AndreaBozzo/ceres-open-data-index huggingface dataset:
Combined ASTER and MODIS Emissivity database over Land (CAMEL) Coefficient Monthly Global 0.05Deg V002

The NASA Making Earth System Data Records for Use in Research Environments ([MEaSUREs](https://earthdata.nasa.gov/community/community-data-system-programs/measures-projects)) Combined Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Moderate Resolution Imaging Spectroradiometer (MODIS) Emissivity for Land (CAMEL) dataset provides monthly coefficients at 0.05 degree (~5 kilometer) resolution (CAM5K30CF). The CAMEL Principal Components Analysis (PCA) input coefficients utilized in the CAMEL high spectral resolution (HSR) algorithm are provided in the CAM5K30CF data product and are congruent to the temporally equivalent CAM5K30EM emissivity data product. Additional details regarding the methodology are available in the User Guide and Algorithm Theoretical Basis Document (ATBD). Provided in the CAM5K30CF product are layers for PCA coefficients, number of PCA coefficients, laboratory version, snow fraction derived from MODIS Snow Cover data (MOD10), latitude, longitude, and the CAMEL quality information. PCA coefficients are dependent on the version of lab PC data and number of PCs used. Improvements/Changes from Previous Version * Version 2 includes two additional laboratory datasets to more accurately characterize snowy scenes.

Tags: earth-science-snow-ice-terrestrial-hydrosphere-snow-cover, earth-science-surface-radiative-properties-land-surface-emissivity, earth-science-vegetation-biosphere-vegetation-index
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 ROSETTA EXTENSION 1 1430 V1.0

This is a Rosetta Radio Science data set, collected during the ROSETTA EXTENSION 1 phase 2016-01-01 to 2016-04-05. It is a Global Gravity measurement at the comet 67P and covers the time 2016-02-18T02:30:45.000 to 2016-02-18T09:11:43.999.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 3 ESC4-MTP023 RDR V3.0

This CODMAC level 3 data set contains radiometric calibrated image data in W/m^2/sr/nm, acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft during the COMET ESCORT 4 mission phase, covering the period from 2015-11-17T23:25:00.000 to 2015-12-15T23:24:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V3.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Lien corrected dataset after the July and October 2018 PSA/PDS external peer reviews. Updated documentation and ancillary files, added document on bandpass filter. Updated SCIENCE_USER_GUIDE_V03.PDF to include one section about FAQ and one section about image data quality. Added shutter backtravel and readout issues to image quality map. Updated DATA_QUALITY_ID keyword in image header. Improved handling of images with missing packets. Included FITs files. Browse products changed to the same size as the original image.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER EARTH OSIWAC 4 EAR2 RDR-REFLECT V1.0

This CODMAC level 4 data set contains radiometric calibrated and geometric distortion corrected (resampled)  image data in reflectance units (normalized and thus without unit),  acquired by the OSIRIS Wide Angle Camera on the Rosetta spacecraft  during the EARTH SWING-BY 2 mission phase, covering the period  from 2007-09-13T00:00:00.000 to 2008-01-27T23:59:59.000. The prime target is planet Earth. This version V1.0 is the first version of this dataset.

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Organization: National Aeronautics and Space Administration
VG2 URA CRS RESAMPLED SUMMARY D2 RATE                                       ELEC 96SEC V1.0

Counting rate from the D2 detector inthe Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 duringthe Uranus encounter. The D2 detector nominally responds to electrons withkinetic energies above approximately 2.5 MeV.

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Organization: National Aeronautics and Space Administration
Murchison Widefield Array 32-T Low-Frequency Source Catalog

The Murchison Widefield Array (MWA) is a new low-frequency, wide-field-of-view radio interferometer under development at the Murchison Radio-astronomy Observatory in Western Australia. The authors have used a 32 element MWA prototype interferometer (MWA-32T) to observe two 50 degree diameter fields in the southern sky, covering a total of ~ 2700 deg&lt;sup&gt;2&lt;/sup&gt;, in order to evaluate the performance of the MWA-32T, to develop techniques for epoch of reionization experiments, and to make measurements of astronomical foregrounds. They developed a calibration and imaging pipeline for the MWA-32T, and used it to produce ~15 arcminutes angular resolution maps of the two fields in the 110-200 MHz band. The authors perform a blind source extraction using these confusion-limited images, and detect 655 sources at high significance with an additional 871 lower significance source candidates. They compare these sources with existing low-frequency radio surveys in their paper in order to assess the MWA-32T system performance, wide-field analysis algorithms, and catalog quality. Their source catalog is found to agree well with existing low-frequency surveys in these regions of the sky and with statistical distributions of point sources derived from Northern Hemisphere surveys; it represents one of the deepest surveys to date of this sky field in the 110-200 MHz band. Observations were conducted with the MWA-32T in 2010 March during a two-week campaign (X13). Data were taken in three 30.72 MHz sub-bands centered at 123.52 MHz, 154.24 MHz, and 184.96 MHz in order to give (nearly) continuous frequency coverage between ~ 110 MHz and ~ 200 MHz. The observing time was divided between two fields. One field was centered on the bright extragalactic source Hydra A at RA (J2000) = 9&lt;sup&gt;h&lt;/sup&gt; 18&lt;sup&gt;m&lt;/sup&gt; 6&lt;sup&gt;s&lt;/sup&gt;, Dec (J2000) = -12^o 5&#39; 45&quot; to facilitate calibration. The other covered the Epoch of Reionization (EoR) field 2, centered at RA (J2000) = 10&lt;sup&gt;h&lt;/sup&gt; 20&lt;sup&gt;m&lt;/sup&gt; 0&lt;sup&gt;s&lt;/sup&gt;, Dec (J2000) = -10&lt;sup&gt;o&lt;/sup&gt; 0&#39; 0&quot;. The EoR2 field is one of two fields at high Galactic latitude that have been identified by the MWA Collaboration as targets for future EoR experiments. Although the centers of the Hydra A and EoR2 fields are separated by 15.3 degrees, there is considerable overlap between them since the half-power beam width of the primary beam is ~ 25 degrees at 150 MHz. Table 1 in the reference paper gives a journal of the observations. This table contains 648 radio sources which were detected in the full-band average map at or above a signal-to-noise ratio of 5. This table was created by the HEASARC in October 2012, based on an electronic version of table 2 from the reference paper as obtained from the ApJ website. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0590 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 1 phase 2014-11-20 to 2015-03-10. It is a Global Gravity measurement at the comet 67P and covers the time 2015-02-19T08:35:00.000 to 2015-02-19T10:34:39.000.

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Organization: National Aeronautics and Space Administration
Combined ASTER and MODIS Emissivity database over Land (CAMEL) Coefficient Climatology Monthly Global 0.05Deg V003

The NASA Making Earth System Data Records for Use in Research Environments ([MEaSUREs](https://earthdata.nasa.gov/about/competitive-programs/measures)) Combined Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Moderate Resolution Imaging Spectroradiometer (MODIS) Emissivity for Land (CAMEL) data suite has been expanded to include a monthly global coefficient climatology product (CAM5K30CFCLIM). The product is provided at 0.05 degree (~5 kilometer) resolution. The CAMEL Principal Components Analysis (PCA) input coefficients utilized in the CAMEL high spectral resolution (HSR) algorithm are provided in the CAM5K30CFCLIM data product. This HSR algorithm is accessible in both [MATLAB](https://lpdaac.usgs.gov/documents/2233/MATLAB_Source_Code.tar.gz) and [FORTRAN](https://lpdaac.usgs.gov/documents/2234/FORTRAN_Source_Code.tar.gz) programming languages, and it corresponds with the temporally equivalent [CAM5K30EMCLIM](https://doi.org/10.5067/MEaSUREs/LSTE/CAM5K30EMCLIM.003) emissivity data product. The HSR emissivity spectra for the same month each year and each unique combination of lab dataset version and number of Principal Components (PC)s are first computed independently and then combined via a weighted average. The weighted average over 2003 through 2021 (19 years) defines the weights by the number of samples from each unique combination. Additional details regarding the methodology are available in the User Guide and Algorithm Theoretical Basis Document (ATBD). Provided in the CAM5K30CFCLIM product are variables for PCA coefficients, the weights and sample numbers of the climatology coefficients used in the average calculation, sets of the number of PCA coefficients, laboratory version numbers, latitude, longitude, and land flag information. PCA coefficients depend on the lab PC data version and the number of PCs used.

Tags: earth-science-snow-ice-terrestrial-hydrosphere-snow-cover, earth-science-surface-radiative-properties-land-surface-emissivity, earth-science-vegetation-biosphere-vegetation-index
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 2 0831 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 2 phase 2015-03-11 to 2015-06-30. It is a Global Gravity measurement at the comet 67P and covers the time 2015-06-07T09:29:20.000 to 2015-06-07T11:19:12.000.

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Organization: National Aeronautics and Space Administration
SAGE-SMC IRAC Single Frame + Mosaic Photometry Catalog

The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. \n\nIn comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.

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Organization: National Aeronautics and Space Administration
EUVE Right Angle Program, 3rd Catalog

The Third Extreme Ultraviolet Explorer (EUVE) Right Angle Program (RAP) Catalog contains information on the detection of 76 extreme ultraviolet (EUV) sources, of which 63 are new detections, using the EUVE&#39;s RAP data. This catalog concentrates on observations made in the last years of the RAP, 1999 and 2000, with a sky coverage of 7% of the sky. The EUVE RAP used the all-sky survey telescopes (also known as &quot;scanners&quot;), 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/Boron or &quot;Lexan&quot;), 200 A (Al/Ti/C or &quot;Al/C&quot;), 400 A (Ti/Sb/Al or &quot;Dagwood&quot;), and 600 A (Sn/SiO or &quot;Tin&quot;). The EUVE RAP3 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 5 (8%) early-type stars, 23 (37%) late-type stars, 1 (2%) white dwarf, 1 (2%) cataclysmic variable, 4 (6%) extragalactic objects, 22 (35%) with no firm classification, and 7 (11%) with no optical identification. This final RAP Catalog, combined with the EUVE All-Sky Survey, the Lampton et al. (1997, ApJS, 108, 545) Faint EUV Source List, and previous RAP Catalogs, brings the total number of EUV sources to nearly 1200. This table was created by the HEASARC in September 2011 based on an ASCII version of Table 1 from the reference paper which was obtained from the AJ web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Combined ASTER and MODIS Emissivity database over Land (CAMEL) Emissivity Monthly Global 0.05Deg V001

The CAM5K30EM.001 dataset was decommissioned as of March 14, 2019. Users are encouraged to use the new improved [CAM5K30EM.003](https://doi.org/10.5067/MEaSUREs/LSTE/CAM5K30EM.003) dataset. The NASA Making Earth System Data Records for Use in Research Environments ([MEaSUREs](https://www.earthdata.nasa.gov/about/competitive-programs/measures)) Combined ASTER and MODIS Emissivity for Land (CAMEL) dataset provides monthly emissivity at 0.05 degree (~5 kilometer) resolution (CAM5K30EM). The CAM5K30EM data product was created by combining the University of Wisconsin-Madison MODIS Infrared Emissivity dataset (UWIREMIS) and the Jet Propulsion Laboratory ASTER Global Emissivity Dataset Version 4 (GED V4). The two datasets have been integrated to capitalize on the unique strengths of each product's characteristics. The integration steps include: adjustment of ASTER GED Version 3 emissivities for vegetation and snow cover variations to produce ASTER GED Version 4, aggregation of ASTER GED Version 4 emissivities from 100 meter resolution to the University of Wisconsin-Madison MODIS Baseline Fit (UWBF) 5 kilometer resolution, merging of the 5 ASTER spectral emissivities with the UWBF emissivity to create CAMEL at 13 hinge points, and extension of the 13 hinge points to high spectral resolution (HSR) utilizing the Principal Component (PC) regression method. Additional details regarding the methodology are available in the User Guide and Algorithm Theoretical Basis Document (ATBD). Provided in the CAM5K30EM product are variables for the CAMEL emissivity, ASTER Normalized Difference Vegetation Index (NDVI), snow fraction derived from MODIS (MOD10), latitude, longitude, CAMEL quality, ASTER quality, and Best Fit Emissivity (BFE) quality information.

Tags: earth-science-snow-ice-terrestrial-hydrosphere-snow-cover, earth-science-surface-radiative-properties-land-surface-emissivity, earth-science-vegetation-biosphere-vegetation-index
Organization: National Aeronautics and Space Administration
Einstein Observatory Clusters of Galaxies Catalog

The Einstein Observatory Clusters of Galaxies Catalog presents the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 which were observed with the Einstein Imaging Proportional Counter (IPC). For each cluster, the authors measured the 0.5 - 4.5 keV counting rate and computed the 0.5 - 4.5 keV source luminosity, as well as the bolometric luminosity within fixed metric radii. They detected 85% of Abell clusters with z &lt; 0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, they measured their X-ray surface brightness profiles and determined their core radii. For about 230 clusters, they then used either their measured core radii and beta values, or mean values derived for this sample, to measure central gas densities and gas masses. They used estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium. This table was created by the HEASARC in June 2005 based on the merger of CDS tables J/ApJ/511/65/table3.dat and table4.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
M 33 XMM-Newton Supernova Remnants Catalog

The authors of this catalog carried out a study of the X-ray properties of the supernova remnant (SNR) population in M 33 with XMM-Newton, comprising deep observations of eight fields in M 33 covering all of the area within the D&lt;sub&gt;25&lt;/sub&gt; contours, and with a typical luminosity of 7.1 x 10&lt;sup&gt;34&lt;/sup&gt; erg/s (0.2-2.0keV). With their deep observations and large field of view they have detected 105 SNRs at the 3-sigma level, of which 54 SNRs are newly detected in X-rays, and three are newly discovered SNRs. Combining XMM-Newton data with deep Chandra survey data allowed detailed spectral fitting of 15 SNRs, for which they have measured temperatures, ionization time-scales and individual abundances. This large sample of SNRs allowed the authors to construct an X-ray luminosity function, and compare its shape to luminosity functions from host galaxies of differing metallicities and star formation rates to look for environmental effects on SNR properties. They concluded that while metallicity may play a role in SNR population characteristics, differing star formation histories on short time-scales, and small-scale environmental effects appear to cause more significant differences between X-ray luminosity distributions. In addition, they analyze the X-ray detectability of SNRs, and find that in M 33 SNRs with higher [SII]/H-alpha ratios, as well as those with smaller galactocentric distances, are more detectable in X-rays. This catalog utilized data from a deep survey of M 33 using an 8 field XMM-Newton mosaic that extends out to the D25 isophote. The point source catalog from this survey was published by W15 (Williams+2015, J/ApJS/218/9). In addition to the catalog of W15, the authors utilized high-resolution observations from the Chandra ACIS Survey of M 33 (ChASeM33, Tullmann+2011, J/ApJS/193/31) for the purposes of obtaining X-ray spectral fits. This table was ingested by the HEASARC in October 2019 based upon the &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/472/308"&gt;CDS Catalog J/MNRAS/472/308&lt;/a&gt; files table2.dat and table3.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 3 OSIWAC 2 EDR MTP020 V1.0

This data set contains images acquired by the OSIRIS Wide Angle Camera during the COMET ESCORT 3 phase of the Rosetta mission at the comet 67P, covering the period from 2015-08-25T23:25:00.000 to 2015-09-22T23:24:59.000.

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Organization: National Aeronautics and Space Administration
2MASS 6X Point Source Working Database Table

During the final months of 2MASS observatory operations, a campaign of targeted "long exposure" observations was carried out during times when no previously unscanned parts of the sky were available for the main survey. These observations used the same freeze-frame scanning technique employed for the survey, but with READ2-READ1 exposures six times longer than was used for normal survey observations (hence they are referred to as "6x" observations). The 2MASS 6x measurements were intended to probe ~1 magnitude deeper than the main survey in unconfused regions.\n\nApproximately 590 deg2 of sky distributed in 30 targeted regions were scanned at least once using the long exposures. Most of this area is concentrated in two large, comprehensive surveys of the Large and Small Magellanic Clouds, 383 deg2 and 127 deg2, respectively. Twenty-eight additional smaller fields were mapped in the 6x mode from both observatories, covering targets that include the Pleiades open cluster, galactic star formation complexes, M31, nearby galaxy clusters and the Lockman Hole. \n\nData processing produced a 6x Image Atlas and 6x point and extended source Working Databases (6x-PSWDB and 6x-XSWDB), analogous to those from the main survey. "Catalogs" of point and extended source detections (6x-PSC and 6x-XSC) that represent uniform, higher reliability single-epoch snapshots of the near infrared sky were drawn from the 6x WDBs using SNR and quality criteria similar to those used to construct the All-Sky Release PSC and XSC (A3.6.c). The 6x-PSC and 6x-XSC have not received the same level of scrutiny and validation as the 2MASS All-Sky PSC and XSC, though.\n\nUnlike the All-Sky Release Catalogs, the 6x Catalogs are not released as separate tables. The 6x Point and Extended Source Catalogs are instead integrated into the respective 6x Point and Extended Source WDBs. Sources comprising the Catalogs are denoted in the WDBs with the cat flag, and have cat="1".

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Organization: National Aeronautics and Space Administration
HEAO 1 A2 Spectra

The A2 experiment was flown on the HEAO-1 satellite, between August, 1977 until January 1979. The experiment consisted of six multi-layer multi-anode collimated gas proportional counters. These were two LEDs (Low Energy Detectors), a MED (Medium Energy Detector), and three HEDs (High Energy Detectors). The first 6-months of mission were dedicated to an all-sky scan after which a pointing phase started. This database accesses the spectra (and associated files) obtained from the A2 MED (small and large field of view) and HEDs (1 and 3 small and large filed of view) detectors during the pointed phase. The spectra were generated for all HEAO-1 A2 pointed observations except for those in more unusual HEAO-1 modes (RAM-11 and &quot;radical RAMs&quot;). Thus the set of spectra created are only a subset (though a fairly complete one) of the entire catalog of HEAO-1 A2 pointed observations. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
30 Doradus Catalog ConeSearch

30 Doradus (a.k.a. the Tarantula Nebula), with its ionizing cluster R136, is one of the few known starbursts in the Local Group. For size (~200 pc in diameter) and density of OB stars, 30 Doradus parallels the regions of intense star formation observed in the starburst knots found in the  interacting galaxies in the Local Universe and the young galaxies at high redshift (z>5). \n\nHTTP is a panchromatic imaging survey of stellar populations in the Tarantula Nebula in the Large Magellanic Cloud that reaches into the sub-solar mass regime. HTTP utilizes the capability of the Hubble Space Telescope to operate the Advanced Camera for Surveys and the Wide Field Camera 3 in parallel to study this remarkable region in the near-ultraviolet, optical, and near-infrared spectral regions, including narrow-band Hα images. The high sensitivity, spatial resolution and broadband coverage of HTTP allow us to dissect the stellar populations and infer an accurate description of the anatomy of the Tarantula Nebula, and therefore to reconstruct for the first time the temporal and spatial evolution of a prototypical starburst on a sub-parsec scale.  \n\nAll available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.

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Organization: National Aeronautics and Space Administration