62 research outputs found

    An improved estimate of daily precipitation from the ERA5 reanalysis

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    Precipitation is an essential climate variable and a fundamental part of theglobal water cycle. Given its importance to society, precipitation is oftenassessed in climate monitoring activities, such as in those led by the Coperni-cus Climate Change Service (C3S). To undertake these activities, C3S predomi-nantly uses ERA5 reanalysis precipitation. Research has shown that short-range forecasts for precipitation made from this reanalysis can provide valu-able estimates of the actual (observed) precipitation in extratropical regionsbut can be less useful in the tropics. While some of these limitations will bereduced with future reanalyses because of the latest advancements, there ispotentially a more immediate way to improve the precipitation estimate.This is to use the precipitation modelled in the Four-Dimensional Variational(4D-Var) data assimilation window of the reanalysis, and it is the aim of thisstudy to evaluate this approach. Using observed 24-h precipitation accumula-tions at 5637 stations from 2001 to 2020, results show that smaller root-mean-square errors (RMSEs) and mean absolute errors are generally foundby using the ERA5 4D-Var precipitation. For example, for all available daysfrom 2001 to 2020, 87.5% of stations have smaller RMSEs. These improvementsare driven by reduced random errors in the 4D-Var precipitation because it isbetter constrained by observations, which are themselves sensitive to orinfluence precipitation. However, there are regions (e.g., Europe) where largerbiases occur, and via the decomposition of the Stable Equitable Error inProbability Space score, this is shown to be because the 4D-Var precipitationhas a wetter bias on ‘dry’ days than the standard ERA5 short-range forecasts.The findings also highlight that the 4D-Var precipitation does improve thediscrimination of ‘heavy’ observed events. In conclusion, an improved ERA5precipitation estimate is largely obtainable, and these results could proveuseful for C3S activities and for future reanalyses, including ERA

    Stars and brown dwarfs in the sigma Orionis cluster IV. IDS/INT and OSIRIS/GTC spectroscopy and Gaia DR2 astrometry

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    Context. Only a few open clusters are as important for the study of stellar and substellar objects, and their formation and evolution, as the young σ Orionis cluster. However, a complete spectroscopic characterisation of its whole stellar population is still missing. Aims. We filled most of that gap with a large spectroscopic and astrometric survey of targets towards σ Orionis. Eventually, it will be one of the open clusters with the lowest proportion of interlopers and the largest proportion of confirmed cluster members with known uncontrovertible youth features. Methods. We acquired 317 low-resolution optical spectra with the Intermediate Dispersion Spectrograph (IDS) at the 2.5 m Isaac Newton Telescope (INT) and the Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) at the 10.4 m Gran Telescopio Canarias (GTC). We measured equivalent widths of Li i, Hα, and other key lines from these spectra, and determined spectral types. We complemented this information with Gaia DR2 astrometric data and other features of youth (mid-infrared excess, X-ray emission) compiled with Virtual Observatory tools and from the literature. Results. Of the 168 observed targets, we determined for the first time spectral types of 39 stars and equivalent widths of Li i and Hα of 34 and 12 stars, respectively. We identified 11 close (ρ </≈ 3 arcsec) binaries resolved by Gaia, of which three are new, 14 strong accretors, of which four are new and another four have Hα emission shifted by over 120 km s^(−1) , two juvenile star candidates in the sparse population of the Ori OB1b association, and one spectroscopic binary candidate. Remarkably, we found 51 non-clustermembers, 35 of which were previously considered as σ Orionis members and taken into account in high-impact works on, for example, disc frequency and initial mass function
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