dataesr/scientific-paragraphs-categorization huggingface dataset:
With limited resolution and distances, the first results were obtained by  Fitzgerald (1968) ;  Neckel & Klare (1980) ;  Arenou et al. (1992) ;  Hakkila et al. (1997). Marshall et al. (2006)  compared the 2MASS photometry to the stellar population synthesis of the Besancon  Model (Robin et al. 2012 ) to obtain extinction density. This approach was also used by  Chen et al. (2013)  and  Schultheis et al. (2014)  which added Glimpse and VVV catalogue to their dataset. Sale et al. (2014)  applied a hierarchical Bayesian method to infer stellar properties and extinction profile with the IPHAS survey. Also using a Bayesian method,  Green et al. (2014)  derived an extinction map from Pan-STARRS data, later combined with  2MASS (Green et al. 2015 , 2018)  and Gaia DR2  (Green et al. 2019)   In this work we use the Field Extinction-Distance Relation Deconvolver (FEDReD) algorithm described in  Babusiaux et al.
(2020). This is a Bayesian deconvolution algorithm which uses an empirical H-R diagram to study photometry and parallax, taking into account the completeness of the field of view under study, to derive both the extinction as a function of distance and the stellar distance distribution. We apply the algorithm to data of the Two Micron All Sky Survey (2MASS,  Skrutskie et al. 2006 ) crossmatched with the second Data Release of Gaia (DR2, Gaia  Collaboration et al. 2018). This paper is organised as follows : in Section 2 we present the data and filters used to select stars. Section 3 is a quick sum up of the FEDReD method. In Section 4 we detail our method to merge every field of view results into a self-consistent map. Section 5 presents our extinction map, with the details of the different visible features and their relation with the other components of the Galactic disk.
Data This work uses photometry and astrometry based on two surveys, Gaia and 2MASS. Gaia DR2 data provides high precision parallax and photometry in G, G BP and G RP bands 2MASS provides photometry in three near -infrared bands: J, H and K s. As Gaia DR2 and 2MASS are full sky surveys, we are able to draw an extinction map of the entire Galactic disk. The 2MASS catalogue is used as a basis for our analysis, as its completeness is easier to model than the Gaia one, the latter being more dependent on the crowding as well as on the Gaia's scanning law. Every star that we study has therefore 2MASS photometry which can be completed with Gaia-DR2 parallax, photometry or both. To select stars in the 2MASS catalogue, we used the ph qual flag and kept every star with at least a ph qual=D for each photometric band.
Comparison with other work We compared our extinction map to one of the most complete available extinction map of the solar neighbourhood, by  Lallement et al. (2019). They basically use the same data as our study (2MASS and Gaia-DR2) limited to stars with a relative parallax error better than 20%. Their results are presented in the reference extinction at 550nm, as we do in this work. We present in Figure  8     The reader can notice the very good agreement between the two maps within the confidence limit of Lallement et al. (  2019 ) results. The presence of Finger-of-God on both maps is also apparent, though at different locations on the two maps, allowing us to really identify them as spurious. The foreground part of the Vela cloud is roughly identical on both works, which confirms this crescent shape.
Conclusion We have used the Gaia DR2 data and 2MASS photometry to estimate the extinction within the Galactic plane. We used data of about 5. 6 million stars to produce an extinction map, reaching about 4 kpc in the direction of the Galactic centre and more than 6 kpc in other directions. Thanks to this result we are able to confirm general structures of the solar neighbourhood, already revealed by recent previous works  (Lallement et al. 2019; Green et al. 2019; Chen et al. 2019b ). The Local arm and the Split represent two structures, close to the Sun, with a high extinction separated by a clean corridor. Nevertheless our map reveals a possible relation between the Split and the Sagittarius arm at larger distance. The Galactic centre direction is dominated by the Sagittarius -Carina complex.
Because of this high extinction, as well as crowding, we are not able to go beyond this complex. We do not distinguish the Sagittarius and the Scutum arm within this complex. The Perseus arm extinction component seems very fragmented, even if the location of masers which trace this arm are visible in the dust. The Vela and Carina complex are the two strongest extinction areas of the forth quadrant. Furthermore, FEDReD's map reveals the extinction prolongation of the Carina Complex and the bubble structure behind the Vela cloud. Finally, we also observe four empty bubbles close to the Sun, and we reveal their ends for two of them. Data corresponding to the maps presented here are available in Tables  1  and 3. We also provide the values of the cumulated extinction A 0 and corresponding asymmetric uncertainties in Tables  2, 4  and 5.
The entire version will be available as a machine-readable form at the CDS In future works, we will also explore the Galactic disk at higher and lower latitudes. This will allow a better study of some structures, for example the Outer arm which is known to be warped. To explore larger distances, and in particular the Galactic centre and the start of spiral arms, we will use deeper nearinfrared surveys, such as UKIDSS  (Lucas et al. 2008) and VISTA (Minniti et al. 2010 ). Moreover we look forward for the future third data release of Gaia mission which will provide better parallax and photometry constraints. Table  1. Some columns and rows of the a 0 extinction density (in mag/kpc) of the map presented in Figure  1. Each column corresponds to a LoS, the longitude is given in the first row (in degree).
Acknowledgements. We thank the referee for suggestions that improved the paper. This work has made use of data from the  European Space Agency (ESA) mission Gaia  (https://www. cosmos. esa. int/gaia),processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www. cosmos. esa. int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication also make use of data products from the  Two Micron All Sky Survey , which is a joint project of the  University of Massachusetts  and the  Infrared Processing and Analysis Center/California Institute of Technology , funded by the  National Aeronautics and Space Administration  and the  National Science Foundation.
In these experiments, the samples of Rb 2 UBr 6 sealed in a thin-walled quartz tube of 6-and 12-mm diameter were used, respectively, for SLAD and NPD instruments. The sample used on the NPD was a polycrystalline, whereas that on the SLAD was a powder one  [14]. For the Rietveld refi nement, the program FullProf was used  [15].
The lack of this effect on our diffraction data could be caused by the lower resolution of used diffractometers, and for determination of the structure, the measurement on the diffractometer with a much better resolution is necessary. This measurement was performed on the DN5 diffractometer in the CENG. The DN5 diffractometer was placed in the SILOE reactor. This instrument was a two-axis diffractometer with a medium resolution. The DN5 diffractometer used a BF3 position-sensitive "banana" detector of 800 cells. Diffraction data were collected in 2 steps of 0. 1° over the range of 3-80°. During the measurement, a neutron wavelength of 2. 48 Å was used for better separation of diffraction lines. The neutron diagram obtained at room temperature is shown in Fig. 2. The obtained result of the experiment shows clearly that at room temperature, the expected splitting of some diffraction lines really occurs.
The low temperature structure of Rb 2 UBr 6 In order to check the stability of this structure in a wider range of temperatures and to make the noticeable effect of lattice vibrations damped, the measurements were also carried out at 4. 2 K. Neutron powder diffraction patterns were taken using an "orange" cryostat at temperatures 300 K, during a slow cooling down in the temperature range of 300-4. 2 K, and at 4. 2 K. During the cooling down, the diffraction data were also noted. With decrease in temperature, it was noticed that the diffraction pattern at 80 K has apparently changed and the pattern was stable up to 4. 2 K. The neutron diagram observed at 4. 2 K is shown in Fig. 4. Splitting of the cubic 004 refl ection observed previously at room temperature indicates that a tetragonal deformation has vanished completely.
The high temperature structures of Rb 2 UBr 6 The dependence of electrical conductivity and the results of differential thermal analysis (DTA) as well as data envelopment analysis (DEA) measurements were shown in the works of Refs. [10, 11]. The thermal data revealed that at 843 K and 967 K, the phase transitions may occur. On the temperature dependence of conductivity, the high rising of conductivity was registered at the temperature region of 740-870 K. Above 870 K, the arising of conductivity is much smaller. The curve is smooth. There were no indicated jumps typical for phase transition of the fi rst order (Fig. 6 ). To describe the structures at elevated temperatures, a neutron diffraction experiment was performed at 300, 600, 850, 900, 940, and 980 K on the SLAD instrument. The SLAD instrument was a two-axis diffractometer with a medium resolution utilizing three banks of position-sensitive detectors that produced a diffraction spectrum in the range of 4-137° with a step of 0.
1°. A vertically focusing monochromator with an incident neutron wavelength of 1. 113(1) was used throughout the experiment. The non--linear background coming from a quartz tube was eliminated by subtracting the measured neutron diffraction profi le for an empty quartz container. In experiments performed at elevated temperatures, a furnace with a tantalum heating element with automatic temperature control was used. The data were corrected for background scattering, container scattering, absorption, and inelastic and multiple scattering and normalized to a vanadium standard using the correct program package. The neutron data at 600, 850, 900, 940, and 980 K are shown in Fig. 7. The DTA data show that up to 843 K, the crystal structure is tetragonal. At 600 K however, a difference in shape of diffraction spectra was also detected.
The fi ttings of the rest of neutron data were performed for the cubic structure. Because the values of electric conductivity at temperatures close to the temperature of melting are high, one may expect disordering of rubidium sublattice. The Rb ions should be distributed randomly over other crystallographic positions. Among them, the stable positions are dodecahedral sites at the (8c) position, whereas quasi-stable octahedral sites are at the (4b) position. We decided to reduce the redistribution of Rb ions only to these positions. The fi nal results are presented in Table  5. It seemed that at 843 K, the transition occurred from the tetragonal to the cubic structure. This however stayed open the question of what was the source of effect observed on the DTA curve at 960 K. It is also seen that the factors of agreements for measurements at 900 K and 940 K were high, suggesting that the structure of the phase at the temperature region   846-960 K may be different.
Short-term, high-cadence chromospheric observations High-cadence Ha observations are widely used in the context of solar flare/CME analyses and monitoring (e. g. ,  Deng et al. , 2002; Huang et al. , 2014). In the case of filament Topical Issue -Space Weather Instrumentation eruptions, such data allow one to follow the pre-, and early-, eruptive dynamics of the filament, which provide insights into both the CME triggering and driving mechanisms when combined with the analysis of other datasets such as photospheric magnetic field data (e. g. ,  Joshi et al. , 2014; Chen et al. , 2018). Adopting the framework of the Torus Instability (one of the main models considered for CME trigger/driver;  Kliem & Török, 2006; Démoulin & Aulanier, 2010) , then Ha imaging can further be used to monitor the slow rise of the filament and predict when it will reach the critical height for the onset of the instability (e.
The optical diameter of the three imagers is 100 mm with 985 mm equivalent focal length. The filters bandwidth, optical resolution on the Sun and observing cadence are given by Table  1. Instruments are enclosed in a temperature controlled box (active heating, passive cooling) supported by an equatorial mount. The detectors are QSI 660i and 690i air cooled cameras using shutterless interline CCD sensors from Sony (3000 dynamic range, 12 bits). MeteoSpace is the first solar automatic station in France. All operations are fully robotized: weather checking, opening and closing the dome, catching the Sun, solar tracking, data acquisition, processing and transfer to the archive, and website update. MeteoSpace is supervised by a main computer connected to several sub-systems, for environment (weather station and full-sky camera), mount steering, instrument and camera control, data archiving and webservice.
Two scintillometers (AiryLab company) provide an estimate of flux and seeing conditions (1 00 typical at Calern) for each image. The instrument J. -M. Malherbe et al. : J. Space Weather Space Clim. 2020, 10, 31  is protected by many house-keeping procedures, including weather phenomena; in case of failure, a short messaging service (SMS) generates an alert to the local staff. Quick look data (JPEG) will be available in real time, while scientific images (FITS) will be delivered a few hours later after calibration and corrections of dark current, geometric distorsion and rotation to present solar north up. Data will be processed and stored at Nice (30 Tera bytes available) but accessed through the BASS2000 national database dedicated to groundbased observations (http://bass2000. obspm. fr); a real-time channel is under development to disseminate high-cadence Ha images for space weather applications.
obspm. fr/pub/meudon/spc/tiff. Datacubes of Hb line are scheduled for 2021. In order to illustrate the Spectroheliograph capabilities, we chose datasets recorded near the last solar maximum (13 Nov 2013) with the new SCMOS detector (which was, at this moment, only available for tests). Figure  7  shows images extracted from Ha line profiles, with many sunspots, filaments and active regions. The composite image comes out from the difference between line core and the sum of the red and blue wings, after normalization by the average values computed in a quiet Sun region near disk center. This method makes all structures of the Sun appear together in a single frame (prominences, chromosphere at the limb, spots, filaments, faculae) with enhanced contrast. The Doppler velocity proxy is made of the contrast of line wings (ratio between the difference and sum of red and blue wings, after normalization by disk center values).
Low cost pre-filters could also be added to limit the contrast loss to À30%. Capabilities could be extended at the end of the space-borne SDO mission by a fourth telescope for Stokes V measurements (magnetograms) in the blue wing of NaD1 5896 Å line. The Spectroheliograph is dedicated to long-term, lowcadence observations of the chromosphere and now delivers (x, y, k) datacubes of Ha, CaII H and K spectral lines, from which classical images are derived. A precise wavelength calibration method of datacubes, using comparison with atlas spectra, is proposed. Observation of Hb line is the next extension. All data are (or will be) freely available to the scientific community through a dedicated web service (BASS2000), which will offer an additional real-time channel to disseminate high cadence MeteoSpace images for space weather applications.
Acknowledgements. We are indebted to the referees and to the editor for helpful comments and suggestions. We thank the observers operating the Spectroheliograph and the technical team of the  MeteoSpace  project. We acknowledge financial support of several institutions as  DGA ,  CNRS/INSU (PNST), Paris and Côte d'Azur observatories, Ile de France DIM/ ACAV. This work has been supported through the  UCA/JEDI  investments managed by the  National Research Agency (ANR)  with the reference number  ANR-15-IDEX-01. If you use data for publication, please insert the following sentence: " Spectroheliograph and MeteoSpace data are courtesy of Paris and Côte d'Azur observatories ". The editor thanks two anonymous reviewers for their assistance in evaluating this paper.
Then, the HSQ film was developed in tetramethylammonium hydroxide (Sigma-Aldrich, 25 wt. % solution in water), a standard aqueous base developer (see further details in Figure  5S  in Supplementary). Cryogenic measurements. The sample was mounted on the cold-finger of a continuous flow helium cryostat, which was cooled to 4. 7 K for imaging with a home-built confocal microscope (see details in Supplementary, Figure  3S ). Experimental control was provided by the Qudi software suite  45. The GeV centers were off resonantly excited by linearly polarized 532 nm green laser to map the fluorescence of GeV ZPL. Band pass filter (599/13 nm) was placed in front of the avalanche photodiode (APD). Spectra were measured after a 560 nm long pass filter (Supplementary, Figure  3S ).
In order to resolve both amplitude and phase, a Mach-Zehnder interferometer was integrated in our setup, in which the optical path difference was modulated by an oscillating mirror in the reference arm (frequency f ~ 300 Hz). The detected signal was then demodulated using pseudo-heterodyne detection method  46  (see further details in Supplementary, Figure  12S-14S ). Numerical simulations. Finite-difference time-domain (FDTD) simulations were performed using a commercial software (FDTD Solutions v8. 11. 318, Lumerical). Perfectly matched layers (PMLs) were applied to enclose the computational domain of 8. 5 µm × 3 µm × 2 µm in all calculations. The finest mesh grid size of 5 nm is used in the simulations. The optical constants of the gold were taken from the experimental data reported by Johnson and Christy 47.
ACKNOWLEDGMENTS This work was supported by the  European Research Council (ERC) , Advanced Grant  341054  (PLAQNAP). FJ acknowledges support of the  DFG, BMBF ,  VW Stiftung  and  EU (ERC, DIADEMS ). VAZ, SB, and  NAM acknowledges support of VILLUM FONDEN  (Grant  16498 ). VAD and LFK thank the  Russian Foundation for Basic Research  (Grant No. 18-03-00936 ) for financial support. AK acknowledges support of the  DFG , the  Carl-Zeiss Foundation ,  IQST , the  Wissenschater-Ruckkehrprogramm GSO/GZS.
2018). No radio bursts were detected during the simultaneous optical observations, and the results from the analysis of the optical data alone are outside the scope of this paper. FRB 121102 had an exposure time of 128 hours with Effelsberg, 26. 25 hours with GBT, 3. 7 hours with AO, 25. 2 hours with NuS-TAR and 240 hours with INTEGRAL. The only session with radio detections at the time of a simultaneous X-ray observation was on September 06, 2017, during a NuSTAR session (see section 3. 2). For some radio observations extended time coverage was performed. That is the case from the 24 to the 28 of September 2017 where EFF and GBT had almost full coverage, in some cases with simultaneous observing as well as one radio telescope taking over from the other. However, as seen in Figure  1  no radio burst was detected in those observations.
Effelsberg telescope We took data using the 7-beam feed array receiver with the Pulsar Fast Fourier Transform Spectrometer (PFFTS,  Barr et al. 2013) , and the high precision pulsar timing backend PSRIX  (Lazarus et al. 2016 ). The PFFTS records data at a central frequency of 1. 36 GHz with 300-MHz of bandwidth divided into 512 frequency channels and a time resolution of 54. 613. However, these data are not synchronized with a maser clock. To compensate, we recorded simultaneously the incoming data of the central beam with the backend used for pulsar timing, PSRIX, as it provides high precision time stamps. This backend's band is centered at 1. 3589 GHz, with a bandwidth of 250 MHz divided into 256 channels and a time resolution of 51. 2. This allows us to obtain the precise time of arrivals (TOAs) of the detected bursts displayed in Table  4.
Green Bank Telescope We observed FRB 121102 with the GBT's S-Band receiver at a center frequency of 2 GHz and a total bandwidth of 800 MHz, though a notch filter between 2. 3 and 2. 36 GHz removes interference from satellite radio, slightly reducing the effective bandwidth. We used the Green Bank Ultimate Pulsar Processing Instrument (GUPPI,  Ransom et al. 2009 ) to coherently dedisperse incoming data at a DM of 560 pc/cm -3 , recording self and cross-polarization products with 512 frequency channels and a sampling time of 10. 24 s. We used the PRESTO routine rfifind to flag samples contaminated by interference and applied this mask in subsequent processing  (Ransom 2011). We searched for bursts using the PRESTO routine single_pulse_search. py, similar to data from Effelsberg, but with slightly different parameters.
Arecibo Observatory The simultaneous observations with NuSTAR were obtained through a DDT to the Arecibo Observatory (project code P3219). Note, only half of the scheduled observations were possible due to the telescope shutdown for hurricane Irma. Similarly, simultaneous observations planned along with INTEGRAL were not possible due to the observatory shutdown after hurricane Maria. Data were recorded with the C-lo receiver and PUPPI pulsar backend. PUPPI recorded filterbank files coherently dedispersed to DM=557 pc cm -3. The recorded bandwidth at 4. 1-4. 9 GHz was divided into 512 channels yielding a frequency resolution of 1. 56 MHz. The time resolution of the data was 10. 24 s. The raw data contain full polarization information, which can be used to obtain the rotation measure and polarization profiles in the event of a detection.
NuSTAR FRB 121102 was observed by NuSTAR  (Harrison et al. 2013 ) between 2017 September 5 and 11 in five separate observations with their start times and durations shown in Table  2. The data were processed using HEASOFT 3 and the standard tools nupipeline and nuproducts. We extracted source photons from a 2 -radius circular region centered on the source position. We used a background region of identical size positioned away from the source. Photon arrival times were corrected to the Solar-System Barycenter using the source position from  Chatterjee et al. (2017).
INTEGRAL FRB 121102 was observed by the INTEGRAL satellite in late September 2017 in pointing mode and then in 2019 in a Target of Opportunity mode. In both cases, the goal was to search for a possible Hard X-Ray/soft gamma-ray counterpart to the radio emission. The log of the observations with start time and duration is shown in Table  2. The INTEGRAL data were processed using the standard INTEGRAL Offline Scientific Analysis (OSA) software 4. No radio burst was triggered by the Effelsberg telescope during the INTEGRAL exposures, preventing a search for a coincident impulsive event. Searches for correlations before or after the radio burst and with signals from other radio facilities are currently underway  (Gouiffes et al, in preparation).