Participation in Civil Society Organizations (CSO) draws on and enriches social, cultural, and human capital. Social impacts of such participation as active citizenship are systemic and ‘ripple’ far beyond the immediate program outputs and outcomes. CSOs and the third sector as a whole must demonstrate and gage the difference they make in the social life of the broader community. This research offers a new approach to conceptualize CSO social impacts through an empirically derived model that accounts for the impacts of active citizenship for individuals, organizations, and the broader community. A conceptual model of systemic social impact is presented as it was developed through an exploratory study of a large Australian CSO using an abductive methodology combining focus groups and a survey. Considering the potential of the model that could account for impacts beyond program outputs and outcomes, we propose several propositions for future testing the conceptual model.

Voluntary assisted dying (VAD) is an end-of-life care option available to eligible Australians living with a terminal condition, though people living with dementia are typically ineligible to choose VAD as part of their end-of-life care. In order to develop equitable research-informed policy and practice, it is crucial to include the perspectives of all key stakeholders, including living experience experts whose voices are currently excluded from Australian VAD research. This study aims to capture the perspectives of people living with dementia by exploring their VAD-related needs and preferences. The study is grounded in a critical and phenomenological conceptual framework that prioritizes inclusive research design. Thirty-six people living with dementia in Australia self-selected to participate in an online survey. It found that the vast majority of participants wanted the option to access VAD themselves, and most wanted provisions for accessing VAD through advance care directives. Through open text responses, the participants expressed many concerns about potential end-of-life suffering and loss of dignity, with their VAD preferences often aligned with their wish to maintain autonomy and human rights. This is the first known Australian study to explore VAD from the perspective of people living with dementia, providing critical insights into their experiences as stakeholders in a highly contested policy and practice environment that is dominated by medico-legal voices. Centring on people living with dementia challenges misconceptions about their capacity to contribute to VAD research, demonstrating their importance as living experience experts and key stakeholders with clear needs and preferences for their end-of-life care.

An emendation in Euripides, Hecuba 1045.

Linkage fabrics are gaining in popularity and finding applications in architecture, aerospace, healthcare, and fashion because they can deliver materials with bespoke flexibility and strength through the geometric design of linkage nodes. In this article, we provide a perspective on linkage fabrics as a new class of programmable materials. We describe the theory and design principles of these linkage fabrics and show how they can be designed and simulated using digital tools, and fabricated using 3D printing. This digital approach overcomes a major obstacle to the adoption of these materials, namely their complexity. We show how simulation methods can be verified and calibrated through experimental testing. This perspective article also discusses design-led research challenges for linkage fabrics such as the development of wearable assistive devices for those with physical disabilities.

JWST is at the forefront of revolutionizing our comprehension of the high-redshift Universe, stretching the boundaries of galaxy detection. Yet, as we strive for a more comprehensive understanding of the high-redshift Universe, concerns arise about the consistency of early estimates of galaxy number density, their stellar masses, and physical properties.

Our study delves into the synergy of NIRCAM and MIRI in the Extended Groth Strip (EGS) field, unveiling insights into the characterization of approximately 300 galaxies at z > 3, including 30 MIRI-detected red massive galaxies selected as HST-dark/faint and Little Red Dots (LRDs). By providing constraints on rest-frame optical and near-infrared emission, MIRI allows for more accurate measurements of stellar mass and helps disentangle the contribution from star formation and AGN activity. Although MIRI data has minimal impact on overall photometric redshift accuracy, it is critical for reliable stellar mass determination, especially at the highest redshifts (z > 7). Excluding MIRI data can lead to overestimating stellar mass by up to 0.15 dex for the general population and 0.4-1 dex for LRDs. Besides, MIRI data significantly improve our ability to constrain the contribution of Active Galactic Nuclei (AGN) to the observed light. For red massive galaxies, or those with the longest NIRCam filters contaminated by strong emission lines, excluding MIRI data can lead to a substantial overestimation of the AGN fraction.

At energies approaching the Planck energy scale 1019GeV, several quantum-gravity theories predict that familiar concepts such as Lorentz (LIV) symmetry can be broken. Such extreme energies are currently unreachable by experiments on Earth, but for photons traveling over cosmological distances the accumulated deviations from the Lorentz symmetry may be measurable using the Cherenkov Telescope Array (CTA). To study the spectral hardening feature observed in some VHE gamma-ray blazars, we calculate the reduction of the EBL gamma-gamma opacity due to the existence of underdense regions along the line of sight to VHE -gamma ray sources and we compared with the possibility of a LIV signature. Considering the LIV effect, we found that the cosmic opacity for VHE-gamma rays with energy more than 10 TeV can be strongly reduced. I will further discuss the impact of LIV on the Compton scattering process, and how future CTA observations may open an exciting window on studies of the fundamental physics.

Detecting the seed black holes from which quasars formed is extremely challenging; however, those seeds that did not grow into supermassive should be found as intermediate-mass black holes (IMBHs) of 100 – 105 M⊙ in local dwarf galaxies. The use of deep multiwavelength surveys has revealed that a population of actively accreting IMBHs (low-mass AGN) exists in dwarf galaxies at least out to z ˜3. The black hole occupation fraction of these galaxies suggests that the early Universe seed black holes formed from direct collapse of gas, which is reinforced by the possible flattening of the black hole-galaxy scaling relations at the low-mass end. This scenario is however challenged by the finding that AGN feedback can have a strong impact on dwarf galaxies, which implies that low-mass AGN in dwarf galaxies might not be the untouched relics of the early seed black holes. This has important implications for seed black hole formation models.

We study the moderate-to-high radiative luminosity active galactic nuclei (HLAGN) within the VLA-COSMOS 3 GHz Large Project. The survey covers 2.6 square degrees centered on the COSMOS field with a 1σ sensitivity of 2.3 μJy/beam across the field. This provides the simultaneously largest and deepest radio continuum survey available to date with exquisite multi-wavelength coverage. The survey yields 10,830 radio sources with signal-to-noise ratios ≥5. A subsample of 1,604 HLAGN is analyzed here. These were selected via a combination of X-ray luminosity and mid-infrared colors. We derive luminosity functions for these AGN and constrain their cosmic evolution out to a redshift of z ∼ 6, for the first time decomposing the star formation and AGN contributions to the radio continuum emission in the AGN. We study the evolution of number density and luminosity density finding a peak at z ∼ 1.5 followed by a decrease out to a redshift z ∼ 6.

We study the interaction of relativistic jets with their environment, using 3-dimen- sional relativistic particle-in-cell simulations for two cases of jet composition: (i) electron-proton (e − − p +) and (ii) electron-positron (e ±) plasmas containing helical magnetic fields. We have performed simulations of “global” jets containing helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities such as the Weibel instability, the kinetic Kelvin-Helmholtz instability and the Mushroom instability. We have found that these kinetic instabilities are suppressed and new types of instabilities can grow. For the e − − p + jet, a recollimation-like instability occurs and jet electrons are strongly perturbed, whereas for the e ± jet, a recollimation-like instability occurs at early times followed by kinetic instability and the general structure is similar to a simulation without a helical magnetic field. We plan to perform further simulations using much larger systems to confirm these new findings.

In the outskirts of massive high-redshift radio galaxies, powerful radio-jets often interact with ambient warm Lyα-emitting gas. We present the discovery of luminous reservoirs of cold molecular gas in these environments, based on CO(1-0) observations with the Australia Telescope Compact Array. The CO-emission is aligned with the radio jets, and found tens of kpc outside the host galaxy. These molecular gas reservoirs have CO luminosities in the range of those found in submm-galaxies (L'CO ~ 4-9 × 1010 K km/s pc2), but they lack any near-infrared counterpart in deep Spitzer imaging. These results suggest that jet-triggered feedback takes place in the circum-galactic environment of high-z radio galaxies. We prefer the interpretation that the CO-emitting gas is formed when the propagating jets enrich, shock and cool pre-existing dusty halo gas. We further argue that sensitive low-surface-brightness CO observations, using radio interferometers in very compact array-configurations, are essential to study the role of the cold molecular medium in the outskirts of massive high-z galaxies.

We analyse the correlations between continuum properties and emission line equivalent widths of star-forming and narrow-line active galaxies from SDSS. We show that emission line strengths can be predicted reasonably well from PCA coefficients of the stellar continuum using local multiple linear regression. Since upcoming sky surveys will make broadband observations only, theoretical modelling of spectra will be essential to estimate physical properties of galaxies. Combined with stellar population synthesis models, our technique will help generate more accurate model spectra and mock catalogues of galaxies to be used to fit data from new surveys. We also show that, by combining PCA coefficients from the pure continuum and the emission lines, a plausible distinction can be made between weak AGNs and quiescent star-forming galaxies. Our method uses a support vector machine, and allows a more refined separation of active and star-forming galaxies than the empirical curve of Kauffmann et al. (2003).

We selected and studied 180 pairs with d V < 800 km s−1 and Dp < 60 kpc containing Markarian (MRK) galaxies to investigate the dependence of galaxies integral parameters, star-formation (SF) and active galactic nuclei (AGN) properties on kinematics of pairs, their structure and large-scale environments. Projected radial separation Dp and perturbation level P are better measures of interaction strength than dV. The latter correlates with the density of large-scale environment and with the morphologies of galaxies. Both galaxies in a pair are of the same nature, the only difference is that MRK galaxies are usually brighter than their neighbors. Specific star formation rates (SSFR) of galaxies in pairs with smaller Dp or d V is in average 0.5 dex higher than that of galaxies in pairs with larger Dp or d V. Closeness of a neighbor with the same and later morphological type increases the SSFR, while earlier-type neighbors do not increase SSFR. Major interactions/mergers trigger SF and AGN more effectively than minor ones. The fraction of AGNs is higher in more perturbed pairs and pairs with smaller Dp. AGNs typically are in stronger interacting systems than star-forming and passive galaxies. There are correlations of both SSFRs and spectral properties of nuclei between pair members.