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Sentinel-3A OLCI Level-4 Global Mapped Apparent Visible Wavelength (AVW) Data, version 2022.0

The Ocean and Land Colour Instrument (OLCI) is the successor to ENVISAT's Medium Resolution Imaging Spectrometer (MERIS) having additional spectral channels, different camera arrangements and simplified on-board processing. The OLCI is a push-broom instrument with five camera modules sharing the field of view. The field of view of the five cameras is arranged in a fan-shaped configuration in the vertical plane, perpendicular to the platform velocity. Each camera has an individual field of view of 14.2° and a 0.6° overlap with its neighbors. The whole field of view is shifted across track by 12.6° away from the sun to minimize the impact of sun glint. OLCI is equipped with on-board calibration hardware based on sun diffusers. There are three sun diffusers--two 'white' diffusers dedicated to radiometric calibration and one dedicated to spectral calibration, with spectral reflectance features. The native resolution is approximately 300m, refered to as Full Resolution (FR). A Reduced Resolution (RR) processing mode provides Level-1B data at sampling rates decreased by a factor of four in both spatial dimensions resulting to resolution of approximately 1.2 km.

Sentinel-3B OLCI Level-4 Global Mapped Apparent Visible Wavelength (AVW) Data, version 2022.0

Sentinel-3A OLCI Level-4 Global Binned Apparent Visible Wavelength (AVW) Data, version 2022.0

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1216 Å in North Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the first H Ly-alpha, 1216 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a North Polar Projection.

All-Wavelength Extended Groth Strip Int. Survey (AEGIS) VLA 20-cm Source Catalog

This table contains results from AEGIS20, a radio survey of the Extended Groth Strip (EGS) conducted with the Very Large Array (VLA) at a frequency of 1.4 GHz. The resulting catalog contains 1122 emitters (HEASARC Note: The abstract of the original reference paper said 1123, but as noted by Willner et al. (2012, ApJ, 756, 72: footnote 10, one entry ('EGS20 J142303.7+532224.5') was listed twice in the original catalog), and it is sensitive to ultraluminous (1012 solar luminosities) starbursts to z <= 1.3, well matched to the redshift range of the DEEP2 spectroscopic survey in this region. The authors use stacking techniques to explore the microJansky-level emission from a variety of galaxy populations selected via conventional criteria - Lyman break galaxies (LBGs), distant red galaxies (DRGs), UV-selected galaxies, and extremely red objects (EROs) - determining their properties as a function of color, magnitude, and redshift and their extinction-free contributions to the history of star formation. This study confirms the familiar pattern that the star formation rate (SFR) density, increases by at least a factor of ~ 5 from z = 0 to 1, although the authors note highly discrepant UV- and radio-based SFR estimates. Their radio-based SFRs become more difficult to interpret at z > 1 where correcting for contamination by radio-loud active galactic nuclei (AGNs) comes at the price of rejecting luminous starbursts. While stacking radio images is a useful technique, accurate radio-based SFRs for z >> 1 galaxies require precise redshifts and extraordinarily high fidelity radio data to identify and remove accretion-related emission. Data were obtained at 1.4 GHz during 2003 to 2005 with the VLA in its B configuration, acquiring seven 3.125 MHz channels every 5 s at each of four intermediate frequencies. Data were obtained at six positions, spaced by 15 arcminutes, concentrating in the northern half of the EGS because of the proximity of 3C 295 (a 23 Jy source at 1.4 GHz). Around 18 hours of data were acquired for each of the field positions. Calibrated visibilities and associated weights were used to generate mosaics of 37 x 5122 x 0.8 arcsec2 pixel images to quilt the VLA's primary beam in each EGS field position. CLEAN boxes were placed tightly around all sources, and a series of IMAGR and CALIB tasks were run, clipping the UV data after subtracting CLEAN components generated by the third iteration of IMAGR. The central images from each of the pointings were then knitted together using FLATN, ignoring data beyond the primary beam's half-power point, to produce a large mosaic. The synthesized beam is circular, with a FWHM of ~ 3.8 arcseconds. To define a sample of radio sources, the authors searched signal-to-noise ratio (S/N) images using the SAD detection algorithm, emulating the technique described by Biggs & Ivison (2006, MNRAS, 371, 963). Sources with >= 4-sigma peaks were fitted with two-dimensional Gaussians using JMFIT, and those with >- 5-sigma peaks that survived were fitted in total intensity. Sources with sizes equal to or smaller than the restoring beam were considered unresolved. No correction is made for bandwidth smearing in the catalog; this is a small effect (~ 5%) given the mosaicking strategy and the use of the B configuration. 38, 79, 171, 496, and 1123 sources are detected with 1.4 GHz flux densities >= 2000, >= 800, >= 320, >= 130 and >= 50 microJansky (µJy) [including the duplicate source mentioned above], where the 5-sigma detection limits at 130 and 50 uJy cover 0.73 and 0.04 deg2, respectively. Confusion is not an issue; the source density on an arcmin2 scale is < 0.01 beam-1. This table was created by the HEASARC in July 2013 based on an electronic versions of the catalog described in the reference paper which was obtained as a FITS file from the first author's web site at <a href="http://www.roe.ac.uk/~rji/aegis20/">http://www.roe.ac.uk/~rji/aegis20/</a>. This is a service provided by NASA HEASARC .

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength LBH1 in South Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the fourth LBH1, 1400-1500 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a South Polar Projection.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1356 Å in North Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the third OI, 1356 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a North Polar Projection.

Sentinel-3B OLCI Level-4 Global Binned Apparent Visible Wavelength (AVW) Data, version 2022.0

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength LBH2 in South Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the fifth LBH2, 1650-1800 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a South Polar Projection.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1304 Å in South Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the second OI, 1304 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a South Polar Projection.

All-Wavelength Extended Groth Strip Int. Survey (AEGIS) 20-cm Fully Id-ed Sample

Infrared 3.6 - 8.0 micron (µm) images of the Extended Groth Strip (EGS) yield plausible counterpart identifications for all but one of 510 radio sources in the AEGIS20 S(1.4 GHz) > 50 microJansky (µJy) sample (Ivison et al. 2007, ApJ, 660, L77, available at the HEASARC as the AEGIS20 database table). This is the first such deep sample that has been effectively 100% identified. Achieving the same identification rate at R band would require observations reaching RAB > 27. Spectroscopic redshifts are available for 46% of the sample and photometric redshifts for an additional 47%. Almost all of the sources with 3.6-um AB magnitudes brighter than 19 have spectroscopic redshifts z < 1.1, while fainter objects predominantly have photometric redshifts with 1 <~ z <~ 3. Unlike more powerful radio sources that are hosted by galaxies having large stellar masses within a relatively narrow range, the AEGIS20 counterparts have stellar masses spanning more than a factor of 10 at z ~ 1. The sources are roughly 10% - 15% starbursts at z <~ 0.5 and 20%-25% active galactic nuclei mostly at z > 1, with the remainder of uncertain nature. Throughout this study, magnitudes are in the AB system, and the notation [w] means the AB magnitude at wavelength w in um. Source distances are based on standard Lambda-CDM cosmology with H0 = 71 km s-1 Mpc-1 and OmegaM = 0.27. Practical calculation of luminosity distances was based on the program ANGSIX (Kayser et al. 1997, A&A, 318, 680). This table was created by the HEASARC in July 2013 based on the electronic versions of Tables 1, 3, 4, and 5 from the reference paper which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1304 Å in Mercator Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the second OI, 1304 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a Transverse Mercator Projection.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1304 Å in North Polar Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the second OI, 1304 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a North Polar Projection.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1216 Å in South Polar Projection

NOAA-20 VIIRS Level-4 Global Binned Apparent Visible Wavelength (AVW) Data, version 2022.0

The Visible and Infrared Imager/Radiometer Suite (VIIRS) is a multi-disciplinary instrument that is being flown on the Joint Polar Satellite System (JPSS) series of spacecraft, including the Suomi National Polar-orbiting Partnership (S-NPP) that launched in October 2011. JPSS is a multi-platform, multi-agency program that consolidates the polar orbiting spacecraft of NASA and the National Oceanic and Atmospheric Administration (NOAA). S-NPP is the initial spacecraft in this series, and VIIRS is the successor to MODIS for Earth science data product generation. VIIRS has 22 spectral bands ranging from 412 nm to 12 nm. There are 16 moderate-resolution bands (750m at nadir), 5 image-resolution bands (375m), and one day-night band (DNB).

OMPS-N21 LP NRT Aerosol Extinction Vertical Profile swath multi-wavelength orbital 3slit

The OMPS-N21 Level 2 LP Aerosol Extinction Vertical Profile swath level 2 3slit (AER) product contains the retrieved aerosol extinction coefficients measured by the Ozone Mapping and Profiling Suite (OMPS) Limb-Profiler (LP) sensor on the NOAA-N21 satellite. The AER product measures stratospheric aerosol abundance and evolution at 6 wavelengths (510, 600, 675, 745, 869 and 997 nm) to complement the OMPS LP measurements of stratospheric and mesospheric profile ozone. This product replaces the previous single wavelength 675 nm (AER675) product. Each granule contains data from the daylight portion of each orbit. Spatial coverage is global (-90 to 90 degrees latitude), and there are about 14.5 orbits per day each measuring three limb profiles spaced approximately 250 km in the cross-track direction. The profiles are measured from the ground up to about 80 km with a vertical resolution of the retrieved profiles of approximately 1.8 km. The files are written using the Hierarchical Data Format Version 5 or HDF5. The /ProfileFields/RetrievedExtCoeff dataset is produced via a neural network trained on LP-L2-AER data for NRT processing.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength LBH2 in Mercator Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the fifth LBH2, 1650-1800 Å, Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a Transverse Mercator Projection.

TIMED Global Ultraviolet Imager (GUVI) Airglow Flux 14-day Movies, at Wavelength 1216 Å in Mercator Projection

GUVI measures FUV Airglow in five Spectral Bands: the atomic HI Lyman-alpha Band, 121.6 nm, two atomic Oxygen OI Bands, 130.4 nm and 135.6 nm, and the molecular Nitrogen Lyman-Birge-Hopfield Short, LBHS, 141 to 152.8 nm, and Lyman-Birge-Hopfield Long, LBHL, 167.2 to 181.2 nm, Bands. The Cross-Track Scanning Spectrograph images a Ground Swath of 3000 km Width providing nearly Contiguous Global Coverage with 15 Orbits per Day. This L1CDisk, Level 1C Disk, Version 3, File provides the calibrated, geolocated, and rectified Intensities for the first H Ly-alpha, 1216 Å Wavelength Band. This is a Movie with mapped Images of the Log Intensities by Orbit by using a Transverse Mercator Projection.

OMPS-NPP LP NRT Aerosol Extinction Vertical Profile swath multi-wavelength orbital 3slit

The OMPS-NPP L2 LP Aerosol Extinction Vertical Profile swath l2 3slit (AER) product contains the retrieved aerosol extinction coefficients measured by the Ozone Mapping and Profiling Suite (OMPS) Limb-Profiler (LP) sensor on the Suomi-NPP satellite. The AER product measures stratospheric aerosol abundance and evolution at 6 wavelengths (510, 600, 675, 745, 869 and 997 nm) to complement the OMPS LP measurements of stratospheric and mesospheric profile ozone. This product replaces the previous single wavelength 675 nm (AER675) product. Each granule contains data from the daylight portion of each orbit measured for a full day. Spatial coverage is global (-90 to 90 degrees latitude), and there are about 14.5 orbits per day each measuring three limb profiles spaced approximately 250 km in the cross-track direction. The profiles are measured from the ground up to about 80 km with a vertical resolution of the retrieved profiles of approximately 1.8 km. The files are written using the Hierarchical Data Format Version 5 or HDF5. The /ProfileFields/RetrievedExtCoeff dataset is produced via a neural network trained on LP-L2-AER data for NRT processing.