KEPLER Mission. The radial velocity data obtained for KIC10618253 in this study, enables us to compare both qph and the corresponding spectroscopic mass ratio (qsp) values. The results indicate that the high precision photometric data for overcontact eclipsing binaries showing total eclipses allow us to obtain the photometric mass ratios as accurate as the spectroscopic values.

Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the binary black hole model for OJ~287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the binary black hole central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level., 24 pages, 11 figures, 3 tables, accepted for publication in ApJ

New photoelectric BVR light curves and radial velocity curves were obtained for the HIPPARCOS discovery DN Boo at the TUBITAK 1 National Observatory of Turkey (TUG) and Dominion Astrophysical Observatory (DAO), respectively, to determine physical nature of the variable. The character of the obtained light curves and double-lined spectroscopic structures in the obtained spectra are revealed that DN Boo is a genuine EW type eclipsing binary. During the analysis of our new observations a simultaneous solution were derived for the photometric and spectroscopic data by using the Wilson–Devinney code and orbital parameters with absolute dimensions of the system were determined for the first time. Finally, the importance of very low mass-ratio contact binaries in the late stages of close binary evolution was discussed.

The published CDMS analyses have used the shape of the phonon signal rising edge to reject low-ionization-yield surface events which produce acoustic phonons more quickly than bulk events do. To achieve better WIMP sensitivity with future larger exposures, we are using a simplified model of phonon production and propagation to construct event position estimators that help us to find more efficient surface event rejection cuts. We describe this model and the resulting new cuts, and summarize the surface event leakage rates and the sensitivity figures of merit of the five surface event rejection methods developed in the second CDMS II Soudan run data analysis.

Free fatty acids are the major lipid fuel of the body. Dysregulation of adipose tissue lipolysis results in increased plasma free fatty acid concentrations, and via that mechanism contributes to insulin resistance in obesity and type 2 diabetes mellitus. Adipose tissue hormone sensitive lipase is thought to be responsible for the production of the majority of free fatty acids. However, a separate contribution comes from the action of endothelial lipases, especially lipoprotein lipase, on triglyceride-rich lipoproteins via a process known as spillover. The primary substrate for spillover appears to be chylomicrons derived from dietary fat. The spillover of fatty acids into the free fatty acid pool varies from one tissue to another. For example, spillover is low ( approximately 14%) in the forearm of healthy volunteers, suggesting that triglyceride fatty acid storage is relatively efficient in skeletal muscle. In contrast, spillover appears to be higher in adipose tissue and may also be higher in the splanchnic bed, based on preliminary data. If systemic spillover is increased in insulin resistant states such as diabetes, this could represent a mechanism contributing to the abnormal increases in plasma concentrations of free fatty acids in that condition.

We present the results of the spectroscopic, photometric and orbital period variation analyses of the detached eclipsing binary \astrobj{V482~Per}. We derived the absolute parameters of the system (M$_{1}$ = 1.51 M$_{\odot}$, M$_{2}$ = 1.29 M$_{\odot}$, R$_{1}$ = 2.39 R$_{\odot}$, R$_{2}$ = 1.45 R$_{\odot}$, L$_{1}$ = 10.15 L$_{\odot}$, L$_{2}$ = 3.01 L$_{\odot}$) for the first time in literature, based on an analysis of our own photometric and spectroscopic observations. We confirm the nature of the variations observed in the system's orbital period, suggested to be periodic by earlier works. A light time effect due to a physically bound, star-sized companion (M$_{3}$ = 2.14 M$_{\odot}$) on a highly eccentric (e = 0.83) orbit, seems to be the most likely cause. We argue that the companion can not be a single star but another binary instead. We calculated the evolutionary states of the system's components, and we found that the primary is slightly evolving after the Main Sequence, while the less massive secondary lies well inside it., Published in New Astronomy, Vol. 41, p. 42-47

In the past year and a half, the Cryogenic Dark Matter Search (CDMS) collaboration has been active at the Soudan mine in installing a system for running ZIP detectors that will be used to search for dark matter in the form of Weakly Interacting Massive Particles. Presently, there is an operating cryogenic system, working electronics, a functional data acquisition and analysis system, passive shielding, an active muon veto, and 12 ZIP detectors. Six of the 12 ZIP detectors have been tested in situ and are fully operational with acceptable noise profiles. CDMS is in the process of commissioning the experiment and expects to be making a background measurement by the end of summer 2003.

We report a first search for weakly interacting massive particles (WIMPs) using the background rejection capabilities of SuperCDMS. An exposure of 577 kg days was analyzed for WIMPs with mass

We report on an improved measurement of the 2νββ half-life of ^(136)Xe performed by EXO-200. The use of a large and homogeneous time-projection chamber allows for the precise estimate of the fiducial mass used for the measurement, resulting in a small systematic uncertainty. We also discuss in detail the data-analysis methods used for double-β decay searches with EXO-200, while emphasizing those directly related to the present measurement. The ^(136)Xe 2νββ half-life is found to be T^(2νββ)_(1/2) = 2.165±0.016(stat)±0.059(sys)×10^(21) yr. This is the most precisely measured half-life of any 2νββ decay to date.

We present results from analysis of combined spectroscopic and photometric data for three eclipsing binary systems: AP And, VZ Cep and V881 Per. Based on new, multicolour photometric light curves and spectroscopically determined mass ratio values, we derived accurate physical parameters of the components. Two of the systems, namely VZ Cep and V881 Per, were found to be magnetically active. The variability of V881 Per was studied in several sets of data [Northern Sky Variability Survey (NSVS), Wide Angle Search for Planets (WASP) and newly derived] gathered at different epochs. We show that the huge differences in the shape of its light curve can be explained by just a single model differing only in number of spots and their location on the surface of the primary component.

We report results of a search for Weakly Interacting Massive Particles (WIMPS) with the silicon detectors of the CDMS II experiment. This blind analysis of 140.2 kg-days of data taken between July 2007 and September 2008 revealed three WIMP-candidate events with a surface-event background estimate of 0.41^{+0.20}_{-0.08}(stat.)^{+0.28}_{-0.24}(syst.). Other known backgrounds from neutrons and 206Pb are limited to < 0.13 and, 5 pages, 4 figures, as accepted by PRL

We present the techniques and results of the calibrations and surface-event rejection cut for the current CDMS-II data set, along with proposals for future analysis of CDMS-II data.

We present the results of the first two data runs of the Cryogenic Dark Matter Search at Soudan Underground Laboratory. These data exclude substantial new parameter space for both spin-independent and spin-dependent WIMP–nucleon interactions within the standard halo model.

SuperCDMS is an experiment designed to directly detect weakly interacting massive particles (WIMPs), a favored candidate for dark matter ubiquitous in the Universe. In this Letter, we present WIMP-search results using a calorimetric technique we call CDMSlite, which relies on voltage-assisted Luke-Neganov amplification of the ionization energy deposited by particle interactions. The data were collected with a single 0.6 kg germanium detector running for ten live days at the Soudan Underground Laboratory. A low energy threshold of 170 eVee (electron equivalent) was obtained, which allows us to constrain new WIMP-nucleon spin-independent parameter space for WIMP masses below 6 GeV/c2, Funding and support were received from the National Science Foundation, the Department of Energy, a Fermilab URA Visiting Scholar Award, NSERC Canada, and MULTIDARK. Fermilab is operated by the Fermi Research Alliance, LLC under Contract No. De-AC02- 07CH11359. SLAC is operated under Contract No. DEAC02- 76SF00515 with the United States Department of Energy

Matter, as we know it, makes up less than 5% of the Universe. Various astrophysical observations have confirmed that one quarter of the Universe and most of the matter content in the Universe is made up of Dark Matter. The nature of Dark Matter is yet to be discovered and is one of the biggest questions in Physics. Particle Physics combined with astrophysical measurements of the abundance gives rise to a Dark Matter candidate called Weakly Interacting Massive Particle (WIMP). The low density of WIMPs in the galaxies and the extremely weak nature of the interaction with ordinary matter make detection of the WIMP an extraordinarily challenging task, with abundant fakes from various radioactive and cosmogenic backgrounds with much stronger electromagnetic interaction. The extremely weak nature of the WIMP interaction dictates detectors that have extremely low naturally occurring radioactive background, a large active volume (mass) of sensitive detector material to maximize statistics, a highly efficient detector based rejection mechanism for the dominant electromagnetic background and sophisticated analysis techniques to reject any residual background. This paper describes the status of the SuperCDMS experiment.

Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, el nombre del grupo de colaboración, si le hubiere, y los autores pertenecientes a la UAM, We report results of a search for weakly interacting massive particles (WIMPs) with the Si detectors of the CDMS II experiment. This report describes a blind analysis of the first data taken with CDMS II’s full complement of detectors in 2006–2007; results from this exposure using the Ge detectors have already been presented. We observed no candidate WIMP-scattering events in an exposure of 55.9 kg-days before analysis cuts, with an expected background of ˞1.1 events. The exposure of this analysis is equivalent to 10.3 kg-days over a recoil energy range of 7–100 keV for an ideal Si detector and a WIMP mass of 10 GeV/c2. These data set an upper limit of 1.7 x 10-41 cm2 on the WIMP-nucleon spin-independent cross section of a 10 GeV/c2 WIMP. These data exclude parameter space for spin-independent WIMP-nucleon elastic scattering that is relevant to recent searches for low-mass WIMPs, This work is supported in part by the National Science Foundation (Grants No. AST-9978911, No. NSF-1102795, No. PHY- 0847342, No. PHY-0542066, No. PHY-0503729, No. PHY- 0503629, No. PHY-0503641, No. PHY-0504224, No. PHY-0705052, No. PHY-0801708, No. PHY-0801712, No. PHY-0802575, No. PHY-0847342, No. PHY-0855299, No. PHY-0855525, No. PHY-1151869, and No. PHY- 1205898), by the Department of Energy (Contracts No. DE-AC03-76SF00098, No. DE-FG02-92ER40701, No. DE-FG03-90ER40569, No. DE-FG03-91ER40618, and No. DE-SC0004022), by the Swiss National Foundation (SNF Grant No. 20-118119), by NSERC Canada (Grants No. SAPIN 341314 and No. SAPPJ 386399), and by MULTIDARK CSD2009-00064 and FPA2012-34694. Fermilab is operated by Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359, while SLAC is operated under Contract No. DE-AC02- 76SF00515 with the U.S. Department of Energy

As neutrinoless double-beta decay experiments become more sensitive and intrinsic radioactivity in detector materials is reduced, previously minor contributions to the background must be understood and eliminated. With this in mind, cosmogenic backgrounds have been studied with the EXO-200 experiment. Using the EXO-200 TPC, the muon flux (through a flat horizontal surface) underground at the Waste Isolation Pilot Plant (WIPP) has been measured to be Φ = 4.07 ± 0.14 (sys) ± 0.03 (stat) × 10−7cm−2 s−1, with a vertical intensity of Iv = 2.97 −0.13 (sys) ± 0.02 (stat) × 10−7cm−2 s−1 sr−1. Simulations of muon-induced backgrounds identified several potential cosmogenic radionuclides, though only 137Xe is a significant background for the 136Xe 0νββ search with EXO-200. Muon-induced neutron backgrounds were measured using γ-rays from neutron capture on the detector materials. This provided a measurement of 137Xe yield, and a test of the accuracy of the neutron production and transport simulations. The independently measured rates of 136Xe neutron capture and of 137Xe decay agree within uncertainties. Geant4 and FLUKA simulations were performed to estimate neutron capture rates, and these estimates agreed to within ∼40% or better with measurements. The ability to identify 136Xe(n, γ) events will allow for rejection of 137Xe backgrounds in future 0νββ analyses.

We present the results of the study of the contact binary system BO CVn. We have obtained physical parameters of the components based on combined analysis of new, multi-color light curves and spectroscopic mass ratio. This is the first time the latter has been determined for this object. We derived the contact configuration for the system with a very high filling factor of about 88 percent. We were able to reproduce the observed light curve, namely the flat bottom of the secondary minimum, only if a third light has been added into the list of free parameters. The resulting third light contribution is significant, about 20-24 percent, while the absolute parameters of components are: M1=1.16, M2=0.39, R1=1.62 and R2=1.00 (in solar units). The O-C diagram shows an upward parabola which, under the conservative mass transfer assumption, would correspond to a mass transfer rate of dM/dt = 6.3 \times 10-8M\odot/yr, matter being transferred from the less massive component to the more massive one. No cyclic, short-period variations have been found in the O-C diagram (but longer-term variations remain a possibility), 16 pages, 5 figures, 5 tables, accepted for publication by New Astronomy

The SciBooNE and MiniBooNE collaborations report the results of a νμ disappearance search in the Δ'm2 region of 0.5-40 eV2. The neutrino rate as measured by the SciBooNE tracking detectors is used to constrain the rate at the MiniBooNE Cherenkov detector in the first joint analysis of data from both collaborations. Two separate analyses of the combined data samples set 90% confidence level (CL) limits on νμ disappearance in the 0.5-40 eV2 Δm2 region, with an improvement over previous experimental constraints between 10 and 30 eV2

The MiniBooNE experiment has prepared an almost pure beam of muon-neutrinos over an energy range of a few-hundred MeV to a few GeV with a sample of roughly one-million neutrino interactions. Detailed cross-section measurements have been performed spanning 89% of the total neutrino-interaction rate. Specifically, three single-pion production mechanisms have been measured in detail. These measurements are important for a myriad of reasons: Neutral-current neutral-pion production is an important background for electron-neutrino appearance searches, Charged-current charged-pion production is the single largest background for quasi-elastic scattering and also provides the purest sample of events at these energies, and charge-current neutral-pion production provides a pure measure of incoherent pion production. Each of these processes required custom event reconstructions due to the particulars of the final-state particles. In addition, the sample selections and analyses will be discussed in detail. Many single-pion cross-section measurements, and their possible implications will be presented.

BetaCage, a gaseous neon time-projection chamber, has been proposed as a viable screener for emitters of low-energy alphas and electrons to which commercial radioactivity counting techniques are insensitive. Using radiopure materials for construction, active and passive shielding from extrinsic backgrounds, large counting area and minimal detector mass, BetaCage will be able to achieve sensitivities of 10^(−5) counts keV^(−1) kg^(−1) day^(−1) in a few days of running time. We report on progress in prototype development work since the last meeting of this workshop.

The authors would like to acknowledge the support of Fermilab, the Department of Energy, and the National Science Foundation in the construction, operation, and data analysis of the Mini Booster Neutrino Experiment.

Using a high-statistics, high-purity sample of {nu}{sub {mu}-}induced charged current, charged pion events in mineral oil (CH{sub 2}), MiniBooNE reports a collection of interaction cross sections for this process. This includes measurements of the CC{pi}{sup +} cross section as a function of neutrino energy, as well as flux-averaged single- and double-differential cross sections of the energy and direction of both the final-state muon and pion. In addition, each of the single-differential cross sections are extracted as a function of neutrino energy to decouple the shape of the MiniBooNE energy spectrum from the results. In many cases, these cross sections are the first time such quantities have been measured on a nuclear target and in the 1 GeV energy range.

Two independent methods are employed to measure the neutrino flux of the anti-neutrino-mode beam observed by the MiniBooNE detector. The first method compares data to simulated event rates in a high purity $\numu$ induced charged-current single $\pip$ (CC1$\pip$) sample while the second exploits the difference between the angular distributions of muons created in $\numu$ and $\numub$ charged-current quasi-elastic (CCQE) interactions. The results from both analyses indicate the prediction of the neutrino flux component of the pre-dominately anti-neutrino beam is over-estimated - the CC1$\pip$ analysis indicates the predicted $\numu$ flux should be scaled by $0.76 \pm 0.11$, while the CCQE angular fit yields $0.65 \pm 0.23$. The energy spectrum of the flux prediction is checked by repeating the analyses in bins of reconstructed neutrino energy, and the results show that the spectral shape is well modeled. These analyses are a demonstration of techniques for measuring the neutrino contamination of anti-neutrino beams observed by future non-magnetized detectors., 15 pages, 7 figures, published in Physical Review D, latest version reflects changes from referee comments

We report a measurement of the flux-averaged neutral-current elastic differential cross section for neutrinos scattering on mineral oil (CH{sub 2}) as a function of four-momentum transferred squared, Q{sup 2}. It is obtained by measuring the kinematics of recoiling nucleons with kinetic energy greater than 50 MeV which are readily detected in MiniBooNE. This differential cross-section distribution is fit with fixed nucleon form factors apart from an axial mass M{sub A} that provides a best fit for M{sub A}=1.39{+-}0.11 GeV. Using the data from the charged-current neutrino interaction sample, a ratio of neutral-current to charged-current quasielastic cross sections as a function of Q{sup 2} has been measured. Additionally, single protons with kinetic energies above 350 MeV can be distinguished from neutrons and multiple nucleon events. Using this marker, the strange quark contribution to the neutral-current axial vector form factor at Q{sup 2}=0, {Delta}s, is found to be {Delta}s=0.08{+-}0.26.

The MiniBooNE experiment at Fermilab reports results from a search for {nu}{sub {mu}{yields}{nu}e} oscillations, using a data sample corresponding to 5.66x10{sup 20} protons on target. An excess of 20.9{+-}14.0 events is observed in the energy range 475

The MiniBooNE experiment at Fermilab reports results from a search for ¯ν_{μ}→¯ν_{e} oscillations, using a data sample corresponding to 5.66×10²⁰ protons on target. An excess of 20.9±14.0 events is observed in the energy range 475E_{ν}^{QE}1250 MeV, which, when constrained by the observed ¯ν_{μ} events, has a probability for consistency with the background-only hypothesis of 0.5%. On the other hand, fitting for ¯ν_{μ}→¯ν_{e} oscillations, the best-fit point has a χ² probability of 8.7%. The data are consistent with ¯ν_{μ}→¯ν_{e} oscillations in the 0.1 to 1.0 eV² Δm² range and with the evidence for antineutrino oscillations from the Liquid Scintillator Neutrino Detector at Los Alamos National Laboratory.