dataesr/scientific-paragraphs-categorization huggingface dataset:
g. the synthetic spectra we adopted assume V macro = 0 km s - 1  ). Therefore, while the line-broadening is measured with a classic rotational kernel, the measurement provided in the catalogue is called vbroad. For the same reason, vbroad refers to the estimate provided by the STA/MTA parts of the spectroscopic pipeline throughout, while V sin i denotes the true projected rotational velocity value (e. g. from simulations) or the value found in other catalogues or surveys (i. e. even when the catalogue or survey itself does not distinguish V sin i from other broadening mechanisms, and/or similarly calls the estimate by a different name). Another estimate of the RVS line-broadening is obtained by the ESP-HS 1 module of the Apsis 2  pipeline  (Creevey et al. 2023). It is published in Gaia DR3 as vsini_esphs (in the astrophysical_parameters table) and is an intermediate result of the analysis of the RVS and BP/RP data when the astrophysical parameters of stars with T eff > 7500 K are derived.
At the resolution of LAMOST, they were unable to distinguish macroturbulence from rotational velocities, and their V sin i estimates include its contribution. In the APOGEE pipeline (García Pérez et al. 2016), the spectral analysis is performed with FERRE (Allende  Prieto et al. 2006) , which finds the best-fitting stellar parameters describing an observed spectrum by interpolating in a grid of synthetic templates. This grid, however, is restricted in the V sin i dimension to the values 1. 5, 3, 6, 12, 24, 48, and 96 km s -1. V sin i is only determined for dwarf stars, while in the giant sub-grids, a macroturbulence velocity broadening, calibrated as a function of metallicity  (Jönsson et al. 2020) , is adopted instead. In GALAH, the stellar atmospheric parameters are derived using the spectrum synthesis code Spectroscopy Made Easy  (Piskunov & Valenti 2017).
Selection of the comparison samples The catalogues we used to compare the line-broadening scales provide in some cases a quality assessment of their data. We used these assessments to only keep the most reliable estimates as follows: -In the GALAH survey, the flag flag_sp reflects the quality of the spectroscopic parameters, and only common targets with flag_sp= 0 were taken into account. -The APOGEE catalogue also provides a flag, f_Vsini, that assesses the quality of the published V sin i determinations. Only common targets with f_Vsini = 0 are considered here. RAVE data were selected on the basis of the height of the CCF given in the catalogue: hcp > 0. 9. -LAMOST data were selected on the basis of their reduced χ 2 such that CHISQ_RED < 5. -The quality of the compiled data from GG was assessed upon the flag n_vsini that indicates when the precision A8, page 6 of 19 is poor (':') or when the datum solely originates from  Uesugi & Fukuda's compilation (1982) , whose quality was already questioned by  Soderblom et al.
in 1989. Only targets with an empty n_vsini flag were used. Figure  10  shows the data that were discarded from the comparison samples using the criteria listed above as grey bars. The cuts produced by this selection in the V sin i distributions are clear: all targets with V sin i 70 km s -1 and V sin i 100 km s -1 are removed from the APOGEE and GALAH comparison samples, respectively. Notes. The size is that of the comparison sample. targets, its intersection with the other ground-based surveys is limited. The LAMOST survey observes the northern hemisphere, whereas RAVE and GALAH are focussed on the southern hemisphere. In addition to being dedicated to hot stars, its intersection with the other ground surveys is therefore also limited. The APOGEE footprint covers both hemispheres. We emphasise that a fraction of these comparisons can be contaminated by incorrect cross-identifications when the different catalogues were cross-matched  (Pineau et al.
Two-by-two comparisons The right upper part of the panels is only populated with the catalogues that contain fast-rotating stars and are able to determine high rotational velocities. The APOGEE survey has a hard upper limit at 96 km s -1 , which partly explains why the lower right quadrant of the Gaia DR3-APOGEE panel is significantly populated. The comparison with LAMOST data is very dispersed because of the much lower resolution and possibly the larger effect of template mismatch. The catalogue content mainly A8, page 8 of 19 consists of OBA targets (T eff > 7500 K), however, therefore it allows an assessment of the vbroad quality in the higher velocity range (V sin i 100 km s -1 ). Whereas the comparison with GG seems in good agreement as soon as vbroad 15 km s -1 , a trend appears at high values (vbroad 200 km s -1 ), where vbroad determinations are systematically higher than their GG counterparts.
Discussion Figure  13  displays the variation in vbroad distribution as a function of the spectral type, as already shown by  Royer (2014) , and compares it with V sin i data from the GG comparison sample. The coloured density plot is based on 63 248 vbroad values of MS stars (3. 5 ≤ log g ≤ 4. 5) brighter than G RVS = 9. The contour plot is derived from 9262 V sin i values compiled by GG, with the same selection criterion on log g. The modes of the distribution seem consistent between vbroad and V sin i. The top panel in logarithmic scale reproduces the overestimation of vbroad at low V sin i, already illustrated by Figs. 11  and 12 , shown here by spectral types later than F5. In the bottom panel, the contour low levels for hot stars do not perfectly coincide with the vbroad distribution counts, suggesting that high-velocity distribution tails are more extended in the Gaia DR3 catalogue.
As a result, the median values are also higher by 8 to 28% from F0-to A0-type stars. This broadening of the Gaia DR3 data is produced by the trend observed between the two velocity scales in Fig. 11. The catalogue-to-catalogue correlation and residual plots of Sect. 4 reproduce the two main features identified during the MC simulations (Sect. 2. 3). The Gaia DR3 vbroad overestimates the low V sin i values, while it tends to underestimate the higher values. From the simulations (Fig. 2 ), we noted a significant impact of the template mismatches for the hot stars due to an incorrect T eff estimate. The comparisons made with the OBA LAM-OST catalogue above 100 km s -1 still present relative residuals (lower panels of Fig. 12 ) that are fairly consistent in magnitude with those found in the simulations (Fig.
Therefore, we recommend in general to remain cautious in the interpretation of the vbroad parameter values. To better help the catalogue user, we provide in Table  3  an estimate of the vbroad domains where both vbroad and its uncertainty are expected to be consistent with V sin i. During the processing of Gaia DR3, the vbroad results obtained by the method described in Sect. 2. 1 were considered. More tests will be conducted during the preparation of the next data release in order to include the estimates from other algorithms (e. g. minimum distance method and use of the CCF width). The method presented in this paper uses the information integrated over the complete RVS domain (i. e. it produces one single CCF). It has obvious advantages for the fainter targets, but it is usually also dominated by the stronger and broader features, which are less sensitive to any additional line-broadening.
Chemin); -the National Natural Science Foundation of China (NSFC) through grants 11573054, 11703065, and 12173069, the China Scholarship Council through grant 201806040200, and the Natural Science Foundation of Shanghai through grant 21ZR1474100; -the Tenure Track Pilot Programme of the Croatian Science Foundation and the École Polytechnique Fédérale de Lausanne and the project TTP-2018-07-1171 'Mining the Variable Sky', with the funds of the Croatian-Swiss Research Programme; -the Czech-Republic Ministry of Education, Youth, and Sports through grant LG 15010 and INTER-EXCELLENCE grant LTAUSA18093, and the Czech Space Office through ESA PECS contract 98058; -the Danish Ministry of Science; -the Estonian Ministry of Education and Research through grant IUT40-1; -the European Commission's Sixth Framework Programme through the European Leadership in Space Astrometry (ELSA) Marie Curie Research Training Network (MRTN-CT-2006-033481), through Marie Curie project PIOF-GA-2009-255267 (Space AsteroSeismology & RR Lyrae stars, SAS-RRL), and through a Marie Curie Transferof-Knowledge (ToK) fellowship (MTKD-CT-2004-014188); the European Commission's Seventh Framework Programme through grant FP7-606740 (FP7-SPACE-2013-1) for the Gaia European Network for Improved data User Services (GENIUS) and through grant 264895 for the Gaia disappearing rapidly in the noise, while in the hottest star (panel d), the main features are the broad lines of the Paschen series.
Acknowledgements. We thank  Dr Elena Pancino  and the anonymous referee for carefully reading the manuscript and for providing us with constructive comments that helped to improve the paper. This work presents results from the  European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the  Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the  Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www. cosmos. esa. int/gaia. The Gaia archive website is https://archives. esac. esa. int/gaia. Full acknowledgements are given in Appendix A. This work has used the following software products: Matplotlib (Hunter 2007, https://matplotlib. org),SciPy (Virtanen et al.
Anders), the  Severo Ochoa Centre of Excellence Programme  ( SEV2015-0493 ), and  MICIN/AEI/10. 13039/501100011033 (and the  European Union  through  European Regional Development Fund 'A way of making Europe')  through grant  RTI2018-095076-B-C21 , the  Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu ') through grant  CEX2019-000918-M , the  University of Barcelona 's official doctoral programme for the development of an  R+D+i  project through an  Ajuts de Personal Investigador en Formació (APIF) grant , the  Spanish Virtual Observatory  through project  AyA2017-84089 , the  Galician Regional Government, Xunta de Galicia , through grants  ED431B-2021/36 ,  ED481A-2019/155 , and  ED481A-2021/296 , the  Centro de Investigación en Tecnologías de la Información y las Comunicaciones (CITIC) , funded by the  Xunta de Galicia  and the  European Union  ( European Regional Development Fund -Galicia 2014-2020 Programme ), through grant  ED431G-2019/01 , the  Red Española de Supercomputación (RES) computer resources at MareNostrum , the  Barcelona Supercomputing Centre -Centro Nacional de Supercomputación (BSC-CNS)  through activities  AECT-2017-2-0002 ,  AECT-2017-3-0006 ,  AECT-2018-1-0017 ,  AECT-2018-2-0013 ,  AECT-2018-3-0011 ,  AECT-2019-1-0010 ,  AECT-2019-2-0014 ,  AECT-2019-3-0003 ,  AECT-2020-1-0004 , and  DATA-2020-1-0010 , the  Departament d'Innovació, Universitats i Empresa de la Generalitat de Catalunya  through grant  2014-SGR-1051  for project ' Models de Programació i Entorns d'Execució Parallels' (MPEXPAR) , and  Ramon y Cajal Fellowship   RYC2018-025968-I  funded by  MICIN/AEI/10.
Data Sources and Measurement After recruitment and informed consent, participants were offered an HIV test (rapid test in 7 sites and standard testing in 1 site) and completed a standardized, structured questionnaire collected by audio, computer-assisted self-interview at 5 sites; computer-assisted personal interview at 2 sites (REDCap and Questionnaire Development System); and computer-assisted self-interview at 1 site (Qualtrics) (see software version numbers in eMethods in Supplement 1). [56] [57] [58]  The questionnaire assessed participant self-reported characteristics and behaviors. Data were transferred to the ROI Data Coordinating Center at the University of Washington for quality review and collation of a national analytic data set.
Statistical Analysis Data were analyzed August through December 2022. We calculated summary statistics for participant characteristic variables overall and stratified by site to assess the variability and degree of association between participant characteristics and sites (Table  1   [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] Gay or lesbian 0. 90 (0. 42-1. 93)   Site IL 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference] 1 [Reference].
Gene expression analyses Total RNAs were extracted from rice root samples using the RNeasy Plant mini kit (Qiagen, France), with addition of an on-column DNase I digestion. First-strand cDNAs were synthesized from 1 μg of total RNA in 20 μl final volume using an oligo-dT(18)-MN primer (Eurogentec, France) and the Omniscript RT kit (Qiagen). Specific primers were designed from O. sativa Nipponbare sequences using Primer3Plus (https://primer3plus. com/) (S1 Table in S1 File) and checked for specificity on O. sativa Kitaake sequences. Quantitative-PCR assays were performed on cDNAs samples (diluted 1/50e) in an Mx30005P thermal cycler (Stratagene, USA) using the Brilliant III Ultra-fast SYBR 1 Green QPCR Master mix with low ROX (Agilent, Santa Clara, CA, USA). Amplifications were performed in duplicate from the five biological samples.
2015). AC Her is the only post-AGB binary system for with a large dust-free cavity was resolved so far. Near-IR observations of AC Her with the long-baseline interferometric array at the Center for High Angular Resolution reveal the three-dimensional orbit of the inner binary and show that the inner cavity cannot be explained by the dynamical truncation of the binary  (Anugu et al. 2023 ). Here we present mid-IR interferometric observations with the four-beam combiner Multi-AperTure mid-Infrared Spectro-Scopic Experiment (MATISSE) installed on the VLTI of ten Galactic post-AGB binary systems together with the reanalysis of the archival MIDI data of AC Her. We aim to constrain the sizes of the cavities of the transition disc candidates and compare them to full-disc systems using geometric models.
Observations The SEDs were taken from the catalogue of Galactic post-AGB binary systems of  Kluska et al. (2022). We used mid-IR interferometric observations of post-AGB binaries obtained with VLTI/MATISSE  (Lopez et al. 2022). MATISSE operates in the L (2. 9-4. 2 µm), M (4. 2-5. 0 µm), and N (8-13 µm) bands. MATISSE combines the light of either the four Unit Telescopes (UTs) or the four Auxiliary Telescopes (ATs) and provides six simultaneous baselines and three independent closure phases (CPs) per measurement. The interferometric observables are the visibilities and the CPs. The visibility is measured as a squared visibility amplitude (V 2  ) in the L band and the visibility amplitude (|V|) or the correlated flux (CF) in the N band. Our data set contains five systems of category 1 (HD 101584, HD 109014, IW Car, IRAS 08544-4431 (hereafter IRAS 08544), and IRAS 15469-5311 (hereafter IRAS 15469)) with an IR excess starting at near-IR wavelengths, and six systems (CT Ori, EP Lyr, AC Her, AD Aql, RU Cen, and ST Pup) with an excess starting at mid-IR wavelengths (categories 2 and 3).
The target selection for the transition disc candidates was based on (1) the lack of near-IR excess, (2) the characteristics in depletion tracers ([Fe/H] ∼ -2. 0, [Zn/Ti] ∼ 2. 0, and T turn-off ∼ 1000 K; see also Table  B. 1 and  Kluska et al. 2022) , and (3) the observability of the systems with MATISSE. The transition disc sample was complemented with data of AC Her taken with the VLTI/MIDI, which operated in the N band as it is the only system for which a dust-free cavity was detected so far. For a log of these observations of AC Her, we refer to  Hillen et al. (2015). The data of the transition disc candidates were compared to full-disc systems in the MATISSE wavelength range. All MATISSE observations were taken in hybrid mode with a low spectral resolution (R ∼ 30) between 2019 and 2023.
For a log of the observations of IRAS 08544, we refer to  Corporaal et al. (2021). Data of IRAS 15469 were taken with the ATs in the small configuration (program ID 105. 20QN, PI: Kluska). Observations of IW Car were carried out using the ATs on the small and medium configurations (program ID 106. 21NK, PI: Kluska). Data of HD 101584, HD 108015, EP Lyr, AD Aql, RU Cen, CT Ori, and ST Pup were taken using the UTs with the GRA4MAT mode using GRAVITY as a fringe tracker to stabilise the fringes of these faint targets (program IDs 109. 23KF and 110. 24AC, PI: Corporaal). The log of these observations is reported in Table  A. 1. The data were reduced and calibrated with the MATISSE data reduction pipeline version 1. 7. 5. We used all data for which no observational or calibration problems occurred (see Appendix A).
In all cases for which reliable L-and N-band data Notes. Reported values are calculated at λ 0 = 10. 5 µm. were obtained, the estimates of the inner rim radii are consistent between these bands. IW Car and EP Lyr are RVb variables (i. e. they show longterm changes in the mean brightness; e. g. ,  Kiss et al. 2007; Manick et al. 2019 ) and indeed show high inclinations (∼60 • ) in the N band. The disc of EP Lyr does not emit in L, and thus no inclination can be derived. The inclination derived for IW Car in L, however, is strongly preferred to be lower (i ∼ 50 deg) than that of other RVb stars (see also Sect. 5). The radial intensity profiles are better constrained in N, covering broader disc regions than in L. However, this is specifically the case for the full-disc sources, where MATISSE probes beyond the inner rim.
The large baseline data of ST Pup are not well reproduced. As a result of the small contribution of the disc to the total flux, any azimuthal modulations of the inner rim do not improve the fit of these baselines. The contribution of its over-resolved component is high. Smaller-scale structures such as the binary component and their respective offsets from the centre likely play a role, but have not been captured in our modelling. In N, higher χ 2 red values are for systems that show prominent silicate features in their visibility curves (AD Aql, RU Cen, and ST Pup) or for a system with a sparse uv coverage (AC Her). For AD Aql, RU Cen, and ST Pup, only the general trend could be reproduced with these geometric modelling because no specific dust species was assumed. The small-baseline data (probing larger scales) of AC Her are not well reproduced with our modelling, while the larger-baseline data and the location of the first zero are reproduced well.
Acknowledgements. We thank the referee for their constructive comments and suggestions that substantially improved the clarity of the paper. A. C. and H. V. W. acknowledge support from  FWO  under contract  G097619N. J. K. acknowledges support from  FWO  under the senior postdoctoral fellowship ( 1281121N ). This project has received funding from the  European Research Council (ERC)  under the  European Union   Horizon Europe programme  (grant agreement No. 101042275 , project Stellar-MADE). D. K. and K. A. acknowledge the support of the  Australian Research Council (ARC)   Discovery Early Career Research Award (DECRA) grant  ( DE190100813 ). This research was supported in part by the  Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions  ( ASTRO 3D ) through project number  CE170100013.
To clarify the magnetic order in each phase we performed single crystal small-angle neutron scattering (SANS) measurements. SANS is generally sensitive to magnetic order if the Fourier transform of the local magnetisation density contains incommensurately modulating spin components m Q ð Þexp iQ Á r ½ + c:c: where components of m Q ð Þ are normal to Q. Here m Q ð Þ is a complex vector and c. c. denotes complex conjugate. Figure  3a  illustrates the transmission geometry of the experiment, where H was applied parallel to both [001] and the neutron beam (see Methods for full details). Typical SANS data summarising the H-evolution of the magnetic order at 1. 9 K during the Hincreasing process are shown in Fig. 3b-h. Starting in the ground state phase I, the SANS data shown in Fig. 3e  agree with previous works  33, 34.
Crystal growth and characterisation Single crystals of EuNiGe 3 were grown by the In-flux method. The phase purity and crystallographic parameters of single crystal samples were confirmed by single crystal X-ray diffraction at room temperature using a STOE STADIVARI four-circle diffractometer equipped with a Dectris EIGER 1 M 2 R CdTe detector and incoming micro-focused Ag Kα radiation of wavelength 0. 56083 Å. Data reduction and correction were performed using the X-Area package  54. Solution, refinement, and absorption correction were done utilizing the JANA 2020 software (version 1. 3. 51)  55. Good agreement between measured and refined intensities of over 331 reflections (184 unique) confirmed our crystals to display the nominal occupancy of the different atoms within uncertainty, and tetragonal lattice parameters of a = 4.
Small-angle neutron scattering (SANS) measurements Unpolarised SANS measurements were carried out using the SANS-I instrument at the Swiss Spallation Neutron Source (SINQ), Paul Scherrer Institute, Switzerland. The SANS data were obtained from ∼5 mg single crystals of typical volume 2 × 2 × 0. 15 mm 3. The widest (001) plane was aligned initially along the neutron beam. The crystal was mounted inside a superconducting cryomagnet providing temperatures down to 2 K, and magnetic fields up to 6. 8 T along the c-axis. The neutron wavelength was selected to be 3. 1 Å (Δλ/λ = 17 %). The incoming beam was collimated over 3 m before the sample, and scattered neutrons collected by a multi-detector placed 1. 85 m behind the sample. The momentum-space resolution in the region of the observed Q-vectors was ∼ 0.
The incoming beam was collimated over a distance of 7. 8 m before the sample, and scattered neutrons collected by a multi-detector placed 1. 9 m behind the sample. In the defined wavelength band, the momentum-space resolution in the region of the observed Q-vectors was ∼0. 03 Å -1. The polarising efficiency of the setup, characterised by the flipping ratio, was measured and found to vary from 6-8 depending on the wavelength and H. By measuring all possible neutron-spin-state combinations of the unscattered beam, fully quantitative corrections for imperfections of the overall polarising efficiency are applied in the data analysis. All unpolarised and polarised SANS data analysis was carried out using GRASP software  57.
Theoretical calculations Spin density functional theory (SDFT) calculations for EuNiGe 3 were performed based on the projector augmented wave scheme  58  implemented in the Vienna ab initio simulation package  59, 60. The lattice constants and the atomic positions were taken from the experiment  61. The exchange correlation functionals proposed by Perdew-Burke-Ernzerhof  62  , E cut = 450 eV as the cutoff energy for the plain wave basis set, and N k = 10 × 10 × 10 as the number of k-points were used in the self-consistent field calculations. For the calculations of the paramagnetic state, we used the open core potential with 4f 7 configuration for Eu element. To illustrate the Fermi surfaces with dense k-grid, we used the Wannier interpolation technique by using the WANNIER90 package  63, 64.