[{"type":"catalog","name":"model_regions_plasmas_mms_2019","id":"sharedcatalog_22","created":"2021-12-08T07:01:12","description":"Prediction from:\nBreuillard Hugo et al. - Automatic Classification of Plasma Regions in Near-Earth Space With Supervised Machine Learning: Application to Magnetospheric Multi Scale 20162019 Observations - 2020\nhttp:\/\/dx.doi.org\/10.3389\/fspas.2020.00055\n\nGenerated by the CDPP\/AMDA team by using:\n* 'MMS1\/FGM\/survey' and 'MMS1\/FPI\/fast mode\/DIS : ions' datasets published in AMDA\n* Pre-trained model publicly available in Gitlab: https:\/\/gitlab.com\/aidaspace\/notebooks_aida\/-\/tree\/master\/04_sitl_classification_region\n\n** This catalog has not been validated by the corresponding author. Please, use it with care. **\n\nThe predicted region is given by \"classes\" with the following mapping: \n* 0 : SW\n* 1 : FS\n* 2 : BS\n* 3 : MSH\n* 4 : MP\n* 5 : BL\n* 6 : MSP\n* 7 : PS\n* 8 : PSBL\n* 9 : LOBE\n","nbIntervals":"12691","surveyStart":"2019-01-01T00:00:04","surveyStop":"2019-12-31T23:56:37","sharedDate":"2021-12-08T07:04:52+00:00"},{"type":"catalog","name":"model_regions_plasmas_cluster_2005","id":"sharedcatalog_23","created":"2021-12-08T08:05:10","description":"Prediction from:\nBreuillard Hugo et al. - Automatic Classification of Plasma Regions in Near-Earth Space With Supervised Machine Learning: Application to Magnetospheric Multi Scale 20162019 Observations - 2020\nhttp:\/\/dx.doi.org\/10.3389\/fspas.2020.00055\n\nGenerated by the CDPP\/AMDA team by using:\n* 'Cluster 1\/FGM\/4 sec' and 'Cluster 1\/CIS-HIA\/ion moments' datasets published in AMDA\n* Pre-trained model publicly available in Gitlab: https:\/\/gitlab.com\/aidaspace\/notebooks_aida\/-\/tree\/master\/04_sitl_classification_region\n\n** This catalog has not been validated by the corresponding author. Please, use it with care. **\n\nThe predicted region is given by \"classes\" with the following mapping: \n* 0 : SW\n* 1 : FS\n* 2 : BS\n* 3 : MSH\n* 4 : MP\n* 5 : BL\n* 6 : MSP\n* 7 : PS\n* 8 : PSBL\n* 9 : LOBE\n","nbIntervals":"27244","surveyStart":"2005-01-01T00:00:04","surveyStop":"2005-12-31T23:55:52","sharedDate":"2021-12-08T08:19:41+00:00"},{"type":"catalog","name":"Dst_Li2020","id":"sharedcatalog_36","created":"2022-10-18T10:47:53.000000","description":"Catalogue from Dongni Li and Shuo Yao 2020 ApJ 891 79\nhttps:\/\/doi.org\/10.3847\/1538-4357\/ab7197\n\nStart Time corresponds to the Main phase start time\nStop Time corresponds to the Recovery phase end time\n\nColumns are:\n- ICME start time\n- Magnetic clouds? (Y)es or (N)o\n- Carbon Cold? (Y)es or (N)o\n- Helium enhanced? (Y)es or (N)o\n- Magnetic field z component minimum (nT)\n- Dst index minimum time\n- Dst minimum value (nT)\n\nOriginal catalogue is at https:\/\/cfn-live-content-bucket-iop-org.s3.amazonaws.com\/journals\/0004-637X\/891\/1\/79\/revision1\/apjab7197t2_mrt.txt?AWSAccessKeyId=AKIAYDKQL6LTV7YY2HIK&Expires=1666616600&Signature=nsKncw9FH%2Fdyh67B6nEmW9Su5b8%3D","nbIntervals":"95","surveyStart":"1998-03-04T12:30:00","surveyStop":"2011-08-08T08:30:00","sharedDate":"2022-10-18T13:06:58+00:00"},{"type":"catalog","name":"Dst_Lu2016","id":"sharedcatalog_37","created":"2022-10-18T11:58:55.000000","description":"Catalogue from Lu et al., PSS, Volume 120, January 2016, p.48-55\nhttps:\/\/doi.org\/10.1016\/j.pss.2015.11.004\n\nThe start time is determined by checking the significant decrease of Dst value from a relatively stable state. The end time is determined by checking the Dst value rising above \u221250 nT after the minimum Dst.\n\nColumn is:\n- Dst minimum value (nT)","nbIntervals":"80","surveyStart":"1995-03-26T05:00:00","surveyStop":"2014-02-19T16:00:00","sharedDate":"2022-10-18T13:07:13+00:00"},{"type":"catalog","name":"Dst_Ji2012","id":"sharedcatalog_38","created":"2022-10-18T12:59:13.000000","description":"Catalogue from Ji et al., 2012  J. Geophys. Res., 117, A03209\nhttps:\/\/doi.org\/10.1029\/2011JA016872\n\nThe start times are defined as the times when there were noticeable decrease of Dst values after the corresponding interplanetary shocks (Storm Sudden Commencements, SSC) by checking the variation of the solar wind data (velocity, density, and magnetic field). The end times are defined as the times when the Dst just recovers to above \u221250 nT after the minimum Dst.\n\nDst min values are in nT.\nAbbreviations are sMC, MC preceded by a fast shock; SH, sheath field; CIR, corotating interaction region; nonMC, ICME that does not show the signature of a magnetic cloud.","nbIntervals":"63","surveyStart":"1998-02-17T12:00:00","surveyStop":"2006-12-16T03:00:00","sharedDate":"2022-10-18T13:07:27+00:00"},{"type":"catalog","name":"THEMIS_MPcrossings_2007-2016_V1","id":"sharedcatalog_39","created":"2022-10-21T15:17:07.000000","description":"THEMIS magnetopause crossings, including time and location of each THEMIS between 2007 and 2016 (inclusive).\n\nArchived data for the manuscript \u201cDo statistical models capture the dynamics of the magnetopause during sudden magnetospheric compressions?\u201d by Staples et al., 2020, Journal of Geophysical Research: Space Physics.\nhttps:\/\/doi.org\/10.1029\/2019JA027289\n\nData can also be found at https:\/\/zenodo.org\/record\/3700504\n\nParameters are:\n- time of each THEMIS probe crossing (start=stop)\n- X coordinate of THEMIS crossing location (GSE) (Re)\n- Y coordinate of THEMIS crossing location (GSE) (Re)\n- Z coordinate of THEMIS crossing location (GSE) (Re)\n- X coordinate of THEMIS crossing location (GSM) (Re)\n- Y coordinate of THEMIS crossing location (GSM) (Re)\n- Z coordinate of THEMIS crossing location (GSM) (Re)\n- THEMIS probe which crosses the magnetopause","nbIntervals":"33946","surveyStart":"2007-04-08T21:46:41","surveyStop":"2016-11-12T12:11:59","sharedDate":"2022-10-21T15:20:00+00:00"},{"type":"catalog","name":"EDR_catalogue","id":"sharedcatalog_40","created":"2023-09-06T14:44:01.000000","description":"from https:\/\/zenodo.org\/record\/8319481\nList of Electron Diffusion Regions (EDR) during the phases 1a & 1b of the NASA\/MMS mission.\nEDR from Lenouvel_et_al._[2021] and Lenouvel_(unpublished) were detected with two distinct machine learning algorithms. The first algorithm (MLP) is detailed in Lenouvel_et_al._[2021]. Both algorithms (MLP and CNN) are described in Q. Lenouvel's PhD manuscript and in \"Advanced Methods for Analyzing In-Situ Observations of Magnetic Reconnection\" submitted to Space Science Reviews by Hasegawa et al..\nFor completeness, other EDR events reported in the literature are added to the list. Note that some events were observed by other MMS spacecraft at slightly different times.","nbIntervals":"72","surveyStart":"2015-09-08T11:01:20","surveyStop":"2017-01-27T12:05:43","sharedDate":"2023-09-06T14:45:43+00:00"},{"type":"catalog","name":"LPP_bowshock_list","id":"sharedcatalog_43","created":"2024-02-08T11:31:00.000000","description":"Bow shock crossings observed by MMS obtained from ML algorithm at LPP. The start\/stop times correspond to +-1min from the original central time. Following columns are X Y Z R theta phi","nbIntervals":"2025","surveyStart":"2015-10-07T11:18:00","surveyStop":"2021-05-24T01:29:00","sharedDate":"2024-02-08T11:35:54+00:00"},{"type":"catalog","name":"MMS_Lalti_BScrossings_2015_2020","id":"sharedcatalog_44","created":"2024-02-14T14:08:28.000000","description":"Bowshock crossings by MMS from Lalti et al., 2022 https:\/\/doi.org\/10.1029\/2022JA030454\nThis catalogue and the overview plots are at https:\/\/doi.org\/10.5281\/zenodo.6343989\nThe start\/stop times correspond to +-1min from the original central time. Following columns are:\nburst_start\nburst_end\nBx_us\nBy_us\nBz_us\nB_us_abs\nsB_us_abs\nDelta_theta_B\nNi_us\nTi_us\nVx_us\nVy_us\nVz_us\nbeta_i_us\nPdyn_us\nthBn\nsthBn\nnormal_x\nnormal_y\nnormal_z\nMA\nsMA\nMf\nsMf\nB_jump\nNi_jump\nTe_jump\npos_x\npos_y\npos_z\nsc_sep_min\nsc_sep_max\nsc_sep_mean\nTQF","nbIntervals":"2797","surveyStart":"2015-10-07T11:19:10","surveyStop":"2020-12-12T11:47:40","sharedDate":"2024-02-14T14:09:40+00:00"},{"type":"catalog","name":"THEMIS_MPcrossings_2007-2016_V2","id":"sharedcatalog_45","created":"2024-02-14T14:36:08.000000","description":"THEMIS magnetopause crossings, including time and location of each THEMIS between 2007 and 2016 (inclusive).\n\nArchived data for the manuscript \u201cDo statistical models capture the dynamics of the magnetopause during sudden magnetospheric compressions?\u201d by Staples et al., 2020, Journal of Geophysical Research: Space Physics.\nhttps:\/\/doi.org\/10.1029\/2019JA027289\n\nThis catalogue is also at https:\/\/zenodo.org\/records\/10655312\nNote this is the Version 2 without duplicated records\n\nParameters are:\n- time of each THEMIS probe crossing (start=stop)\n- X coordinate of THEMIS crossing location (GSE) (Re)\n- Y coordinate of THEMIS crossing location (GSE) (Re)\n- Z coordinate of THEMIS crossing location (GSE) (Re)\n- X coordinate of THEMIS crossing location (GSM) (Re)\n- Y coordinate of THEMIS crossing location (GSM) (Re)\n- Z coordinate of THEMIS crossing location (GSM) (Re)\n- THEMIS probe which crosses the magnetopause","nbIntervals":"29141","surveyStart":"2007-04-08T21:46:41","surveyStop":"2016-11-12T12:11:59","sharedDate":"2024-02-14T14:39:15+00:00"},{"type":"catalog","name":"TailXing_opportunities_Europa","id":"sharedcatalog_27","created":"2022-02-23T12:31:49","description":" Generated by the CDPP team from TailXing_opportunities_v12.csv\n Times for the expected footprint tail crossings by Juno, according to magnetic model JRM09\n Version 12: Put together on Apr 2021, Vincent Hue, SwRI. Contact vhue@swri.org for any suggestions\/improvements\n Kernel list:\n  - naif0012.tls\n  - JNO_SCLKSCET.00112.tsc\n  - jup230.bsp\n  - rbsp_general010.tf\n  - spk_ref_180429_210731_180509.bsp\n  - spk_rec_110805_111026_120302.bsp\n  - spk_rec_111026_120308_120726.bsp\n  - spk_rec_120308_120825_121109.bsp\n  - spk_rec_120825_130515_130708.bsp\n  - spk_rec_130515_131005_151210.bsp\n  - spk_rec_131005_131014_131101.bsp\n  - spk_rec_131014_131114_140222.bsp\n  - spk_rec_131114_140918_141208.bsp\n  - spk_rec_140903_151003_160118.bsp\n  - spk_rec_151003_160312_160418.bsp\n  - spk_rec_160312_160522_160614.bsp\n  - spk_rec_160522_160729_160909.bsp\n  - spk_rec_160729_160923_161027.bsp\n  - spk_rec_160923_161115_161121.bsp\n  - spk_rec_161115_170106_170113.bsp\n  - spk_rec_170106_170228_170307.bsp\n  - spk_rec_170228_170422_170427.bsp\n  - spk_rec_170422_170608_170621.bsp\n  - spk_rec_170608_170728_170803.bsp\n  - spk_rec_170728_170918_170922.bsp\n  - spk_rec_170918_171121_171127.bsp\n  - spk_rec_171121_180113_180117.bsp\n  - spk_rec_180113_180307_180312.bsp\n  - spk_rec_180307_180429_180504.bsp\n  - spk_rec_180429_180621_180626.bsp\n  - spk_rec_180620_180812_180821.bsp\n  - spk_rec_180812_181004_181011.bsp\n  - spk_rec_181004_181126_181205.bsp\n  - spk_rec_181126_190118_190124.bsp\n  - spk_rec_190118_190312_190319.bsp\n  - spk_rec_190312_190504_190509.bsp\n  - spk_rec_190504_190626_190627.bsp\n  - spk_rec_190626_190817_190822.bsp\n  - spk_rec_190817_191010_191022.bsp\n  - spk_rec_191010_191201_191210.bsp","nbIntervals":"218","surveyStart":"2016-08-27T12:15:21","surveyStop":"2025-08-15T20:48:57","sharedDate":"2022-02-23T12:35:52+00:00"},{"type":"catalog","name":"TailXing_opportunities_Ganymede","id":"sharedcatalog_28","created":"2022-02-23T12:32:03","description":" Generated by the CDPP team from TailXing_opportunities_v12.csv\n Times for the expected footprint tail crossings by Juno, according to magnetic model JRM09\n Version 12: Put together on Apr 2021, Vincent Hue, SwRI. Contact vhue@swri.org for any suggestions\/improvements\n Kernel list:\n  - naif0012.tls\n  - JNO_SCLKSCET.00112.tsc\n  - jup230.bsp\n  - rbsp_general010.tf\n  - spk_ref_180429_210731_180509.bsp\n  - spk_rec_110805_111026_120302.bsp\n  - spk_rec_111026_120308_120726.bsp\n  - spk_rec_120308_120825_121109.bsp\n  - spk_rec_120825_130515_130708.bsp\n  - spk_rec_130515_131005_151210.bsp\n  - spk_rec_131005_131014_131101.bsp\n  - spk_rec_131014_131114_140222.bsp\n  - spk_rec_131114_140918_141208.bsp\n  - spk_rec_140903_151003_160118.bsp\n  - spk_rec_151003_160312_160418.bsp\n  - spk_rec_160312_160522_160614.bsp\n  - spk_rec_160522_160729_160909.bsp\n  - spk_rec_160729_160923_161027.bsp\n  - spk_rec_160923_161115_161121.bsp\n  - spk_rec_161115_170106_170113.bsp\n  - spk_rec_170106_170228_170307.bsp\n  - spk_rec_170228_170422_170427.bsp\n  - spk_rec_170422_170608_170621.bsp\n  - spk_rec_170608_170728_170803.bsp\n  - spk_rec_170728_170918_170922.bsp\n  - spk_rec_170918_171121_171127.bsp\n  - spk_rec_171121_180113_180117.bsp\n  - spk_rec_180113_180307_180312.bsp\n  - spk_rec_180307_180429_180504.bsp\n  - spk_rec_180429_180621_180626.bsp\n  - spk_rec_180620_180812_180821.bsp\n  - spk_rec_180812_181004_181011.bsp\n  - spk_rec_181004_181126_181205.bsp\n  - spk_rec_181126_190118_190124.bsp\n  - spk_rec_190118_190312_190319.bsp\n  - spk_rec_190312_190504_190509.bsp\n  - spk_rec_190504_190626_190627.bsp\n  - spk_rec_190626_190817_190822.bsp\n  - spk_rec_190817_191010_191022.bsp\n  - spk_rec_191010_191201_191210.bsp","nbIntervals":"197","surveyStart":"2016-08-27T12:12:24","surveyStop":"2025-08-15T21:19:27","sharedDate":"2022-02-23T12:36:04+00:00"},{"type":"catalog","name":"TailXing_opportunities_Io","id":"sharedcatalog_29","created":"2022-02-23T12:32:21","description":" Generated by the CDPP team from TailXing_opportunities_v12.csv\n Times for the expected footprint tail crossings by Juno, according to magnetic model JRM09\n Version 12: Put together on Apr 2021, Vincent Hue, SwRI. Contact vhue@swri.org for any suggestions\/improvements\n Kernel list:\n  - naif0012.tls\n  - JNO_SCLKSCET.00112.tsc\n  - jup230.bsp\n  - rbsp_general010.tf\n  - spk_ref_180429_210731_180509.bsp\n  - spk_rec_110805_111026_120302.bsp\n  - spk_rec_111026_120308_120726.bsp\n  - spk_rec_120308_120825_121109.bsp\n  - spk_rec_120825_130515_130708.bsp\n  - spk_rec_130515_131005_151210.bsp\n  - spk_rec_131005_131014_131101.bsp\n  - spk_rec_131014_131114_140222.bsp\n  - spk_rec_131114_140918_141208.bsp\n  - spk_rec_140903_151003_160118.bsp\n  - spk_rec_151003_160312_160418.bsp\n  - spk_rec_160312_160522_160614.bsp\n  - spk_rec_160522_160729_160909.bsp\n  - spk_rec_160729_160923_161027.bsp\n  - spk_rec_160923_161115_161121.bsp\n  - spk_rec_161115_170106_170113.bsp\n  - spk_rec_170106_170228_170307.bsp\n  - spk_rec_170228_170422_170427.bsp\n  - spk_rec_170422_170608_170621.bsp\n  - spk_rec_170608_170728_170803.bsp\n  - spk_rec_170728_170918_170922.bsp\n  - spk_rec_170918_171121_171127.bsp\n  - spk_rec_171121_180113_180117.bsp\n  - spk_rec_180113_180307_180312.bsp\n  - spk_rec_180307_180429_180504.bsp\n  - spk_rec_180429_180621_180626.bsp\n  - spk_rec_180620_180812_180821.bsp\n  - spk_rec_180812_181004_181011.bsp\n  - spk_rec_181004_181126_181205.bsp\n  - spk_rec_181126_190118_190124.bsp\n  - spk_rec_190118_190312_190319.bsp\n  - spk_rec_190312_190504_190509.bsp\n  - spk_rec_190504_190626_190627.bsp\n  - spk_rec_190626_190817_190822.bsp\n  - spk_rec_190817_191010_191022.bsp\n  - spk_rec_191010_191201_191210.bsp","nbIntervals":"233","surveyStart":"2016-08-27T12:19:27","surveyStop":"2025-08-15T20:10:40","sharedDate":"2022-02-23T12:36:25+00:00"},{"type":"catalog","name":"MEXShockCrossings","id":"sharedcatalog_30","created":"2022-02-28T06:55:51","description":" Generated by the CDPP team from Data_MEX.txt\n DOI : https:\/\/doi.org\/10.5281\/zenodo.6240624\n Lists of martian bow shock crossings with the corresponding extrapolated terminator altitudes (RTD).\n DATA_MEX.txt includes 11820 shock crossings by the Mars express spacecraft published by Hall et al. (2016) and Sanchez-Cano et al. (2019).\n The crossing time is the start time. The stop time is the crossing time + 1 min.","nbIntervals":"11820","surveyStart":"2004-04-17T17:42:03","surveyStop":"2015-05-23T21:09:14","sharedDate":"2022-02-28T06:57:23+00:00"},{"type":"catalog","name":"MGSShockCrossings","id":"sharedcatalog_31","created":"2022-02-28T06:56:10","description":" Generated by the CDPP team from Data_MGS.txt\n DOI : https:\/\/doi.org\/10.5281\/zenodo.6240624\n Lists of martian bow shock crossings with the corresponding extrapolated terminator altitudes (RTD).\n DATA_MGS.txt includes 544 bow shock crossings from the Mars Global Surveyor spacecraft from September 1997 to September 1998.\n The crossing time is the start time. The stop time is the crossing time + 1 min.","nbIntervals":"544","surveyStart":"1997-09-15T18:49:00","surveyStop":"1998-09-13T19:56:00","sharedDate":"2022-02-28T06:58:03+00:00"},{"type":"catalog","name":"MAVENShockCrossings","id":"sharedcatalog_32","created":"2022-02-28T06:56:30","description":" Generated by the CDPP team from Data_MAVEN.txt\n DOI : https:\/\/doi.org\/10.5281\/zenodo.6240624\n Lists of martian bow shock crossings with the corresponding extrapolated terminator altitudes (RTD).\n DATA_MAVEN.txt includes 3837 shock crossings by the Mars Atmosphere and Volatile EvolutioN spacecraft from November 2014 to April 2017 published by Fang et al. (2017) and Gruesbeck et al. (2018).\n The crossing time is the start time. The stop time is the crossing time + 1 min.","nbIntervals":"3837","surveyStart":"2014-11-12T12:37:00","surveyStop":"2017-04-03T23:41:44","sharedDate":"2022-02-28T06:58:17+00:00"},{"type":"catalog","name":"listOfICMEs_Nguyen","id":"sharedcatalog_33","created":"2019-04-18T13:19:33","description":"List of ICMEs from Nguyen et al., 2019 https:\/\/doi.org\/10.3847\/1538-4357\/ab0d24\nSee also:\nhttps:\/\/github.com\/gautiernguyen\/Automatic-detection-of-ICMEs-at-1-AU-a-deep-learning-approach.\nThe catalog consists of the union of the different WIND ICME lists ('LJ': Jian et al. 2006; 'Lepping': Lepping et al. 2006; 'RC': Richardson & Cane 2010; 'Chi': Chi et al. 2016; 'Chinchilla': Nieves-Chinchilla et al. 2018), of newly discovered events ('FP') and of extra events ('Turc').\n","nbIntervals":"653","surveyStart":"1997-09-03T13:40:00","surveyStop":"2015-12-31T23:59:00","sharedDate":"2022-03-09T10:08:39+00:00"},{"type":"catalog","name":"ICME_multi-catalog","id":"sharedcatalog_41","created":"2023-11-23T15:19:02.000000","description":"source : https:\/\/edatos.consorciomadrono.es\/dataset.xhtml?persistentId=doi:10.21950\/XGUIYX\nName: Carlos Larrodera\nInstitution: University of Alcal\u00e1\nEmail: carlos.larrodera@uah.es\nORCID: 0000-0003-4231-7690\n\nDescription of the project\nThe main idea of the project is to gather the information of different Interplanetary Coronal Mass Ejections (ICMEs) seen by different spacecraft to obtain a combined catalog that ranges between 0.25 to 5 AU and between 1975 and 2022.\nThis allows us to study statistically the different structures present in the ICMEs along with their evolution with distance and time.\n\nDescription of the dataset\nWe have obtained a list of around 2000 separate ICMEs detailed in this file. It should be noted that the only inherited information from the original catalogs are the dates\nThe file contains the following fields:\n\n- icme_start: Date of the beginning of the ICME (*) ; this is the Start Time of the catalogue\n- mo_start: Date of the beginning of the magnetic obstacle (MO) (**)\n- mo_end: Date of the end of the ICME; this is the Stop Time of the catalogue\n- r_heliodist: Heliocentric distance of the spacecraft that detected the ICME (units=Km)\n- spacecraft: Spacecraft that detected the ICME\n- theta: Longitude (HCI reference system)\n- lati: Latitude (HCI reference system)\n- cat_source: Original catalog from which the ICME belongs (***)\n- flg_sheath: Flag for presence of sheath: (1) ICME has a sheath (0) ICME has no sheath\n- v_aver_0048_sw: Upstream average solar wind speed. Time range covered: Between 0h and 48h before the ICME (units=Km\/s)\n- v_std_0048_sw: Upstream standard deviation solar wind speed. Time range covered: Between 0h and 48h before the ICME  (units=Km\/s)\n- B_aver_0048_sw: Upstream average solar wind magnetic field. Time range covered: Between 0h and 48h before the ICME  (units=nT)\n- B_std_0048_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 0h and 48h before the ICME  (units= nT)\n- N_aver_0048_sw: Upstream average solar wind density. Time range covered: Between 0h and 48h before the ICME  (units= cm-3)\n- N_std_0048_sw: Upstream standard deviation solar wind density. Time range covered: Between 0h and 48h before the ICME  (units=cm-3)\n- T_aver_0048_sw: Upstream average solar wind temperature. Time range covered: Between 0h and 48h before the ICME  (units=K)\n- T_std_0048_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 0h and 48h before the ICME  (units=K)\n- v_aver_0024_sw: Upstream average solar wind speed. Time range covered: Between 0h and 24h before the ICME (units=Km\/s)\n- v_std_0024sw: Upstream standard deviation solar wind speed. Time range covered: Between 0h and 24h before the ICME  (units=Km\/s)\n- B_aver_0024_sw: Upstream average solar wind magnetic field. Time range covered: Between 0h and 24h before the ICME  (units=nT)\n- B_std_0024_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 0h and 24h before the ICME  (units= nT)\n- N_aver_0024_sw: Upstream average solar wind density. Time range covered: Between 0h and 24h before the ICME  (units= cm-3)\n- N_std_0024_sw: Upstream standard deviation solar wind density. Time range covered: Between 0h and 24h before the ICME  (units=cm-3)\n- T_aver_0024_sw: Upstream average solar wind temperature. Time range covered: Between 0h and 24h before the ICME  (units=K)\n- T_std_0024_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 0h and 24h before the ICME  (units=K)\n- v_aver_2448_sw: Upstream average solar wind speed. Time range covered: Between 24h and 48h before the ICME (units=Km\/s)\n- v_std_2448_sw: Upstream standar deviation solar wind speed. Time range covered: Between 24h and 48h before the ICME (units=Km\/s)\n- B_aver_2448_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 24h and 48h before the ICME  (units=Km\/s)\n- B_std_2448_sw: Upstream average solar wind magnetic field. Time range covered: Between 24h and 48h before the ICME  (units=nT)\n- N_aver_2448_sw: Upstream standard deviation solar wind density. Time range covered: Between 24h and 48h before the ICME  (units= nT)\n- N_std_2448_sw: Upstream average solar wind density. Time range covered: Between 24h and 48h before the ICME  (units= cm-3)\n- T_aver_2448_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 24h and 48h before the ICME  (units=cm-3)\n- T_std_2448_sw: Upstream average solar wind temperature. Time range covered: Between 24h and 48h before the ICME  (units=K)\n- v_aver_0012h_sw: Upstream average solar wind speed. Time range covered: Between 0h and 12h before the ICME (units=Km\/s)\n- v_std_0012h_sw: Upstream standard deviation solar wind speed. Time range covered: Between 0h and 12h before the ICME  (units=Km\/s)\n- B_aver_0012h_sw: Upstream average solar wind magnetic field. Time range covered: Between 0h and 12h before the ICME  (units=nT)\n- B_std_0012h_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 0h and 12h before the ICME  (units= nT)\n- N_aver_0012h_sw: Upstream average solar wind density. Time range covered: Between 0h and 12h before the ICME  (units= cm-3)\n- N_std_0012h_sw: Upstream standard deviation solar wind density. Time range covered: Between 0h and 12h before the ICME  (units=cm-3)\n- T_aver_0012h_sw: Upstream average solar wind temperature. Time range covered: Between 0h and 12h before the ICME  (units=K)\n- T_std_0012h_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 0h and 12h before the ICME  (units=K)\n- v_aver_1224h_sw: Upstream average solar wind speed. Time range covered: Between 12h and 24h before the ICME (units=Km\/s)\n- v_std_1224h_sw: Upstream standard deviation solar wind speed. Time range covered: Between 12h and 24h before the ICME  (units=Km\/s)\n- B_aver_1224h_sw: Upstream average solar wind magnetic field. Time range covered: Between 12h and 24h before the ICME  (units=nT)\n- B_std_1224h_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 12h and 24h before the ICME  (units= nT)\n- N_aver_1224h_sw: Upstream average solar wind density. Time range covered: Between 12h and 24h before the ICME  (units= cm-3)\n- N_std_1224h_sw: Upstream standard deviation solar wind density. Time range covered: Between 12h and 24h before the ICME  (units=cm-3)\n- T_aver_1224h_sw: Upstream average solar wind temperature. Time range covered: Between 12h and 24h before the ICME  (units=K)\n- T_std_1224h_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 12h and 24h before the ICME  (units=K)\n- v_aver_2436h_sw: Upstream average solar wind speed. Time range covered: Between 24h and 36h before the ICME (units=Km\/s)\n- v_std_2436h_sw: Upstream standard deviation solar wind speed. Time range covered: Between 24h and 36h before the ICME  (units=Km\/s)\n- B_aver_2436h_sw: Upstream average solar wind magnetic field. Time range covered: Between 24h and 36h before the ICME  (units=nT)\n- B_std_2436h_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 24h and 36h before the ICME  (units= nT)\n- N_aver_2436h_sw: Upstream average solar wind density. Time range covered: Between 24h and 36h before the ICME  (units= cm-3)\n- N_std_2436h_sw: Upstream standard deviation solar wind density. Time range covered: Between 24h and 36h before the ICME  (units=cm-3)\n- T_aver_2436h_sw: Upstream average solar wind temperature. Time range covered: Between 24h and 36h before the ICME  (units=K)\n- T_std_2436h_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 24h and 36h before the ICME  (units=K)\n- v_aver_3648h_sw: Upstream average solar wind speed. Time range covered: Between 36h and 48h before the ICME (units=Km\/s)\n- v_std_3648h_sw: Upstream standard deviation solar wind speed. Time range covered: Between 36h and 48h before the ICME  (units=Km\/s)\n- B_aver_3648h_sw: Upstream average solar wind magnetic field. Time range covered: Between 36h and 48h before the ICME  (units=nT)\n- B_std_3648h_sw: Upstream standard deviation solar wind magnetic field. Time range covered: Between 36h and 48h before the ICME  (units= nT)\n- N_aver_3648h_sw: Upstream average solar wind density. Time range covered: Between 36h and 48h before the ICME  (units= cm-3)\n- N_std_3648h_sw: Upstream standard deviation solar wind density. Time range covered: Between 36h and 48h before the ICME  (units=cm-3)\n- T_aver_3648h_sw: Upstream average solar wind temperature. Time range covered: Between 36h and 48h before the ICME  (units=K)\n- T_std_3648h_sw: Upstream standard deviation solar wind temperature. Time range covered: Between 36h and 48h before the ICME  (units=K)\n- v_aver_sh: Sheath average speed (units=km\/s)\n- v_std_sh: Sheath standard deviation speed (units=km\/s)\n- B_aver_sh: Sheath average magnetic field (units=nT)\n- B_std_sh: Sheath standard deviation magnetic field (units=nT)\n- N_aver_sh: Sheath average density (units=cm-3)\n- N_std_sh: Sheath standard deviation density (units=cm-3)\n- T_aver_sh: Sheath average temperature (units=K)\n- T_std_sh: Sheath standard deviation temperature (units=K)\n- v_aver_mo_cat_II: Magnetic Obstacle Cat II average speed (units=km\/s)\n- v_std_mo_cat_II: Magnetic Obstacle Cat II standard deviation speed (units=km\/s)\n- B_aver_mo_cat_II: Magnetic Obstacle Cat II average magnetic field (units=nT)\n- B_std_mo_cat_II: Magnetic Obstacle Cat II standard deviation magnetic field (units=nT)\n- N_aver_mo_cat_II: Magnetic Obstacle Cat II average density (units=cm-3)\n- N_std_mo_cat_II: Magnetic Obstacle Cat II standard deviation density (units=cm-3)\n- T_aver_mo_cat_II: Magnetic Obstacle Cat II average temperature (units=K)\n- T_std_mo_cat_II: Magnetic Obstacle Cat II standard deviation temperature (units=K)\n- v_aver_mo_cat_I: Magnetic Obstacle Cat I average speed (units=km\/s)\n- v_std_mo_cat_I: Magnetic Obstacle Cat I standard deviation speed (units=km\/s)\n- B_aver_mo_cat_I: Magnetic Obstacle Cat I average magnetic field (units=nT)\n- B_std_mo_cat_I: Magnetic Obstacle Cat I standard deviation magnetic field (units=nT)\n- N_aver_mo_cat_I: Magnetic Obstacle Cat I average density (units=cm-3)\n- N_std_mo_cat_I: Magnetic Obstacle Cat I standard deviation density (units=cm-3)\n- T_aver_mo_cat_I: Magnetic Obstacle Cat I average temperature (units=K)\n- T_std_mo_cat_I: Magnetic Obstacle Cat I standard deviation temperature (units=K)\n- dur_sh: Duration of the sheath (units=hours)\n- dur_mo_cat_II: Duration of the magnetic obstacle Cat II (units=hours)\n- dur_mo_cat_I: Duration of the magnetic obstacle Cat I (units=hours)\n- scycle: Solar cycle to which it belongs the ICME according to the icme_start date\n- v_sh_bg_mean: Average speed at the beginning of the sheath (units=km\/s) (****)\n- v_sh_bg_std: Standard deviation of the speed at the beginning of the sheath (units=km\/s) (****)\n- v_sh_end_mean: Average speed at the end of the sheath (units=km\/s) (****)\n- v_sh_end_std: Standard deviation of the speed at the end of the sheath (units=km\/s) (****)\n- v_sh_max: Maximum value of speed in the sheath (units=km\/s)\n- v_sh_min: Minimum value of speed in the sheath (units=km\/s)\n- B_sh_bg_mean: Average magnetic field at the beginning of the sheath (units=nT) (****)\n- B_sh_bg_std: Standard deviation of the magnetic field at the beginning of the sheath (units=nT) (****)\n- B_sh_end_mean: Average magnetic field at the end of the sheath (units=nT) (****)\n- B_sh_end_std: Standard deviation of the magnetic field at the end of the sheath (units=nT) (****)\n- B_sh_max: Maximum value of magnetic field in the sheath (units=nT)\n- B_sh_min: Minimum value of magnetic field in the sheath (units=nT)\n- N_sh_bg_mean: Average density at the beginning of the sheath (units=cm-3) (****)\n- N_sh_bg_std: Standard deviation of the density at the beginning of the sheath (units=cm-3) (****)\n- N_sh_end_mean: Average density at the end of the sheath (units=cm-3) (****)\n- N_sh_end_std: Standard deviation of the density at the end of the sheath (units=cm-3) (****)\n- N_sh_max: Maximum value of density in the sheath (units=cm-3)\n- N_sh_min: Minimum value of density in the sheath (units=cm-3)\n- T_sh_bg_mean: Average temperature at the beginning of the sheath (units=K) (****)\n- T_sh_bg_std: Standard deviation of the temperature at the beginning of the sheath (units=K) (****)\n- T_sh_end_mean: Average temperature at the end of the sheath (units=K) (****)\n- T_sh_end_std: Standard deviation of the temperature at the end of the sheath (units=K) (****)\n- T_sh_max: Maximum value of temperature in the sheath (units=K)\n- T_sh_min: Minimum value of temperature in the sheath (units=K)\n- v_mo_bg_mean: Average speed at the beginning of the magnetic obstacle (units=km\/s) (*****)\n- v_mo_bg_std: Standard deviation of the speed at the beginning of the magnetic obstacle (units=km\/s) (*****)\n- v_mo_end_mean: Average speed at the end of the magnetic obstacle (units=km\/s) (*****)\n- v_mo_end_std: Standard deviation of the speed at the end of the magnetic obstacle (units=km\/s) (*****)\n- v_mo_max: Maximum value of speed in the magnetic obstacle (units=km\/s) (*****)\n- v_mo_min: Minimum value of speed in the magnetic obstacle (units=km\/s) (*****)\n- B_mo_bg_mean: Average magnetic field at the beginning of the magnetic obstacle (units=nT) (*****)\n- B_mo_bg_std: Standard deviation of the magnetic field at the beginning of the magnetic obstacle (units=nT) (*****)\n- B_mo_end_mean: Average magnetic field at the end of the magnetic obstacle (units=nT) (*****)\n- B_mo_end_std: Standard deviation of the magnetic field at the end of the magnetic obstacle (units=nT) (*****)\n- B_mo_max: Maximum value of magnetic field in the magnetic obstacle (units=nT) (*****)\n- B_mo_min: Minimum value of magnetic field in the magnetic obstacle (units=nT) (*****)\n- N_mo_bg_mean: Average density at the beginning of the magnetic obstacle (units=cm-3) (*****)\n- N_mo_bg_std: Standard deviation of the density at the beginning of the magnetic obstacle (units=cm-3) (*****)\n- N_mo_end_mean: Average density at the end of the magnetic obstacle (units=cm-3) (*****)\n- N_mo_end_std: Standard deviation of the density at the end of the magnetic obstacle (units=cm-3) (*****)\n- N_mo_max: Maximum value of density in the magnetic obstacle (units=cm-3) (*****)\n- N_mo_min: Minimum value of density in the magnetic obstacle (units=cm-3) (*****)\n- T_mo_bg_mean: Average temperature at the beginning of the magnetic obstacle (units=K) (*****)\n- T_mo_bg_std: Standard deviation of the temperature at the beginning of the magnetic obstacle (units=K) (*****)\n- T_mo_end_mean: Average temperature at the end of the magnetic obstacle (units=K) (*****)\n- T_mo_end_std: Standard deviation of the temperature at the end of the magnetic obstacle (units=K) (*****)\n- T_mo_max: Maximum value of temperature in the magnetic obstacle (units=K) (*****)\n- T_mo_min: Minimum value of temperature in the magnetic obstacle (units=K) (*****)\n- size_mo: Size of the magnetic obstacle (units=km) (*****)\n- size_sh: Size of the sheath (units=km)\n\nNotes\n(*) The term ICME define, sheath (if present) and the magnetic obstacle. If the ICME does not present a sheath, the ICME will be the magnetic obstacle. \n(**) If the ICME does not have a sheath, the 'icme_start' and 'mo_start' will be the same. The 'magnetic obstacle Cat I', refers to the magnetic obstacle that follows a sheath, while 'magnetic obstacle Cat II', refers to the magnetic obstacle of ICMEs without a sheath.\n(***) List of catalogs\ncat_1: M\u00f6stl et al. (2020). doi: 10.3847\/1538-4357\/abb9a1 \ncat_2: Nieves-Chinchilla et al. (2008) doi:  10.1007\/s11207-018-1247-z\ncat_3: STEREO ICME List (https:\/\/parker.gsfc.nasa.gov\/ICME_catalogs\/STEREO\/ICME_catalog_viewer_STEREO.php)\ncat_5: Helios ICME List (https:\/\/parker.gsfc.nasa.gov\/ICME_catalogs\/Helios\/ICME_catalog_viewer_Helios.php)\ncat_6: Solar Orbiter ICME List (https:\/\/parker.gsfc.nasa.gov\/ICME_catalogs\/SO\/ICME_catalog_viewer_SO.php)\ncat_7: Parker Solar Probe List (https:\/\/parker.gsfc.nasa.gov\/ICME_catalogs\/PSP\/ICME_catalog_viewer_PSP.php)\ncat_8: Commission et al. (2014) doi: 10.2769\/88565\ncat_9: Regnault et al (2010) doi: 10.1029\/2020JA028150\ncat_10: Richardson and Cane (2010) doi: 10.1007\/s11207-010-9568-6\ncat_11: Jian et al. (2018) doi: 10.3847\/1538-4357\/aab189 \ncat_12: Jian et al. (2006) doi: 10.1007\/s11207-006-0133-2  \ncat_13: Du et al. (2010) doi: 10.1007\/s11207-009-9505-8 \n(****) These values have been computed by averaging the values from the boundary (beginning or end) \u00b1 10 minutes. Therefore, a standard deviation is also obtained.\n(*****) These values have been computed by averaging the values from the boundary (beginning or end) \u00b1 10 minutes. Therefore, a standard deviation is also obtained. MO represent the magnetic obstacle that it is present in all the ICMEs, not specifically to those with or without sheaths.\n","nbIntervals":"2003","surveyStart":"1975-01-08T12:00:00","surveyStop":"2022-10-21T22:39:00","sharedDate":"2023-11-23T15:20:14+00:00"},{"type":"catalog","name":"cassini","id":"sharedcatalog_9","created":"2020-06-04T14:49:26","description":"The orbit numbers for cassini are presented following the names given to successive revolutions of the cassini mission around Saturn. \n        Following scientific publications, the orbit numbers are given as : \n        * Saturn Orbit Insertion (rev 0) - not specified\n        * Rev. A\n        * Rev. B\n        * Rev. C\n        * Rev. 3 ~ orbit number 3\n        * Rev. 4 ~ orbit number 4 \n        * ... \n        ","nbIntervals":"297","surveyStart":"2004-06-27T02:00:00","surveyStop":"2017-09-15T11:58:00","sharedDate":"2025-01-07T12:53:06+00:00"},{"type":"catalog","name":"juicecr51","id":"sharedcatalog_46","created":"2024-02-22T14:27:52","description":"The Jupiter Icy Moons Explorer (JUICE) is an interplanetary spacecraft that was launched on 14 April 2023 the European Space Agency (ESA). The mission is planned to study Ganymede, Callisto, and Europa, three of Jupiter's Galilean moons. They are thought to have significant bodies of liquid water beneath their icy surfaces which would make them potentially habitable environments. This catalog has been created using spice kernels provided by https:\/\/s2e2.cosmos.esa.int\/bitbucket\/projects\/spice_kernels\/repos\/juice\/browse (CReMA 5.1) and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"65","surveyStart":"2031-11-02T02:33:58","surveyStop":"2034-12-13T00:52:36","sharedDate":"2025-01-07T12:53:13+00:00"},{"type":"catalog","name":"juno","id":"sharedcatalog_10","created":"2025-01-07T11:58:06","description":"Juno will improve our understanding of the solar system's begninnings by revealing the origin and evolution of Jupiter. Mission starts on august 5th 2011 and will reach Jupiter on July 4yj 2016. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"67","surveyStart":"2016-07-31T19:46:02","surveyStop":"2024-12-10T21:12:42","sharedDate":"2025-01-07T12:53:17+00:00"},{"type":"catalog","name":"maven","id":"sharedcatalog_11","created":"2024-08-21T09:21:19","description":"Mars Atmosphere And Volatile Evolution Mission (MAVEN) is a satellite optimised for determining the role that loss of volatile compounds-such as carbon dioxide, nitrogen dioxide, and water-from Mars' atmisphere to space has played through time, giving insight into the history of Mars' atmosphere and climate, liquid water, and planetary habitability. The mission was launched on November 18th 2013 and reached Mars in September 2014 where it continued operating more than 2 years. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"21798","surveyStart":"2014-09-22T19:33:16","surveyStop":"2024-08-13T13:41:04","sharedDate":"2025-01-07T12:53:21+00:00"},{"type":"catalog","name":"messenger","id":"sharedcatalog_12","created":"2020-06-04T14:00:59","description":"The Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER) mission, launched on 2004-08-03, was mainly designed to study the characteristics and environment of Mercury from orbit. After an Earth flyby July-August, 2005, Venus flybys October-November, 2006, and May-June, 2007, and Mercury flybys December 2007 - January 2008, September-October, 2008, and September-October, 2009, MESSENGER entered Mercury orbit 2011-03-04. Much data of interest tothe heliospheric community was obtained during the cruise phases between planetary encounters from a magnetometer and an energetic particle and plasma spectrometer. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"4103","surveyStart":"2011-03-18T18:54:28","surveyStop":"2015-04-30T15:15:51","sharedDate":"2025-01-07T12:53:25+00:00"},{"type":"catalog","name":"mex","id":"sharedcatalog_13","created":"2023-04-03T09:32:49","description":"Mars Express, so called because of the rapid and streamlined development time, represents ESA's first visit to another planet in the Solar System. The spacecraft borrowed technology from ESA's Rosetta mission (currently accompanying comet 67P\/Churyumov-Gerasimenko along its orbit) and the Mars 96 mission. The mission started on June 2nd 2003. Since beginning science operations in 2004, the durable orbiter has given scientists an entirely new view of Earth's intriguing neighbour, and is helping to answer fundamental questions about the geology, atmosphere, surface environment, history of water and potential for life on Mars.This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"24295","surveyStart":"2004-01-10T20:13:30","surveyStop":"2023-03-31T20:18:27","sharedDate":"2025-01-07T12:53:29+00:00"},{"type":"catalog","name":"psp","id":"sharedcatalog_14","created":"2023-04-03T09:31:46","description":"Parker Solar Probe will swoop to within 4 million miles of the sun's surface, facing heat and radiation like no spacecraft before it. Launching on august 12th 2018, Parker Solar Probe will provide new data on solar activity and make critical contributions to our ability to forecast major space-weather events that impact life on Earth. The mission is named for physicist Eugene Parker, who first theorized the existence of the solar wind and the complex interactions involving plasmas, magnetic fields, and energetic particles involved in 1958. He is the first living person to have a NASA spacecraft named after him. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug).","nbIntervals":"23","surveyStart":"2019-01-20T01:04:04","surveyStop":"2025-08-02T13:59:28","sharedDate":"2025-01-07T12:53:33+00:00"},{"type":"catalog","name":"solo","id":"sharedcatalog_15","created":"2023-04-03T09:31:46","description":"Solar Orbiter is a Sun-observing satellite, under development by the European Space Agency. The mission was launched with an Atlas V from the Cape Canaveral AFS in Florida on 09 February 2020. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug).","nbIntervals":"21","surveyStart":"2020-10-12T11:53:07","surveyStop":"2030-08-21T07:20:31","sharedDate":"2025-01-07T12:53:37+00:00"},{"type":"catalog","name":"vex","id":"sharedcatalog_16","created":"2023-04-03T11:21:18","description":"Venus Express is a satellite optimised for studying the atmosphere of Venus, from the surface right up to the ionosphere. Launched on November 9th 2005, it arrived at Venus in April 2006 and continued operating for more than eight years. The mission ended on December 16th 2014. This catalog has been created using spice kernels provided by spdf and the JPL's orbnum tool (https:\/\/naif.jpl.nasa.gov\/pub\/naif\/utilities\/PC_Linux_64bit\/orbnum.ug)","nbIntervals":"3186","surveyStart":"2006-04-24T05:48:44","surveyStop":"2014-12-31T12:23:54","sharedDate":"2025-01-07T12:53:41+00:00"},{"type":"catalog","name":"BepiCoordObs_Windows_of_Opportunities","id":"sharedcatalog_21","created":"2020-07-03T14:48:14","description":" BepiColombo coordinated observations catalogue is made in the framework of the ESA\/JAXA working group: \"BepiColombo's cruise phase coordinated observations\". It includes potential windows of opportunities for coordinated measurements with different spacecraft in the inner and outer heliosphere from 01\/10\/2020 until 31\/12\/2025. The spacecraft comprise of BepiColombo (Bepi), Solar Orbiter (SolO), Parker Solar Probe (PSP), Stereo A and Juice. In addition to these missions, planets were also added: Venus, Earth, Mars and Jupiter. This investigation was done using AMDA's \"Data Mining\" and \"Statistics\" tools. The latest kernels for the objects ephemeris were used at the time the catalogue was generated (june 2020).\n \n Columns of the catalogue are:\n \n Start_time End_time Geometry Spacecraft SolarWind_speed BepiColombo_flybys SolarOrbiter_flybys Juice_flybys min_bepi_r_sun max_bepi_r_sun avg_bepi_r_sun min_bepi_lon_hee max_bepi_lon_hee avg_bepi_lon_hee min_bepi_lat_hee max_bepi_lat_hee avg_bepi_lat_hee min_so_r_sun max_so_r_sun avg_so_r_sun min_so_lon_hee max_so_lon_hee avg_so_lon_hee min_so_lat_hee max_so_lat_hee avg_so_lat_hee min_psp_r_sun max_psp_r_sun avg_psp_r_sun min_psp_lon_hee max_psp_lon_hee avg_psp_lon_hee min_psp_lat_hee max_psp_lat_hee avg_psp_lat_hee min_sta_r_hee max_sta_r_hee avg_sta_r_hee min_sta_lon_hee max_sta_lon_hee avg_sta_lon_hee min_sta_lat_hee max_sta_lat_hee avg_sta_lat_hee min_juice_cruise_r max_juice_cruise_r avg_juice_cruise_r min_juice_cruise_lon_hee max_juice_cruise_lon_hee avg_juice_cruise_lon_hee min_juice_cruise_lat_hee max_juice_cruise_lat_hee avg_juice_cruise_lat_hee min_r_venus max_r_venus avg_r_venus min_venus_lon_hee max_venus_lon_hee avg_venus_lon_hee min_venus_lat_hee max_venus_lat_hee avg_venus_lat_hee min_r_earth max_r_earth avg_r_earth min_earth_lon_hee max_earth_lon_hee avg_earth_lon_hee min_earth_lat_hee max_earth_lat_hee avg_earth_lat_hee min_r_mars max_r_mars avg_r_mars min_mars_lon_hee max_mars_lon_hee avg_mars_lon_hee min_mars_lat_hee max_mars_lat_hee avg_mars_lat_hee min_r_jupiter max_r_jupiter avg_r_jupiter min_jupiter_lon_hee max_jupiter_lon_hee avg_jupiter_lon_hee min_jupiter_lat_hee max_jupiter_lat_hee avg_jupiter_lat_hee","nbIntervals":"1174","surveyStart":"2020-09-01T00:00:00","surveyStop":"2025-10-30T18:30:00","sharedDate":"2020-07-03T14:48:41+00:00"},{"type":"timeTable","name":"FTE_c1","id":"sharedtimeTable_0","created":"2018-01-18T16:25:22","description":"FTE list from Cluster 1 data. From \"A new multivariate time series data analysis technique: Automated detection of flux transfer events using Cluster data\" by Karimabadi et al., JGR, VOL. 114, A06216, doi:10.1029\/2009JA014202, 2009, http:\/\/www.agu.org\/journal\/ja\/ja0906\/2009JA014202\/ The list is available as Auxiliary material \"Data Set S3\" Transformation into AMDA Time Table by V. Genot, CESR, Toulouse, France 29\/06\/2009.  - millisec have been omitted - the original event corresponds to the StartTime of the Time Table - if StopTime-StartTime = 1 sec then the event is a magnetosheath FTE - if StopTime-StartTime = 2 sec then the event is a magnetospheric FTE ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"782","surveyStart":"2001-02-02T16:39:57","surveyStop":"2003-06-19T18:47:50","sharedDate":"2018-01-18T16:26:18+00:00"},{"type":"timeTable","name":"FTE_c3","id":"sharedtimeTable_1","created":"2018-01-18T16:27:29","description":"FTE list from Cluster 3 data. From \"A new multivariate time series data analysis technique: Automated detection of flux transfer events using Cluster data\" by Karimabadi et al., JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114, A06216, doi:10.1029\/2009JA014202, 2009 http:\/\/www.agu.org\/journals\/ja\/ja0906\/2009JA014202\/ The list is available as Auxiliary material \"Data Set S3\" Transformation into AMDA Time Table by V. Genot, CESR, Toulouse, France 29\/06\/2009 : - millisec have been omitted - the original event corresponds to the StartTime of the Time Table - if StopTime-StartTime = 1 sec then the event is a magnetosheath FTE - if StopTime-StartTime = 2 sec then the event is a magnetospheric FTE ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"738","surveyStart":"2001-02-02T16:27:12","surveyStop":"2003-06-19T18:47:50","sharedDate":"2018-01-18T16:28:11+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_CHBG","id":"sharedtimeTable_10","created":"2018-01-18T16:47:29","description":"THEMIS substorms list based on overview jpegs at station CHBG Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"4","surveyStart":"2007-12-07T04:04:00","surveyStop":"2008-03-04T05:38:01","sharedDate":"2018-01-18T16:47:36+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_FSIM","id":"sharedtimeTable_11","created":"2018-01-18T16:47:53","description":"THEMIS substorms list based on overview jpegs at station FSIM Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"184","surveyStart":"2007-12-05T09:04:00","surveyStop":"2008-04-01T07:37:01","sharedDate":"2018-01-18T16:48:00+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_FSMI","id":"sharedtimeTable_12","created":"2018-01-18T16:48:18","description":"THEMIS substorms list based on overview jpegs at station FSMI Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"179","surveyStart":"2007-12-08T07:10:00","surveyStop":"2008-04-01T07:26:01","sharedDate":"2018-01-18T16:48:33+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_FYKN","id":"sharedtimeTable_13","created":"2018-01-18T16:48:49","description":"THEMIS substorms list based on overview jpegs at station FYKN Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"106","surveyStart":"2008-01-29T07:40:00","surveyStop":"2008-03-31T08:56:01","sharedDate":"2018-01-18T16:48:55+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_GAKO","id":"sharedtimeTable_14","created":"2018-01-18T16:49:12","description":"THEMIS substorms list based on overview jpegs at station GAKO Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"66","surveyStart":"2007-12-12T09:59:00","surveyStop":"2008-03-31T08:56:01","sharedDate":"2018-01-18T16:49:27+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_GBAY","id":"sharedtimeTable_15","created":"2018-01-18T16:49:48","description":"THEMIS substorms list based on overview jpegs at station GBAY Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"19","surveyStart":"2008-01-05T08:50:00","surveyStop":"2008-04-01T03:51:01","sharedDate":"2018-01-18T16:49:56+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_GILL","id":"sharedtimeTable_16","created":"2018-01-18T16:50:16","description":"THEMIS substorms list based on overview jpegs at station GILL Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"150","surveyStart":"2007-12-05T01:40:00","surveyStop":"2008-04-01T07:41:01","sharedDate":"2018-01-18T16:50:22+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_INUV","id":"sharedtimeTable_17","created":"2018-01-18T16:50:42","description":"THEMIS substorms list based on overview jpegs at station INUV Substorm identification is done purely by visible inspection of all-sky images  There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"274","surveyStart":"2007-12-01T08:04:00","surveyStop":"2008-04-02T08:55:01","sharedDate":"2018-01-18T16:50:50+00:00"},{"type":"timeTable","name":"TT_BOW_CLUSTER","id":"sharedtimeTable_2","created":"2018-01-18T16:31:19","description":"List of shocks from: MULTIPLE SPACECRAFT BOW SHOCK CROSSINGS DATABASE at NSSDC (http:\/\/ftpbrowser.gsfc.nasa.gov\/bowshock.html) The original list had only one time per row, the crossing time. In the present table, we substracted 5 min from the crossing time to get the Start Time and added 5 min to get the Stop  Time Creation Date : 2007-03-20T17:00:00 ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"388","surveyStart":"2001-02-02T20:29:00","surveyStop":"2002-05-20T10:49:00","sharedDate":"2018-01-18T16:31:37+00:00"},{"type":"timeTable","name":"MPX_table","id":"sharedtimeTable_3","created":"2018-01-18T16:33:34","description":"Magnetopause crossings from Geosynchronous LANL1994_084 Magnetospheric Plasma Analyzer abs(deriv_((CDAWEB_L4_K0_MPA_temp_hip(1))\/(CDAWEB_L4_K0_MPA_dens_hip))\/((CDAWEB_L4_K0_MPA_temp_hip(1))\/(CDAWEB_L4_K0_MPA_dens_hip)))>0.05; CDAWEB_L4_K0_MPA_temp_hip(1) => parameter from External Data Base; CDAWEB_L4_K0_MPA_dens_hip => parameter from External Data Base; ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"19","surveyStart":"2000-05-24T01:54:00","surveyStop":"2000-08-12T06:40:20","sharedDate":"2018-01-18T16:33:58+00:00"},{"type":"timeTable","name":"Event_list_tail_hall_reconnection_SC1","id":"sharedtimeTable_4","created":"2018-01-18T16:41:14","description":"Cluster spacecraft 1 event list of ion diffusion region encounters (with Hall signatures), from Eastwood et al. (JGR, in press, 2010).; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"17","surveyStart":"2001-08-22T09:43:00","surveyStop":"2005-09-26T09:51:00","sharedDate":"2018-01-18T16:41:40+00:00"},{"type":"timeTable","name":"Event_list_tail_hall_reconnection_SC3","id":"sharedtimeTable_5","created":"2018-01-18T16:41:59","description":"Cluster spacecraft 3 event list of ion diffusion region encounters (with Hall signatures), from Eastwood et al. (JGR, in press, 2010).; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"12","surveyStart":"2001-08-22T09:43:00","surveyStop":"2003-10-09T02:27:00","sharedDate":"2018-01-18T16:42:07+00:00"},{"type":"timeTable","name":"Storm_SC_1868_1967","id":"sharedtimeTable_6","created":"2018-01-18T16:43:51","description":"Storm Sudden Commencements (SSC) 1868-1967 -- see http:\/\/www.ngdc.noaa.gov\/stp\/SOLAR\/ftpSSC.html -- Events +- 30 min; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"2462","surveyStart":"2004-02-29T19:46:16","surveyStop":"2104-02-05T04:52:17","sharedDate":"2018-01-18T16:43:59+00:00"},{"type":"timeTable","name":"Storm_SC_1968_present","id":"sharedtimeTable_7","created":"2018-01-18T16:44:17","description":"Storm Sudden Commencements (SSC) 1968-present -- see http:\/\/www.ngdc.noaa.gov\/stp\/SOLAR\/ftpSSC.html -- Events +- 30 min; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:48; \n ","nbIntervals":"1261","surveyStart":"1970-01-05T05:37:00","surveyStop":"2106-01-17T19:13:17","sharedDate":"2018-01-18T16:44:25+00:00"},{"type":"timeTable","name":"Substorm_onset_Frey","id":"sharedtimeTable_8","created":"2018-01-18T16:44:44","description":"Substorm onset observations by the IMAGE-FUV instrument between May 2000 and December 31, 2002  From Frey et al., JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109, A10304, doi:10.1029\/2004JA010607, 2004  see also http:\/\/www.agu.org\/journals\/ja\/ja0410\/2004JA010607\/supplement.shtml   Event +- 30 min; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"2437","surveyStart":"2000-05-16T17:17:17","surveyStop":"2002-12-31T21:17:54","sharedDate":"2018-01-18T16:44:54+00:00"},{"type":"timeTable","name":"THEMIS_Substorm_2007-2008_ATHA","id":"sharedtimeTable_9","created":"2018-01-18T16:46:54","description":"THEMIS substorms list based on overview jpegs at station ATHA  Substorm identification is done purely by visible inspection of all-sky images There is no guarantee that a certain feature is really a substorm  Please see ftp:\/\/justice.ssl.berkeley.edu\/events\/ for more details; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"16","surveyStart":"2007-12-07T08:33:00","surveyStop":"2008-04-01T05:38:01","sharedDate":"2018-01-18T17:01:43+00:00"},{"type":"timeTable","name":"Cluster1_BS_crossings_Nguyen2021","id":"sharedtimeTable_155","created":"2022-11-08T15:48:36.000000","description":"Cluster 1 bow shock crossings (2001-2012) from the 4 papers \"Massive Multi-Mission Statistical Study and Analytical Modeling of the Earth's Magnetopause\" by Nguyen et al., 2021\nhttps:\/\/doi.org\/10.1029\/2021JA029773\nhttps:\/\/doi.org\/10.1029\/2021JA029774\nhttps:\/\/doi.org\/10.1029\/2021JA030112\nhttps:\/\/doi.org\/10.1029\/2021JA029776\n\nData can also be found at:\nhttps:\/\/zenodo.org\/record\/5668298\n\nThe shock timing is the middle of the 10min interval.","nbIntervals":"3225","surveyStart":"2001-02-04T00:12:00.000","surveyStop":"2012-06-22T18:24:00.000","sharedDate":"2022-11-08T15:53:02+00:00"},{"type":"timeTable","name":"shock_SERPENTINE_SOLO_cycle25","id":"sharedtimeTable_174","created":"2024-04-22T06:20:58.000000","description":"In-situ shock crossings at Solar Orbiter catalogued in WP4 of SERPENTINE H2020 project (responsible: D. Trotta)","nbIntervals":"61","surveyStart":"2020-04-19T05:06:15","surveyStop":"2023-04-22T08:12:11","sharedDate":"2024-04-22T08:05:27+00:00"},{"type":"timeTable","name":"SERPENTINE_shock_Wind_cycle25","id":"sharedtimeTable_176","created":"2024-04-22T03:46:36.000000","description":"In-situ shock crossings at L1 (WInd spacecraft) catalogued in WP4 of SERPENTINE H2020 project (responsible: D. Trotta)","nbIntervals":"27","surveyStart":"2020-12-02T10:11:50.000","surveyStop":"2023-05-12T06:17:28.000","sharedDate":"2024-04-23T11:54:40+00:00"},{"type":"timeTable","name":"callisto_flyby","id":"sharedtimeTable_51","created":"2018-01-19T15:04:54","description":"Time Table generated by Nicolas Andre @ CDPP;Description: Galileo Callisto flybys C3, C9-10, C20-23, C30Creation Date :  Wed Aug 24 20:49:00 2011;; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:54; \n ","nbIntervals":"8","surveyStart":"1996-11-04T13:15:10","surveyStop":"2001-05-25T11:45:04","sharedDate":"2018-01-19T15:17:46+00:00"},{"type":"timeTable","name":"ganymede_flyby","id":"sharedtimeTable_52","created":"2018-01-19T15:05:14","description":"Time Table generated by Nicolas Andre @ CDPP;Description: Galileo Ganymede flybys G1, G2, G7-8, G28-29Creation Date :  Wed Aug 24 20:50:00 2011;; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:55; \n ","nbIntervals":"8","surveyStart":"1996-06-27T06:07:08","surveyStop":"2000-12-28T08:55:21","sharedDate":"2018-01-19T15:17:58+00:00"},{"type":"timeTable","name":"juno_orbits_apoapsis","id":"sharedtimeTable_53","created":"2018-07-13T09:01:21","description":"site web LASP\nhttp:\/\/lasp.colorado.edu\/home\/mop\/missions\/juno\/trajectory-information\/","nbIntervals":"33","surveyStart":"2016-07-31T19:46:02","surveyStop":"2021-07-03T19:26:51","sharedDate":"2018-07-16T13:48:12+00:00"},{"type":"timeTable","name":"conjonctions_mex-mgs_2004_0","id":"sharedtimeTable_37","created":"2018-01-19T14:50:02","description":"conjonctions between MGS and MEX, distance < 400 km; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"28","surveyStart":"2004-05-07T06:53:00","surveyStop":"2004-12-26T23:43:40","sharedDate":"2018-01-19T14:51:13+00:00"},{"type":"timeTable","name":"conjonctions_mex-mgs_2005_0","id":"sharedtimeTable_38","created":"2018-01-19T14:50:25","description":"conjonctions between MGS and Mex, distance<400km; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"38","surveyStart":"2005-01-01T07:33:50","surveyStop":"2005-12-25T16:26:00","sharedDate":"2018-01-19T14:51:21+00:00"},{"type":"timeTable","name":"conjonctions_mex-mgs_2006_0","id":"sharedtimeTable_39","created":"2018-01-19T14:50:45","description":"conjonctions MGS and Mex, distance<400km; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"30","surveyStart":"2006-03-17T17:08:00","surveyStop":"2006-11-02T15:19:20","sharedDate":"2018-01-19T14:51:29+00:00"},{"type":"timeTable","name":"List_of_Cassini_narrowband_radio_events","id":"sharedtimeTable_40","created":"2018-01-19T14:54:39","description":"After Ye, Sheng-Yi et al. (2009), Source locations of narrowband radio emissions detected at Saturn, Journal of Geophysical REsearch, 114, A06219, doi:10.1029\/2008JA013855; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"30","surveyStart":"2005-09-25T00:00:00","surveyStop":"2007-05-26T23:59:59","sharedDate":"2018-01-19T14:59:38+00:00"},{"type":"timeTable","name":"List_of_Titan_around_midnight_LT","id":"sharedtimeTable_41","created":"2018-01-19T14:55:21","description":"From http:\/\/www-pw.physics.uiowa.edu\/~jbg\/cas.html  Titan between ~2300 and ~0100 Local Time; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"92","surveyStart":"2004-06-29T00:00:00","surveyStop":"2008-06-23T00:00:00","sharedDate":"2018-01-19T15:00:09+00:00"},{"type":"timeTable","name":"List_of_Cassini_HST_observations","id":"sharedtimeTable_42","created":"2018-01-19T14:55:58","description":"This table lists time periods which include HST auroral observations of Saturn (Proposal ID #11984, 11645, 11566, 10862, 10506, 10156, 10083).   HST observations can be visualized with Aladin from http:\/\/archive.stsci.edu\/hst\/  ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"18","surveyStart":"2004-01-08T00:00:00","surveyStop":"2009-03-07T23:59:59","sharedDate":"2018-01-19T15:00:21+00:00"},{"type":"timeTable","name":"List_of_Cassini_reconnection_events","id":"sharedtimeTable_43","created":"2018-01-19T14:56:20","description":"Table from Jackman, C. M. et al. (2009), On the character and distribution of lower-frequency radio emissions at Saturn and their relationship to substorm-like events, Journal of Geophysical Research, 114, A08211, doi:10.1029\/2008JA013997   Reconnection extended by 10 min; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"9","surveyStart":"2004-07-02T01:50:00","surveyStop":"2006-09-06T15:40:01","sharedDate":"2018-01-19T15:00:32+00:00"},{"type":"timeTable","name":"List_of_Cassini_Titan_flybys","id":"sharedtimeTable_44","created":"2018-01-19T14:56:57","description":"Titan's flyby T0A to T82\n; \n        Historic: ;\n        Creation Date :  2016-09-06T12:51:24; \n ","nbIntervals":"83","surveyStart":"2004-10-26T14:00:00","surveyStop":"2012-02-19T10:13:00","sharedDate":"2018-01-19T15:00:44+00:00"},{"type":"timeTable","name":"List_of_Cassini_reconnection_events_extended","id":"sharedtimeTable_45","created":"2018-01-19T14:57:37","description":"Table from Jackman, C. M. et al. (2009), On the character and distribution of lower-frequency radio emissions at Saturn and their relationship to substorm-like events, Journal of Geophysical Research, 114, A08211, doi:10.1029\/2008JA013997   Reconnection extended by 10 min  One additional event from Russell et al. (2008) Titan's influence on Saturnian substorm occurence, Geophysical Research Letters, 35, L12105, doi:10.1029\/2008GL034080   List_of_Cassini_reconnection_events_extended extended by 600 min; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"10","surveyStart":"2004-07-01T15:50:00","surveyStop":"2006-09-07T01:40:01","sharedDate":"2018-01-19T15:00:55+00:00"},{"type":"timeTable","name":"HST_Proposal_11984","id":"sharedtimeTable_46","created":"2018-01-19T14:58:08","description":"Observing Saturn's high latitude polar auroras -- HST Proposal 11984 Jonathan Nichols, University of Leicester  http:\/\/archive.stsci.edu\/proposal_search.php?id=11984&mission=hst; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"20","surveyStart":"2009-02-17T04:20:43","surveyStop":"2009-03-07T04:37:09","sharedDate":"2018-01-19T15:01:04+00:00"},{"type":"timeTable","name":"List_of_Enceladus_flybys_2004_2010","id":"sharedtimeTable_47","created":"2018-01-19T14:58:34","description":"Includes targetted and untargetted flybys; done by Nicolas Andre ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"15","surveyStart":"2005-02-17T03:10:50","surveyStop":"2010-12-21T01:27:10","sharedDate":"2018-01-19T15:01:15+00:00"},{"type":"timeTable","name":"Cassini_MP_crossings_timetable","id":"sharedtimeTable_48","created":"2018-01-19T14:58:59","description":"Name: Cassini_MP_crossings_timetable;\nHistoric: Extended by 5 min;\nCreation Date:2017-10-06T14:07:06;\n\nList of Saturn's magnetopause crossings by Cassini obtained in Pilkington, N. M., N. Achilleos, C. S. Arridge, P. Guio, A. Masters, L. C. Ray, N. Sergis, M. F. Thomsen, A. J. Coates, and M. K. Dougherty (2015), Internally driven large-scale changes in the size of Saturn's magnetosphere, J. Geophys. Res. Space Physics, 120, 7289\u20137306, doi:10.1002\/2015JA021290.\nhttp:\/\/dx.doi.org\/10.1002\/2015JA021290\nCourtesy to A. Masters & N. Pilkington; \n        Historic: ;\n        Creation Date :  2017-11-02T14:33:11; \n ","nbIntervals":"1605","surveyStart":"2004-06-28T18:37:00","surveyStop":"2013-02-07T20:10:00","sharedDate":"2018-01-19T15:01:26+00:00"},{"type":"timeTable","name":"Magnetic_Clouds","id":"sharedtimeTable_22","created":"2018-01-19T10:38:55","description":"Magnetic Clouds from WIND\/MFI 1995-2007 -- Estimated start and end times from a magnetic field model [Lepping et al., 1990] which assumes that the field within the magnetic cloud is force free, i.e., so that the electrical current and the magnetic field are parallel and proportional in strength everywhere within its volume -- see http:\/\/lepmfi.gsfc.nasa.gov\/mfi\/mag_cloud_pub1.html ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"106","surveyStart":"1995-02-08T05:48:00","surveyStop":"2007-11-20T12:54:00","sharedDate":"2018-01-19T10:39:38+00:00"},{"type":"timeTable","name":"CIR_SAMPEX","id":"sharedtimeTable_23","created":"2018-01-19T10:50:55","description":"Corotating Interaction Regions from Mazur et al., APJ, 566, 2002, Charge States of Energetic Particles from Corotating Interaction Regions as Constraints on Their Source  http:\/\/iopscience.iop.org\/0004-637X\/566\/1\/555\/pdf\/0004-637X_566_1_555.pdf ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"14","surveyStart":"1992-12-08T00:00:00","surveyStop":"1995-06-02T00:00:00","sharedDate":"2018-01-19T10:51:12+00:00"},{"type":"timeTable","name":"ace_v_600","id":"sharedtimeTable_24","created":"2018-01-19T10:51:57","description":"ACE 1998-2009 ;  sw(1)>600;  sw(1): ACE SWEPAM swe_final v_bulk Units: km\/s;; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"975","surveyStart":"1998-05-02T04:20:10","surveyStop":"2009-02-28T07:09:40","sharedDate":"2018-01-19T10:52:13+00:00"},{"type":"timeTable","name":"reconnection_exhaust_Gosling","id":"sharedtimeTable_26","created":"2018-01-19T14:32:32","description":"ACE Magnetic Reconnection Exhaust List 31 December 2009 J. T. Gosling Acknowledgment: Tai Phan assisted in the identification of some of these events. Start times should be good to within better than 5 minutes. There probably are additional, as yet unidentified, events in the data, particularly after January 2006. Events were identified using the unedited SWEPAM data set available at Los Alamos. Some of these events are not obvious in the level 2 SWEPAM data because of the editing process used in producing the level 2 data set.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"148","surveyStart":"1997-11-04T01:09:00","surveyStop":"2007-03-11T05:23:01","sharedDate":"2018-01-19T14:35:22+00:00"},{"type":"timeTable","name":"CIR_Borovsky_Denton","id":"sharedtimeTable_27","created":"2018-01-19T14:36:34","description":"CIR list from Borovsky and Denton, JGR, 2010, http:\/\/dx.doi.org\/10.1029\/2009JA014966 The CIR events are picked with three criteria: (1) that they have a clear, dominant shear zone as seen in the local-Parker-spiral coordinate system, (2) that they do not contain interplanetary shocks, and (3) that they are followed by long (3 days or more) intervals of high-speed (600 km\/s or more) wind.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"27","surveyStart":"2003-05-05T10:30:00","surveyStop":"2008-11-25T04:30:01","sharedDate":"2018-01-19T14:36:48+00:00"},{"type":"timeTable","name":"Richardson_Cane_ICME_list","id":"sharedtimeTable_28","created":"2018-01-19T14:39:02","description":"Near-Earth Interplanetary Coronal Mass Ejections Since January 1996 - Updated 2011-04-11 See Richardson and Cane, Solar Physics, 2010 : http:\/\/dx.doi.org\/10.1007\/s11207-010-9568-6; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"341","surveyStart":"1996-05-27T15:00:00","surveyStop":"2011-03-31T04:00:00","sharedDate":"2018-01-19T14:39:14+00:00"},{"type":"timeTable","name":"interplanetary_shocks_Wind1995","id":"sharedtimeTable_29","created":"2018-01-19T14:39:51","description":"List of interplanetary shocks observed by the Wind spacecraft in 1995 and compiled by J. Kasper (jkasper@cfa.harvard.edu) \t ; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"21","surveyStart":"1995-01-01T19:36:00","surveyStop":"1995-12-24T05:57:01","sharedDate":"2018-01-19T14:40:02+00:00"},{"type":"timeTable","name":"Jian_SIR_list","id":"sharedtimeTable_30","created":"2018-01-19T14:40:27","description":"Stream Interaction Regions (SIR) from Wind and ACE Data during 1995-2009 Compiled by Dr. Lan Jian at UCLA\/IGPP. Latest Update on 21 April 2011 http:\/\/www-ssc.igpp.ucla.edu\/~jlan\/ACE\/Level3\/SIR_List_from_Lan_Jian.pdf The SIR include corotating interaction regions (CIR) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycles. Five of the following criteria are used for SIR identification: 1) overall increase of solar wind speed, 2) pile-up of total pressure with gradual declines at two sides, 3) enhancement of magnetic field, 4) first increase and then drop of proton number density, 5) increase of proton temperature, 6) change of entropy, 7) solar wind velocity deflection.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"577","surveyStart":"1995-01-01T19:37:00","surveyStop":"2009-12-26T10:00:00","sharedDate":"2018-01-19T14:40:35+00:00"},{"type":"timeTable","name":"Jian_CIR_list","id":"sharedtimeTable_31","created":"2018-01-19T14:41:13","description":"Corotating Interaction Regions (CIR) from Wind and ACE Data during 1995-2009 Compiled by Dr. Lan Jian at UCLA\/IGPP. Latest Update on 21 April 2011 http:\/\/www-ssc.igpp.ucla.edu\/~jlan\/ACE\/Level3\/SIR_List_from_Lan_Jian.pdf The SIR include corotating interaction regions (CIR) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycles. Five of the following criteria are used for SIR identification: 1) overall increase of solar wind speed, 2) pile-up of total pressure with gradual declines at two sides, 3) enhancement of magnetic field, 4) first increase and then drop of proton number density, 5) increase of proton temperature, 6) change of entropy, 7) solar wind velocity deflection.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"416","surveyStart":"1995-01-01T19:37:00","surveyStop":"2009-12-26T10:00:00","sharedDate":"2018-01-19T14:41:24+00:00"},{"type":"timeTable","name":"Jian_Stream_Interface_list","id":"sharedtimeTable_32","created":"2018-01-19T14:41:50","description":"Stream Interface (time of the discontinuity) from Wind and ACE Data during 1995-2009 Compiled by Dr. Lan Jian at UCLA\/IGPP. Latest Update on 21 April 2011 http:\/\/www-ssc.igpp.ucla.edu\/~jlan\/ACE\/Level3\/SIR_List_from_Lan_Jian.pdf The SIR include corotating interaction regions (CIR) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycles. Stream interface is the boundary between slow and fast streams. If the boundary is sharp and clear, we can see the drop of proton density and the increase of proton temperature simultaneously. However, only about 20% of SIRs have such sharp separation. To identify stream interface uniformly for all the SIRs, the interface is defined at the peak of total pressure.  The Start Time corresponds to the observed discontinuity. Stop Time = Start Time + 1 sec  Note that the discontinuity of the SIR 1995-11-27\/1995-11-29 cannot be determined because of a data gap.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"576","surveyStart":"1995-01-02T05:56:00","surveyStop":"2009-12-25T17:48:01","sharedDate":"2018-01-19T14:42:00+00:00"},{"type":"timeTable","name":"Jian_ICME_list","id":"sharedtimeTable_33","created":"2018-01-19T14:46:20","description":"Interplanetary Coronal Mass Ejections (ICMEs) from Wind and ACE Data during 1995 - 2009 Compiled by Dr. Lan Jian at UCLA\/IGPP. Latest Update on 25 October 2010 http:\/\/www-ssc.igpp.ucla.edu\/~jlan\/ACE\/Level3\/ICME_List_from_Lan_Jian.pdf ICMEs are identified requiring at least three of the following criteria: field enhancement, smooth field rotations over a relatively large scale, quieter field than background, low proton temperature, high alpha particle abundance, low beta, declining solar wind speed, bi-directional suprathermal electron flux, etc.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"290","surveyStart":"1995-02-08T03:10:00","surveyStop":"2009-12-13T22:39:00","sharedDate":"2018-01-19T14:46:30+00:00"},{"type":"timeTable","name":"Cartwright_Moldwin_flux_ropes_1AU","id":"sharedtimeTable_34","created":"2018-01-19T14:47:04","description":"List of Small-Scale Solar Wind Flux Ropes From \"Heliospheric evolution of solar wind small-scale magnetic flux ropes\", Cartwright and Moldwin, JGR, 2010 The list is here restricted to events at 1 AU from IMP 8, Wind, and ACE. The small-scale flux rope selection was done in three parts: (1) a visual survey of the solar wind magnetic field data sets, (2) a removal of compressive Alfven waves, and (3) a model validation of the events. http:\/\/dx.doi.org\/10.1029\/2009JA014271; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"164","surveyStart":"1975-05-29T15:10:00","surveyStop":"2007-11-30T14:14:00","sharedDate":"2018-01-19T14:47:14+00:00"},{"type":"timeTable","name":"shocksSTA_AMDA","id":"sharedtimeTable_35","created":"2018-01-19T14:47:41","description":"10 minute intervals centered on IP shocks from STEREO between 2007-december 2011.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"121","surveyStart":"2007-01-14T19:30:08","surveyStop":"2011-12-28T20:52:09","sharedDate":"2018-01-19T14:47:52+00:00"},{"type":"timeTable","name":"shocksSTB_AMDA","id":"sharedtimeTable_36","created":"2018-01-19T14:48:15","description":"10 minute intervals centered on IP shocks from STEREO between 2007-december 2011.; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"115","surveyStart":"2007-01-14T19:56:27","surveyStop":"2011-12-26T23:55:46","sharedDate":"2018-01-19T14:48:24+00:00"},{"type":"timeTable","name":"SERPENTINE_shock_STA_cycle25","id":"sharedtimeTable_175","created":"2024-04-22T03:45:59.000000","description":"In-situ shock crossings at STEREO-A catalogued in WP4 of SERPENTINE H2020 project (responsible: D. Trotta)","nbIntervals":"33","surveyStart":"2020-12-01T07:28:00.000","surveyStop":"2023-05-19T16:28:00.000","sharedDate":"2024-04-23T11:54:07+00:00"},{"type":"timeTable","name":"Solar_Proton_Events","id":"sharedtimeTable_18","created":"2018-01-18T16:53:48","description":"Solar Proton Events list from SWPC - see http:\/\/www.swpc.noaa.gov\/ftpdir\/indices\/SPE.txt ; Particle events ; Time span = January 1976 - December 2008 ; Start time= Start time, Stop time = Maximum time; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:49; \n ","nbIntervals":"221","surveyStart":"1970-01-01T00:00:00","surveyStop":"2006-12-13T09:25:00","sharedDate":"2018-01-18T16:54:39+00:00"},{"type":"timeTable","name":"carrington_rotation","id":"sharedtimeTable_21","created":"2018-01-18T16:55:25","description":"Carrington rotation dates (rotations 1 to 2171) -- rounded to the closest second; \n        Historic: From old AMDA;\n        Creation Date :  2013-11-22T13:52:50; \n ","nbIntervals":"2170","surveyStart":"1970-01-21T06:59:02","surveyStop":"2106-01-31T05:23:54","sharedDate":"2018-01-18T17:07:29+00:00"},{"type":"timeTable","name":"sep_SERPENTINE_STA_cycle25","id":"sharedtimeTable_177","created":"2024-04-22T05:24:05.000000","description":"SEP events (flare time, protons 25MeV peak time) at STA catalogued for solar cylce 25 as part of SERPENTINE H2020 project, WP2 (resp. Nina Dresing)","nbIntervals":"35","surveyStart":"2020-11-29T12:34:00.000","surveyStop":"2023-05-17T04:20:20.000","sharedDate":"2024-04-23T11:58:05+00:00"},{"type":"timeTable","name":"sep_SERPENTINE_SOLO_cycle25","id":"sharedtimeTable_178","created":"2024-04-22T05:24:37.000000","description":"SEP events (flare time, protons 25MeV peak time) at Solar Orbiter catalogued for solar cylce 25 as part of SERPENTINE H2020 project, WP2 (resp. Nina Dresing)","nbIntervals":"25","surveyStart":"2020-11-29T12:34:00.000","surveyStop":"2023-05-16T20:10:10.000","sharedDate":"2024-04-23T11:58:21+00:00"},{"type":"timeTable","name":"sep_SERPENTINE_Bepi_cycle25","id":"sharedtimeTable_179","created":"2024-04-22T05:28:37.000000","description":"SEP events (flare time, protons 25MeV peak time) at Bepi Colombo catalogued for solar cylce 25 as part of SERPENTINE H2020 project, WP2 (resp. Nina Dresing)","nbIntervals":"11","surveyStart":"2021-04-17T16:03:00.000","surveyStop":"2023-05-16T19:15:15.000","sharedDate":"2024-04-23T11:58:36+00:00"},{"type":"timeTable","name":"sep_SERPENTINE_L1_cycle25","id":"sharedtimeTable_180","created":"2024-04-22T05:29:04.000000","description":"SEP events (flare time, protons 25MeV peak time) at L1 catalogued for solar cylce 25 as part of SERPENTINE H2020 project, WP2 (resp. Nina Dresing)","nbIntervals":"44","surveyStart":"2020-11-29T12:34:00.000","surveyStop":"2023-05-17T00:06:06.000","sharedDate":"2024-04-23T11:58:51+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2015August","id":"sharedtimeTable_68","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"587","surveyStart":"2015-08-01T00:39:34","surveyStop":"2015-08-31T18:40:14","sharedDate":"2025-05-04T20:27:23+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2015September","id":"sharedtimeTable_69","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"700","surveyStart":"2015-09-01T12:11:14","surveyStop":"2015-09-30T16:43:04","sharedDate":"2025-05-04T20:27:30+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2015October","id":"sharedtimeTable_70","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"871","surveyStart":"2015-10-01T06:49:14","surveyStop":"2015-10-31T15:24:34","sharedDate":"2025-05-04T20:27:34+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2015November","id":"sharedtimeTable_71","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"658","surveyStart":"2015-11-01T03:23:14","surveyStop":"2015-11-30T13:07:34","sharedDate":"2025-05-04T20:27:38+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2015December","id":"sharedtimeTable_72","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"841","surveyStart":"2015-12-01T00:19:33","surveyStop":"2015-12-31T23:45:44","sharedDate":"2025-05-04T20:27:42+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016January","id":"sharedtimeTable_73","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"878","surveyStart":"2016-01-01T00:56:44","surveyStop":"2016-01-31T23:47:34","sharedDate":"2025-05-04T20:27:46+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016February","id":"sharedtimeTable_74","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1083","surveyStart":"2016-02-01T06:18:54","surveyStop":"2016-02-29T23:45:14","sharedDate":"2025-05-04T20:27:50+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016March","id":"sharedtimeTable_75","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"527","surveyStart":"2016-03-01T00:29:15","surveyStop":"2016-03-31T23:14:04","sharedDate":"2025-05-04T20:27:54+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016April","id":"sharedtimeTable_76","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1238","surveyStart":"2016-04-01T16:37:14","surveyStop":"2016-04-30T21:19:24","sharedDate":"2025-05-04T20:27:58+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016May","id":"sharedtimeTable_77","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1940","surveyStart":"2016-05-01T10:38:24","surveyStop":"2016-05-31T15:49:44","sharedDate":"2025-05-04T20:28:02+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016June","id":"sharedtimeTable_78","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"812","surveyStart":"2016-06-01T05:49:24","surveyStop":"2016-06-30T16:52:04","sharedDate":"2025-05-04T20:28:06+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016July","id":"sharedtimeTable_79","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1144","surveyStart":"2016-07-01T00:54:14","surveyStop":"2016-07-31T10:39:14","sharedDate":"2025-05-04T20:28:10+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016August","id":"sharedtimeTable_80","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1559","surveyStart":"2016-08-01T01:49:54","surveyStop":"2016-08-31T23:58:54","sharedDate":"2025-05-04T20:28:14+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016September","id":"sharedtimeTable_81","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1594","surveyStart":"2016-09-01T02:06:04","surveyStop":"2016-09-30T22:58:44","sharedDate":"2025-05-04T20:28:18+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016October","id":"sharedtimeTable_82","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1083","surveyStart":"2016-10-01T17:57:14","surveyStop":"2016-10-31T13:05:04","sharedDate":"2025-05-04T20:28:21+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016November","id":"sharedtimeTable_83","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1048","surveyStart":"2016-11-01T09:13:44","surveyStop":"2016-11-30T15:49:24","sharedDate":"2025-05-04T20:28:25+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2016December","id":"sharedtimeTable_84","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1067","surveyStart":"2016-12-01T05:24:48","surveyStop":"2016-12-31T13:31:04","sharedDate":"2025-05-04T20:28:29+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2017January","id":"sharedtimeTable_85","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"1228","surveyStart":"2017-01-01T01:51:33","surveyStop":"2017-01-31T12:18:23","sharedDate":"2025-05-04T20:28:33+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2017February","id":"sharedtimeTable_86","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"386","surveyStart":"2017-02-03T22:55:43","surveyStop":"2017-02-28T00:04:33","sharedDate":"2025-05-04T20:28:37+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2017March","id":"sharedtimeTable_87","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"36","surveyStart":"2017-03-01T07:04:13","surveyStop":"2017-03-22T23:10:13","sharedDate":"2025-05-04T20:28:41+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2017April","id":"sharedtimeTable_88","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: http:\/\/mmsburst.sr.unh.edu\/","nbIntervals":"646","surveyStart":"2017-04-08T09:04:13","surveyStop":"2017-04-30T19:35:03","sharedDate":"2025-05-04T20:28:45+00:00"},{"type":"timeTable","name":"MMS_Burst_Mode_2017May","id":"sharedtimeTable_89","created":"2020-08-26T00:00:55","description":"Time intervals for which MMS burst mode data are available. source: 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