dataesr/scientific-paragraphs-categorization huggingface dataset:
ACKNOWLEDGMENTS This study was support by the  European Research Council  (grant no. 267255 ) and the  Deep Carbon Observatory (DCO). We would like to thank all those who participated in our air sampling campaigns from around the world ( Alexandre N. Krot ,  Axel Hofmann ,  Paul Steele ,  Philippe Robidoux ,  Ray Langenfelds , Theo Renauld,  Thomas Dehais ,  Yuji Sano ). We gratefully acknowledge the  NOAA Air Resources Laboratory (ARL)  for the provision of the HYSPLIT transport and dispersion model and READY website (http://www. ready. noaa. gov)used in this publication. We thank an anonymous reviewer and  Mark Kurz  for constructive comments, and  David Shuster  for careful edition. This work is dedicated to our colleague  Pete Burnard , who sadly passed away in July 2015. Pete played an essential role in the development of this project.
Definition 3. 1. Let S be a minors system. A norm for S is the data of a commutative monoid U and a morphism of set species N : S → U , that satisfies the following axioms. (N1) N (X) = N (X|A) N (X/A) for every X ∈ S[E] and A ⊆ E. (N2) N (X ⊕ Y ) = N (X) for every X ∈ S[E] and Y ∈ S[∅]. (N3) N (1 S ) = 1. We note that relations (N2) and (N3) imply that we have N (X) = 1 for every X ∈ S[∅]. A case that will be of special interest for us is when U is the multiplicative monoid R × of a commutative K-algebra R. In this case we will denote the K-linear extension of N again by N : KS → R, and will still call the extension a norm. Remark 3. 2. In [37, Theorem 1] one considers morphisms of set species r : S → N that satisfy r(X) = r(X|A) + r(X/A), r(X ⊕ Y ) = r(X) + r(Y ) and r(1 S ) = 0: these appear as the parameters r j (S) in the exponents of  [37, Theorem 1].
Acknowledgements. The genesis of this project took place at the 2016  Borel Seminar  in conversations between the second and third authors and  Spencer Backman  and  Matthias Lenz , whom we thank, together with the seminar organisers for bringing us together. The first author thanks  Camille Combe  and  Emeric Gioan  for many interesting conversations on the themes of this paper. Joseph Kung  and  Iain Moffatt  had many valuable comments on a draft of this paper. We also thank the anonymous referees for their suggestions.
We suggest that the DIB carrier columns of the high irradiation DIBs are much stronger in the redshifted clouds and are responsible for some of the observed departures. Such effects, however, can not explain a shift among DIBs from the same species and the result on the 9577, 9632 Å C + 60 bands. In this work, we have revisited the case of HD 37022 using recent VLT/UVES spectra of HD 37022 acquired as part of the EDIBLES survey  (Cox et al. 2017). EDIBLES spectra of two additional targets, HD 54662 and HD 79186, are also used for comparison. Details on the observations, data reduction and targets can be found in  Cox et al. (2017). We have selected three exposures based on the weakness and rare similarity of the telluric water vapor lines. The precipitable water vapour (PWV) at the time of the HD 54662 and HD 79186 observations was 1.
34 and 1. 51 mm respectively, according to the ESO Paranal radiometer, well below average conditions. No data was available for the HD 37022 observation. However, we also checked by eye all EDIBLES exposures and could easily select the low PWV conditions based on the depths of the lines. We have used the spectra of the three targets to investigate further the locations of the stellar and interstellar absorptions around the two strong C + 60 bands. HD 54662 and HD 79186 are characterized by E(B-V)= 0. 32 and 0. 28 respectively, similar to the colour excess of 0. 31 for HD 37022 but their 9577 Å bands are significantly weaker than for the peculiar HD 37022 that is known for its particularly strong absorptions. This difference and the quality of the data are illustrated in Fig. 2. We have used the UVES data to measure the radial velocity differences between the stellar absorptions for the three stars.
This is why unnormalized spectra must be used and closely inspected before any conclusion is drawn. An example is the case of the ESPaDOnS spectrum of Cyg OB-2 5 (BD+40 1220) used in the aforementioned studies. This binary system has strong emission features associated with the colliding winds of the two members, as studied in detail by  (Rauw et al. 1999 ). The authors have published series of spectra recorded at all phases of the system. Fig. 5  shows the average of the profiles of the 4634 and 4640 Å N iii and 4686 Å He ii emission lines observed by  Rauw et al. (1999)  for orbital phases 0. 178 and 0. 193, superimposed onto the ESPaDOnS spectrum. The emission line shapes are found to be consistent with the observations for such phases. Additionally, in order to match the data a Doppler shift of +216 km s -1 has to be applied, also consistent with the same range of orbital phase (see Fig.
Acknowledgements. We thank our referee for his thorough review. M. E. acknowledges funding from the  "Region Ile-de-France " through the  DIM-ACAV  project. R. L. acknowledges support from " Agence Nationale de la Recherche " through the  STILISM  project ( ANR-12-BS05-0016-02 ) and the  CNRS PCMI national program. JC acknowledges support from an  NSERC   Discovery Grant. Based on observations collected at the  European Organisation for Astronomical Research in the Southern Hemisphere  under  ESO  programme  194. C-0833  ( ED-IBLES Survey , PI. N. L. J. Cox). Based on observations obtained at the  Canada-France-Hawaii Telescope (CFHT)  under programme  05AO5  (PI. B. H. Foing). CFHT is operated by the  National Research Council of Canada , the  "Centre National de la Recherche Scientifique" of France , and the  University of Hawaii.
Acknowledgements This project has received funding from the  European Union   Horizon 2020 research and innovation programme  under grant agreement no. 646176  (EXTMOS). Calculations were performed using resources from the  GENCI-CINES/IDRIS French  national supercomputing centers, the  CCIPL (Centre de Calcul Intensif des Pays de la Loire ), and  Grenoble CIMENT  ( Calcul Intensif, Modélisation, Expérimentation Numérique et Technologique ) computational mesocenters. C. A. G and D. J. are indebted to the  LumoMat consortium  for support through the  FCPol-Resp  project.
trial registration number NCT03088319; Pre-results. bACkground Mounting evidence shows that the perinatal period is a time of increased vulnerability for mood disturbances and the onset of psychiatric disorders. 1 2 Among puerperal disorders, baby blues, postnatal depression (PND) and puerperal psychosis are the most frequent. 1 ile baby blues appears to be a normal adaptive phenomenon, PND and puerperal psychosis are psychopathologies associated with maternal suffering and have negative consequences for the offspring and the family. PND, the most common childbearing complication, has a prevalence range of 10%-20% in Western countries. 2 3 It is described as a non-psychotic depressive episode of mild to moderate severity, beginning in or extending into the first postnatal year. 4 In the literature, two postpartum peaks have been identified: 4 weeks and 6 months postdelivery.
General design Central tendency and the variability of the continuous variables will be described depending on whether or not they follow a normal distribution (using the Shapiro-Wilk test). If there is normal distribution, data will be summarised using means and SD, if not medians and ranges will be used. VAS variables will be analysed like ordinal data and described as above. If required, class gathering into categorical variables will be performed. These variables will be described as absolute values and percentages. Any variable with more than 10% missing data will not be analysed.
Context. The recent claims of g-mode detection have restarted the search for these potentially extremely important modes. These claims can be reassessed in view of the different data sets available from the SoHO instruments and ground-based instruments. Aims. We produce a new calibration of the GOLF data with a more consistent p-mode amplitude and a more consistent time shift correction compared to the time series used in the past. Methods. The calibration of 22 yr of GOLF data is done with a simpler approach that uses only the predictive radial velocity of the SoHO spacecraft as a reference. Using p modes, we measure and correct the time shift between ground-and space-based instruments and the GOLF instrument. Results. The p-mode velocity calibration is now consistent to within a few percent with other instruments.
Introduction The detection of g modes remains a major objective of helioseismology. The benefit of detecting these modes would be to obtain the structure and dynamics of the very inner core of the Sun. There have been several claims of g-mode detection (see  Appourchaux et al. 2010 , for a review). Recently,  Fossat et al. (2017)  using the propagation time of the p-mode wave packet claimed to have detected the signature of g modes. In order to test that detection claim, we made longer data sets using a new calibration strategy for the GOLF data. Since the beginning of helioseismology, solar radial velocities have always been measured using solar spectral lines. The intensitiesaretypicallymeasuredintheblueandredwings(I b and I r )ofthe line and the displacement is deduced by calibrating the ratio I r -I b I r + I b with respect to known radial velocities (see  Elsworth et al.
(2017)   Schunker et al. (2018)  reproduced Fig. 10  of  Fossat et al. (2017). They showed that using different fitting procedures, the prominent peaks at 210 nHz and its acolytes would smear out or even disappear, as seen for the time series sampled at 60 s. This leads us to investigate how the GOLF data are calibrated and whether a different calibration might or might not reproduce the results of  Fossat et al. (2017). This work has been divided in two parts. The present paper (Part I) explains how a new calibration of the GOLF data has been obtained. The accompanying paper (Part II) investigates the results obtained by  Fossat et al. (2017)  and compares it with different time series. The first section of this present paper explains the calibration procedure, the extraction of the velocity, and the time corrections applied.
Extraction of the velocity The data used for the new calibration start on 11 April 1996 and end on 10 April 2018. The technique used for the calibration is derived from that of  García et al. (2005)  using the so-called X method. Since GOLF operates only in one wing of the Sodium lines, the following ratio is computed as a proxy to the two-wing signal: X = 1 2 P + + P - P + -P -, (1) where P + and P -are the signals measured in the same wing (blue or red) using a weak magnetic field modulation that induces a wavelength change. The bracket denotes a low-frequency filtering of the slope proxy (i. e. the derivative). The division by P + -P -is needed since it provides a way to normalise to the slope of the line. The procedure for computing the radial velocity starts by computing the photomultiplier (PM) signals as follows: 1.
The calibration of the X 1 and X 2 ratios with respect to the solar radial velocity is done using the technique described in  García et al. (2005) , in which they assume that the ratio X can be modelled as follows: X = f (V) = a + bV 1 + αV 2 + βV 4 , (2) where a, b, α and β are parameters, and V = V grav + V orb is the radial velocity including the gravitational redshift (V grav = 636 m s -1 ) and the contribution generated by the spacecraft orbiting the Sun (V orb ). The residual velocity (V X , made of the oscillation signals and other contributions) is excluded from the model since this is what we want to extract. The orbital spacecraft velocities are obtained from the VIRGO Data Center, which provides computation of the solar radial velocity on a 60 s cadence. The velocity used here is the predictive, not the measured, velocity since the SoHO operation team stopped providing the reconstructed velocity after 1998 because the predictive one was good enough.
Correction of time shifts As outlined in  García et al. (2005) , the GOLF data may lose synchronisation with respect to the basic temporal cadence. In principle, ancillary data allow us to quantify the resulting induced shifts thanks to a daily pulse (DP) generated on board SoHO. The precise time datation according to the Temps Atomique International (TAI) is available in the header of the raw daily data files. However, in a few cases, the GOLF clock could not be synchronised on the DP, and in order to check for potential unknown time jumps, we used data from other instruments such as the Global Oscillation Network Group 3  , the Birmingham Solar Oscillation Network 4  , and the Sun Photometer Monitor of the Variability of Irradiance and Gravity Oscillations instrument 5. The measurement of the time shift is done using the p modes themselves with the following procedure: 1.
Select a sub-series from two instruments (e. g. GOLF, BiSON, GONG, SPM) with a typical duration of one day. When the cadence differs, resample the sub-series to a common temporal cadence of 60 s using linear interpolation (e. g. for BiSON). The integration is one day as well as the sampling (for display purposes, other integration times of 10 days and 45 days have been used with one-day sampling). 2. Compute the backward difference filter (BDF) 6  , for each instrument but GONG, for which it has already been applied. 3. Compute the cross correlation C for a range of ±13 mins by steps of 1 min. 4. Compute the cross correlation envelope C env using the Hilbert transform H (C env = C 2 + H(C) 2 ) 7. 5. Fit the cross correlation envelope using least squares with a Gaussian to obtain an estimate of the time shift between the two data sets.
The precision of the time shift obtained by fitting the correlation of the p modes is far more precise than the fitting of the correlation provided by the envelope. The former is related to the p-mode phase velocity while the latter is related to the p-mode group velocity. Figure  4  gives an example of what is fitted. We found that the GONG data for l = 0 and the VIRGO/SPM data do not present any temporal jumps as shown in Fig. 5. As it is unlikely that both time series would have time jumps at the same date, the blue SPM and GONG then provide two references for a constant time base. The GONG data were then used as a time reference to check and correct GOLF datation. On close inspection, Fig. 5  shows that the time delay in this time series is modulated with a periodicity of almost 6 months.
For the p-mode frequency range and a 60 s cadence, the filtering factor in power ranges from 0. 8 to 1. 5, while for the noise it ranges from 0. 14 to 0. 31. For the last step, the formation height was corrected for GOLF during the red-wing mode by multiplying the amplitudes by 1. 11. For GONG, the resulting velocities were multiplied by 1. 17 in order to take into account the different formation height of GONG; the factor was adjusted post-facto. No other correction for formation height was applied to the remaining data sets. We note two different amplitude regimes in the time series used by  Fossat et al. (2017) , occurring at the beginning of the time series and after 2002 for about 2 yr, both in the blue wing. These two differences are related to the way that the temperature of the cathode of the photomultipliers is used to correct the calibration  (Garcia, 2018, priv.
Acknowledgements. The GOLF instrument onboard SoHO is based on a consortium of institutes (IAS,  CEA/Saclay, Nice and Bordeaux Observatories from France , and  IAC from Spain)  involving a cooperative effort of scientists, engineers, and technicians, to whom we are indebted. GOLF data are available at the MEDOC data and operations centre ( CNES/CNRS/Univ. Paris-Sud ) at medoc. ias. u-psud. fr. SoHO is a mission of international collaboration between  ESA  and  NASA. This work uses data obtained by the  Global Oscillation Network Group (GONG) program , managed by the  National Solar Observatory , which is operated by  AURA, Inc. under a cooperative agreement with the  National Science Foundation. The data were acquired by instruments operated by the  Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory ,  Instituto de Astrofísica de Canarias , and  Cerro Tololo Interamerican Observatory.
Code development -individual and communal In his essay on the "Performativity of code: Software and Cultures of Circulation," Adrian MacKenzie makes an important distinction between the software of an operating system (in this case he is referring to Linux) and the hardware of the machine: [An] operating system may not be reducible to a conventional commodified object if it constantly modulates as it moves through a distributed collective of programmers and system administrators. By contrast, the same thing cannot be said for computer hardware. Almost without exception, computer hardware is commodified and its production is industrial. […] Linux represents a form of collective agency in the process of constituting itself. This ongoing constitution is performative with respect to the efficacy of Linux as a technical object and with respect to the fabrication of Linux as a cultural entity.
, 2012). Immunization of rabbits offered an overall efficacy of 90%, mainly via reducing the number of adults and egg hatching  (Rodríguez-Mallon et al. , 2012). During bovine immunization studies against R. microplus and an overall vaccine efficacy of 96% was obtained  (Rodríguez-Mallon et al. , 2015). As a consequence of these results a vaccine composition based on the P0 peptide was patented recently due to its potential as protective vaccine antigen against a range of ectoparasites  (Mallon et al. , 2015). Since the generation of tick sequence databases (genome and transcriptome), in silico vaccinology approaches have been used with success to identify protective antigens, as evident from a next generation multi-peptide tick vaccine that has been developed  (Schetters et al. , 2016). Future studies are now needed to identify protective antigen epitopes to reduce costs associated with production of a commercially viable vaccine.
e. , genomes, shot-gun, expressed sequence tags and suppression subtractive hybridization or SSH libraries, microarray and RNA sequencing transcriptomic datasets, etc. ), representing different life stages and different conditions, have been expanding for many metazoan parasite species of economic importance  (Anstead et al. , 2015; Greene et al. , 2015; Lv et al. , 2015; Schwarz et al. , 2015; Tyagi et al. , 2015; De La Fuente et al. , 2016a,b; Kuleš et al. , 2016; Arlian and Morgan, 2017; Barrero et al. , 2017). These growing repositories of genetic information enable researchers to gain access to a greater complement of molecules involved in parasite and parasitehost biology, also enabling evolutionary analyses to determine parasite diversity and encoded protein conservation/divergence within and between parasitic and non-parasitic species  (Lv et al.
The excellent ability of the NHC-Boranes and especially the new one, to be used as photopolymerization co-initiators has been analyzed by Laser Flash Photolysis (LFP). The rate constants for elementary reactions of the three boranes and their derived NHC-boryl radicals obtained by LFP correlated well with the molecular modeling data and show that the key for the observed reactivity is the ability of the tetrazolydinyl NHC-Borane to repair the peroxyl radicals formed by the reactions of the macroradicals with oxygen.
For the NHC-boryl radicals addition to the olefin, all measurements were performed under a N 2 -saturated atmosphere with solutions degassed for at least 10 minutes prior to use, to avoid any unwanted reaction of the radicals with dioxygen. The kinetics data are again gathered in Table  1. Interestingly, 3• reacts one order of magnitude less rapidly with O 2 than 1• and 2• (k O2 = 1. 9 x 10 8 M -1 s -1 vs. ~10 9 M -1 s -1 , see Table  1 ). The problem of oxygen inhibition is not acute in viscous resins, because the concentration of dioxygen is limited by diffusion. From the point of view of the addition to the monomer, 3 did not underperform despite its relatively slower addition rate. We know from previous work that the NHC-Boryl addition step is not rate-determining. 36 That explains why all NHCBs performed similarly in that case.
24 C-BH 2 -OO• + NHC-BH 3 à NHC-BH 2 -OOH + NHC-BH 2 • (5) In equation 3, the reaction was found to be more exothermic with 1• (-79. 1 kcal. mol -  ) that with 2• (-77. 8 kcal. mol -  ) and, especially, 3• (-75. 8 kcal. mol -  ). In contrast, while all hydrogen transfers to the bora-peroxyl radicals are almost thermoneutral, only with 3 it is an exothermic process (ΔH = -0. 4 kcal. mol -  vs. 2. 1 kcal. mol -  for 1 and 1. 4 kcal. mol -  for 2). -Electronegativities and charge-transfer abilities of NHC-boryl radicals: The Mulliken electronegativity of the three NHC-boryl radicals was determined using Parr and Pearson's model (Eq 6a). The latter uses the ionization potential (IP) and the electron affinity (EA) of the radicals, which can be calculated (DFT level). The data are summarized in Table  2.
2C  and Table  S1 ); they intersected with excellent statistical significance with the genes identified in the Sun-Tag cells (p<1e-53). Moreover, we found the expression of genes significantly regulated in only one system, to nevertheless display highly coherent expression changes in the other system (Fig. 2D ). Hence, to improve statistical power and expand on Nanog targets we combined the SunTag and 44iN datasets to test for those genes with coherent Nanog response across both systems (Fig. 2E  and Fig. S2D ). Combining with those genes already identified, this resulted in 457 genes (Fig. 2E  and Fig. S2D ), which generally display extremes of expression differences between Dox-treated SunTag (high Nanog) and untreated 44iN cells (low/absent Nanog); they globally behave in a concordant way when long-term Nanognull cells are compared to wild-type cells (Fig.
S2D ), or when their expression is analysed in published datasets (Fig. S2E ). Genes activated by Nanog are enriched in regulators of stem cell maintenance (FDR<2. 99e-16), while repressed genes are enriched in differentiation processes such as nervous system development (FDR<6. 89e-10). Hence, we have defined the compendium of Nanog-responsive genes in undifferentiated ES cells with unprecedented completion. Strikingly, neither Klf4 nor Esrrb belong to our list of Nanog-responsive genes. Nanog rewires the pluripotency network to control its targets. Having established a list of Nanog-responsive genes, we aimed at exploring the mechanisms by which Nanog influences their expression, focusing on a potential role of Nanog in modulating binding of other regulators such as pluripotency TFs (Oct4, Sox2 and Esrrb) and the chromatin remodeller Brg1 that is functionally associated with selfrenewal  (Ho et al.
, 2009; Kidder et al. , 2009). To do this, we first established a list of 27,782 regulatory elements bound by Nanog using six datasets derived from four independent published studies (Table  S2 ) and used 44iN cells to address how Nanog impacts TF binding and chromatin accessibility at these sites. We noticed that at some Nanog binding regions, Esrrb, Oct4, Sox2, and Brg1, display a strong reduction of binding and decreased chromatin accessibility, after 24 hours of Dox withdrawal (Fig. 3A ). This observation can be generalised to a large proportion of regions and is particularly prominent in the case of Esrrb (Fig. 3B ). We then divided Nanog binding regions in two major groups Fig. 3B  and Fig. S3 , based on the presence of other TFs (regions of co-binding) or not (Nanog-solo regions). In Nanog-solo regions, which display lower levels of Nanog binding, the chromatin is less accessible irrespective of Nanog (Fig.