dataesr/scientific-paragraphs-categorization huggingface dataset:
(2011) , as well as 163 stars observed by  Fulbright et al. (in prep. ). The targets of both of these data sets are drawn from RAVE, while the stellar parameters have been obtained from an equivalent-width analysis of high resolution spectra. In addition, the very metal-poor giant star CD-38245 ([M/H]= -4. 2 dex,  Cayrel et al. 2004 ), which has been observed twice by RAVE, has been included in the list, in order to calibrate the results at the very metal-poor regime. Metal-rich giant stars have been explored thanks to the CFLIB library  (Valdes et al. 2004 ). The entire spectral library was downloaded from the webpage 8  of that project, excluding only spectra which did not include the wavelength range around the IR Ca II triplet. The final comparison catalogue is the same as in K11, where once again, we used the updated values that can be found in the PASTEL database, and discarded the stars for which the dispersion in the literature values were greater than 100 K, 0.
Equivalent-width corrections for the opacity of the neighbouring lines The EW library is built using the driver ewfind of the spectrum synthesis code MOOG  (Sneden 1973 ) which computes the EW of every line as if they were isolated. Nevertheless, line blends when not carefully taken into account can lead to abundance over-estimations. In the case of lines instrumentally (but not physically) blended, the observed blend has a total EW that is the sum of the EWs of the two isolated lines, and thus no problem arises. However, when two lines are physically blended (i. e. not instrumentally), the quantity of radiation absorbed by one line is affected by the opacity of the neighbouring line, and the total EW of the blend is smaller than the sum of the two isolated EWs. In this case the blend in the constructed model is too strong, leading to abundance overestimations.
Such criteria leave 313,874 spectra selected from the RAVE database. Besides the chemical abundances of this selected sample, we provide some extra statistical quantities and flags to be employed for further quality selection: 1. χ 2 between best matching model and observed spectrum: the lower the values the better the expected abundance precision. We suggest a user reject spectra with χ 2 > 2000. 2. the value f rac which represents the fraction of the observed spectrum which satisfactorily matches the model. We suggest a user reject spectra with f rac < 0. 7 (see B11 for further details). The application of these quality flags is left to the user. The number of spectra which meet all such quality flags is 187,305. In Fig. 19  we show the distribution of the chemical abundances, given the above mentioned criteria, for SNR>20 pixel -1 and SNR>40 pixel -1.
RADIAL VELOCITIES The radial velocities for this fourth data release are based on the RAVE pipeline described in  Siebert et al. (2011b) , therefore only a brief reminder of the general features is given here. The radial velocities are obtained using a standard cross-correlation algorithm in Fourier space on the continuum subtracted spectra. First, an estimate of the radial velocity is obtained using a subset of 10 template spectra. This first estimate, with an accuracy better than 5 km s -1 is used to put the spectrum in the zero velocity frame. A new template is constructed using the full template database using a penalised chi-square technique described in  Zwitter et al. (2008). The new template is   then used to derive the final, more precise, radial velocity. The internal error is obtained as the error on the determination of the maximum of the correlation function.
CONCLUSIONS The fourth public data release of the RAVE survey includes the stellar atmospheric parameters of 482 430 spectra obtained from April 2004 to December 2012. Compared to the previous catalogue of DR3, a new input catalogue, based on DENIS DR3 and 2MASS, is used to select the observed targets. The new input catalogue has the major new feature of extending to lower Galactic latitudes and providing more accurate astrometry, leading to fibre placement better matching stellar positions on the sky, which results in higher signal-to-noise spectra. In addition, the parameters have been revisited, thanks to a new pipeline, presented in  Kordopatis et al. (2011a) , and 809 reference spectra that allowed us to validate the effective temperatures and surface gravities, and calibrate the metallicities.
That is, at face value the distribution functions for derived stellar parameters are consistent with plausible astrophysical expectations. In addition to the atmospheric parameters obtained with the new pipeline, those obtained with the DR3 pipeline are also published since they have been used in published analyses. However, they are of lower reliability than our DR4 dataset, so situations demanding their re-analysis should be rather rare. The abundances of six individual elements, namely aluminium, silicon, titanium, iron, magnesium and nickel are published, using an improved version of the  Boeche et al. (2011)  chemical pipeline. The reliability of these elemental abundances varies according to the effective temperature, surface gravity and metallicity of the star, the signal-to-noise ratio of the spectrum, and of course the element itself.
Our design strategy started with an ESA radius of curvature of ∼50 mm and a gap of 2. 5 mm. Then we used an automated computer optimization system (optimizer) to refine the design for maximum performance within the constraints listed above. The optimizer created and evaluated different geometries using the electro-optics simulation software SIMION ®  (Dahl 2000). SIMION simulates a design then returns a certain value (determined by a function that can be the throughput, for example) to the optimizer that compares the performance with previous designs. For JADE-E, the optimizer worked within a parameter space defined by the user and explored the effects of varying the parameters. Using a simplex algorithm, the optimizer adjusted the parameters until it found a local minimum. We changed the initial conditions and modified the parameter space and repeated many optimizations until we found a design that gave excellent results.
The magnetic field vector components are measured and broadcast to JADE (and other instruments onboard) nominally once per second, with a resolution of 1 nT. The vector orientation is calculated and a table of deflection voltages is created for the next energy sweep. If the deflection angle falls outside the ±35 • JADE-E FOV, a limit is set to 35 • and the voltages are calculated accordingly. Note that over the Juno mission the spacecraft spin axis orientation and orbit does not require JADE-E to deflect more than ±30 • to track the magnetic field direction. If the voltage required to track the field direction exceeds 10 kV, e. g. at the upper end of the energy range and for large deflections, then the voltage is set at 10 kV. If the magnetic field vector information is missing or comes late for the next DFL angle calculation, then JADE software extrapolates (propagates) the next orientation using the latest value received.
Instrument Processor Board The Instrument Processor Board (IPB, Fig. 30 ) is the computing platform on which the JADE Flight Software runs. Figure  31    The IPB responds to spacecraft commands, transmits low-rate Science and Housekeeping telemetry, and transmits high-rate, synchronous Burst Mode Science data. Through the JSIB, the IPB controls the sensors and reads back telemetry data collected. The data is then formatted into packets and transmitted to the spacecraft. The spacecraft synchronizes communication using the one half pulse-per-second (1/2PPS) signal. Every two seconds the spacecraft asserts a 1/2PPS signal, which is used in concert with a spacecraft command to precisely update JADE's 1 µs resolution system timer. Spacecraft commands are received and buffered on the IPB over a Universal Asynchronous Receive and Transmit (UART) interface.
Low Speed Telemetry is written by the software into a buffer and transmitted to the Spacecraft over the UART interface. During Burst Mode, JADE transmits high speed burst data, which is written into a buffer and transmitted at a higher rate across a dedicated high-speed synchronous serial interface. The IPB is responsible for system resets of JADE for operational and fault tolerant purposes. The JADE instrument can be reset by power cycling, spacecraft command, or JADE software reset. Watchdog resets for both the processor and the FPGA ensure a software fault does not cause an instrument failure. The IPB has the following memory: 128 KB PROM for the boot code; 512 KB EEPROM to hold copies of the Flight Software and Flight Look-Up Tables  ;  and 4  MB SRAM used for Code and Data when the software is executing.
Radiation Shielding The shielding thickness can be calculated to stop electrons above a given threshold. However, in the process of stopping or slowing down these electrons, secondary radiation (e. g. , electrons, Bremstrahlung radiation in the form of X-rays, and γ -rays) is generated that may provide an additional source of background in the detectors. Using the Geant 4 software (open source software downloadable from http://geant4. web. cern. ch/geant4/), we simulated the transmission of primary and generation of secondary particles resulting from interactions between a tantalum shield and >1 MeV electrons as they either penetrate or get stopped. The results were (1) that the background due to primary electrons was greatly attenuated by the Ta shield-the thicker the shield, the greater the attenuation, and (2) that the background count rates from secondary γ -rays are more than 10 times the rates from primary and secondary electrons.
Shielding Modeling and Optimization Given the shielding numbers from Sect. 2. 5. 2 (5 and 8. 5 g/cm 2 for JADE-I and JADE-E, respectively), we optimized the geometry of the shielding by examining all possible ray paths that intersect anywhere on the anode from any direction in space. To evaluate the shielding thickness we imported the mechanical design with our first estimate of the shielding into the NOVICE software to conduct the ray tracing. Then, we evaluated the amount of shielding in all directions and scaled up or down the thicknesses of the different shielding parts. We iterated between design modifications and ray tracing results until the shielding was reasonably optimized while maintaining a feasible mechanical design. In addition to minimizing background counting on the anodes, we also estimated the shielding thickness around the JADE pre-amplifiers, as these include parts, cannot exceed 50 kRad TID (100 kRad with a Radiation Dose Margin (RDM) of 2) at the end of mission; this requirement translates to be 3.
6 × 10 6 ions were launched into the JADE-I electro-optics for each of the 32 nominal ESA voltages settings; it was also measured directly in calibration using 10 and 40 keV ions of 3 different species. Figure  64  shows geometric factor assuming 100 % foil and grid transmission and detection efficiency. During flight calibration, we measured the total effective geometric factor, including actual transmission through all grids and structures, and the measurement efficiency of the MCPs. The incident flux of particles was measured using the ABM. Figure  65  shows the The inner = 0 data is taken when the beam is incident between two anodes and partially obstructed by these mechanical structures. The geometric factor for events with valid TOF is ∼4 × 10 -4 cm 2 sr eV/eV for the full FOV and ∼4 × 10 -5 cm 2 sr eV/eV per pixel.
07 cm 2 for the start anode vs 2. 79 cm 2 for each stop anode), the larger number of starts from UV is probably due to photo-electrons being created inside the sensor. Since the JADE-I sensor primarily operates at the distance of Jupiter's orbit, the sensitivity to stray light in the sensor is not significant, and we estimate a background rate at Jupiter (5 AU) of ∼0. 2 Hz. 69 ). The majority of the orbit is spent in LRS mode with typical accumulation times of 5 or 10 minutes, depending on available telemetry. In the transition region approaching and leaving perijove, but before HRS, we collect LRS data with an intermediate rate of 30 or 60 s, again depending on available telemetry. This intermediate rate LRS will also be used near the equatorial current sheet around apojove. The Juno attitude difference during MWR and GRAV orbits (see Fig.
Burst During Auroral Field Line Crossings The most critical JADE measurements occur on the auroral field-line crossings. Active field lines are small-less than 1,000 km wide according to HST observations. Juno crosses these field lines at ∼50 km/s, and the critical data occur in ∼20 s intervals, with the exact timing of the crossings unknown. Burst mode is designed to capture these auroral crossings. The highest possible resolution data is captured and prioritized by how 'interesting' the data is, as defined by the Waves quality factor (see Sect. 4. 4. 2. 6 for Burst details). Waves flight software sets the quality flag based on (1) the number of solitary structures in the Waves wideband data, (2) the amplitude of waves near the electron cyclotron frequency, and (3) sudden changes in broadcast magnetic field direction or magnitude  (Kurth et al.
2013, this issue). Waves broadcasts a Burst trigger when the quality flag rating is above a threshold. When a Waves trigger is broadcast, the spacecraft continues collecting data for 30 s; data ±30 s from the trigger are stored with the associated quality flag. There is telemetry to transmit ∼7 60-s bursts during each perijove, and more are added to the plan as bandwidth allows. JADE can only store burst data if it is in Burst mode when the Waves trigger is sent. Burst mode recording sessions are defined by time-tagged command loads uploaded 2 orbits in advance of execution. These recording sessions are planned during the auroral crossings using trajectory and field-line model predictions.
Orbital Trim Maneuver (OTM) Each orbit an OTM is needed to precisely time the orbits with respect to Jupiter's rotation rate so that evenly spaced global maps of Jupiter can be gathered. These OTMs are scheduled for 4 hours after each perijove, although the precise timing may evolve. Because of the use of the Juno thrusters for the OTM, JADE pauses data collection and JADE-I MCP and TOF are set to 0 V. The spacecraft mini-sequence that commands OTMs also contains commands to ramp the noted JADE voltages down prior to the maneuver, and then ramp them back up after the maneuver. Once the voltages are restored to nominal operating voltage, data collection resumes in LRS.
JADE-E Sweeping by Mode JADE-E sweeps through its 64 ESA steps in 1 s, regardless of mode. A low-resolution, 32-step sweep is taken every 0. 5 s, hitting every other energy step in the first half second where voltage is increasing, then filling in the skipped voltages during the second half of the second where the voltages are decreasing. ESA steps are 0, 2, 4,. , 30, 31, 29,. , 1 (Fig. 73 ). The reason for sweeping up then down is to minimize the largest single step taken and therefore minimizing the HVPS settling time. Because the intrinsic resolution of JADE data is 1 s, no additional temporal resolution is required. There are 3 JADE-E sweep tables that can be updated; at launch, table 1 covered the full energy range from 0. 1 to ∼100 keV, table 2 is a limited range solar wind sweep from 0.
1-5 keV, and table 3 is a calibration table with 4 energies. In HRS and Burst all 3 JADE-E sensors collect data, and deflectors are set to remain field-aligned according to the real-time magnetic field. The JADE software compensates for an ∼1 s latency in this vector by propagating from its last position to the time at the next sweep start, using the updated spin rate. In LRS only one sensor is operational. In Cal, all three sensors are active. Deflection is based on sweep tables, not magnetic field alignment.
High Voltage Control Each high voltage power supply can also be individually switched on/off by the JSIB. FSW controls which supplies are enabled for each mode by setting power control bits in JSIB FPGA registers. FSW is commanded to enable/disable high voltage sources based on the mode to conserve power. Commands nominally come from onboard via stored sequences or macros. The ion sensor and electron sensors each have an MCP, an ESA, and two DFL voltages. Additionally, the ion sensor has a TOF voltage. Since JADE-E's ESAs and deflectors both have positive polarity they use a single bulk power supply. However, because JADE-I's ESA uses a negative voltage and the deflectors have a positive voltage, JADE requires separate bulk power supplies for the positive and negative voltages. The JADE-I MCP and TOF are static supplies, staying at a fixed voltage during science data collection after being commanded to the appropriate voltage.
The FSW reads the direct events from the JSIB as an array mapped into JSIB FPGA memory and transmits them over a selectable interval (nominally 10 minutes in HRS and Burst, and 10 hours in LRS). The JSIB histograms the TOF measurements into a data product with 32 ESA steps (all 8 DFL summed together in HRS and Burst) and 128 TOF bins (256 for Direct Event data only). The TOF information is represented in digital values corresponding to asserted delay line taps and coarse ticks, which the ground processing converts into nanoseconds. The FSW transmits this data product in Burst mode, and reduces resolution in HRS mode by summing adjacent energy rows into 16 ESA steps, preserving the 128-bin TOF resolution. In LRS and Cal modes, the FSW accumulates this product over a selectable number of seconds (nominally 5 or 10 minutes for LRS, and 30 s for Cal), and reduces row and column resolution by summing adjacent rows and columns to form a 16 ESA by 64 TOF histogram.
The JSIB classifies each particle with a valid TOF as a specific ion species via a lookup table provided by FSW. The FSW generates this table on-the-fly by retrieving the ESA voltage and comparing it against a stored table in non-volatile memory (EEPROM) to determine which TOF ranges map to which species for each ESA step. The FSW writes this table to the JSIB as an array in the JSIB FPGA memory space, so the JSIB can use the energy step and TOF as a lookup table to determine the correct species. The JSIB produces a data product with 32 ESA steps by 8 DFL steps by 12 positional anodes. The FSW produces this data product in Burst mode. In HRS mode, the FSW reduces DFL resolution by summing adjacent DFL steps to create a data product of 32 ESA steps by 4 DFL steps by 12 positional anodes. During LRS and Cal modes, away from the polar regions and away from the prime science, the FSW reads the histograms from the JSIB and further accumulates them over a commendable number of seconds, nominally 10 minutes in LRS and 30 s during Cal.
Low Voltage Engineering (LVENG) LVENG is entered immediately following successful Bootup and in this mode, the FSW first validates the Science Program Lookup Tables and then checks for the presence of the JSIB. If the JSIB is not present, or the Lookup Tables are corrupted, the Science Program stays in this mode and refuses to enter any other Science modes. In LVENG, all power supply voltages are set to 0, all JADE-E sensors are powered off (JADE-I low voltage remains powered), stims are disabled, and data buffers are cleared. Once in LVENG, the FSW produces housekeeping data and waits for commanding to one of the other modes.
High Rate Science (HRS) High rate science is the primary science mode for JADE, and is the mode that JADE is in for each of the critical perijove intervals, which includes the critical auroral crossings. In HRS, JADE-I and all three JADE-E sensors are nominally on with the DFL and ESA voltages sweeping at high rate to attain high temporal resolution observations. The broadcast magnetic field vector onboard Juno is received by JADE and used to determine which of the three JADE-E sensors has positive deflection, which has negative deflection, and which remains undeflected. Deflector voltages are swept via table. 4. 4. 2. 6 Burst Science (Burst) Burst science mode is simply an extension of HRS, but at higher resolution (no collapsing of dimensions and no accumulation of multiple samples). Data products are sent directly to the spacecraft over dedicated serial lines and include all ion species.
Large tables like the ESA and DFL sweep tables are updated by either overwriting the whole sweep table or the entire LUT. Updates can be either temporary or permanent. Ion TOF Tables The TOF of an ion is measured between the START and STOP signals generated by JADE-I electronics. For each of the 32 JADE-I energy steps, the JSIB converts the time between the START and STOP into digital numbers, and uses it for the subsequent ion data processing. The delta time between the START and STOP signals is proportional to the M/q of the ion and is used to distinguish ion species. See Sect. 3. 3. 2 for more detail. Large tables like the Ion TOF table can be updated by either replacing the whole sweep table or the entire LUT. Updates can be either temporary or permanent. 4. 4. 3. 2 JADE Macros JADE macros are a series of relative-timed commands stored in the LUT.
Lossy Compression Most JADE products are lossy compressed by JADE except for Ion Direct Events, HVENG products, and housekeeping telemetry. Burst products transmitted over the high speed interface are also not compressed by JADE although they are subsequently compressed by the spacecraft. Two 32-8 bit compression tables are provided for LRS and Cal Science products. This compression is implemented as a binary search through a step table of 256 values, where at most 8 comparisons are made before determining the compressed value. In contrast, HRS utilizes two 16-8 bit LUT compression tables where the value to be compressed is treated as an index into the table. Before each data product gets lossy compressed to 8 bits, the Science Program subtracts the minimum data value from each product element and reports the subtracted value in telemetry.
Burst Data Flow There are two ways to record JADE Burst data: bin recording and continuous recording. JADE must be commanded into and out of these Burst modes. The time spent in Burst mode is called a record session. 4. 4. 5. 1 Bin Recording Burst JADE records data as a series of bins, which are regions of memory designed to hold N words of recorded burst data. The number of bins, size of bins, and amount of data recorded in the bin leading up to the quality factor data is configurable by command. During any one record session, all bins are the same size, with the number and size configurable via command, subject to a minimum of 10 s of data. Once the bin is no longer being written to, it is a "saved bin" and is typically associated with a Waves quality factor. If no Waves quality factors are received with empty bins remaining, JADE data fills them with high-rate data, and those bins are saved without an associated quality factor.
When there are no remaining empty bins the spacecraft first records over any bins without an associated Waves quality factor in a circular manner. If there are no empty bins and no bins without an associated Waves quality factor, data with an associated higher Waves quality factor overwrites the lowest quality factor data. Another key aspect of Burst is the "quality point," which is where the recorded data associated with the quality factor resides. As part of the configuration of bins (number of bins, size of bins, etc. ), the number of 32-bit words desired before the quality point is specified. If, at the time the quality factor is received from Waves, the scratch bin contains the specified number of words or more, the recording is allowed to continue until exactly the number of specified words precedes the quality point.