These are the unprocessed electron back scatter diffraction patterns (EBSPs) collected from the mesas of electron beam induced deposition (EBID) material, in addition to the Mathematica notebook used to process the images. Each of the 12 EBID mesa has 10 EBSPs collected at 20 kV and 10 kV, in addition to several longer line scans that step from the silicon substrate onto the EBID mesa.

The file contains Level 1 3D electron distributions in burst mode from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Ahead spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

"Since the summer of 2000 we have successfully deployed a high resolution x-ray microcalorimeter spectrometer, based on the spaceflight XRS instrument, at the Electron Beam Ion Trap (EBIT) facility at the Lawrence Livermore National Laboratory. Over the last decade, this highly successful partnership has made fundamental measurements in laboratory astrophysics including the measurements of the absolute cross sections of all the Fe L shell transitions from Fe XVII to Fe XXIV, line ratios in Fe and Ni L shell transitions, measurements of Fe K shell emission over a wide range of electron energies, and direct measurements of charge exchange emission from highly ionized Fe, O, N, and most recently L shell S, using a variety of donor gases. This work has resulted in the publication of over 30 peer-reviewed articles with many more either submitted or in preparation. The newest addition to the facility, the ECS microcalorimeter spectrometer, developed under this program, has performed flawlessly as a facility-class instrument since 2007. We propose here to continue our highly successful partnership and deploy new technology to resolve lines in the important 1/4 keV band that encompasses the M-shell iron emission and the L shell emission, including charge exchange, of many of the lower-Z elements, such as Si, S, Mg, Ne, Ca, and Ar. We thus propose completing a new spectrometer that will bring substantially improved performance to the laboratory astrophysics program at EBIT and will enable fundamentally new measurements. Thus, in addition to maintaining the current spectrometers, which will begin this work, a significant component of this proposal is the completion of a new spectrometer leveraged off of the substantial progress in high-resolution x-ray detectors developed for the International X-ray Observatory mission. The spectrometer will be composed of a detector system with unparalleled spectral resolution: 2 eV resolution across the 0.05-10 keV band. This will allow

The file contains Level 1 3D electron distributions in burst mode from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Behind spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

This X-ray transition table provides the energies and wavelengths for the K and L transitions connecting energy levels having principal quantum numbers n = 1, 2, 3, and 4. The elements covered include Z = 10, neon to Z = 100, fermium. There are two unique features of this database: (1) all experimental values are on a scale consistent with the International System of measurement (the SI) and the numerical values are determined using constants from the Recommended Values of the Fundamental Physical Constants: 1998 [115] and (2) accurate theoretical estimates are included for all transitions. Version 1.2

The file contains Level 1 3D electron distributions from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Ahead spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

The NIST Database for the Simulation of Electron Spectra for Surface Analysis (SESSA) can be used to simulate Auger-electron spectra and X-ray photoelectron spectra of nanostructures such as islands, lines, spheres, and layered spheres on surfaces. As for earlier versions, such simulations can be performed for multilayer films. Users can specify the compositions and dimensions of each material in the sample structure as well as the measurement configuration. The database contains extensive physical data needed for quantitative interpretations of observed spectra. A more detailed description of SESSA has been published [W. Smekal, W. S. M. Werner, and C. J. Powell Surf. Interface Anal. 37, 1059 (2005)].

The file contains Level 1 3D electron distributions from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Behind spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

THEMIS-D: Electrostatic Analyzers (ESA): Electron/Ion Ground-Calculated Energy Fluxes (5eV - 25 keV for Ions and 6eV - 30 KeV for Electrons) and Moments (density, velocity, pressure, and temperature). The satellite has 2 modes Fast and Slow survey and 3 data types: FULL, REDUCED and BURST. FULL: 88 angles x 32 energies, time resolution of 128 spins(395 seconds) in slow survey and 32 spins(98 seconds) in fast survey. REDUCED: spin time resolution(3 sec) but angles averaged into 1 angular spectra x 32 energies in slow survey or 6 angular spectra(90 degree x 90 degree window) x 32 energies in fast survey. BURST: 88 angles x 32 energies and spin time resolution(3 sec) but only available sporadically and for short duration. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. These moments are processed on the ground. They should be regarded as approximations but will improve in quality as our processing routines are improved over the course of the mission to account for additional sources of variance.

Precipitating Electrons And ions observed at nominally 850 km Altitude and over a Range of Energies from 30 eV to 30 keV by using the Special Sensor J, SSJ, Instrument. Please contact Rob.Redmon@noaa.gov with Questions and Comments. Many Individuals made Important Contributions including: D. Hardy, E. Holeman, F. Rich, D. Ober, G. Wilson, J. Machuzak, K. Kadinsky-Cade, J. McGarity, W.F. Denig, K. Martin, R. Redmon, D. Knipp, L. Kilcommons.