dataesr/scientific-paragraphs-categorization huggingface dataset:
The images were convolved to a common angular resolution of 25 which is essentially the poorest resolution of the considered wavelengths. The convolution kernels of  Aniano et al. (2011)  were used to take the different instrumental responding functions into account. For the ATLASGAL images, any uniform astronomical signal on spatial scales larger than 2. 5 has been filtered out together with atmospheric emission during the data reduction  (Schuller et al. 2009 ). The filtering of Hi-GAL images was performed using the CUPIDfindback algorithm of the Starlink suite. For further details on the algorithm please see the online document for findback 2. Following  Yuan et al. (2017) , we run the algorithm iteratively using a common filtering box of 2. 5 to get stable background images which were subtracted from the post-convolution data for Hi-GAL bands to remove large-scale structures.
Dust Properties Intensity as a function of wavelength for each pixel was obtained from the smoothed and background-removed far-IR to sub-mm image data and modeled to a modified blackbody. I ν = B ν (T )µ H 2 m H κ ν N H 2 /R gd (1) where κ ν = κ 600 ν 600 GHz β cm 2 g -1. (2) Here, µ H 2 = 2. 8 is the mean molecular weight adopted from  Kauffmann et al. (2008) , m H is the mass of a hydrogen atom, N H 2 is the H 2 column density, R gd = 100 is the gas to dust 2 http://starlink. eao. hawaii. edu/starlink/findback. html ratio, κ 600 = 5. 0 cm 2 g -1 is the dust opacity at 600 GHz for coagulated grains with thin ice mantles  (Ossenkopf & Henning 1994). The dust emissivity index β was fixed to 1. 75  (Ossenkopf & Henning 1994; Planck Collaboration et al. 2014). Free parameters in this model are the dust temperature N H 2 and column density T dust.
Line Emission Figure  4  shows the full band spectra towards the SMA1 peak. Cross-checking the rest frequencies with the Splatalogue molecular database, we have identified 103 emission lines with peaks > 3σ where 1σ = 80 mJy beam -1. These transitions are from 19 species (26 isotopologues) including nitrogen-bearing species (e. g. , HC 3 N, CH 3 CN), complex organic molecules (e. g. , CH 3 CHO, CH 3 OCH 3 ), and classical tracers of bulk motions (e. g. , CO, SiO). We extracted spectra of all detected transitions towards the SMA1 peak and used the GILDAS /CLAS S software to perform Gaussian profile fitting to get the line peak intensities, velocity centroids, linewidths, and velocity-integrated intensities. The systemic velocity of SMA1 was estimated to be 50. 3±0. 1 km s -1 via averaging line centers of transitions with FWHM ≤ 9 km s -1 and I peak ≥ 0.
2012). GRS 13 CO (1 -0) channel maps are shown in Figure  8. Intriguingly, emission spatially associated with filament F1 mainly originates from gas with velocity smaller than 51 km s -1 while the gas associated with filaments F2 and F3 is systematically red-skewed with velocities larger than 50 km s -1. The variation of velocity indicates bulk motions in these filaments. Spectra of 13 CO (1 -0) have been extracted along the filaments with a step-size of half the angular resolution (∼ 46 ) of the GRS observations, and fitted to a one-dimensional Gaussian profile using the GILDAS/CLASS software. The resultant centroid velocities of the extracted spectra are shown in Figure  9  (a) as color-coded circles. The smoothly varying velocity along filaments F1, F2, and F3 is reminiscent of the situation in the SDC13 infrared dark clouds where longitudinal filamentary collapse has been reported  (Peretto et al.
Intriguingly, the absorption dips of the source averaged HCO + and 13 CO spectra are both red-skewed with respect to the systemic velocity. This feature is consistent with a global collapse scenario as suggested in  Jin et al. (2016). We estimated the infall velocity by fitting the clumpaveraged HCO + spectrum using the RATRAN 1D Monte Carlo radiative transfer code  (Hogerheijde & van der Tak 2000). The input parameters include the clump size, density profile, kinematic temperature profile, HCO + fractional abundance (X HCO + )and infall velocity. We deduced a power-law density profile (ρ ∝ r -1. 5 ) based on the mass (∼ 590 M ) and radius (∼ 0. 39 pc) of C1. Following  Peretto et al. (2013) , we used a constant temperature which is approximately the source-averaged dust temperature of C1 (21 K, see Table  2 ).
Sandfly trapping and virus detection A total of 4,770 (3,158 females and 1,162 males) sandflies were collected and identified morphologically. They were allocated to 315 pools (198 female and 117 male pools). The number of sandflies and pools originating from individual villages are shown in Table  1  and Fig 1. The most abundant species were P. papatasi (57. 57%) and Sergentomyia spp. (31. 05%). The less abundant species were; P. alexandri, P. mascitti, P. tobbi, P. mongolensis, P. sergenti, P. caucasicus, P. major, P. bergeroti, and P. kandelakii. Pool #131 that consisted of 30 non-engorged female Sergentomyia spp. trapped in the Shordakesh in Dasliboroun village, in July 2011 was positive with primers pair N-Phlebo1S/ 1R  [29]. The resulting 502-nt sequence in the polymerase gene was most closely related to Sandfly fever Turkey virus (SFTV-GenBank acc no: GQ847513) with sequence identities of 94% and 81% at the AA and nt levels, respectively.
Complete genome sequencing Supernatant corresponding to passage 2 of DASHV infected Vero cells was used for complete genome characterization using Next Generation Sequencing (NGS) as previously described  [2] ; viral sequences were identified from the contigs based on the best BLAST similarity against reference databases using the CLC Genomics Workbench 7. 0. 4. Reads > 30 nucleotides long were trimmed using CLC Genomic Workbench 6. 5, with a minimum of 99% quality per base and mapped to reference sequences on Genbank. Parameters were set such that each accepted read had to map to the reference sequence for at least 50% of its length, with a minimum of 80% identity to the reference. Sequence gaps were completed by PCR, designing specific primers based on NGS results and for the extremities using the primers previously defined  [14] , and PCR fragments were sequenced either by Sanger sequencing or by NGS.
Pairwise genetic distances and phylogenetic analysis based on complete coding sequences Complete coding regions of the S, M and L segments of phleboviruses were collected from Genbank (http://www. ncbi. nlm. nih. gov/genbank) and were aligned together with DASHV using the CLUSTAL algorithm of the MEGA 6 software  [63]. Nucleotide (nt) and amino acid (AA) distances were calculated with the p-distance method. Neighbour-joining (NJ) analysis (Kimura 2-parameter model) was carried out using AA alignments, with 1000 bootstrap pseudoreplications. ML analysis was also performed using the best model defined for each gene. Since there was no obvious difference in the topology of the trees for viruses closely related with DASHV using either NJ or ML, final analysis including a larger set of sequences was performed using NJ.
Phylogenetic analysis using partial polymerase sequences A total of 24 homologous sequences most closely related with DASHV were aligned using Clustal W in MEGA6  [63]. The evolutionary history was inferred either by using the Maximum Likelihood method based on the Tamura 3-parameter model gamma distributed with invariant sites  [63]  or by the neighbour-joining method using the Kimura-2 parameter model. All positions with less than 95% site coverage were eliminated, so that they were a total of 160 positions in the final dataset. Evolutionary analysis was conducted in MEGA6.
complete genomic sequence of DASHV consisted of 6,444nts, 4,413 nts and 1,802 nts for the L, M and S segments, respectively (GenBank acc. no KP771821, KP771822, and KP771823). The polymerase gene encoded a 6,270-nt long ORF (2,090 AA), whereas the glycoprotein gene encoded a 1,342-nt long ORF (4,026 AA, further cleaved into a 531-AA long Gn and a 478-AA long Gc). The small segment encoded a 738-nt and an 801-nt long ORF which were translated to nucleocapsid protein (246 AA) and nonstructural protein 267 AA), respectively.
This work was supported through funds received from  EU  grant  FP7-261504 EDENext  and this paper is catalogued by the  EDENext Steering Committee  (http://www. edenext. eu),the  European Virus Archive goes Global (EVAg)  project in the European Union's  Horizon 2020 research and innovation programme  under grant agreement No  653316  (http://global. europeanvirus-archive. com/). The present article partly was supported by  Cellular and Molecular Biology Research Center, Shahid Beheshti University of Medical Sciences ,  1573 ) The work of RNC was done under the frame of EurNegVec ( TD1303 )  COST Action. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.
Interventions were regarded as systemic treatment with any type of corticosteroid preparation, whereas controls were standard therapy or placebo. Data from trials of acute respiratory distress syndrome (ARDS) were included when separate data were available for participants with sepsis or when contact with study authors resulted in provision of the data. Studies that were included for analysis in the Cochrane review were initially included in this analysis. However, we excluded all data from children (<18 years), as well as those studies that were designed to investigate the effect of corticosteroids on respiratory function in ARDS and pneumonia (primary outcome measures were purely respiratory function). Cross-over studies where both groups received steroids and no information was published on outcomes at the cross-over were also excluded.
ICU LoS Only a small subset of the database provided information for ICU LoS; thus, NMA was not performed for this outcome. However, results from two studies suggest that hydrocortisone infusion may reduce the ICU LoS compared with placebo. One of the studies provided strong evidence supporting this hypothesis (mean difference of 7 days, 95% CI 2. 35 to 11. 7 days), whereas the other study yielded a less precise result (mean difference of 9 days, 95% CI -3. 64 to 21. 6 days).
However, this ability is significantly reduced by dividing the patients into multiple treatment groups, whereby the number of patients in each group is fewer. The limitations of the study include that there were few direct comparisons of treatment regimens (all but two studies were intervention versus placebo). This means that the strength of inference made in an NMA between different interventions is not as robust as it could be and that consistency between direct and indirect evidence could not be assessed. This study used data from the last 50 years. Improvements in intensive care over the last half-century are myriad, and the breadth of patients, in terms of both age and co-morbidities now treated within a critical care environment, has increased. This means that bias will have inevitably crept in.
32 In particular, the data concerning natives of the tribes (2,042 individuals counted in 1911) are debatable, according to inspector of colonies Paul Pégourier: 32 See Shineberg 1983. A general census was conducted in 1911. The fundamental flaw in the organisation of this census was the disruption it occasioned for the natives, since some tribes lived 30 kilometres or more from the office of the Administrator. Under these conditions, it is no wonder that the results recorded in the Civil Register were uncertain, as the Administrator of Houaïlou rightly remarked in his report on the subject in 1918. (Pégourier 1919, p. 25)  Pégourier put forward an estimate of the 'population of the districts' of Houaïlou of 1,878 individuals (without any indication as to how he arrived at this number). 33 On his prophylactic tour in 1912, Dr Leboeuf counted 1,983 inhabitants.
-Are the difficulties coming up again? Yes, that's it, they're digging up the war axe, that's what's happening. Well, so much the better as long as each person takes responsibility. and paid jointly by the ADCK and the customary councils -has been built up. The collectors meet together once or twice a year to share their experiences and discuss problems raised by collection (as relates to both archiving and protection or transmission of the data gathered). The meeting of the collectors itself forms part of the process initiated by the ADCK, and aims to increase the interactions between those who collect, to reinforce their faith in the importance of what they are doing, and to contribute to motivating everybody when the collectors return to their regions of origin. The most important aspect is thus perhaps not so much the resulting collection as the process of bringing collectors and the institution into a relationship with local scholars and knowledge valued in and of themselves.
Thanks to the collection of Kanak oral heritage, the data collected has been archived in the mediathèque at the Tjibaou Cultural Centre (on minidisk), and transcriptions are made in vernacular languages and published in an annual report on activities sent to each customary council that has signed agreements with the ADCK. Two types of document are contained in these reports: texts describing practical skills related to weaving, horticulture, medicine, dance, fishing and hunting, the organisation of ceremonies and the vocabulary of kinship; and texts made up of knowledge about society and history: clan histories, genealogical speeches and explanations of place names. What are the effects of this process of 'collection'? Firstly, it changes the status of 'intangible heritage': however rigorous the collectors and however faithful the transcriptions, to collect is to alter.
For us society is being constructed now, so we need the data now, you see. People didn't understand the point of collecting data that can be used to identify people and legitimacies through creation of the customary land register, so [the ADCK collectors] do their work which is linked to their own concerns, but it's not linked to our concerns. Well, in short, the kid who in 20 years or 30 years is going to reread the thing, won't that revive conflicts? … Inevitably in the history of oral societies, the more you have information that goes back in time, the more you say it's the truth. But which truth? Is it really the truth? (Extract from interview, July 2008) This comment raises the question of the goals of the customary councils and the ADCK, as actors involved in the process of collection.
Foam slices were added to the devices to prevent direct contact of SWD pupae with cotton or silicagel. RH and temperatures were checked directly into experimental tubes using Ibutton's Hygrochron (Maxim Integrated, San Jose, CA, USA), and K thermocouples (measuring accuracy: ±0. 5 • C) connected to Testo thermometers (Model 175 T3; TESTO Limited, Hampshire, England). As previously described, preliminary assays were first performed in order to calibrate the number and duration of sampling times to get emergence data spanning from 0 to 100%. Again, at least seven durations were used for each tested temperature (details in Table  S5 ). Flies were considered as alive when the adult eclosed from the puparium.
Recently, a consortium of scientists has published a useful review with the updated situation of SWD all over the world  (Asplen et al. , 2015). The authors suggested a few directions for future research to improve the accuracy of SWD management. Acquisition of novel data on the biology of SWD at low temperature was highlighted as a priority, and we believe the present dataset may provide valuable elements in this regard. The present study is one of the first to provide a global description of SWD basal thermal tolerance, especially bringing new information about heat stress tolerance and the interaction between temperature and relative humidity. In a context of global climate change and considering the winter temperature warming on temperate region, these results together with previous data from the literature highlight that SWD will most likely be able to tolerate mild cold stress conditions for several consecutive days (e.
9. 0)  (Caporaso et al. , 2010). Sequence reads with an average quality score below 25 and more than 1 ambiguous base were discarded. Sequences which passed quality filters were truncated to 150bp length to facilitate comparisons with the Illumina HiSeq reads of  Berg et al. (2016a) , giving rise to a dataset containing 15,197,186 reads total, with a mean of 74,862 and median of 51,932 reads per sample. Resulting fasta files were concatenated into one file, and the 16S rRNA gene sequences were further analyzed using QIIME. De novo OTU extraction was performed with the uclust option in QIIME. Singletons were removed from centroid consideration using the USEARCH  (Edgar, 2010)  suite. Resulting reads were clustered using the UPARSE algorithm at 3. 0% (4 mismatches) clustering radius. Centroids were mapped to the Greengenes 13.
8 database for taxonomic assignment at 97% (3. 0% clustering radius) identity. Centroids failing to map to the database were evaluated with UTAX for a de novo taxonomic assignment. Sequences that match plant chloroplast, mitochondrial, or archaeal 16S rRNA were removed. Sequences used for our meta-analysis are available from public databases, including the European Nucleotide Archive for the Schulenburg lab data (www. ebi. ac. uk/ena; accession number ERP014530); the Sequence Read Archive database for the Samuel lab data (www. ncbi. nlm. nih. gov/sra; accession number SRS1849345), and the MG-RAST metagenomic archive for the Shapira lab data (http://metagenomics. anl. gov; accession numbers mgp13213 and mgp21372). The sample names, accession numbers, and additional meta-data are presented in Supplementary Table  1.
ACKNOWLEDGMENTS We thank the members of the  Félix, Samuel, Shapira, and Schulenburg labs for discussion. We are grateful for funding to KD and HS from the  German Science Foundation  within the Collaborative Research Center CRC 1182 on the origin and function of metaorganisms (projects A1. 1, A1. 2, and  A4. 3 ). MB is supported by the  National Science Foundation Graduate Research Fellowship Program  ( DGE 1106400 ).
Context. This paper presents an overview of the photometric data that are part of the first Gaia data release. Aims. The principles of the processing and the main characteristics of the Gaia photometric data are presented. Methods. The calibration strategy is outlined briefly and the main properties of the resulting photometry are presented. Results. Relations with other broadband photometric systems are provided. The overall precision for the Gaia photometry is shown to be at the milli-magnitude level and has a clear potential to improve further in future releases.
Introduction The ESA Gaia satellite mission, launched in December 2013, started its full-sky astrometric, photometric and spectroscopic survey of the Milky Way Galaxy in July 2014  (Gaia Collaboration et al. 2016b ). The first large-scale publication of data from the mission took place on 14 September 2016, when positions and broadband magnitudes were published for 1. 14 billion stars. This paper gives an overview of the photometric data that are part of that data release. The Gaia photometric data consists of three systems: broadband G (350 -1000 nm) magnitudes, optimised for the astrometric data to collect a maximum of light, but also provide accurate integrated flux measurements over the mission; integrated fluxes in a blue G BP (330 -680 nm) and red G RP (640 -1000 nm) channel, obtained from the integration of dispersion spectra; and low-resolution BP and RP dispersion spectra.
The wavelengths coverage is still based on the pre-mission specification  (Jordi et al. 2010) , a full calibration of the actual passbands will be carried out as part of the next Gaia data release. The photometric data presented here and included in Gaia Data Release 1 (DR1) only concerns the G band and was obtained from the processing of data collected during the first 14 months of the Gaia mission. A more comprehensive description of the data included in Gaia DR1 is presented in Gaia  Collaboration et al. (2016a). It should be noted that this is only a first reduction, with a partial external calibration, and a number of issues in the data and the calibration models still to be resolved. This paper provides a general overview of the photometric processing. It is accompanied by three other papers describing specific aspects of the photometric processing in much more detail: a paper on the calibration principles  (Carrasco et al.
2016) , one on the technical issues presented by the processing of the Gaia photometric data and on the solutions implemented  (Riello et al. 2017 ) and one on the extensive validation activities that preceded the release  (Evans et al. 2017 ). Among the papers accompanying Gaia DR1, the two papers  Eyer et al. (2016)  and  Clementini et al. (2016)  show the huge potential and exquisite quality of the Gaia photometry. Section 2 describes the input data with an emphasis on the use and implications for the data presented here. The calibration models and principles of the calibrations are presented in Sect. 3. Precision and internal consistency of the data is described in Sect. 4. In Sect. 5 we show some comparisons between the Gaia G band and other photometric systems. A brief summary of results is given in Sect.
The input data This section provides a brief overview of the input data from which the Gaia photometry has been derived. Gaia observations are obtained through CCDs operating in time-delayed integration (TDI) mode, integrating the signal as it moves across a CCD in approximately 4. 5 seconds. A single pixel has an integration time of ≈ 0. 001 s, corresponding to a movement along scan of ≈ 0. 06 arcsec. Integration times can be shortened for bright stars by using so-called gates. The shortest gate, as used for the brightest stars, integrates over just 4 pixels. Pixels in the across-scan direction are about 0. 18 arcsec. The movement across scan for a full CCD transit can vary between ±4 across-scan pixels. We refer to Gaia  Collaboration et al. (2016b)  and  Carrasco et al. (2016)  for a more detailed description of the instrument and the data.
In the SM1 and SM2 CCD strips charges are integrated over about half the CCD width, this corresponds to gate 12 being permanently active with a resulting effective exposure time of 2. 9 seconds. The data are accumulated onboard in samples of 2 by 2 pixels. With the full width half maximum of the point spread function at about 1. 8 pixels (0. 1 arcsec), it is clear that the images on the SM detectors are undersampled. There is no further compensation for bright images, which as a result tend to be saturated. For the faintest stars (down to magnitude 20. 7) the resolution of the data as sent back to Earth is further reduced to 4 by 4 pixels. The different binning strategies are referred to as window classes. The SM data are always provided in the form of 2D images. This is important for analysing data on close binary stars, although that has not yet been implemented at this stage of the data reductions.
Small-scale calibrations The small-scale calibrations represent the local response variations on the CCDs, generally related to the manufacturing process. Because of this there is no distinction between the two fields of view, but all other aspects of calibration units remain the same. The small-scale calibrations try to model in detail the response variations of the CCDs as a function of the across-scan coordinate. Known small-scale discontinuities are related to socalled stitch blocks, which are small rectangular areas on the CCD. As the small-scale variations are linked to the CCDs rather than the telescope, it is possible to use data accumulated over long time intervals (many months to a year). For the current Gaia DR1 publication, all 14 months of data was used in a single set of small-scale calibrations.