5,716 research outputs found
Electroconvulsive Therapy Practice Changes in Older Individuals Due to COVID-19: Expert Consensus Statement
© 2020 American Association for Geriatric Psychiatry The ubiquitous coronavirus 2019 (COVID-19) pandemic has required healthcare providers across all disciplines to rapidly adapt to public health guidelines to reduce risk while maintaining quality of care. Electroconvulsive therapy (ECT), which involves an aerosol-generating procedure from manual ventilation with a bag mask valve while under anesthesia, has undergone drastic practice changes in order to minimize disruption of treatment in the midst of COVID-19. In this paper, we provide a consensus statement on the clinical practice changes in ECT specific to older adults based on expert group discussions of ECT practitioners across the country and a systematic review of the literature. There is a universal consensus that ECT is an essential treatment of severe mental illness. In addition, there is a clear consensus on what modifications are imperative to ensure continued delivery of ECT in a manner that is safe for patients and Northwell Health, while maintaining the viability of ECT services. Approaches to modifications in ECT to address infection control, altered ECT procedures, and adjusting ECT operations are almost uniform across the globe. With modified ECT procedures, it is possible to continue to meet the needs of older patients while mitigating risk of transmission to this vulnerable population
Absorption-selected galaxies trace the low-mass, late-type, star-forming population at
We report on the stellar content, half-light radii and star formation rates
of a sample of 10 known high-redshift () galaxies selected on
strong neutral hydrogen (HI) absorption (log(N(HI)/cm) toward
background quasars. We use observations from the {\it Hubble Space Telescope}
(HST) Wide Field Camera 3 in three broad-band filters to study the spectral
energy distribution(SED) of the galaxies. Using careful quasar point spread
function subtraction, we study their galactic environments, and perform the
first systematic morphological characterisation of such absorption-selected
galaxies at high redshifts. Our analysis reveals complex, irregular hosts with
multiple star-forming clumps. At a spatial sampling of 0.067 arcsec per pixel
(corresponding to 0.55 kpc at the median redshift of our sample), 40% of our
sample requires multiple S\'ersic components for an accurate modelling of the
observed light distributions. Placed on the mass-size relation and the `main
sequence' of star-forming galaxies, we find that absorption-selected galaxies
at high redshift extend known relations determined from deep
luminosity-selected surveys to an order of magnitude lower stellar mass, with
objects primarily composed of star-forming, late-type galaxies. We measure
half-light radii in the range 0.4 to 2.6 kpc based on the
reddest band (F160W) to trace the oldest stellar populations, and stellar
masses in the range 8 to 10
derived from fits to the broad-band SED. Spectroscopic and SED-based star
formation rates are broadly consistent, and lie in the range log(SFR/Myr) 0.0 to 1.7.Comment: 17 pages, Accepted for publication in MNRAS. This revision has minor
text change
ALMA observations of a metal-rich damped Ly{\alpha} absorber at z = 2.5832: evidence for strong galactic winds in a galaxy group
We report on the results of a search for CO(3-2) emission from the galaxy
counterpart of a high-metallicity Damped Ly-alpha Absorber (DLA) at z=2.5832
towards the quasar Q0918+1636. We do not detect CO emission from the previously
identified DLA galaxy counterpart. The limit we infer on M_gas / M_star is in
the low end of the range found for DLA galaxies, but is still consistent with
what is found for other star-forming galaxies at similar redshifts. Instead we
detect CO(3-2) emission from another intensely star-forming galaxy at an impact
parameter of 117 kpc from the line-of-sight to the quasar and 131 km s^-1
redshifted relative to the velocity centroid of the DLA in the quasar spectrum.
In the velocity profile of the low- and high-ionisation absorption lines of the
DLA there is an absorption component consistent with the redshift of this
CO-emitting galaxy. It is plausible that this component is physically
associated with a strong outflow in the plane of the sky from the CO-emitting
galaxy. If true, this would be further evidence, in addition to what is already
known from studies of Lyman-break galaxies, that galactic outflows can be
traced beyond 100 kpc from star-forming galaxies. The case of this z=2.583
structure is an illustration of this in a group environment.Comment: 7 pages, 5 figures, accepted for publication in MNRA
Использование микроконтроллера ESP32 совместно с гироприборами MPU-6050 и BNO055 при создании самобалансирующих роботов
Статья посвящена анализу возможностей электронных приборов, таких как гироскоп, акселерометр, магнитометр. Приводятся результаты тестирования и действующие алгоритмы. Анализируются возможности их применения в разных вариантах расчетов. Делаются выводы по развитию возможностей и устранению недостатков полученной комплексной системы позиционирования робота
Constraints on a Massive Dirac Neutrino Model
We examine constraints on a simple neutrino model in which there are three
massless and three massive Dirac neutrinos and in which the left handed
neutrinos are linear combinations of doublet and singlet neutrinos. We examine
constraints from direct decays into heavy neutrinos, indirect effects on
electroweak parameters, and flavor changing processes. We combine these
constraints to examine the allowed mass range for the heavy neutrinos of each
of the three generations.Comment: latex, 29 pages, 7 figures (not included), MIT-CTP-221
Chandra spectroscopy of the hot star beta Crucis and the discovery of a pre-main-sequence companion
In order to test the O star wind-shock scenario for X-ray production in less
luminous stars with weaker winds, we made a pointed 74 ks observation of the
nearby early B giant, beta Cru (B0.5 III), with the Chandra HETGS. We find that
the X-ray spectrum is quite soft, with a dominant thermal component near 3
million K, and that the emission lines are resolved but quite narrow, with
half-widths of 150 km/s. The forbidden-to-intercombination line ratios of Ne IX
and Mg XI indicate that the hot plasma is distributed in the wind, rather than
confined near the photosphere. It is difficult to understand the X-ray data in
the context of the standard wind-shock paradigm for OB stars, primarily because
of the narrow lines, but also because of the high X-ray production efficiency.
A scenario in which the bulk of the outer wind is shock heated is broadly
consistent with the data, but not very well motivated theoretically. It is
possible that magnetic channeling could explain the X-ray properties, although
no field has been detected on beta Cru. We detected periodic variability in the
hard (hnu > 1 keV) X-rays, modulated on the known optical period of 4.58 hours,
which is the period of the primary beta Cep pulsation mode for this star. We
also have detected, for the first time, an apparent companion to beta Cru at a
projected separation of 4 arcsec. This companion was likely never seen in
optical images because of the presumed very high contrast between it and beta
Cru in the optical. However, the brightness contrast in the X-ray is only 3:1,
which is consistent with the companion being an X-ray active low-mass
pre-main-sequence star. The companion's X-ray spectrum is relatively hard and
variable, as would be expected from a post T Tauri star.Comment: Accepted for publication in MNRAS; 19 pages, 15 figures, some in
color; version with higher-resolution figures available at
http://astro.swarthmore.edu/~cohen/papers/bcru_mnras2008.pd
Synthesis, Characterization and Magnetic Susceptibility of the Heavy Fermion Transition Metal Oxide LiV_{2}O_{4}
The preparative method, characterization and magnetic susceptibility \chi
measurements versus temperature T of the heavy fermion transition metal oxide
LiV_{2}O_{4} are reported in detail. The intrinsic \chi(T) shows a nearly
T-independent behavior below ~ 30 K with a shallow broad maximum at about 16 K,
whereas Curie-Weiss-like behavior is observed above 50-100 K. Field-cooled and
zero-field-cooled magnetization M measurements in applied magnetic fields H =
10 to 100 G from 1.8 to 50 K showed no evidence for spin-glass ordering.
Crystalline electric field theory for an assumed cubic V point group symmetry
is found insufficient to describe the observed temperature variation of the
effective magnetic moment. The Kondo and Coqblin-Schrieffer models do not
describe the magnitude and T dependence of \chi with realistic parameters. In
the high T range, fits of \chi(T) by the predictions of high temperature series
expansion calculations provide estimates of the V-V antiferromagnetic exchange
coupling constant J/k_{B} ~ 20 K, g-factor g ~ 2 and the T-independent
susceptibility. Other possible models to describe the \chi(T) are discussed.
The paramagnetic impurities in the samples were characterized using isothermal
M(H) measurements with 0 < H <= 5.5 Tesla at 2 to 6 K. These impurities are
inferred to have spin S_{imp} ~ 3/2 to 4, g_{imp} ~ 2 and molar concentrations
of 0.01 to 0.8 %, depending on the sample.Comment: 19 typeset RevTeX pages, 16 eps figures included, uses epsf; to be
published in Phys. Rev.
PHASES High Precision Differential Astrometry of delta Equulei
delta Equulei is among the most well-studied nearby binary star systems.
Results of its observation have been applied to a wide range of fundamental
studies of binary systems and stellar astrophysics. It is widely used to
calibrate and constrain theoretical models of the physics of stars. We report
27 high precision differential astrometry measurements of delta Equulei from
the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES).
The median size of the minor axes of the uncertainty ellipses for these
measurements is 26 micro-arcseconds. These data are combined with previously
published radial velocity data and other previously published differential
astrometry measurements using other techniques to produce a combined model for
the system orbit. The distance to the system is determined to within a
twentieth of a parsec and the component masses are determined at the level of a
percent. The constraints on masses and distance are limited by the precisions
of the radial velocity data; we outline plans improve this deficiency and
discuss the outlook for further study of this binary.Comment: Accepted by AJ. Complete versions of tables 2-7 now available at
http://stuff.mit.edu/~matthew1/deltaEquTables/ (removed from astroph server
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