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MODIS is playing a vital role in the development of validated, global, interactive Earth system models able to predict global change accurately enough to assist policy makers in making sound decisions concerning the protection of our environment.","distribution_titles":["View this dataset's algorithm theoretical basis document","View information related to this dataset","Download this dataset through a directory map","View this dataset's processing history"],"harvest_record":"https://catalog.data.gov/harvest_record/00fe5ae9-0ea2-44b8-bb5b-a11980f437ed","harvest_record_raw":"https://catalog.data.gov/harvest_record/00fe5ae9-0ea2-44b8-bb5b-a11980f437ed/raw","has_download":true,"has_spatial":true,"identifier":"C1615934263-OB_DAAC","keyword":["earth-science","national-geospatial-data-asset","ngda","ocean-temperature","oceans"],"last_harvested_date":"2026-10-07T01:01:22.404993","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/GSFC/SED/ESD/GCDC/OB.DAAC","slug":"terra-modis-level-3-global-binned-4m-nighttime-sea-surface-temperature-sst4-data-version-r","spatial_centroid":null,"spatial_shape":null,"theme":["geospatial"],"title":"Terra MODIS Level-3 Global Binned 4\u00b5m Nighttime Sea Surface Temperature (SST4) Data, version R2019.0","type":"dataset"},{"_score":76.91341,"_sort":[1791334797047,76.91341,2,"1a7d537c-d3ef-4dbd-a519-fed0b1114c06"],"access_level":"public","dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"In recent times long-term stay has become a common occurrence in the International Space Station (ISS). However adaptation to the space environment can sometimes pose physiological problems to the astronauts after their return. Therefore it is important to develop healthcare technologies for astronauts. In this study hair an easy-to-obtain sample was identified as the candidate. In order to investigate the genetic changes in human hair during space flight the hair follicles of 10 astronauts were analyzed by DNA microarray and real time q-PCR analyses. Space environment induced gene expression of hair follicles of astronaut was measured 6 differnent times included 2 in flight on orbit. Ten independent experiments were performed on differing astronauts. and the sampling day was differed for each astronaut because of their schedules.","distribution":[{"@type":"dcat:Distribution","description":"GeneLab Study Page","downloadURL":"https://genelab-data.ndc.nasa.gov/genelab/accession/GLDS-174","format":"HTML","mediaType":"text/html","title":"Effects of a Closed Space Environment on Gene Expression in Hair Follicles of Astronauts in the International Space Station"}],"identifier":"nasa_genelab_GLDS-174_5rt9-fftx","issued":"2021-05-21","keyword":["data-collection","exposure-duration","labeling","normalization-data-transformation","nucleic-acid-hybridization","rna-extraction","sex","spaceflight","treatment-protocol"],"landingPage":"https://data.nasa.gov/dataset/effects-of-a-closed-space-environment-on-gene-expression-in-hair-follicles-of-astronauts-i","license":"http://www.usa.gov/publicdomain/label/1.0/","modified":"2025-04-23","programCode":["026:005"],"publisher":{"@type":"org:Organization","name":"National Aeronautics and Space Administration"},"theme":["Earth Science"],"title":"Effects of a Closed Space Environment on Gene Expression in Hair Follicles of Astronauts in the International Space Station"},"description":"In recent times long-term stay has become a common occurrence in the International Space Station (ISS). However adaptation to the space environment can sometimes pose physiological problems to the astronauts after their return. Therefore it is important to develop healthcare technologies for astronauts. In this study hair an easy-to-obtain sample was identified as the candidate. In order to investigate the genetic changes in human hair during space flight the hair follicles of 10 astronauts were analyzed by DNA microarray and real time q-PCR analyses. Space environment induced gene expression of hair follicles of astronaut was measured 6 differnent times included 2 in flight on orbit. Ten independent experiments were performed on differing astronauts. and the sampling day was differed for each astronaut because of their schedules.","distribution_titles":["Effects of a Closed Space Environment on Gene Expression in Hair Follicles of Astronauts in the International Space Station"],"harvest_record":"https://catalog.data.gov/harvest_record/68bf6945-d885-433e-ad9e-b7ac1861ce1e","harvest_record_raw":"https://catalog.data.gov/harvest_record/68bf6945-d885-433e-ad9e-b7ac1861ce1e/raw","has_download":true,"has_spatial":false,"identifier":"nasa_genelab_GLDS-174_5rt9-fftx","keyword":["data-collection","exposure-duration","labeling","normalization-data-transformation","nucleic-acid-hybridization","rna-extraction","sex","spaceflight","treatment-protocol"],"last_harvested_date":"2026-10-07T00:59:57.047051","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":"National Aeronautics and Space Administration","slug":"effects-of-a-closed-space-environment-on-gene-expression-in-hair-follicles-of-astronauts-i","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"Effects of a Closed Space Environment on Gene Expression in Hair Follicles of Astronauts in the International Space Station","type":"dataset"},{"_score":21.750237,"_sort":[1791334789532,21.750237,1,"2b7594c9-ec1d-4a7b-817e-c0f75bda5a5b"],"access_level":"public","dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"Space environment is suspected to generate reactive oxygen species (ROS) and induce oxidative stress in plants however little is known about the gene expression of ROS gene network in plants grown in long-term space flight. RNA-Seq was used to define the large-scale gene expression profiles of Mizuna harvested after 27 days cultivation in the international space station to understand the molecular response and adaptation to space environment.Results: Total reads of transcripts from the Mizuna grown in the international space station as well as on the ground by RNA-Seq using next generation sequencing technology showed 8,258 and 14,170 transcripts up- and down-regulated in the space-grown Mizuna respectively when compared with those from the ground-grown Mizuna. A total of 20 in 32 ROS oxidative marker genes were up-regulated including high expression of 4 hallmarks and preferentially expressed gene associated with ROS-scavenging genes was thioredoxin glutaredoxin and alternative oxidase genes. In the transcription factors of ROS gene network MEKK1-MKK4-MPK3 OXI1-MKK4-MPK3 and OXI1-MPK3 of MAP cascades induction of WRKY22 by MEKK1-MKK4-MPK3 cascade induction of WRKY25 and repression of ZAT7 by Zat12 were suggested. RbohD and RbohF genes were up-regulated preferentially in NADPH oxidase genes which produce ROS.Conclusions: Our large-scale transcriptome analysis demonstrated that the space environment induced oxidative stress and ROS gene network was activated in the space-grown Mizuna some of which were common genes up-regulated by abiotic and biotic stress and were preferentially up-regulated genes by the space environment even though Mizuna grew in the space as well as on the ground showing that plants could acclimate to the space environment by reprograming the expression of ROS gene network.","distribution":[{"@type":"dcat:Distribution","description":"GeneLab Study Page","downloadURL":"https://genelab-data.ndc.nasa.gov/genelab/accession/GLDS-59","format":"HTML","mediaType":"text/html","title":"RNA-Seq transcriptome analysis of reactive oxygen species gene network in Mizuna plants grown in long-term space flight"}],"identifier":"nasa_genelab_GLDS-59_af4u-mnh4","issued":"2018-06-26","keyword":["library-construction","nucleic-acid-extraction","nucleic-acid-sequencing","sample-collection","space-flight"],"landingPage":"https://data.nasa.gov/dataset/rna-seq-transcriptome-analysis-of-reactive-oxygen-species-gene-network-in-mizuna-plants-gr","modified":"2025-04-23","programCode":["026:005"],"publisher":{"@type":"org:Organization","name":"National Aeronautics and Space Administration"},"theme":["Earth Science"],"title":"RNA-Seq transcriptome analysis of reactive oxygen species gene network in Mizuna plants grown in long-term space flight"},"description":"Space environment is suspected to generate reactive oxygen species (ROS) and induce oxidative stress in plants however little is known about the gene expression of ROS gene network in plants grown in long-term space flight. RNA-Seq was used to define the large-scale gene expression profiles of Mizuna harvested after 27 days cultivation in the international space station to understand the molecular response and adaptation to space environment.Results: Total reads of transcripts from the Mizuna grown in the international space station as well as on the ground by RNA-Seq using next generation sequencing technology showed 8,258 and 14,170 transcripts up- and down-regulated in the space-grown Mizuna respectively when compared with those from the ground-grown Mizuna. A total of 20 in 32 ROS oxidative marker genes were up-regulated including high expression of 4 hallmarks and preferentially expressed gene associated with ROS-scavenging genes was thioredoxin glutaredoxin and alternative oxidase genes. In the transcription factors of ROS gene network MEKK1-MKK4-MPK3 OXI1-MKK4-MPK3 and OXI1-MPK3 of MAP cascades induction of WRKY22 by MEKK1-MKK4-MPK3 cascade induction of WRKY25 and repression of ZAT7 by Zat12 were suggested. RbohD and RbohF genes were up-regulated preferentially in NADPH oxidase genes which produce ROS.Conclusions: Our large-scale transcriptome analysis demonstrated that the space environment induced oxidative stress and ROS gene network was activated in the space-grown Mizuna some of which were common genes up-regulated by abiotic and biotic stress and were preferentially up-regulated genes by the space environment even though Mizuna grew in the space as well as on the ground showing that plants could acclimate to the space environment by reprograming the expression of ROS gene network.","distribution_titles":["RNA-Seq transcriptome analysis of reactive oxygen species gene network in Mizuna plants grown in long-term space flight"],"harvest_record":"https://catalog.data.gov/harvest_record/f74b1baf-f484-48a9-bc88-95156b609a0d","harvest_record_raw":"https://catalog.data.gov/harvest_record/f74b1baf-f484-48a9-bc88-95156b609a0d/raw","has_download":true,"has_spatial":false,"identifier":"nasa_genelab_GLDS-59_af4u-mnh4","keyword":["library-construction","nucleic-acid-extraction","nucleic-acid-sequencing","sample-collection","space-flight"],"last_harvested_date":"2026-10-07T00:59:49.532391","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":"National Aeronautics and Space Administration","slug":"rna-seq-transcriptome-analysis-of-reactive-oxygen-species-gene-network-in-mizuna-plants-gr","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"RNA-Seq transcriptome analysis of reactive oxygen species gene network in Mizuna plants grown in long-term space flight","type":"dataset"},{"_score":7.8896737,"_sort":[1791334786104,7.8896737,3,"76f15315-5217-48c1-806c-ea2d0db795b2"],"access_level":"public","dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"Because of their ubiquity and resistance to spacecraft decontamination bacterial spores are considered likely potential forward contaminants on robotic missions to Mars. Thus it is important to understand their global responses to long-term exposure to space or Mars environments. As part of the PROTECT experiment spores of B. subtilis 168 were exposed to real space conditions and to simulated martian conditions for 559 days in low Earth orbit mounted on the EXPOSE-E exposure platform outside the European Columbus module on the International Space Station. Upon return spores were germinated total RNA extracted and fluorescently labeled and used to probe a custom Bacillus subtilis microarray to identify genes preferentially activated or repressed relative to ground control spores. Increased transcript levels were detected for a number of stress-related regulons responding to DNA damage (SOS response SP-beta prophage induction) protein damage (CtsR/Clp system) oxidative stress (PerR regulon) and cell envelope stress (SigV regulon). Spores exposed to space demonstrated a much broader and more severe stress response than spores exposed to simulated Mars conditions. The results are discussed in the context of planetary protection for a hypothetical journey of potential forward contaminant spores from Earth to Mars and their subsequent residence on Mars. Two-color microarrays were performed comparing germination of Space-exposed or Mars-exposed vs. ground-control (Earth) spores.","distribution":[{"@type":"dcat:Distribution","description":"GeneLab Study Page","downloadURL":"https://genelab-data.ndc.nasa.gov/genelab/accession/GLDS-28","format":"HTML","mediaType":"text/html","title":"Bacillus subtilis spores PROTECT experiment Space-exposed and Mars-exposed vs. Earth-control"}],"identifier":"nasa_genelab_GLDS-28_dgmm-uid9","issued":"2018-06-26","keyword":["bioassay_data_transformation","environment-exposure","feature_extraction","gravitation","grow","hybridization","image_aquisition","labeling","nucleic_acid_extraction","p-gse37124-1","p-gse37124-2","p-gse37124-3","p-gse37124-4","p-gse37124-5","p-gse37124-6","p-gse37124-7","p-gse37124-8","specified_biomaterial_action"],"landingPage":"https://data.nasa.gov/dataset/bacillus-subtilis-spores-protect-experiment-space-exposed-and-mars-exposed-vs-earth-contro","modified":"2025-04-23","programCode":["026:005"],"publisher":{"@type":"org:Organization","name":"National Aeronautics and Space Administration"},"theme":["Earth Science"],"title":"Bacillus subtilis spores PROTECT experiment Space-exposed and Mars-exposed vs. Earth-control"},"description":"Because of their ubiquity and resistance to spacecraft decontamination bacterial spores are considered likely potential forward contaminants on robotic missions to Mars. Thus it is important to understand their global responses to long-term exposure to space or Mars environments. As part of the PROTECT experiment spores of B. subtilis 168 were exposed to real space conditions and to simulated martian conditions for 559 days in low Earth orbit mounted on the EXPOSE-E exposure platform outside the European Columbus module on the International Space Station. Upon return spores were germinated total RNA extracted and fluorescently labeled and used to probe a custom Bacillus subtilis microarray to identify genes preferentially activated or repressed relative to ground control spores. Increased transcript levels were detected for a number of stress-related regulons responding to DNA damage (SOS response SP-beta prophage induction) protein damage (CtsR/Clp system) oxidative stress (PerR regulon) and cell envelope stress (SigV regulon). Spores exposed to space demonstrated a much broader and more severe stress response than spores exposed to simulated Mars conditions. The results are discussed in the context of planetary protection for a hypothetical journey of potential forward contaminant spores from Earth to Mars and their subsequent residence on Mars. Two-color microarrays were performed comparing germination of Space-exposed or Mars-exposed vs. ground-control (Earth) spores.","distribution_titles":["Bacillus subtilis spores PROTECT experiment Space-exposed and Mars-exposed vs. Earth-control"],"harvest_record":"https://catalog.data.gov/harvest_record/88f43a41-aafe-435c-833c-90568af82e8b","harvest_record_raw":"https://catalog.data.gov/harvest_record/88f43a41-aafe-435c-833c-90568af82e8b/raw","has_download":true,"has_spatial":false,"identifier":"nasa_genelab_GLDS-28_dgmm-uid9","keyword":["bioassay_data_transformation","environment-exposure","feature_extraction","gravitation","grow","hybridization","image_aquisition","labeling","nucleic_acid_extraction","p-gse37124-1","p-gse37124-2","p-gse37124-3","p-gse37124-4","p-gse37124-5","p-gse37124-6","p-gse37124-7","p-gse37124-8","specified_biomaterial_action"],"last_harvested_date":"2026-10-07T00:59:46.104864","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":"National Aeronautics and Space Administration","slug":"bacillus-subtilis-spores-protect-experiment-space-exposed-and-mars-exposed-vs-earth-contro","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"Bacillus subtilis spores PROTECT experiment Space-exposed and Mars-exposed vs. Earth-control","type":"dataset"},{"_score":11.831917,"_sort":[1791334783660,11.831917,2,"f72f7357-7dd9-4ea7-ab7d-c06682fa908f"],"access_level":"public","dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"Anticipating the risk for infectious disease during space exploration and habitation is a critical factor to ensure safety health and performance of the crewmembers. As a ubiquitous environmental organism that is occasionally part of the human flora Pseudomonas aeruginosa could pose a health hazard for the immuno-compromised astronauts. In order to gain insights in the behavior of P. aeruginosa in spaceflight conditions two spaceflight-analogue culture systems i.e. the rotating wall vessel (RWV) and the random position machine (RPM) were used. Microarray analysis of P. aeruginosa PAO1 grown in the low shear modeled microgravity (LSMMG) environment of the RWV compared to the normal gravity control (NG) revealed a regulatory role for AlgU (RpoE). Specifically P. aeruginosa cultured in LSMMG exhibited increased alginate production and up-regulation of AlgU-controlled transcripts including those encoding stress-related proteins. This study also shows the involvement of Hfq in the LSMMG response consistent with its previously identified role in the Salmonella LSMMG- and spaceflight response. Furthermore cultivation in LSMMG increased heat and oxidative stress resistance and caused a decrease in the culture oxygen transfer rate. Interestingly the global transcriptional response of P. aeruginosa grown in the RPM was similar to that in NG. The possible role of differences in fluid mixing between the RWV and RPM is discussed with the overall collective data favoring the RWV as the optimal model to study the LSMMG-response of suspended cells. This study represents a first step towards the identification of specific virulence mechanisms of P. aeruginosa activated in response to spaceflight-analogue conditions and could direct future research regarding the risk assessment and prevention of Pseudomonas infections for the crew in flight and the general public.","distribution":[{"@type":"dcat:Distribution","description":"GeneLab Study Page","downloadURL":"https://genelab-data.ndc.nasa.gov/genelab/accession/GLDS-14","format":"HTML","mediaType":"text/html","title":"Response of Pseudomonas aeruginosa PAO1 to low shear modeled microgravity"}],"identifier":"nasa_genelab_GLDS-14_fg6b-h7es","issued":"2021-05-21","keyword":["bioassay_data_transformation","data-transformation","feature_extraction","genelab-microarray-data-processing-protocol","grow","hybridization","image_aquisition","labeling","microgravity-simulation","nucleic_acid_extraction","p-gse16970-1","p-gse16970-2","p-gse16970-3","p-gse16970-4","p-gse16970-5","p-gse16970-6","p-gse16970-7","p-gse16970-8","specified_biomaterial_action"],"landingPage":"https://data.nasa.gov/dataset/response-of-pseudomonas-aeruginosa-pao1-to-low-shear-modeled-microgravity","license":"http://www.usa.gov/publicdomain/label/1.0/","modified":"2025-04-23","programCode":["026:005"],"publisher":{"@type":"org:Organization","name":"National Aeronautics and Space Administration"},"theme":["Earth Science"],"title":"Response of Pseudomonas aeruginosa PAO1 to low shear modeled microgravity"},"description":"Anticipating the risk for infectious disease during space exploration and habitation is a critical factor to ensure safety health and performance of the crewmembers. As a ubiquitous environmental organism that is occasionally part of the human flora Pseudomonas aeruginosa could pose a health hazard for the immuno-compromised astronauts. In order to gain insights in the behavior of P. aeruginosa in spaceflight conditions two spaceflight-analogue culture systems i.e. the rotating wall vessel (RWV) and the random position machine (RPM) were used. Microarray analysis of P. aeruginosa PAO1 grown in the low shear modeled microgravity (LSMMG) environment of the RWV compared to the normal gravity control (NG) revealed a regulatory role for AlgU (RpoE). Specifically P. aeruginosa cultured in LSMMG exhibited increased alginate production and up-regulation of AlgU-controlled transcripts including those encoding stress-related proteins. This study also shows the involvement of Hfq in the LSMMG response consistent with its previously identified role in the Salmonella LSMMG- and spaceflight response. Furthermore cultivation in LSMMG increased heat and oxidative stress resistance and caused a decrease in the culture oxygen transfer rate. Interestingly the global transcriptional response of P. aeruginosa grown in the RPM was similar to that in NG. The possible role of differences in fluid mixing between the RWV and RPM is discussed with the overall collective data favoring the RWV as the optimal model to study the LSMMG-response of suspended cells. This study represents a first step towards the identification of specific virulence mechanisms of P. aeruginosa activated in response to spaceflight-analogue conditions and could direct future research regarding the risk assessment and prevention of Pseudomonas infections for the crew in flight and the general public.","distribution_titles":["Response of Pseudomonas aeruginosa PAO1 to low shear modeled microgravity"],"harvest_record":"https://catalog.data.gov/harvest_record/3273dc2b-1906-47d8-b17d-cbfe405f1067","harvest_record_raw":"https://catalog.data.gov/harvest_record/3273dc2b-1906-47d8-b17d-cbfe405f1067/raw","has_download":true,"has_spatial":false,"identifier":"nasa_genelab_GLDS-14_fg6b-h7es","keyword":["bioassay_data_transformation","data-transformation","feature_extraction","genelab-microarray-data-processing-protocol","grow","hybridization","image_aquisition","labeling","microgravity-simulation","nucleic_acid_extraction","p-gse16970-1","p-gse16970-2","p-gse16970-3","p-gse16970-4","p-gse16970-5","p-gse16970-6","p-gse16970-7","p-gse16970-8","specified_biomaterial_action"],"last_harvested_date":"2026-10-07T00:59:43.660954","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":"National Aeronautics and Space Administration","slug":"response-of-pseudomonas-aeruginosa-pao1-to-low-shear-modeled-microgravity-1bea8","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"Response of Pseudomonas aeruginosa PAO1 to low shear modeled microgravity","type":"dataset"},{"_score":16.079765,"_sort":[1791334780386,16.079765,7,"ec47d45b-3303-4776-9d40-a735dd1d8af1"],"access_level":"public","dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"The JAXA MHU-2 mission had two objectives: 1) To increase understanding of effects of spaceflight on the gut environment (microbiota and metabolites) and immune system using multi-omics based analysis; 2) To evaluate whether fructo-oligosaccharides added to the diet as prebiotics improve the gut environment and immune function during spaceflight. Twelve 16-18 week old male C57BL/6J mice were singly housed in the JAXA Habitat Cage Units (HCUs) on the ISS for 30 days. Six flight mice were housed in microgravity while six were exposed to simulated 1g by centrifugation. These two flight groups were further divided in half so that three mice in each group received standard JAXA chow while the other three were fed chow supplemented with fructooligosaccharides (FOS). Mice were returned live and euthanized and dissected <1 day after splashdown. Ground controls (n=6) were asynchronous and housed in HCUs. Vivarium controls (n=6) were asynchronous and housed in standard habitats. Three ground control and three vivarium animals received standard chow while the other three each ground control and vivarium animals received FOS-supplemented chow. Ground and vivarium samples were dissected by a separate dissection team than flight samples. Femoral skin was dissected 30 minutes after euthanasia and snap frozen in liquid nitrogen. Total RNA was extracted and sequenced at a target depth of 60 M clusters per sample (ribodepleted paired end 150). Study Factor Levels: 1)Spaceflight ug Std. Chow: 3; 2)Spaceflight ug FOS: 3; 3) Spaceflight Artificial 1g Std. Chow: 3; 4)Spaceflight Artificial 1g FOS: 3; 5)Ground 1g Std. Chow: 3; 6)Ground 1g FOS: 3; 7)Vivarium 1g Std. 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We used this unique environment to evaluate the effects of microgravity on kidney proximal tubule epithelial cell (PTEC) response to serum exposure and vitaminD biotransformation capacity. To test if microgravity alters the pathologic response of the proximal tubule to serum exposure, we treated PTECs cultured in a microphysiological system (PT-MPS) with human serum and measured biomarkers of toxicity and inflammation (KIM-1 and IL-6) and conducted global transcriptomics via RNAseq on cells undergoing flight (microgravity) and respective controls(ground). Given the profound bone loss observed in microgravity and PTECs produce the active form of vitamin D, we treated 3D cultured PTECs with 25(OH)D 3 (vitamin D) and monitored vitamin D metabolite formation, conducted global transcriptomics via RNAseq, and evaluated transcript expression of CYP27B1, CYP24A1, or CYP3A5 in PTECs undergoing flight (microgravity) and respective ground controls. 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Vogt                                       |\n| Data Supplier                     | National Space Science Data Center                   |\n| Data Sampling Rate                | Variable (1 hr for FPHA Data, 15 min for all others) |\n| Data Set Start Time               | 1979-02-28T00:00:00.000Z                             |\n| Data Set Stop Time                | 1979-03-21T23:45:00.000Z                             |\n+------------------------------------------------------------------------------------------+\n\nThe following Description has been adapted from NSSDC CRS, 1979:\n\nAs its Name implies, the Cosmic Ray Subsystem (CRS) was designed for Cosmic Ray Studies (Stone et al., 1977b). It consists of two High Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The Detectors have large Geometric Factors (about 0.48 cm^2 sr to 8 cm^2 sr) and long Electronic Time Constants (\u223c24 \u00b5s) for low Power Consumption and good Stability. Normally, the Data are primarily derived from comprehensive (\u03b4E[1], \u03b4E[2] and E) Pulse-Height Information about individual Events. Because of the high Particle Fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on Counting Rates in single Detectors and various Coincidence Rates. In Interplanetary Space, Guard Counters are placed in Anticoincidence with the Primary Detectors to reduce the Background from High-Energy Particles penetrating through the Sides of the Telescopes. These Guard Counters were turned off in the Jovian Magnetosphere when the accidental Anticoincidence Rate became high enough to block a substantial Fraction of the desired Counts. Fortunately, under these Conditions the Spectra were sufficiently soft that the Background, due to penetrating Particles, was small.\n\nThe Data on Proton and Ion Fluxes at Jupiter were obtained with the LET. The Thicknesses of individual Solid-State Detectors in the LET and their Trigger Thresholds were chosen such that, even in the Jovian Magnetosphere, Electrons made, at most, a very minor Contribution to the Proton Counting Rates (Lupton and Stone, 1972). Dead Time Corrections and accidental Coincidences were small (<20%) throughout most of the Magnetotail, but were substantial (>50%) at Flux Maxima within 40 Rj Of Jupiter. Data have been included in this Package for those Periods when the Corrections are less than \u223c50% and can be corrected by the User with the Dead Time appropriate to the Detector (2 \u03b4s to 25 \u03b4s). The high Counting Rates, however, caused some Baseline Shift which may have raised Proton Thresholds significantly. In the Inner Magnetosphere, the L[2] Counting Rate was still useful because it never rolled over. This Rate is due to 1.8 MeV to 13 MeV Protons penetrating L[1] (0.43 cm^2 sr) and >9 MeV Protons penetrating the Shield (8.4 cm^2 sr). For an E^-2 Spectrum, the two Groups would make comparable Contributions, but in the Magnetosphere, for the E^-3 to E^-4 Spectrum above 2.5 MeV (McDonald et al., 1979), the Contribution from Protons penetrating the Shield would be only 3% to 14%.\n\nThe LET L[1]L[2]L[4] and L[1]L[2]L[3] Coincidence-Anticoincidence Rates give the Proton Flux between 1.8 MeV and 8 MeV and 3 MeV to 8 MeV with a small Alpha Particle Contribution (~10^-3). Corrections are required for Dead Time Losses in L[1], accidental L[1]L[2] Coincidences and Anticoincidence Losses from L[4]. Data are given only for Periods when these Corrections are relatively small. In addition to the Rates listed in the Table, the Energy lost in Detectors L[1], L[2] and L[3] was measured for individual Particles. For Protons, this covered the Energy Range from 0.42 MeV to 8.3 MeV. Protons can be identified positively by the \u03b4E versus E Technique, their Spectra obtained and accidental Coincidences greatly reduced. Because of Telemetry Limitations, however, only a small Fraction of the Events could be transmitted, and Statistics become poor unless Pulse-Height Data are averaged over a Period of one Hour.\n\nHET and LET Detectors share the same Data Lines and Pulse-Height Analyzers. Thus, the Telescopes can interfere with one another during Periods of high Counting Rates. To prevent such an Interference and explore different Coincidence Conditions, the Experiment was cycled through four Operating Modes, each 192 s long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] Coincidence Requirements. The TET was cycled through various Coincidence Conditions, including Singles from the Front Detectors. At the Expense of some Time Resolution, this Procedure permitted us to obtain significant Data in the Outer Magnetosphere and excellent Data during the long Passage through the Magnetotail Region.\n\nSome of the published Results from this Experiment required extensive Corrections for Dead Time, accidental Coincidences and Anticoincidences (Vogt et al., 1979a, Vogt et al., 1979b, Schardt et al., 1981, Gehrels, 1981). These Corrections can be applied only on a case-by-case Basis after a careful Study of the Environment and many Self-Consistency Checks. They cannot be applied on a systematic Basis and we have no Computer Programs to do so. Therefore, Data from such Periods are not included in the Data Center Submission. The Scientists on the CRS Team will, however, be glad to consider special Requests if the desired Information can be extracted from the Data.\n\n* Description of the Data\n* =======================\n\n(1) LD1 RATE gives the nominal >0.43 MeV Proton Flux (cm^2 s sr)^-1. This Rate includes all Particles which pass through a 0.8 mg/cm^2 Aluminum Foil and deposits more than 220 keV in a 34.6 \u00b5m Silicon Detector on Voyager 1 (209 keV, 33.9 \u00b5m on Voyager 2) Therefore, Heavy Ions, such as Oxygen and Sulfur are also detected, however, their Contribution is believed to be relatively small. Only a small Percentage of the Pulses in this Detector are larger than the maximum Energy that can be deposited by a Proton. Heavy Ions would produce such large Pulses, unless their Energy Spectra were much steeper than the Proton Spectrum. The true Flux, F(t), can be calculated from the Data:\n\nF(t) = F/(1-1.26x10^-4 F)\n\nand Corrections are small for F<1000 (cm^2 s)^-1.\n\n(2) The LD2 RATE is not suitable for an Absolute Flux Determination and is given in counts per second. The Detector responds to Protons and Ions that penetrate either (a) 0.8 mg/cm^2 Aluminum plus 8.0 mg/cm^2 Silicon and lose at least 200 keV in a 35 \u00b5m Si Detector (1.8 MeV to 13 MeV) or (b) pass through >140 mg/cm^2 Aluminum. For an E^-2 Proton Spectrum, the Contributions from (a) and (b) would be about equal, however, the Proton Spectrum is substantially softer throughout most of the Magnetosphere and the Detector should respond primarily to (a). Dead Time Corrections are given by\n\nR(t) = R/(1-2.55x10^-5 R)\n\nwhere R is the Count Rate in counts per second. Thus, Correction to the supplied data are small for R<4000 counts per second, but become so large in the middle Magnetosphere that the Magnitude of even relative intensity Changes becomes uncertain.\n\n(3) LD L[1].L[2].L[4]. SL COINCIDENCE RATE gives the total Proton Flux (cm^2 s sr)^-1 between 1.8 MeV and 8.1 MeV with a small Admixture of Alpha Particles. Accidental Coincidences become subst","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/Voyager1_CRS_Jupiter_PT15M","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/Voyager1/CRS/Jupiter/PT15M","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/data/VG1-J-CRS-5-SUMM-FLUX-V1.0/AAREADME.TXT","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds%3A%2F%2FPPI%2FVG1-J-CRS-5-SUMM-FLUX-V1.0","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/8637-8y51","keyword":["energeticparticles"],"landingPage":"https://doi.org/10.48322/8637-8y51","license":"https://www.usa.gov/government-works","modified":"2026-09-28","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"PPI"},"theme":["Heliophysics"],"title":"Voyager 1 Jupiter Cosmic Ray Subsystem (CRS) Derived Proton, Ion, and Electron Fluxes, Version 1.0, 15 min Browse Data"},"description":"* Data Set Overview\n* =================\n\n+------------------------------------------------------------------------------------------+\n| Data Set Characteristics          | Value                                                |\n--------------------------------------------------------------------------------------------\n| Instrument Principal Investigator | Rochus E. Vogt                                       |\n| Data Supplier                     | National Space Science Data Center                   |\n| Data Sampling Rate                | Variable (1 hr for FPHA Data, 15 min for all others) |\n| Data Set Start Time               | 1979-02-28T00:00:00.000Z                             |\n| Data Set Stop Time                | 1979-03-21T23:45:00.000Z                             |\n+------------------------------------------------------------------------------------------+\n\nThe following Description has been adapted from NSSDC CRS, 1979:\n\nAs its Name implies, the Cosmic Ray Subsystem (CRS) was designed for Cosmic Ray Studies (Stone et al., 1977b). It consists of two High Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The Detectors have large Geometric Factors (about 0.48 cm^2 sr to 8 cm^2 sr) and long Electronic Time Constants (\u223c24 \u00b5s) for low Power Consumption and good Stability. Normally, the Data are primarily derived from comprehensive (\u03b4E[1], \u03b4E[2] and E) Pulse-Height Information about individual Events. Because of the high Particle Fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on Counting Rates in single Detectors and various Coincidence Rates. In Interplanetary Space, Guard Counters are placed in Anticoincidence with the Primary Detectors to reduce the Background from High-Energy Particles penetrating through the Sides of the Telescopes. These Guard Counters were turned off in the Jovian Magnetosphere when the accidental Anticoincidence Rate became high enough to block a substantial Fraction of the desired Counts. Fortunately, under these Conditions the Spectra were sufficiently soft that the Background, due to penetrating Particles, was small.\n\nThe Data on Proton and Ion Fluxes at Jupiter were obtained with the LET. The Thicknesses of individual Solid-State Detectors in the LET and their Trigger Thresholds were chosen such that, even in the Jovian Magnetosphere, Electrons made, at most, a very minor Contribution to the Proton Counting Rates (Lupton and Stone, 1972). Dead Time Corrections and accidental Coincidences were small (<20%) throughout most of the Magnetotail, but were substantial (>50%) at Flux Maxima within 40 Rj Of Jupiter. Data have been included in this Package for those Periods when the Corrections are less than \u223c50% and can be corrected by the User with the Dead Time appropriate to the Detector (2 \u03b4s to 25 \u03b4s). The high Counting Rates, however, caused some Baseline Shift which may have raised Proton Thresholds significantly. In the Inner Magnetosphere, the L[2] Counting Rate was still useful because it never rolled over. This Rate is due to 1.8 MeV to 13 MeV Protons penetrating L[1] (0.43 cm^2 sr) and >9 MeV Protons penetrating the Shield (8.4 cm^2 sr). For an E^-2 Spectrum, the two Groups would make comparable Contributions, but in the Magnetosphere, for the E^-3 to E^-4 Spectrum above 2.5 MeV (McDonald et al., 1979), the Contribution from Protons penetrating the Shield would be only 3% to 14%.\n\nThe LET L[1]L[2]L[4] and L[1]L[2]L[3] Coincidence-Anticoincidence Rates give the Proton Flux between 1.8 MeV and 8 MeV and 3 MeV to 8 MeV with a small Alpha Particle Contribution (~10^-3). Corrections are required for Dead Time Losses in L[1], accidental L[1]L[2] Coincidences and Anticoincidence Losses from L[4]. Data are given only for Periods when these Corrections are relatively small. In addition to the Rates listed in the Table, the Energy lost in Detectors L[1], L[2] and L[3] was measured for individual Particles. For Protons, this covered the Energy Range from 0.42 MeV to 8.3 MeV. Protons can be identified positively by the \u03b4E versus E Technique, their Spectra obtained and accidental Coincidences greatly reduced. Because of Telemetry Limitations, however, only a small Fraction of the Events could be transmitted, and Statistics become poor unless Pulse-Height Data are averaged over a Period of one Hour.\n\nHET and LET Detectors share the same Data Lines and Pulse-Height Analyzers. Thus, the Telescopes can interfere with one another during Periods of high Counting Rates. To prevent such an Interference and explore different Coincidence Conditions, the Experiment was cycled through four Operating Modes, each 192 s long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] Coincidence Requirements. The TET was cycled through various Coincidence Conditions, including Singles from the Front Detectors. At the Expense of some Time Resolution, this Procedure permitted us to obtain significant Data in the Outer Magnetosphere and excellent Data during the long Passage through the Magnetotail Region.\n\nSome of the published Results from this Experiment required extensive Corrections for Dead Time, accidental Coincidences and Anticoincidences (Vogt et al., 1979a, Vogt et al., 1979b, Schardt et al., 1981, Gehrels, 1981). These Corrections can be applied only on a case-by-case Basis after a careful Study of the Environment and many Self-Consistency Checks. They cannot be applied on a systematic Basis and we have no Computer Programs to do so. Therefore, Data from such Periods are not included in the Data Center Submission. The Scientists on the CRS Team will, however, be glad to consider special Requests if the desired Information can be extracted from the Data.\n\n* Description of the Data\n* =======================\n\n(1) LD1 RATE gives the nominal >0.43 MeV Proton Flux (cm^2 s sr)^-1. This Rate includes all Particles which pass through a 0.8 mg/cm^2 Aluminum Foil and deposits more than 220 keV in a 34.6 \u00b5m Silicon Detector on Voyager 1 (209 keV, 33.9 \u00b5m on Voyager 2) Therefore, Heavy Ions, such as Oxygen and Sulfur are also detected, however, their Contribution is believed to be relatively small. Only a small Percentage of the Pulses in this Detector are larger than the maximum Energy that can be deposited by a Proton. Heavy Ions would produce such large Pulses, unless their Energy Spectra were much steeper than the Proton Spectrum. The true Flux, F(t), can be calculated from the Data:\n\nF(t) = F/(1-1.26x10^-4 F)\n\nand Corrections are small for F<1000 (cm^2 s)^-1.\n\n(2) The LD2 RATE is not suitable for an Absolute Flux Determination and is given in counts per second. The Detector responds to Protons and Ions that penetrate either (a) 0.8 mg/cm^2 Aluminum plus 8.0 mg/cm^2 Silicon and lose at least 200 keV in a 35 \u00b5m Si Detector (1.8 MeV to 13 MeV) or (b) pass through >140 mg/cm^2 Aluminum. For an E^-2 Proton Spectrum, the Contributions from (a) and (b) would be about equal, however, the Proton Spectrum is substantially softer throughout most of the Magnetosphere and the Detector should respond primarily to (a). Dead Time Corrections are given by\n\nR(t) = R/(1-2.55x10^-5 R)\n\nwhere R is the Count Rate in counts per second. Thus, Correction to the supplied data are small for R<4000 counts per second, but become so large in the middle Magnetosphere that the Magnitude of even relative intensity Changes becomes uncertain.\n\n(3) LD L[1].L[2].L[4]. SL COINCIDENCE RATE gives the total Proton Flux (cm^2 s sr)^-1 between 1.8 MeV and 8.1 MeV with a small Admixture of Alpha Particles. 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The Spacecraft Charge may seriously affect the Density Measurements. The Temperature of each Component is, however, independent of the Spacecraft Potential. To obtain the best Estimate of the Electron Density, the Encounter Period is divided into four Regions and four different Analysis Methods are used.\n\n* Parameters\n* ==========\n\n* Derived Parameters\n* ==================\n\n+------------------------------------------------------------+\n| Parameter Characteristics           | Value                |\n--------------------------------------------------------------\n| Sampling Parameter Name             | TIME                 |\n| Sampling Parameter Resolution       | N/A                  |\n| Minimum Sampling Parameter          | UNK                  |\n| Maximum Sampling Parameter          | UNK                  |\n| Sampling Parameter Interval         | UNK                  |\n| Minimum Available Sampling Interval | UNK                  |\n| Data Set Parameter Name             | ELECTRON DENSITY     |\n| Noise Level                         | UNK                  |\n| Data Set Parameter Unit             | CM^-3                |\n+------------------------------------------------------------+\n\nElectron Density: A derived Parameter equaling the Number of Electrons per Unit Volume over a specified Range of Electron Energy. Different Forms of Electron Density are derived distinguished by Method of Derivation (Maxwellian Fit, Method of Moments) or by the some Selection Criteria (i.e., hot Electron and cold Electron Density). In general, if more than one Electron Component is analyzed, either by Moment or Fit, a total Density will be provided which is the Sum of the Electron Densities. If the Electron do not have a Maxwellian Distribution the actual Distribution can be represented as the Sum of several Maxwellians, in which case the Density of each Maxwellian is given.\n\n+------------------------------------------------------------+\n| Parameter Characteristics           | Value                |\n--------------------------------------------------------------\n| Sampling Parameter Name             | TIME                 |\n| Sampling Parameter Resolution       | N/A                  |\n| Minimum Sampling Parameter          | UNK                  |\n| Maximum Sampling Parameter          | UNK                  |\n| Sampling Parameter Interval         | UNK                  |\n| Minimum Available Sampling Interval | UNK                  |\n| Data Set Parameter Name             | ELECTRON TEMPERATURE |\n| Noise Level                         | UNK                  |\n| Data Set Parameter Unit             | EV                   |\n+------------------------------------------------------------+\n\nElectron Temperature: A derived Parameter giving an Indication of the Mean Energy per Electron, assuming the Shape of the Electron Energy Spectrum to be Maxwellian (i.e. highest entropy shape). Given that the Electron Energy Spectrum is not exactly Maxwellian, the Electron Temperature can be defined integrally (whereby the Mean Energy obtained by integrating under the actual Electron Energy Spectrum is set equal to the Integral under a Maxwellian, where the Temperature is a free Parameter for which to solve), or differentially (whereby the Slopes of the actually Electron Energy Spectrum at various Energies are matched to the Slopes of a corresponding Maxwellian). The Temperature Parameter is often qualified with a Range of applicable Energies. Temperatures can be angularly anisotropic. If the Electrons do not have a Maxwellian Distribution the actual Distribution can be represented as the Sum of several Maxwellians, each with a separate Temperature.\n\nElectron Rate: A measured Parameter equaling the Number of Electrons hitting a Particle Detector per specified Accumulation Interval. The counted Electrons may or may not be discriminated as to their Energies (e.g. greater than E1, or between E1 and E2).\n\nElectron Current: A measured Parameter equaling the Rate at which negative Charge is collected by a Particle Detector. The Electrons contributing to this Current may be restricted by Energy. Electrons always have a Charge of 1, so this Quantity corresponds directly to the Electron Rate.\n\n* References\n* ==========\n\n* Zhang, M., J. D. Richardson, and E. C. Sittler, Jr., Voyager 2 electron observations in the magnetosphere of Neptune, J. Geophys. Res., 96, 19,085-19,100, 1991.\n\n* J. W. Belcher, H. S. Bridge, et al., Plasma observations near Neptune: Initial results from Voyager 2, Science, 246, 1478-1483, 1989.\n\n* Scudder, J. D., E. C. Sittler, Jr. and H. S. Bridge, A survey of the plasma electron environment of Jupiter: a view from Voyager, J. Geophys. Res., 86, 8319-8342, 1981.\n\n* Sittler, E. C., Jr., K. W. Ogilvie and R. S. Selesnick, Survey of electrons in the Uranian magnetosphere: Voyager 2 observations, J. Geophys. Res., 92, 15,263-15,281, 1987.","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/Voyager2_PLS_Neptune_PT96S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/Voyager2/PLS/Neptune/PT96S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/data/VG2-N-PLS-5-RDR-ELEMAGSPHERE-96SEC-V1.0/AAREADME.TXT","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds%3A%2F%2FPPI%2FVG2-N-PLS-5-RDR-ELEMAGSPHERE-96SEC-V1.0","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/mk9a-kp53","keyword":["thermalplasma"],"landingPage":"https://doi.org/10.48322/mk9a-kp53","license":"https://www.usa.gov/government-works","modified":"2026-09-28","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"PPI"},"theme":["Heliophysics"],"title":"Voyager 2 Neptune Plasma Science (PLS) Derived Electron Magnetosphere, Version 1.0, 96 s Reduced Data Record (RDR) Data"},"description":"* Data Set Overview\n* =================\n\nThe Electron Spectra are fit using several isotropic Maxwellian Distribution functions to find Electron Parameters. The Spacecraft Charge may seriously affect the Density Measurements. The Temperature of each Component is, however, independent of the Spacecraft Potential. To obtain the best Estimate of the Electron Density, the Encounter Period is divided into four Regions and four different Analysis Methods are used.\n\n* Parameters\n* ==========\n\n* Derived Parameters\n* ==================\n\n+------------------------------------------------------------+\n| Parameter Characteristics           | Value                |\n--------------------------------------------------------------\n| Sampling Parameter Name             | TIME                 |\n| Sampling Parameter Resolution       | N/A                  |\n| Minimum Sampling Parameter          | UNK                  |\n| Maximum Sampling Parameter          | UNK                  |\n| Sampling Parameter Interval         | UNK                  |\n| Minimum Available Sampling Interval | UNK                  |\n| Data Set Parameter Name             | ELECTRON DENSITY     |\n| Noise Level                         | UNK                  |\n| Data Set Parameter Unit             | CM^-3                |\n+------------------------------------------------------------+\n\nElectron Density: A derived Parameter equaling the Number of Electrons per Unit Volume over a specified Range of Electron Energy. Different Forms of Electron Density are derived distinguished by Method of Derivation (Maxwellian Fit, Method of Moments) or by the some Selection Criteria (i.e., hot Electron and cold Electron Density). In general, if more than one Electron Component is analyzed, either by Moment or Fit, a total Density will be provided which is the Sum of the Electron Densities. If the Electron do not have a Maxwellian Distribution the actual Distribution can be represented as the Sum of several Maxwellians, in which case the Density of each Maxwellian is given.\n\n+------------------------------------------------------------+\n| Parameter Characteristics           | Value                |\n--------------------------------------------------------------\n| Sampling Parameter Name             | TIME                 |\n| Sampling Parameter Resolution       | N/A                  |\n| Minimum Sampling Parameter          | UNK                  |\n| Maximum Sampling Parameter          | UNK                  |\n| Sampling Parameter Interval         | UNK                  |\n| Minimum Available Sampling Interval | UNK                  |\n| Data Set Parameter Name             | ELECTRON TEMPERATURE |\n| Noise Level                         | UNK                  |\n| Data Set Parameter Unit             | EV                   |\n+------------------------------------------------------------+\n\nElectron Temperature: A derived Parameter giving an Indication of the Mean Energy per Electron, assuming the Shape of the Electron Energy Spectrum to be Maxwellian (i.e. highest entropy shape). Given that the Electron Energy Spectrum is not exactly Maxwellian, the Electron Temperature can be defined integrally (whereby the Mean Energy obtained by integrating under the actual Electron Energy Spectrum is set equal to the Integral under a Maxwellian, where the Temperature is a free Parameter for which to solve), or differentially (whereby the Slopes of the actually Electron Energy Spectrum at various Energies are matched to the Slopes of a corresponding Maxwellian). The Temperature Parameter is often qualified with a Range of applicable Energies. Temperatures can be angularly anisotropic. If the Electrons do not have a Maxwellian Distribution the actual Distribution can be represented as the Sum of several Maxwellians, each with a separate Temperature.\n\nElectron Rate: A measured Parameter equaling the Number of Electrons hitting a Particle Detector per specified Accumulation Interval. The counted Electrons may or may not be discriminated as to their Energies (e.g. greater than E1, or between E1 and E2).\n\nElectron Current: A measured Parameter equaling the Rate at which negative Charge is collected by a Particle Detector. The Electrons contributing to this Current may be restricted by Energy. Electrons always have a Charge of 1, so this Quantity corresponds directly to the Electron Rate.\n\n* References\n* ==========\n\n* Zhang, M., J. D. Richardson, and E. C. Sittler, Jr., Voyager 2 electron observations in the magnetosphere of Neptune, J. Geophys. Res., 96, 19,085-19,100, 1991.\n\n* J. W. Belcher, H. S. Bridge, et al., Plasma observations near Neptune: Initial results from Voyager 2, Science, 246, 1478-1483, 1989.\n\n* Scudder, J. D., E. C. Sittler, Jr. and H. S. Bridge, A survey of the plasma electron environment of Jupiter: a view from Voyager, J. Geophys. Res., 86, 8319-8342, 1981.\n\n* Sittler, E. C., Jr., K. W. Ogilvie and R. S. Selesnick, Survey of electrons in the Uranian magnetosphere: Voyager 2 observations, J. Geophys. 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Air masses at NAS Wallops Flight Facility were influenced by anthropogenic emissions along the eastern United States compared to the relatively clean marine boundary layer over the ocean off the coast of Natal. As part of the Natal deployment, ozonesondes were launched from the Natal area to provide data on the general state of the atmosphere as well as serve as a frame of reference when compared to the seasonally averaged ozone data from this site.\n\nseasonally averaged ozone data from this site. Sulfur gases and their reaction products play important roles in the chemistry of the global troposphere as well as the biogeochemical sulfur cycle. The sulfur database from CITE 3, and the results from both intercomparison studies and photochemical budget studies, significantly enhanced the ability to evaluate the confidence in the existing databases. Detailed description related to the motivation, implementation, and instrument payloads are available in the CITE 3 overview paper. 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These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the CVP1 mission phase.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-cvp1-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-cvp1-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-29","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER X SREM 5 CVP1 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. 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These are CODMAC Level 5 derived data, and measure the radiation in the spacecraft environment during the Medium Term Plan 15 period of the ESCORT 2 mission phase.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc2-mtp015-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-srem-5-esc2-mtp015-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-29","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P SREM 5 ESCORT 2 MTP015 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. 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Vogt                                       |\n| Data Supplier                     | National Space Science Data Center                   |\n| Data Sampling Rate                | Variable (1 hr for FPHA Data, 15 min for all others) |\n| Data Set Start Time               | 1979-07-03T00:00:00.000Z                             |\n| Data Set Stop Time                | 1979-08-03T23:45:00.000Z                             |\n+------------------------------------------------------------------------------------------+\n\nThe following Description has been adapted from NSSDC CRS, 1979:\n\nAs its Name implies, the Cosmic Ray Subsystem (CRS) was designed for Cosmic Ray Studies (Stone et al., 1977b). It consists of two High Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The Detectors have large Geometric Factors (about 0.48 cm^2 sr to 8 cm^2 sr) and long Electronic Time Constants (\u223c24 \u00b5s) for low Power Consumption and good Stability. Normally, the Data are primarily derived from comprehensive (\u03b4E[1], \u03b4E[2] and E) Pulse-Height Information about individual Events. Because of the high Particle Fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on Counting Rates in single Detectors and various Coincidence Rates. In Interplanetary Space, Guard Counters are placed in Anticoincidence with the Primary Detectors to reduce the Background from High-Energy Particles penetrating through the Sides of the Telescopes. These Guard Counters were turned off in the Jovian Magnetosphere when the accidental Anticoincidence Rate became high enough to block a substantial Fraction of the desired Counts. Fortunately, under these Conditions the Spectra were sufficiently soft that the Background, due to penetrating Particles, was small.\n\nThe Data on Proton and Ion Fluxes at Jupiter were obtained with the LET. The Thicknesses of individual Solid-State Detectors in the LET and their Trigger Thresholds were chosen such that, even in the Jovian Magnetosphere, Electrons made, at most, a very minor Contribution to the Proton Counting Rates (Lupton and Stone, 1972). Dead Time Corrections and accidental Coincidences were small (<20%) throughout most of the Magnetotail, but were substantial (>50%) at Flux Maxima within 40 Rj Of Jupiter. Data have been included in this Package for those Periods when the Corrections are less than \u223c50% and can be corrected by the User with the Dead Time appropriate to the Detector (2 \u03b4s to 25 \u03b4s). The high Counting Rates, however, caused some Baseline Shift which may have raised Proton Thresholds significantly. In the Inner Magnetosphere, the L[2] Counting Rate was still useful because it never rolled over. This Rate is due to 1.8 MeV to 13 MeV Protons penetrating L[1] (0.43 cm^2 sr) and >9 MeV Protons penetrating the Shield (8.4 cm^2 sr). For an E^-2 Spectrum, the two Groups would make comparable Contributions, but in the Magnetosphere, for the E^-3 to E^-4 Spectrum above 2.5 MeV (McDonald et al., 1979), the Contribution from Protons penetrating the Shield would be only 3% to 14%.\n\nThe LET L[1]L[2]L[4] and L[1]L[2]L[3] Coincidence-Anticoincidence Rates give the Proton Flux between 1.8 MeV and 8 MeV and 3 MeV to 8 MeV with a small Alpha Particle Contribution (~10^-3). Corrections are required for Dead Time Losses in L[1], accidental L[1]L[2] Coincidences and Anticoincidence Losses from L[4]. Data are given only for Periods when these Corrections are relatively small. In addition to the Rates listed in the Table, the Energy lost in Detectors L[1], L[2] and L[3] was measured for individual Particles. For Protons, this covered the Energy Range from 0.42 MeV to 8.3 MeV. Protons can be identified positively by the \u03b4E versus E Technique, their Spectra obtained and accidental Coincidences greatly reduced. Because of Telemetry Limitations, however, only a small Fraction of the Events could be transmitted, and Statistics become poor unless Pulse-Height Data are averaged over a Period of one Hour.\n\nHET and LET Detectors share the same Data Lines and Pulse-Height Analyzers. Thus, the Telescopes can interfere with one another during Periods of high Counting Rates. To prevent such an Interference and explore different Coincidence Conditions, the Experiment was cycled through four Operating Modes, each 192 s long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] Coincidence Requirements. The TET was cycled through various Coincidence Conditions, including Singles from the Front Detectors. At the Expense of some Time Resolution, this Procedure permitted us to obtain significant Data in the Outer Magnetosphere and excellent Data during the long Passage through the Magnetotail Region.\n\nSome of the published Results from this Experiment required extensive Corrections for Dead Time, accidental Coincidences and Anticoincidences (Vogt et al., 1979a, Vogt et al., 1979b, Schardt et al., 1981, Gehrels, 1981). These Corrections can be applied only on a case-by-case Basis after a careful Study of the Environment and many Self-Consistency Checks. They cannot be applied on a systematic Basis and we have no Computer Programs to do so. Therefore, Data from such Periods are not included in the Data Center Submission. The Scientists on the CRS Team will, however, be glad to consider special Requests if the desired Information can be extracted from the Data.\n\n* Description of the Data\n* =======================\n\n(1) LD1 RATE gives the nominal >0.43 MeV Proton Flux (cm^2 s sr)^-1. This Rate includes all Particles which pass through a 0.8 mg/cm^2 Aluminum Foil and deposits more than 220 keV in a 34.6 \u00b5m Silicon Detector on Voyager 1 (209 keV, 33.9 \u00b5m on Voyager 2) Therefore, Heavy Ions, such as Oxygen and Sulfur are also detected, however, their Contribution is believed to be relatively small. Only a small Percentage of the Pulses in this Detector are larger than the maximum Energy that can be deposited by a Proton. Heavy Ions would produce such large Pulses, unless their Energy Spectra were much steeper than the Proton Spectrum. The true Flux, F(t), can be calculated from the Data:\n\nF(t) = F/(1-1.26x10^-4 F)\n\nand Corrections are small for F<1000 (cm^2 s)^-1.\n\n(2) The LD2 RATE is not suitable for an Absolute Flux Determination and is given in counts per second. The Detector responds to Protons and Ions that penetrate either (a) 0.8 mg/cm^2 Aluminum plus 8.0 mg/cm^2 Silicon and lose at least 200 keV in a 35 \u00b5m Si Detector (1.8 MeV to 13 MeV) or (b) pass through >140 mg/cm^2 Aluminum. For an E^-2 Proton Spectrum, the Contributions from (a) and (b) would be about equal, however, the Proton Spectrum is substantially softer throughout most of the Magnetosphere and the Detector should respond primarily to (a). Dead Time Corrections are given by\n\nR(t) = R/(1-2.55x10^-5 R)\n\nwhere R is the Count Rate in counts per second. Thus, Correction to the supplied data are small for R<4000 counts per second, but become so large in the middle Magnetosphere that the Magnitude of even relative intensity Changes becomes uncertain.\n\n(3) LD L[1].L[2].L[4]. SL COINCIDENCE RATE gives the total Proton Flux (cm^2 s sr)^-1 between 1.8 MeV and 8.1 MeV with a small Admixture of Alpha Particles. Accidental Coincidences become subst","distribution":[{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/Voyager2_CRS_Jupiter_PT15M","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/Voyager2/CRS/Jupiter/PT15M","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/data/VG2-J-CRS-5-SUMM-FLUX-V1.0/AAREADME.TXT","format":"TXT","mediaType":"text/plain"},{"@type":"dcat:Distribution","downloadURL":"https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds%3A%2F%2FPPI%2FVG2-J-CRS-5-SUMM-FLUX-V1.0","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/frcx-k575","keyword":["energeticparticles"],"landingPage":"https://doi.org/10.48322/frcx-k575","license":"https://www.usa.gov/government-works","modified":"2026-09-29","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"PPI"},"theme":["Heliophysics"],"title":"Voyager 2 Jupiter Cosmic Ray Subsystem (CRS) Derived Proton, Ion, and Electron Fluxes, Version 1.0, 15 min Browse Data"},"description":"* Data Set Overview\n* =================\n\n+------------------------------------------------------------------------------------------+\n| Data Set Characteristics          | Value                                                |\n--------------------------------------------------------------------------------------------\n| Instrument Principal Investigator | Rochus E. Vogt                                       |\n| Data Supplier                     | National Space Science Data Center                   |\n| Data Sampling Rate                | Variable (1 hr for FPHA Data, 15 min for all others) |\n| Data Set Start Time               | 1979-07-03T00:00:00.000Z                             |\n| Data Set Stop Time                | 1979-08-03T23:45:00.000Z                             |\n+------------------------------------------------------------------------------------------+\n\nThe following Description has been adapted from NSSDC CRS, 1979:\n\nAs its Name implies, the Cosmic Ray Subsystem (CRS) was designed for Cosmic Ray Studies (Stone et al., 1977b). It consists of two High Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The Detectors have large Geometric Factors (about 0.48 cm^2 sr to 8 cm^2 sr) and long Electronic Time Constants (\u223c24 \u00b5s) for low Power Consumption and good Stability. Normally, the Data are primarily derived from comprehensive (\u03b4E[1], \u03b4E[2] and E) Pulse-Height Information about individual Events. Because of the high Particle Fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on Counting Rates in single Detectors and various Coincidence Rates. In Interplanetary Space, Guard Counters are placed in Anticoincidence with the Primary Detectors to reduce the Background from High-Energy Particles penetrating through the Sides of the Telescopes. These Guard Counters were turned off in the Jovian Magnetosphere when the accidental Anticoincidence Rate became high enough to block a substantial Fraction of the desired Counts. Fortunately, under these Conditions the Spectra were sufficiently soft that the Background, due to penetrating Particles, was small.\n\nThe Data on Proton and Ion Fluxes at Jupiter were obtained with the LET. The Thicknesses of individual Solid-State Detectors in the LET and their Trigger Thresholds were chosen such that, even in the Jovian Magnetosphere, Electrons made, at most, a very minor Contribution to the Proton Counting Rates (Lupton and Stone, 1972). Dead Time Corrections and accidental Coincidences were small (<20%) throughout most of the Magnetotail, but were substantial (>50%) at Flux Maxima within 40 Rj Of Jupiter. Data have been included in this Package for those Periods when the Corrections are less than \u223c50% and can be corrected by the User with the Dead Time appropriate to the Detector (2 \u03b4s to 25 \u03b4s). The high Counting Rates, however, caused some Baseline Shift which may have raised Proton Thresholds significantly. In the Inner Magnetosphere, the L[2] Counting Rate was still useful because it never rolled over. This Rate is due to 1.8 MeV to 13 MeV Protons penetrating L[1] (0.43 cm^2 sr) and >9 MeV Protons penetrating the Shield (8.4 cm^2 sr). For an E^-2 Spectrum, the two Groups would make comparable Contributions, but in the Magnetosphere, for the E^-3 to E^-4 Spectrum above 2.5 MeV (McDonald et al., 1979), the Contribution from Protons penetrating the Shield would be only 3% to 14%.\n\nThe LET L[1]L[2]L[4] and L[1]L[2]L[3] Coincidence-Anticoincidence Rates give the Proton Flux between 1.8 MeV and 8 MeV and 3 MeV to 8 MeV with a small Alpha Particle Contribution (~10^-3). Corrections are required for Dead Time Losses in L[1], accidental L[1]L[2] Coincidences and Anticoincidence Losses from L[4]. Data are given only for Periods when these Corrections are relatively small. In addition to the Rates listed in the Table, the Energy lost in Detectors L[1], L[2] and L[3] was measured for individual Particles. For Protons, this covered the Energy Range from 0.42 MeV to 8.3 MeV. Protons can be identified positively by the \u03b4E versus E Technique, their Spectra obtained and accidental Coincidences greatly reduced. Because of Telemetry Limitations, however, only a small Fraction of the Events could be transmitted, and Statistics become poor unless Pulse-Height Data are averaged over a Period of one Hour.\n\nHET and LET Detectors share the same Data Lines and Pulse-Height Analyzers. Thus, the Telescopes can interfere with one another during Periods of high Counting Rates. To prevent such an Interference and explore different Coincidence Conditions, the Experiment was cycled through four Operating Modes, each 192 s long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] Coincidence Requirements. The TET was cycled through various Coincidence Conditions, including Singles from the Front Detectors. At the Expense of some Time Resolution, this Procedure permitted us to obtain significant Data in the Outer Magnetosphere and excellent Data during the long Passage through the Magnetotail Region.\n\nSome of the published Results from this Experiment required extensive Corrections for Dead Time, accidental Coincidences and Anticoincidences (Vogt et al., 1979a, Vogt et al., 1979b, Schardt et al., 1981, Gehrels, 1981). These Corrections can be applied only on a case-by-case Basis after a careful Study of the Environment and many Self-Consistency Checks. They cannot be applied on a systematic Basis and we have no Computer Programs to do so. Therefore, Data from such Periods are not included in the Data Center Submission. The Scientists on the CRS Team will, however, be glad to consider special Requests if the desired Information can be extracted from the Data.\n\n* Description of the Data\n* =======================\n\n(1) LD1 RATE gives the nominal >0.43 MeV Proton Flux (cm^2 s sr)^-1. This Rate includes all Particles which pass through a 0.8 mg/cm^2 Aluminum Foil and deposits more than 220 keV in a 34.6 \u00b5m Silicon Detector on Voyager 1 (209 keV, 33.9 \u00b5m on Voyager 2) Therefore, Heavy Ions, such as Oxygen and Sulfur are also detected, however, their Contribution is believed to be relatively small. Only a small Percentage of the Pulses in this Detector are larger than the maximum Energy that can be deposited by a Proton. Heavy Ions would produce such large Pulses, unless their Energy Spectra were much steeper than the Proton Spectrum. The true Flux, F(t), can be calculated from the Data:\n\nF(t) = F/(1-1.26x10^-4 F)\n\nand Corrections are small for F<1000 (cm^2 s)^-1.\n\n(2) The LD2 RATE is not suitable for an Absolute Flux Determination and is given in counts per second. The Detector responds to Protons and Ions that penetrate either (a) 0.8 mg/cm^2 Aluminum plus 8.0 mg/cm^2 Silicon and lose at least 200 keV in a 35 \u00b5m Si Detector (1.8 MeV to 13 MeV) or (b) pass through >140 mg/cm^2 Aluminum. For an E^-2 Proton Spectrum, the Contributions from (a) and (b) would be about equal, however, the Proton Spectrum is substantially softer throughout most of the Magnetosphere and the Detector should respond primarily to (a). Dead Time Corrections are given by\n\nR(t) = R/(1-2.55x10^-5 R)\n\nwhere R is the Count Rate in counts per second. Thus, Correction to the supplied data are small for R<4000 counts per second, but become so large in the middle Magnetosphere that the Magnitude of even relative intensity Changes becomes uncertain.\n\n(3) LD L[1].L[2].L[4]. SL COINCIDENCE RATE gives the total Proton Flux (cm^2 s sr)^-1 between 1.8 MeV and 8.1 MeV with a small Admixture of Alpha Particles. 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