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3,139 results for “fitting”
THEMIS-C: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data
THEMIS-C: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.
VOYAGER 2 SATURN PLASMA DERIVED ION FITS 96 SEC
THIS DATA SET CONTAINS THE ION PARAMETERS IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) WITH FORMAL 1 SIGMA ERRORS OBTAINED FROM VOYAGER 2 DATA AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS TO OBTAIN PLASMA DENSITIES, TEMPERATURES, AND VELOCITY. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE NITROGEN OUTSIDE OF 14 RS AND OXYGEN ELSEWHERE. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. THE VALUES FOR POSITION AND MAGNETIC FIELD GIVEN IN THE DATA SET ARE ONLY APPROXIMATE AND SHOULD NOT BE USED FOR PUBLICATION. PARAMETERS WHICH ARE IDENTICALLY 0 AND HAVE UNCERTAINTIES OF 0 WERE NOT FIT DUE TO INSUFFICIENT DATA THESE NUMBERS ARE THUS NOT REAL VALUES. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: EACH DATA RECORD CONSISTS OF 5+2N LINES, WHERE N IS THE NUMBER OF IONS FIT. LINE 1: S (A1, INDICATES THE START OF A NEW FIT) TIME OF SPECTRUM SPACECRAFT LOCATION BRHO,BPHI,BZ(3F7.3) MONTHDAYYEAR(I7) ROUTINE USED INCORPORATING THE FULL RESPONSE FUNCTION OF THE INSTRUMENT FOR L MODES DATA): CHI-SQUARE FROM FIT (E7.3) (I2): LINES 2-5 TELL WHICH CHANNELS WERE FIT: CUP IDENTIFIER (A,B,C,D) (A1) AND ENDING CHANNEL OF EACH SET (2-20I3): LINE 6 FOR IONS: F (LINE IDENTIFIER) (A1) (I1)ION MASS, CHARGE (I3,I2) (6E10.3), WHERE THE X* VARIABLES ARE FORMAL 1 SIGMA UNCERTAINTIES: LINE 7 IDENTIFIER), ION SPECIES NUMBER (A1, I1) VZ,XVZ,WPAR,XWPAR,WPER, XWPER (6E10.3). LINES 6 AND 7 REPEAT ONCE FOR EACH ION SPECIES. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. V'S ARE VELOCITIES IN KM/S, W'S THERMAL SPEEDS IN KM/S, AND DEN'S DENSITIESIN CM-3. VALUES OF B AND POSITION INFORMATION MAY BE UNRELIABLE AND SHOULD BE VERIFIED BEFORE USE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).
STEREO-B/SECCHI/HI-1 FITS data
The Heliospheric Imager-1 (HI-1) telescope is part of the Sun Earth Connection Coronal and Heliospheric Investigations (SECCHI) instrument suite on the NASA STEREO mission. The SECCHI on the two STEREO spacecraft are identical suites of remote sensing instruments designed to observe coronal mass ejections (CMEs) at the Sun and in transit outwards to 1 AU. The HI-1 telescope observes the inner heliosphere from 12 to 84 solar radii with the band-pass wavelength of 450-750 nm.
THEMIS-E: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data
THEMIS-E: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.
VG2 URA PLS DERIVED RDR ION FIT 48SEC V1.0
This data set contains the ion densities and temperatures along with formal 1 Sigma errors obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. The plasma was assumed to be rigidly corotating. Uncertainties in plasma parameters are a factor of 2 in the charging region from 1939-2158 on day 24, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987).
THEMIS-D: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data
THEMIS-D: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.
VOYAGER 1 SATURN PLASMA DERIVED ION FITS 96 SEC
THIS DATA SET CONTAINS THE ION PARAMETERS IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) WITH FORMAL 1 SIGMA ERRORS OBTAINED FROM VOYAGER 1 DATA AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS TO OBTAIN PLASMA DENSITIES, TEMPERATURES, AND VELOCITY. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L~10 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. THE VALUES FOR POSITION AND MAGNETIC FIELD GIVEN IN THE DATA SET ARE ONLY APPROXIMATE AND SHOULD NOT BE USED FOR PUBLICATION. PARAMETERS WHICH ARE IDENTICALLY 0 AND HAVE UNCERTAINTIES OF 0 WERE NOT FIT DUE TO INSUFFICIENT DATA DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: EACH DATA RECORD CONSISTS OF 5+2N LINES, WHERE N IS THE NUMBER OF IONS FIT. LINE 1: S (A1, INDICATES THE START OF A NEW FIT) HRMIN(I5),SEC.MSEC(F7.3) RADIUS(F7.3),RHO(F7.3) MODE OF FITTER(I4) THIS DATA SET, INDICATING PROGRAMS INCORPORATING THE FULL RESPONSE FUNCTION OF THE INSTRUMENT FOR L MODES DATA): CHI-SQUARE FROM FIT (E7.3) TELL WHICH CHANNELS WERE FIT: CUP IDENTIFIER (A,B,C,D) (A1) NUMBER OF SETS OF CHANNELS FIT (I3) CHANNEL OF EACH SET (2-20I3): LINE 6 F (LINE IDENTIFIER) (A1) MASS, CHARGE (I3,I2) WHERE THE X* VARIABLES ARE FORMAL 1 SIGMA UNCERTAINTIES: LINE 7 NUMBER (A1, I1) 6 AND 7 REPEAT ONCE FOR EACH ION SPECIES. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. V'S ARE VELOCITIES IN KM/S, W'S THERMAL SPEEDS IN KM/S, AND DENSITIES IN CM-3. VALUES OF B AND POSITION INFORMATION MAY BE UNRELIABLE AND SHOULD BE VERIFIED BEFORE USE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).
STEREO-B/SECCHI/Cor1 FITS data
The COR1 telescope is the inner coronagraph of the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite aboard the twin Solar Terrestrial Relations Observatory (STEREO) spacecraft. Like all coronagraphs, COR1 is designed to measure the weak light from the solar corona in the presence of scattered light from the much brighter solar photosphere. It designed to observe the white light corona from 1.4 to 4 solar radii.
STEREO-B/SECCHI/HI-2 FITS data
The Heliospheric Imager-2 (HI-2) telescope is part of the Sun Earth Connection Coronal and Heliospheric Investigations (SECCHI) instrument suite on the NASA STEREO mission. The SECCHI on the two STEREO spacecraft are identical suites of remote sensing instruments designed to observe coronal mass ejections (CMEs) at the Sun and in transit outwards to 1 AU. The HI-2 telescope observes the inner heliosphere from 66 to 318 solar radii with the band-pass wavelength of 450-750 nm.
STEREO-B/SECCHI/Cor2 FITS data
Cor2 is one of the coronagraphs aboard the STEREO-B spacecraft. It is part of the SECCHI instrument suite. It observes the off-limb corona between 2.5-15 solar radii in visible light. It acquires both total and polarized brightness images.
Acute Effects of Whole-Body Vibration Alone or in Combination With Maximal Voluntary Contractions on Cardiorespiratory, Musculoskeletal, and Neuromotor Fitness in Obese Male Adolescents
<p>Musculoskeletal and neuromotor fitness (MSMF) is reduced in obesity. Physical exercise (including whole-body vibration exercise [WBVE]) is reported to improve components related to MSMF. The aim of the study is to evaluate the acute effects of WBVE and maximal voluntary contraction (MVC), alone and in combination, on the cardiorespiratory and MSMF in obese adolescents. Eight obese adolescents performed 3 tests (WBVE, MVC, and MVC + WBVE) in different days and randomly. The outcome measures were diastolic blood pressure (DBP), systolic blood pressure (SBP), mean arterial pressure (MAP), heart rate (HR), peripheral oxygen saturation (SpO<sub>2</sub>), handgrip strength (HS), one-leg standing balance (OLSB) test, sit-and-reach (SR) test, stair climbing test (time: <em>T</em> <sub>SCT</sub> and power: <em>P</em> <sub>SCT</sub>), and sit-to-stand test (time: <em>T</em> <sub>STS</sub>and power: <em>P</em> <sub>STS</sub>). No significant changes were observed in SBP, DBP, MAP, and SpO<sub>2</sub> after the 3 tests, only an HR increase being observed after MVC + WBVE (<em>P</em> < .01) and MVC alone (<em>P</em> < .05). No significant differences were found in HS, OLSB, <em>T</em> <sub>STS</sub>, and <em>P</em> <sub>STS</sub> after the 3 different sessions. An increase in SR was found after MVC + WBVE, MVC, and WBVE (<em>P</em> < .01, <em>P</em> < .05, and <em>P</em> < .01, respectively), while a decrease in <em>T</em> <sub>SCT</sub> (<em>P</em> < .01) and an increase in <em>P</em> <sub>SCT</sub> were observed only after WBVE (<em>P</em> < .01). Taking into account the positive WBVE effects on cardiorespiratory and MSMF, WBVE might represent a nonimpact, viable, and safe exercise suitable for obese patients, which need MSMF improvement without overloading joints.</p>
FIT Method
<p>This is the data generated from the publication: "Fluorescence-Aided Identification Technique (FIT) Improves Tooth Surface Clean-Up after Debonding of Buccal and Lingual Orthodontic Appliances". </p>
Bazin fitting routine applied to PLAsTiCC transients
<p>Bazin fitting routine applied to PLAsTiCC transients.</p>
VOYAGER 2 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC
not applicable
VOYAGER 1 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC
not applicable
VOYAGER 2 SATURN PLASMA DERIVED ION FITS 96 SEC V1.0
not applicable
VOYAGER 1 SATURN PLASMA DERIVED ION FITS 96 SEC V1.0
not applicable
maXs fit-files complete - Heidelberg
<p>fit-files of maXs30 Thorium measurements</p>
The impact of breeding experience and social status on group interactions and fitness in a communally breeding species
<p>In group breeding species, not only prior breeding experiences, but also an individual's social status and that of the group members it interacts with, may influence an individual's future behaviour and fitness. Here, we report an experimental study on the facultatively communal breeding burying beetles, <em>Nicrophorus vespilloides</em>, in which we tested the combined effects of prior breeding experience and dominance status (dominant vs. subordinate) of focal individuals and those of other group members on aggressive interactions, parental investment and fitness during a future breeding event. In the presence of inexperienced subordinates, there was less aggressiveness towards experienced dominants than to inexperienced dominants, which resulted in a lower injury degree of dominants. Compared to inexperienced dominant or subordinate individuals, experienced dominants with prior breeding experience increased their parental investment, whereas experienced subordinates reduced their parental investment and by doing so avoid the escalation of aggressive interactions. Consequently, dominants may benefit from the presence of experienced subordinates because they gain enhanced benefits in reproduction, or suffer less from aggressive interactions with others. Our results highlight the importance of an individual's own breeding experience and social status and that of other group members for mediating individual behaviour and social interactions in groups resulting in higher net fitness.</p>
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Allen Brain Atlas
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Annotated Behaviour and Observability Dataset (ABODe)
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.