396 research outputs found
The Role and Responsibility of the Public
It\u27s the title of the conference—the court of public opinion—and the topic of this panel. Professor Christopher Schroeder of Duke Law School is joined by media and public policy professor Kim Gross, senior attorney for the Institute for Justice Scott Bullock, and litigation director of the ACLU Steve Shapiro to contemplate both the influence of the media on public opinion and ways to use the media as an advocacy tool.
Gross discusses her research into the influence of media coverage on the public, followed by Bullock and Shapiro who explain the ways in which public interest law may choose to incorporate a media strategy into a larger legal battle. Questions/themes/discussion topics Media framing How media coverage can influence public opinion Factors that influence the media\u27s power How the Duke lacrosse case differs from typical crime coverage Legal strategies of public interest organizations Winning in the court of law, but losing in the court of public opinion Losing in the court of law, but winning in the court of public opinio
Power spectrum of the SDSS luminous red galaxies: constraints on cosmological parameters
In this paper we determine the constraints on cosmological parameters using
the CMB data from the WMAP experiment together with the recent power spectrum
measurement of the SDSS Luminous Red Galaxies (LRGs). Specifically, we focus on
spatially flat, low matter density models with adiabatic Gaussian initial
conditions. The spatial flatness is achieved with an additional quintessence
component whose equation of state parameter w_eff is taken to be independent of
redshift. Throughout most of the paper we do not allow any massive neutrino
contribution and also the influence of the gravitational waves on the CMB is
taken to be negligible. The analysis is carried out separately for two cases:
(i) using the acoustic scale measurements as presented in H\"utsi (2006), (ii)
using the full SDSS LRG power spectrum and its covariance matrix. We are able
to obtain a very tight constraint on the Hubble constant: H_0 = 70.8
^{+2.1}_{-2.0} km/s/Mpc, which helps in breaking several degeneracies between
the parameters and allows us to determine the low redshift expansion law with
much higher accuracy than available from the WMAP + HST data alone. The
positive deceleration parameter q_0 is found to be ruled out at 5.5 \sigma
confidence level. Finally, we extend our analysis by investigating the effects
of relaxing the assumption of spatial flatness and also allow for a
contribution from massive neutrinos.Comment: Final version accepted in A&A, added analysis for the models with
massive neutrinos and non-flat spatial geometrie
BLAST: Correlations in the Cosmic Far-Infrared Background at 250, 350, and 500 microns Reveal Clustering of Star-Forming Galaxies
We detect correlations in the cosmic far-infrared background due to the
clustering of star-forming galaxies in observations made with the Balloon-borne
Large Aperture Submillimeter Telescope, BLAST, at 250, 350, and 500 microns. We
perform jackknife and other tests to confirm the reality of the signal. The
measured correlations are well fit by a power law over scales of 5-25
arcminutes, with Delta I/I = 15.1 +/- 1.7%. We adopt a specific model for
submillimeter sources in which the contribution to clustering comes from
sources in the redshift ranges 1.3 <= z <= 2.2, 1.5 <= z <= 2.7, and 1.7 <= z
<= 3.2, at 250, 350, and 500 microns, respectively. With these distributions,
our measurement of the power spectrum, P(k_theta), corresponds to linear bias
parameters, b = 3.8 +/- 0.6, 3.9 +/- 0.6 and 4.4 +/- 0.7, respectively. We
further interpret the results in terms of the halo model, and find that at the
smaller scales, the simplest halo model fails to fit our results. One way to
improve the fit is to increase the radius at which dark matter halos are
artificially truncated in the model, which is equivalent to having some
star-forming galaxies at z >= 1 located in the outskirts of groups and
clusters. In the context of this model we find a minimum halo mass required to
host a galaxy is log (M_min / M_sun) = 11.5 (+0.4/-0.1), and we derive
effective biases $b_eff = 2.2 +/- 0.2, 2.4 +/- 0.2, and 2.6 +/- 0.2, and
effective masses log (M_eff / M_sun) = 12.9 +/- 0.3, 12.8 +/- 0.2, and 12.7 +/-
0.2, at 250, 350, and 500 microns, corresponding to spatial correlation lengths
of r_0 = 4.9, 5.0, and 5.2 +/- 0.7 h^-1 Mpc, respectively. Finally, we discuss
implications for clustering measurement strategies with Herschel and Planck.Comment: Accepted for publication in the Astrophysical Journal. Maps and other
results available at http://blastexperiment.info
Effect of early vasopressin vs norepinephrine on kidney failure in patients with septic shock. The VANISH Randomized Clinical Trial
IMPORTANCE: Norepinephrine is currently recommended as the first-line vasopressor in septic shock; however, early vasopressin use has been proposed as an alternative. OBJECTIVE: To compare the effect of early vasopressin vs norepinephrine on kidney failure in patients with septic shock. DESIGN, SETTING, AND PARTICIPANTS: A factorial (2×2), double-blind, randomized clinical trial conducted in 18 general adult intensive care units in the United Kingdom between February 2013 and May 2015, enrolling adult patients who had septic shock requiring vasopressors despite fluid resuscitation within a maximum of 6 hours after the onset of shock. INTERVENTIONS: Patients were randomly allocated to vasopressin (titrated up to 0.06 U/min) and hydrocortisone (n = 101), vasopressin and placebo (n = 104), norepinephrine and hydrocortisone (n = 101), or norepinephrine and placebo (n = 103). MAIN OUTCOMES AND MEASURES: The primary outcome was kidney failure-free days during the 28-day period after randomization, measured as (1) the proportion of patients who never developed kidney failure and (2) median number of days alive and free of kidney failure for patients who did not survive, who experienced kidney failure, or both. Rates of renal replacement therapy, mortality, and serious adverse events were secondary outcomes. RESULTS: A total of 409 patients (median age, 66 years; men, 58.2%) were included in the study, with a median time to study drug administration of 3.5 hours after diagnosis of shock. The number of survivors who never developed kidney failure was 94 of 165 patients (57.0%) in the vasopressin group and 93 of 157 patients (59.2%) in the norepinephrine group (difference, -2.3% [95% CI, -13.0% to 8.5%]). The median number of kidney failure-free days for patients who did not survive, who experienced kidney failure, or both was 9 days (interquartile range [IQR], 1 to -24) in the vasopressin group and 13 days (IQR, 1 to -25) in the norepinephrine group (difference, -4 days [95% CI, -11 to 5]). There was less use of renal replacement therapy in the vasopressin group than in the norepinephrine group (25.4% for vasopressin vs 35.3% for norepinephrine; difference, -9.9% [95% CI, -19.3% to -0.6%]). There was no significant difference in mortality rates between groups. In total, 22 of 205 patients (10.7%) had a serious adverse event in the vasopressin group vs 17 of 204 patients (8.3%) in the norepinephrine group (difference, 2.5% [95% CI, -3.3% to 8.2%]). CONCLUSIONS AND RELEVANCE: Among adults with septic shock, the early use of vasopressin compared with norepinephrine did not improve the number of kidney failure-free days. Although these findings do not support the use of vasopressin to replace norepinephrine as initial treatment in this situation, the confidence interval included a potential clinically important benefit for vasopressin, and larger trials may be warranted to assess this further. TRIAL REGISTRATION: clinicaltrials.gov Identifier: ISRCTN 20769191
Clustering of sub-millimeter galaxies in a self-regulated baryon collapse model
We have investigated the Cosmic Infrared Background (CIB) anisotropies in the
framework of the physical evolutionary model for proto-spheroidal galaxies by
Granato et al. (2004). After having re-calibrated the cumulative flux function
at m using the available determinations of the
shot noise amplitude (the original model already correctly reproduces it at
shorter wavelengths) the CIB power spectra at wavelengths from m to
mm measured by {\it Planck}, {\it Herschel}, SPT and ACT experiments have
been fitted using the halo model with only 2 free parameters, the minimum halo
mass and the power-law index of the mean occupation function of satellite
galaxies. The best-fit {\it minimum} halo mass is , higher than, but consistent within the errors, with the
estimate by Amblard et al. (2011) and close to the estimate by Planck
Collaboration (2011). The redshift evolution of the volume emissivity of
galaxies yielded by the model is found to be consistent with that inferred from
the data. The derived {\it effective} halo mass, , of sub-millimeter galaxies is close to that
estimated for the most efficient star-formers at the same redshift. The
effective bias factor and the comoving clustering radius at yielded
by the model are substantially lower than those found for a model whereby the
star formation is fueled by steady gas accretion, but substantially higher than
those found for a merging-driven galaxy evolution with a top-heavy initial mass
function.Comment: 9 pages, 4 figure
(In)formalization and the civilizing process : applying the work of Norbert Elias to housing-based anti-social behaviour interventions in the UK
This paper uses Norbert Elias's theory of the civilizing process to examine trends in social conduct in the UK and to identify how problematic “anti‐social” behaviour is conceptualized and governed through housing‐based mechanisms of intervention. The paper describes how Elias's concepts of the formalization and informalization of conduct and the construction of established and outsider groups provide an analytical framework for understanding social relations. It continues by discussing how de‐civilizing processes are also evident in contemporary society, and are applied to current policy discourse around Respect and anti‐social behaviour. The paper uses the governance of “anti‐social” conduct through housing mechanisms in the UK to critique the work of Elias and concludes by arguing that a revised concept of the civilizing process provides a useful analytical framework for future studies
Primordial Black Holes: sirens of the early Universe
Primordial Black Holes (PBHs) are, typically light, black holes which can
form in the early Universe. There are a number of formation mechanisms,
including the collapse of large density perturbations, cosmic string loops and
bubble collisions. The number of PBHs formed is tightly constrained by the
consequences of their evaporation and their lensing and dynamical effects.
Therefore PBHs are a powerful probe of the physics of the early Universe, in
particular models of inflation. They are also a potential cold dark matter
candidate.Comment: 21 pages. To be published in "Quantum Aspects of Black Holes", ed. X.
Calmet (Springer, 2014
Looking Good: Mediatisation and International NGOs
Many international NGOs value those parts of their work that are suited to media representation: campaigning, advocacy, projects that produce the right sort of images. In this article I make three points about this change. First, those parts of the NGO most reliant on media – such as the campaign desk – may be becoming more powerful. This can change the internal dynamics of NGOs. Second, the increasing use of media means that NGOs, like other organisations, hold themselves accountable in new ways. Third, NGOs may appear to look more and more like media organisations. These changes have received relatively little attention in the literature on NGOs, though they reflect a broader set of debates about the role of media in society. Using a case analysis of an international NGO, I suggest that the concept of mediatisation might be a useful way to understand some of the changes observed in the NGO sector
BIOSAFETY. Safeguarding gene drive experiments in the laboratory.
Multiple stringent confinement strategies should be used whenever possibleThis is the author accepted manuscript. The final version is available from AAAS via http://dx.doi.org/10.1126/science.aac793
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