Defining the Social Dimension of Triple Bottom Line for the Australian Dairy Industry: Challenges, Priorities and Opportunities

Understanding the social impact the dairy industry has on employees and local communities is part of Dairy Australia’s commitment to the Triple Bottom Line (TBL) framework, which emphasises that businesses have social, environmental and economic impacts and responsibilities. This social impact assessment project, currently underway, aims to identify and quantify the social value of the dairy industry, whilst proactively identifying areas for improvements. Through an online survey for employees and a random postal survey of 15,000 dairy community residents, the project investigates how Australians perceive the Dairy Industry, as well as their wellbeing, quality of life, community involvement and work experiences. This paper provides an overview of the study, outlining why developing quantifiable indicators for the social dimension of TBL that are designed to be as rigorous as current financial reporting is a business priority. Examples of how the findings will contribute to the identification and management of issues, measures of industry sustainability and future strategy are discussed

The ‘Art’ of Copyright: A Practitioner’s Perspective

This is the 31st Manges lecture, and I am honored to be the first private practitioner to deliver it. Copyright law is rich in its constitutional and legislative heritage, in its doctrinal underpinnings, and in its interplay with other important legal and social regimes and norms. This complex heritage has been honored—and its contours provocatively discussed—by prior Manges lecturers spanning the federal judiciary, members of Congress, three Registers of Copyright, numerous scholars in the field—including Bob Gorman, and international copyright experts, among others. An important dimension of this copyright matrix not yet explored in this setting is the central role practicing attorneys have played in the continuing evolution of copyright law. Whereas the pace of legislative change in copyright law is glacial, its evolution via court decision and evolving commercial practice is continual. And it is the practicing bar: who are confronted with myriad real world, time sensitive applications of this body of law; who create the factual records and who brief and argue the legal issues that undergird judicial decisions in the field; who negotiate complex license agreements in reliance on understandings of copyright law with broad consequences for the dissemination of works of creative expression; and who, like Horace Manges, represent the spectrum of affected parties and industries in the halls of Congress, before the Copyright Office, Justice Department, Office of the Solicitor General, and other relevant federal agencies on all matters relating to copyright. Not limited to copyright, those of us in private practice tend to take our cases— and usually our clients—as we find them. In my own experience, applied to the copyright sphere, this intellectual flexibility has had enormous advantages. I say this because, to be effective counselors and advocates, copyright practitioners need fully to appreciate the balancing act that is copyright law. *This is a transcript of the 31st Annual Horace S. Manges Lecture delivered by R. Bruce Rich on March 26, 2018. Mr. Rich is a senior partner at Weil, Gotshal & Manges LLP and currently co-heads the firm’s Intellectual Property/Media practice

A Consent Theory of Unconscionability: An Empirical Study of Law in Action

This Article provides the findings of an empirical study of 187 court cases in which the issue of the unconscionability of a contract or a contract term was addressed by the courts. The cases were drawn from two time periods. The first set of cases can be viewed as the first generation of Uniform Commercial Code (U.C.C.)-style unconscionability cases from 1968-1980. The second generation of unconscionability cases were from the time period of 1991-2003. The two groups of cases allow us to not only analyze a series of questions and factors, but also to make intergenerational or longitudinal observations. The analysis is directed at answering four questions: (1) What are the standards used by courts in making unconscionability decisions?, (2) What type of evidence is considered by courts in making their decisions?, (3) What are the operative facts or factors that are most predictive of unconscionability decisions?, and (4) How do these findings inform us on the doctrine of unconscionability both as to its reflection in the law (expressed doctrine) and in application (law in fact)

HI Power Spectra and the Turbulent ISM of Dwarf Irregular Galaxies

HI spatial power spectra (PS) were determined for a sample of 24 nearby dwarf irregular galaxies selected from the LITTLE THINGS (Local Irregulars That Trace Luminosity Extremes - The HI Nearby Galaxy Survey) sample. The two-dimensional (2D) power spectral indices asymptotically become a constant for each galaxy when a significant part of the line profile is integrated. For narrow channel maps, the PS become shallower as the channel width decreases, and this shallowing trend continues to our single channel maps. This implies that even the highest velocity resolution of 1.8 km/s is not smaller than the thermal dispersion of the coolest, widespread HI component. The one-dimensional PS of azimuthal profiles at different radii suggest that the shallower PS for narrower channel width is mainly contributed by the inner disks, which indicates that the inner disks have proportionally more cooler HI than the outer disks. Galaxies with lower luminosity (M_B > -14.5 mag) and star formation rate (SFR, log(SFR (M\odot/yr)) < -2.1) tend to have steeper PS, which implies that the HI line-of-sight depths can be comparable with the radial length scales in low mass galaxies. A lack of a correlation between the inertial-range spectral indices and SFR surface density implies that either non-stellar power sources are playing a fundamental role in driving the interstellar medium (ISM) turbulent structure, or the nonlinear development of turbulent structures has little to do with the driving sources.Comment: 16 pages, 9 figures, 2 tables. Accepted by Ap

The Stellar and Gas Kinematics of the LITTLE THINGS Dwarf Irregular Galaxy NGC 1569

In order to understand the formation and evolution of dIm galaxies, one needs to understand their three-dimensional structure. We present measurements of the stellar velocity dispersion in NGC 1569, a nearby post-starburst dIm galaxy. The stellar vertical velocity dispersion, $\sigma_{\rm z}$, coupled with the maximum rotational velocity derived from \ion{H}{1} observations, $V_{\rm max}$, gives a measure of how kinematically hot the galaxy is, and, therefore, indicates its structure. We conclude that the stars in NGC 1569 are in a thick disk with a $V_{\rm max} / \sigma_{\rm z}$ = 2.4 $\pm$ 0.7. In addition to the structure, we analyze the ionized gas kinematics from \ion{O}{3} observations along the morphological major axis. These data show evidence for outflow from the inner starburst region and a potential expanding shell near supermassive star cluster (SSC) A. When compared to the stellar kinematics, the velocity dispersion of the stars increase in the region of SSC A supporting the hypothesis of an expanding shell. The stellar kinematics closely follow the motion of the gas. Analysis of high resolution \ion{H}{1} data clearly reveals the presence of an \ion{H}{1} cloud that appears to be impacting the eastern edge of NGC 1569. Also, an ultra-dense \ion{H}{1} cloud can be seen extending to the west of the impacting \ion{H}{1} cloud. This dense cloud is likely the remains of a dense \ion{H}{1} bridge that extended through what is now the central starburst area. The impacting \ion{H}{1} cloud was the catalyst for the starburst, thus turning the dense gas into stars over a short timescale, $\sim$ 1 Gyr. We performed a careful study of the spectral energy distribution using infrared, optical, and ultraviolet photometry producing a state-of-the-art mass model for the stellar disk. This mass modeling shows that stars dominate the gravitational potential in the inner 1 kpc.Comment: 49 pages, 25 figures, accepted in A