6 research outputs found
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A pilot fidelity study of Listen-Empathize-Agree-Partner (LEAP) with Assertive Community Treatment (ACT) mental health clinicians
The primary objective of this study was to examine clinicians' fidelity to a promising new clinical intervention known as Listen-Empathize-Agree-Partner (LEAP) that addresses issues of poor insight, therapeutic alliance, and treatment adherence prevalent in the schizophrenia population. A secondary purpose of this study was to assess the factor structure of a measure developed to examine the core principles of the LEAP method. Forty-eight mental health clinicians working in Assertive Community Treatment (ACT) programs randomized into intervention and control groups were assessed for fidelity to the LEAP method via the LEAP Fidelity Measure (LFM), a self-report instrument. Results revealed a three-factor structure of this measure which were labeled "Reflective Listening, Delaying and Opining," "Partnering on Shared Goals," and "Client-Centered Listening and Empathizing." Multivariate Analyses of Variance indicated that clinicians who were trained in LEAP had significantly higher levels of fidelity to the "Reflective Listening, Delaying and Opining" and "Partnering on Shared Goals" components than clinicians who were not trained in this method. There were no significant differences between the groups on the "Client-Centered Listening and Empathizing" component. Analyses did not reveal significant gender differences or effects based on years of general and specific ACT clinical experience between the two groups. However, in a post hoc analysis, a modest correlation between gender and fidelity to the "Client-Centered Listening and Empathizing" component showed that male clinicians tended to report higher fidelity to this specific set of interventions when compared to their female counterparts. These results are discussed within the context of feasibility in training and implementing LEAP in real-world community mental health clinical settings. Additionally, limitations of this study and implications for future research are discussed
Eccentricities of Double Neutron Star Binaries
Recent pulsar surveys have increased the number of observed double neutron
stars (DNS) in our galaxy enough so that observable trends in their properties
are starting to emerge. In particular, it has been noted that the majority of
DNS have eccentricities less than 0.3, which are surprisingly low for binaries
that survive a supernova explosion that we believe imparts a significant kick
to the neutron star. To investigate this trend, we generate many different
theoretical distributions of DNS eccentricities using Monte Carlo population
synthesis methods. We determine which eccentricity distributions are most
consistent with the observed sample of DNS binaries. In agreement with
Chaurasia & Bailes (2005), assuming all double neutron stars are equally as
probable to be discovered as binary pulsars, we find that highly eccentric,
coalescing DNS are less likely to be observed because of their accelerated
orbital evolution due to gravitational wave emission and possible early
mergers. Based on our results for coalescing DNS, we also find that models with
vanishingly or moderately small kicks (sigma < about 50 km/s) are inconsistent
with the current observed sample of such DNS. We discuss the implications of
our conclusions for DNS merger rate estimates of interest to ground-based
gravitational-wave interferometers. We find that, although orbital evolution
due to gravitational radiation affects the eccentricity distribution of the
observed sample, the associated upwards correction factor to merger rate
estimates is rather small (typically 10-40%).Comment: 9 pages, 8 figures, accepted by ApJ. Figures reduced and some content
changed, references adde
Searching for Gravitational Waves from the Inspiral of Precessing Binary Systems: Astrophysical Expectations and Detection Efficiency of "Spiky'' Templates
Relativistic spin-orbit and spin-spin couplings has been shown to modify the
gravitational waveforms expected from inspiraling binaries with a black hole
and a neutron star. As a result inspiral signals may be missed due to
significant losses in signal-to-noise ratio, if precession effects are ignored
in gravitational-wave searches. We examine the sensitivity of the anticipated
loss of signal-to-noise ratio on two factors: the accuracy of the precessing
waveforms adopted as the true signals and the expected distributions of
spin-orbit tilt angles, given the current understanding of their physical
origin. We find that the results obtained using signals generated by
approximate techniques are in good agreement with the ones obtained by
integrating the 2PN equations. This shows that a complete account of all
high-order post-Newtonian effects is usually not necessary for the
determination of detection efficiencies. Based on our current astrophysical
expectations, large tilt angles are not favored and as a result the decrease in
detection rate varies rather slowly with respect to the black hole spin
magnitude and is within 20--30% of the maximum possible values.Comment: 7 fig., accepted by Phys. Rev. D Minor modification
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Through-going Muons in the LUX Dark Matter Search
Dark matter makes up most of the mass of the universe, and yet the true nature of this mysterious substance remains unknown. The LUX experiment uses a detector consisting of target xenon nuclei to search for Weakly Interacting Massive Particles, a promising dark matter candidate. The LUX detector is a 370 kg dual-phase xenon time projection chamber. Incident radiation interacts with xenon atoms, resulting in a recoil nucleus or electron that causes both ionization and excitation of Xe along the recoil track. De-excitation of Xe results in the emission of 175 nm scintillation light, and the properties of this scintillation can be used to determine the nature of the incident radiation - possibly identifying WIMP dark matter.LUX has placed world-leading limits on the WIMP-nucleon interaction cross section. The rarity of such interactions requires a thorough understanding of backgrounds in order to implement appropriate background-reducing measures and an effective event-rejection methodology. The LUX water tank surrounds the xenon detector and serves as an active shield, reducing background radiation but also identifying high energy cosmic ray muons that can lead to the production of a highly undesirable neutron background. Since signals created by neutrons may appear very similar to those of WIMPs, care must be taken to not only reduce neutron backgrounds as much as possible, but to also understand any neutron backgrounds that may be present.The goal of this dissertation was to develop a method to identify cosmic ray muons that traverse both the LUX Xe detector and water tank, and to measure a muon flux at the LUX detector depth. The xenon gas-liquid interface served as a fiducial surface through which muon flux was measured. Simultaneous signals between Xe and water detectors were analyzed, and xenon pulse shapes were used to determine the energy and track geometry of the interaction. Muons passing the Xe liquid surface exhibited a particular signature in their pulse shape; this signature was used to identify through-going muons and calculate muon flux.In a previous work, muon flux measurements were taken at sites above the LUX detector, and muon transport models were used to predict vertical muon flux as 4.40 x 10^-9 muons s^-1 cm^-2 at the LUX detector depth. In this work, a flux of 4.60 +/- 0.33_(stat) x 10^-9 muons s^-1 cm^-2 is measured through the LUX water tank and xenon detector liquid surface. The resulting neutrons expected to be seen during the full LUX exposure is ~1 x 10^-1. While expected the background contribution from muon-induced neutrons poses little problem for the LUX WIMP search, an understanding of this background becomes increasingly important as target volumes grow for future generation experiments
Recommended from our members
Through-going Muons in the LUX Dark Matter Search
Dark matter makes up most of the mass of the universe, and yet the true nature of this mysterious substance remains unknown. The LUX experiment uses a detector consisting of target xenon nuclei to search for Weakly Interacting Massive Particles, a promising dark matter candidate. The LUX detector is a 370 kg dual-phase xenon time projection chamber. Incident radiation interacts with xenon atoms, resulting in a recoil nucleus or electron that causes both ionization and excitation of Xe along the recoil track. De-excitation of Xe results in the emission of 175 nm scintillation light, and the properties of this scintillation can be used to determine the nature of the incident radiation - possibly identifying WIMP dark matter.LUX has placed world-leading limits on the WIMP-nucleon interaction cross section. The rarity of such interactions requires a thorough understanding of backgrounds in order to implement appropriate background-reducing measures and an effective event-rejection methodology. The LUX water tank surrounds the xenon detector and serves as an active shield, reducing background radiation but also identifying high energy cosmic ray muons that can lead to the production of a highly undesirable neutron background. Since signals created by neutrons may appear very similar to those of WIMPs, care must be taken to not only reduce neutron backgrounds as much as possible, but to also understand any neutron backgrounds that may be present.The goal of this dissertation was to develop a method to identify cosmic ray muons that traverse both the LUX Xe detector and water tank, and to measure a muon flux at the LUX detector depth. The xenon gas-liquid interface served as a fiducial surface through which muon flux was measured. Simultaneous signals between Xe and water detectors were analyzed, and xenon pulse shapes were used to determine the energy and track geometry of the interaction. Muons passing the Xe liquid surface exhibited a particular signature in their pulse shape; this signature was used to identify through-going muons and calculate muon flux.In a previous work, muon flux measurements were taken at sites above the LUX detector, and muon transport models were used to predict vertical muon flux as 4.40 x 10^-9 muons s^-1 cm^-2 at the LUX detector depth. In this work, a flux of 4.60 +/- 0.33_(stat) x 10^-9 muons s^-1 cm^-2 is measured through the LUX water tank and xenon detector liquid surface. The resulting neutrons expected to be seen during the full LUX exposure is ~1 x 10^-1. While expected the background contribution from muon-induced neutrons poses little problem for the LUX WIMP search, an understanding of this background becomes increasingly important as target volumes grow for future generation experiments