The data from this instrument consists of sets of measurements of Xray intensity as a function of diffraction angle. Almost all of it is collected using a position-sensitive detector (PSD), and is stored in CIF format.

This data presented with this data set includes: (a) The IRAS Detector File which provides for each detector of the focal plane array its operational status, associated filter, location, dimension, sterradiance, and readout time offset; (b) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 1 (12 microns); (c) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 2 (25 microns); (d) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 3 (60 microns); (e) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 4 (100 microns).

This data presented with this data set includes: (a) The IRAS Detector File which provides for each detector of the focal plane array its operational status, associated filter, location, dimension, sterradiance, and readout time offset; (b) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 1 (12 microns); (c) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 2 (25 microns); (d) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 3 (60 microns); (e) The transmission and response values given in this table are to energy/wavelength and represent averages over all of the IRAS detectors of Band 4 (100 microns).

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.

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 data include 15-second average raw count rates in Channels 1 - 3 and First Order (26 - 34 nm, average of Ch1 and Ch3) and Central Order (0.1 - 50 nm, Ch2) photon fluxes, as well as SOHO Heliocentric location and distance. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. The original ASCII dataset Version 4 science product release notes are available at https://lasp.colorado.edu/eve/data_access/eve_data/lasp_soho_sem_data/long/LASP_SOHO_SEM_release_notes_v4.pdf. Description of the CELIAS-SEM instrument and scientific scope can be found on the CELIAS home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.

This table contains the first results of the authors' optical spectroscopy program aimed to provide redshifts and identifications for the X-ray sources in the Extended Chandra Deep Field South (ECDFS). A total of 339 sources (listed herein) were targeted using the IMACS spectrograph at the Magellan telescopes and the VIMOS spectrograph at the VLT. The authors have measured redshifts for 186 X-ray sources, including archival data and a literature search. They find that the active galactic nucleus (AGN) host galaxies have on average redder rest-frame optical colors than nonactive galaxies, and that they live mostly in the "green valley." The dependence of the fraction of AGNs that are obscured on both luminosity and redshift is confirmed at high significance and the observed AGN spatial density is compared with the expectations from existing luminosity functions. These AGNs show a significant difference in the mid-IR to X-ray flux ratio for obscured and unobscured AGNs, which can be explained by the effects of dust self-absorption on the former. This difference is larger for lower luminosity sources, which is consistent with the dust opening angle depending on AGN luminosity. This table was created by the HEASARC in April 2009 based on the electronic version of Table 2 from the Treister et al. (2009) paper obtained from the ApJ web site, except for the source positions which were taken from Virani et al. (2006). The full table from the latter paper is also available in Browse (the ECDFSCXO table). This is a service provided by NASA HEASARC .

Energy dispersive X-ray spectroscopy (EDX) tomographic tilt series of a needle-shaped sample extracted from NIST SRM 2135c.Sample description: This SRM consists of alternating layers of nickel and chromium on a silicon substrate (see SRM certificate for further detail).Data description. The scan size for each spectrum image (SI) is 128 pixels x 100 pixels and 4000 spectral channels deep. EDX data were collected using the following parameters:Beam energy (keV): 300.0Probe current: 0.5 nAPixel size: 3.0 nmDwell time per pixel: 200 msecEnergy resolution: 10 eV/channelThe SI's were collected over a 180 degree range of specimen tilts with a 5 degree tilt step between each acquisition.

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually operates in Slow Survey (SS) Mode (60 s Resolution) outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Partial Moments that come from performing the Standard Moment Integrals over a limited Portion of Velocity Space. The resulting Quantities are named similarly to their corresponding Standard Moments, but are decorated with 'part' to differentiate. For example, density_part is the Density Moment integrated from a particular Energy Step to Infinity. These Partial Moments are formed from the indicated Data Type (DES/DIS Burst, FS or SS). For convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually Operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Results from integrating the standard Moments of Phase Space Distributions formed from the indicated Data Type (DES/DIS Burst, FS or SS). For Convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.