Temperature mapping study of United States distribution systems

The purpose of this one-year temperature mapping study was to determine the extreme temperatures and respective durations commercial pharmaceutical products are expected to be exposed to during routine ambient distribution within the continental United States. Extreme temperature conditions may affect the safety and efficacy of pharmaceutical products during distribution. Knowing the value and duration of the extreme temperatures that products are likely to experience in the ambient (uncontrolled) distribution environment allows for improved product degradation testing, optimized thermal package design and scientifically based determination as to when logistical and environmental controls should be used. Before this study, testing was performed using profiles provided by standards organizations. This study was designed to provide company specific data that may be used to design tests, validate, or modify existing test procedures throughout the organization. To achieve this, packages were shipped to selected locations across the United States from the company\u27s Eastern, Southern, and Western Distribution Centers (DCs) during peak summer and winter conditions. The packages were equipped with data logging instrumentation that recorded the temperature and the time-of-day. As a result of this project, the organization now has first hand knowledge of the expected extremes and durations within its United States distribution environment. This information is now in use for study design, logistical decision-making, and proving that appropriate testing has been performed to regulatory bodies

Sense about science - making sense of crime

Booklet 'Making Sense of Crime' published by registered charity 'Sense About Science'There’s always heated debate about crime in the media and a lot of political argument about how we should respond to it. But these arguments rarely provide insight into what actually causes crime, what lies behind trends over time and in different places, and how best to go about reducing it. Values inform how a society decides to deal with crime. We may decide that rehabilitation is a better principle than punishment, and this will influence how we decide what is most effective. However, we also expect these choices to be disciplined by sound evidence, because if crime policy ignores what works and what doesn’t, there are likely to be bad social consequences. And with over £10bn spent annually on tackling crime through the police, prisons, probation and courts, unless we look at evidence we can’t see how effective any of it is. Crime policy usually has twin aims – to prevent crime, and to seek justice by punishing those who commit offences. Research shows there’s only a loose link, if any, between the way offenders are punished and the number of offences committed. There is no reliable evidence for example, that capital punishment reduces serious crimes as its supporters claim. Yet politicians and commentators regularly claim that more punishments are a way to cut crime. Academic, government and community organisations have all said crime policies need to be based more on evidence, but much of the evidence available at the moment is poor or unclear. Debates about crime rarely reflect how strong the evidence behind opposing policies is, and even when politicians honestly believe they’re following the evidence, they tend to select evidence that supports their political views. This guide looks at some of the key things we do know and why it has been so difficult to make sense of crime policy. An important point throughout is that policymakers sometimes have to make decisions when things are not clear-cut. They have a better chance of making effective policies if they admit to this uncertainty – and conduct robust research to find out more. In the following pages we have shared insights from experts in violent crime, policing, crime science, psychology and the media’s influence on the crime debate. They don’t have all the answers, but we hope they leave you better-placed to hold policymakers and commentators to account and promote a more useful discussion about crime

The Low-Velocity, Rapidly Fading Type Ia Supernova 2002es

SN 2002es is a peculiar subluminous Type Ia supernova (SN Ia) with a combination of observed characteristics never before seen in a SN Ia. At maximum light, SN 2002es shares spectroscopic properties with the underluminous SN 1991bg subclass of SNe Ia, but with substantially lower expansion velocities (~6000 km/s) more typical of the SN 2002cx subclass. Photometrically, SN 2002es differs from both SN 1991bg-like and SN 2002cx-like supernovae. Although at maximum light it is subluminous (M_B=-17.78 mag), SN 2002es has a relatively broad light curve (Dm15(B)=1.28 +/- 0.04 mag), making it a significant outlier in the light-curve width vs. luminosity relationship. We estimate a 56Ni mass of 0.17 +/- 0.05 M_sun synthesized in the explosion, relatively low for a SN Ia. One month after maximum light, we find an unexpected plummet in the bolometric luminosity. The late-time decay of the light curves is inconsistent with our estimated 56Ni mass, indicating that either the light curve was not completely powered by 56Ni decay or the ejecta became optically thin to gamma-rays within a month after maximum light. The host galaxy is classified as an S0 galaxy with little to no star formation, indicating the progenitor of SN 2002es is likely from an old stellar population. We also present a less extensive dataset for SN 1999bh, an object which shares similar observed properties. Both objects were found as part of the Lick Observatory Supernova Search, allowing us to estimate that these objects should account for ~2.5% of SNe Ia within a fixed volume. We find that current theoretical models are unable to explain the observed of characteristics of SN 2002es.Comment: 19 pages, 15 figures, Submitted to Ap

Prospectus, September 22, 1982

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Understanding controls on biotic assemblages and ecological status in Zambian rivers for the development of sustainable monitoring protocols

We search for galaxies with a strong Balmer break (Balmer Break Galaxies; BBGs) at $z \sim 6$ over a 0.41 deg$^2$ effective area in the COSMOS field. Based on rich imaging data, including data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), three candidates are identified by their extremely red $K - [3.6]$ colors as well as by non-detection in X-ray, optical, far-infrared (FIR), and radio bands. The non-detection in the deep ALMA observations suggests that they are not dusty galaxies but BBGs at $z \sim 6$, although contamination from Active Galactic Nuclei (AGNs) at $z \sim 0$ cannot be completely ruled out for the moment. Our spectral energy distribution (SED) analyses reveal that the BBG candidates at $z \sim 6$ have stellar masses of $\approx 5 \times 10^{10} M_{\odot}$ dominated by old stellar populations with ages of $\gtrsim 700$ Myr. Assuming that all the three candidates are real BBGs at $z \sim 6$, we estimate the stellar mass density (SMD) to be $2.4^{+2.3}_{-1.3} \times 10^{4} M_{\odot}$ Mpc$^{-3}$. This is consistent with an extrapolation from the lower redshift measurements. The onset of star formation in the three BBG candidates is expected to be several hundred million years before the observed epoch of $z \sim 6$. We estimate the star-formation rate density (SFRD) contributed by progenitors of the BBGs to be 2.4 -- 12 $\times 10^{-5} M_{\odot}$ yr$^{-1}$Mpc$^{-3}$ at $z > 14$ (99.7\% confidence range). Our result suggests a smooth evolution of the SFRD beyond $z = 8$.Comment: 29 pages, 16 figures, 4 tables, accepted for publication in Ap

Balmer Break Galaxy Candidates at z ∼ 6: A Potential View on the Star Formation Activity at z ≳ 14

We search for galaxies with a strong Balmer break (Balmer break galaxies; BBGs) at z ~ 6 over a 0.41 deg² effective area in the COSMOS field. Based on rich imaging data, including data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), three candidates are identified by their extremely red K–[3.6] colors, as well as by nondetection in the X-ray, optical, far-infrared, and radio bands. The nondetection in the deep ALMA observations suggests that they are not dusty galaxies but BBGs at z ~ 6, although contamination from active galactic nuclei at z ~ 0 cannot be completely ruled out for the moment. Our spectral energy distribution analyses reveal that the BBG candidates at z ~ 6 have stellar masses of ≈5 × 10¹⁰ M_⊙ dominated by old stellar populations with ages of ≳ 700 Myr. Assuming that all three candidates are real BBGs at z ~ 6, we estimate the stellar mass density to be 2.4_(-1.3)^(+2.3) x {10⁴ M_⊙ Mpc⁻³. This is consistent with an extrapolation from the lower-redshift measurements. The onset of star formation in the three BBG candidates is expected to be several hundred million yr before the observed epoch of z ~ 6. We estimate the star formation rate density (SFRD) contributed by progenitors of the BBGs to be 2.4–12 × 10⁻⁵ M_⊙ yr⁻¹ Mpc⁻³ at z > 14 (99.7% confidence range). Our result suggests a smooth evolution of the SFRD beyond z = 8

Constraints on the Progenitor System of the Type Ia Supernova SN 2011fe/PTF11kly

Type Ia supernovae (SNe) serve as a fundamental pillar of modern cosmology, owing to their large luminosity and a well-defined relationship between light-curve shape and peak brightness. The precision distance measurements enabled by SNe Ia first revealed the accelerating expansion of the universe, now widely believed (though hardly understood) to require the presence of a mysterious "dark" energy. General consensus holds that Type Ia SNe result from thermonuclear explosions of a white dwarf (WD) in a binary system; however, little is known of the precise nature of the companion star and the physical properties of the progenitor system. Here we make use of extensive historical imaging obtained at the location of SN 2011fe/PTF11kly, the closest SN Ia discovered in the digital imaging era, to constrain the visible-light luminosity of the progenitor to be 10-100 times fainter than previous limits on other SN Ia progenitors. This directly rules out luminous red giants and the vast majority of helium stars as the mass-donating companion to the exploding white dwarf. Any evolved red companion must have been born with mass less than 3.5 times the mass of the Sun. These observations favour a scenario where the exploding WD of SN 2011fe/PTF11kly, accreted matter either from another WD, or by Roche-lobe overflow from a subgiant or main-sequence companion star.Comment: 22 pages, 6 figures, submitte