dataesr/scientific-paragraphs-categorization huggingface dataset:
2021). The amplitude and period of Europa's libration potentially provides information about the thickness and rigidity of the ice shell. On average, Europa presents the same face toward Jupiter, but the eccentricity of its orbit leads to a variable orbital velocity, and hence libration. The forced libration, which is the component due to Jupiter's gravitational torque on the dynamic figure of Europa, is of interest in potentially providing geophysical information. However, while the libration amplitude can be large (130 m; Bills 2005), the sensitivity to the ice shell thickness is poor except in the case of a very thin crust  (Van Hoolst et al. 2013). The EIS NAC will acquire a geodesy dataset of 50-100 m/pixel framing images, covering all longitudes and obtained as much as possible near the extrema of libration.
This procedure assumes that the body is in a Cassini state, a state of minimum energy that accounts for the coplanarity of spin, orbit precession, and orbit angular velocity  (Peale et al. 2002). By combining measurements of Europa's ephemeris and orientation, Europa Clipper will allow us to confirm whether the icy moon is in a Cassini state, and thus whether we can measure the polar moment of inertia directly from the measured obliquity, which is expected to be ∼0. 05°  (Chen et al. 2014). Radiometric Doppler data collected by Europa Clipper during all close encounters will provide critical information on Europa's ephemerides. Doppler data acquired near the pericenter are very sensitive to the relative position of the spacecraft with respect to the moon. Gravitational torques exerted on the ice shell by an asymmetric silicate interior should provide a strong coupling mechanism on the long timescales of the pole precession  (Van Hoolst et al.
The principal method of acquiring such topography is REASON altimeter, EIS WAC three-channel stereo (NAC targeted stereo is also possible), and limb profiles. All of these datasets must be controlled to each other and co-analyzed for the best results. The measurement of transects across topographic elevations either from digital terrain models or by the collection of REASON altimetry groundtracks or limb profiles allows determination of the thickness of the elastic portion of the ice shell. On terrestrial as well as on icy bodies, the topography at short baselines is often supported by the flexure of the cold upper layer of the crust. By measuring this flexure from the elevation profiles and by assuming a range for the rheological properties of the ice, the effective elastic thickness of the shell can be inferred.
Surface Composition MISE, EIS, and Europa-UVS will map Europa's surface composition at global and regional scales at unprecedented resolution (> 70% of the surface at 10-km/pixel scale) over a 0. 1-5 µm spectral range. EIS color data can reveal color centers characteristic of irradiated chlorides. Oceanic material that erupted onto the surface (e. g. , at chaos regions or condensed as cryovolcanic plume fallout) will be sputtered by high-energy particles and then sampled by MASPEX and SUDA. Together with Europa-UVS, these instruments will measure the abundance of key exospheric species (e. g. , H 2 O, O 2 , H 2 ) and trace organics and salt derivatives (Na and K). MASPEX measurements of the composition of low-weight organic volatiles as well as potential ice grains may point to the presence of clathrate hydrates in the crust (see  Becker et al.
7. In an idealized case, these three investigations alone would provide us with a solution to the three quantities identified in the Europa Clipper's Level-1 science requirements. However, such precision would require both that the measurements themselves have zero uncertainty (which is an unrealistic scenario) and that the equations are linearly independent. Additional information to resolve this potential inherent nonlinearity is provided in the form of the auxiliary measurements described in Sect. 2. 4. These additional datasets can provide context, which can serve to narrow the parameter space and simplify the relationships. Although no single instrument can fully characterize the ice shell, a combination of measurements provides a much more complete picture. Figure  8  provides a hypothetical example of how this synergy can work in practice.
The subsurface sounding experiment characterizes the shallow subsurface and will constrain the thermophysical structure of the ice shell. These will result in an estimate of the minimum thickness of Europa's ice shell and narrow down the thickness of the conductive portion of the ice. The tidal deformation measurements are sensitive to a combination of the thickness of the ice shell and its rigidity, providing an additional independent constraint on the thickness of the elastic portion of the ice shell. While each of these investigations alone will reveal critical information about the interior of Europa, none of them can provide a comprehensive view. Together, they support each other and are highly complementary. Combining multiple datasets is a powerful way of characterizing the interior of Europa and habitability of its subsurface ocean.
Acknowledgements We thank  David Hinkle  of  JPL  for creating the cutaway Fig. 1 illustrating the potential interior of Europa. We thank two anonymous referees whose thorough reviews have substantially improved the paper. This work was supported by  NASA  through the  Europa Clipper  project. A portion of this work was carried out at the  Jet Propulsion Laboratory, California Institute of Technology , under contract with the  National Aeronautics and Space Administration. No new data were used in producing this manuscript.
Data analysis The measurements of inclusive, prompt, and non-prompt J/ψ production were performed in a similar way to previous analyses in pp and p-Pb collisions at other centre-of-mass energies  [20, [32] [33] [34]. However, in this article TRD-triggered events were used for the first time for the J/ψ analysis. The minimum J/ψ p T of the TRD-triggered analysis is 2 GeV/c, where the single-electron efficiencies result in a J/ψ efficiency of about 10% increasing with rising p T , as shown in section 3. 1. For the measurement in the p T interval 0-2 GeV/c, the small available MB data sample was used. In a first step, tracks with good quality were selected, which in addition had to fulfil the requirement of a minimum transverse momentum of 1 GeV/c and a pseudorapidity of |η| < 0. 84 to reject tracks outside the TRD kinematic acceptance.
For the non-prompt J/ψ, PYTHIA 6. 4  [36]  was used to generate the bb pairs hadronising into beauty hadrons, subsequently forced to decay into J/ψ. The J/ψ decays were then simulated using the EvtGen package  [37]  together with the PHOTOS model  [38]  for a proper description of the QED radiative decay channel (J/ψ → e + e -γ). The MC simulation assumes the prompt J/ψ to be unpolarised, while the non-prompt J/ψ JHEP07(2023)137  Invariant mass distribution of e + e -pairs from J/ψ decays and from correlated and uncorrelated background sources for the lowest (left) and the highest (right) p T interval considered in the analysis. For the highest p T interval, the distributions were scaled by a factor 4 for better visibility. have a small residual polarisation arising from the contributions of the different b-hadron decay channels as implemented in EvtGen  [37].
However, no significant conclusion can be drawn due to the limited size of the MB data sample. To enhance the precision of the p T -integrated R pPb value, an extrapolation down to zero-p T of the cross section measured with the TRD-triggered data sample is used instead of the minimum bias result. The measured visible cross section for p T > 2 GeV/c corresponds to about two-thirds of the p T -integrated cross section at midrapidity. The extrapolation JHEP07(2023)137 method uses the p T measurement in p-Pb collisions at √ s NN = 5. 02 TeV assuming that cold nuclear matter effects influencing J/ψ production are the same at both collision energies. This is very well supported by the findings at forward and backward rapidity by the ALICE and LHCb collaborations within their present measurement accuracy  [22, 23].
The calculation by Vogt et al. is based on a pure shadowing scenario employing the next-to-leading order (NLO) Color Evaporation Model (CEM) with the EPS09 shadowing parametrisation  [71]. This older parton JHEP07(2023)137  distribution function was obtained before collider data were available. The calculation by Arleo et al. [72]  includes effects of momentum broadening, coherent parton energy loss and no nuclear shadowing of the gluon PDF. The model by Zhuang et al. [12]  includes final-state effects (so-called hot nuclear matter effects), where the cc states interact with the system generated in the collision, as well as nuclear shadowing using the EPS09 gluon nPDF. The theoretical models describing the forward and backward rapidity results, also agree within uncertainties with the measurement at midrapidity.
Also depicted is the transport calculation by Du et al. [13] , based on the kinetic rate-equation approach within a fireball model and previously used for heavy-ion and d-Au collisions, for the p-Pb collision system. Shadowing effects were considered in the calculation by Vogt et al. via the pre-LHC EPS09 nPDFs. The theoretical calculations describe the low p T data where the model should be applicable. The calculation by Lansberg et al. [68]  tends to be systematically below the data in the p T range below 10 GeV/c, only approaching unity at 20 GeV/c. The approach based on the CEM and EPS09 nPDFs as well as the NLO pQCD calculation of Duwentäser et al. are closest to the data. The latter calculation has the smallest uncertainties profiting from the latest version of the nCTEQ15HQ nPDF set.
This research was approved by the Institutional Review Board [anonymized for peer review] (Research Protocol 2017-1027). All studies are reported, and no subject was removed from the original databases. Sample sizes for each study was determined a priori and without any extension on the basis of initial looks at the results. However, because not all participants answered every question, we used pairwise deletion on the variables for which we did not have re-sponses. Consequently, the number of participants in each analysis fluctuates a little around the total sample size.
86). We recruited 199 undergraduate students (32. 00% male; Mage = 19. 15, SD = 1. 42). A sensitivity analysis showed that this sample enabled us to detect an effect size of ρ = 0. 20 at 80% power. As in Study 1, participants completed a computerized questionnaire that was sent to them via email but instead participated in exchange for course credit. All other measures were the same: Feelings thermometer about the deviant fans rUS =. 67, and rAustralia =. 74; blame rUS =. 80, and rAustralia =. 84; punishment; and a 9 fine. The primary analyses were conducted on evaluations of the deviant fans in an independent-samples t-test, but the results do not change when analyzed as a mixeddesign (see the supplementary information on the OSF for these analysis). Therefore, these data were computed as if they came from a between-subjects design to fit with the rest of the studies.
Study 4 (France, 2016) A paper-pencil questionnaire was distributed among 143 undergraduate students (21. 70% male; Mage = 19. 20, SD = 1. 23) in exchange for course credit. A sensitivity analysis showed that this sample enabled us to detect an effect size of ρ = 0. 23 at 80% power. Participants were asked to read the answers of a young vs. old person target to a previous research questionnaire about homosexuality. In the 2016 European Social Survey (ESS), 88. 3% of French respondents indicated that they at least 'agreed' with the statement that 'Gays and lesbians should be free to live life as they wish', indicating that homophobia is at least a somewhat deviant attitude. Analyses were conducted using the ESS online analysis tool. Weights were applied according to recommendations by the Weighting European Social Survey Data guide.
Results All dependent variables were z-scored, and all analyses were independent-samples t-tests. Across all studies and all dependent measures, we did not find any evidence for an effect of group membership on deviance punishment. More precisely, we found no 13 evidence for the prediction that deviant ingroup members would be evaluated more harshly than deviant outgroup members (see Table  1 ). Therefore, we conducted a minimeta analysis of our results  (Goh et al. , 2016)  to limit the risk of making Type II errors regarding the existence of this effect in our datasets. We meta-analyzed the results of the present six studies using the Major package for Jamovi  (Hamilton, 2018). Means and standard deviations from all studies were weighted by sample size for their respective experimental group (Restricted Maximum-likelihood with mean standardized differences).
The final sample size was N = 1132 (Mage = 23. 83, SDage = 4. 78, 27. 27% male). As can be seen in Figure  1 , we found no evidence for the presence of the effect of group membership on deviance punishment in our data, b = -0. 01, 95% CI[-0. 07, 0. 06], SE = 0. 03, Z = -0. 15, p =. 88. Effect size was d = -0. 01, 95% CI[-0. 07, 0. 06] and model AIC = -13. 61, log-Likelihood = 8. 81. As an alternative way of conducting the metaanalysis, a mixed model was computed with dependent variables as a nested factor within studies within countries according to the following equation: judg cond + (1 | dv/study/country). Results from this analysis and scripts can be seen in the 'supplementary analysis' section (https://osf. io/5mqgw/) and converge in finding no support for substantial differences between in and outgroup deviant targets, t = 0.
Aims. We aim to measure very precise and accurate model-independent masses and distances of detached binary stars. Precise masses at the <1% level are necessary to test and calibrate stellar interior and evolution models, while precise and independent orbital parallaxes are essential to check for the next Gaia data releases. Methods. We combined RV measurements with interferometric observations to determine orbital and physical parameters of ten double-lined spectroscopic systems. We report new relative astrometry from VLTI/GRAVITY and, for some systems, new VLT/UVES spectra to determine the radial velocities of each component. Results. We measured the distance of ten binary systems and the mass of their components with a precision as high as 0. 03% (average level 0. 2%). They are combined with other stellar parameters (effective temperatures, radii, flux ratios, etc.
Despite these limitations, we have spectra of really good quality with a high signal-to-noise ratio (S/N), ranging from ∼30 to ∼500. Raw data were reduced using the UVES pipeline v6. 1. 6 within the EsoReflex environment  (Freudling et al. 2013). To extract the RVs, we used the broadening function (BF) formalism  (Rucinski 1999)  implemented in the RaveSpan software 1  (Pilecki et al. 2017 ; see also e. g. Pilecki et al. 2018 Pilecki et al. , 2013;; Gallenne et al. 2016; Graczyk et al. 2015). We used templates from the synthetic library of LTE spectra of  Coelho et al. (2005)  in the range 3760-4520 Å, 4625-5600 Å, and 5675-6645 Å (corresponding to the BLUE, REDL, and REDU UVES spectra). For some stars, the S/N was low in the blue part, so we only kept the red part. The templates were chosen to match the atmospheric properties of the hottest star in the systems.
2002). The HARPS spectrograph provides a high spectral resolution of R ∼ 115 000 in the wavelength range 3800-6900 and allows for precise RV measurements. The data were reduced by the instrument data reduction software. Our spectroscopic dataset was supplemented with public HARPS-reduced spectra downloaded from the ESO archive 2  and public SOPHIE-reduced spectra downloaded from the dedicated database 3. SOPHIE (Spectrographe pour l'Observation des Phénomènes des Intérieurs stellaires et des Exoplanètes,  Bouchy & Sophie Team 2006)  is also a visible echelle spectrograph providing a resolution R ∼ 40 000 in high-efficiency mode. All RVs were estimated the same way as described previously. A summary of the RVs used is listed in Table  2.
1 and detailed in Table  D. 1, were selected using the SearchCal 4  software  (Bonneau et al. 2006 (Bonneau et al. , 2011;; Chelli et al. 2016)  provided by the Jean-Marie Mariotti Center (JMMC). The data were reduced with the GRAVITY data reduction pipeline described in  Lapeyrere et al. (2014). The main procedure is to compute squared visibilities and triple products for each baseline and spectral channel, and to correct for photon and readout noises. In Fig. 1 , we present an example of the observables for one observation of AK For. The binary nature of the system is clearly detected. For each epoch, we proceeded to a grid search to find the global minimum and the location of the companions. For this, we used the interferometric tool CANDID 5   (Gallenne et al. 2015)  to search for the companion using all available observables.
2014) , the resulting spectral accuracy is expected to be of the order of the spectral resolution: in high resolution mode (R ∼ 4000), the spectral accuracy is expected to be ∼0. 55 nm (0. 025%), whereas in medium resolution (R ∼ 500), it is expected to be ∼4. 4 nm (0. 2%). One can verify the final accuracy of the spectral calibration by fitting the telluric features in the GRAVITY spectra. We did this using PMOIRED 6  (Mérand 2022) using a synthetic interpolated grid of telluric spectra computed with MOLECFIT  (Smette et al. 2015). For the AK For dataset, we find an average wavelength bias per epoch ranging from ∼-0. 006% to ∼+0. 019% in both medium and high spectral resolution mode. The spectral calibration is displayed in Fig. A. 1. This confirms that taking the spectral resolution for the accuracy of the spectral calibration is a reasonable choice in high resolution, whereas it is better than expected in medium resolution.
2014)  to measure the static aberrations of the science channel and to construct a complex aberration map, which is then used in fitting a binary model to complex visibilities. They present a binary test case with a 200 mas separation observed with the ATs, and show that accurate astrometry mostly depends on a consistent treatment of the pupil-plane distortions rather than a precise fibre alignment. They also demonstrate that in the specific case of the S2 orbit around the Galactic Centre, phase aberrations introduced a shift up to 0. 5 mas on the separation, which is not negligible. In this paper, our binaries have angular separations substantially smaller than the binary cases reported by GRAVITY Collaboration (2021). To quantify the effect of static aberrations on smaller binary separations, we performed our own test using the public script provided by the GRAVITY team to create aberration maps 7  and extract the amplitude, phase error, and intensity at the given position in the fibre.
Our tests consisted in comparing different binary star models (i. e. various separations and flux ratios) with and without static aberrations in order to assess an additional systematic uncertainty. We created binary models of two unresolved stars with flux ratios of 5%, 10%, 30%, 50%, and 80%; separations of  2, 5, 10, 15, 20, 30, and 50 mas; and projection angles of 0, 45, 90, 135, 180, 225, 270, and 315  • (we set the typical error of 2% on the visibilities and 0. 5 • for the closure phases). In addition, for each position (∆α, ∆δ), we added a random offset in the range  [-0. 3, 0. 3] mas at each telescope (from a uniform distribution) to take possible fibre misalignments into account. We chose this range because it corresponds to about twice the mean value of all offsets of our entire dataset 8.
AK Fornacis This is a low-mass eclipsing binary system composed of two similar main-sequence stars in a 3. 98 d orbit. Hełminiak et al. (2014)  studied this system using both RVs and photometry during eclipses and derived very precise stellar parameters. We used the RVs they reported (from the CORALIE and FEROS spectrographs) and we complemented the dataset with HARPS data. A zero-point offset between our RVs and those from  Hełminiak et al. (2014)  were determined by fitting each dataset independently, and taking the difference in the systemic velocities. We found an offset of +261 m s -1 which we added to the HARPS RVs. Our final parameters measured from our combined astrometric and RVs' orbital fit are listed in Table  6 , and the orbit  + 10] T p (days) [T p,0 -10, T p,0 + 10] e [0, 1] K 1 (km s -1 ) [K 1,0 -10, K 1,0 + 10] K 2 (km s -1 ) [K 2,0 -10, K 2,0 + 10] γ 1 (km s -1 ) [γ 1,0 -10, γ 1,0 + 10] γ 2 (km s -1 ) [γ 1,0 -10, γ 1,0 + 10] ω ( • ) [0, 360] Ω ( • ) [0, 360] a (mas) [0,300] i ( • ) [0, 180] Notes.
o Leo This system is composed of a F8-G0 giant star and a hotter A7m III-IV companion, as identified by  Ginestet & Carquillat (2002). Hummel et al. (2001)  presented the first threedimensional solution by combining photoelectric RVs and astrometry from interferometry. They measured M 1 = 2. 12 ± 0. 01 M , M 2 = 1. 87 ± 0. 01 M , and d = 41. 4 ± 0. 1 pc. The composite spectra were more deeply studied by  Griffin (2002)  who determined effective temperatures of 7600 K and 6100 K for the giant and dwarf component, respectively. Piccotti et al. (2020)  updated the orbit with new RVs from  Massarotti et al. (2008)  and measured M 1 = 2. 093 ± 0. 068 M and M 2 = 1. 857 ± 0. 058 M. We obtained new UVES spectroscopic and interferometric data to improve the solutions and to obtain more precise masses and distances.
In our combined fit displayed in Fig. 5 , we used the RVs of  Graczyk et al. (2022) , which are the most precise and they were also determined with the broadening function method from the RaveSpan software. We measured the masses at a 0. 08% precision and the distance at 0. 2%. Our masses are in good agreement with those measured by  Graczyk et al. (2022)  at a ∼0. 5σ level, but they are in slight agreement (∼2σ) with  Sybilski et al. (2018). However, they assumed a fixed eccentricity in their fitting process which likely results in underestimated uncertainties because the masses are directly linked to the eccentricity such that M ∝ (1e 2 ) 3/2. As a check, we combined our astrometry with their RVs and found an agreement at 1. 1σ with our values. In addition, RVs from  Sybilski et al. (2018)  are less precise and accurate than ours, providing a reduced χ 2 of the secondary RVs larger (χ 2 r = 15.
05, 0. 1, and 0. 2 for M 1. 2 M , 1. 2 M < M < 1. 3, and M 1. 3 M , respectively. We retrieved several isochrones from the PARSEC database tool 10 , with ages ranging from log t = 6. 6 to 10. 13 with a step of 0. 05 (i. e. ∼0. 005-13 Ga), and metallicities from Z = 0. 003 to 0. 06 (i. e. -0. 7 ≤ [Fe/H] ≤ +0. 6, using [Fe/H] ∼ log (Z/Z )), with a step of 0. 001 (fine enough to avoid re-interpolation). The BaSTI isochrones are pre-computed in their database 11 , we downloaded models for t = 0. 1-9. 5 Ga by a step of ∼0. 2 Ma and Z = 0. 002, 0. 004, 0. 008, 0. 01, 0. 0198, 0. 03, and 0. 04 (i. e. -1. 0 ≤ Fe/H ≤ 0. 3). For fitting purposes, we created an interpolated grid of the BaSTI isochrones in Z, from 0. 002 to 0. 04 with a step of 0. 001. We also computed MIST isochrones from their database tool 12 using the standard age grid from 0.
(2010). As the flux ratio is close to 1, we found similar temperatures between the stars (error is the stan-A119, page 14 of 30 dard deviation between the relations). This is consistent with 5996 ± 330 K estimated by Gaia (assuming a single star). To go a step further, we disentangled our UVES spectra and estimated the effective temperatures. For disentangling, we used all spectra with the RaveSpan software which utilises the method presented in  González & Levato (2006). We ran two iterations choosing a median value for the normalisation of the spectra. We then performed a spectral analysis using the Stellar Parameters And Chemical abundances Estimator code SP_Ace 15   (Boeche & Grebel 2016). This tool employs a new method based on a library of general curve-of-growth (GCOG) in the spectral range 4800-6860 Å.