Improving phenotyping in winter barley cultivars towards waterlogging tolerance by combining field trials under natural conditions with controlled growth condition experiments

Additional rainfall in Northern Europe due to global climate change is increasing the incidences of field flooding. Flooding causes hypoxic stress that results in a reduced capacity for photosynthesis, reduction in nutrient availability and uptake, increased production of toxic metabolites by anaerobic bacteria in the soil, and ultimately yield losses and crop death. To overcome hypoxic environmental conditions, new cultivars need to be bred and tested for waterlogging tolerance. We scored 403 winter barley cultivars from the ‘Association Genetics of UK Elite Barley’ (AGOUEB) population, taking advantage of the phenotypic changes associated with hypoxic stress. This enabled us to identify an initial set of waterlogging sensitive and tolerant cultivars. Comparative analysis of a subset of 65 cultivars exposed to waterlogging stress under field and growth cabinet environments showed variability in scores due to varying sensitivity to waterlogging over multi-season field trials. In field trials, we observed waterlogging damage resulting in reductions in biomass, grain yield and crop height. However, the effects varied between seasons and the severity of waterlogging due to differences in the topography of the field and the amount of rainfall. To overcome the seasonal variations in environmental conditions in multi-season field trials, we developed in parallel, an enhanced phenotyping method by complementing field experiments with phenotyping under controlled growth conditions. The phenotyping scoring method allows for the grouping of cultivars by sensitivity and tolerance to waterlogging, with limited variance between cultivars scored in the field and controlled conditions. Together, these two complementary approaches maximise the data available to breeders, allowing for the reliable selection of more tolerant cultivars able to grow under flooding conditions

On the properties of the massive binary black hole merger GW170729

International audienceWe present a detailed investigation into the properties of GW170729, the gravitational wave with the most massive and distant source confirmed to date. We employ an extensive set of waveform models, including new improved models that incorporate the effect of higher-order waveform modes which are particularly important for massive systems. We find no indication of spin-precession, but the inclusion of higher-order modes in the models results in an improved estimate for the mass ratio of (0.3–0.8) at the 90% credible level. Our updated measurement excludes equal masses at that level. We also find that models with higher-order modes lead to the data being more consistent with a smaller effective spin, with the probability that the effective spin is greater than zero being reduced from 99% to 94%. The 90% credible interval for the effective spin parameter is now (-0.01-0.50). Additionally, the recovered signal-to-noise ratio increases by ∼0.3 units compared to analyses without higher-order modes; the overall Bayes factor in favor of the presence of higher-order modes in the data is 5.1∶1. We study the effect of common spin priors on the derived spin and mass measurements, and observe small shifts in the spins, while the masses remain unaffected. We argue that our conclusions are robust against systematic errors in the waveform models. We also compare the above waveform-based analysis which employs compact-binary waveform models to a more flexible wavelet- and chirplet-based analysis. We find consistency between the two, with overlaps of ∼0.9, typical of what is expected from simulations of signals similar to GW170729, confirming that the data are well-described by the existing waveform models. Finally, we study the possibility that the primary component of GW170729 was the remnant of a past merger of two black holes and find this scenario to be indistinguishable from the standard formation scenario

Search for intermediate-mass black hole binaries in the third observing run of Advanced LIGO and Advanced Virgo

International audienceIntermediate-mass black holes (IMBHs) span the approximate mass range 100−105 M⊙, between black holes (BHs) that formed by stellar collapse and the supermassive BHs at the centers of galaxies. Mergers of IMBH binaries are the most energetic gravitational-wave sources accessible by the terrestrial detector network. Searches of the first two observing runs of Advanced LIGO and Advanced Virgo did not yield any significant IMBH binary signals. In the third observing run (O3), the increased network sensitivity enabled the detection of GW190521, a signal consistent with a binary merger of mass ∼150 M⊙ providing direct evidence of IMBH formation. Here, we report on a dedicated search of O3 data for further IMBH binary mergers, combining both modeled (matched filter) and model-independent search methods. We find some marginal candidates, but none are sufficiently significant to indicate detection of further IMBH mergers. We quantify the sensitivity of the individual search methods and of the combined search using a suite of IMBH binary signals obtained via numerical relativity, including the effects of spins misaligned with the binary orbital axis, and present the resulting upper limits on astrophysical merger rates. Our most stringent limit is for equal mass and aligned spin BH binary of total mass 200 M⊙ and effective aligned spin 0.8 at 0.056 Gpc−3 yr−1 (90% confidence), a factor of 3.5 more constraining than previous LIGO-Virgo limits. We also update the estimated rate of mergers similar to GW190521 to 0.08 Gpc−3 yr−1.Key words: gravitational waves / stars: black holes / black hole physicsCorresponding author: W. Del Pozzo, e-mail: [email protected]† Deceased, August 2020