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BackgroundFire simulators are increasingly used to predict fire spread. Australian fire agencies have been concerned at not having an objective basis to choose simulators for this purpose.AimsWe evaluated wildland fire simulators currently used in Australia: Australis, Phoenix, Prometheus and Spark. The evaluation results are outlined here, together with the evaluation framework.MethodsSpatial metrics and visual aids were designed in consultation with simulator end-users to assess simulator performance. Simulations were compared against observations of fire progression data from 10 Australian historical fire case studies. For each case, baseline simulations were produced using as inputs fire ignition and fuel data together with gridded weather forecasts available at the time of the fire. Perturbed simulations supplemented baseline simulations to explore simulator sensitivity to input uncertainty.Key resultsEach simulator showed strengths and weaknesses. Some simulators displayed greater sensitivity to different parameters under certain conditions.ConclusionsNo simulator was clearly superior to others. The evaluation framework developed can facilitate future assessment of Australian fire simulators.ImplicationsCollection of fire behaviour observations for routine simulator evaluation using this framework would benefit future simulator development.

Star formation in the Galactic disc is primarily controlled by gravity, turbulence, and magnetic fields. It is not clear that this also applies to star formation near the Galactic Centre. Here we determine the turbulence and star formation in the CMZ cloud G0.253+0.016. Using maps of 3 mm dust emission and HNCO intensity-weighted velocity obtained with ALMA, we measure the volume-density variance σρ /ρ 0=1.3±0.5 and turbulent Mach number $\\mathcal{M}$ = 11±3. Combining these with turbulence simulations to constrain the plasma β = 0.34±0.35, we reconstruct the turbulence driving parameter b=0.22±0.12 in G0.253+0.016. This low value of b indicates solenoidal (divergence-free) driving of the turbulence in G0.253+0.016. By contrast, typical clouds in the Milky Way disc and spiral arms have a significant compressive (curl-free) driving component (b > 0.4). We speculate that shear causes the solenoidal driving in G0.253+0.016 and show that this may reduce the star formation rate by a factor of 7 compared to nearby clouds.

We have produced human alpha1-antitrypsin (A1AT), a major therapeutic protein, in genetically engineered tobacco plastids. Four different expression vectors have been evaluated which encode A1AT under the control of various 5' and 3' plastid expression elements. The use of heterologous promoter and terminator sequences derived from the corn and soybean plastid genomes leads to simpler and predictable recombinant genome patterns, avoiding unwanted recombination products between introduced and resident tobacco sequences. High level expression of unglycosylated A1AT, representing up to 2% of total soluble proteins, has been measured in leaves of transgenic tobacco lines. Some heterogeneity in the recombinant A1AT is detected after 2D protein separation, but the chloroplast-made protease inhibitors are fully active and bind to porcine pancreatic elastase.

Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) with gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic data set, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets. Instead, we suggest that breakout of a wide-angle, mildly relativistic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed radio and x-ray emission. We posit that all neutron star mergers may lead to a wide-angle cocoon breakout, sometimes accompanied by a successful jet and sometimes by a choked jet.

The polluter-pays principle requires States to take any actions that may be necessary to ensure that polluters bear the full environmental and social costs of their activities. One step to implement this principle is the development of regulations on environmental Civil Liability. The adoption of the UN-ECE Protocol on Civil Liability and Compensation for Damage caused by the Transboundary Effects of Industrial Accidents on Transboundary Waters (Kiev Protocol) in May 2003 was the result of a three-year negotiation process undertaken in the aftermath of the Baia Mare accident in Romania. The accident caused transboundary water pollution in the downstream countries Hungary and Yugoslavia. Owing to the absence of applicable liability rules, no compensation was ever paid for the damage caused by the pollution. The Cartagena Protocol on Biosafety mandates the Parties to establish rules and procedures in the field of liability and redress. Here there is likely to be a longer negotiation process before an agreed regime on liability and redress for damage arising from the use of living modified organisms (LMOs) becomes available, owing to the complexity and the particularities of gene technology.

Outflow activity is associated with all stages of early stellar evolution, from deeply embedded protostellar objects to visible young stars. Herbig-Haro (HH) objects are the optical manifestations of this powerful mass loss. Analysis of HH flows, and in particular of the subset of highly collimated HH jets, provides indirect but important insights into the nature of the accretion and mass-loss processes that govern the formation of stars. The recent recognition that HH flows may attain parsec-scale dimensions opens up the possibility of partially reconstructing the mass-ejection history of the newly born driving sources and, therefore, their mass-accretion history. Furthermore, HH flows are astrophysical laboratories for the analysis of shock structures, of hydrodynamics in collimated flows, and of their interaction with the surrounding environment. HH flows may be an important source of turbulence in molecular clouds. Recent technological developments have enabled detailed observations of outflows from young stars at near-infrared, mid-infrared, submillimeter, millimeter, and centimeter wavelengths, providing a comprehensive picture of the outflow phenomenon of young stars.

Nicotiana benthamiana is an invaluable model plant and biotechnology platform with a ~3 Gb allotetraploid genome. To further improve its usefulness and versatility, we have produced high-quality chromosome-level genome assemblies, coupled with transcriptome, epigenome, microRNA and transposable element datasets, for the ubiquitously used LAB strain and a related wild accession, QLD. In addition, single nucleotide polymorphism maps have been produced for a further two laboratory strains and four wild accessions. Despite the loss of five chromosomes from the ancestral tetraploid, expansion of intergenic regions, widespread segmental allopolyploidy, advanced diploidization and evidence of recent bursts of Copia pseudovirus (Copia) mobility not seen in other Nicotiana genomes, the two subgenomes of N. benthamiana show large regions of synteny across the Solanaceae. LAB and QLD have many genetic, metabolic and phenotypic differences, including disparate RNA interference responses, but are highly interfertile and amenable to genome editing and both transient and stable transformation. The LAB/QLD combination has the potential to be as useful as the Columbia-0/Landsberg errecta partnership, utilized from the early pioneering days of Arabidopsis genomics to today.Chromosome-level genome reference sequence assemblies of the model and biofactory Nicotiana benthamiana line, and a wild relative, have been generated and annotated for gene models, tissue-specific transcriptomes, microRNAs and epigenetic landscapes.

The inner few hundred parsecs of the Milky Way, the Central Molecular Zone (CMZ), is our closest laboratory for understanding star formation in the extreme environments (hot, dense, turbulent gas) that once dominated the universe. We present an update on the first large-area survey to expose the sites of star formation across the CMZ at high-resolution in submillimeter wavelengths: the CMZoom survey with the Submillimeter Array (SMA). We identify the locations of dense cores and search for signatures of embedded star formation. CMZoom is a three-year survey in its final year and is mapping out the highest column density regions of the CMZ in dust continuum and a variety of spectral lines around 1.3 mm. CMZoom combines SMA compact and subcompact configurations with single-dish data from BGPS and the APEX telescope, achieving an angular resolution of about 4″ (0.2 pc) and good image fidelity up to large spatial scales.

FEEDBACK is a SOFIA (Stratospheric Observatory for Infrared Astronomy) legacy program dedicated to study the interaction of massive stars with their environment. It performs a survey of 11 galactic high mass star-forming regions in the 158 m (1.9 THz) line of [C ii] and the 63 m (4.7 THz) line of [O i]. We employ the 14 pixel Low Frequency Array and 7 pixel High Frequency Array upGREAT heterodyne instrument to spectrally resolve (0.24 MHz) these far-infrared fine structure lines. With a total observing time of 96h, we will cover ∼6700 arcmin2 at 14 1) angular resolution for the [C ii] line and 6 3 for the [O i] line. The observations started in spring 2019 (Cycle 7). Our aim is to understand the dynamics in regions dominated by different feedback processes from massive stars such as stellar winds, thermal expansion, and radiation pressure, and to quantify the mechanical energy injection and radiative heating efficiency. This is an important science topic because feedback of massive stars on their environment regulates the physical conditions and sets the emission characteristics in the interstellar medium (ISM), influences the star formation activity through molecular cloud dissolution and compression processes, and drives the evolution of the ISM in galaxies. The [C ii] line provides the kinematics of the gas and is one of the dominant cooling lines of gas for low to moderate densities and UV fields. The [O i] line traces warm and high-density gas, excited in photodissociations regions with a strong UV field or by shocks. The source sample spans a broad range in stellar characteristics from single OB stars, to small groups of O stars, to rich young stellar clusters, to ministarburst complexes. It contains well-known targets such as Aquila, the Cygnus X region, M16, M17, NGC7538, NGC6334, Vela, and W43 as well as a selection of H ii region bubbles, namely RCW49, RCW79, and RCW120. These [C ii] maps, together with the less explored [O i] 63 m line, provide an outstanding database for the community. They will be made publically available and will trigger further studies and follow-up observations.

The environment within the inner few hundred parsecs of the Milky Way, known as the “Central Molecular Zone” (CMZ), harbours densities and pressures orders of magnitude higher than the Galactic Disc; akin to that at the peak of cosmic star formation (Kruijssen & Longmore 2013). Previous studies have shown that current theoretical star-formation models under-predict the observed level of star-formation (SF) in the CMZ by an order of magnitude given the large reservoir of dense gas it contains. Here we explore potential reasons for this apparent dearth of star formation activity.