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Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. 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Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. 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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.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/2e2b3d39-8886-4999-901e-254ad0072e77","harvest_record_raw":"https://catalog.data.gov/harvest_record/2e2b3d39-8886-4999-901e-254ad0072e77/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-cdfsm160","keyword":["__"],"last_harvested_date":"2026-09-02T00:16:01.145544","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":0,"publisher":"NASA/IPAC Infrared Science Archive","slug":"spitzer-wide-area-infrared-extragalactic-survey-cdfs-mips-160-micron-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey CDFS MIPS 160 micron Catalog","type":"dataset"},{"_score":5.655895,"_sort":[1788308159565,5.655895,5,"9e031615-9039-463a-a4d2-83fc8630b6e7"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. 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Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2k/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_2K_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_2K_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/2K/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2k/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/wzv1-4232","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/wzv1-4232","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 2K Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/9fae87c3-8c1b-4310-8137-1f8cfecde3ed","harvest_record_raw":"https://catalog.data.gov/harvest_record/9fae87c3-8c1b-4310-8137-1f8cfecde3ed/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/wzv1-4232","keyword":["ephemeris","instrumentstatus"],"last_harvested_date":"2026-09-02T00:15:50.654145","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"SPDF","slug":"barrel-2k-ephemeris-ephm-geographic-and-magnetic-coordinates-level-2-4-s-data","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"BARREL 2K Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data","type":"dataset"},{"_score":23.933508,"_sort":[1788308150022,23.933508,1,"dc4bfa10-b95f-4b5d-85d4-5e301fb5576b"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Planetary Data System","hasEmail":"mailto:pds-operator@jpl.nasa.gov"},"description":"This data set contains derived electron and proton flux energies in MeV from the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft, which had the primary target of comet 67P/Churyumov-Gerasimenko. These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the Medium Term Plan 22 period of the ESCORT 4 mission phase.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc4-mtp022-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc4-mtp022-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P SREM 5 ESCORT 4 MTP022 V1.0"},"description":"This data set contains derived electron and proton flux energies in MeV from the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft, which had the primary target of comet 67P/Churyumov-Gerasimenko. These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the Medium Term Plan 22 period of the ESCORT 4 mission phase.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/9318bb73-d014-456b-a079-5c94f9da8fba","harvest_record_raw":"https://catalog.data.gov/harvest_record/9318bb73-d014-456b-a079-5c94f9da8fba/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc4-mtp022-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc4-mtp022-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-02T00:15:50.022673","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"Small Bodies","slug":"rosetta-orbiter-67p-srem-5-escort-4-mtp022-v1-0-2adaf","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P SREM 5 ESCORT 4 MTP022 V1.0","type":"dataset"},{"_score":13.983667,"_sort":[1788308146459,13.983667,1,"d11e7e25-4f9d-4553-b77a-c3005e7a1d53"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Planetary Data System","hasEmail":"mailto:pds-operator@jpl.nasa.gov"},"description":"The MARIE (Martian Radiation Environment Experiment), aboard the 2001 Mars Odyssey spacecraft, was launched on April 7, 2001, and arrived at Mars on October 24, 2001. Data were collected intermittently during the cruise phase, starting in late April and ending in late July. A problem with MARIE's onboard computer occurred in early August, and the instrument was turned off until early March 2002, after Odyssey 's mapping orbit had been established. Data have been collected from that time to the present without major interruption. Routine minor interruptions of up to 48 hours have occurred during the orbital phase when the instrument's data is erased from local storage (after having been downloaded). MARIE is oriented to point in the direction opposite Odyssey's velocity vector. Space radiation is for the most part isotropic, so the orientation of Odyssey is usually not critical and references to external coordinate systems are not a part of the data returned by MARIE. There is one exception to the statement that space radiation is isotropic: During the early stages of solar particle events, there can be directionality in the particle flux.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ody-m-mar-2-redr-raw-data-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ody-m-mar-2-redr-raw-data-v1.0::99.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"planetary plasma interactions"},"theme":["Planetary Science"],"title":"ODYSSEY MARS MARIE REFORMATTED RAW DATA V1.0"},"description":"The MARIE (Martian Radiation Environment Experiment), aboard the 2001 Mars Odyssey spacecraft, was launched on April 7, 2001, and arrived at Mars on October 24, 2001. Data were collected intermittently during the cruise phase, starting in late April and ending in late July. A problem with MARIE's onboard computer occurred in early August, and the instrument was turned off until early March 2002, after Odyssey 's mapping orbit had been established. Data have been collected from that time to the present without major interruption. Routine minor interruptions of up to 48 hours have occurred during the orbital phase when the instrument's data is erased from local storage (after having been downloaded). MARIE is oriented to point in the direction opposite Odyssey's velocity vector. Space radiation is for the most part isotropic, so the orientation of Odyssey is usually not critical and references to external coordinate systems are not a part of the data returned by MARIE. There is one exception to the statement that space radiation is isotropic: During the early stages of solar particle events, there can be directionality in the particle flux.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/a931209d-794c-40c2-8812-749adcb82b51","harvest_record_raw":"https://catalog.data.gov/harvest_record/a931209d-794c-40c2-8812-749adcb82b51/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ody-m-mar-2-redr-raw-data-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ody-m-mar-2-redr-raw-data-v1.0::99.0","keyword":["__"],"last_harvested_date":"2026-09-02T00:15:46.459945","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"planetary plasma interactions","slug":"odyssey-mars-marie-reformatted-raw-data-v1-0-9b8aa","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ODYSSEY MARS MARIE REFORMATTED RAW DATA V1.0","type":"dataset"},{"_score":7.7285423,"_sort":[1788308139325,7.7285423,2,"fe69d7ff-cf63-4cc6-a408-9c9dbe2b7477"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"HEASARC Help Desk","hasEmail":"mailto:andrew.ptak@nasa.gov"},"description":"The XMM-Large Scale Structure (XMM-LSS) survey, covering an area of 11.1 square degrees, contains more than 6,000 X-ray point-like sources detected with the XMM-Newton Observatory to a flux of 3 x 10<sup>-15</sup> erg/s/cm<sup>2</sup> in the 0.5-2.0 keV band. The vast majority of these sources have optical (CFHTLS: Canada France Hawaii Telescope Legacy Survey), infrared (SWIRE: Spitzer Wide-area InfraRed Extragalactic legacy survey) InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS), near-infrared (UKIDSS: UKIRT Infrared Deep Sky Survey) and/or ultraviolet (GALEX: Galaxy Evolution Explorer) counterparts. The authors wished to investigate the environmental properties of the different types of the XMM-LSS X-ray sources by defining their environment using the i'-band CFHTLS W1 catalog of optical galaxies to a magnitude limit of 23.5 magnitudes. They have classified 4,435 X-ray selected sources on the basis of their spectra, spectral energy distributions (SEDs), and X-ray luminosities, and estimated their photometric redshifts, which have a 4-11 band photometry with an accuracy of sigma[Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.076, with 22.6% outliers for i' < 26 mag. The authors estimated the local overdensities of 777 X-ray sources that have spectro-z or photo-z calculated by using more than seven bands (accuracy of sigma[(Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.061, with 13.8% outliers) within the volume-limited region defined by 0.1 <= z <= 0.85 and -23.5 < M_i'_ < -20. Although X-ray sources may be found in variety of environments, a high fraction (~55-60%), as verified by comparing with the random expectations, reside in overdense regions. The galaxy overdensities within which X-ray sources reside show a positive recent redshift evolution (at least for the range studied; z <~ 0.85). The authors also find that X-ray selected galaxies, when compared to AGN, inhabit significantly higher galaxy overdensities, although their spatial extent appear to be smaller than that of AGN. Hard AGN (harness ratios HR >= -0.2) are located in more overdense regions than soft AGN (HR < -0.2), which is clearly seen in both redshift ranges, although it appears to be stronger in the higher redshift range (0.55 < z < 0.85). Furthermore, the galaxy overdensities (with delta > 1.5, where delta is defined in equation (3) of the reference paper) within which soft AGN are embedded appear to evolve more rapidly compared to the corresponding overdensities around hard AGN. This table contains the spectroscopic and/or photometric redshifts for 4,206 X-ray selected sources in the XMM-LSS field which have optical counterparts and have been classified by the authors. This table was created by the HEASARC in September 2013 based on <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/557/A81\">CDS Catalog J/A+A/557/A81</a> file table2.dat This is a service provided by NASA HEASARC .","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlssclas.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlssclas&","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"ivo://nasa.heasarc/xmmlssclas","keyword":["__"],"landingPage":"ivo://nasa.heasarc/xmmlssclas","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"High Energy Astrophysics Science Archive Research Center"},"theme":["Astrophysics"],"title":"XMM-Newton Large-Scale Structure Optical Counterparts and Redshifts"},"description":"The XMM-Large Scale Structure (XMM-LSS) survey, covering an area of 11.1 square degrees, contains more than 6,000 X-ray point-like sources detected with the XMM-Newton Observatory to a flux of 3 x 10<sup>-15</sup> erg/s/cm<sup>2</sup> in the 0.5-2.0 keV band. The vast majority of these sources have optical (CFHTLS: Canada France Hawaii Telescope Legacy Survey), infrared (SWIRE: Spitzer Wide-area InfraRed Extragalactic legacy survey) InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS), near-infrared (UKIDSS: UKIRT Infrared Deep Sky Survey) and/or ultraviolet (GALEX: Galaxy Evolution Explorer) counterparts. The authors wished to investigate the environmental properties of the different types of the XMM-LSS X-ray sources by defining their environment using the i'-band CFHTLS W1 catalog of optical galaxies to a magnitude limit of 23.5 magnitudes. They have classified 4,435 X-ray selected sources on the basis of their spectra, spectral energy distributions (SEDs), and X-ray luminosities, and estimated their photometric redshifts, which have a 4-11 band photometry with an accuracy of sigma[Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.076, with 22.6% outliers for i' < 26 mag. The authors estimated the local overdensities of 777 X-ray sources that have spectro-z or photo-z calculated by using more than seven bands (accuracy of sigma[(Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.061, with 13.8% outliers) within the volume-limited region defined by 0.1 <= z <= 0.85 and -23.5 < M_i'_ < -20. Although X-ray sources may be found in variety of environments, a high fraction (~55-60%), as verified by comparing with the random expectations, reside in overdense regions. The galaxy overdensities within which X-ray sources reside show a positive recent redshift evolution (at least for the range studied; z <~ 0.85). The authors also find that X-ray selected galaxies, when compared to AGN, inhabit significantly higher galaxy overdensities, although their spatial extent appear to be smaller than that of AGN. Hard AGN (harness ratios HR >= -0.2) are located in more overdense regions than soft AGN (HR < -0.2), which is clearly seen in both redshift ranges, although it appears to be stronger in the higher redshift range (0.55 < z < 0.85). Furthermore, the galaxy overdensities (with delta > 1.5, where delta is defined in equation (3) of the reference paper) within which soft AGN are embedded appear to evolve more rapidly compared to the corresponding overdensities around hard AGN. This table contains the spectroscopic and/or photometric redshifts for 4,206 X-ray selected sources in the XMM-LSS field which have optical counterparts and have been classified by the authors. This table was created by the HEASARC in September 2013 based on <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/557/A81\">CDS Catalog J/A+A/557/A81</a> file table2.dat This is a service provided by NASA HEASARC .","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/21774b2d-5b9a-436e-9ead-cccf494732fc","harvest_record_raw":"https://catalog.data.gov/harvest_record/21774b2d-5b9a-436e-9ead-cccf494732fc/raw","has_download":true,"has_spatial":false,"identifier":"ivo://nasa.heasarc/xmmlssclas","keyword":["__"],"last_harvested_date":"2026-09-02T00:15:39.325103","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"High Energy Astrophysics Science Archive Research Center","slug":"xmm-newton-large-scale-structure-optical-counterparts-and-redshifts","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"XMM-Newton Large-Scale Structure Optical Counterparts and Redshifts","type":"dataset"},{"_score":5.4992447,"_sort":[1788308129754,5.4992447,4,"6031b78a-712b-4b2e-86a8-674778c3f1be"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2m/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_2M_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_2M_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/2M/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2m/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/ve82-v240","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/ve82-v240","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 2M Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/d716f8dc-7b73-4923-8ebb-831a382e961b","harvest_record_raw":"https://catalog.data.gov/harvest_record/d716f8dc-7b73-4923-8ebb-831a382e961b/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/ve82-v240","keyword":["ephemeris","instrumentstatus"],"last_harvested_date":"2026-09-02T00:15:29.754215","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":4,"publisher":"SPDF","slug":"barrel-2m-ephemeris-ephm-geographic-and-magnetic-coordinates-level-2-4-s-data","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"BARREL 2M Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data","type":"dataset"},{"_score":7.7285423,"_sort":[1788308113454,7.7285423,2,"530800b7-71e2-4419-8a74-400857dbc9c4"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"HEASARC Help Desk","hasEmail":"mailto:andrew.ptak@nasa.gov"},"description":"The authors studied the X-ray properties of the young (~1-8M yr) open cluster around the hot (O8 III) star Lambda Ori and compared them with those of the similarly-aged Sigma Ori cluster in order to investigate the possible effects of the different ambient environments. They analyzed an XMM-Newton observation of the cluster using EPIC imaging and low-resolution spectral data. They studied the variability of the detected sources, and performed a spectral analysis of the brightest sources in the field using multi-temperature models. The authors detected 167 X-ray sources above a 5-sigma detection threshold the properties of which are listed in this table, of which 58 are identified with known cluster members and candidates, from massive stars down to low-mass stars with spectral types of ~ M5.5. Another 23 sources were identified with new possible photometric candidates. Late-type stars have a median log L<sub>X</sub>/L<sub>bol</sub> ~ -3.3, close to the saturation limit. Variability was observed in ~ 35% of late-type members or candidates, including six flaring sources. The emission from the central hot star Lambda Ori is dominated by plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with a wind origin. The coronae of late-type stars can be described by two plasma components with temperatures T<sub>1</sub> ~ 0.3-0.8 keV and T<sub>2</sub> ~ 0.8-3 keV, and subsolar abundances Z ~ 0.1-0.3 Z<sub>sun</sub>, similar to what is found in other star-forming regions and associations. No significant difference was observed between stars with and without circumstellar discs, although the smallness of the sample of stars with discs and accretion does not definitive conclusions to be drawn. The authors concluded that the X-ray properties of Lambda Ori late-type stars are comparable to those of the coeval Sigma Ori cluster, suggesting that stellar activity in Lambda Ori has not been significantly affected by the different ambient environment. The lambda Ori cluster was observed by XMM-Newton from 20:46 UT on September 28, 2006 to 12:23 UT on September 29, 2006 (Obs. ID 0402050101), for a total duration of 56ks, using both the EPIC MOS and PN cameras and the RGS instruments. The EPIC cameras were operated in full frame mode with the thick filter. This table was created by the HEASARC in November 2011 based on <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A150\">CDS Catalog J/A+A/530/A150</a> files tablea1.dat ('X-ray sources detected in the Lambda Ori Cluster'), table1,dat ('X-ray and optical properties of sources identified with known cluster members and candidates') and table2.dat ('X-ray sources identified with possible new cluster candidates'). It does not include the objects listed in tablea2.dat ('3-sigma upper limits and optical properties of undetected cluster members and candidates'). This is a service provided by NASA HEASARC .","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/W3Browse/all/lamorixmm.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=lamorixmm&","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"ivo://nasa.heasarc/lamorixmm","keyword":["__"],"landingPage":"ivo://nasa.heasarc/lamorixmm","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"High Energy Astrophysics Science Archive Research Center"},"theme":["Astrophysics"],"title":"Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog"},"description":"The authors studied the X-ray properties of the young (~1-8M yr) open cluster around the hot (O8 III) star Lambda Ori and compared them with those of the similarly-aged Sigma Ori cluster in order to investigate the possible effects of the different ambient environments. They analyzed an XMM-Newton observation of the cluster using EPIC imaging and low-resolution spectral data. They studied the variability of the detected sources, and performed a spectral analysis of the brightest sources in the field using multi-temperature models. The authors detected 167 X-ray sources above a 5-sigma detection threshold the properties of which are listed in this table, of which 58 are identified with known cluster members and candidates, from massive stars down to low-mass stars with spectral types of ~ M5.5. Another 23 sources were identified with new possible photometric candidates. Late-type stars have a median log L<sub>X</sub>/L<sub>bol</sub> ~ -3.3, close to the saturation limit. Variability was observed in ~ 35% of late-type members or candidates, including six flaring sources. The emission from the central hot star Lambda Ori is dominated by plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with a wind origin. The coronae of late-type stars can be described by two plasma components with temperatures T<sub>1</sub> ~ 0.3-0.8 keV and T<sub>2</sub> ~ 0.8-3 keV, and subsolar abundances Z ~ 0.1-0.3 Z<sub>sun</sub>, similar to what is found in other star-forming regions and associations. No significant difference was observed between stars with and without circumstellar discs, although the smallness of the sample of stars with discs and accretion does not definitive conclusions to be drawn. The authors concluded that the X-ray properties of Lambda Ori late-type stars are comparable to those of the coeval Sigma Ori cluster, suggesting that stellar activity in Lambda Ori has not been significantly affected by the different ambient environment. The lambda Ori cluster was observed by XMM-Newton from 20:46 UT on September 28, 2006 to 12:23 UT on September 29, 2006 (Obs. ID 0402050101), for a total duration of 56ks, using both the EPIC MOS and PN cameras and the RGS instruments. The EPIC cameras were operated in full frame mode with the thick filter. This table was created by the HEASARC in November 2011 based on <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A150\">CDS Catalog J/A+A/530/A150</a> files tablea1.dat ('X-ray sources detected in the Lambda Ori Cluster'), table1,dat ('X-ray and optical properties of sources identified with known cluster members and candidates') and table2.dat ('X-ray sources identified with possible new cluster candidates'). It does not include the objects listed in tablea2.dat ('3-sigma upper limits and optical properties of undetected cluster members and candidates'). This is a service provided by NASA HEASARC .","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/c320f892-44a6-437c-a420-0fcd0417316f","harvest_record_raw":"https://catalog.data.gov/harvest_record/c320f892-44a6-437c-a420-0fcd0417316f/raw","has_download":true,"has_spatial":false,"identifier":"ivo://nasa.heasarc/lamorixmm","keyword":["__"],"last_harvested_date":"2026-09-02T00:15:13.454293","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"High Energy Astrophysics Science Archive Research Center","slug":"lambda-orionis-cluster-xmm-newton-x-ray-point-source-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog","type":"dataset"},{"_score":5.3967113,"_sort":[1788308112514,5.3967113,2,"59565f0f-6da3-44ad-91eb-871545b105bf"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2p/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_2P_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_2P_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/2P/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/2p/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/rncw-7m94","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/rncw-7m94","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 2P Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/d92f2efd-dbf9-4b58-9863-232225708659","harvest_record_raw":"https://catalog.data.gov/harvest_record/d92f2efd-dbf9-4b58-9863-232225708659/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/rncw-7m94","keyword":["ephemeris","instrumentstatus"],"last_harvested_date":"2026-09-02T00:15:12.514243","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"SPDF","slug":"barrel-2p-ephemeris-ephm-geographic-and-magnetic-coordinates-level-2-4-s-data","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"BARREL 2P Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data","type":"dataset"},{"_score":5.3967113,"_sort":[1788308107699,5.3967113,2,"e41c3164-6e5f-4c65-b4bb-6996a6c72137"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. 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A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. 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A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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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.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/60f684bf-7bc7-4962-af13-314aaf408ca5","harvest_record_raw":"https://catalog.data.gov/harvest_record/60f684bf-7bc7-4962-af13-314aaf408ca5/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-cdfs","keyword":["__"],"last_harvested_date":"2026-09-02T00:13:45.209752","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"NASA/IPAC Infrared Science Archive","slug":"spitzer-wide-area-infrared-extragalactic-survey-cdfs-optical-irac-mips24-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey CDFS Optical-IRAC-MIPS24 Catalog","type":"dataset"},{"_score":13.948866,"_sort":[1788308023185,13.948866,1,"cc7ff9d6-c6b9-4209-be34-fae6c476a0b0"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Planetary Data System","hasEmail":"mailto:pds-operator@jpl.nasa.gov"},"description":"This volume contains Experiment Data acquired by GIADA during 'Mars swing-by' phase. More in detail it refers to the data provided during the following in-flight tests: 'Active Payload Checkout n. 4' (PC4) held on 24/25-11-2006 and 04-12-2006; 'Passive Payload Checkout n. 5' (PC5) held on 20/21-05-2007. It also contains documentation which describes the GIADA experiment. The data reported in this data set have been converted from ADC counts to engineering values. The quality of the Housekeeping and Calibration data is good. Scientific data are due to noise, as no grain event is expected during this mission phase. These data must be only considered to evaluate GIADA behaviour and not as real scientific data. Data reported by GDS and IS are due to noise as no dust event is expected during this mission phase. MBS frequency changes, once normalised for frequency vs. temperature dependence, if present, are due to deposition of contaminants existing in the S/C environment. 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It also contains documentation which describes the GIADA experiment. The data reported in this data set have been converted from ADC counts to engineering values. The quality of the Housekeeping and Calibration data is good. Scientific data are due to noise, as no grain event is expected during this mission phase. These data must be only considered to evaluate GIADA behaviour and not as real scientific data. Data reported by GDS and IS are due to noise as no dust event is expected during this mission phase. MBS frequency changes, once normalised for frequency vs. temperature dependence, if present, are due to deposition of contaminants existing in the S/C environment. Housekeeping and Calibration data from all GIADA sub-systems are useful to evaluate instrument health and behaviour when compared with similar data acquired during other mission phases.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/03825549-9c48-471e-b835-8d1b01c37349","harvest_record_raw":"https://catalog.data.gov/harvest_record/03825549-9c48-471e-b835-8d1b01c37349/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-mars-marsswingby-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-mars-marsswingby-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-02T00:13:43.185099","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"Small Bodies","slug":"rosetta-orbiter-check-giada-2-mars-marsswingby-v1-0-4be6a","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 MARS MARSSWINGBY V1.0","type":"dataset"},{"_score":13.559139,"_sort":[1788308022781,13.559139,1,"327ec5b4-873c-4920-a2ac-f1e243f2d79a"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"IRSA Support","hasEmail":"mailto:irsasupport@ipac.caltech.edu"},"description":"COSMOS is an astronomical survey designed to probe the formation and evolution of galaxies as a function of cosmic time (redshift) and large scale structural environment. The survey covers a 2 square degree equatorial field with imaging by most of the major space-based telescopes (Hubble, Spitzer, GALEX, XMM, Chandra) and a number of large ground based telescopes (Subaru, VLA, ESO-VLT, UKIRT, NOAO, CFHT, and others). Over 2 million galaxies are detected, spanning 75% of the age of the universe.\\n\\nThis catalog was created using u*-band priors and the EM-algorithm. Appropriate references for a description of the method are: Guillaume, M. et al. 2006, Proceedings of the SPIE, Volume 6064, pp. 332-341. This is the current reference, and contains all the basics of the method and algorithm. A more specific reference for this catalog is Zamojski et al. (2008).\\n\\nThe algorithm was run on the four NUV and the four FUV GALEX images covering the COSMOS field. It was run on the \"-int\" images (intensity maps) obtained as a product of the GALEX pipeline processing, version 1.61. The u*-band mosaic image and SExtractor catalog used as priors in this run were generously provided by Henry McCracken (IAP) and are based on CFHT-u* observations of the COSMOS field.","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/SCS?table=galex_emphot_v3&","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/data/COSMOS/gator_docs/cosmos_galex_colDescriptions.html","format":"HTML","mediaType":"text/html"}],"identifier":"ivo://irsa.ipac/cosmos/catalog/cosmos-galex","keyword":["__"],"landingPage":"ivo://irsa.ipac/cosmos/catalog/cosmos-galex","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"NASA/IPAC Infrared Science Archive"},"theme":["Astrophysics"],"title":"GALEX/COSMOS Prior-based Photometry Catalog"},"description":"COSMOS is an astronomical survey designed to probe the formation and evolution of galaxies as a function of cosmic time (redshift) and large scale structural environment. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4a/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_4A_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_4A_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/4A/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4a/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/an8a-3b17","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/an8a-3b17","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 4A Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. 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BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N >= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 µJy (µJy) beam<sup>-1</sup> in the central 1 deg<sup>2</sup>, and of 15 uJy in the 2 deg<sup>2</sup> field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and < 55 mas, respectively. This table was created by the HEASARC in September 2007 based on the electronic version of Table 3 from the reference paper which was obtained from the ApJ web site. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4b/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_4B_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_4B_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/4B/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4b/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/501n-7c49","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/501n-7c49","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 4B Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4c/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_4C_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_4C_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/4C/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4c/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/xm4d-w960","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/xm4d-w960","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 4C Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.\n\nThe current release of all BARREL CDF data products are Version 10 files.\n\nBARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.\n\nBARREL Data Usage Policy\n\nBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/81d89edc-8c57-4b01-911c-87db61633097","harvest_record_raw":"https://catalog.data.gov/harvest_record/81d89edc-8c57-4b01-911c-87db61633097/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/xm4d-w960","keyword":["ephemeris","instrumentstatus"],"last_harvested_date":"2026-09-02T00:13:20.611728","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":3,"publisher":"SPDF","slug":"barrel-4c-ephemeris-ephm-geographic-and-magnetic-coordinates-level-2-4-s-data","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"BARREL 4C Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data","type":"dataset"},{"_score":24.592596,"_sort":[1788307995962,24.592596,2,"87ce5b98-dbe0-4540-a050-d06304c1b1c5"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Planetary Data System","hasEmail":"mailto:pds-operator@jpl.nasa.gov"},"description":"This data set contains derived electron and proton flux energies in MeV from the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft. 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These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the CRUISE 1 mission phase.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/3248ccd0-895c-4642-9233-0fcf0d7a66a4","harvest_record_raw":"https://catalog.data.gov/harvest_record/3248ccd0-895c-4642-9233-0fcf0d7a66a4/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-cr1-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-cr1-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-02T00:13:15.962578","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"Small Bodies","slug":"rosetta-orbiter-x-srem-5-cruise-1-v1-0-6b26d","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER X SREM 5 CRUISE 1 V1.0","type":"dataset"},{"_score":5.500475,"_sort":[1788307992010,5.500475,2,"9a4feb79-9d3f-4ddb-9734-aeb2676af452"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"HEASARC Help Desk","hasEmail":"mailto:andrew.ptak@nasa.gov"},"description":"The authors monitored the Cassiopeia dwarf galaxy (IC 10) in a series of 10 Chandra ACIS-S observations to capture its variable and transient X-ray source population, which is expected to be dominated by High Mass X-ray Binaries (HMXBs). They present a sample of 21 X-ray sources that are variable between observations at the 3-sigma level, from a catalog of 110 unique point sources (the HEASARC notes that there are actually 111 sources in the CDS version of the catalog from which this HEASARC table originates). The authors find four transients (flux variability ratio greater than 10) and a further eight objects with ratios >5. The observations span the years 2003-2010 and reach a limiting luminosity of >10<sup>35</sup> erg/s, providing sensitivity to X-ray binaries in IC 10 as well as flare stars in the foreground Milky Way. The nature of the variable sources is investigated from light curves, X-ray spectra, energy quantiles, and optical counterparts. The purpose of this study is to discover the composition of the X-ray binary population in a young starburst environment. IC 10 provides a sharp contrast in stellar population age (<10 million years) when compared to the Magellanic Clouds (40-200 Myr) where most of the known HMXBs reside. The authors find 10 strong HMXB candidates, 2 probable background active galactic nuclei, 4 foreground flare-stars or active binaries, and 5 not yet classifiable sources. Complete classification of the sample requires optical spectroscopy for radial velocity analysis and deeper X-ray observations to obtain higher S/N spectra and search for pulsations. A catalog (contained in this HEASARC table) has been created and supporting data sets (the data used to create the light curves shown in Figures 3, 4 and 5 in the reference paper) are available at <a href=\"http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/\">http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/</a>. A monitoring series of 7x15 ks Chandra/ACIS observations, spaced at roughly six-week intervals was obtained during 2009-2010. A pair of very deep ACIS-S3 observations (2x45ks) made in 2006 November provided a reference data set for improved source positions and spectral information. The original Wang+ (2005, MNRAS, 362, 1065) Chandra (ACIS-S3) observation of 30 ks made in 2003 was also included in this analysis. The complete listing of 10 Chandra observation identifiers (ObsIDs) comprising the data set is summarized in Table 1 of the reference paper, also shown here: <pre> MJD |Date |ObsID|Flag|Exp.|RA(J2000)Dec(J2000)|Roll|Num. Sources ks hh mm ss dd mm ss deg. 52710.7|2003 Mar 12 |03953|a |28.9|00 20 25 +59 16 55|339.27|31 54041.8|2006 Nov 2 |07082| |40.1|00 20 04 +59 16 45|223.70|48 54044.2|2006 Nov 5 |08458| |40.5|00 20 04 +59 16 45|223.70|41 55140.7|2009 Nov 5 |11080| |14.6|00 20 17 +59 17 56|226.53|19 55190.2|2009 Dec 25 |11081| | 8.1|00 20 19 +59 18 02|286.15|24 55238.5|2010 Feb 11 |11082| |14.7|00 20 23 +59 17 10|320.56|24 55290.6|2010 Apr 4 |11083| |14.7|00 20 34 +59 19 01| 10.32|25 55337.8|2010 May 21 |11084| |14.2|00 20 25 +59 20 16| 67.89|27 55397.5|2010 Jul 20 |11085| |14.5|00 20 11 +59 19 13|121.25|22 55444.6|2010 Sep 5 |11086| |14.7|00 20 15 +59 18 11|157.71|27 |2006 Nov 2-5 |57082|b |80.6|00 20 04 +59 16 45|223.70|63 </pre> Flag values as follows: <pre> a = ObsID 03953 used about half of the CCD area in subarray mode. b = Merged 2006 data set referred to as ObsID 57082 consists of the nearly contiguous ObsIDs 07082 and 08458, which had identical pointings. </pre> Roll is the spacecraft roll angle, and Num. Sources is the number of unique point sources detected in each observation after combining wavdetect lists from the soft (S: 0.3-1.5 keV), broad (B: 0.3-8 keV) and hard (H: 2.5-8 keV) energy bands. This table was created by the HEASARC in November 2017 based upon the <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/836/50\">CDS Catalog J/ApJ/836/50</a> file table2.dat. This is a service provided by NASA HEASARC .","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/W3Browse/all/ic10cxo.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=ic10cxo&","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"ivo://nasa.heasarc/ic10cxo","keyword":["__"],"landingPage":"ivo://nasa.heasarc/ic10cxo","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"High Energy Astrophysics Science Archive Research Center"},"theme":["Astrophysics"],"title":"IC 10 Chandra X-ray Point Source Catalog"},"description":"The authors monitored the Cassiopeia dwarf galaxy (IC 10) in a series of 10 Chandra ACIS-S observations to capture its variable and transient X-ray source population, which is expected to be dominated by High Mass X-ray Binaries (HMXBs). 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IC 10 provides a sharp contrast in stellar population age (<10 million years) when compared to the Magellanic Clouds (40-200 Myr) where most of the known HMXBs reside. The authors find 10 strong HMXB candidates, 2 probable background active galactic nuclei, 4 foreground flare-stars or active binaries, and 5 not yet classifiable sources. Complete classification of the sample requires optical spectroscopy for radial velocity analysis and deeper X-ray observations to obtain higher S/N spectra and search for pulsations. A catalog (contained in this HEASARC table) has been created and supporting data sets (the data used to create the light curves shown in Figures 3, 4 and 5 in the reference paper) are available at <a href=\"http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/\">http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/</a>. A monitoring series of 7x15 ks Chandra/ACIS observations, spaced at roughly six-week intervals was obtained during 2009-2010. A pair of very deep ACIS-S3 observations (2x45ks) made in 2006 November provided a reference data set for improved source positions and spectral information. The original Wang+ (2005, MNRAS, 362, 1065) Chandra (ACIS-S3) observation of 30 ks made in 2003 was also included in this analysis. The complete listing of 10 Chandra observation identifiers (ObsIDs) comprising the data set is summarized in Table 1 of the reference paper, also shown here: <pre> MJD |Date |ObsID|Flag|Exp.|RA(J2000)Dec(J2000)|Roll|Num. Sources ks hh mm ss dd mm ss deg. 52710.7|2003 Mar 12 |03953|a |28.9|00 20 25 +59 16 55|339.27|31 54041.8|2006 Nov 2 |07082| |40.1|00 20 04 +59 16 45|223.70|48 54044.2|2006 Nov 5 |08458| |40.5|00 20 04 +59 16 45|223.70|41 55140.7|2009 Nov 5 |11080| |14.6|00 20 17 +59 17 56|226.53|19 55190.2|2009 Dec 25 |11081| | 8.1|00 20 19 +59 18 02|286.15|24 55238.5|2010 Feb 11 |11082| |14.7|00 20 23 +59 17 10|320.56|24 55290.6|2010 Apr 4 |11083| |14.7|00 20 34 +59 19 01| 10.32|25 55337.8|2010 May 21 |11084| |14.2|00 20 25 +59 20 16| 67.89|27 55397.5|2010 Jul 20 |11085| |14.5|00 20 11 +59 19 13|121.25|22 55444.6|2010 Sep 5 |11086| |14.7|00 20 15 +59 18 11|157.71|27 |2006 Nov 2-5 |57082|b |80.6|00 20 04 +59 16 45|223.70|63 </pre> Flag values as follows: <pre> a = ObsID 03953 used about half of the CCD area in subarray mode. b = Merged 2006 data set referred to as ObsID 57082 consists of the nearly contiguous ObsIDs 07082 and 08458, which had identical pointings. </pre> Roll is the spacecraft roll angle, and Num. Sources is the number of unique point sources detected in each observation after combining wavdetect lists from the soft (S: 0.3-1.5 keV), broad (B: 0.3-8 keV) and hard (H: 2.5-8 keV) energy bands. This table was created by the HEASARC in November 2017 based upon the <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/836/50\">CDS Catalog J/ApJ/836/50</a> file table2.dat. This is a service provided by NASA HEASARC .","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/e3029a16-d3df-41a9-8f03-2d5a0e034bd2","harvest_record_raw":"https://catalog.data.gov/harvest_record/e3029a16-d3df-41a9-8f03-2d5a0e034bd2/raw","has_download":true,"has_spatial":false,"identifier":"ivo://nasa.heasarc/ic10cxo","keyword":["__"],"last_harvested_date":"2026-09-02T00:13:12.010402","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"High Energy Astrophysics Science Archive Research Center","slug":"ic-10-chandra-x-ray-point-source-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"IC 10 Chandra X-ray Point Source Catalog","type":"dataset"},{"_score":25.133083,"_sort":[1788307986280,25.133083,2,"54a1b5cb-7593-48d4-b330-8fac0d37d49c"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Planetary Data System","hasEmail":"mailto:pds-operator@jpl.nasa.gov"},"description":"This data set contains derived electron and proton flux energies in MeV from the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft. These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the EARTH 1 mission phase.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-ear1-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-ear1-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER X SREM 5 EARTH 1 V1.0"},"description":"This data set contains derived electron and proton flux energies in MeV from the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft. These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the EARTH 1 mission phase.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/5a19c1e2-5998-4dc8-accb-4ced8aefa618","harvest_record_raw":"https://catalog.data.gov/harvest_record/5a19c1e2-5998-4dc8-accb-4ced8aefa618/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-ear1-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-ear1-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-02T00:13:06.280338","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"Small Bodies","slug":"rosetta-orbiter-x-srem-5-earth-1-v1-0-846be","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER X SREM 5 EARTH 1 V1.0","type":"dataset"},{"_score":5.500475,"_sort":[1788307985368,5.500475,1,"9776c999-8aa0-469c-908a-140dc874fc46"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4e/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://relativisticballoons.blogspot.com","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://alexahalford.weebly.com/barrel-2013---2016.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf","format":"PDF","mediaType":"application/pdf"},{"@type":"dcat:Distribution","downloadURL":"https://barrel.rmillan.host.dartmouth.edu/index.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=BAR_4E_L2_EPHM&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/pub/data/barrel/Campaigns_and_launches.txt","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://doi.org/10.1007/s11214-013-9971-z","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://github.com/PRBEM/IRBEM","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/BARREL_4E_Ephemeris_L2_PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/BARREL/4E/Ephemeris/L2/PT4S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://prbem.github.io/IRBEM/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/barrel/l2/4e/ephem/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.nasa.gov/mission-pages/rbsp/barrel/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/j5ay-np19","keyword":["ephemeris","instrumentstatus"],"landingPage":"https://doi.org/10.48322/j5ay-np19","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"BARREL 4E Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data"},"description":"Geographic and Magnetic Coordinates: The ephemeris data products, which include the balloon epoch time, latitude, longitude, and altitude, are each returned from the payload once every 4s. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI.\n\nThe BARREL PI can be contacted at: Robyn.Millan@dartmouth.edu.\n\nAn online copy of the BARREL Data Usage Policy document can be found at: https://barrel.rmillan.host.dartmouth.edu/documents/data.use.policy.pdf.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/dbfabd96-7ca1-4ae0-a8d3-6096216b51de","harvest_record_raw":"https://catalog.data.gov/harvest_record/dbfabd96-7ca1-4ae0-a8d3-6096216b51de/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/j5ay-np19","keyword":["ephemeris","instrumentstatus"],"last_harvested_date":"2026-09-02T00:13:05.368123","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"SPDF","slug":"barrel-4e-ephemeris-ephm-geographic-and-magnetic-coordinates-level-2-4-s-data","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"BARREL 4E Ephemeris (EPHM) Geographic and Magnetic Coordinates, Level 2, 4 s Data","type":"dataset"},{"_score":11.839088,"_sort":[1788307980971,11.839088,2,"be4eb2da-4fa0-4e5d-bcc2-ca9bad80bc3b"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"IRSA Support","hasEmail":"mailto:irsasupport@ipac.caltech.edu"},"description":"COSMOS is an astronomical survey designed to probe the formation and evolution of galaxies as a function of cosmic time (redshift) and large scale structural environment. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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Geographic coordinates are obtained from an onboard Global Positioning System, GPS, unit. Magnetic coordinates are derived by using the International Radiation Belt Environment Modeling, IRBEM, FORTRAN library.\n\nThe BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. 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For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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This will help you ensure that your science results are valid.\n\n* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.\n* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually.\n* If BARREL team members are not part of the author list, then users should Credit/Acknowledge the BARREL team as follows: We acknowledge the BARREL team (PI: Robyn Millan) for use of BARREL data.\n* Users are also requested to provide the PI with a copy of each manuscript that uses BARREL data upon submission of that manuscript for consideration of publication. 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BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.\n\nThe initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.\n\nLater campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.\n\nSumming over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: \"By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count.\" Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.\n\nThe information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. 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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.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/de18d2da-9550-4706-95de-c83a28ccba5d","harvest_record_raw":"https://catalog.data.gov/harvest_record/de18d2da-9550-4706-95de-c83a28ccba5d/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-lhm160","keyword":["__"],"last_harvested_date":"2026-09-02T00:12:35.734647","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":0,"publisher":"NASA/IPAC Infrared Science Archive","slug":"spitzer-wide-area-infrared-extragalactic-survey-lockman-hole-mips-160-micron-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey Lockman Hole MIPS 160 micron Catalog","type":"dataset"},{"_score":12.388157,"_sort":[1788307945953,12.388157,0,"fe3b391f-4f9b-4099-a4da-34c9c25f8b44"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III). 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The XMM-LSS field (centered at RA (J2000) = 02<sup>h</sup> 24<sup>m</sup> 00.27<sup>s</sup>, Dec (J2000) = -04<sup>o</sup> 09' 47.6") is currently being followed up using observations across a wide range of wavelengths, and in their paper the authors present the observational results of a low frequency radio survey of the XMM-LSS field using the Very Large Array at 74 and 325 MHz. This survey will map out the locations of the extragalactic radio sources relative to the large scale structure as traced by the X-ray emission. This is of particular interest because radio galaxies and radio-loud AGN show strong and complex interactions with their small and larger scale environment, and different classes of radio galaxies are suggested to lie at different places with respect to the large scale structure. For the phase calibration of the radio data, the authors used standard self-calibration at 325 MHz and field-base calibration at 74 MHz. Polyhedron-based imaging as well as mosaicking methods were used at both frequencies. At 74 MHz, the resolution was 30 arcseconds, the median 5-sigma sensitivity was ~ 162 mJy/beam and 666 sources were detected over an area of 132 square degrees. At 325 MHz, the resolution was 6.7 arcseconds, the median 5-sigma sensitivity was 4 mJy/beam, and 847 sources were detected over an area of 15.3 square degrees. At 325 MHz, a region of diffuse radio emission which is a cluster halo or relic candidate was detected. The observations were conducted using the VLA in July 2003 in the A-configuration (most extended) and in June 2002 in the B-configuration. This table contains the VLA 325-MHz source list, comprising 605 single sources and 615 components of 237 multiple sources, for a total of 1220 entries. (Notice that, in Section 4.1 of the reference paper, somewhat different numbers are given, i.e., the authors quote 621 single sources and 226 multiple sources). 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The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. 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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). 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The ~ 17' x 17' field of view fully encompasses three cluster core radii and almost twice the half-mass radius. They detected 180 sources to a limiting flux of ~ 4.3 x10 <sup>-16</sup> erg/cm<sup>2</sup>/s (L<sub>x</sub> = 1.2 x 10<sup>30</sup> erg/s at the 4.9 kpc distance to the cluster). After accounting for the number of active galactic nuclei and possible foreground stars among the detected X-ray sources, they estimate that 45-70 of the sources are cluster members. Four of the X-ray sources have previously been identified as accreting compact binaries in the cluster - three cataclysmic variables (CVs) and one quiescent neutron star. Correlating the Chandra positions with known variable stars yields 8 matches, of which 5 are probable cluster members that are likely to be binary stars with active coronae. Extrapolating these optical identifications to the remaining unidentified X-ray source population, the authors estimate that 20 - 35 of the sources are CVs and a similar number are active binaries. This likely represents most of the CVs in the cluster, but only a small fraction of all the active binaries. The authors place a 2-sigma upper limit of L<sub>x</sub> < 3 x 10<sup>30</sup> erg/s on the integrated luminosity of any additional faint, unresolved population of sources in the core of the cluster. In their paper, they explore the significance of these findings in the context of primordial versus dynamical channels for CV formation. They note that the number of CVs per unit mass in Omega Cen is at least 2 - 3 times lower than in the field, suggesting that primordial binaries that would otherwise lead to CVs are being destroyed in the cluster environment. The authors obtained 2 exposures of Omega Cen using the imaging array of the Advanced CCD Imaging Spectrometer (ACIS-I) on 2000 January 24 - 25, in "very faint" (VF) mode. The total exposure time was 72.4 ks. The authors determined source counts using 95% encircled energy radii as determined from model PSFs, derived using the CIAO tool mkpsf at an intermediate energy of ~ 1.5 keV (the PSF shape being somewhat energy dependent). Counts were extracted in three bands: "soft" (0.5 - 1.5 keV), "medium" (0.5 - 4.5 keV), and "hard" (1.5 - 6.0 keV). The authors determined the background to subtract from each source by dividing the image into 1 arcminute-wide annuli centered on the aim point in chip 3 (the innermost "annulus" being a circle of radius 1.5 arcminutes). Background values adopted for sources in a given annulus were averages determined from several source-free regions within that annulus, after verifying that the background levels were azimuthally symmetric. For 12 sources ( source_numbers 11b, 12b, 13e, 22c, 32c, 41b, 41c, 84a, 84b, 84c, 93a, and 93b) that fell in the chip gaps or near the outer edge of a chip, background regions were chosen specifically to reflect these conditions. Local background determinations were also made for a small number of sources to the west of the cluster center that lie on or near a large diffuse X-ray source ~7 arcminutes west of the cluster center (see below). Following background subtraction, the authors applied aperture corrections and also corrected for reduced effective exposure times off-axis and in the chip gaps using the exposure map. This table was created by the HEASARC in June 2011 based on the electronic versions of Table 1 from the reference paper which was obtained from the CDS (their catalog J/ApJ/697/224 file table1.dat). This is a service provided by NASA HEASARC .","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/W3Browse/all/omegcencxo.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=omegcencxo&","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"ivo://nasa.heasarc/omegcencxo","keyword":["__"],"landingPage":"ivo://nasa.heasarc/omegcencxo","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"High Energy Astrophysics Science Archive Research Center"},"theme":["Astrophysics"],"title":"Omega Centauri Globular Cluster Chandra X-Ray Point Source Catalog"},"description":"The authors analyzed a ~ 70 ks Chandra Advanced CCD Imaging Spectrometer (ACIS) exposure of the globular cluster Omega Cen (NGC 5139). 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The authors obtained 2 exposures of Omega Cen using the imaging array of the Advanced CCD Imaging Spectrometer (ACIS-I) on 2000 January 24 - 25, in "very faint" (VF) mode. The total exposure time was 72.4 ks. The authors determined source counts using 95% encircled energy radii as determined from model PSFs, derived using the CIAO tool mkpsf at an intermediate energy of ~ 1.5 keV (the PSF shape being somewhat energy dependent). Counts were extracted in three bands: "soft" (0.5 - 1.5 keV), "medium" (0.5 - 4.5 keV), and "hard" (1.5 - 6.0 keV). The authors determined the background to subtract from each source by dividing the image into 1 arcminute-wide annuli centered on the aim point in chip 3 (the innermost "annulus" being a circle of radius 1.5 arcminutes). Background values adopted for sources in a given annulus were averages determined from several source-free regions within that annulus, after verifying that the background levels were azimuthally symmetric. 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The catalog is a renewed and expanded version of the previous Catalog of Neighboring Galaxies by Karachentsev et al. (2004, AJ, 127, 2031). It collects data on the following galaxy observables: angular diameters, apparent magnitudes in the far-UV, B, and K<sub>s</sub> bands, H-alpha and H I fluxes, morphological types, H I-line widths, radial velocities, and distance estimates. In this Local Volume (LV) sample, 108 dwarf galaxies still remain without measured radial velocities. The catalog also lists calculated global galaxy parameters: the linear Holmberg diameters, absolute B magnitudes, surface brightnesses, H I masses, stellar masses estimated via K-band luminosity, H I rotational velocities corrected for galaxy inclination, indicative masses within the Holmberg radius, and three kinds of "tidal index" which quantify the local density environment. 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This catalog is based on three highest Planck frequency channels (i.e., 857, 545, 353 GHz), which are designed to cover the Galactic cold dust emission peak. The 217 GHz band is not included for two reasons: first, the band is contaminated by the CO J=2->1 emission line, which is expected to be significant towards dense regions; second, the contamination by the cosmic microwave background may become problematic at high latitude. The Planck data are combined with the IRIS all-sky data (Miville-Deschenes & Lagache 2005). The IRIS 3THz (100{mu}m) data were chosen to complement the Planck data because it is a good tracer of Galactic warm (~20 K) dust, among other reasons provided in the paper. This table was created by the HEASARC in March 2019 based upon the <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/594/A28\">CDS Catalog J/A+A/594/A28</a> file pgcc.dat. 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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). 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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). 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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). 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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.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/530bbbf4-1ade-4ed5-91de-f03775979ae0","harvest_record_raw":"https://catalog.data.gov/harvest_record/530bbbf4-1ade-4ed5-91de-f03775979ae0/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-lhm70","keyword":["__"],"last_harvested_date":"2026-09-02T00:09:02.903239","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":0,"publisher":"NASA/IPAC Infrared Science Archive","slug":"spitzer-wide-area-infrared-extragalactic-survey-lockman-hole-mips-70-micron-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey Lockman Hole MIPS 70 micron Catalog","type":"dataset"},{"_score":9.183046,"_sort":[1788307734282,9.183046,2,"c7a7edea-39ba-4bd2-94b5-bca21a53f408"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"HEASARC Help Desk","hasEmail":"mailto:andrew.ptak@nasa.gov"},"description":"The low-frequency radio survey of the XMM-Large Scale Structure (XMM-LSS) field centered at RA (J2000) = 2<sup>h</sup>24<sup>m</sup>00<sup>s</sup>, Dec (J2000) = -4<sup>0</sup>09'47" aims to study the connection between the extragalactic radio source populations and their environment as traced by X-ray and optical emission. In their paper, the authors present new radio observations of the XMM-LSS field carried out using the Giant Meterwave Radio Telescope (GMRT) at 240 and 610 MHz. These observations complement the observations presented by Cohen at al. (2003, ApJ, 591, 640; <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/591/640\">CDS Cat. <J/ApJ/591/640></a>) and Tasse et al. (2006, A&A, 456, 791; <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/456/791\">CDS Cat. <J/A+A/456/791></a>) at 74 and 325 MHz with the Very Large Array (VLA). At 240 and 610 MHz, the authors reach noise levels of ~2.5 and ~0.3 mJy/beam, leading to the detection of 466 and 769 sources over 18.0 and 12.7 degree<sup>2</sup> with resolutions of 14.7 arcseconds and 6.5 arcseconds, respectively. Combining these data with the available source lists at 74 MHz, 325 MHz (Tasse et al., 2006) and 1400MHz (NVSS), the authors built a multifrequency catalog containing 1611 radio sources. They checked for consistency of the astrometry and flux density estimates. They fit a simple synchrotron radiation model to the flux density measurements of the 318 radio sources that were detected in at least 4 bands. While ~26% of them showed signature of spectral ageing, ~6% showed self absorption. This table contains the GMRT 240-MHz source list, comprising 388 single sources and 183 components of multiple sources, for a total of 571 entries. For the multiple sources, each component (A, B, etc.) is listed separately, in order of decreasing brightness. This table was created by the HEASARC in February 2012 based on CS Catalog J/A+A/471/1105 file table3.dat. This is a service provided by NASA HEASARC .","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/W3Browse/all/gmrtxl240m.html","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=gmrtxl240m&","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"ivo://nasa.heasarc/gmrtxl240m","keyword":["__"],"landingPage":"ivo://nasa.heasarc/gmrtxl240m","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"High Energy Astrophysics Science Archive Research Center"},"theme":["Astrophysics"],"title":"Giant Metrewave Radio Telescope XMM Large Scale Structure 240-MHz Source Catalog"},"description":"The low-frequency radio survey of the XMM-Large Scale Structure (XMM-LSS) field centered at RA (J2000) = 2<sup>h</sup>24<sup>m</sup>00<sup>s</sup>, Dec (J2000) = -4<sup>0</sup>09'47" aims to study the connection between the extragalactic radio source populations and their environment as traced by X-ray and optical emission. In their paper, the authors present new radio observations of the XMM-LSS field carried out using the Giant Meterwave Radio Telescope (GMRT) at 240 and 610 MHz. These observations complement the observations presented by Cohen at al. (2003, ApJ, 591, 640; <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/591/640\">CDS Cat. <J/ApJ/591/640></a>) and Tasse et al. (2006, A&A, 456, 791; <a href=\"https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/456/791\">CDS Cat. <J/A+A/456/791></a>) at 74 and 325 MHz with the Very Large Array (VLA). At 240 and 610 MHz, the authors reach noise levels of ~2.5 and ~0.3 mJy/beam, leading to the detection of 466 and 769 sources over 18.0 and 12.7 degree<sup>2</sup> with resolutions of 14.7 arcseconds and 6.5 arcseconds, respectively. Combining these data with the available source lists at 74 MHz, 325 MHz (Tasse et al., 2006) and 1400MHz (NVSS), the authors built a multifrequency catalog containing 1611 radio sources. They checked for consistency of the astrometry and flux density estimates. They fit a simple synchrotron radiation model to the flux density measurements of the 318 radio sources that were detected in at least 4 bands. While ~26% of them showed signature of spectral ageing, ~6% showed self absorption. This table contains the GMRT 240-MHz source list, comprising 388 single sources and 183 components of multiple sources, for a total of 571 entries. For the multiple sources, each component (A, B, etc.) is listed separately, in order of decreasing brightness. This table was created by the HEASARC in February 2012 based on CS Catalog J/A+A/471/1105 file table3.dat. This is a service provided by NASA HEASARC .","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/8e65481c-31e0-4021-8fde-ad54f44076ee","harvest_record_raw":"https://catalog.data.gov/harvest_record/8e65481c-31e0-4021-8fde-ad54f44076ee/raw","has_download":true,"has_spatial":false,"identifier":"ivo://nasa.heasarc/gmrtxl240m","keyword":["__"],"last_harvested_date":"2026-09-02T00:08:54.282472","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":2,"publisher":"High Energy Astrophysics Science Archive Research Center","slug":"giant-metrewave-radio-telescope-xmm-large-scale-structure-240-mhz-source-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Giant Metrewave Radio Telescope XMM Large Scale Structure 240-MHz Source Catalog","type":"dataset"},{"_score":13.654705,"_sort":[1788307725588,13.654705,1,"fdf22fc2-5d79-4f8a-a5e8-85bac40d7e87"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"IRSA Support","hasEmail":"mailto:irsasupport@ipac.caltech.edu"},"description":"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.","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/SCS?table=elaiss1_cat_f05&","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/data/SPITZER/SWIRE/SWIRE_ES1_columns.html","format":"HTML","mediaType":"text/html"}],"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-es1","keyword":["__"],"landingPage":"ivo://irsa.ipac/spitzer/catalog/swire/swire-es1","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"NASA/IPAC Infrared Science Archive"},"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey ELAIS-S1 Optical-IRAC-MIPS24 Catalog"},"description":"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.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/2fc0f1de-f082-4aab-a37d-3879013a6ce1","harvest_record_raw":"https://catalog.data.gov/harvest_record/2fc0f1de-f082-4aab-a37d-3879013a6ce1/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/spitzer/catalog/swire/swire-es1","keyword":["__"],"last_harvested_date":"2026-09-02T00:08:45.588748","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":1,"publisher":"NASA/IPAC Infrared Science Archive","slug":"spitzer-wide-area-infrared-extragalactic-survey-elais-s1-optical-irac-mips24-catalog","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Spitzer Wide-area InfraRed Extragalactic Survey ELAIS-S1 Optical-IRAC-MIPS24 Catalog","type":"dataset"},{"_score":9.286556,"_sort":[1788307719673,9.286556,1,"ea0cd8c7-d210-4a79-90a1-058b90494604"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"HEASARC Help Desk","hasEmail":"mailto:andrew.ptak@nasa.gov"},"description":"The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius >= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10<sup>29.5</sup> - 10<sup>31.5</sup> erg s<sup>-1</sup>. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties. 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The present DataSet collects the GIADA data of ESC1 phase. 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The three highest Planck bands (857, 545, 353 GHz) have been combined with IRAS data at 3 THz to perform a multi-frequency detection of sources colder than their local environment. After rejection of possible extragalactic contaminants, the PGCC catalogue contains 13188 Galactic sources spread across the whole sky, i.e., from the Galactic plane to high latitudes, following the spatial distribution of the main molecular cloud complexes. The median temperature of PGCC sources lies between 13 and 14.5 K, depending on the quality of the flux density measurements, with a temperature ranging from 5.8 to 20 K after removing sources with the 1% largest temperature estimates. Using seven independent methods, reliable distance estimates have been obtained for 5574 sources, which allows the derivation of physical properties such as their mass, physical size, mean density and luminosity.","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/SCS?table=com_pccs2_gcc&","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://irsa.ipac.caltech.edu/data/Planck/release_2/docs/README.html","format":"HTML","mediaType":"text/html"}],"identifier":"ivo://irsa.ipac/planck/catalog/pgcc","keyword":["__"],"landingPage":"ivo://irsa.ipac/planck/catalog/pgcc","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"NASA/IPAC Infrared Science Archive"},"theme":["Astrophysics"],"title":"Planck Catalog of Galactic Cold Clumps"},"description":"The Planck Catalogue of Galactic Cold Clumps (PGCC) is an observational catalogue consisting exclusively of Galactic cold sources. 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Using seven independent methods, reliable distance estimates have been obtained for 5574 sources, which allows the derivation of physical properties such as their mass, physical size, mean density and luminosity.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/30c80fe9-258b-479b-9576-c33815c03340","harvest_record_raw":"https://catalog.data.gov/harvest_record/30c80fe9-258b-479b-9576-c33815c03340/raw","has_download":true,"has_spatial":false,"identifier":"ivo://irsa.ipac/planck/catalog/pgcc","keyword":["__"],"last_harvested_date":"2026-09-02T00:07:40.277181","organization":{"aliases":[""],"code_repo_exempt":false,"code_repo_url":null,"description":null,"id":"f4ca4614-8901-409b-8553-2e994ad10023","logo":"https://raw.githubusercontent.com/GSA/logo/refs/heads/master/nasa.png","name":"National Aeronautics and Space Administration","organization_type":"Federal Government","slug":"nasa"},"parent_identifier":null,"popularity":3,"publisher":"NASA/IPAC Infrared Science Archive","slug":"planck-catalog-of-galactic-cold-clumps","spatial_centroid":null,"spatial_shape":null,"theme":["Astrophysics"],"title":"Planck Catalog of Galactic Cold Clumps","type":"dataset"},{"_score":6.7982273,"_sort":[1788307659893,6.7982273,4,"a846fc7b-a55a-4c6e-8932-a1c8af5f307f"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"NASA Space Physics Data Facility","hasEmail":"mailto:NASA-SPDF-Support@nasa.onmicrosoft.com"},"description":"'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with the spectrum analyzers. The PWI Spectrum Analyzers were designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The pair consisted of a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz, and a 14-channel analyzer covering the range from 5.62 Hz to 10 kHz. These analyzers have a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The center frequencies and bandwidths of the 20- and 14-channel analyzers are identical. The 20-channel analyzer was nominally intended for electric field measurements (which extend up to higher frequencies than the magnetic measurements), and the 14-channel analyzer was nominally intended for magnetic field measurements. All channels are sampled simultaneously so that electric-to-magnetic field ratios could be accurately determined. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/isee/isee1/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://www-pw.physics.uiowa.edu/isee/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://www-pw.physics.uiowa.edu/plasma-wave/isee/data/ISEE1/cdf/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=ISEE1_PWI_SA&index=sp_phys","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/hapi","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/ISEE1_PWE_SA_PT1S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/ISEE1/PWE/SA/PT1S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/isee/isee1/","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/zw5z-3r03","keyword":["spectrum","waves-passive"],"landingPage":"https://doi.org/10.48322/zw5z-3r03","license":"https://www.usa.gov/government-works","modified":"2026-09-01","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"CDAWeb, RadioPlasmaWaveGroup"},"theme":["Heliophysics"],"title":"ISEE 1 Plasma wave experiment (PWE) Spectrum Analyzer"},"description":"'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with the spectrum analyzers. The PWI Spectrum Analyzers were designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The pair consisted of a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz, and a 14-channel analyzer covering the range from 5.62 Hz to 10 kHz. These analyzers have a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The center frequencies and bandwidths of the 20- and 14-channel analyzers are identical. The 20-channel analyzer was nominally intended for electric field measurements (which extend up to higher frequencies than the magnetic measurements), and the 14-channel analyzer was nominally intended for magnetic field measurements. All channels are sampled simultaneously so that electric-to-magnetic field ratios could be accurately determined. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. 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