Quantifying annual variation in catchability for commercial and research fishing

Biomass indices, from commercial catch per unit of effort (CPUE) or random trawl surveys, are commonly used in fisheries stock assessments. Uncertainty in such indices, often ex-pressed as a coefficient of variation (CV), has two components: observation error, and annual variation in catchability. Only the former can be estimated directly. As a result, the CVs used for these indices either ignore the annual-variation component or assume a value for it (often implicitly). Two types of data for New Zealand stocks were examined: 48 sets of residuals and catchability estimates from stock assessments using either CPUE or trawl survey indices; and biomass estimates from 17 time series of trawl surveys with between 4 and 25 species per time series. These data show clear evidence of significant annual variation in catchability. With the trawl survey data, catchability was detectably extreme for many species in about one year in six. The assessment data suggest that this annual variability typically has a CV of about 0.2. For commercial CPUE the variability is slightly less, and a typical total CV (including both components) of 0.15 to 0.2. This is much less than the values of 0.3 to 0.35 that have commonly been assumed in New Zealand. Some estimates of catchability are shown to be implausible

Brownian motion of a charged particle driven internally by correlated noise

We give an exact solution to the generalized Langevin equation of motion of a charged Brownian particle in a uniform magnetic field that is driven internally by an exponentially-correlated stochastic force. A strong dissipation regime is described in which the ensemble-averaged fluctuations of the velocity exhibit transient oscillations that arise from memory effects. Also, we calculate generalized diffusion coefficients describing the transport of these particles and briefly discuss how they are affected by the magnetic field strength and correlation time. Our asymptotic results are extended to the general case of internal driving by correlated Gaussian stochastic forces with finite autocorrelation times.Comment: 10 pages, 4 figures with subfigures, RevTeX, v2: revise

Curriculum transformation with students as partners

8732142. That was my student ID as an undergraduate (now one of the authors). It was a number, not a name. It distinguished students from professors and all other teaching staff and, in a symbolic way, reminded us all of our firm place as students, as learners. There was a big power differential between students and teachers in the 1980s. What we learned was prescribed, transmitted and tested in implicit ways (no rubrics or marking criteria in those days) and rarely were our skills tested – just what we knew and could recall at a given time. Sometimes people say that teaching is an act. Indeed, sage on the stage suggests this precisely. But being a student is also an act. Students also assume roles and personas. If we want curriculum transformation, we seek to put a stop to acting – to engage students and staff in authentic learning. MIDAS is our curriculum transformation project in the Faculty of Engineering and Information Technology (FEIT) at UTS – More Innovative Design-Able Students. In MIDAS, we want students and teachers to be their authentic selves in a true teaching and learning partnership. MIDAS seeks mutual respect in people, not the fulfilment of roles. MIDAS doesn’t see students as numbers, but as partners, as people who can learn, contribute, inspire, teach and create … and it sees teachers as people who also learn, contribute, inspire, teach and creat

The orbits of the quadruple star system 88 Tau A from PHASES differential astrometry and radial velocity

We have used high precision differential astrometry from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) project and radial velocity measurements covering a time-span of 20 years to determine the orbital parameters of the 88 Tau A system. 88 Tau is a complex hierarchical multiple system comprising a total of six stars; we have studied the brightest 4, consisting of two short-period pairs orbiting each other with an 18-year period. We present the first orbital solution for one of the short-period pairs, and determine the masses of the components and distance to the system to the level of a few percent. In addition, our astrometric measurements allow us to make the first determination of the mutual inclinations of the orbits. We find that the sub-systems are not coplanar.Comment: Corrected Author Ordering; 12 Pages, Accepted for publication in Ap

The Phases Differential Astrometry Data Archive. IV. The Triple Star Systems 63 Gem A and HR 2896

Differential astrometry measurements from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) are used to constrain the astrometric orbit of the previously known ≾2 day subsystem in the triple system 63 Gem A and have detected a previously unknown two-year Keplerian wobble superimposed on the visual orbit of the much longer period (213 years) binary system HR 2896. 63 Gem A was already known to be triple from spectroscopic work, and absorption lines from all three stars can be identified and their individual Doppler shifts measured; new velocities for all three components are presented to aid in constraining the orbit and measuring the stellar masses. In fact, 63 Gem itself is a sextuple system: the hierarchical triple (Aa1-Aa2)-Ab (in which Aa1 and Aa2 orbit each other with a rapid period just under 2 days, and Ab orbits these every two years), plus three distant common proper motion companions. The very small astrometric perturbation caused by the inner pair in 63 Gem A stretches the limits of current astrometric capabilities, but PHASES observations are able to constrain the orientation of the orbit. The two bright stars comprising the HR 2896 long-period (213 year) system have a combined spectral type of K0III and the newly detected object's mass estimate places it in the regime of being an M dwarf. The motion of the stars are slow enough that their spectral features are always blended, preventing Doppler studies. The PHASES measurements and radial velocities (when available) have been combined with lower precision single-aperture measurements covering a much longer time frame (from eyepiece measurements, speckle interferometry, and adaptive optics) to improve the characterization of the long-period orbits in both binaries. The visual orbits of the short- and long-period systems are presented for both systems and used to calculate two possible values of the mutual inclinations between inner and outer orbits of 152° ± 12° or a less likely value of 31° ± 11° for 63 Gem A and 10.°2 ± 2.°4 or 171.°2 ± 2.°8 for HR 2896. The first is not coplanar, whereas the second is either nearly coplanar or anti-coplanar

Temperament theory and congregation studies: different types for different services?

Temperament theory and psychological type theory provide a tool for assessing and interpreting the profile of church congregations. In this study the profiles of the three congregations (Ns = 43, 110, 43) at one Anglican church (given the pseudonym of Holy Trinity Church) are situated against the normative profile generated by the congregations at 140 Anglican churches (N = 3302). The data demonstrate that normative profile attracts a high proportion of the Epimethean Temperament at 72%. The two morning services at Holy Trinity Church replicated the profile at 65% and 74%. The evening service, however, attracted a significantly lower proportion of the Epimethean Temperament (47%) with a corresponding significantly higher proportion of the Apollonian Temperament. These findings support the view that individual churches are able to offer diverse provisions that generate congregations with distinctively different psychological profiles