data set : JUNO J/SW JOVIAN AURORAL DISTRIBUTION CALIBRATED V1.0
This data set consists of all of the calibrated data collected by the JADE (Jovian Auroral Plasma Distributions Experiment) on-board the Juno spacecraft. For more information about the instrument and data sets, see [MCCOMASETAL2017B] and [WILSON2016].

data set : JUNO J ENERGETIC PARTICLE DETECTOR UNCALIBRATED V1.0
The JUNO JEDI uncalibrated observations consist of energetic particle data collected by the JEDI instruments during Jupiter Science Orbit operations of the JUNO mission.

data set : JNO J JED 3 CDR V1.0
The JUNO JEDI calibrated observations consist of energetic particle data collected by the JEDI instruments during Jupiter Science Orbit operations of the JUNO mission.

data set : JUNO E/J/S/SS WAVES EXPERIMENT DATA RECORDS V1.0
The Juno Waves EDR complete data set includes all Waves science and housekeeping instrument packets for the entire Juno mission.

data set : JUNO E/J/S/SS WAVES CALIBRATED BURST FULL RESOLUTION V2.0
The Juno Waves calibrated burst waveform full resolution data set includes all high rate science waveform information calibrated in units of electric or magnetic field for the entire Juno mission.

data set : JUNO E/J/SS WAVES CALIBRATED SURVEY FULL RESOLUTION V2.0
The Juno Waves calibrated full resolution survey data set includes all low rate science spectral information calibrated in units of spectral density for the entire Juno mission.

data set : MARS EXPRESS MARS HRSC 4 MESOSPHERIC CLOUDS V1.0
Mars Express Legacy Archive HRSC mesospheric cloud dataset

data set : MARS EXPRESS MARS OMEGA 4 ATMOSPHERIC PROFILES V1.0
Mars Express Legacy Archive Piccialli et al. 2016 dataset

data set : MEX-M-OMEGA-5-DDR-H2OCLOUDS-MAPS-V1.0
Mars Express Legacy Archive Szantai et al. 2024 dataset

data set : MARS EXPRESS MARS PFS 5 DERIVED MAPS V1.0
Mars Express Legacy Archive Sindoni et al. 2011 dataset

data set : MARS EXPRESS MARS SPICAM 4 IR ATMOSPHERIC PROFILES V1.0
Mars Express Legacy Archive Fedorova et al. 2021 dataset

data set : MARS EXPRESS MARS SPICAM 4 UV ATMOSPHERIC PROFILES V1.0
Mars Express Legacy Archive Forget et al. 2009 dataset

data set : MARS EXPRESS MARS MRS 5 OCCULTATION 9102 V1.0
This is a Mars Express Radio Science data set, collected during the occultation season 02 2004-12-08 to 2005-01-04.

data set : OMEGA FLIGHT EXPERIMENT DATA RECORDS FROM NINTH MISSION EXT
N/A

data set : MEX MARS VMC RAW DATA EXT9 V1.0
Raw data from the Visual Monitoring Camera on Mars Express.

data set : MEX MARS VMC CALIBRATED DATA EXT9 V1.0
Calibrated data from the Visual Monitoring Camera on Mars Express.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4441 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-23T14:13:32.100 to 2024-03-23T14:35:40.300.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4442 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-24T04:12:09.000 to 2024-03-24T04:34:17.000.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4444 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-26T05:07:23.300 to 2024-03-26T05:29:31.300.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4446 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-27T02:05:21.400 to 2024-03-27T02:27:27.300.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4447 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-28T06:02:43.200 to 2024-03-28T06:24:51.200.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4449 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-29T23:58:52.200 to 2024-03-30T00:21:00.700.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4450 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-03-30T06:58:10.300 to 2024-03-30T07:20:18.200.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4453 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-10-27T06:34:36.300 to 2024-10-27T06:54:48.000.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4458 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-11-29T17:06:24.000 to 2024-11-29T17:28:32.100.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4468 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-12-27T09:13:44.100 to 2024-12-27T09:35:51.800.

data set : MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 9 4469 V1.0
This is a MEX MaRS Occultation measurement covering the time 2024-12-28T06:11:58.000 to 2024-12-28T06:34:05.700.

collection : urn:nasa:pds:context:facility:* context products
The PDS4 Context Products for Facilities, e.g. Keck Observatory, A. Hofmeister Laboratory

bundle : BepiColombo MCAM bundle
The BepiColombo MTM MCAM bundle contains all images and contextual informationfor the monitoring cameras onboard the Mercury Transfer Module of the BepiColombo mission

bundle : PSA Bundle
PSA Master Bundle

bundle : Instrument FREND
ExoMars 2016 FREND Bundle

target : HD 48915
HD 48915, alf CMa

target : HD 93521
HD 93521

target : Zeta Cassiopeiae
Zeta Cassiopeiae

target : HR 1996
HR 1996

target : HD 172167
Target Context for Vega

target : Landolt SA 92
The Landolt standards are based on [Landolt 1992] above. Title: UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equatorJournal: Astronomical Journal (ISSN 0004-6256), vol. 104, no. 1, July 1992, p. 340-371, 436-491. Research supported by Space Telescope Science Institute.DOI: 10.1086/116242

target : HD 100889
HD 100889

target : Landolt SA 104
The Landolt standards are based on [Landolt 1992] above. Title: UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equatorJournal: Astronomical Journal (ISSN 0004-6256), vol. 104, no. 1, July 1992, p. 340-371, 436-491. Research supported by Space Telescope Science Institute.DOI: 10.1086/116242

target : HD 15318
HD 15318, Xi Orionis

target : HD 30739
HD 30739

target : HD 42560
HD 45260, Xi Orionis

target : PLEIADES
Target Context for Pleiades

bundle : PSA Context Bundle
PSA Context Bundle

facility : ESA's tracking station network ESTRACK
ESA's tracking station network – Estrack – is a global system of ground stations providing links between satellites in orbit and ESOC, the European Space Operations Centre, Darmstadt, Germany. The core Estrack network comprises seven stations in seven countries. The essential task of all ESA ground tracking stations is to communicate with spacecraft, transmitting commands and receiving scientific data and spacecraft status information.

instrument : Camera System (Jupiter Amorum ac Natorum Undique Scrutator)
The BepiColombo mission is designed to orbit Mercury after one swingby at planet Earth and two swingbys at Venus. It has been launched on October 20, 2018 in Kourou, French Guayana and will use the swingbys to slow down and reach Mercury first in October 2021. During the long cruise phase, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena. The magnetic field data collected during the Earth swingby have been used to improve the calibration and to fine tune the instrument SPICE frame kernels. The magnetic field observation at Venus will augment the knowledge of the Venus magnetosphere. Stable orbits around Mercury can be flown from 2025 onwards after lots of complex manoeuvres, the separation of the Mercury Planetary Orbiter (MPO), the Mercury Transfer Module (MTM), and the Mercury Magnetospheric Orbiter (MMO, so called MIO). MPO will be injected into an initial 480 km ×1500 km polar orbit around Mercury with a 2.3h orbital period. At Mercury, we will conduct a global mapping of the planetary magnetic field, determine the dynamo generated field and investigate the secular variation. Furthermore, the study of induced magnetic fields and field-aligned currents will help to reveal the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument the MIO-MGF on-board the MIO spacecraft, the magnetometers at Mercury will investigate the reaction of the highly dynamic magnetosphere to changes in the solar wind. The magnetometer instrument MPO-MAG on-board the MPO spacecraft has been provided by the Institute for Geophysics and extraterrestrial Physics at the Technische Universitaet Braunschweig, Germany under lead of the PI Daniel Heyner. The instrument comprises two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They observe the magnetic field with vector rates of up to 128 Hz at a maximum range of +-2048 nT. For the sake of a flexible adaption to occurring telemetry (TM) restrictions the vector rate can be set to 0.5 Hz, 1 Hz, 2 Hz, 4 Hz, 16 Hz, 32 Hz, 64 Hz, and 128 Hz. For an optimal adaption to the ambient magnetic field the instrument can be operated in the following ranges (+-): 8 nT, 16 nT, 32 nT, 64 nT, 128 nT, 256 nT, 1024 nT, 2048 nT. Furthermore the data can be compressed before the downlink in order to shrink the transmitted TM volume. A special feature is the so called Selective Downlink (S/D) mode minimizing the downlink TM volume drastically. Here, the instrument is operated at full data rate and stores the high resolution data in an onboard ring buffer, but does not send them down. Only a low sampled data stream is generated in parallel and instantaneously transmitted to Earth, where the data are analysed in order to detect special features. According to a possibly detected event the transmission of a limited set of high resolution data from the buffer will be triggered. For maintenance purposes the instrument is equipped with several calibration and special modes. The magnetometer is a fully digital instrument, where the magnetic field signal measured by the sensor is amplified and immediately converted into its digital equivalent, which acts as input to an FPGA. This device generates a dynamic digital feedback signal, which is converted into an analogue feedback signal and connected to the sensor’s feedback coil. Additionally the FPGA generates the excitation signal that is conditioned by the drive electronics before injection to the excitation coil. On the other side, the FPGA is connected to the Instrument Controller, which collects the magnetic field data and controls the magnetometer. Besides the science data of both sensors also housekeeping data (HK) is generated for a proper surveillance of the instrument. The science data are made available to the public via the Planetary Science Archive (PSA) hosted by ESA and the Planetary Data System (PDS) operated by NASA. Data are provided at different processing levels (raw, calibrated, derived) and various convenient coordinate systems (unit reference frame: URF, s/c-frame: SCF, celestial coordinates like e.g. ECLIPJ2000: E2K). The data are PDS4 compliant and organized by calibration level, mission phases, sensor, coordinate system, and measurement rate. They are clustered in files on daily basis. Although MPO-MAG is located on a boom, spacecraft magnetic disturbance fields have a high impact on the magnetic field observations. The disturbances are manifold. They are present at DC as well as on AC level and are caused by varying s/c currents, thruster and reaction wheel operations due to AOCS needs, P/L activities and possibly other sources. All these disturbances are subject to advanced data cleaning procedures under permanent improvements. We hold the calibration dear for the maximization of the resolution and the S/N ratio of the expected tiny magnetic signatures in order to reveal more secrets of Mercury's interior structure. Finally a general warning is stated here: * Use the data with caution and analytic expertise. * Please read the provided documentation carefully. * In any doubt of the "realness" of a detected structure please contact the PI team for clarification. The MPOMAG instrument is described in full detail in [HEYNERETAL2020]. The Experiment to Archive Interface Control Document [RICHTERTAL2020] is part of current the dataset. The Experiment User Manual [FISCHERETAL2017] is also part of this dataset.

instrument : Radiation Monitor
The BepiColombo mission is designed to orbit Mercury after one swingby at planet Earth and two swingbys at Venus. It has been launched on October 20, 2018 in Kourou, French Guayana and will use the swingbys to slow down and reach Mercury first in October 2021. During the long cruise phase, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena. The magnetic field data collected during the Earth swingby have been used to improve the calibration and to fine tune the instrument SPICE frame kernels. The magnetic field observation at Venus will augment the knowledge of the Venus magnetosphere. Stable orbits around Mercury can be flown from 2025 onwards after lots of complex manoeuvres, the separation of the Mercury Planetary Orbiter (MPO), the Mercury Transfer Module (MTM), and the Mercury Magnetospheric Orbiter (MMO, so called MIO). MPO will be injected into an initial 480 km ×1500 km polar orbit around Mercury with a 2.3h orbital period. At Mercury, we will conduct a global mapping of the planetary magnetic field, determine the dynamo generated field and investigate the secular variation. Furthermore, the study of induced magnetic fields and field-aligned currents will help to reveal the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument the MIO-MGF on-board the MIO spacecraft, the magnetometers at Mercury will investigate the reaction of the highly dynamic magnetosphere to changes in the solar wind. The magnetometer instrument MPO-MAG on-board the MPO spacecraft has been provided by the Institute for Geophysics and extraterrestrial Physics at the Technische Universitaet Braunschweig, Germany under lead of the PI Daniel Heyner. The instrument comprises two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They observe the magnetic field with vector rates of up to 128 Hz at a maximum range of +-2048 nT. For the sake of a flexible adaption to occurring telemetry (TM) restrictions the vector rate can be set to 0.5 Hz, 1 Hz, 2 Hz, 4 Hz, 16 Hz, 32 Hz, 64 Hz, and 128 Hz. For an optimal adaption to the ambient magnetic field the instrument can be operated in the following ranges (+-): 8 nT, 16 nT, 32 nT, 64 nT, 128 nT, 256 nT, 1024 nT, 2048 nT. Furthermore the data can be compressed before the downlink in order to shrink the transmitted TM volume. A special feature is the so called Selective Downlink (S/D) mode minimizing the downlink TM volume drastically. Here, the instrument is operated at full data rate and stores the high resolution data in an onboard ring buffer, but does not send them down. Only a low sampled data stream is generated in parallel and instantaneously transmitted to Earth, where the data are analysed in order to detect special features. According to a possibly detected event the transmission of a limited set of high resolution data from the buffer will be triggered. For maintenance purposes the instrument is equipped with several calibration and special modes. The magnetometer is a fully digital instrument, where the magnetic field signal measured by the sensor is amplified and immediately converted into its digital equivalent, which acts as input to an FPGA. This device generates a dynamic digital feedback signal, which is converted into an analogue feedback signal and connected to the sensor’s feedback coil. Additionally the FPGA generates the excitation signal that is conditioned by the drive electronics before injection to the excitation coil. On the other side, the FPGA is connected to the Instrument Controller, which collects the magnetic field data and controls the magnetometer. Besides the science data of both sensors also housekeeping data (HK) is generated for a proper surveillance of the instrument. The science data are made available to the public via the Planetary Science Archive (PSA) hosted by ESA and the Planetary Data System (PDS) operated by NASA. Data are provided at different processing levels (raw, calibrated, derived) and various convenient coordinate systems (unit reference frame: URF, s/c-frame: SCF, celestial coordinates like e.g. ECLIPJ2000: E2K). The data are PDS4 compliant and organized by calibration level, mission phases, sensor, coordinate system, and measurement rate. They are clustered in files on daily basis. Although MPO-MAG is located on a boom, spacecraft magnetic disturbance fields have a high impact on the magnetic field observations. The disturbances are manifold. They are present at DC as well as on AC level and are caused by varying s/c currents, thruster and reaction wheel operations due to AOCS needs, P/L activities and possibly other sources. All these disturbances are subject to advanced data cleaning procedures under permanent improvements. We hold the calibration dear for the maximization of the resolution and the S/N ratio of the expected tiny magnetic signatures in order to reveal more secrets of Mercury's interior structure. Finally a general warning is stated here: * Use the data with caution and analytic expertise. * Please read the provided documentation carefully. * In any doubt of the "realness" of a detected structure please contact the PI team for clarification. The MPOMAG instrument is described in full detail in [HEYNERETAL2020]. The Experiment to Archive Interface Control Document [RICHTERTAL2020] is part of current the dataset. The Experiment User Manual [FISCHERETAL2017] is also part of this dataset.

instrument : Radar for Icy Moons Exploration
The BepiColombo mission is designed to orbit Mercury after one swingby at planet Earth and two swingbys at Venus. It has been launched on October 20, 2018 in Kourou, French Guayana and will use the swingbys to slow down and reach Mercury first in October 2021. During the long cruise phase, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena. The magnetic field data collected during the Earth swingby have been used to improve the calibration and to fine tune the instrument SPICE frame kernels. The magnetic field observation at Venus will augment the knowledge of the Venus magnetosphere. Stable orbits around Mercury can be flown from 2025 onwards after lots of complex manoeuvres, the separation of the Mercury Planetary Orbiter (MPO), the Mercury Transfer Module (MTM), and the Mercury Magnetospheric Orbiter (MMO, so called MIO). MPO will be injected into an initial 480 km ×1500 km polar orbit around Mercury with a 2.3h orbital period. At Mercury, we will conduct a global mapping of the planetary magnetic field, determine the dynamo generated field and investigate the secular variation. Furthermore, the study of induced magnetic fields and field-aligned currents will help to reveal the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument the MIO-MGF on-board the MIO spacecraft, the magnetometers at Mercury will investigate the reaction of the highly dynamic magnetosphere to changes in the solar wind. The magnetometer instrument MPO-MAG on-board the MPO spacecraft has been provided by the Institute for Geophysics and extraterrestrial Physics at the Technische Universitaet Braunschweig, Germany under lead of the PI Daniel Heyner. The instrument comprises two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They observe the magnetic field with vector rates of up to 128 Hz at a maximum range of +-2048 nT. For the sake of a flexible adaption to occurring telemetry (TM) restrictions the vector rate can be set to 0.5 Hz, 1 Hz, 2 Hz, 4 Hz, 16 Hz, 32 Hz, 64 Hz, and 128 Hz. For an optimal adaption to the ambient magnetic field the instrument can be operated in the following ranges (+-): 8 nT, 16 nT, 32 nT, 64 nT, 128 nT, 256 nT, 1024 nT, 2048 nT. Furthermore the data can be compressed before the downlink in order to shrink the transmitted TM volume. A special feature is the so called Selective Downlink (S/D) mode minimizing the downlink TM volume drastically. Here, the instrument is operated at full data rate and stores the high resolution data in an onboard ring buffer, but does not send them down. Only a low sampled data stream is generated in parallel and instantaneously transmitted to Earth, where the data are analysed in order to detect special features. According to a possibly detected event the transmission of a limited set of high resolution data from the buffer will be triggered. For maintenance purposes the instrument is equipped with several calibration and special modes. The magnetometer is a fully digital instrument, where the magnetic field signal measured by the sensor is amplified and immediately converted into its digital equivalent, which acts as input to an FPGA. This device generates a dynamic digital feedback signal, which is converted into an analogue feedback signal and connected to the sensor’s feedback coil. Additionally the FPGA generates the excitation signal that is conditioned by the drive electronics before injection to the excitation coil. On the other side, the FPGA is connected to the Instrument Controller, which collects the magnetic field data and controls the magnetometer. Besides the science data of both sensors also housekeeping data (HK) is generated for a proper surveillance of the instrument. The science data are made available to the public via the Planetary Science Archive (PSA) hosted by ESA and the Planetary Data System (PDS) operated by NASA. Data are provided at different processing levels (raw, calibrated, derived) and various convenient coordinate systems (unit reference frame: URF, s/c-frame: SCF, celestial coordinates like e.g. ECLIPJ2000: E2K). The data are PDS4 compliant and organized by calibration level, mission phases, sensor, coordinate system, and measurement rate. They are clustered in files on daily basis. Although MPO-MAG is located on a boom, spacecraft magnetic disturbance fields have a high impact on the magnetic field observations. The disturbances are manifold. They are present at DC as well as on AC level and are caused by varying s/c currents, thruster and reaction wheel operations due to AOCS needs, P/L activities and possibly other sources. All these disturbances are subject to advanced data cleaning procedures under permanent improvements. We hold the calibration dear for the maximization of the resolution and the S/N ratio of the expected tiny magnetic signatures in order to reveal more secrets of Mercury's interior structure. Finally a general warning is stated here: * Use the data with caution and analytic expertise. * Please read the provided documentation carefully. * In any doubt of the "realness" of a detected structure please contact the PI team for clarification. The MPOMAG instrument is described in full detail in [HEYNERETAL2020]. The Experiment to Archive Interface Control Document [RICHTERTAL2020] is part of current the dataset. The Experiment User Manual [FISCHERETAL2017] is also part of this dataset.

instrument : Particle Environment Package
The BepiColombo mission is designed to orbit Mercury after one swingby at planet Earth and two swingbys at Venus. It has been launched on October 20, 2018 in Kourou, French Guayana and will use the swingbys to slow down and reach Mercury first in October 2021. During the long cruise phase, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena. The magnetic field data collected during the Earth swingby have been used to improve the calibration and to fine tune the instrument SPICE frame kernels. The magnetic field observation at Venus will augment the knowledge of the Venus magnetosphere. Stable orbits around Mercury can be flown from 2025 onwards after lots of complex manoeuvres, the separation of the Mercury Planetary Orbiter (MPO), the Mercury Transfer Module (MTM), and the Mercury Magnetospheric Orbiter (MMO, so called MIO). MPO will be injected into an initial 480 km ×1500 km polar orbit around Mercury with a 2.3h orbital period. At Mercury, we will conduct a global mapping of the planetary magnetic field, determine the dynamo generated field and investigate the secular variation. Furthermore, the study of induced magnetic fields and field-aligned currents will help to reveal the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument the MIO-MGF on-board the MIO spacecraft, the magnetometers at Mercury will investigate the reaction of the highly dynamic magnetosphere to changes in the solar wind. The magnetometer instrument MPO-MAG on-board the MPO spacecraft has been provided by the Institute for Geophysics and extraterrestrial Physics at the Technische Universitaet Braunschweig, Germany under lead of the PI Daniel Heyner. The instrument comprises two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They observe the magnetic field with vector rates of up to 128 Hz at a maximum range of +-2048 nT. For the sake of a flexible adaption to occurring telemetry (TM) restrictions the vector rate can be set to 0.5 Hz, 1 Hz, 2 Hz, 4 Hz, 16 Hz, 32 Hz, 64 Hz, and 128 Hz. For an optimal adaption to the ambient magnetic field the instrument can be operated in the following ranges (+-): 8 nT, 16 nT, 32 nT, 64 nT, 128 nT, 256 nT, 1024 nT, 2048 nT. Furthermore the data can be compressed before the downlink in order to shrink the transmitted TM volume. A special feature is the so called Selective Downlink (S/D) mode minimizing the downlink TM volume drastically. Here, the instrument is operated at full data rate and stores the high resolution data in an onboard ring buffer, but does not send them down. Only a low sampled data stream is generated in parallel and instantaneously transmitted to Earth, where the data are analysed in order to detect special features. According to a possibly detected event the transmission of a limited set of high resolution data from the buffer will be triggered. For maintenance purposes the instrument is equipped with several calibration and special modes. The magnetometer is a fully digital instrument, where the magnetic field signal measured by the sensor is amplified and immediately converted into its digital equivalent, which acts as input to an FPGA. This device generates a dynamic digital feedback signal, which is converted into an analogue feedback signal and connected to the sensor’s feedback coil. Additionally the FPGA generates the excitation signal that is conditioned by the drive electronics before injection to the excitation coil. On the other side, the FPGA is connected to the Instrument Controller, which collects the magnetic field data and controls the magnetometer. Besides the science data of both sensors also housekeeping data (HK) is generated for a proper surveillance of the instrument. The science data are made available to the public via the Planetary Science Archive (PSA) hosted by ESA and the Planetary Data System (PDS) operated by NASA. Data are provided at different processing levels (raw, calibrated, derived) and various convenient coordinate systems (unit reference frame: URF, s/c-frame: SCF, celestial coordinates like e.g. ECLIPJ2000: E2K). The data are PDS4 compliant and organized by calibration level, mission phases, sensor, coordinate system, and measurement rate. They are clustered in files on daily basis. Although MPO-MAG is located on a boom, spacecraft magnetic disturbance fields have a high impact on the magnetic field observations. The disturbances are manifold. They are present at DC as well as on AC level and are caused by varying s/c currents, thruster and reaction wheel operations due to AOCS needs, P/L activities and possibly other sources. All these disturbances are subject to advanced data cleaning procedures under permanent improvements. We hold the calibration dear for the maximization of the resolution and the S/N ratio of the expected tiny magnetic signatures in order to reveal more secrets of Mercury's interior structure. Finally a general warning is stated here: * Use the data with caution and analytic expertise. * Please read the provided documentation carefully. * In any doubt of the "realness" of a detected structure please contact the PI team for clarification. The MPOMAG instrument is described in full detail in [HEYNERETAL2020]. The Experiment to Archive Interface Control Document [RICHTERTAL2020] is part of current the dataset. The Experiment User Manual [FISCHERETAL2017] is also part of this dataset.

instrument : GAnymede Laser Altimeter
The BepiColombo mission is designed to orbit Mercury after one swingby at planet Earth and two swingbys at Venus. It has been launched on October 20, 2018 in Kourou, French Guayana and will use the swingbys to slow down and reach Mercury first in October 2021. During the long cruise phase, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena. The magnetic field data collected during the Earth swingby have been used to improve the calibration and to fine tune the instrument SPICE frame kernels. The magnetic field observation at Venus will augment the knowledge of the Venus magnetosphere. Stable orbits around Mercury can be flown from 2025 onwards after lots of complex manoeuvres, the separation of the Mercury Planetary Orbiter (MPO), the Mercury Transfer Module (MTM), and the Mercury Magnetospheric Orbiter (MMO, so called MIO). MPO will be injected into an initial 480 km ×1500 km polar orbit around Mercury with a 2.3h orbital period. At Mercury, we will conduct a global mapping of the planetary magnetic field, determine the dynamo generated field and investigate the secular variation. Furthermore, the study of induced magnetic fields and field-aligned currents will help to reveal the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument the MIO-MGF on-board the MIO spacecraft, the magnetometers at Mercury will investigate the reaction of the highly dynamic magnetosphere to changes in the solar wind. The magnetometer instrument MPO-MAG on-board the MPO spacecraft has been provided by the Institute for Geophysics and extraterrestrial Physics at the Technische Universitaet Braunschweig, Germany under lead of the PI Daniel Heyner. The instrument comprises two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They observe the magnetic field with vector rates of up to 128 Hz at a maximum range of +-2048 nT. For the sake of a flexible adaption to occurring telemetry (TM) restrictions the vector rate can be set to 0.5 Hz, 1 Hz, 2 Hz, 4 Hz, 16 Hz, 32 Hz, 64 Hz, and 128 Hz. For an optimal adaption to the ambient magnetic field the instrument can be operated in the following ranges (+-): 8 nT, 16 nT, 32 nT, 64 nT, 128 nT, 256 nT, 1024 nT, 2048 nT. Furthermore the data can be compressed before the downlink in order to shrink the transmitted TM volume. A special feature is the so called Selective Downlink (S/D) mode minimizing the downlink TM volume drastically. Here, the instrument is operated at full data rate and stores the high resolution data in an onboard ring buffer, but does not send them down. Only a low sampled data stream is generated in parallel and instantaneously transmitted to Earth, where the data are analysed in order to detect special features. According to a possibly detected event the transmission of a limited set of high resolution data from the buffer will be triggered. For maintenance purposes the instrument is equipped with several calibration and special modes. The magnetometer is a fully digital instrument, where the magnetic field signal measured by the sensor is amplified and immediately converted into its digital equivalent, which acts as input to an FPGA. This device generates a dynamic digital feedback signal, which is converted into an analogue feedback signal and connected to the sensor’s feedback coil. Additionally the FPGA generates the excitation signal that is conditioned by the drive electronics before injection to the excitation coil. On the other side, the FPGA is connected to the Instrument Controller, which collects the magnetic field data and controls the magnetometer. Besides the science data of both sensors also housekeeping data (HK) is generated for a proper surveillance of the instrument. The science data are made available to the public via the Planetary Science Archive (PSA) hosted by ESA and the Planetary Data System (PDS) operated by NASA. Data are provided at different processing levels (raw, calibrated, derived) and various convenient coordinate systems (unit reference frame: URF, s/c-frame: SCF, celestial coordinates like e.g. ECLIPJ2000: E2K). The data are PDS4 compliant and organized by calibration level, mission phases, sensor, coordinate system, and measurement rate. They are clustered in files on daily basis. Although MPO-MAG is located on a boom, spacecraft magnetic disturbance fields have a high impact on the magnetic field observations. The disturbances are manifold. They are present at DC as well as on AC level and are caused by varying s/c currents, thruster and reaction wheel operations due to AOCS needs, P/L activities and possibly other sources. All these disturbances are subject to advanced data cleaning procedures under permanent improvements. We hold the calibration dear for the maximization of the resolution and the S/N ratio of the expected tiny magnetic signatures in order to reveal more secrets of Mercury's interior structure. Finally a general warning is stated here: * Use the data with caution and analytic expertise. * Please read the provided documentation carefully. * In any doubt of the "realness" of a detected structure please contact the PI team for clarification. The MPOMAG instrument is described in full detail in [HEYNERETAL2020]. The Experiment to Archive Interface Control Document [RICHTERTAL2020] is part of current the dataset. The Experiment User Manual [FISCHERETAL2017] is also part of this dataset.

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