{"after":"WzE3ODg5MTIwNzc5MzQsOC4zMjc3NTEsMSwiMjJjMzU1YzEtZWIyMy00MzU2LWJmNjItYjlhYTQwYzEzNzM2Il0=","results":[{"_score":46.804268,"_sort":[1788916560503,46.804268,3,"da751899-d3a3-4965-b615-8b937f5a2ad0"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Miryam Strautkalns","hasEmail":"mailto:miryam.strautkalns@nasa.gov"},"description":"This chapter discussed some of the algorithmic choices one encounters when designing an IVHM system. While it would be generally desirable to be able to pick a particular set of algorithms for a particular problem, the reality is a bit more complex. Depending on the budget, the performance requirements, the computational constraints, sensor availability, access to historical data, operational and environmental conditions, robustness to changing system configurations, algorithm maintenance needs, etc., no one algorithm will perform best in all situations. Indeed, it is necessary to evaluate these constraints during the algorithm design process and determine the best choice on a case-by-case analysis. The trade-offs between different choices are very real, and sometimes no solution can be found, which means that some of the constraints have to be relaxed. The simplest solution is generally preferred over a more complex one, but it is also important to consider that there is no free lunch. Finally, any health management solution also has to undergo verification and validation (V&V) and, in some cases, certification. Some of these issues are topics of other chapters in this book.","distribution":[{"@type":"dcat:Distribution","description":"Pre_R-405_Chapter_7.pdf","downloadURL":"https://c3.nasa.gov/dashlink/static/media/publication/Pre_R-405_Chapter_7.pdf","format":"PDF","mediaType":"application/pdf","title":"Pre_R-405_Chapter_7.pdf"}],"identifier":"DASHLINK_673","issued":"2013-03-20","keyword":["ames","dashlink","nasa"],"landingPage":"https://c3.nasa.gov/dashlink/resources/673/","modified":"2025-03-31","programCode":["026:029"],"publisher":{"@type":"org:Organization","name":"Dashlink"},"title":"Algorithms and their Impact on Integrated Vehicle Health Management - Chapter 7"},"description":"This chapter discussed some of the algorithmic choices one encounters when designing an IVHM system. While it would be generally desirable to be able to pick a particular set of algorithms for a particular problem, the reality is a bit more complex. 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Prognostics of such components is becoming a very important research field as a result of the need to provide aircraft systems with system level health management information. This paper focuses on a prognostics application for electronics components within avionics systems, and in particular its application to an Isolated Gate Bipolar Transistor (IGBT). This application utilizes the remaining useful life prediction, accomplished by employing the particle filter framework, leveraging data from accelerated aging tests on IGBTs. These tests induced thermal-electrical overstresses by applying thermal cycling to the IGBT devices. 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In-situ state monitoring, including measurements of steady-state voltages and currents, electrical transients, and thermal transients are recorded and used as potential precursors of failure.","distribution_titles":["coarse_mixed_nc.tar.gz","coarse_tet_nc.tar.gz","fine_mixed_nc.tar.gz","fine_tet_nc.tar.gz_part1","fine_tet_nc.tar.gz_part2","medium_mixed_nc.tar.gz","medium_tet_nc.tar.gz"],"harvest_record":"https://catalog.data.gov/harvest_record/5accc3d7-6552-43f7-b65b-fdfe1600d017","harvest_record_raw":"https://catalog.data.gov/harvest_record/5accc3d7-6552-43f7-b65b-fdfe1600d017/raw","has_download":true,"has_spatial":false,"identifier":"DASHLINK_763","keyword":["ames","dashlink","nasa"],"last_harvested_date":"2026-09-09T01:15:48.189310","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":"Dashlink","slug":"towards-prognostics-for-electronics-components","spatial_centroid":null,"spatial_shape":null,"theme":[],"title":"Towards Prognostics for Electronics Components","type":"dataset"},{"_score":11.032864,"_sort":[1788916498429,11.032864,2,"bab33ec7-dad1-40fa-9270-949a29c72e4d"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Miryam Strautkalns","hasEmail":"mailto:miryam.strautkalns@nasa.gov"},"description":"Prognostics is an emerging concept in condition based maintenance (CBM) of critical systems. Along with developing the fundamentals of being able to confidently predict Remaining Useful Life (RUL), the technology calls for fielded applications as it inches towards maturation. This requires a stringent performance evaluation so that the significance of the concept can be fully exploited. Currently, prognostics concepts lack standard definitions and suffer from ambiguous and inconsistent interpretations. This lack of standards is in part due to the varied end-user requirements for different applications, time scales, available information, domain dynamics, etc. to name a few issues. Instead, the research community has used a variety of metrics based largely on convenience with respect to their respective requirements. Very little attention has been focused on establishing a common ground to compare different efforts. This paper surveys the metrics that are already used for prognostics in a variety of domains including medicine, nuclear, automotive, aerospace, and electronics. It also considers other domains that involve prediction-related tasks, such as weather and finance.  Differences and similarities between these domains and health maintenance have been analyzed to help understand what performance evaluation methods may or may not be borrowed. Further, these metrics have been categorized in several ways that may be useful in deciding upon a suitable subset for a\r\nspecific application. Some important prognostic concepts have been defined using a notational framework that enables interpretation of different metrics coherently. Last, but not the \r\nleast, a list of metrics has been suggested to assess critical aspects of RUL predictions before they are fielded in real applications.","distribution":[{"@type":"dcat:Distribution","description":"Chapter_OVG V5.1.pdf","downloadURL":"https://c3.nasa.gov/dashlink/static/media/publication/Chapter_OVG_V5.1.pdf","format":"PDF","mediaType":"application/pdf","title":"Chapter_OVG V5.1.pdf"}],"identifier":"DASHLINK_393","issued":"2011-06-07","keyword":["ames","dashlink","nasa"],"landingPage":"https://c3.nasa.gov/dashlink/resources/393/","modified":"2025-03-31","programCode":["026:029"],"publisher":{"@type":"org:Organization","name":"Dashlink"},"title":"Metrics for Evaluating Performance of Prognostics Techniques"},"description":"Prognostics is an emerging concept in condition based maintenance (CBM) of critical systems. 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It also considers other domains that involve prediction-related tasks, such as weather and finance.  Differences and similarities between these domains and health maintenance have been analyzed to help understand what performance evaluation methods may or may not be borrowed. Further, these metrics have been categorized in several ways that may be useful in deciding upon a suitable subset for a\r\nspecific application. Some important prognostic concepts have been defined using a notational framework that enables interpretation of different metrics coherently. 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Determining the health state of these systems using traditional methods is becoming more difficult as the number of sensors and component interactions grows. Data-driven monitoring techniques have been developed to address these issues by\r\nanalyzing system operations data to automatically characterize normal system behavior. The Inductive Monitoring System is a data-driven system health monitoring software tool that has been successfully applied to several aerospace applications. Inductive Monitoring System uses a data mining technique called clustering to analyze archived system data and characterize\r\nnormal interactions between parameters. This characterization, or model, of nominal operation is stored in a knowledge base that can be used for real-time system monitoring or\r\nfor analysis of archived events. Ongoing and developing Inductive Monitoring System space operations applications include International Space Station flight control, spacecraft vehicle\r\nsystem health management, launch vehicle ground operations, and fleet supportability. As a common thread of discussion this paper will employ the evolution of the Inductive Monitoring\r\nSystem data-driven technique as related to several Integrated Systems Health Management elements. Thematically, the projects listed will be used as case studies. The maturation of Inductive Monitoring System via projects where it has been deployed or is currently being\r\nintegrated to aid in fault detection will be described. The paper will also explain how Inductive Monitoring System can be used to complement a suite of other Integrated System Health Management tools, providing initial fault detection support for diagnosis and recovery.","distribution":[{"@type":"dcat:Distribution","description":"IEEE_Aero_2004_PITEX.pdf","downloadURL":"https://c3.nasa.gov/dashlink/static/media/publication/IEEE_Aero_2004_PITEX.pdf","format":"PDF","mediaType":"application/pdf","title":"IEEE_Aero_2004_PITEX.pdf"}],"identifier":"DASHLINK_669","issued":"2013-02-01","keyword":["ames","dashlink","nasa"],"landingPage":"https://c3.nasa.gov/dashlink/resources/669/","modified":"2025-03-31","programCode":["026:029"],"publisher":{"@type":"org:Organization","name":"Dashlink"},"title":"General Purpose Data-Driven System Monitoring for Space Operations"},"description":"Modern space propulsion and exploration system designs are becoming increasingly\r\nsophisticated and complex. Determining the health state of these systems using traditional methods is becoming more difficult as the number of sensors and component interactions grows. Data-driven monitoring techniques have been developed to address these issues by\r\nanalyzing system operations data to automatically characterize normal system behavior. The Inductive Monitoring System is a data-driven system health monitoring software tool that has been successfully applied to several aerospace applications. Inductive Monitoring System uses a data mining technique called clustering to analyze archived system data and characterize\r\nnormal interactions between parameters. This characterization, or model, of nominal operation is stored in a knowledge base that can be used for real-time system monitoring or\r\nfor analysis of archived events. Ongoing and developing Inductive Monitoring System space operations applications include International Space Station flight control, spacecraft vehicle\r\nsystem health management, launch vehicle ground operations, and fleet supportability. As a common thread of discussion this paper will employ the evolution of the Inductive Monitoring\r\nSystem data-driven technique as related to several Integrated Systems Health Management elements. Thematically, the projects listed will be used as case studies. The maturation of Inductive Monitoring System via projects where it has been deployed or is currently being\r\nintegrated to aid in fault detection will be described. The paper will also explain how Inductive Monitoring System can be used to complement a suite of other Integrated System Health Management tools, providing initial fault detection support for diagnosis and recovery.","distribution_titles":["IEEE_Aero_2004_PITEX.pdf"],"harvest_record":"https://catalog.data.gov/harvest_record/80774f0d-6feb-4677-8f02-748278c09412","harvest_record_raw":"https://catalog.data.gov/harvest_record/80774f0d-6feb-4677-8f02-748278c09412/raw","has_download":true,"has_spatial":false,"identifier":"DASHLINK_669","keyword":["ames","dashlink","nasa"],"last_harvested_date":"2026-09-09T01:14:49.892441","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":"Dashlink","slug":"general-purpose-data-driven-system-monitoring-for-space-operations","spatial_centroid":null,"spatial_shape":null,"theme":[],"title":"General Purpose Data-Driven System Monitoring for Space Operations","type":"dataset"},{"_score":11.858278,"_sort":[1788916373812,11.858278,9,"09334128-0ded-4630-830c-c742ed56c217"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"undefined","hasEmail":"mailto:sdps@oceancolor.gsfc.nasa.gov"},"description":"Title: Unsupervised Anomaly Detection for Liquid-Fueled Rocket Propulsion Health Monitoring.\r\n\r\nAbstract: This article describes the results of applying four unsupervised anomaly detection algorithms to data from two rocket propulsion testbeds. The first testbed uses historical data from the Space Shuttle Main Engine. The second testbed uses data from an experimental rocket engine test stand located at NASA Stennis Space Center. The article describes nine anomalies detected by the four algorithms. The four algorithms use four different definitions of anomalousness. Orca uses a nearest-neighbor approach, defining a point to be an anomaly if its nearest neighbors in the data space are far away from it. The Inductive Monitoring System clusters the training data, and then uses the distance to the nearest cluster as its measure of anomalousness. GritBot learns rules from the training data, and then classifies points as anomalous if they violate these rules. One-class support vector machines map the data into a high-dimensional space in which most of the normal points are on one side of a hyperplane, and then classify points on the other side of the hyperplane as anomalous. Because of these different definitions of anomalousness, different algorithms detect different anomalies. We therefore conclude that it is useful to use multiple algorithms.","distribution":[{"@type":"dcat:Distribution","description":"NASA Ocean Color Web - Algorithm Description Documentation","downloadURL":"https://oceancolor.gsfc.nasa.gov/resources/atbd/","format":"HTML","mediaType":"text/html","title":"View this dataset's algorithm theoretical basis document"},{"@type":"dcat:Distribution","description":"NASA Ocean Color Web - Data Citation Guidelines","downloadURL":"https://oceancolor.gsfc.nasa.gov/resources/how-to-cite/","format":"HTML","mediaType":"text/html","title":"View information related to this dataset"},{"@type":"dcat:Distribution","description":"NASA Ocean Color Web - Data Distribution Site","downloadURL":"https://oceandata.sci.gsfc.nasa.gov/directdataaccess/Level-3%20Mapped/Terra-MODIS/","format":"HTML","mediaType":"text/html","title":"Download this dataset through a directory map"},{"@type":"dcat:Distribution","description":"NASA Ocean Color Web - Processing History","downloadURL":"https://oceancolor.gsfc.nasa.gov/data/reprocessing/","format":"HTML","mediaType":"text/html","title":"View this dataset's processing history"},{"@type":"dcat:Distribution","description":"OB.DAAC OPeNDAP Site for Terra MODIS Standard Mapped Image (SMI) Product","downloadURL":"https://oceandata.sci.gsfc.nasa.gov/opendap/MODIST/L3SMI/","format":"HTML","mediaType":"text/html","title":"Use OPeNDAP to access the dataset's data"}],"identifier":"DASHLINK_171","issued":"2010-09-22","keyword":["ames","dashlink","nasa"],"landingPage":"https://c3.nasa.gov/dashlink/resources/171/","modified":"2025-04-01","programCode":["026:029"],"publisher":{"@type":"org:Organization","name":"Dashlink"},"title":"Unsupervised Anomaly Detection for Liquid-Fueled Rocket Prop..."},"description":"Title: Unsupervised Anomaly Detection for Liquid-Fueled Rocket Propulsion Health Monitoring.\r\n\r\nAbstract: This article describes the results of applying four unsupervised anomaly detection algorithms to data from two rocket propulsion testbeds. The first testbed uses historical data from the Space Shuttle Main Engine. The second testbed uses data from an experimental rocket engine test stand located at NASA Stennis Space Center. The article describes nine anomalies detected by the four algorithms. The four algorithms use four different definitions of anomalousness. Orca uses a nearest-neighbor approach, defining a point to be an anomaly if its nearest neighbors in the data space are far away from it. The Inductive Monitoring System clusters the training data, and then uses the distance to the nearest cluster as its measure of anomalousness. GritBot learns rules from the training data, and then classifies points as anomalous if they violate these rules. One-class support vector machines map the data into a high-dimensional space in which most of the normal points are on one side of a hyperplane, and then classify points on the other side of the hyperplane as anomalous. 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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-193","format":"HTML","mediaType":"text/html","title":"During development the Sku6 mutant roots engage different genes than wild type Col-0 roots either on the ground or in spaceflight."}],"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":["During development the Sku6 mutant roots engage different genes than wild type Col-0 roots either on the ground or in spaceflight."],"harvest_record":"https://catalog.data.gov/harvest_record/670b879b-57bb-4b0c-b2f6-53837d337d8e","harvest_record_raw":"https://catalog.data.gov/harvest_record/670b879b-57bb-4b0c-b2f6-53837d337d8e/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":"2026-09-09T01:12:25.957279","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":"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":14.796691,"_sort":[1788916322386,14.796691,23,"ee184d4b-5040-4d8c-b447-e3682352386b"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"GeneLab Outreach","hasEmail":"mailto:genelab-outreach@lists.nasa.gov"},"description":"Fatigue experiments were conducted on aluminum lap-joint specimens, and lamb wave signals were recorded for each specimen at several time points (i.e., defined as number of cycles in fatigue testing). Signals from piezo actuator-receiver sensor pairs were reported and it was observed that these signals were directly related to the crack lengths developed during fatigue testing. Optical measurements of surface crack lengths are also provided as the ground truth. The data set is split in training and validation to facilitate the application of data-driven methods. \n\nThis data set was generated at Arizona State University by Prof. Yongming Liu, Dr. Tishun Peng, and their collaborators. The data set was used for the Prognostics Health Management (PHM) Data Challenge for the 2019 Conference on Prognostics and Health Management. Other than the data set authors, the following individuals helped put together the 2019 PHM data challenge and make the data set publicly available: Matteo Corbetta and Portia Banerjee (KBR, Inc, NASA Ames), Kurt Doughty (Collins Aerospace), Kai Goebel (PARC), and Scott Clements (Lockheed Martin).\n\nData Set Citation: \nPeng T, He J, Xiang Y, Liu Y, Saxena A, Celaya J, Goebel K. Probabilistic fatigue damage prognosis of lap joint using Bayesian updating. Journal of Intelligent Material Systems and Structures. 2015 May;26(8):965-79.\n\nPublication Citation: \nHe J, Guan X, Peng T, Liu Y, Saxena A, Celaya J, Goebel K. A multi-feature integration method for fatigue crack detection and crack length estimation in riveted lap joints using Lamb waves. Smart Materials and Structures. 2013 Sep 4;22(10):105007.","distribution":[{"@type":"dcat:Distribution","description":"GeneLab Study Page","downloadURL":"https://genelab-data.ndc.nasa.gov/genelab/accession/GLDS-161","format":"HTML","mediaType":"text/html","title":"Rodent Research-3-CASIS: Mouse adrenal gland transcriptomic proteomic and epigenomic data"}],"identifier":"https://data.nasa.gov/api/views/awzu-cpt8","issued":"2023-03-31","keyword":["degradation","ivhm","phm","prognostics","structures"],"landingPage":"https://data.nasa.gov/dataset/fatigue-crack-growth-in-aluminum-lap-joint","license":"https://www.usa.gov/government-works","modified":"2025-05-29","programCode":["026:001"],"publisher":{"@type":"org:Organization","name":"PCoE"},"theme":["Raw Data"],"title":"Fatigue Crack Growth in Aluminum Lap Joint"},"description":"Fatigue experiments were conducted on aluminum lap-joint specimens, and lamb wave signals were recorded for each specimen at several time points (i.e., defined as number of cycles in fatigue testing). Signals from piezo actuator-receiver sensor pairs were reported and it was observed that these signals were directly related to the crack lengths developed during fatigue testing. Optical measurements of surface crack lengths are also provided as the ground truth. The data set is split in training and validation to facilitate the application of data-driven methods. \n\nThis data set was generated at Arizona State University by Prof. Yongming Liu, Dr. Tishun Peng, and their collaborators. The data set was used for the Prognostics Health Management (PHM) Data Challenge for the 2019 Conference on Prognostics and Health Management. Other than the data set authors, the following individuals helped put together the 2019 PHM data challenge and make the data set publicly available: Matteo Corbetta and Portia Banerjee (KBR, Inc, NASA Ames), Kurt Doughty (Collins Aerospace), Kai Goebel (PARC), and Scott Clements (Lockheed Martin).\n\nData Set Citation: \nPeng T, He J, Xiang Y, Liu Y, Saxena A, Celaya J, Goebel K. Probabilistic fatigue damage prognosis of lap joint using Bayesian updating. Journal of Intelligent Material Systems and Structures. 2015 May;26(8):965-79.\n\nPublication Citation: \nHe J, Guan X, Peng T, Liu Y, Saxena A, Celaya J, Goebel K. A multi-feature integration method for fatigue crack detection and crack length estimation in riveted lap joints using Lamb waves. 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The dataset was used for the prognostics challenge competition at the International Conference on Prognostics and Health Management (PHM08). The challenge is still open for the researchers to develop and compare their efforts against the winners of the challenge in 2008.\n\nData sets consist of multiple multivariate time series. Each data set is further divided into training and test subsets. Each time series is from a different aircraft engine \u2013 i.e., the data can be considered to be from a fleet of engines of the same type. Each engine starts with different degrees of initial wear and manufacturing variation which is unknown to the user. This wear and variation is considered normal, i.e., it is not considered a fault condition. There are three operational settings that have a substantial effect on engine performance. These settings are also included in the data. 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The challenge is still open for the researchers to develop and compare their efforts against the winners of the challenge in 2008.\n\nData sets consist of multiple multivariate time series. Each data set is further divided into training and test subsets. Each time series is from a different aircraft engine \u2013 i.e., the data can be considered to be from a fleet of engines of the same type. Each engine starts with different degrees of initial wear and manufacturing variation which is unknown to the user. This wear and variation is considered normal, i.e., it is not considered a fault condition. There are three operational settings that have a substantial effect on engine performance. These settings are also included in the data. The data are contaminated with sensor noise.","distribution_titles":["PHMDC2019_Data.zip"],"harvest_record":"https://catalog.data.gov/harvest_record/8136c6e9-5371-423c-b700-1cf0c2b6f073","harvest_record_raw":"https://catalog.data.gov/harvest_record/8136c6e9-5371-423c-b700-1cf0c2b6f073/raw","has_download":true,"has_spatial":false,"identifier":"https://data.nasa.gov/api/views/nk8v-ckry","keyword":["degradation","phm","prognostics"],"last_harvested_date":"2026-09-09T01:12:01.180225","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":18,"publisher":"PCoE","slug":"phm-2008-challenge","spatial_centroid":null,"spatial_shape":null,"theme":["Raw Data"],"title":"PHM 2008 Challenge","type":"dataset"},{"_score":9.386318,"_sort":[1788916309060,9.386318,1,"6a26ac46-df6f-4f4f-9bf9-e49318d78102"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","accrualPeriodicity":"irregular","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Thomas Morgan","hasEmail":"mailto:thomas.h.morgan@nasa.gov"},"description":"The Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2016-09-30. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. Grains crushing was tested on D0 in February and March. C3 was used for expose from May. Emitter C extractor control voltage got a short in June and from August it was used with tip voltage control only. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-C-COSIMA-3-V4.0, RO-C-COSIMA-3-V5.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file. This was fixed in the version RO-C-COSIMA-3-V3.0.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v6.0","issued":"2021-05-21","keyword":["67p-churyumov-gerasimenko-1-1969-r1","calibration","international-rosetta-mission"],"landingPage":"https://pds.nasa.gov/ds-view/pds/viewDataset.jsp?dsid=RO-C-COSIMA-3-V6.0","license":"http://www.usa.gov/publicdomain/label/1.0/","modified":"2025-07-17","programCode":["026:005"],"publisher":{"@type":"org:Organization","name":"National Aeronautics and Space Administration"},"references":["https://pds.nasa.gov"],"theme":["Earth Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3\n                                      V6.0"},"description":"The Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2016-09-30. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. Grains crushing was tested on D0 in February and March. C3 was used for expose from May. Emitter C extractor control voltage got a short in June and from August it was used with tip voltage control only. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-C-COSIMA-3-V4.0, RO-C-COSIMA-3-V5.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file. This was fixed in the version RO-C-COSIMA-3-V3.0.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/013ac3d4-e5d2-40a6-80db-d9af572db0c6","harvest_record_raw":"https://catalog.data.gov/harvest_record/013ac3d4-e5d2-40a6-80db-d9af572db0c6/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v6.0","keyword":["67p-churyumov-gerasimenko-1-1969-r1","calibration","international-rosetta-mission"],"last_harvested_date":"2026-09-09T01:11:49.060068","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":"rosetta-orbiter-67p-cosima-3-v6-0","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3\n                                      V6.0","type":"dataset"},{"_score":67.82397,"_sort":[1788916189466,67.82397,2,"d1478f07-6cd8-4429-a651-d6ed8b76638c"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Thomas Morgan","hasEmail":"mailto:thomas.h.morgan@nasa.gov"},"description":"The Natural Resource Protection and Child Health Indicators, 2022 Release, is produced in support of the U.S. Millennium Challenge Corporation (MCC) as selection criteria for funding eligibility. The Natural Resource Protection Indicator (NRPI) and Child Health Indicator (CHI) are based on proximity-to-target scores ranging from 0 to 100 (at target). The NRPI covers 220 countries and is calculated based on the weighted average percentage of biomes under protected status. The CHI is a composite index for 195 countries derived from the average of three proximity-to-target scores for access to at least basic water and sanitation together with child mortality rates. The 2022 release includes a consistent time series of NRPI scores for 2010 to 2022 and CHI scores for 2010 to 2020.","identifier":"C2601447797-SEDAC","issued":"2022-12-31","keyword":["earth-science","environmental-impacts","human-dimensions","public-health","sustainability"],"language":["en-US"],"modified":"2025-07-17","programCode":["026:001"],"publisher":{"@type":"org:Organization","name":"SEDAC"},"references":["https://doi.org/10.7927/5bbs-e174","https://doi.org/10.7927/6t8a-es66","https://doi.org/10.7927/7ppx-6m60","https://doi.org/10.7927/80dp-h987","https://doi.org/10.7927/H41Z4299","https://doi.org/10.7927/H45Q4T1N","https://doi.org/10.7927/H46M34RP","https://doi.org/10.7927/H48913TX","https://doi.org/10.7927/H49G5JRZ","https://doi.org/10.7927/H4G73BM2","https://doi.org/10.7927/H4NZ85MP","https://doi.org/10.7927/H4SQ8XGT","https://doi.org/10.7927/r6mv-sv82"],"spatial":"-180.0 -55.0 180.0 90.0","temporal":"2010-01-01T00:00:00Z/2022-12-31T00:00:00Z","theme":["NRMI","geospatial"],"title":"Natural Resource Protection and Child Health Indicators, 2022 Release"},"description":"The Natural Resource Protection and Child Health Indicators, 2022 Release, is produced in support of the U.S. Millennium Challenge Corporation (MCC) as selection criteria for funding eligibility. 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These indicators are successors to the Natural Resource Management Index (NRMI), which was produced from 2006 to 2011 and was based on the same underlying data. Like the NRMI, the Natural Resource Protection Indicator (NRPI) and Child Health Indicator (CHI) are based on proximity-to-target scores ranging from 0 to 100 (at target). The NRPI covers 221 countries and is calculated based on the weighted average percentage of biomes under protected status. The CHI is a composite index for 188 countries derived from the average of three proximity-to-target scores for access to improved sanitation, access to improved water, and child mortality. The 2013 release includes a consistent time series of NRPIs and CHIs for 2006 to 2013.","distribution":[{"@type":"dcat:Distribution","description":"Documentation Page","downloadURL":"http://sedac.ciesin.columbia.edu/data/set/nrmi-natural-resource-protection-child-health-indicators-2013/docs","format":"HTML","mediaType":"text/html","title":"View documentation related to this dataset"},{"@type":"dcat:Distribution","description":"Sample browse graphic of the data set.","downloadURL":"https://sedac.ciesin.columbia.edu/downloads/maps/nrmi/nrmi-natural-resource-protection-child-health-indicators-2013/sedac-logo.jpg","format":"JPEG","mediaType":"image/jpeg","title":"Get a related visualization"},{"@type":"dcat:Distribution","description":"Search results for publications that cite this dataset by its DOI.","downloadURL":"https://scholar.google.com/scholar?q=10.7927%2FH4NZ85MP","format":"HTML","mediaType":"text/html","title":"Google Scholar search results"}],"identifier":"C1000000420-SEDAC","issued":"2013-12-31","keyword":["earth-science","environmental-impacts","human-dimensions","public-health","sustainability"],"language":["en-US"],"modified":"2025-07-17","programCode":["026:001"],"publisher":{"@type":"org:Organization","name":"SEDAC"},"references":["https://doi.org/10.7927/6t8a-es66","https://doi.org/10.7927/H41Z4299","https://doi.org/10.7927/H45Q4T1N","https://doi.org/10.7927/H46M34RP","https://doi.org/10.7927/H48913TX","https://doi.org/10.7927/H49G5JRZ","https://doi.org/10.7927/H4G73BM2","https://doi.org/10.7927/H4SQ8XGT","https://doi.org/10.7927/r6mv-sv82"],"spatial":"-180.0 -55.0 180.0 90.0","temporal":"2006-01-01T00:00:00Z/2012-12-31T00:00:00Z","theme":["NRMI","geospatial"],"title":"Natural Resource Protection and Child Health Indicators, 2013 Release"},"description":"The Natural Resource Protection and Child Health Indicators, 2013 Release, are produced in support of the U.S. Millennium Challenge Corporation as selection criteria for funding eligibility. 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UN SDG 11 is \"make cities and human settlements inclusive, safe, resilient and sustainable\". Improving access to public transport services is integral to achieving the objectives of SDG 11. According to the UN Sustainable Transport, Sustainable Development 2021 Interagency Report, \"only about half the world's urban population have convenient access to public transport\". The report highlights that access to sustainable transport can help reduce food insecurity, boost economies, empower women, and connect people to key health, education, and financial services. As one measure of progress towards SDG 11, the UN has established SDG indicator 11.2.1. The indicator was computed as the proportion of WorldPop gridded population within either 0.5 kilometer walking distance to a low-capacity OpenStreetMap (OSM) public transport point or 1 kilometer walking distance to a high-capacity OSM public transport point. 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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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UN SDG 9 is \"build resilient infrastructure, promote inclusive and sustainable industrialization and foster innovation\". Addressing inadequate access to roads, especially in rural areas, is critical to achieving SDG 9. According to the UN Sustainable Transport, Sustainable Development 2021 Interagency Report, sustainable transportation helps to eliminate poverty, promote food security, improve access to key health services, increase trade competitiveness, and bolster human rights. As one measure of progress towards SDG 9, the UN has established SDG indicator 9.1.1. The indicator was computed as the proportion of WorldPop gridded population within 2 kilometers to an OpenStreetMap (OSM) all-season road. The SDG indicator 9.1.1 data set provides estimates for the proportion of the rural population with access to all-season roads for 209 countries and 45,073 subnational Units. The data set is available at both national and level 2 subnational resolutions.","identifier":"C2762297641-SEDAC","issued":"2023-07-31","keyword":["earth-science","human-dimensions","infrastructure"],"language":["en-US"],"modified":"2025-07-17","programCode":["026:001"],"publisher":{"@type":"org:Organization","name":"SEDAC"},"references":["https://doi.org/10.7927/1a5z-3h71","https://doi.org/10.7927/eavc-4k45","https://doi.org/10.7927/gxnr-sx57","https://doi.org/10.7927/zc4h-hh18"],"spatial":"-180.0 -90.0 180.0 90.0","temporal":"2015-01-01T00:00:00Z/2022-12-31T00:00:00Z","theme":["SDGI","geospatial"],"title":"SDG Indicator 9.1.1: Rural Access Index (RAI), 2023 Release"},"description":"The SDG Indicator 9.1.1: The Rural Access Index (RAI), 2023 Release data set, part of the SDGI collection, measures the proportion of the rural population who live within 2 kilometers of an all-season road for a given statistical area. 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The data set is available at both national and level 2 subnational resolutions.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/ac164c91-75cd-4861-8f29-5ca97590393c","harvest_record_raw":"https://catalog.data.gov/harvest_record/ac164c91-75cd-4861-8f29-5ca97590393c/raw","has_download":false,"has_spatial":true,"identifier":"C2762297641-SEDAC","keyword":["earth-science","human-dimensions","infrastructure"],"last_harvested_date":"2026-09-09T00:54:01.721443","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":13,"publisher":"SEDAC","slug":"sdg-indicator-9-1-1-rural-access-index-rai-2023-release","spatial_centroid":null,"spatial_shape":null,"theme":["SDGI","geospatial"],"title":"SDG Indicator 9.1.1: Rural Access Index (RAI), 2023 Release","type":"dataset"},{"_score":13.775702,"_sort":[1788915171033,13.775702,0,"7dca6f0a-80bd-454e-865a-52fbfd4751c8"],"dcat":{"@type":"dcat:Dataset","accessLevel":"public","bureauCode":["026:00"],"contactPoint":{"@type":"vcard:Contact","fn":"Open Science Data Repository Help Desk","hasEmail":"mailto:arc-dl-osdr-help@mail.nasa.gov"},"description":"Spaceflights significantly impacts astronaut health, causing muscle atrophy, bone loss, cardiovascular deconditioning and immune system dysregulation, especially during long missions. To explore molecular changes, we generated a single-cell RNA sequencing dataset, of 216 samples from 28 mouse organs and tissues under spaceflight and control conditions. Since spaceflight effects closely resemble aspects of aging, we included two age groups (3 and 8 months) to assess age-related influences. Our data revealed that spaceflight drives age-independent systemic changes, primarily affecting tissue remodeling and alterations in cytoskeleton, membrane and extracellular matrix (ECM), particularly in endothelial cells. In contrast, aging has a weaker impact, mainly altering immune regulation in an age-dependent manner. These findings suggest that cytoskeletal and ECM changes may contribute to immune Dysregulation.","distribution":[{"@type":"dcat:Distribution","downloadURL":"http://purl.bioontology.org/ontology/NCBITAXON/10090","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://osdr.nasa.gov/bio/repo/data/missions/SpaceX-16","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://osdr.nasa.gov/bio/repo/data/studies/OSD-918","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://www.ncbi.nlm.nih.gov/geo/query/acc.cgi","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"10.26030/necm-6v21","keyword":["biological-and-physical-sciences","genelab","nasa"],"license":"https://www.usa.gov/government-works","modified":"2026-08-10","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Open Science Data Repository"},"theme":["Biological and Physical Sciences"],"title":"Spaceflight induces systemic effects on extracellular matrix and immune system in different age-stages - Blood data"},"description":"Spaceflights significantly impacts astronaut health, causing muscle atrophy, bone loss, cardiovascular deconditioning and immune system dysregulation, especially during long missions. 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However, the influence of sex hormones on muscle strength in micro- and partial-gravity environments (e.g., the Moon or Mars) is not fully understood. The purpose of this study was to determine the influence of gonadectomy (castration/ovariectomy) on progression of muscle atrophy in both micro- and partial-gravity environments in male and female rats. Male and female Fischer rats (n equals 120) underwent castration/ovariectomy (CAST/OVX) or sham surgery (SHAM) at 11 weeks of age. After 2 weeks of recovery, rats were exposed to hindlimb unloading (0g), partial weight bearing at 40% of normal loading (0.4g, Martian gravity), or normal loading (1.0g) for 28 days. In males, CAST did not exacerbate body weight loss or other metrics of musculoskeletal health. In females, OVX animals tended to have greater body weight loss and greater gastrocnemius loss. Within 7 days of exposure to either microgravity or partial gravity, females had detectable changes to estrous cycle, with greater time spent in low-estradiol phases diestrus and metestrus (\u223c47% in 1g vs. 58% in 0g and 72% in 0.4g animals, P equals 0.005). We conclude that in males testosterone deficiency at the initiation of unloading has little effect on the trajectory of muscle loss. In females, initial low estradiol status may result in greater musculoskeletal losses. This study derives results from Estrous Cycle Monitoring (Cytology).","distribution":[{"@type":"dcat:Distribution","downloadURL":"http://purl.bioontology.org/ontology/NCBITAXON/10116","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://osdr.nasa.gov/bio/repo/data/experiments/OS-891","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://osdr.nasa.gov/bio/repo/data/studies/OSD-617","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"10.26030/k1ez-4x16","keyword":["biological-and-physical-sciences","genelab","nasa"],"license":"https://www.usa.gov/government-works","modified":"2026-08-10","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Open Science Data Repository"},"theme":["Biological and Physical Sciences"],"title":"Influence of gonadectomy on muscle health in micro- and partial-gravity environments in rats (Estrous Cycle Monitoring)"},"description":"Gonadal hormones, such as testosterone and estradiol, modulate muscle size and strength in males and females. 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This N2O gas cell acts as a filter for the effects of N2O present in the atmosphere. The global distribution of N2O is well known, so the N2O signal can be used to detect the presence of clouds in the field of view and to correct the simultaneous CO measurement for systematic errors in the data.SRL-1 Mission GoalsThe MAPS SRL-1 mission took place during Northern Hemisphere Spring when global biomass burning does not typically occur. Some burning may occur for the purpose of clearing the damaged and felled trees in the forests of North America after the rather severe winter. The goals of the MAPS SRL-1 mission are to provide a validated, near-global atlas of the distribution of tropospheric Carbon Monoxide during the mission, and to assess the health status of the MAPS instrument as the mission progresses. SL1 SummaryHigh concentrations of carbon monoxide over the Northern Hemisphere can be seen in measurements made by the Measurement of Air Pollution from Space(MAPS) instrument. 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This N2O gas cell acts as a filter for the effects of N2O present in the atmosphere. The global distribution of N2O is well known, so the N2O signal can be used to detect the presence of clouds in the field of view and to correct the simultaneous CO measurement for systematic errors in the data.SRL-1 Mission GoalsThe MAPS SRL-1 mission took place during Northern Hemisphere Spring when global biomass burning does not typically occur. Some burning may occur for the purpose of clearing the damaged and felled trees in the forests of North America after the rather severe winter. The goals of the MAPS SRL-1 mission are to provide a validated, near-global atlas of the distribution of tropospheric Carbon Monoxide during the mission, and to assess the health status of the MAPS instrument as the mission progresses. SL1 SummaryHigh concentrations of carbon monoxide over the Northern Hemisphere can be seen in measurements made by the Measurement of Air Pollution from Space(MAPS) instrument. These April 1994 measurements, made from the Space Shuttle Endeavour(STS-59), show large sources of air pollution in the lower atmosphere (2 to 10 miles above the surface) over the industrialized Northern Hemisphere.The data that are available from MAPS SRL1 include a 5 by 5 degree gridded box (MAPS_SRL1_5X5_HDF) and a second by second data product (MAPS_SRL1_COSEC_HDF). These data sets are available from the Langley DAAC.","distribution_titles":["Original Metadata"],"harvest_record":"https://catalog.data.gov/harvest_record/018cf225-f0b6-4c5e-9769-6d7d839b5166","harvest_record_raw":"https://catalog.data.gov/harvest_record/018cf225-f0b6-4c5e-9769-6d7d839b5166/raw","has_download":true,"has_spatial":true,"identifier":"10.5067/MAPS_SRL1_CO5X5_HDF","keyword":["earth-science-air-quality-atmosphere-carbon-monoxide","earth-science-atmospheric-chemistry-atmosphere-carbon-and-hydrocarbon-compounds","earth-science-atmospheric-chemistry-atmosphere-nitrogen-compounds"],"last_harvested_date":"2026-09-09T00:44:20.371737","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":"NASA/LARC/SD/ASDC","slug":"measurement-of-air-pollution-from-satellites-maps-space-radar-laboratory-1-srl1-carbon-mon-2a9d2","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"Measurement of Air Pollution from Satellites (MAPS) Space Radar Laboratory - 1 (SRL1) Carbon Monoxide 5 degree by 5 degree data","type":"dataset"},{"_score":11.735914,"_sort":[1788914624754,11.735914,1,"cb25ea06-50c2-4272-90b1-daaff14910d0"],"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":"Payload Checkout 12 (PC12) was an active checkout where a target independent opportunity to perform interactive operations and to request spacecraft pointing was given to all Rosetta payload teams. All Rosetta payload took part in this scenario The Active Payload Checkout 12 ran for 23 consecutive days starting on the 23th April 2010 until the 14th May 2010.During PC12 GIADA performs only a passive test (GD01) similar to the previous Passive Payload Checkouts. This passive test (GD01), which includes standard procedures and full functional verification, was executed by switching on Main and Redundant I/Fs in sequence and executing similar procedures for the two cases. 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.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr5-cruise5-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr5-cruise5-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-07","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 CR5 CRUISE5 V1.0"},"description":"Payload Checkout 12 (PC12) was an active checkout where a target independent opportunity to perform interactive operations and to request spacecraft pointing was given to all Rosetta payload teams. All Rosetta payload took part in this scenario The Active Payload Checkout 12 ran for 23 consecutive days starting on the 23th April 2010 until the 14th May 2010.During PC12 GIADA performs only a passive test (GD01) similar to the previous Passive Payload Checkouts. This passive test (GD01), which includes standard procedures and full functional verification, was executed by switching on Main and Redundant I/Fs in sequence and executing similar procedures for the two cases. 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/40a6d4d3-457d-47e0-a183-9f0186d98944","harvest_record_raw":"https://catalog.data.gov/harvest_record/40a6d4d3-457d-47e0-a183-9f0186d98944/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr5-cruise5-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr5-cruise5-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:43:44.754267","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-cr5-cruise5-v1-0-3f899","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 CR5 CRUISE5 V1.0","type":"dataset"},{"_score":11.000978,"_sort":[1788914523693,11.000978,1,"c74d8dd0-8e35-4efd-9247-aac815aa0d22"],"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 Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2015-06-30. The operations are either expose, storage, spectra, total intensity, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v3.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v3.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-07","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V3.0"},"description":"The Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2015-06-30. The operations are either expose, storage, spectra, total intensity, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/406154a4-d48e-4e76-946b-8a1604780895","harvest_record_raw":"https://catalog.data.gov/harvest_record/406154a4-d48e-4e76-946b-8a1604780895/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v3.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v3.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:42:03.693566","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-cosima-3-v3-0-f22ee","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V3.0","type":"dataset"},{"_score":10.543594,"_sort":[1788914314321,10.543594,1,"57705fcf-2436-497c-8b87-0ef6bab98b43"],"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":"Payload Checkout 8 (PC8) was an active checkout where a target independent opportunity to perform interactive operations and request spacecraft pointing was given to all Rosetta payload t All Rosetta payload took part in this scenario.The Active Payl Checkout 8 ran for 2 consecutive days (05-06 July2008) plus 26 consecutive days starting on the 9th July 2008 until the 1st A 2008. This is approximately twice the allocated time of the ac PC6 scenario that preceded it. PC8 consists of two pha similar to the previous Passive Payload Checkouts the 2nd phas an active test; GD02 is a Non nominal operational configuratio test (Only Impact Sensor operational and cover closed), in GD0 we have successfully tested a non-standard configuration, in was a test to investigate interference from other instruments. Redundant I/Fs in sequence and executing similar procedures fo two cases. GD02, GD03 and GD_INT were executed only on Main I/ 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 normalized 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.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr4a-cruise4a-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr4a-cruise4a-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-07","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 CR4A CRUISE4A V1.0"},"description":"Payload Checkout 8 (PC8) was an active checkout where a target independent opportunity to perform interactive operations and request spacecraft pointing was given to all Rosetta payload t All Rosetta payload took part in this scenario.The Active Payl Checkout 8 ran for 2 consecutive days (05-06 July2008) plus 26 consecutive days starting on the 9th July 2008 until the 1st A 2008. This is approximately twice the allocated time of the ac PC6 scenario that preceded it. PC8 consists of two pha similar to the previous Passive Payload Checkouts the 2nd phas an active test; GD02 is a Non nominal operational configuratio test (Only Impact Sensor operational and cover closed), in GD0 we have successfully tested a non-standard configuration, in was a test to investigate interference from other instruments. Redundant I/Fs in sequence and executing similar procedures fo two cases. GD02, GD03 and GD_INT were executed only on Main I/ 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 normalized 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/16b55e99-cfb2-452e-bef2-495594caef5d","harvest_record_raw":"https://catalog.data.gov/harvest_record/16b55e99-cfb2-452e-bef2-495594caef5d/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr4a-cruise4a-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr4a-cruise4a-v1.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:38:34.321270","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-cr4a-cruise4a-v1-0-0c35f","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 CR4A CRUISE4A V1.0","type":"dataset"},{"_score":3.5011768,"_sort":[1788914178205,3.5011768,2,"67e6ffeb-8035-4ff9-b6bc-9e7fbf2b2775"],"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":"SPAN-E Level 2 Electron Full 3D Spectra Data\n--------------------------------------------\n\nFile Naming Format: psp_swp_spb_sf0_L2_16Ax8Dx32E_YYYYMMDD_v01.cdf\n\nThe SF0 products are the Full 3D Electron spectra from each individual SPAN-E instrument, SPAN-Ae and SPAN-B. Units are in differential energy flux, degrees, and eV. One spectrum comprises decreasing steps in Energy specified by the number in the filename, alternating sweeps in Theta/Deflection, also specified by the number in the filename, and a number of Phi/Anode directions, also specified by the number in the filename. The sample filename above includes 16 Anodes, 8 Deflections, and 32 Energies.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in \"Full Sweep\", normal cadence survey mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B during cruise phase periods when the spacecraft is pointed away from the sun are taken in sunlight.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spb_sf0_16ax8dx32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=PSP_SWP_SPB_SF0_L2_16AX8DX32E&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://doi.org/10.1007/s11214-015-0206-3","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/ParkerSolarProbe_SWEAP_SPAN-B_Level2_Electrons3D_PT14S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/ParkerSolarProbe/SWEAP/SPAN-B/Level2/Electrons3D/PT14S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spb_sf0_16ax8dx32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu/Data.html","format":"HTML","mediaType":"text/html"}],"identifier":"https://doi.org/10.48322/f1vx-0f86","keyword":["instrumentstatus","thermalplasma"],"landingPage":"https://doi.org/10.48322/f1vx-0f86","license":"https://www.usa.gov/government-works","modified":"2026-09-07","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-B Full 3D Electron Spectra, Level 2 (L2), 14 s Data"},"description":"SPAN-E Level 2 Electron Full 3D Spectra Data\n--------------------------------------------\n\nFile Naming Format: psp_swp_spb_sf0_L2_16Ax8Dx32E_YYYYMMDD_v01.cdf\n\nThe SF0 products are the Full 3D Electron spectra from each individual SPAN-E instrument, SPAN-Ae and SPAN-B. Units are in differential energy flux, degrees, and eV. One spectrum comprises decreasing steps in Energy specified by the number in the filename, alternating sweeps in Theta/Deflection, also specified by the number in the filename, and a number of Phi/Anode directions, also specified by the number in the filename. The sample filename above includes 16 Anodes, 8 Deflections, and 32 Energies.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in \"Full Sweep\", normal cadence survey mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B during cruise phase periods when the spacecraft is pointed away from the sun are taken in sunlight.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/ae0b5a12-104a-4889-94c6-1f3c8c0bf62c","harvest_record_raw":"https://catalog.data.gov/harvest_record/ae0b5a12-104a-4889-94c6-1f3c8c0bf62c/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/f1vx-0f86","keyword":["instrumentstatus","thermalplasma"],"last_harvested_date":"2026-09-09T00:36:18.205191","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":"psp-solar-wind-electrons-alphas-and-protons-sweap-span-b-full-3d-electron-spectra-level-2-","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-B Full 3D Electron Spectra, Level 2 (L2), 14 s Data","type":"dataset"},{"_score":3.683281,"_sort":[1788914174528,3.683281,1,"0371a43c-b561-4dd1-b742-98f04649d586"],"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":"SPAN-E Level 2 ELectron Energy Spectra Data\n-------------------------------------------\n\nFile Naming Format: psp_swp_spb_sf1_L2_32E_YYYYMMDD_v01.cdf\n\nThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.\n\nThe larger Theta angles (deflection angles) are artificially enhanced in the \"sf1\" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spb_sf1_32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=PSP_SWP_SPB_SF1_L2_32E&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://doi.org/10.1007/s11214-015-0206-3","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/ParkerSolarProbe_SWEAP_SPAN-B_Level2_ElectronsFullSpectra_PT1.74S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/ParkerSolarProbe/SWEAP/SPAN-B/Level2/ElectronsFullSpectra/PT1.74S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spb_sf1_32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu/Data.html","format":"HTML","mediaType":"text/html"}],"identifier":"https://doi.org/10.48322/db2p-rk78","keyword":["instrumentstatus","thermalplasma"],"landingPage":"https://doi.org/10.48322/db2p-rk78","license":"https://www.usa.gov/government-works","modified":"2026-09-07","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-B Electron Energy Spectra, Level 2 (L2), 1.74 s Data"},"description":"SPAN-E Level 2 ELectron Energy Spectra Data\n-------------------------------------------\n\nFile Naming Format: psp_swp_spb_sf1_L2_32E_YYYYMMDD_v01.cdf\n\nThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.\n\nThe larger Theta angles (deflection angles) are artificially enhanced in the \"sf1\" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. 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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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In each File, following a detailed Description of the Format, the Data consist of a Listing of Counts accumulated in the H10-H27 Spin-Averaged Counting Rates during the Intervals between successive Readouts, organized into Columns as described below. The first four Columns give the Start Time of the Counting Rate Accumulation Period as Fractional Year (to 12 Decimal Places) and as Year since 1900, Day of Year, and Milliseconds of Day at the Start of the Accumulation, followed by one Column giving the Duration of the Accumulation Period in Milliseconds (it is the same for all Rates except H13, which is read out twice in each Accumulation Period, and is thus represented as H13a and H13b, see below and embedded Documentation in each Daily File), and 19 Columns giving the Counts accumulated in that Period for each Rate. All Fields except for the Fractional Year are in Integer Format. The Start Time for H13a is the Time given as the Start Time for the Line, but (to sufficient accuracy) its Accumulation Period is half the Period given under \"Coverage\". Again, to sufficient accuracy, the Start Time for H13b is the Time given plus half the Accumulation Period, and the Accumulation Period for H13b is half the Period given under \"Coverage\". Each Line contains Data for one single Readout of the Rates H10-H12, H13a, H13b, and H14-H27. All Readouts where at least one of the Rates has a Non-fill Value are included. Where Fill does occur it is indicated by -1. Since the Accumulation Period for each Readout is forced to include an Integral Number of Spacecraft Spins in order to produce pure Spin-Averaged Measurements, the Lengths of the Accumulation Periods vary in a Cyclic Manner as the Period of the Telemetry Cycle beats with the Spacecraft Spin Period. At the most common Science Telemetry Rate, 2048 bps, each Rate in this File is Readout on average once every 128 s, except for H13 which is Readout on average twice in every 128 s. At 2048 bps, the Cycle of Accumulation Periods is 132, 132, 120, 132, 132,, 120, 132, etc., seconds. No Noise Removal or Despiking has been done, so Caution must be used in interpreting isolated large Increases or Decreases in the Counting Rates.","distribution":[{"@type":"dcat:Distribution","downloadURL":"http://ufa.esac.esa.int/ufa-sl-server/data-action?PROTOCOL=HTTP&PRODUCT_TYPE=ALL&FILE_NAME=ReadMeHETFullRes.doc&FILE_PATH=%2Fufa%2FHiRes%2FCOSPIN%2FHET","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://ufa.esac.esa.int/ufa-sl-server/data-action?PROTOCOL=HTTP&PRODUCT_TYPE=ALL&FILE_NAME=het_usernotes.pdf&FILE_PATH=%2Fufa%2FHiRes%2Fdoc%2Fcospin","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://ufa.esac.esa.int/ufa/#data","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"http://ufa.esac.esa.int/ufa/#instruments","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/Ulysses_COSPIN_HET_Rates_Omni2_PT128S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/Ulysses/COSPIN/HET/Rates/Omni2/PT128S","format":"BIN","mediaType":"application/octet-stream"}],"identifier":"https://doi.org/10.48322/78qg-8e67","keyword":["energeticparticles"],"landingPage":"https://doi.org/10.48322/78qg-8e67","license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"UlyssesFinalArchive"},"theme":["Heliophysics"],"title":"Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Full Resolution Heavy Ion Counts and Accumulation Times for Spin-Averaged Coincidence Counting Rates, OMNI2 H10-H27, 128 s Data"},"description":"A Directory containing Daily FTP downloadable Files containing Readout-by-Readout Listings of the Counts accumulated in the H1-H27 Spin-Averaged Counting Rates. The Rates H10-H13 are Coincidence Counting Rates corresponding primarily to Heavy Nuclei (Z>2) with Penetrating Power equivalent to Carbon-12 Nuclei in the approximate Energy Ranges 26-36, 44-127, 127-173, and >173 MeV/n, respectively. H14-H27 are single Detector Counting Rates giving, in order, the total Number of Counts above the lowest level Discriminator Thresholds of Detectors D1-D6, K1-K6 (or D7-D12), A (or D13), and the Anti-Coincidence Scintillator S. The single Detector Counting Rates are provided simply to assess the Health of the Detectors and are of little use scientifically. The Naming Convention for the Daily Files is uly_het_full_rat_omni2_YYYDDD.txt, where YYY indicates the three digit Year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and DDD indicates the three digit Day of Year (January 1 = 1). In each File, following a detailed Description of the Format, the Data consist of a Listing of Counts accumulated in the H10-H27 Spin-Averaged Counting Rates during the Intervals between successive Readouts, organized into Columns as described below. The first four Columns give the Start Time of the Counting Rate Accumulation Period as Fractional Year (to 12 Decimal Places) and as Year since 1900, Day of Year, and Milliseconds of Day at the Start of the Accumulation, followed by one Column giving the Duration of the Accumulation Period in Milliseconds (it is the same for all Rates except H13, which is read out twice in each Accumulation Period, and is thus represented as H13a and H13b, see below and embedded Documentation in each Daily File), and 19 Columns giving the Counts accumulated in that Period for each Rate. All Fields except for the Fractional Year are in Integer Format. The Start Time for H13a is the Time given as the Start Time for the Line, but (to sufficient accuracy) its Accumulation Period is half the Period given under \"Coverage\". Again, to sufficient accuracy, the Start Time for H13b is the Time given plus half the Accumulation Period, and the Accumulation Period for H13b is half the Period given under \"Coverage\". Each Line contains Data for one single Readout of the Rates H10-H12, H13a, H13b, and H14-H27. All Readouts where at least one of the Rates has a Non-fill Value are included. Where Fill does occur it is indicated by -1. Since the Accumulation Period for each Readout is forced to include an Integral Number of Spacecraft Spins in order to produce pure Spin-Averaged Measurements, the Lengths of the Accumulation Periods vary in a Cyclic Manner as the Period of the Telemetry Cycle beats with the Spacecraft Spin Period. At the most common Science Telemetry Rate, 2048 bps, each Rate in this File is Readout on average once every 128 s, except for H13 which is Readout on average twice in every 128 s. At 2048 bps, the Cycle of Accumulation Periods is 132, 132, 120, 132, 132,, 120, 132, etc., seconds. No Noise Removal or Despiking has been done, so Caution must be used in interpreting isolated large Increases or Decreases in the Counting Rates.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/b1c1b021-b39b-4ac8-95a8-44262a5232e2","harvest_record_raw":"https://catalog.data.gov/harvest_record/b1c1b021-b39b-4ac8-95a8-44262a5232e2/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/78qg-8e67","keyword":["energeticparticles"],"last_harvested_date":"2026-09-09T00:30:59.099986","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":"UlyssesFinalArchive","slug":"ulysses-cosmic-ray-and-solar-particle-investigation-cospin-high-energy-telescope-het-full--47958","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Full Resolution Heavy Ion Counts and Accumulation Times for Spin-Averaged Coincidence Counting Rates, OMNI2 H10-H27, 128 s Data","type":"dataset"},{"_score":12.657721,"_sort":[1788913814178,12.657721,1,"171c5c9a-11dc-438f-bce8-68681da1dd00"],"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 'Cruise 2' phase. 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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.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr2-cruise2-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-x-gia-2-cr2-cruise2-v1.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER CHECK GIADA 2 CR2 CRUISE2 V1.0"},"description":"This volume contains Experiment Data acquired by GIADA during 'Cruise 2' phase. More in detail it refers to the data provided during the following in-flight tests: 'Passive Payload Checkout n. 1' (PC1) held on 02/03-10-2005; 'Passive Payload Checkout n. 2' (PC2) held on 05/06-03-2006. 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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The dataset includes state-of-health data, suchas temperature and voltage readings, needed for the analysis of the countingdata. The EDR is an intermediate data product derived from the raw datarecords using reversible operations. All higher order data products arederived from the EDR. An automated pipeline is used to process the EDR fromthe raw data records.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.dawn-x-grand-2-edr-cruise-counts-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.dawn-x-grand-2-edr-cruise-counts-v1.0::3.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"DAWN GRAND RAW (EDR) CRUISE CHECKOUT/BACKGROUND COUNTS V1.0"},"description":"The GRaND EDR are a time-ordered collection of gamma rayand neutron counting data and histograms acquired by GRaND during all phasesof the Dawn mission. The dataset includes state-of-health data, suchas temperature and voltage readings, needed for the analysis of the countingdata. The EDR is an intermediate data product derived from the raw datarecords using reversible operations. All higher order data products arederived from the EDR. An automated pipeline is used to process the EDR fromthe raw data records.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/18b6f559-316b-4c6b-bb11-1fe91edc218f","harvest_record_raw":"https://catalog.data.gov/harvest_record/18b6f559-316b-4c6b-bb11-1fe91edc218f/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.dawn-x-grand-2-edr-cruise-counts-v1.0;urn:nasa:pds:context_pds3:data_set:data_set.dawn-x-grand-2-edr-cruise-counts-v1.0::3.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:28:59.615017","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":"dawn-grand-raw-edr-cruise-checkout-background-counts-v1-0-4b6e2","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"DAWN GRAND RAW (EDR) CRUISE CHECKOUT/BACKGROUND COUNTS V1.0","type":"dataset"},{"_score":9.305582,"_sort":[1788913699798,9.305582,1,"eceaa171-ba75-4018-b064-2f727b7cab7c"],"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 Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2016-09-30. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. Grains crushing was tested on D0 in February and March. C3 was used for expose from May. Emitter C extractor control voltage got a short in June and from August it was used with tip voltage control only. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-C-COSIMA-3-V4.0, RO-C-COSIMA-3-V5.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file. This was fixed in the version RO-C-COSIMA-3-V3.0.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v6.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v6.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V6.0"},"description":"The Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains data from 2002-05-29 up to 2016-09-30. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. Grains crushing was tested on D0 in February and March. C3 was used for expose from May. Emitter C extractor control voltage got a short in June and from August it was used with tip voltage control only. 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Since PC13 was scheduled as the final Cruise Phase Checkout, a number of additional payload operations were also executed to close out pending and essential requirements, and/or configure instruments for the upcoming Deep Space Hibernation Phase. Given the importance of this final checkout all Rosetta payload, except Osiris, took part in this scenario The Payload Checkout 13 ran for 9 consecutive days starting on the 1st December 2010 until the 9th December 2010. An RSI passive checkout was also completed on 14th December 2010. The Scenario was covered by dedicated NNO and DSN. During PC13 GIADA performs only a passive test (GD01) similar to the previous Passive Payload Checkouts. This passive test (GD01), which includes standard procedures and full functional verification, was executed by switching on Main and Redundant I/Fs in sequence and executing similar procedures for the two cases. 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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This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/dd36c748-99da-40f3-9643-8142cfb9e66e","harvest_record_raw":"https://catalog.data.gov/harvest_record/dd36c748-99da-40f3-9643-8142cfb9e66e/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v4.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v4.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:18:35.812525","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-cosima-3-v4-0-6781f","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V4.0","type":"dataset"},{"_score":9.544455,"_sort":[1788913041555,9.544455,1,"a591c5a5-582d-4c19-aded-f6c40a573628"],"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 Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains calibrated housekeeping and raw spectra with COSIMA onboard automatic mass calibration for the period from 2002-05-29 up to 2016-01-12. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-C-COSIMA-3-V4.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file. This was fixed in the version RO-C-COSIMA-3-V3.0.","identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v5.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v5.0::1.0","keyword":["__"],"license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"Small Bodies"},"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V5.0"},"description":"The Rosetta COSIMA data contains the operational history of the 72 dust collecting substrates from the installation inside the instrument. This dataset contains calibrated housekeeping and raw spectra with COSIMA onboard automatic mass calibration for the period from 2002-05-29 up to 2016-01-12. The operations are either expose, storage, spectra, peaks, scans, heating, imaging or grain lists. The data is grouped by the substrate and time. Up to the 2014-08 the aim of the data has been the instrument health and operational functionality, not statistically significant substrate background spectra. From 2014-08 onward the D0 substrate set was used to collect dust collected in the vicinity of 67P/CHURYUMOV GERASIMENKO 1 (1969 R1) and dust analysis with TOF-SIMS. From 2014-10-23 onward due to an instrument failure, the SIMS data became scientifically unusable. While other SIMS parameter sets were tested, substrates CF were exposed from mid 2015-12 and C7 from mid 2015-02. End of March 2015 SIMS became operational again. D1 and CD were exposed and SIMS was done with CD, CF and D1. In June TOF-SIMS was done with CF and D1. In July C7 was measured again, while CD was used for expose and TOF-SIMS up to October. D2 was exposed in September. This data set supersedes all previous COSIMA datasets, like RO-C-COSIMA-3-V1.0, RO-C-COSIMA-3-V2.0, RO-C-COSIMA-3-V3.0, RO-C-COSIMA-3-V4.0, RO-CAL-COSIMA-2-V1.0 and RO-CAL-COSIMA-3-V3.0 Also, in the above previous versions, the values of the temperature in the HK data where given in Celsius although Kelvin was written in the description of the table in the FMT file. This was fixed in the version RO-C-COSIMA-3-V3.0.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/f246ad8b-e13b-4729-b799-d09cd01cf914","harvest_record_raw":"https://catalog.data.gov/harvest_record/f246ad8b-e13b-4729-b799-d09cd01cf914/raw","has_download":false,"has_spatial":false,"identifier":"urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v5.0;urn:nasa:pds:context_pds3:data_set:data_set.ro-c-cosima-3-v5.0::1.0","keyword":["__"],"last_harvested_date":"2026-09-09T00:17:21.555414","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-cosima-3-v5-0-f3b88","spatial_centroid":null,"spatial_shape":null,"theme":["Planetary Science"],"title":"ROSETTA-ORBITER 67P COSIMA 3 V5.0","type":"dataset"},{"_score":3.5011768,"_sort":[1788912889443,3.5011768,2,"f0a9e31a-f5fb-44c8-8a17-22a5228c3246"],"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":"SPAN-E Level 2 Electron Full 3D Spectra Data\n--------------------------------------------\n\nFile Naming Format: psp_swp_spa_sf0_L2_16Ax8Dx32E_YYYYMMDD_v01.cdf\n\nThe SF0 products are the Full 3D Electron spectra from each individual SPAN-E instrument, SPAN-Ae and SPAN-B. Units are in differential energy flux, degrees, and eV. One spectrum comprises decreasing steps in Energy specified by the number in the filename, alternating sweeps in Theta/Deflection, also specified by the number in the filename, and a number of Phi/Anode directions, also specified by the number in the filename. The sample filename above includes 16 Anodes, 8 Deflections, and 32 Energies.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in \"Full Sweep\", normal cadence survey mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B during cruise phase periods when the spacecraft is pointed away from the sun are taken in sunlight.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.","distribution":[{"@type":"dcat:Distribution","downloadURL":"ftps://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spa_sf0_16ax8dx32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=PSP_SWP_SPA_SF0_L2_16AX8DX32E&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://doi.org/10.1007/s11214-015-0206-3","format":"HTML","mediaType":"text/html"},{"@type":"dcat:Distribution","downloadURL":"https://helio.data.nasa.gov/dataset/ParkerSolarProbe_SWEAP_SPAN-A_Level2_ElectronsFull3D_PT14S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://hpde.io/NASA/NumericalData/ParkerSolarProbe/SWEAP/SPAN-A/Level2/ElectronsFull3D/PT14S","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://spdf.gsfc.nasa.gov/pub/data/psp/sweap/spe/l2/spa_sf0_16ax8dx32e/","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu","format":"BIN","mediaType":"application/octet-stream"},{"@type":"dcat:Distribution","downloadURL":"https://sweap.cfa.harvard.edu/Data.html","format":"HTML","mediaType":"text/html"}],"identifier":"https://doi.org/10.48322/7j5c-zg65","keyword":["instrumentstatus","thermalplasma"],"landingPage":"https://doi.org/10.48322/7j5c-zg65","license":"https://www.usa.gov/government-works","modified":"2026-09-08","programCode":["026:000"],"publisher":{"@type":"org:Organization","name":"SPDF"},"theme":["Heliophysics"],"title":"PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Full 3D Electron Spectra, Level 2 (L2), 14 s Data"},"description":"SPAN-E Level 2 Electron Full 3D Spectra Data\n--------------------------------------------\n\nFile Naming Format: psp_swp_spa_sf0_L2_16Ax8Dx32E_YYYYMMDD_v01.cdf\n\nThe SF0 products are the Full 3D Electron spectra from each individual SPAN-E instrument, SPAN-Ae and SPAN-B. Units are in differential energy flux, degrees, and eV. One spectrum comprises decreasing steps in Energy specified by the number in the filename, alternating sweeps in Theta/Deflection, also specified by the number in the filename, and a number of Phi/Anode directions, also specified by the number in the filename. The sample filename above includes 16 Anodes, 8 Deflections, and 32 Energies.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in \"Full Sweep\", normal cadence survey mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B during cruise phase periods when the spacecraft is pointed away from the sun are taken in sunlight.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.","distribution_titles":[],"harvest_record":"https://catalog.data.gov/harvest_record/f432746a-bb1d-46d2-913b-59b1e332e25f","harvest_record_raw":"https://catalog.data.gov/harvest_record/f432746a-bb1d-46d2-913b-59b1e332e25f/raw","has_download":true,"has_spatial":false,"identifier":"https://doi.org/10.48322/7j5c-zg65","keyword":["instrumentstatus","thermalplasma"],"last_harvested_date":"2026-09-09T00:14:49.443815","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":"psp-solar-wind-electrons-alphas-and-protons-sweap-span-a-full-3d-electron-spectra-level-2-","spatial_centroid":null,"spatial_shape":null,"theme":["Heliophysics"],"title":"PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Full 3D Electron Spectra, Level 2 (L2), 14 s Data","type":"dataset"},{"_score":3.683281,"_sort":[1788912887601,3.683281,1,"e07f598f-c4f8-42f7-9298-2a61ac608591"],"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":"SPAN-E Level 2 ELectron Energy Spectra Data\n-------------------------------------------\n\nFile Naming Format: psp_swp_spa_sf1_L2_32E_YYYYMMDD_v01.cdf\n\nThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.\n\nThe larger Theta angles (deflection angles) are artificially enhanced in the \"sf1\" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.\n\n* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.\n\n* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: \"We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.\".\n\n* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. 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The units are differential energy flux and eV. The sample filename above includes 32 Energies.\n\nThe larger Theta angles (deflection angles) are artificially enhanced in the \"sf1\" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.\n\nParker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes\n--------------------------------------------------------------------------------\n\nNovember 19, 2019 Initial Data Release\n--------------------------------------\n\nOverview of Measurements\n------------------------\n\nThe SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.\n\nThe prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.\n\nEach SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.\n\nSPAN-E Level 2 Version 01 Release Notes\n---------------------------------------\n\nThe SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of \u00b160\u00b0 in Theta and 240\u00b0 in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.\n\nThis data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.\n\nThe data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)\n\nGeneral Remarks for Version 01 Data\n-----------------------------------\n\nUsers interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.\n\nDue to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.\n\nThe fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.\n\nThe instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.\n\nA general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.\n\nLastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.\n\nSPAN-E Encounter 1 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an instrument commanding error for the two hours surrounding perihelion 1. These and other instrument diagnostic tests are indicated with the QUALITY_FLAG variable in the CDFs.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 1: as a result the microchannel plate, MCP, noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution with this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nSPAN-E Cruise Phase Remarks\n---------------------------\n\nThe cruise mode rates of SPAN-E are greatly reduced compared to the encounter mode rates. When the PSP spacecraft is in a communications slew, the SPAN-B instrument occasionally reaches its maximum allowable operating temperature and is powered off by SWEM.\n\nTiming for the SF1 products in cruise phase is not corrected in v01, and thus it is not advised to use the data at this time for scientific analysis. The typical return of SF0 products is one spectrum out of every 32 survey spectra is returned every 15 minutes or so. One out of every four 27.75 s SF1 spectra is produced every 111 s.\n\nSPAN-E Encounter 2 Remarks\n--------------------------\n\nSPAN-E operated nominally for the majority of the second encounter. Exceptions include instrument diagnostic and health checks and a few instances of corrupted high-energy sweep tables. These tests and corrupted table loads are indicated with the QUALITY_FLAG parameter.\n\nThe mechanical attentuator was engaged for the 8 days around perihelion 2: as a result the MCP noise due to thermal effects and cosmic rays are artificially enhanced and are particularly obvious at higher energies. Exercise caution in this data release if looking for halo electrons when the mechanical attenuator is engaged.\n\nParker Solar Probe SWEAP Rules of the Road\n------------------------------------------\n\nAs part of the development of collaboration with the broader Heliophysics community, the mission has drafted a \"Rules of the Road\" to govern how PSP instrument data are to be used.\n\n* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.\n\n* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. 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The release of cytokines and chemokines by cultured alveolar epithelial cells and monocytes stimulated by PM2.5 samples collected over time periods as short as 30 minutes was detectable and responsive to PM2.5 samples of different chemical compositions. Results obtained from the bioassay system in both cell types were reproducible and of sufficient precision to allow detection of differences between PM2.5 samples collected over short time intervals. \r\n\r\nThe Baltimore Supersite collected high-quality ambient air quality measurements with unprecedented temporal resolution at industrially influenced urban sites from August of 2001 to November of 2002 with two intensive measurement campaigns. A data set of project results was constructed to take advantage of advanced multivariate statistical techniques. 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This data was obtained between May 1999 and December 2006 at the Fresno supersite. A multiwavelength aethalometer (Model AE30S) operated at the Fresno supersite from May 12, 1999 to December 31, 2006. The collected aerosol sample was illuminated with light from seven light emitting diodes at wavelengths of 370, 470, 520, 590, 660, 880, and 950 nm. Aerosol samples were collected for five minute periods. The air sample was collected through a sharp cut size-selective cyclone to limit the size of particles to aerodynamic diameters of 2.5 um and less. The concentration of black carbon corresponded to the 880 nm measurement. The black carbon equivalents at the other six wavelengths were also determined.\r\n\r\nThe Fresno Supersite is one of several Supersites established in urban areas within the United States by the EPA to better understand the measurement, sources, and health effects of suspended particulate matter (PM). 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This data set contains measurements taken from six meteorological instruments operated at the Fresno supersite from May 24, 2000 to December 31, 2006. The ambient temperature was measured by a Met One Instruments aspirated thermistor, Model 060A-2. The barometric pressure was measured by a Met One pressure transducer, Model 090D. The relative humidity was measured by a Met One aspirated thin film capacitor, Model 083V. The solar radiation was measured by a LI-COR Inc. pyranometer, Model LI-200SA. The wind speed was measured by a Met One Instruments 3-cup anemometer, Model 010-SC. The wind direction was measured by a Met One Instruments High-Sensitivity wind vane, Model 025-5C. All six instruments reported 5 minute samples.\r\n\r\nThe Fresno Supersite is one of several Supersites established in urban areas within the United States by the EPA to better understand the measurement, sources, and health effects of suspended particulate matter (PM). 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The overall objective of the Los Angeles Super Site in Southern California Particle Center and Supersite (SCPCS) is to conduct monitoring and research that contributes to a better understanding of the measurement, sources, size distribution, chemical composition and physical state, spatial and temporal variability, and linkages to health effects of airborne particulate matter in the Los Angeles Basin.\r\n\r\nThe U.S. EPA Particulate Matter (PM) Super Sites Program was an ambient air monitoring research program designed to provide information of value to the atmospheric sciences, and human health and exposure research communities. 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The main collaborators were the Environmental Technology Centre of the Environmental Protection Service and the Chemistry Department of the University of Toronto. The breadth of the study also necessitated that many other organizations provide support, such as the Greater Vancouver Regional District, the Pacific Environmental Science Centre and the Ontario Ministry of the Environment. North American Research Strategy for Tropospheric Ozone (NARSTO), which has since disbanded, was a public/private partnership, whose membership spanned across government, utilities, industry, and academe throughout Mexico, the United States, and Canada. The primary mission was to coordinate and enhance policy-relevant scientific research and assessment of tropospheric pollution behavior; activities provide input for science-based decision-making and determination of workable, efficient, and effective strategies for local and regional air-pollution management. 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Through targeted airborne and ground-based observations, DISCOVER-AQ enabled more effective use of current and future satellites to diagnose ground level conditions influencing air quality.\n\nDISCOVER-AQ employed two NASA aircraft, the P3-B and King Air, with the P-3B completing in-situ spiral profiling of the atmosphere (aerosol properties, meteorological variables, and trace gas species). The King Air conducted both passive and active remote sensing of the atmospheric column extending below the aircraft to the surface. Data from an existing network of surface air quality monitors, AERONET sun photometers, Pandora UV/vis spectrometers and model simulations were also collected. Further, DISCOVER-AQ employed many surface monitoring sites, with measurements being made on the ground, in conjunction with the aircraft. The B200 and P-3B conducted flights in Baltimore-Washington, D.C. in 2011, Houston, TX in 2013, San Joaquin Valley, CA in 2013, and Denver, CO in 2014. These regions were targeted due to being in violation of the National Ambient Air Quality Standards (NAAQS).\n\nThe first objective of DISCOVER-AQ was to determine and investigate correlations between surface measurements and satellite column observations for the trace gases ozone (O3), nitrogen dioxide (NO2), and formaldehyde (CH2O) to understand how satellite column observations can diagnose surface conditions. DISCOVER-AQ also had the objective of using surface-level measurements to understand how satellites measure diurnal variability and to understand what factors control diurnal variability. Lastly, DISCOVER-AQ aimed to explore horizontal scales of variability, such as regions with steep gradients and urban plumes.","distribution_titles":["Original Metadata"],"harvest_record":"https://catalog.data.gov/harvest_record/2acf6e52-6205-415b-b2ef-0e3234ba03a1","harvest_record_raw":"https://catalog.data.gov/harvest_record/2acf6e52-6205-415b-b2ef-0e3234ba03a1/raw","has_download":true,"has_spatial":true,"identifier":"10.5067/ASDC/SUBORBITAL/DISCOVERAQ_Texas_Ground_Ancillary_Analysis_Data_1","keyword":["earth-science-aerosols-atmosphere-aerosol-extinction","earth-science-altitude-atmosphere-planetary-boundary-layer-height","earth-science-atmospheric-chemistry-atmosphere-carbon-and-hydrocarbon-compounds","earth-science-atmospheric-chemistry-atmosphere-nitrogen-compounds","earth-science-atmospheric-chemistry-atmosphere-oxygen-compounds","earth-science-atmospheric-temperature-atmosphere-surface-temperature","earth-science-atmospheric-water-vapor-atmosphere-water-vapor-indicators","earth-science-precipitation-atmosphere-liquid-precipitation"],"last_harvested_date":"2026-09-09T00:01:17.934917","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/LARC/SD/ASDC","slug":"discover-aq-texas-deployment-analysis-and-ancillary-ground-site-data","spatial_centroid":null,"spatial_shape":null,"theme":["Earth Science"],"title":"DISCOVER-AQ Texas Deployment Analysis and Ancillary Ground Site Data","type":"dataset"}],"sort":"last_harvested_date"}