dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements These works have been supported by the  European Union 's  Horizon 2020 research and innovation program  under grant agreement No  771134. The project NETFIB was carried out under the  ERA-NET Cofund SusCrop  (Grant  N°771134 ), being part of the  Joint Programming Initiative on Agriculture, Food Security and Climate Change (FACCE-JPI). This work has also been supported by  EIPHI Graduate School  under (" ANR-17-EURE-0002 ").
Affinity measurements by surface plasmon resonance A Biacore T200 instrument and HBS-EP+ running buffer was used throughout (GE healthcare). Anti-human IgG was first attached to the CM5 chip by amine coupling following the manufacturer protocol (GE healthcare). Recombinant mouse CD27-human Fc (R&D systems) was then captured for 1 min at a flow rate of 10 ml/min. The flow rate was then increased to 30 ml/ min before injection of serially diluted CD70 fusion proteins. The chip was regenerated with injection of MgCl 2 (3 M) for 1 min at flow rate 20 ml/min. The k a and k d were determined using the Biacore Bioevaluation software and the K D values were calculated as k a /k d. To examine the binding of dtCD70-Fc and anti-CD27 mAb to FcRn, ~2000 response units of dtCD70-Fc or anti-CD27 were immobilized onto a CM5 chip via amine coupling.
The ion transfer tube temperature was set to 275°C. The scan range was 400-1600 m/z. The HCD collision energy was set to 50%, appropriate for fragmentation of glycopeptide ions. Precursor and fragment detection were performed using an Orbitrap at a resolution MS1 = 100,000. MS2 = 30,000. The AGC target for MS1 = 4e5 and MS2 = 5e4 and injection time: MS1 = 50ms MS2 = 54ms. Data analysis and glycopeptide identification were performed using Byonic (Version 2. 7) and Byologic software (Version 2. 3; Protein Metrics Inc. ). The glycopeptide fragmentation data were evaluated manually for each glycopeptide; the peptide was scored as true-positive when the correct b and y fragment ions were observed along with oxonium ions corresponding to the glycan identified. The MS data were searched using the Protein Metrics 305 N-glycan library with sulfated glycans added manually.
Flow cytometry Antibodies used for staining were purchased from eBioscience: anti-CD8a-APC (53-6. 7), anti-CD62L-eFluor450 (MEL-14), anti-CD45. 1-eFluor450 (A20) and anti-CD44-FITC (IM7). The numbers of adoptively transferred OT-I T cells were checked by staining with PE-labelled H-2K b OVA 257-264 tetramers and their naïve phenotype confirmed by CD62L/CD44 staining (~95% CD62L high and CD44 low). Throughout, a blocking anti-FcgRII/ III antibody (2. 4G2; 10 mg/ml) was added to cells for 15 minutes at 4°C prior to incubation with surface staining antibodies for 30 minutes at 4°C. Red blood cells were then lysed and cells were washed prior to analysis on a BD FACS Canto II using the BD FACSDiva software.
Its depth and the host brightness make planet d easily detectable with CHEOPS, and therefore HD 22946 was observed several times with this instrument within the Guaranteed Time Observations (GTO) programmes CH_PR110048 and CH_PR100031, with the main scientific goals being to uncover the true orbital period of planet d and to refine the parameters of the HD 22946 system based on CHEOPS and TESS observations via joint analysis of the photometric data, supplemented with ESPRESSO spectroscopic observations of HD 22946. The present paper is organised as follows. In Sect. 2, we provide a brief description of observations and data reduction. In Sect. 3, we present the details of our data analysis and our first results, including stellar parameters, period aliases of HD 22946d from the TESS data, and a search for TTVs.
e. minimal systematic noise elsewhere in the light curve), we concluded that this signal is a bona fide transit event and that the transits in sector numbers 4 and 30 are very likely caused by the same object, that is, by planet d. Outliers were cleaned using a 3σ clipping, where σ is the standard deviation of the light curve. With this clipping procedure, we discarded 300 data points out of 61 987, which is ∼0. 5% of the TESS data. Subsequently, we visually inspected the dataset in order to check the effect of the outlier removal, which we found to be reasonable. As TESS uses as time stamps Barycentric TESS Julian Date (i. e. BJD TDB -2 457 000. 0), during the next step we converted all TESS time stamps to BJD TDB. 1 See https://mast. stsci. edu/portal/Mashup/Clients/Mast/ Portal. html 2.
2. 1). The marginal probability for each period alias of planet d was calculated using the MonoTools package (see Sect. 3. 2). We were not able to observe all the highest-probability aliases, because some were not visible during the two-week period of visibility. Within the program number CH_PR110048, we therefore planned to observe the three highest-probability aliases of planet d with CHEOPS, but due to observability constraints and conflicts with other observations, only two visits 2 of planet d aliases were scheduled. Its true orbital period was confirmed during the second observation. The remaining three visits were scheduled in the framework of the program number CH_PR100031. Based on these CHEOPS observations, three transits of planet b were recorded during visits 1, 3, and 5, the transit of planet c was observed twice during visits 2 and 4, and a single transit of planet d (in multiple transit feature with planet c) was detected during the CHEOPS visit 4.
The imagettes are frames of 30 pixels in radius centred on the target, which do not need to be co-added before download owing to their smaller size. We used a tool specifically developed for photometric extraction of imagettes using point-spread function photometry, called PIPE 3  ; see for example  Szabó et al. (2021 Szabó et al. ( , 2022)). The PIPE photometry has a S/N comparable to that of DRP photometry, but has the advantage of shorter cadence, and therefore we decided to use this CHEOPS product in this work. The average uncertainty of the PIPE data points is 160 ppm. The PIPE CHEOPS observations were processed using the dedicated data decorrelation and transit analysis software called pycheops 4   (Maxted et al. 2022). This package includes downloading, visualising, and decorrelating CHEOPS data, fitting transits and eclipses of exoplanets, and calculating light-curve noise.
We first cleaned the light curves from outlier data points using the pycheops built-in function clip_outliers, which removes outliers from a dataset by calculating the mean absolute deviation (MAD) from the light curve following median smoothing, and rejects data greater than the smoothed dataset plus the MAD multiplied by a clipping factor. The clipping factor equal to five was reasonable in our cases, which we checked visually. With this clipping procedure, we discarded 30 data points out of 3195, which is ∼0. 9% of the CHEOPS data. The next step was the extraction of the detrending parameters. During this procedure, the software gives a list of the parameters necessary for the detrending. The most important decorrelation is subtraction of the roll-angle effect. In order to keep the cold plate radiators facing away from the Earth, the spacecraft rolls during its orbit.
We find a value of R s = 1. 117 ± 0. 009 R ⊙ , which is in 3σ agreement with the value of 1. 157 ± 0. 025 R ⊙ presented by the discoverers. We finally determined the stellar mass M s and stellar age t s using two different sets of stellar evolutionary models, the MonoTools package 8  (Osborn et al. 2022) , which is able to model transit light curves in case of multiple transits, duotransits, and monotransits, as well as multiple systems with combinations of such candidates, with both radial velocities and transit photometry. The package calculates a marginalised probability distribution across all allowed aliases for a given transit model by combining priors for each alias. The probabilities are estimated based on two major assumptions, namely that short-period orbits are highly favoured over long-period ones due to a combination of geometric probability and window function, and that planets in multi-planet systems have low eccentricities  (Kipping et al.
2013; Van Eylen & Albrecht 2015; Kipping 2018). More details about this software can be found in  Osborn et al. (2022). The TESS data described in Sect. 2. 1 were used during the fitting procedure using MonoTools. In the case of planet b, we set as input parameters the reference mid-transit time of T c = 2 458 385. 7318 BJD TDB , the orbital period of P orb = 4. 040330 ± 0. 000010 days, the transit duration (transit width) of W = 3. 4 h, and the transit depth of D = 134 ppm. In the case of planet c, the inputs were T c = 2 458 386. 1878 BJD TDB , P orb = 9. 573117 ± 0. 000020 days, W = 3. 8 h, and D = 389 ppm. For planet d, we set as input parameters the two mid-transit times detected by TESS, namely t tr,1 = 2 458 425. 1657 BJD TDB and t tr,2 = 2 459 136. 5357 BJD TDB , the transit duration of W = 6.
5 h and the transit depth of D = 478 ppm. These parameters were calculated from the TESS data alone. The orbital period aliases of planet d with a probability of p > 1% are listed in Table  5. The software MonoTools forecasted that a transit of planet d with the orbital period alias number 2 would take place on 25 October 2021, with a midtransit time of T c = 2 459 513. 1441 BJD TDB. This forecasted event was observed during the third CHEOPS visit (see Table  2 ), but the expected transit of planet d did not happen; only the transit of planet b was recorded that time. After this observation, we were able to exclude the period alias of P = 41. 8454 days from the list of possible aliases. The next forecast predicted a transit of planet d on 28 October 2021, with a mid-transit time of T c = 2 459 515.
9338 BJD TDB , which means that, in this case, the alias number 4 (see Table  5 ) was preferred as its true orbital period. This forecasted event was observed with CHEOPS during its fourth visit. This time, the transit of planet d was successfully detected together with a transit of planet c, confirming that the period alias of P = 47. 4248 days is the true orbital period of planet d. This result also confirms that the 8 See https://github. com/hposborn/MonoTools A44, page 5 of 14  A&A 674, A44 (2023)  second transit-like feature of planet d, observed by TESS in sector number 30, was a real transit event and not an instrumental artifact as considered by C22. Alternatively, the dip observed at 2 459 136. 5357 BJD TDB was a mixture of instrumental effects and the transit of planet d. With this gathered knowledge about the true orbital period of planet d, we were able to combine CHEOPS and TESS photometric observations and RV measurements in order to improve the orbital and planetary parameters of the HD 22946 system, which were previously obtained only from the TESS and RV data by the discoverers.
CHEOPS, TESS, and RV combined model In order to produce accurate planetary parameters for all three planets, we built a combined model using all available data, that is, TESS photometry (described in Sect. 2. 1), CHEOPS photometry (described in Sect. 2. 2), and ESPRESSO RVs (described in Sect. 2. 3). The combined model was built using the PyMC3 package 9  (Salvatier et al. 2016) , which performs Hamiltonian Monte Carlo (HMC) sampling, with Keplerian orbits modeled with exoplanet package 10 (Foreman-Mackey et al. 2021). We used Gaussian processes (GPs) to model the stellar variability present in the TESS light curve, opting for a simple harmonic oscillator (SHO) kernel implemented in the celerite package  (Foreman-Mackey et al. 2017 ) and a quality factor Q = 1/ √ 2, as is common for quasi-periodic stellar variability.
Therefore, we can improve the light curve by decorrelating the flux data against metadata generated for the instrument and target. To decipher which decorrelation vectors provide improvement, we ran an initial PyMC3 model for each CHEOPS visit using all available ancillary data -sin and cos of rollangle, background flux, x and y centroid positions, onboard temperature and time (which also fits short-timescale stellar variability). These parameters are normalised to have µ = 0. 0 and σ = 1. 0, and decorrelation parameters are given normal priors with µ = 0. 0 and σ set by the root-mean-square (RMS) noise for each CHEOPS visit. For each visit model, we also included parameters for any planetary transits present in order to ensure the transits would not bias the model. After HMC sampling, we assessed each decorrelation parameter using the average and standard deviations, keeping only those parameters with a Bayes Factor of BF > 1.
Despite this detrending, shorter-timescale variation can also be present as a function of roll angle (φ). Pure detrending against sin and cos of roll angle removes the largest amplitude systematic trends at low frequencies. These are those closest in timescale to the transit feature, and so a simpler detrending technique for such timescales guards against overfitting of the transit. However, the CHEOPS light curve typically 9 See https://pypi. org/project/pymc3/ 10 See https://pypi. org/project/exoplanet/ also contains systematic noise correlated with roll angle that is at a lower amplitude and higher frequency. This is not therefore adequately removed by simple sin and cos decorrelation. It is this noise that a more flexible GP is better able to model. We therefore also included a GP to model the variation of flux with roll-angle effects.
2019), and we lack the high number of RVs capable of resolving any differences in e, we chose to fit only circular orbits. In order to guard against unphysical negative values, we used broad log-normal priors for the key transit and RV amplitude parameters, that is, for R p /R s (planet-tostar radius ratio) and K (RV semi-amplitude). The quantities derived in Sect. 3. 1 are used as priors on the stellar parameters in the model. For all datasets -CHEOPS, TESS, and ESPRESSO -, we included a jitter term using a wide log-normal prior. We then sampled the combined model using the PyMC_ext 'sample' function, which is specifically written for astrophysical applications, and allows us to group independent dataset parameters (e. g. the CHEOPS visit-specific decorrelation parameters) together, thereby speeding up sampling greatly.
Search for transit-timing variations In order to look for potential TTVs, we also ran a combined model using unconstrained timing for each planetary transit thanks to the TTVorbit function of exoplanet, and an independent analysis using the Allesfitter software 11  (Günther & Daylan 2019 , 2021) , applying a nested sampling fit. Although C22 already performed such an analysis and found no obvious sign of TTVs in the system, we repeated this procedure, but in this case using the CHEOPS data as well. This means mainly that we included three transits of planet d in the analysis and used a longer time baseline. We used the same dataset as in Sect. 3. 3, which was co-fitted with a GP using the celerite SHO kernel in both cases. All planetary and system parameters were fixed as derived previously, only the GP hyperparameters, the detrending parameters, and the observed-minus-calculated (O-C) parameters for individual mid-transit times were fitted.
Both solutions are consistent with a linear ephemeris, which means we did not find any indication of a quadratic trend in the data, in agreement with the conclusion made by the discoverers. As an illustration, Estimated planet mass (♣)  2. 42 ± 0. 12 6. 04 ± 0. 17 7. 32 ± 0. 28 M p,est (M ⊕ ) Estimated planet mass (♡)  2. 61 ± 0. 27 ( †)  6. 61 ± 0. 17 ( ‡)  7. 90 ± 0. 28 ( ‡) ρ p (g cm -3 ) planet density (⋆)  18. 96 3. 15 10. 80 K (m s -1 ) RV semi-amplitude Notes. Based on the joint fit of the TESS and CHEOPS photometric data and RV observations. Table  shows  the best-fitting value of the given parameter and its ±1σ uncertainty. The fitted values correspond to quantile 0. 50 (median) and the uncertainties to quantils ±0. 341 in the parameter distributions obtained from the samples. (⋆) Only the 3σ upper limits are listed here due to the low number of the RV observations.
040301 +0. 000023 -0. 000042 days and P orb,c = 9. 573096 +0. 000026 -0. 000023 days, and expected an orbital period of P orb = 46 ± 4 days for planet d, which was estimated based on the transit duration and depth along with stellar mass and radius through Kepler's third law, assuming circular orbits. We confirmed this prediction, finding an orbital period for planet d of P orb = 47. 42489 ± 0. 00011 days. The improved ratios of the orbital periods are P orb,c /P orb,b = 2. 37 and P orb,d /P orb,c = 4. 95. Based on the Kepler database, the adjacent planet pairs in multiple systems show a broad overall peak between period ratios of 1. 5 and 2, followed by a declining tail to larger period ratios. In addition, there appears to be a sizeable peak just interior to the period ratio 5  (Steffen & Hwang 2015) ; therefore, we can say that the period ratios in HD 22946 fall into statistics and the seemingly large orbital gap between planets c and d is not anomalous.
In the combined model, we determined the impact parameter b, which is the projected relative distance of the planet from the stellar disk centre during the transit midpoint in units of R s. Converting these parameter values to the orbit inclination angle values we can obtain i = 88. 90 +0. 16  -0. 05 deg, i = 88. 52 Fig. 2. TESS observations of the transiting planets HD 22946b, HD 22946c, and HD 22946d from sector numbers 3, 4, and 30 overplotted with the best-fitting model. This model was derived based on the entire CHEOPS and TESS photometric dataset and the RV observations from ESPRESSO via joint analysis of the data. The left-hand panels show the non-detrended data overplotted with the full model, while the right-hand panels show the detrended data overplotted with the transit model. We averaged the TESS data for better visualisation of the transit events using a running average with steps and width of 0.
009 and 0. 09 day, respectively. We note that an interruption in communications between the instrument and spacecraft occurred at 2 458 418. 54 BJD TDB , resulting in an instrument turn-off until 2 458 421. 21 BJD TDB. No data were collected during this period. angle of planet d was not determined by C22. According to the improved parameter values, it seems that only the orbits of planets b and c are well aligned. planet d is probably not in the same plane as planets b and c. Based on the combined TESS and CHEOPS photometry observations, we redetermined the radii of the planets, which are 1. 362 ± 0. 040 R ⊕ , 2. 328 ± 0. 039 R ⊕ , and 2. 607 ± 0. 060 R ⊕ for planets b, c, and d, respectively. The CHEOPS observations are an added value, because compared to the corresponding parameter values presented in C22 (R p,b = 1.
We estimated that another 48 ESPRESSO RVs are needed to measure the predicted masses of all planets in HD 22946. planet c could be a suitable target for future atmospheric characterisation via transmission spectroscopy. We can also conclude that planet d as a warm sub-Neptune is very interesting, because there are only a few similar confirmed exoplanets to date. Thanks to the synergy of TESS and CHEOPS missions, there is a growing sample of planets, such as HD 22946d. Such objects are worth investigating in the near future, for example in order to investigate their composition and internal structure. Finally, we can mention that future photometric and/or spectroscopic observations could also be oriented to searching for further possible planets in this system. log σ TESS  [ppt]  log of scatter in the TESS data -2.
845   [ppt]  the average offset of the median-normalised flux -1st CHEOPS visit 0. 007 ± 0. 011 x mean,2nd,CHEOPS  [ppt]  the average offset of the median-normalised flux -2nd CHEOPS visit 0. 066 ± 0. 011 x mean,3rd,CHEOPS  [ppt]  the average offset of the median-normalised flux -3rd CHEOPS visit 0. 039 ± 0. 010 x mean,4th,CHEOPS  [ppt]  the average offset of the median-normalised flux -4th CHEOPS visit 0. 314 ± 0. 014 x mean,5th,CHEOPS  [ppt]  the average offset of the median-normalised flux -5th CHEOPS visit 0. 061 ± 0. 011 x mean,TESS  [ppt]  the average offset of the median-normalised flux in TESS data 0. 0179 +0. 0085 -0. 0084 Notes. Based on the joint fit of the TESS and CHEOPS photometric data, and RV observations. The table shows the best-fitting value of the given parameter and its ±1σ uncertainty.
Acknowledgements. We thank the anonymous reviewer for the helpful comments and suggestions. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria,  Belgium ,  France ,  Germany ,  Hungary ,  Italy ,  Portugal ,  Spain ,  Sweden , and the  United Kingdom. The  CHEOPS Consortium  would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the  Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the  NASA   Explorer Program.
A. Br. was supported by the  SNSA. A. C. C. acknowledges support from  STFC  consolidated grant numbers  ST/R000824/1  and  ST/V000861/1 , and  UKSA  grant number  ST/R003203/1. B. -O. D. acknowledges support from the  Swiss State Secretariat for Education, Research and Innovation (SERI)  under contract number  MB22. 00046. This project has received funding from the  European Research Council (ERC)  under the European Union's  Horizon 2020 research and innovation programme  (project  FOUR ACES ; grant agreement No  724427 ). It has also been carried out in the frame of the  National Centre  for Competence in Research PlanetS supported by the  Swiss National Science Foundation (SNSF). D. E. acknowledges financial support from the  Swiss National Science Foundation  for project  200021_200726.
D. G. gratefully acknowledges financial support from the  CRT foundation  under Grant No. 2018. 2323 " Gaseousor rocky? Unveiling the nature of small worlds ". This work was also partially supported by a grant from the  Simons Foundation (PI Queloz , grant number  327127 ). This work has been carried out within the framework of the NCCR PlanetS supported by the  Swiss National Science Foundation  under grants  51NF40_182901  and  51NF40_205606. I. R. I. acknowledges support from the  Spanish Ministry of Science and Innovation  and the  European Regional Development Fund  through grant  PGC2018-098153-B-C33 , as well as the support of the  Generalitat de Catalunya/CERCA programme. This work was granted access to the HPC resources of MesoPSL financed by the  Région Île-de-France  and the project  Equip@Meso  (reference  ANR-10-EQPX-29-01 ) of the programme  Investissements d'Avenir  supervised by the  Agence Nationale pour la Recherche.
K. G. I. and M. N. G. are the  ESA   CHEOPS Project Scientists  and are responsible for the  ESA CHEOPS Guest Observers Programme. They do not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. The Belgian participation to CHEOPS has been supported by the  Belgian Federal Science Policy Office (BELSPO)  in the framework of the  PRODEX Program , and by the  University of Liège  through an  ARC  grant for Concerted Research Actions financed by the  Wallonia-Brussels Federation ; L. D. is an F. R. S. -FNRS  Postdoctoral Researcher. L. M. S. gratefully acknowledges financial support from the  CRT foundation  under Grant No.