AndreaBozzo/ceres-open-data-index huggingface dataset:
2MASS Calibration Extended Source Working Database

Photometric calibration for 2MASS was performed using observations of calibration fields made at regular intervals during each night of survey operations. Measurements of standard stars in the fields were used to derive the photometric zero point offsets as a function of time during each night. Atmospheric extinction coefficients were derived from 2MASS observations made over long periods.\n\n2MASS calibration fields, or tiles, are 1° long in declination and approximately 8.5' wide in right ascension. There are 35 regular survey calibration fields distributed at approximately two hour intervals in right ascension near declinations of approximately -30°, 0° and +30°. An additional five calibration fields were defined in and around the Large and Small Magellanic Clouds to support the deep observation (6x) campaign towards the end of survey operations.\n\nOver the course of the survey, the regular calibration fields were scanned between 562 and 3692 times in nominally photometric conditions. Equatorial fields were observed from both observatories, so were observed more frequently than those near ±30° which were observed with only one telescope. The special Magellanic Cloud calibration fields were observed 108 to 468 times between November 2000 and February 2001.\n\nCalibration scan Atlas Images, and Point and Extended Source Working Databases (Cal-PSWDB and Cal-XSWDB), analogous to those from the main survey, were produced from the calibration scan pipeline data reduction. The calibration Image Atlas and WDBs are the fundamental processing archives of the data from 73,230 calibration scans taken in photometric conditions during 2MASS survey operations. The Cal-WDBs contain positions, magnitudes and characteristics of 191,464,020 and 403,811 point and extended "source" extractions, respectively. The calibration Image Atlas contains 878,769 FITS images in the three survey bandpasses redundantly covering ~5 deg2 of sky. Unlike the main survey and 6x observations, "Catalogs" have not been derived from the Calibration WDBs.

Tags: __
Organization: National Aeronautics and Space Administration
PEP SPIRE 500 micron Catalog

The PACS Evolutionary Probe (PEP, Lutz et al. 2011) is a Herschel guaranteed time deep extragalactic survey (KPGT_dlutz_1) targeting six among the most popular "blank fields", ten lensing clusters of galaxies, and two z ~1 clusters at wavelengths of 100, and 160 microns. PEP includes SPIRE observations of the two z ~1 clusters at wavelengths of 250, 350, and 500 microns. SPIRE coverage of all other fields is available from the HerMES survey (Oliver et al. 2010). In addition, deep SPIRE GOODS-N data are provided by the GOODS-Herschel program (Elbaz et al. 2011).\n\nPEP used the Starfinder IDL code (Diolaiti et al. 2000a,b) to blindly extract the PACS catalogs, by means of PSF-fitting. PEP adopted the "direct" noise maps and extracted PSFs directly from the observed maps (see documentation). The released catalogs include all sources above a S/N threshold of 3 sigma, derived directly from the measured fluxes and flux uncertainties. Users should keep in mind that the error estimate does not take into account confusion noise. PEP recommends to use any flux below 0.6 mJy in the green band and below 2.0 mJy in the red band with care.

Tags: __
Organization: National Aeronautics and Space Administration
VEGA1 CRUISE MAGNETOMETER DATA

On Dec 15, 1984, the Vega spacecraft was launched to first flyby Venus at which time landers were released and then continue to a flyby of Halley. The magnetic field experiments MISCHA carried four fluxgate sensors, with three sensors mounted on a boom at the end of the solar panels and the fourth sensor mounted one meter closer. During the cruise phase, the TRASSA-1 mode of the instrument (1 vector/2.5 min) was used. The sensors were switched to the TRASSA-2 mode (1 vector/min) during the flyby which started roughly two days before the encounter. From 3 h before closest approach (CA) until 1 hour after CA, the HS-mode 1 vector/6s) and the DT-mode (1 vector/100ms) was used [DELVAETAL1991].

Tags: __
Organization: National Aeronautics and Space Administration
Airborne Multi-angle Imaging SpectroRadiometer (AirMISR) Data from the Snow and Ice 2001 Campaign

The AIRMISR_SNOW_ICE_2001 data were acquired during the Colorado snow albedo field experiment in the Yampa Valley of Colorado during February and March, 2001. This experiment focused on snow albedo and atmospheric characterization as part of a validation effort for estimating snow albedo from the Multiangle Imaging SpectroRadiometer (MISR) and the Moderate Resolution Imaging Spectroradiometer (MODIS) data. The validation site is located at 40.4N, 106.8W, just south of Steamboat Springs, Colorado. AirMISR and MODIS Airborne Simulator (MAS) data were collected on March 8, 2001. The Airborne Multi-angle Imaging SpectroRadiometer (AirMISR) is an airborne instrument for obtaining multi-angle imagery similar to that of the satellite-borne Multi-angle Imaging SpectroRadiometer (MISR) instrument, which is designed to contribute to studies of the Earth's ecology and climate. AirMISR flies on the NASA ER-2 aircraft. The Jet Propulsion Laboratory in Pasadena, California built the instrument for NASA. Unlike the satellite-borne MISR instrument, which has nine cameras oriented at various angles, AirMISR uses a single camera in a pivoting gimbal mount. A data run by the ER-2 aircraft is divided into nine segments, each with the camera positioned to a MISR look angle. The gimbal rotates between successive segments, such that each segment acquires data over the same area on the ground as the previous segment. This process is repeated until all nine angles of the target area are collected. The swath width, which varies from 11 km in the nadir to 32 km at the most oblique angle, is governed by the camera's instantaneous field-of-view of 7 meters cross-track x 6 meters along-track in the nadir view and 21 meters x 55 meters at the most oblique angle. The along-track image length at each angle is dictated by the timing required to obtain overlap imagery at all angles, and varies from about 9 km in the nadir to 26 km at the most oblique angle. Thus, the nadir image dictates the area of overlap that is obtained from all nine angles. A complete flight run takes approximately 13 minutes. The 9 camera viewing angles are: 0 degrees or nadir 26.1 degrees, fore and aft 45.6 degrees, fore and aft 60.0 degrees, fore and aft 70.5 degrees, fore and aft. For each of the camera angles, images are obtained at 4 spectral bands. The spectral bands can be used to identify vegetation and aerosols, estimate surface reflectance and for ocean color studies. The center wavelengths of the 4 spectral bands are: 443 nanometers, blue 555 nanometers, green 670 nanometers, red 865 nanometers, near-infrared. Two types of AirMISR data products are available - the Level 1 Radiometric product (L1B1) and the Level 1 Georectified radiance product (L1B2).

Tags: earth-science-infrared-wavelengths-spectral-engineering-infrared-radiance, earth-science-visible-wavelengths-spectral-engineering-visible-radiance
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 8 4215 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2021-01-01 to 2022-12-31. It is a Occultation measurement and covers the time 2021-04-17T05:29:15.399 to 2021-04-17T06:09:54.349.

Tags: __
Organization: National Aeronautics and Space Administration
Spitzer Wide-area InfraRed Extragalactic Survey ELAIS-S1 MIPS24 Single-Band Catalog

The Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), the largest Spitzer Legacy program, is a wide-area, imaging survey to trace the evolution of dusty, star-forming galaxies, evolved stellar populations, and AGN as a function of environment, from redshifts z~3 to the current epoch. SWIRE surveys 6 high-latitude fields, totaling ~50 sq. deg. in all 7 Spitzer bands: 3.6, 4.5, 5.8, and 8 microns with IRAC and 24, 70, and 160 microns with MIPS (Lonsdale et al. 2003). The SWIRE Legacy Extragalactic Source Catalogs will eventually contain in excess of 2 million IR-selected galaxies, from those dominated by the light of stellar populations detected primarily by IRAC, to starbursts, ultra-luminous infrared galaxies and AGN detected also by MIPS.\n\nThe main SWIRE catalogs for 24 micron data are the Optical-IRAC-MIPS24 bandmerged catalogs. The bandmerged catalogs require a detection in the shortest IRAC band (3.6 microns). The SWIRE project has produced single-band 24 micron catalogs to cover regions that lie outside the IRAC images, and to include sources that for some reason were not associated with a 3.6 micron detection.

Tags: __
Organization: National Aeronautics and Space Administration
Early-Type Galaxies Chandra X-Ray Point Source Catalog

This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L&lt;sub&gt;X&lt;/sub&gt;). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L&lt;sub&gt;X&lt;/sub&gt; XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L&lt;sub&gt;X&lt;/sub&gt; &gt; 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L&lt;sub&gt;GC&lt;/sub&gt;&lt;sup&gt;Alpha&lt;/sup&gt; Z&lt;sub&gt;Fe&lt;/sub&gt;&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33 +/- 0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L&lt;sub&gt;X&lt;/sub&gt; &gt; 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau&lt;sub&gt;L&lt;/sub&gt; and the duty cycle is F&lt;sub&gt;d&lt;/sub&gt;, their results imply ~ 1.5(Tau&lt;sub&gt;L&lt;/sub&gt;/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F&lt;sub&gt;d&lt;/sub&gt;&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminosities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D&lt;sub&gt;25&lt;/sub&gt; (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D&lt;sub&gt;25&lt;/sub&gt; restriction should mitigate against contamination by background AGNs. This table was created by the HEASARC in February 2009 based on the electronic versions of Table 6 from the paper which was obtained from the Astrophysical Journal web site. This is a service provided by NASA HEASARC .

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 3 OSINAC 3 RDR MTP018 V2.0

This data set contains images acquired by the OSIRIS Narrow Angle Camera during the COMET ESCORT 3 phase of the Rosetta mission at the comet 67P, covering the period from 2015-06-30T23:25:00.000 to 2015-07-28T23:24:59.000. This version V2.0 supersedes previous deliveries of the same dataset.

Tags: __
Organization: National Aeronautics and Space Administration
Deep GLIMPSE Archive

Deep GLIMPSE is the sixth in a series of large area projects to map regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). Deep GLIMPSE is a Warm Mission Spitzer Cycle 8 Exploration Science Program (PIDs 80074 and 80253) that mapped 125 degrees of longitude of the Far Side of the Galaxy. Warm Mission Spitzer has two IRAC bands, centered at approximately 3.6 and 4.5 μm. The Galactic longitudes covered by Deep GLIMPSE are l=265◦-350◦and 25◦-65◦. The latitude width is about 2.1◦. The latitude center follows the Galactic warp at a Galactocentric distance of 13 kpc to survey the Far Outer Galaxy.\n\nThe Deep GLIMPSE Archive (GLMDPA or the “Archive”) consists of point sources with less stringent selection critera than the Catalog. The information provided is in the same format as the Catalog. The Catalog is a subset of the Archive, but the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.

Tags: __
Organization: National Aeronautics and Space Administration
XMM-Newton COSMOS (XMM-COSMOS) Survey Photometric Redshift Catalog

In their paper, the authors release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. The authors demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGNlike X-ray luminosities. Preselecting the library on the bases of the source properties allowed them to reach an accuracy sigma[Delta-z/(1+Z&lt;sub&gt;spec&lt;/sub&gt;)] ~ 0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. These Chandra sources are not contained in this table but are available in the HEASARC table CCOSMPHOTZ). In addition, in this study the authors released revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg&lt;sup&gt;2&lt;/sup&gt; of COSMOS, and these are the sources listed in the present table. For 248 sources, their updated photometric redshift differs from the previous release by Delta-z &gt; 0.2. These changes are predominantly due to the inclusion of newly available deep H-band^ photometry (H&lt;sub&gt;AB&lt;/sub&gt; = 24 mag). The authors illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band. This table contains the photometric redshifts and related quantities for 1735 XMM-Newton sources over the entire 2 square degrees of the COSMOS field. Notice that in the original as-published paper no positional information was provided. The HEASARC has assumed that the source numbers used in the present catalog are in the same source numbering scheme as used by Cappelluti et al. (2009, A&amp;A, 497, 635, the XMM-Newton Wide-Field Survey in the COSMOS Field Point-like X-ray Source Catalog, available at the HEASARC as the XMMCOSMOS table) and thus obtained the positions and (position-based) names corresponding to these X-ray sources from the latter. This table was created by the HEASARC in November 2011 based on an electronic version of Table 5 from the reference paper which was obtained from the ApJ website. This is a service provided by NASA HEASARC .

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 EXT3-MTP031 RDR-STRLIGHT V1.0

This CODMAC level 4 data set contains solar stray light corrected, radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm, acquired by the OSIRIS Wide Angle Camera on the Rosetta spacecraft during the ROSETTA EXTENSION 3 mission phase, covering the period from 2016-06-28T23:25:00.000 to 2016-07-26T23:24:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V1.0 is the first version of this dataset: Lien corrected dataset after October 2018 PSA/PDS external peer review.

Tags: __
Organization: National Aeronautics and Space Administration
AirMOSS: In Situ Soil Moisture and Tree Measurements, Harvard Forest, 2012-2013

This dataset provides in situ measurements of soil temperature, moisture, conductivity, measured diameter of tree at breast height (DBH) and total height collected at the Harvard Forest, Petersham, Massachusetts, USA, during October 2012 and July - August 2013. These measurements were collected in support of the Airborne Microwave Observatory of Subcanopy and Subsurface (AirMOSS) project to validate root-zone soil measurements and carbon flux model estimates.

Tags: earth-science-ecosystems-biosphere-terrestrial-ecosystems-forests, earth-science-soils-land-surface-soil-moisture-water-content, earth-science-soils-land-surface-soil-temperature, earth-science-vegetation-biosphere-plant-characteristics, earth-science-vegetation-biosphere-vegetation-species
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0514 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 2014-12-30T12:35:25.000 to 2014-12-30T17:59:11.000.

Tags: __
Organization: National Aeronautics and Space Administration
Chandra Deep Field South 1-Megasecond Catalog

The Chandra Deep Field South (CDFS) 1-Megasecond Catalog is the source catalog obtained from a 942 kilosecond exposure, using the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-ray Observatory. Eleven individual pointings made between 1999 October and 2000 December were combined to generate the final image used for object detection. Catalog generation proceeded simultaneously using two different methods: a method of the authors&#39; own design using a modified version of the SExtractor algorithm, and a wavelet transform technique developed specifically for Chandra observations. The detection threshold was set in order to have less than 10 spurious sources, as assessed by extensive simulations. The catalog as published was subdivided into four sections: the primary list consisting of objects common to the two detection methods, two secondary lists containing sources which were detected by either the SExtractor algorithm alone or by the wavelet technique alone, and the fourth list consisting of possible diffuse or extended sources. The flux limits at the aimpoint for the soft (0.5 - 2 keV) and hard (2 - 10 keV) bands are 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg/s/cm&lt;sup&gt;2&lt;/sup&gt; and 4.5 x 10&lt;sup&gt;-16&lt;/sup&gt; erg/s/cm&lt;sup&gt;2&lt;/sup&gt;, respectively. The total number of sources is 346; out of them, 307 were detected in the 0.5 - 2 keV band, and 251 in the 2 - 10 keV band. Optical identifications are also presented for the catalogued sources. The primary optical data are R band imaging from VLT/FORS1 to a depth of R ~ 26.5 (Vega). In regions of the field not covered by the VLT/FORS1 deep imaging, the authors use R-band data obtained with the Wide Field Imager (WFI) on the ESO-MPI 2.2 m telescope, as part of the ESO Imaging Survey (EIS), which cover the entire X-ray survey. The FORS1/Chandra offsets are small, ~1 arcsecond. Coordinate cross-correlation finds 85% of the Chandra sources covered by FORS1 R to have counterparts within the 3-sigma error box (&gt;~1.5 arcseconds, depending on off-axis angle and X-ray signal-to-noise). The unidentified fraction of sources, approximately 10% - 15%, is close to the limit expected from the observed X-ray flux to R-band ratio distribution for the identified sample. This online catalog was created by the HEASARC in June 2002 based on machine-readable versions of 2, 3 and 4 of Giacconi et al. (2002) that were obtained from the CDS. This is a service provided by NASA HEASARC .

Tags: __
Organization: National Aeronautics and Space Administration
SDSS NBCKDE Catalog of Photometrically Selected Quasar Candidates

This table contains a catalog of 1,015,082 quasar candidates selected from the photometric imaging data of the Sloan Digital Sky Survey (SDSS) using a non-parametric Bayesian classification kernel density estimator (NBC-KDE). It excludes 157,075 initial candidates that were culled as known or likely contaminants. The objects are all point sources to a limiting magnitude of i = 21.3 from 8417 deg&lt;sup&gt;2&lt;/sup&gt; of imaging from SDSS Data Release 6 (DR6). This sample extends the previous catalog (Paper I: Richards et al. 2004, ApJS, 155, 257) by using the latest SDSS public release data and probing both ultraviolet (UV)-excess and high-redshift quasars. While the addition of high-redshift candidates reduces the overall efficiency (quasars:quasar candidates) of the catalog to ~80%, it is expected to contain no fewer than 850,000 bona fide quasars, which is ~8 times the number of the previous sample and ~10 times the size of the largest spectroscopic quasar catalog. Cross-matching between this photometric catalog and spectroscopic quasar catalogs from both the SDSS and 2dF survey yields 88,879 spectroscopically confirmed quasars. For judicious selection of the most robust UV-excess sources (~500,000 objects in all), the efficiency is nearly 97 - more than sufficient for detailed statistical analyses. The catalog&#39;s completeness to type 1 (broad-line) quasars is expected to be no worse than 70%, with most missing objects occurring at z &lt; 0.7 and 2.5 &lt; z &lt; 3.0. In addition to classification information, the authors provide photometric redshift estimates (typically good to Delta(z) +/- 0.3 [2-sigma]) and cross-matching with radio, X-ray, and proper-motion catalogs. Finally, the authors have considered the catalog&#39;s utility for determining the optical luminosity function of quasars and are able to confirm the flattening of the bright-end slope of the quasar luminosity function at z ~ 4 as compared to z ~ 2. Much more information on the SDSS is available at the project&#39;s web site at &lt;a href="http://www.sdss.org/"&gt;http://www.sdss.org/&lt;/a&gt;. This table was created by the HEASARC based on an electronic version of Table 1 in the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .

Tags: __
Organization: National Aeronautics and Space Administration