Adsorption of uranyl to SWy-1 montmorillonite was evaluated experimentally and results were modeled to identify likely surface complexation reactions responsible for removal of uranyl from solution. Uranyl was contacted with SWy-1 montmorillonite in a NaCIO4 electrolyte solution at three ionic strengths (I = 0.001, 0.01, 0.1), at pH 4 to 8.5, in a N2(g) atmosphere. At low ionic strength, adsorption decreased from 95% at pH 4 to 75% at pH 6.8. At higher ionic strength, adsorption increased with pH from initial values less than 75%; adsorption edges for all ionic strengths coalesced above a pH of 7. A site-binding model was applied that treated SWy-1 as an aggregate of fixed-charge sites and edge sites analogous to gibbsite and silica. The concentration of fixed-charge sites was estimated as the cation exchange capacity, and non-preference exchange was assumed in calculating the contribution of fixed-charge sites to total uranyl adsorption. The concentration of edge sites was estimated by image analysis of transmission electron photomicrographs. Adsorption constants for uranyl binding to gibbsite and silica were determined by fitting to experimental data, and these adsorption constants were then used to simulate SWy-1 adsorption results. The best simulations were obtained with an ionization model in which AlOH2+ was the dominant aluminol surface species throughout the experimental range in pH. The pH-dependent aqueous speciation of uranyl was an important factor determining the magnitude of uranyl adsorption. At low ionic strength and low pH, adsorption by fixed-charge sites was predominant. The decrease in adsorption with increasing pH was caused by the formation of monovalent aqueous uranyl species, which were weakly bound to fixed-charge sites. At higher ionic strengths, competition with Na+ decreased the adsorption of UO22+ to fixed-charge sites. At higher pH, the most significant adsorption reactions were the binding of UO22+ to AlOH and of (UO2)3(OH)5+ to SiOH edge sites. Near-saturation of AlOH sites by UO22+ allowed significant contributions of SiOH sites to uranyl adsorption.

The term “blue justice” was coined in 2018 during the 3rd World Small-Scale Fisheries Congress. Since then, academic engagement with the concept has grown rapidly. This article reviews 5 years of blue justice scholarship and synthesizes some of the key perspectives, developments, and gaps. We then connect this literature to wider relevant debates by reviewing two key areas of research – first on blue injustices and second on grassroots resistance to these injustices. Much of the early scholarship on blue justice focused on injustices experienced by small-scale fishers in the context of the blue economy. In contrast, more recent writing and the empirical cases reviewed here suggest that intersecting forms of oppression render certain coastal individuals and groups vulnerable to blue injustices. These developments signal an expansion of the blue justice literature to a broader set of affected groups and underlying causes of injustice. Our review also suggests that while grassroots resistance efforts led by coastal communities have successfully stopped unfair exposure to environmental harms, preserved their livelihoods and ways of life, defended their culture and customary rights, renegotiated power distributions, and proposed alternative futures, these efforts have been underemphasized in the blue justice scholarship, and from marine and coastal literature more broadly. We conclude with some suggestions for understanding and supporting blue justice now and into the future.

This study investigated the influence of density and floor area on stress and the adaptation process of cats in animal shelters and boarding catteries. Sixty-three rescued cats were observed on 113 days in a shelter at group densities of 0.3-0.9 animals m−2. In addition, 49 rescued cats were observed during their first week after being admitted to a control group housed at a density of 0.5 or 0.8 animals m−2, and 44 boarding cats were observed in single cages of either 0.7 or 1.0 m2 floor area during their first week in a cattery.

Group density was highly correlated with the stress level of animals housed in groups. A stress level of ‘weakly tense ‘ was reached when the group density reached 0.6 animals m−2. During the first week of their stay, stress levels among cats which had been newly admitted to groups housed at 0.5 or 0.8 animals m−2 did not differ significantly. On days 1, 2 and 6 after admission, boarding cats housed in single cages with a floor area of 1.0m2 had significantly lower stress levels than animals in cages with a floor area of 0.7m2.

Group density was clearly shown to influence the adaptation process of cats which were housed for several weeks in groups. In order to avoid high stress levels, a group density of 0.6 animals m−2 should not be exceeded. However, the minimum spatial requirement for singly housed cats remains unknown.

For cats, appropriate housing conditions and a quick adjustment to new surroundings should be promoted during temporary stays in animal shelters and boarding catteries. In this study the development of stress in 140 boarding cats during a two-week stay under single-, pairand group-housing conditions in a boarding cattery was investigated and compared with the stress levels of 45 control cats which had been at the animal shelter for several weeks. Signs of stress were recorded by a non-invasive Cat-Stress-Score.

Overall, the levels of stress in boarding cats declined during the two weeks of boarding, with a pronounced decline in the first days, but did not reach the stress levels of the control group by the end of the second week of housing. In the second week, the average stress level of about one third of all boarding cats was rated higher than ‘weakly tense’ with 4 per cent of cats rated even higher than ‘very tense’. Neither housing style (single, paired or grouped) nor age had an influence on stress levels.

It was concluded that about two thirds of the boarding cats adjusted well to the boarding cattery during a two-week stay, while for the other third, temporary boarding was more stressful. For 4 per cent of the animals the two-week stay in a boarding cattery was classified as inappropriate because no reduction of their high stress levels occurred.

Single- and group-housing conditions for cats in animal shelters represent spatially and socially very different housing types. This study investigated whether the socialization of the cat towards conspecifics and people influences adaptation to these two housing types. Socialization towards conspecifics and people was determined in 169 rescued cats by means of two behavioural tests and a socialization questionnaire. Stress levels of the cats in the single- and group-housing condition were recorded by the non-invasive Cat-Stress-Score. Cats which were non-socialized towards conspecifics (n-SC) were more stressed than cats socialized towards conspecifics (SC) in the group enclosure. During the first hour and on days 6 and 7 in the observation cage, the n-SC were significantly less stressed under the single-than under the group-housing condition. The other members of the group had a higher stress level when a n-SC entered the group than if the new cat was a SC. Among the SC, there was no detectable difference in stress levels between the single-and group-housing condition. Cats which were non-socialized towards people (n-SP) were more stressed than cats socialized towards people (SP) during the whole stay under both single- and group-housing conditions.

It was concluded that n-SC should be held under single-housing conditions in animal shelters. For SC both the single- and group-housing condition are equally recommended for stays of a few weeks. For n-SP, stays in animal shelters should be avoided because of their high stress levels.

Ethological observations of the introduction of new charges into a large mixed-sex group in a dog shelter, and the later behaviour of the dogs in the run, were used to investigate a method of early assessment of the dogs’ reactions to the new situation. Subjects were divided qualitatively into four categories according to their interactional behaviour during the first two days (‘dog-oriented’, ‘human-oriented’, ‘dog & human friendly’, ‘asocial’). This classification was compared to an independent division resulting from statistical analysis of the dogs ‘ entry-sequences, and was found to be consistent for 80 per cent of dogs. One week after entry, both female and male dogs received distinctively fewer social interactions by conspecifics and tended to direct more interaction-initiating behaviour towards the keeper, thus demonstrating an integration process; females became more physically active and initiated significantly more interactions with other dogs; for males, the contrary was found. Qualitative comparison between first visitors and regular guests suggest that experienced dogs integrate faster, showing fewer behavioural signs of distress and engaging more often in investigatory behaviour. Results indicate that the assessment of dogs from their behaviour during the entry-sequence is a valid method to predict later tendencies. Males and females should be handled differently during introduction. The stress of entry into an existing group can therefore be reduced, improving the animals’ welfare.

What effect does political instability in the form of a potential secession from a political union have on business formation? Using newly collected data on business creation, we show that entrepreneurial activity in Ireland in the late nineteenth century was much lower than Scotland, and this divergence fluctuated over time. Several factors may have contributed to this, but we argue that political uncertainty about the prospect of a devolved government in Ireland played a role. The effects were most acute in the North of Ireland, the region that was most concerned by potential changes.

While unobscured and radio-quiet active galactic nuclei are regularly being found at redshifts $z > 6$ , their obscured and radio-loud counterparts remain elusive. We build upon our successful pilot study, presenting a new sample of low-frequency-selected candidate high-redshift radio galaxies (HzRGs) over a sky area 20 times larger. We have refined our selection technique, in which we select sources with curved radio spectra between 72–231 MHz from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey. In combination with the requirements that our GLEAM-selected HzRG candidates have compact radio morphologies and be undetected in near-infrared $K_{\rm s}$ -band imaging from the Visible and Infrared Survey Telescope for Astronomy Kilo-degree Infrared Galaxy (VIKING) survey, we find 51 new candidate HzRGs over a sky area of approximately $1200\ \mathrm{deg}^2$ . Our sample also includes two sources from the pilot study: the second-most distant radio galaxy currently known, at $z=5.55$ , with another source potentially at $z \sim 8$ . We present our refined selection technique and analyse the properties of the sample. We model the broadband radio spectra between 74 MHz and 9 GHz by supplementing the GLEAM data with both publicly available data and new observations from the Australia Telescope Compact Array at 5.5 and 9 GHz. In addition, deep $K_{\rm s}$ -band imaging from the High-Acuity Widefield K-band Imager (HAWK-I) on the Very Large Telescope and from the Southern Herschel Astrophysical Terahertz Large Area Survey Regions $K_{\rm s}$ -band Survey (SHARKS) is presented for five sources. We discuss the prospects of finding very distant radio galaxies in our sample, potentially within the epoch of reionisation at $z \gtrsim 6.5$ .

We present Hubble Space Telescope Wide Field Camera 3 photometric and grism observations of the candidate ultra-high-redshift ($z>7$) radio galaxy, GLEAM J0917–0012. This radio source was selected due to the curvature in its 70–230 MHz, low-frequency Murchison Widefield Array radio spectrum and its faintness in K-band. Follow-up spectroscopic observations of this source with the Jansky Very Large Array and Atacama Large Millimetre Array were inconclusive as to its redshift. Our F105W and F0986M imaging observations detect the host of GLEAM J0917–0012 and a companion galaxy, $\sim$ one arcsec away. The G102 grism observations reveal a single weak line in each of the spectra of the host and the companion. To help identify these lines we utilised several photometric redshift techniques including template fitting to the grism spectra, fitting the ultraviolet (UV)-to-radio photometry with galaxy templates plus a synchrotron model, fitting of the UV-to-near-infrared photometry with EAZY, and fitting the radio data alone with RAiSERed. For the host of GLEAM J0917–0012 we find a line at $1.12\,\mu$m and the UV-to-radio spectral energy distribution (SED) fitting favours solutions at $z\sim 2$ or $z\sim 8$. While this fitting shows a weak preference for the lower redshift solution, the models from the higher redshift solution are more consistent with the strength of the spectral line. The redshift constraint by RAiSERed of $>6.5$ also supports the interpretation that this line could be Lyman$-\alpha$ at $z=8.21$; however EAZY favours the $z\sim 2$ solution. We discuss the implications of both solutions. For the companion galaxy we find a line at $0.98\,\mu$m and the SED fitting favours solutions at $z<3$ implying that the line could be the [OII]$\lambda3727$ doublet at $z=1.63$ (although the EAZY solution is $z\sim 2.6\pm 0.5$). Further observations are still required to unambiguously determine the redshift of this intriguing candidate ultra-high-redshift radio galaxy.

The remnant phase of a radio galaxy begins when the jets launched from an active galactic nucleus are switched off. To study the fraction of radio galaxies in a remnant phase, we take advantage of a $8.31$ deg$^2$ subregion of the GAMA 23 field which comprises of surveys covering the frequency range 0.1–9 GHz. We present a sample of 104 radio galaxies compiled from observations conducted by the Murchison Widefield Array (216 MHz), the Australia Square Kilometer Array Pathfinder (887 MHz), and the Australia Telescope Compact Array (5.5 GHz). We adopt an ‘absent radio core’ criterion to identify 10 radio galaxies showing no evidence for an active nucleus. We classify these as new candidate remnant radio galaxies. Seven of these objects still display compact emitting regions within the lobes at 5.5 GHz; at this frequency the emission is short-lived, implying a recent jet switch off. On the other hand, only three show evidence of aged lobe plasma by the presence of an ultra-steep-spectrum ($\alpha<-1.2$) and a diffuse, low surface brightness radio morphology. The predominant fraction of young remnants is consistent with a rapid fading during the remnant phase. Within our sample of radio galaxies, our observations constrain the remnant fraction to $4\%\lesssim f_{\mathrm{rem}} \lesssim 10\%$; the lower limit comes from the limiting case in which all remnant candidates with hotspots are simply active radio galaxies with faint, undetected radio cores. Finally, we model the synchrotron spectrum arising from a hotspot to show they can persist for 5–10 Myr at 5.5 GHz after the jets switch of—radio emission arising from such hotspots can therefore be expected in an appreciable fraction of genuine remnants.

A new, variable phase contrast microscope, the PolanretTM, has been developed which is particularly suited to the optical screening of thin sections for electron microscopy with regard to tissue orientation and section quality.

By preliminary examination, defects in preparation of the specimen can be discovered immediately after sectioning and prior to staining or examination with the electron microscope. Such examination of unprocessed sections which are thinner than conventional light microscopy sections is possible because the Polanret TM system can make exceptionally small differences in optical path. Using the PolanretTM microscope, the phase and amplitude can be adjusted continuously so as to achieve optimum specimen contrast. The microscope can thus be used to visualize specimen defects and intracellular details in a way which conventional phase microscopy is unable to do.

This preliminary screening technique was evaluated for its usefulness in detecting microtome knife defects, i.e., scratches and chatter, so that corrective measures could be taken.

We present a detailed analysis of the radio galaxy PKS $2250{-}351$, a giant of 1.2 Mpc projected size, its host galaxy, and its environment. We use radio data from the Murchison Widefield Array, the upgraded Giant Metre-wavelength Radio Telescope, the Australian Square Kilometre Array Pathfinder, and the Australia Telescope Compact Array to model the jet power and age. Optical and IR data come from the Galaxy And Mass Assembly (GAMA) survey and provide information on the host galaxy and environment. GAMA spectroscopy confirms that PKS $2250{-}351$ lies at $z=0.2115$ in the irregular, and likely unrelaxed, cluster Abell 3936. We find its host is a massive, ‘red and dead’ elliptical galaxy with negligible star formation but with a highly obscured active galactic nucleus dominating the mid-IR emission. Assuming it lies on the local M–$\sigma$ relation, it has an Eddington accretion rate of $\lambda_{\rm EDD}\sim 0.014$. We find that the lobe-derived jet power (a time-averaged measure) is an order of magnitude greater than the hotspot-derived jet power (an instantaneous measure). We propose that over the lifetime of the observed radio emission (${\sim} 300\,$Myr), the accretion has switched from an inefficient advection-dominated mode to a thin disc efficient mode, consistent with the decrease in jet power. We also suggest that the asymmetric radio morphology is due to its environment, with the host of PKS $2250{-}351$ lying to the west of the densest concentration of galaxies in Abell 3936.