dataesr/scientific-paragraphs-categorization huggingface dataset:
No. 05P15HGFNA , No. 05P19HGFNA , No. 05P21HGFN1 , No. 05P15UMFNA , and No. 05P21UMFN1 ) and the  Max-Planck Society. J. E. gratefully acknowledges financial support through  NWO-natuurkunde Projectruimte grant  (Project No. 680-91-103 ) and support from the  Rosalind Franklin  Fellowship program partly financed by the  European Commission  under  Marie Sklodowska -Curie Action FP7 MSC COFUND scheme. M. L. acknowledges funding from the  European Research Council (ERC)  under the European Union's  Horizon 2020 research and innovation program  (Grant Agreement No. 819957 ). D. R. and M. G. acknowledge support from the  Spanish MICINN  (Project No. FPA2015-67694-P  and  PID2019-104093GB-I00/AEI/10. 01339/501100011033 ). We acknowledge  M. Wang  and  W. Huang  from the  Institute of Modern Physics, Chinese Academy of Sciences in Lanzhou, China , for their atomic mass evaluation.
Acknowledgments. We would like to thank an anonymous referee and the Associate Editor, who made a number of very helpful suggestions. We would also like to thank  Ellen Powell  for useful comments and our industrial partners, specifically  Prof. P. Smith  and  Dr. G. Dobson  of the  ANSWERS group from Jacobs , for the use of the picture in Figure 1. Funding. The SCH, AEK and MW were supported by  EPSRC  grant  EP/P009220/1.
Global search of the EL parent body There are 15 putative X-complex families  (Nesvorny et al. 2015; Delbo et al. 2019 ) and, as a first criterion, we investigated which of them have geometric albedo values (p V ) compatible with those of the ELs. To do so, first we retrieved all the EL spectra from the Reflectance Experiment Laboratory (RELAB) and the Planetary Spectrophotometer Facility (PSF) meteorite spectra databases and using the method of  Beck et al. (2021)  we calculated their average geometric visible albedo p V and its standard deviation, finding a value between 0. 11 and 0. 23 (Fig. 1B ). For each of these asteroid families, we then retrieved from the Minor Planet Physical Properties Catalogue the p V -values of their members, and computed their average  (Table A. 1). Twelve families can be excluded as the source of the ELs because their average p V -values are out of the range of the ELs (Fig.
2019). It is natural to attempt to assign Athor members with Zitatype spectra to the Zita family and vice versa. However, we carefully inspected (i) whether or not the Zita-type asteroids that were originally assigned to the Athor family  (Delbo et al. 2019)  are placed inside the V-shape of Athor family, and (ii) whether or not their orbital elements are overlapping with the Zita family as well, and vice versa. We also visually inspected the spectra of each asteroid in order to assess the possibility that they were spectrally misclassified, that is, members of Athor and Zita are required to be within the spectroscopic X-complex. We find that asteroids (10 309) and (21 475), previously classified within the X-complex on the basis of spectrophotometric data and consequently originally included in Zita family, are in reality S-types, and should therefore be excluded from the Zita family.
In the search for an answer, we proceeded as follows: First, we calculated the average reflectance spectrum of all the ELs present in the RELAB and PSF databases after their normalisation to 1 at 0. 55 µm. We find that the EL reflectance spectra have very small dispersion with a relative standard deviation of <2. 5% between 0. 7 and 2. 5 µm, implying that EL spectra are very similar to each other. Using the method described in Appendix B. 2, we then found that only the Xc and the Xe Bus DeMeo spectral types provide a spectral curve match to the normalised reflectance spectra of ELs. However, the absolute reflectance value (p V ) of Xe is out of the range of ELs. We therefore deduce that only Xc asteroids with p V between 0. 11 and 0. 23 provide a good match to the ELs. In addition to the Athor family members, we also pinpointed nine asteroids that appear to be Xc-types with p V values in the EL range.
We calculated that the size of the Athor family progenitor (the parent body of the family), finding a value of 64 km in diameter. However, the most likely diameter of the EL original planetesimal is 240-420 km, as is estimated by best-fitting thermal evolution models to EL thermo-chronometric data  (Trieloff et al. 2022). A planetesimal of the size of the Athor family progenitor would have been too small and would therefore have had an excessively fast cooling rate to be consistent with the EL thermo-chronometers, which instead indicate a slow cooling rate  (Trieloff et al. 2022). The only possibility to explain the size difference between the Athor family progenitor and the original EL planetesimal is that the Athor family progenitor was a 64 km-diameter collisional fragment of the much larger EL planetesimal (Fig.
Conclusions We report the discovery of a unique source of the rare EL enstatite chondrite meteorites, namely the Athor asteroid family. The EL original planetesimal accreted in the terrestrial region and a comparison of its size to that of the Athor family progenitor suggests that the former broke via an impact, and a fragment of it (the progenitor of Athor) was transported into the inner main belt. The latter suffered a new catastrophic collision, forming the currently observed Athor family. NIR spectra (black points) were obtained from our survey and are presented after we applied a 2σ clipping in order to eliminate the scattered datapoints inside the telluric bands (grey areas) by as much as possible. We also present their existing VIS counterpart (grey points) obtained also from our survey or retrieved from the literature, as well as the SDSS data (red points).
In order to match the Athor family average spectrum we used the databases of the meteorite reflectance spectra from RELAB (Brown University) and PSF (University of Winnipeg). L9, page 9 of 13 For curve matching, we performed a Monte Carlo simulation, where at each iteration, the Athor family average reflectance R(λ) is varied within the standard deviation of the reflectance distribution of the family members σ(λ) and compared to all meteorite reflectances R(λ) M. For this, we again use Eq. B. 2 assigning O = R, M = RM , and σ = σ. The meteorite spectrum scoring the best comparison (minimum χ 2 M ) was recorded. After 10 5 Monte Carlo iterations, the distribution of scoring is a good approximation of the probability that a meteorite spectrum matches the average reflectance of Athor family members.
Acknowledgements. We acknowledge support from the  ANR   ORIGINS  ( ANR-18-CE31-0014 ). CA was supported by the  French National Research Agency  under the project " Investissements d'Avenir" UCA JEDI  ( ANR-15-IDEX-01 ) and by a  European Space Agency Research Fellowship. AM acknowledges support from the  ERC  advanced grant HolyEarth N. 101019380. KJW acknowledges support through  Project ESPRESSO , a  NASA   SSERVI program  at  SwRI. CA and MD were Visiting Astronomers at the  Infrared Telescope Facility , which is operated by the  University of Hawaii  under contract  80HQTR19D0030  with the  National Aeronautics and Space Administration. This work is partially based on observations collected at  Copernico telescope (Asiago, Italy) of the INAF -Osservatorio Astronomico di Padova. These results made use of the  Lowell Discovery Telescope at Lowell Observatory.
Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the LDT in partnership with  Boston University , the  University of Maryland , the  University of Toledo ,  Northern Arizona University and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from  John  and  Ginger Giovale  and by a grant from the  Mt. Cuba Astronomical Foundation. This work is based on data provided by the  Minor Planet Physical Properties Catalogue  ( MP3C ) of the  Observatoire de la Côte d'Azur  (mp3c. oca. eu). Meteorite spectra acquired from the  NASA RELAB facility  ( Brown University ) and Planetary Spectrophotometer Facility ( University of Winnipeg ) databases. We thank  S. J. Bus ,  A. C.
µmreflectance ratio vs. 0. 56 µm absolute reflectance plot for the reflectance spectra of those carbonaceous chondrites passing the curve-matching step and for all EL and EH reflectance spectra in the RELAB and PSF databases including those passing the curve-matching step. The filenames of the curve-matched meteorites are given in TableB. 3. 8 7 Number of asteroids 2 3 4 5 6 Asteroid Number 161 689 757 1490 1998 1998 2015 Original Membership Athor core Zita Athor core Athor halo Athor halo Athor halo Athor halo NIR This work This work This work n/a This work This work This work VIS (a) This work (a) This work This work (a) This work SDSS n/a n/a yes n/a yes yes yes NIR Slope %µm -1 7. 22 ± 0. 1 25. 35 ± 0. 33 6. 19 ± 0. 15 -8. 80 ± 0. 14 8. 80 ± 0. 14 22. 84 ± 0. 29 Spectral Class Xc, Xn T, X Xe, Xc Xe, Xc Xc, Cgh Cgh, Xc X, Xk p V 0.
A further matching parameter is the absolute value of 5 10 15 20 25 30 NIR slope (% m 1 ) 0 File name Database Group ccmt40. txt RELAB EH c1mt122c. txt RELAB EH 90814c. 011. txt PSF CV camt40. txt RELAB EH camp226. txt RELAB CM chmt40. txt RELAB EH clmb64. txt RELAB CM 091104a. 016. txt PSF EH 90814c. 012. txt PSF CV s1tb46. txt RELAB Aubrites cgn021. txt RELAB EL c1mp226a2. txt RELAB CM mgn021. txt RELAB EL c1mt122d. txt RELAB EH cgn017. txt RELAB EL cgn019. txt RELAB EL mgn017. txt RELAB EL ing angle 0 0 the 1. 8/0. 8 the reflectance, which is typically calculated at 0. 56 µm. We addressed this matching at a second step. Initially, using an established procedure (Eq. 2 from Beck et al. 2021), we cor- rected the meteorite absolute reflectances, which are typically measured with an emission angle of 30 • and incident illuminat- (Cloutis et al.
Its unprecedentedly close approach to the Sun will also create a unique opportunity to carry on measurements of neutrons in the close vicinity of the Sun that decay very rapidly and may not be detected by any other satellite. They are very important in the determination of small-scale physical processes producing high energy particles such as micro-and nano-flares. ICARUS I will be completely focused on in situ measurements and from 20-30 solar radii until returning to the similar distances around another pole of the Sun it will perform rapid measurements of plasma distribution functions, from thermal to non thermal and energetic tails, energetic minor ions fluxes and composition, electric and magnetic fields, neutron and X-ray fluxes. It will register the data of measurements into the common Data Processing Unit (DPU) that will encode and transmit to the ICARUS II immediately.
In addition, EUV spectra would also yield significant details regarding solar wind structures. Spectra of the waves and turbulence in coronal structures can be identified using measurements of the velocity distributions of ions and electrons. Doppler shifts and abundances of ions can be determined in order to assess the fast and slow solar wind source regions. ICARUS II will measure also energetic particles and their composition. This will allow their transport in the inner heliosphere to be traced. The second important task consists of receiving, collecting, and storing the data that ICARUS I will transmit in the regime of direct transmission immediately after registering in situ measurements. The data transmission from the regions close to the Sun may undergo an extremely high level of scattering, thus the relay through the receiver that will allow good quality of data transmission will be quite important for the success of the mission.
These data then will be re-transmitted to the Earth. This role of relay implies that ICARUS II should be placed along the line almost perpendicular to the plane of the ICARUS I trajectory (see Fig. 5 ). It should have onboard high quality and as large as possible memory to store the data. To obtain maximum outcome from remote sensing the sampling rate of magnetograph and spectroscopic measurements should be quite high. This issue should be addressed during preliminary study of the project feasibility. It is also necessary to have an onboard high quality X-band receiver. ICARUS II can have an onboard additional optional instrument for the studies of dust in the heliosphere. A baseline scientific payload for ICARUS II is listed in Table  3. The trajectory of ICARUS II may be in the ecliptic plane and it can be determined using the studies of trajectories for the Solar Orbiter mission.
We collected a new set of velocity data in the direction of these two targets, useful for completing the existing collection of data available in the literature. In this paper, we analyze these two galaxy structures from their spectroscopic properties and we discuss the evolutionary state of the TriAus complex supercluster. In Sect. 2, we present the observations and data reduction. Section 3 contains the results as well as a dynamical analysis of the two clusters, aimed at studying the velocity dispersion in each cluster centre, as well as its variations with the radius until the measured limit of the shear up to 8 arcmin (equivalent to a radius of 0. 5 h -1 70 Mpc at the cluster redshift). In Sect. 4, we analyze the TriAus supercluster as a whole. We adopt, whenever necessary, H 0 = 70 h 70 km s -1 Mpc -1 , Ω M = 0.
X-ray data For the study of the Triangulum Australis cluster in X-rays, we used data from an observation with XMM-Newton with the A66, page 3 of 11 ter with all recession velocities available in the range of 9500 ≤ v ≤ 19 000 km s -1 , with a step size of 500 km s -1. The lines show Gaussian distributions fitted to the data including all galaxies (dashed line) and excising the substructure of 26 galaxies (solid line). observation ID 0093620101. The exposure time is 9, 9. 8, and 3. 2 ks for the MOS1, MOS2, and PN detectors respectively. The exposures have been cleaned from times affected by solar flares. For the image analysis, we focused on the 0. 5-2 keV energy band, since this provides the best signal to noise ratio (S/N) above the background. To obtain an overview on the place of the Triangulum Australis cluster in the large-scale structure environment, we use the results of the identification of galaxy clusters in the ROSAT All-Sky Survey  (Trümper 1993).
Velocities catalogue From the observing runs, we obtained a set of 131 heliocentric radial recessional velocities (some of them were observed two times) belonging to the two clusters, namely: 76 for TriAus and 55 for AS0794). Table  A. 1 in Appendix A lists the details of these new observations: (1) object number, (2) right ascension (J2000), (  3 ) declination (J2000), (  4 ) heliocentric radial reces- sional velocity in km s -1 , (5) associated error in km s -1 , (6) R value from  Tonry & Davis (1979)  and (  7 ) notes. Some galaxies have been previously observed and adding their velocities available from the NED database 3  we obtained a total of 296 velocities for TriAus and 109 for AS0794 in the range of 5000 ≤ V ≤ 30 000 km s -1. From the linear regression to compare 43 velocities in common with the literature, we obtain v obs = 0.
AS0794 cluster Figure  5  shows the combined resulting distribution of 78 galaxies (55 from the present paper and 23 from NED) in the AS0794 cluster as wedge diagrams in right ascension and declination of the whole velocity data available until 20 000 km s -1. Figure  6  shows the recession velocity histogram of these galaxies in the range of 11 000 ≤ v ≤ 17 500 km s -1 , with a step size of 500 km s -1. The histogram shows the Gaussian distribution centered at 12 669 km s -1 with a dispersion σ = 464 +72 -70 km s -1. We see on these two diagrams that there are galaxies with higher velocities than the cluster, spread towards and around the average velocity ( 15 000 km s -1 ) of the TriAus cluster. We can suggest that AS0794 is slightly in front of the main structure linked to the TriAus complex, as dicussed below.
Triangulum Australis complex as a part of a larger superstructure The TriAus cluster appears to be associated with other clusters in its vicinity. Four clusters were already identified   3. 2  and 3  are represented in blue, green, and red circles in the ranges of 8000 ≤ v < 12 000 km s -1 , 12 000 ≤ v < 18 000 km s -1 , and 18 000 ≤ v < 20 000 km s -1 , respectively. clusters confirms the extension of the network in which the SSC is embedded, as suggested by these authors. The location of this set of clusters is shown in their Fig. 9. However the string of clusters passes directly behind a region of extremely high extinction of the galactic disk. We added galaxies from the NED database within a radius of 10 • around the center of the TriAus and ARA clusters, with a total of 2328 galaxies including the above four clusters already identified by  Radburn-Smith et al.
(2006) ,  Kocevski & Ebeling (2006). The velocity histogram in Fig. 5  A66, page 7 of 11 Notes. Asterisks refer to clusters already listed in Table  3  and numbers in the last column refer to the numbers in Fig. 9. The coordinates give the X-ray maximum, which may be different from the optical center quoted in Table  3. of  Radburn-Smith et al. (2006)  shows the four rich clusters at z 0. 05, which correspond to the recessional velocity histogram shown here (Fig. 7 ) centered at V = 15 077 km s -1 , with a dispersion of σ = 3355 ± 51 km s -1. To study the interactions of the above wide TriAus region with the SSC, we extracted from the NED database all galaxies with velocities between V = 8000 and V = 20 000 km s -1 to cover a wide region ranging ranging between RA = 12h30m and 20h00m and from Dec = -30 • to Dec = -90 • (J2000).
We added the SSC velocity catalogue  (Quintana et al. 2020)  in the same velocity range and we finally obtained a set of 13 152 galaxies in this region, after eliminating duplicate objects. Figure  8  shows the wedge diagrams from RA = 12h30 to RA = 18h and from Dec = -30 • to Dec = -90 • for these 13 152 galaxies. Many clusters are clearly visible, particularly in the region of the SSC and also around the TriAus centre. Several very elongated structures are strongly affected by extinction from the galactic plane. In order to identify the already known structures in this wide area, we selected 50 identified clusters of galaxies from the NED database in the wide region ranging from RA = 13h20m to 20h00m and from Dec = -30 • to Dec = -90 • (J2000), including the SSC and TriAus, and with velocities ranging between 8000 and 20 000 km s -1 , which are listed in Table  2 : (1) cluster name, (2) alternative name, (3) right ascension (J2000), (  4 ) declination (J2000), (5) average heliocentric radial velocity in km s -1.
The size of the Hilbert space hints at the existence of two blocks of different sizes (denoted N 1 and N 2 in the following). A first simple test is to compare the expectation value r RSOS 0. 452 to the values obtained for two GOE blocks of different sizes (Fig. 3  in Sec. III D). This leads to a possible value around α = N1 N1+N2 ∈ [0. 27, 0. 3], corresponding to a size ratio N 1 /N 2 ∈ [0. 37, 0. 43], close to φ -2 = lim L→∞ F L-1 F L+1 0. 382. This strongly suggests that the spectrum of the periodic RSOS chain is composed of two independent GOE blocks of size N 1 = F L-1 and N 2 = F L+1. In the top panel of Fig. 7 , we also represent the predicted value r m=2,α=1/(1+φ 2 ) = 0. 453186, to which the numerical data indeed appear to tend. This is further confirmed by the numerical distribution of P (r) (bottom panel of Fig.
ACKNOWLEDGMENTS We thank  B. Georgeot ,  L. Herviou  for useful discussions as well as  R. Vasseur  for earlier insightful correspondence on the two-block structure of the periodic RSOS chain. This work benefited from the support of  the  project  THERMOLOC ANR-16-CE30-0023-02  and  the  project  COCOA ANR-17-CE30-0024-01  of the  French National Research Agency (ANR) , and by the  French Programme Investissements d'Avenir under the program   ANR-11-IDEX-0002-02 , reference  ANR-10-LABX-0037-NEXT. We acknowledge the use of HPC resources from CALMIP (grants  2018-P0677  and  2019-P0677 ) and  GENCI  (grant  x2019050225 ). We use the libraries PETSc 109,110 , SLEPc 111,112 and Strumpack 113,114 for the many-body computations presented in this manuscript.
Magnetic susceptibility The zero-field-cooled (ZFC) magnetic susceptibility at 500 Oe for each LnTaO 4 compound is plotted in Fig. 5(a). No sharp peaks in the susceptibility were observed for any of the eight compounds except TbTaO 4 , which had a peak at 2. 9 K. Field-cooled (FC) susceptibility at 500 Oe was also measured on TbTaO 4 and found to be identical to the ZFC data, suggesting three-dimensional antiferromagnetic ordering without glassiness. The susceptibility was fitted to the modified Curie-Weiss law: χ = χ 0 + C (T -θ CW ) , ( 1 ) where χ 0 is the temperature-independent contribution to the susceptibility. Linear fitting of (χ -χ 0 ) -1 against T [Fig. 5(b) ] was carried out in the temperature range 50-300 K. The effective magnetic moment was calculated from the experimental data using μ eff /μ B = √ 8C and compared with the theoretical paramagnetic moment g J √ J (J + 1).
C. Magnetic structure of TbTaO 4 We obtained high-resolution PND data for the magnetic phase of TbTaO 4 at 1. 5 K using the D2B beamline at the ILL  [52]. Variable-temperature PND was also carried out on the D1B beamline in order to track the evolution of the magnetic structure with temperature. On cooling below T = 2. 3 K, magnetic Bragg peaks were observed to appear and increase in intensity as the temperature was lowered. No discernible diffuse scattering was observed above this temperature. The magnetic peaks could be indexed to a commensurate magnetic cell with k = 0 in the magnetic space group 14. 77 (P2 1 /c). Refinement of the magnetic structure using TOPAS [Fig. 4(b)]  shows Tb moments parallel to the a axis in A-type antiferromagnetic order: The moments coalign within the ac plane, forming ferromagnetic slabs coupled antiferromagnetically along b [Fig.
ACKNOWLEDGMENTS N. D. K. thanks  Sundeep Vema  for carrying out the reactions at 1600 • C,  Farheen Sayed  for the SPS experiments, and  James Analytis  for technical advice on producing Fig. 10. We acknowledge funding from the  EPSRC  (Grants No. EP/T028580/1 , No. EP/R513180/1 , and No. EP/M000524/1 ). The authors gratefully acknowledge the technical and human support provided at the  Institut Laue-Langevin (ILL), Grenoble, France.
6] < 19 is 0. 15. The photometric calibration is in excellent agreement with previous WISE measurements. We extracted source number counts from the 3. 6 µm band mosaics, and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s.
Introduction The Euclid mission will survey 15 000 deg 2 of the extragalactic sky to investigate the nature of dark energy and dark matter and to study the formation and evolution of galaxies  (Laureijs et al. 2011). To this end, Euclid will obtain high resolution and high signal-to-noise imaging of a billion galaxies in a broad optical filter to measure their shapes, and in three near-infrared (NIR) filters to measure their colours. It will also obtain high signal-tonoise NIR spectroscopy of about thirty million of these galaxies to measure abundances and redshifts. Additionally, photometric redshifts will be determined by combining the Euclid data with optical photometry from external surveys. To reach the required precision on cosmological parameters and satisfy the stringent mission requirements on completeness and spectroscopic purity and to shape noise bias, Euclid must also obtain observations with a 40 times longer exposure per pixel than the main survey over regions covering at least 40 deg 2.