dataesr/scientific-paragraphs-categorization huggingface dataset:
The data presented in this article can be consulted online (see Data Availability Statement). They represent natural conditions closely while providing the measurement detail currently only possible in the laboratory. Thus, apart from providing physical insights, they may be of particular interest for the further development of (process-based) numerical models. manuscript. The experiments described in this work were funded by the European Community's Horizon 2020 Programme through the grant to the budget of the Integrated Infrastructure Initiative HYDRALAB+, Contract 654110, and were conducted as part of the transnational access project RESIST. FG acknowledges funding from the Agency for Management of University and Research Grants (AGAUR). DH acknowledges funding from the French DGA funded ANR ASTRID Maturation project MESURE (ANR-16-ASMA-0005-01).
Study design and participants We conducted a multicentre, parallel-group, analyst-blinded RCT to explore the effectiveness of a stepped-care programme versus enhanced care as usual (eCAU) among HCWs with psychological distress. The trial protocol was prospectively registered on 28 July 2021 (identifier NCT04980326) and described in detail elsewhere  24  (online supplemental file 1). After recruitment started, the Project Executive Board agreed to modify the criterion for completing the interventions (see the Statistical analysis section), which modified one of the prespecified secondary analyses (per-protocol analysis). These changes did not affect our primary intention-to-treat (ITT) analysis. Our target population consisted of HCWs employed by the Department of Health. All participants provided written informed consent, and none was paid for taking part in the study.
Assessment of safety and adverse events Local project managers monitored suicidal thoughts across assessment points by including the following items in the outcomes list: 'Since the last assessment (about two months ago), have you seriously considered or have plans to end your life?' Similarly, local project managers and intervention providers registered any serious adverse event reported by the participants and informed the independent RESPOND (Preparedness of health systems to reduce mental health and psychosocial concerns resulting from the COVID-19 pandemic) Ethics and Data Advisory Board, chaired by Dr Sonja Rutten.
Statistical analysis Overview Our broad aim was to explore the effect of the intervention on mental health outcomes. We used linear and logistic mixed models with robust SEs to estimate the treatment effect at t 2 , t 3 and t 4. All models included both the randomisation group and the outcome score measured at baseline as fixed effects and allowed for an individual random intercept for each participant. We did not impute missing data. We analysed the stepped-care programme as a single intervention (regardless of whether the participant steps up to PM+ or finishes the intervention after the DWM). All statistical analyses were performed in Madrid and independently replicated in Barcelona using R (main packages: lme4, emmeans, clubSandwich and genodds). The statistical analysis protocol  24  and the full analytical code (https://github.
FINDINGS We randomised 232 participants between 3 November 2021 and 31 March 2022, all of whom were included in the ITT analysis (see figure  1 ). Participants included 200 women (86%) with a mean age of 37. 5 years (SD 10. 3). Most (n=215, 93%) were or had been involved in the direct care of patients with COVID-19, and more than half (n=137, 59%) had been infected with COVID-19. Most participants reported symptoms compatible with a probable diagnosis of major depressive disorder (n=124, 53%) or a probable diagnosis of an anxiety disorder (n=134, 58%) (see table  1 ). Three in four participants stepped up to PM+ (n=86, 75%). Recruitment stopped when the target sample size was achieved. At the end of our follow-up period (31 August 2022), data were available for 184 participants (79. 3%), and the overall decrease in anxiety and depression symptoms at the primary endpoint (t 4 ) was larger in the intervention arm compared with the eCAU (baseline-adjusted mean difference 4.
Second, we covered a relatively short follow-up period of 21 weeks. Although the effects of cognitive-behavioural therapies often persist over time, this still poses a major challenge for psychological treatments research,  39  and we do not know whether our positive effects would decrease with longer follow-up periods. Third, we collected all outcomes using self-reports, which increases the probability of social desirability effects. In light of the barriers to conducting inperson assessments and/or collecting objective data during the COVID-19 pandemic, self-reports may have still been the most feasible method to answer our main research question. 40 Fourth, although we measured PTSD symptoms, we are not sure about the actual exposure of our sample to traumatic events, which hinders the interpretation of our findings.
Eclipses unveil stratospheric turbidity The brightness of the Moon during eclipse is highly sensitive to aerosol abundance in the stratosphere. Dark total lunar eclipses indicate high turbidity, whereas a ruddy disk signifies a clear stratosphere  18, 19. To reconstruct past stratospheric turbidity across the Medieval Climate Anomaly to Little Ice Age transition, we comprehensively reexamined a large corpus of historical sources (Supplementary Dataset S1) written in the twelfth and thirteenth centuries, in search of credible lunar eclipse observations (Fig. 1 ). In China and Korea, lunar eclipses were recorded by official astronomers and preserved in sources such as the astronomical treatises and five-elements treatises of official dynastic histories, whereas Japanese eclipse observations are found in more diverse writings such as the diaries of courtiers, chronicles or temple records.
In Europe, annals and chronicles from monasteries and towns represent the main sources. In Arabic sources, lunar eclipse observations are frequently found in universal chronicles  20. According to the latest catalogues of lunar eclipses  21, 22  , 64 (Europe), 59 (Middle East) and 64 (East Asia) total lunar eclipses occurred and would have been visible, weather permitting, between 1100 and 1300 ce. A total of 180 European, 10 Middle Eastern and 199 East Asian accounts describe 51, 7 and 61 individual total lunar eclipses, respectively. In Europe, although 12 individual eclipses are described in only one surviving source, many are corroborated in several accounts, up to 16 in the case of the eclipse of 11 February 1161 ce (Supplementary Dataset S1). This success in finding observations of retro-calculated eclipses for Europe (80%; Extended Data Table  1 ) is notable and comparable with that of later periods for which documentation is more abundant  16, 17  (for example, 82%, 1665-1881 ce).
It ranges from L = 0 (very dark) to L = 4 (very bright copper-red or orange eclipse). Of the 37 total lunar eclipses with brightness recorded in Eurasian sources, only six were rated L = 0, emphasizing the rarity and significance of such observations (Fig. 2a  and Supplementary Dataset S1). These events occurred on the night of 5-6 May 1110 ce, 12-13 January 1172 ce, 2-3 December 1229 ce, 18-19 May 1258 ce, 12-13 November 1258 ce and 22-23 November 1276 ce. All testimonies are reported in Supplementary Dataset S1, with each description stressing a near-complete and prolonged disappearance of the lunar disk. One of the most outstanding accounts was retrieved from Japanese sources and pertains to the total lunar eclipse of 2 December 1229 ce. Although Asian sources rarely detail coloration  20, 29  , the Meigetsuki (明月記, The Record of the Bright Moon) written by Fujiwara no Teika (藤原定家, 1162-1241 ce) reports an extremely dark lunar eclipse despite clear weather.
The Meigetsuki notes that the coloration of the Moon was deemed so unusual that the astronomers expressed fear over its appearance: "Regarding the recent total lunar eclipse, although on previous occasions there has been totality, the old folk had never seen it like this time, with the location of the disk of the Moon not visible, just as if it had disappeared during the eclipse. Moreover, the duration was very long, and the change was extreme. It was truly something to fear. Indeed, in my seventy years I have never heard of or seen [such a thing]; the official astronomers spoke of it fearfully […]" (Fig. 1c  and Supplementary Dataset S1). All the dark (L = 0) lunar eclipses-in May 1110 ce, January 1172 ce, December 1229 ce, May 1258 ce, November 1258 ce and November 1276 ce-are contemporary with five of the seven largest HMP volcanic sulfate signals recorded in polar ice cores (UE1, UE2, UE4, Samalas and UE5; Fig.
Timing of HMP eruptions We constrained the timing of HMP eruptions by developing a four-step procedure that integrates evidence from our eclipse record, global aerosol simulations, modern satellite observations and tree-ring reconstructions (see Methods and Extended Data Fig. 1 ). 7] [18] [19]  , which showed that, for 46 well-observed lunar eclipses between 1880-1888 ce and 1960-2001 ce, dark total lunar eclipses (L = 0) only occurred when SAOD exceeded about 0. 1. Next, drawing on observations for the 1883 Krakatau and 1991 Pinatubo eruptions (from the Sato/GISS and GloSSAC v2 datasets)  37, 38  , SAOD simulations  39  (from the eVolv2k datasets for UE1 to UE6 and both the circa 1257 ce Samalas and 1815 ce Tambora eruptions) and IPSL-CM5A-LR  40  climate model outputs (for Samalas and Tambora), we evaluated the post-eruptive duration of elevated stratospheric turbidity, that is, SAOD ≥ 0.
Then, to provide further constraint on the timing of each HMP eruption, we evaluated independently dated Northern Hemisphere tree-ring-based summer temperature reconstructions for post-volcanic climatic response (Sch2015 (ref. 41 ), N-TREND2015 (ref. 42 ), NVOLC v2 (ref. 7 )). Taking UE2 (Fig. 3a ) as an example, combining the dark lunar eclipse date of January 1172 ce with the eVolv2k, Sato/GISS and GloSSAC v2 datasets, we find a high to very high probability that the event occurred between July 1170 and October 1171 ce (Fig. 3b ). The peak cooling observed in Sch2015 and NVOLC v2 in summer 1172 ce reduces the likelihood of an eruption occurring between summer 1170 and autumn 1171 ce (Fig. 3c ); we thus bracket the eruption date between May and August 1171 ce (Fig. 3d ). We similarly constrain the probable time windows of other large HMP events to Northern Hemisphere winter 1108/1109 ce (UE1; Extended Data Fig.
Stratospheric or tropospheric aerosols? Stratospheric aerosols profoundly affect the brightness and coloration of the eclipsed Moon by reducing the transmission of sunlight into the Earth's umbra  18, 19. Here we use lunar eclipse coloration to distinguish between tropospheric and stratospheric aerosol veils (see Methods). The dark lunar eclipses observed after UE1, UE2, UE4, Samalas and UE5 indicate stratospheric aerosol veils (Fig. 4 ), consistent with Δ 33 S isotope records from Dome C, Antarctica 3. Although UE3 (circa 1182 ce) registers as the second greatest Northern Hemispheric extratropical eruption of the last millennium in terms of ice-core sulfate deposition  4  (second only to Laki 1783-1784 ce), the reddish lunar eclipse of 11 December 1182 ce (Fig. 2a ) points to a comparatively low stratospheric aerosol burden, while tree-ring reconstructions show limited cooling (Supplementary Dataset S2).
Further consideration of eclipse coloration, in conjunction with tree-ring-based summer temperature reconstructions, suggests that for four HMP eruptions associated with lesser VSSI around 1127, 1210, 1222 and 1262 ce, sulfate aerosols were mostly confined to the troposphere and any climatic impacts were limited (Fig. 4  and Supplementary Dataset S2). The nature and timing of UE6 remain enigmatic (Fig. 4 ). A bipolar sulfate deposition distribution is observed around 1286 ce, implying a tropical eruption, whereas sulfur isotopic analysis suggests that the associated Antarctic deposition was stratospheric in origin  20. However, the reddish lunar eclipse of 22 October 1287 ce (Fig. 2a ), described in three independent records (Supplementary Dataset S1) from England and Italy, precludes substantial Northern Hemisphere stratospheric aerosol presence at this time.
Implications Our identification of marked stratospheric dust veils in 1110, 1172, 1229, 1258 and 1276 ce using contemporary observations of dark total lunar eclipses corroborates the general accuracy of the revised ice-core chronologies for Greenland (NS1-2011) and Antarctica (WD2014), while adding precision to the chronological framework of HMP eruptions. Given the inherent uncertainties in ice-core chronologies, our dataset of precisely dated dark total lunar eclipses offers a new, reliable and independent suite of chronological tie points that can complement established age markers in 536, 774/5, 939, 993/4, 1258, 1601 and 1816 ce to aid future chronology development. Our findings also suggest that five other events, likely associated with tropospheric-only aerosol veils, had a limited impact on climate.
Investigation of historical sources and development of a lunar eclipse database European and Middle Eastern lunar eclipse observations. We extensively reexamined hundreds of annals and chronicles, written in the twelfth and thirteenth centuries ce, searching for references to lunar eclipses. For Europe, contemporary sources are mostly accessible in compilations of medieval texts edited in the series of the (1) Monumenta Germaniae Historica, (2) Rerum Britannicarum Medii AEvi, (3) Recueil des historiens des Gaules et de la France and (4) Rerum Italicarum Scriptores. Descriptions or observations of lunar eclipses originate from across Europe, namely, Austria, the Czech Republic, England, France, Germany, Iceland, Italy, Sweden and Switzerland. In a few instances, lunar obscurations were observed in the Middle East by Christians engaged in the Crusades.
These chronicles were found in the Recueil des historiens des croisades, edited and published in the nineteenth century. Most sources consulted were composed by monks or clerics and, to a lesser extent, by urban laymen. Nearly all were composed in Latin, although the vernacular was occasionally used. Furthermore, we included observations retrieved from Ukrainian and Russian chronicles in our database  51. We also examined observations of lunar eclipses recorded in Arabic chronicles based on an existing compilation  52. However, because none of these sources contains information on the colour of the eclipsed Moon, we did not analyse them further. East Asian lunar eclipse observations. In China and Korea, eclipse records are mainly found in the Treatise on Astronomy, Treatise on the Calendar and Treatise on the Five Elements of the official dynastic histories  20.
Care was taken to identify second-hand reports, that is, those that a given author did not witness but instead drew information on from another source. Frequent duplication occurred in Western and Eastern Christian sources owing to common underlying source materials and the scribal practices of copying, synthesizing and piecemeal updating of annals and chronicles. A table listing all total lunar eclipses records for which information about the colour of the Moon could be retrieved, and providing summary context for the historical sources investigated, is presented in Supplementary Dataset S1. An extended version of Supplementary Dataset S1 containing all descriptions of total lunar eclipses from Europe, the Middle East and East Asia considered in this study (with or without reference to colour), along with the eclipse visibility maps, can be accessed from the Zenodo repository: https://doi.
7] [18] [19]  (step 1. 3). The analysis of 46 lunar eclipses that occurred between 1880-1888 and 1960-2001 ce showed that Danjon values of L = 4, 3, 2 and 1 can be closely associated to SAOD values of 0, 0. 01, 0. 02 and 0. 04, respectively, and that an SAOD value of 0. 1 or greater is needed for a dark total lunar eclipse (L = 0) to occur. Constraining eruption dates using global aerosol simulations and satellite observations. To determine the period (T dark ) when SAOD exceeded 0. 1, that is, conditions for a dark total lunar eclipse (step 2. 1), we used four (five for Samalas) SAOD time series. For UE1-UE6, we extracted SAOD time series around the 1883 ce Krakatau and 1991 ce Pinatubo eruptions from the Sato/GISS dataset  37. This dataset, based on satellite observations, ground-based optical measurements and volcanological evidence, reports SAOD at 550 nm since 1850 ce.
We also extracted SAOD time series for the Pinatubo eruption from the Global Space-based Stratospheric Aerosol Climatology (GloSSAC v2) dataset  38  , which spans the period 1979-2018 ce. As observational data are unavailable before the mid-nineteenth century, we estimated the residence time of volcanic stratospheric aerosols for each eruption (UE1-UE6) from the eVolv2k database  4. In the case of the 1257 ce Samalas eruptions, we also relied on results of the IPSL climate model (IPSL-CM5A-LR)  40  , as it treats aerosol microphysics and has been validated for the well-observed case of the 1991 ce Pinatubo eruption  58. Each SAOD time series covers a 56-month time window (4 months before the eruption and 52 months after). For eruptions releasing more sulfur than Pinatubo, substantial uncertainties remain about the residence time of aerosols in the stratosphere  44  , and the time window for SAOD ≥ 0.
1 differs depending on the aerosol model selected (see Methods). Accordingly, for each month within the 56-month time window, we determined the probability for the SAOD = 0. 1 threshold to be exceeded on the basis of agreement between time series. Probability was defined as 'very high' if all the time series (four for UE1-UE6, five for Samalas) indicated exceedance of the threshold in a given month. Likewise, probability was considered 'high' or 'medium' if at least three or two, respectively, datasets agreed and as 'low' if only one dataset indicated threshold exceedance (step 2. 2). SAOD time series provide, for each eruption, the most probable time interval [Month min: Month max] during which a dark lunar eclipse can be observed after an eruption. Reciprocally, we can assume that the most probable eruption date falls within the time interval [Month max: Month min] before the date of the dark lunar eclipse (step 2.
iii. The physical appearance of the Moon during totality must be explicitly described and the colour of the eclipsed disk indicated. iv. Reports should be contemporary with the event and preferably by an eyewitness. These conditions are not always met for the medieval sources available (see Supplementary Dataset S1 for more information). v. Our study suggests that only lunar eclipses occurring within about 20 months of an eruption are useful for dating purposes and for discriminating the tropospheric versus stratospheric transport of volcanic aerosols. At a given location, the interval between two successive total lunar eclipses ranges between 6 months and 3-4 years (refs. 17, 63 ). The irregular occurrence of total lunar eclipses can therefore prevent the dating of a volcanic eruption if the eclipse occurs outside this 20-month period.
(3) The climatological datasets used for calibration. NVOLC v2 uses monthly mean (1805-1972 ce) JJA temperature anomalies (40-90° N) from the recently released Berkeley Earth Surface Temperature (BEST) dataset  98. Schneider et al. 41  calibrated their proxy records against monthly mean JJA temperature anomalies (1901-1976 ce) derived from the 5° × 5° CRUTEM4v network 99 (30-90°). Wilson et al. 42  scaled their proxy record to CRUTEM4v (40-75° N) MJJA land temperatures during the 1880-1988 ce period. The combination of these differences in tree-ring networks, transfer functions, climatological reference datasets, calibration periods as well as target season inevitably results in differences in the cooling magnitudes for specific events. Our study relies on state-of-the art reconstructions that efficiently capture post-volcanic summer cooling but several avenues may improve the peak cooling detection and refine the timing of HMP eruptions: i.
Potential dates of HMP (1100-1300 ce) volcanic eruptions (UE1 and UE5) using a four-step procedure. a, Residence time of volcanic stratospheric aerosols and time windows with SAOD exceeding about 0. 1. The residence time of aerosols is based on global mean SAOD 550 time series from the Sato/GISS 37  and GloSSAC v2 (ref. 38  ) datasets (for the 1883 ce Krakatau and 1991 ce Pinatubo eruptions) and simulated by the EVA forcing generator 4, 39  (for UE1 and UE5). Probability of occurrence of HMP eruptions based on the timing of dark lunar eclipse dates (b) and tree-ring records 7, 41, 42  (c). d, Integration of b and c to estimate the most probable time windows for the UE1 and UE5 eruptions.
Acknowledgements S. G. , C. C. , M. K. and M. Stoffel were supported by the  Swiss National Science Foundation Sinergia Project CALDERA  ( CRSII5_183571 ). S. G. acknowledges  A. Harrak  ( Department of Near and Middle Eastern Civilizations, University of Toronto ),  F. Espenak  ( NASA Goddard Space Flight Center ),  F. Hierink  ( Institute for Environmental Sciences, University of Geneva ) and  P. Souyri  ( Department of East Asian Studies, University of Geneva ) for providing advice on the manuscript. F. Lavigne was supported by  Institut Universitaire de France  ( IUF, Academic Institute of France ). M. K. received funding from the  EUR   IPSL -Climate Graduate School  project, managed by the  ANR  within the  "Investissements d'avenir" programme  under reference  ANR-11-IDEX-0004-17-EURE-0006.
Data availability The historical data underlying this study can be found in Supplementary Dataset S1 and is available on Zenodo at https://doi. org/10. 5281/ zenodo. 6907654. The tree-ring-based reconstructions can be downloaded at https://doi. org/10. 5281/zenodo. 3724674. Ice-core data can be retrieved from the following link and repository: https://doi. org/10. 1038/nature14565 and https://doi. org/10. 1594/WDCC/eVolv2k_ v2. SAOD time series can be obtained from the following links: https:// data. giss. nasa. gov/modelforce/strataer/ and https://doi. org/10. 1594/ WDCC/eVolv2k_v2. Source data are provided with this paper.
: Shōka 2. 10. 16 " 21016 Clear in the morning. After the hour of the Snake [9 am-11 am], heavy rain and flooding. Houses were swept away and people drowned. At the hour of the Horse [11 am-1 pm] the weather began to clear. During the hour of the Rat [11 pm-1 am] the Moon was eclipsed; it was not properly visible" (see Supplementary Dataset S1).
2 | 2 Potential dates of HMP (1100-1300 ce) volcanic eruptions (UE1 and UE5) using a four-step procedure. a, Residence time of volcanic stratospheric aerosols and time windows with SAOD exceeding about 0. 1. The residence time of aerosols is based on global mean SAOD 550 time series from the Sato/GISS 37  and GloSSAC v2 (ref. 38  ) datasets (for the 1883 ce Krakatau and 1991 ce Pinatubo eruptions) and simulated by the EVA forcing generator 4, 39  (for UE1 and UE5). Probability of occurrence of HMP eruptions based on the timing of dark lunar eclipse dates (b) and tree-ring records 7, 41, 42  (c). d, Integration of b and c to estimate the most probable time windows for the UE1 and UE5 eruptions.
Lastly, this study presents specific instances exemplifying the LINAC's adaptability, enabling the execution of hitherto unprecedented experiments. By enabling independent variations of the temporal parameters of the radiation beam implicated in the FLASH effect, these experiments facilitate the acquisition of quantitative data concerning the effect's dependence on these specific parameters. This novel approach hopefully contributes to a more comprehensive understanding of the FLASH effect, shedding light on its intricate radiobiological behavior and offering valuable insights for optimizing its clinical implementation.