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35 results for “EUV”
EUV optical constants data set
<p>Dataset of optical constants in the extreme ultraviolet (EUV) spectral range, including 13.5nm, obtained from reflectivity measurements.</p>
Composite X-EUV + optical model spectrum of the planet-hosting star HIP 67522 (HD 120411)
<p>Composite spectrum of HIP 67522 obtained by joining a Phoenix photospheric spectrum with the X-EUV spectrum synthesized from the reconstructed plasma Emission Measure Distribution (EMD) vs. temperature in chromosphere, transition region, and corona. The FITS file contains 3 extensions with the spectrum, the EMD, and the plasma chemical abundances, derived from the analysis of X-ray and FUV high-resolution spectra, obtained with simultaneous observations with XMM-Newton and HST.</p> <p>In the attached figure, the upper panel shows the specific flux at Earth, while the bottom panel is the photon flux at a distance of 1 AU. In green the Phoenix spectrum resampled to a wavelength resolution of 1 Angstrom, down to 1700 A; the XUV spectrum in the range 1-1700 A instead has a resolution of 0.01 A. The green and blue segments in the upper panel, at about 200 nm, mark the Phoenix model flux and the observed flux integrated over the OM UVM2 band.</p>
EUV-ML solar physics dataset from STEREO + SOHO, 2 solar cycles
<p>A unified ML-ready dataset of all SOHO EIT and STEREO EUVI EUV images, aligned and set to 512x512 pixels, are available via the NASA TOPS ODR in HelioCloud at s3://gov-nasa-hdrl-data1/contrib/euvml/ (inside of AWS, and with free egress via https). We also provide the software used to create it via a public github repository, and a sample Python Jupyter Notebook (in this Zenodo link, and in the HelioCloud sample tutorials) for accessing them via the 'cloudcatalog' Python client.We</p> <p>We created a full set of ML-ready EUV data from 1995 to present, accessible via the cloud, by bringing in historical restoration of the STEREO/SOHO era into a machine-learning (ML) -ready dataset. This work will enable research on events, evolution of solar irradiance, segmentation approaches, 360 degree maps of the sun, and other research topics as well as for use with space weather. The reduced dataset is 6TB in size. The data will be freely available to scientists both within the AWS cloud and for downloading for local use on their laptops. The creation of this dataset had several steps, starting with the mechnical ingest stage (get the raw data), an analysis of best approach to create the ML-ready set, bulk processing, uploading the cloud, and dissemination and promotion. The task also required determination best approaches for cadence matching, interpolation, and effective spans of contiguous data for ML applications.</p> <p>Work was funded under NASA Heliophysics 21-LWSTM21_2-0018, award number 80NSSC22K0643.</p>
EUV-Induced Hydrogen Desorption As A Step Towards Large-Scale Silicon Quantum Device Patterning
<p><strong>Dataset: </strong>STM, XPS and PEEM raw data, processed data and the codes used for data fitting our <a href="https://doi.org/10.1038/s41467-024-44790-6">published work</a> are all available here.</p> <p><strong>Abstract: </strong>Atomically precise hydrogen desorption lithography using scanning tunnelling microscopy (STM) has enabled the development of single-atom, quantum-electronic devices on a laboratory scale. Scaling up this technology to mass-produce these devices requires bridging the gap between the precision of STM and the processes used in next-generation semiconductor manufacturing. Here, we demonstrate the ability to remove hydrogen from a monohydride Si(001):H surface using extreme ultraviolet (EUV) light. We quantify the desorption characteristics using various techniques, including STM, X-ray photoelectron spectroscopy (XPS), and photoemission electron microscopy (XPEEM). Our results show that desorption is induced by secondary electrons from valence band excitations, consistent with an exactly solvable non-linear differential equation and compatible with the current 13.5 nm (~92 eV) EUV standard for photolithography; the data imply useful exposure times of order minutes for the 300 W sources characteristic of EUV infrastructure. This is an important step towards the EUV patterning of silicon surfaces without traditional resists, by offering the possibility for parallel processing in the fabrication of classical and quantum devices through deterministic doping.</p> <p> </p>
The height-dependent delayed ionospheric response to solar EUV - artificial run
<p>These artificial runs use the TIE-GCM v2.0 model in its 2.5 × 2.5 configuration as the real condition model run. In order to converge to stable initial condition the TIE GCM runs for 30 days prior to the final simulation starting at 21 September 2010. This initial run was configured with default parameters. Both model runs start at 21 October 2010 and are calculated with default parameters except for the switched off auroral parameterization as well as the switched off high-latitude potential model. The influence of noise in solar activity is reduced by applying an artificial noise free sinusoidal time series for the F10.7 input.</p>
Raw ptychography data for manuscript with title 'Structured Illumination Ptychography and At-wavelength Characterization with an EUV diffuser at 13.5 nm Wavelength'
<p>- Given are the HDF files containing the raw diffraction patterns<br> - Although some meta-data might be available in these files, these might not be correct. The following data were used for reconstruction:<br> wavelength: 13.5 nm<br> distance sample <-> detector: ~29.2 mm<br> sCMOS pixel size: 11 um<br> Number of incoherent modes: 4<br> Initial probe guess: 9 um<br> For the reconstruction, OPR was used (Although it might have not been necessary for all data. However, to have comparable results it was used for each reconstruction)<br> - For each scenario, there are two data sets to calculate the Fourier ring correlation (FRC)<br> - For the analysis of the diffuser the reconstructed probe of the data set "dp_diffuser_max_dynam_range.hdf5" was used</p> <p>- Data were measured at the Institute of Applied Physics in Jena using a Fiber Laser driven High-order harmonic source</p> <p>Please contact me (wilhelm.eschen@uni-jena.de) for additional support.</p>
"Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index" Figures, Scripts, and Data
<p>These tar files, scripts, and datasets were used in the paper "Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index," submitted for publication to the Space Weather Journal. More information on what is included in this archive can be found the the ReadMe file. </p>
The height-dependent delayed ionospheric response to solar EUV - data comparison - secondary files 141 - 143
<p><strong>Secondary files for doy 141 - 143</strong></p> <p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p>
The height-dependent delayed ionospheric response to solar EUV - data comparison - secondary files 135 - 140
<p><strong>Secondary files for doy 135 - 140</strong></p> <p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p>
The height-dependent delayed ionospheric response to solar EUV - data comparison - secondary files 129 - 134
<p><strong>Secondary files for doy 129 - 134</strong></p> <p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p>
The height-dependent delayed ionospheric response to solar EUV - data comparison - secondary files 117 - 122
<p><strong>Secondary files for doy 117 - 122</strong></p> <p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p>
The height-dependent delayed ionospheric response to solar EUV - data comparison
<p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p> <p>Secondary files:</p> <p>117 - 122: <a href="https://zenodo.org/record/6004534">https://zenodo.org/record/6004534</a></p> <p>123 - 128: <a href="https://zenodo.org/record/6006516">https://zenodo.org/record/6006516</a></p> <p>129 - 134: <a href="https://zenodo.org/record/6009777">https://zenodo.org/record/6009777</a></p> <p>135 - 140: <a href="https://zenodo.org/record/6014195">https://zenodo.org/record/6014195</a></p> <p>141 - 143: <a href="https://zenodo.org/record/6014201">https://zenodo.org/record/6014201</a></p> <p> </p>
Ionospheric Connection Explorer (ICON) EUV Lunar Calibration Data
<p>This dataset provides the processed lunar calibraton data for the Ionospheric Connection Explorer Extreme Ultraviolet Spectrometer (ICON EUV) that were used in the study by Sirk et al. (2024, submitted).</p>
The height-dependent delayed ionospheric response to solar EUV - data comparison - secondary files 123 - 128
<p><strong>Secondary files for doy 123 - 128</strong></p> <p>For comparison with the observational results a TIE-GCM v2.0 model run in the 2.5 × 2.5 configuration is calculated. In order to converge to stable initial condition the model runs for 30 days prior to the final simulation starting at 28 March 2019. This initial run is configured with default parameters. The final run from 27 April 2019 to 24 May 2019 uses the default configuration of TIE-GCM with the Heelis Electric Convection Field Model (Heelis et al., 1982) as the high-latitude potential model. The input forcing is used from the NASA/GSFC’s OMNI data set</p>
Exploration of the Transition Region-Corona Interface With the Multi-Order Solar EUV Spectrograph Project
<p> We propose to observe the solar upper transition region and lower corona in Ne VII 46.5 nm with the Multi-Order Solar EUV Spectrograph (MOSES) rocket payload. The solar plasma in this temperature range, about 500,000 K, has not been imaged at rapid cadence since Skylab (Feldman, 1987). The unique observational capabilities of MOSES, demonstrated already in He II 30.4 nm, enable simultaneous imaging and measurement of line widths and doppler shifts over a large (20&rsquo; x 10&rsquo;) field of view, with typical active region exposure times of 10 s. These observations will reveal the 3D dynamics of outflows and reconnection events in active regions, quiet Sun, and coronal holes. The primary objectives of this one-year proposal are (1) instrument calibration, (2) launch of the rocket in summer of 2012, and (3) data analysis, including exploration of new techniques to recover more spectral information from the MOSES data. Prior NASA funding has enabled data analysis and publication of results from the first flight, upgrades to the payload, and increased reliability of our ground support equipment. Procurement of optics to observe the Ne VII 46.5 nm line is in process. With the help of additional funding from Montana Space Grant Consortium, we have also developed an EUV calibration facility optimized for testing the MOSES payload.</p> <p> N/A</p>
EUVE Archive and Observation Log
This catalog of the EUVE Science Archive has been constructed based on information provided by personnel of the Center for Extreme-Ultraviolet Astrophysics (CEA), and is made available in the current EUVEMASTER database table. Most of the information in the catalog is also in the headers of the FITS files. The HEASARC now has nearly all of the 1378 pointed EUVE Deep Survey/Spectrometer (DS/S) datasets that were processed by CEA until its closing in March 2001. There are a small number of observations that were made in the year 2000 for which the HEASARC does not currently have the corresponding datasets. Notice that this catalog does not contain entries corresponding to EUVE observations in scan mode or where the files received by the HEASARC were not of the normal image or events type. This is the 7th (and possibly final) version of the EUVEMASTER database, last updated in June 2001. This catalog has been constructed based on information provided by staff members of the Center for Extreme-Ultraviolet Astrophysics (CEA) in Berkeley, CA, whose help is gratefully acknowledged. This is a service provided by NASA HEASARC .
IMAGE Extreme UltraViolet (EUV) Imager, Modified Data 2 (M2), 10 min Data
The IMAGE extreme ultraviolet (EUV) imager detects resonantly scattered solar EUV photons with a wavelength of 30.4 nm that have been resonantly scattered by singly ionized helium (Sandel et al., 2000). The sizeable database of IMAGE global snapshots from the extreme ultraviolet (EUV) imager provides revolutionary observations of spatial and temporal plasma distributions throughout the plasmasphere. In this study, the IMAGE EUV data have been mapped to the equator using the approach detailed in Gallagher et al. (2005). IMAGE EUV data have been used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient in order to identify the magnetic local time, MLT, dependent plasmapause position as a function of time. This description has been adapted from text appearing in Katus et al. (2015).
ROSAT Archival WFC EUV Data
The WFCPOINT database table contains the list of ROSAT-Wide Field Camera calibration (CAL), performance verification (PV), and AO phase observations. For each observation listed in WFCPOINT, the target name, celestial co-ordinates, sequence number, PI name, and proposal title are given. The date of the observation, date that the data were distributed, and the date that the data will be released to the public are also given. The public release date is nominally 1 year and 14 days after the distribution date; however, because of some processing problems with a few datasets, the actual release date will be delayed from the given date. One duplicate entry was removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
EUVE Bright Sources
This database table contains a detailed list of verified bright EUVE sources detected during the survey phase of the EUVE mission (calibration targets are also included). Two distinct surveys, the all-sky and deep surveys, were conducted by the four EUVE telescopes during the first six months of the mission. Further documentation is available through the HEASARC. This is a service provided by NASA HEASARC .
EUVE Right Angle Program, 2nd Catalog
The Second Extreme Ultraviolet Explorer (EUVE) Right Angle Program (RAP) Catalog contains information on the detection of 235 extreme ultraviolet (EUV) sources, of which 169 are new detections, using the EUVE's RAP data. This catalog included observations made since the first EUVE RAP catalog (1994 January) and covered 17% of the sky. The EUVE RAP used the all-sky survey telescopes (also known as "scanners"), which were mounted at right angles to the Deep Survey and Spectrometer instruments, to obtain photometric data in four wavelength bands centered at 100 Angstroms (Lexan/B), 200 A (Al/Ti/C), 400 A (Ti/Sb/Al or Dagwood), and 550 A (Sn/SiO). The EUVE RAP2 Catalog contains source count rates and probable source identifications from the available catalogs and literature. The source distribution is similar to previous EUV catalogs with 2% early-type stars, 45% late-type stars, 8% white dwarfs, 6% extragalactic objects, 24% with no firm classification, and 15% with no optical identification. This database was created at the HEASARC in May 2002 based on the ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/AJ/117/2466">CDS Catalog J/AJ/117/2466</a> and is derived from Tables 2, 3, and 4 the published paper. This is a service provided by NASA HEASARC .
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
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.