Spacecraft A
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CoCa (COmet CAmera) is the imaging system on Spacecraft A and is provided by a consortium led by the University of Bern in Switzerland including DLR Adlershof, LAM Marseille, the Konkoly Thege Miklos Astronomical Institute Budapest and their industrial partners. It is designed to provide high resolution imaging of the nucleus of the selected comet in 4 filters at selected broadband optical wavelengths. To provide high performance at low cost, it relies on designs successfully developed for previous flight programs. For a 1000 km fly-by, CoCa will provide 8 m per pixel images at a repetition frequency of 1 image per second. CoCa will therefore provide the highest quality imaging of the surface and the dust in the near-nucleus environment over a range of phase angles. The system is constructed to provide over 2500 images during the fly-by for subsequent downlink and can allow saturation on the nucleus to provide optimum signal-to-noise on the dust coma at all times through the fly-by. The optics of CoCa are protected from high velocity dust impacts by the Rotating Mirror Assembly (RMA) that will be provided by CSL in Liege and Thales-Alenia Space Switzerland.
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The Camera Support Unit (CSU) for the current CoCa design
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PI: Nicolas Thomas, University of Bern, Switzerland
Deputy PI: Antoine Pommerol, University of Bern, Switzerland
Deputy PI: Antoine Pommerol, University of Bern, Switzerland
Thomas Beck, University of Bern, Switzerland
Wei Wang Jungo, University of Bern, Switzerland
Neville Mehta, University of Bern, Switzerland
Claudio Zimmermann, University of Bern, Switzerland
Daniele Piazza, University of Bern, Switzerland
Nico Haslebacher, University of Bern, Switzerland
Mirko Meier, University of Bern, Switzerland
Thierry De Roche, University of Bern, Switzerland
Sebastian Wolf, University of Bern, Switzerland
Martin Rieder, University of Bern, Switzerland
Mathias Brändli, University of Bern, Switzerland
Martin Diego Busch, University of Bern, Switzerland
Harald Michaelis, DLR, Germany
Jean-Baptiste Vincent, DLR, Germany
Luisa M. Lara, Instituto de Astrofísica de Andalucía - CSIC, Spain
Jose M. Castro-Marin, Instituto de Astrofísica de Andalucía - CSIC, Spain
Jaime Jiménez Ortega, Instituto de Astrofísica de Andalucía - CSIC, Spain
Tim Arnold, The Open University, UK
Chiaki Crews, The Open University, UK
Akos Kereszturi, Research Centre for Astronomy and Earth Sciences, Konkoly Astronomical Institute, Hungary
Gabor Troznai, SGF Ltd., Hungary
Balazs Zabori, Centre for Energy Research, Hungary
Olivier Groussin, Laboratoire d'Astrophysique de Marseille, France
Laurent Jorda, Laboratoire d'Astrophysique de Marseille, France
Zsolt Kovács, Admatis Ltd., Hungary
Máté Krisztián Kubi, Admatis Ltd., Hungary
Richard Flonta, Admatis Ltd., Hungary
Gergo Rakosi, Admatis Ltd., Hungary
Wei Wang Jungo, University of Bern, Switzerland
Neville Mehta, University of Bern, Switzerland
Claudio Zimmermann, University of Bern, Switzerland
Daniele Piazza, University of Bern, Switzerland
Nico Haslebacher, University of Bern, Switzerland
Mirko Meier, University of Bern, Switzerland
Thierry De Roche, University of Bern, Switzerland
Sebastian Wolf, University of Bern, Switzerland
Martin Rieder, University of Bern, Switzerland
Mathias Brändli, University of Bern, Switzerland
Martin Diego Busch, University of Bern, Switzerland
Harald Michaelis, DLR, Germany
Jean-Baptiste Vincent, DLR, Germany
Luisa M. Lara, Instituto de Astrofísica de Andalucía - CSIC, Spain
Jose M. Castro-Marin, Instituto de Astrofísica de Andalucía - CSIC, Spain
Jaime Jiménez Ortega, Instituto de Astrofísica de Andalucía - CSIC, Spain
Tim Arnold, The Open University, UK
Chiaki Crews, The Open University, UK
Akos Kereszturi, Research Centre for Astronomy and Earth Sciences, Konkoly Astronomical Institute, Hungary
Gabor Troznai, SGF Ltd., Hungary
Balazs Zabori, Centre for Energy Research, Hungary
Olivier Groussin, Laboratoire d'Astrophysique de Marseille, France
Laurent Jorda, Laboratoire d'Astrophysique de Marseille, France
Zsolt Kovács, Admatis Ltd., Hungary
Máté Krisztián Kubi, Admatis Ltd., Hungary
Richard Flonta, Admatis Ltd., Hungary
Gergo Rakosi, Admatis Ltd., Hungary
Christian Kintziger, Centre Spatial de Liège, Belgium
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MIRMIS is the hyper spectral and multispectral remote sensing instrument (0.9 to ~25 µm) for Comet Interceptor. This wavelength range includes spectral features for CO2, water ice, CO, mineral compositions and is rich in thermophysical data.
MIRMIS is made up of two integrated modules (Near-IR (NIR)/Mid-IR (MIR) and a thermal infrared imager (TIRI)) with one thermal, mechanical and electrical interface to the spacecraft. NIR is a 0.9 to 1.7 µm hyperspectral imager, MIR is a 2.5 to 5 µm point spectrometers and TIRI (Thermal Infrared Imager) is a 6 to 25 µm multispectral thermal imager. MIRMIS/NIR and MIRMIS/MIR are supplied by VTT Finland with the UK providing MIRMIS/TIRI (Oxford) and overall integration of the instrument. The MIRMIS instrument team includes members from the UK, Finland and US. Mass = 8.8 kg Dimensions= 548.5 x 282.0 x 127.8 mm |
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Team Members
PI: Neil Bowles (University of Oxford, UK)
Co-PI: Antti Näsilä (VTT, Finland)
Co-PI: Geronimo Villanueva (NASA Goddard Space Flight Center, United States)
Tristram Warren, University of Oxford, UK
Katherine Shirley, University of Oxford, UK
Mario Fernández Palos
David Korda, University of Helsinki, Finland
Tomas Kohout, University of Helsinki, Finland
Antti Penttilä, University of Helsinki, Finland
Tilak Hewagma, NASA Goddard Space Flight Center, United States
Shahid Aslam, NASA Goddard Space Flight Center, United States
Benjamin Greenhagen, NASA Goddard Space Flight Center, United States
Kerri Donaldson Hanna, University of Oxford/University of Central Florida, United States
PI: Neil Bowles (University of Oxford, UK)
Co-PI: Antti Näsilä (VTT, Finland)
Co-PI: Geronimo Villanueva (NASA Goddard Space Flight Center, United States)
Tristram Warren, University of Oxford, UK
Katherine Shirley, University of Oxford, UK
Mario Fernández Palos
David Korda, University of Helsinki, Finland
Tomas Kohout, University of Helsinki, Finland
Antti Penttilä, University of Helsinki, Finland
Tilak Hewagma, NASA Goddard Space Flight Center, United States
Shahid Aslam, NASA Goddard Space Flight Center, United States
Benjamin Greenhagen, NASA Goddard Space Flight Center, United States
Kerri Donaldson Hanna, University of Oxford/University of Central Florida, United States
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The MANiaC instrument contains a time-of-flight mass spectrometer and a neutral density gauge, both attached to an electronics unit. Combining the measurements of the two sensors results in the absolute neutral gas densities of different volatile species along the flyby trajectory of the Comet Interceptor spacecraft.
MANiaC is set to measure the abundances of the major volatile species in the cometary coma. These include H2O, CO2, CO, and possibly O2. Depending on the outgassing activity of the target comet, also minor species, such as organic molecules and heavy isotopologues of water, can be measured. Furthermore, information on the composition of dust grains may be obtained in case such a particle by chance enters the instrument. |
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PI: Martin Rubin, University of Bern, Switzerland
Deputy PI: Peter Wurz, University of Bern, Switzerland
Thomas Beck, University of Bern, Switzerland
Wei Wang Jungo, University of Bern, Switzerland
Alexander Stettler, University of Bern, Switzerland
Neville Mehta, University of Bern, Switzerland
Thomas Gerber, University of Bern, Switzerland
Daniele Piazza, University of Bern, Switzerland
Mirko Meier, University of Bern, Switzerland
Thierry De Roche, University of Bern, Switzerland
Sebastian Wolf, University of Bern, Switzerland
Martin Rieder, University of Bern, Switzerland
Mathias Brändli, University of Bern, Switzerland
Martin Diego Busch, University of Bern, Switzerland
Luisa M. Lara, Instituto de Astrofísica de Andalucia CSIC, Spain
Jose M. Castro-Marin, Instituto de Astrofísica de Andalucia CSIC, Spain
Jaime Jiménez Ortega, Instituto de Astrofísica de Andalucia CSIC, Spain
Manfred Steller, Space Research Institute, Graz, Austria
Gunter Laky, Space Research Institute / Austrian Academy of Sciences, Austria
Harald Jeszenszky, Space Research Institute / Austrian Academy of Sciences, Austria
Joerg Knollenberg, Space Research Institute / Austrian Academy of Sciences, Austria
Harald Ottacher, Space Research Institute / Austrian Academy of Sciences, Austria
Jean-Baptiste Vincent, DLR Institute for Planetary Research, Germany
Philippe Garnier, IRAP UPS CNRS, France
Nicolas Andre, IRAP UPS CNRS, France
Deputy PI: Peter Wurz, University of Bern, Switzerland
Thomas Beck, University of Bern, Switzerland
Wei Wang Jungo, University of Bern, Switzerland
Alexander Stettler, University of Bern, Switzerland
Neville Mehta, University of Bern, Switzerland
Thomas Gerber, University of Bern, Switzerland
Daniele Piazza, University of Bern, Switzerland
Mirko Meier, University of Bern, Switzerland
Thierry De Roche, University of Bern, Switzerland
Sebastian Wolf, University of Bern, Switzerland
Martin Rieder, University of Bern, Switzerland
Mathias Brändli, University of Bern, Switzerland
Martin Diego Busch, University of Bern, Switzerland
Luisa M. Lara, Instituto de Astrofísica de Andalucia CSIC, Spain
Jose M. Castro-Marin, Instituto de Astrofísica de Andalucia CSIC, Spain
Jaime Jiménez Ortega, Instituto de Astrofísica de Andalucia CSIC, Spain
Manfred Steller, Space Research Institute, Graz, Austria
Gunter Laky, Space Research Institute / Austrian Academy of Sciences, Austria
Harald Jeszenszky, Space Research Institute / Austrian Academy of Sciences, Austria
Joerg Knollenberg, Space Research Institute / Austrian Academy of Sciences, Austria
Harald Ottacher, Space Research Institute / Austrian Academy of Sciences, Austria
Jean-Baptiste Vincent, DLR Institute for Planetary Research, Germany
Philippe Garnier, IRAP UPS CNRS, France
Nicolas Andre, IRAP UPS CNRS, France
Dust, Fields and Plasma (DFP) comprises several individual sensors/elements, detailed below.
DFP PI: Hanna Rothkaehl (CBK PAN, Warsaw, Poland)
Instrument Manager: Jędrzej Baran
DFP PI: Hanna Rothkaehl (CBK PAN, Warsaw, Poland)
Instrument Manager: Jędrzej Baran
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FGM-A shall perform 3D magnetic field measurements for boundary detection & characterisation and for resolving structure inside the boundary.
Furthermore FGM-A shall measure simultaneously with magnetic field experiments onboard B1 and B2 the magnetic field in order to resolve various wave modes, (e.g. ion cyclotron waves, mirror modes). FGM A consists of two boom mounted fluxgate sensors, outboard sensor merged with Compliment LP
FGM (A) Unit Co-PI: Uli Auster, TU Braunschweig, Germany Marina Galand Karl Heinz Glassmeier Werner Magnes Chris Carr Emanuele Cupido Charlotte Götz Ingo Richter Gerhard Berghofer |
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SCIENA measures ions in the energy range from a few eV up to 15 keV, and energetic neutral atoms - ENAs - in the solar wind energy range, 300 eV to 3 keV. Ions are measure in a near 2π hemisphere, whereas the ENA are observed in a slit some 30° wide and 150° long. The measurement goal is to assess the energy input from the solar wind and from cometary ions picked up by the solar wind upstream of the observation point. The scientific goal is to understand how the solar wind interacts with and affect the comet environment. Which plasma boundaries form and how do these affect the energy and momentum transfer from the solar wind to the coma? ENA observation may shed light on the role of charge changing reactions in stripping away the solar wind.
Measurements: Ions: Energy range 10 eV - 15 keV Angular coverage near 2π in 24- 48 pixels Time resolution 0.5 - 1s / energy spectra, 20 - 50 s per full distribution function |
ENA: Energy range 300 eV - 3 keV Angular coverage ~ 30° x 150° Time resolution 0.5 - 10s / energy spectra, 5 - 50 s per full scan |
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SCIENA Unit Co-PI: Hans Nilsson, Swedish Institute of Space Physics (IRF), Sweden
Team Members: (IRF) Xiaodong Wang Manabu Shimoyama Martin Wieser |
Yoshifumi Futaana
Vesa Alatalo Andreas Edström Jonas Olsen Magnus Oja Robert Labudda Joakim Peterson Rikard Ottermark Máté Kerényi Leif Kalla Robert Labudda |
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LEES will determine the electron density, temperature, and the velocity distribution functions of the in situ plasma environment of the solar wind and comet. LEES will detect the suprathermal photoelectrons created during neutral-plasma interactions in the coma and trace the magnetic connectivity between the spacecraft and the cometary environment. In addition LEES will measure the properties of negatively charged ions and dust of cometary origin. The energy range covered by LEES will be from a few eV up to 1 keV. Particles are measured in 360° azimuth angles with elevation angles ranging from -40° to 70°.
Measurements: Energy range 10 eV - 1 keV in 90 energy bins Energy resolution 0.07 Angular coverage 2.8 π sr Time resolution 8s / energy spectra LEES Unit Co-PI: Nicolas Andre, IRAP, France. LEES Deputy Unit Co-PI: Lubomir Prech, Charles University, Czech Republic Team Members Andrey Fedorov Benoît Lavraud Philippe Garnier Vincent Génot Jakub Vaverka |
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The COMetary Plasma Light InstruMENT unit (COMPLIMENT) will provide the following measurements:
-Electric field and waves (1 component) -High cadence independent ion and electron densities -Electron temperature(s) -S/C potential -Integrated EUV flux -Nanodust impacts (signal processed by DFP-DAPU)in order to addressed the structure and dynamics of the ionized and dusty cometary environment and its interactions with the escaping cometary atmosphere. To do so, COMPLIMENT is composed of :
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Merged COMPLIMENT-FGM sensor (EM0) on the FGM deployable boom during plasma chamber tests at LPC2E, Orléans, France.
Integration of merged probe EM0 – FGM sensor embedded in probe inner shield
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COMPLIMENT Unit Co-PI: Pierre Henri, CNRS (LPC2E, Orléans & Lagrange, Nice), France.
COMPLIMENT Deputy Unit Co-PI: Niklas Edberg, IRF-Uppsala, Sweden.
COMPLIMENT Deputy Unit Co-PI: Johan De Keyser, BIRA, Belgium
with strong instrumental modeling contributions from LAPLACE, Toulouse, France; KTH, Stockholm, Sweden; Lagrange, Nice Observatory, France.
Team members
Olivier Le Duff
Clémence Agrapart
Gaetan Wattieaux
Fabrice Colin
Aude-Lyse Millet
Walter Puccio
Anders Eriksson
Victoria Cripps
Jesper Fredriksson
Martin Berglund
Dan Ohlsson
Sylvain Ranvier
Frederk Dhooghe
Joakim Peterson IRF-K, Kiruna, Sweden
Elias Odelstad
Magnus Oja
COMPLIMENT Deputy Unit Co-PI: Niklas Edberg, IRF-Uppsala, Sweden.
COMPLIMENT Deputy Unit Co-PI: Johan De Keyser, BIRA, Belgium
with strong instrumental modeling contributions from LAPLACE, Toulouse, France; KTH, Stockholm, Sweden; Lagrange, Nice Observatory, France.
Team members
Olivier Le Duff
Clémence Agrapart
Gaetan Wattieaux
Fabrice Colin
Aude-Lyse Millet
Walter Puccio
Anders Eriksson
Victoria Cripps
Jesper Fredriksson
Martin Berglund
Dan Ohlsson
Sylvain Ranvier
Frederk Dhooghe
Joakim Peterson IRF-K, Kiruna, Sweden
Elias Odelstad
Magnus Oja
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Dust Impact Sensor and Counter (DISC) is part of the Dust Field Plasma (DFP) suite and will be produced in two units, one on S/C A and one on S/C B2. DISC, devoted to characterize in situ the cometary dust environment, is a monitoring instrument: when a dust particle impacts its sensitive surface the momentum and mass of the particle is measured.
DISC will:
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DISC Unit Co-PI: Vincenzo Della Corte, INAF-IAPS, Rome, Italy
DISC Deputy Unit Co-PI: Alessandra Rotundi, University "Parthenope", Naples, Italy
Giuseppe Sindoni
Andrea Longobardo
Alice Maria Piccirillo
Federico Di Paolo
Ivano Bertini
Laura Inno
DISC Deputy Unit Co-PI: Alessandra Rotundi, University "Parthenope", Naples, Italy
Giuseppe Sindoni
Andrea Longobardo
Alice Maria Piccirillo
Federico Di Paolo
Ivano Bertini
Laura Inno
DAPU Unit Co-PI: Ivana Kolmasova, IAP, Praque, Czech Republic
Jan Souček
Ondřej Santolík
Radek Lán
Luděk Uhlíř
Jiří Jánský
David Píša
Benjamin Grison
Jan Souček
Ondřej Santolík
Radek Lán
Luděk Uhlíř
Jiří Jánský
David Píša
Benjamin Grison
Information to follow
Probe B1
Probe B1 PI
Ryu Funase (JAXA)
Ryu Funase (JAXA)
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PS is comprised of a magnetometer (MAG) and a cometary ion mass
spectrometer (CIMS). MAG is a three-axis fundamental mode orthogonal fluxgate magnetometer. CIMS is a combination of an electrostatic analyser and a TOF mass spectrometer. Its field of view covers the substantial part of the cometary velocity distribution function and the solar wind ion distributions. PS will identify plasma boundaries, as well as provide us with coma composition. Magnetometer: Dynamic range: +/-512 nT Accuracy: 1 nT Angular accuracy: 5deg Sampling rate: 64Hz Ion mass spectrometer: Energy range: 10 eV/q - 12 keV/q FOV: ~ 2pi str Mass resolution: ~30 |
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Instrument PI
Satoshi Kasahara (The University of Tokyo)
Instrument deputy-PI
Ayako Matsuoka (Kyoto Univ.)
Team Members (magnetometer)
Naofumi Murata (JAXA)
Yuki Harada (Kyoto Univ.)
Team members (ion analyser)
Shoichiro Yokota (Osaka Univ.)
Kazushi Asamura (JAXA)
Yoshifumi Saito (JAXA)
Satoshi Kasahara (The University of Tokyo)
Instrument deputy-PI
Ayako Matsuoka (Kyoto Univ.)
Team Members (magnetometer)
Naofumi Murata (JAXA)
Yuki Harada (Kyoto Univ.)
Team members (ion analyser)
Shoichiro Yokota (Osaka Univ.)
Kazushi Asamura (JAXA)
Yoshifumi Saito (JAXA)
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Hydrogen Imager (HI) is a Cassegrain-type UV (121.6nm) imager with band-pass filters. The comet activity such as water production rate and its spatial variation can be calculated from the data. The characteristics of Hydrogen including isotope ratio and temperature are also in the targets.
HI will measure the spatial distribution of Hydrogen (Ly-alpha: 121.6nm) brightness in the coma through both image and light-curve modes. The image mode takes brightness maps with FOV of 4x4degrees (256x256 pixels), and the light-curve mode takes emission profile of H and possibly D around the nucleus. |
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Instrument PI
Kazuo Yoshioka (The Univertisy of Tokyo)
Team members:
Go Murakami (JAXA)
Masaki Kuwabara (JAXA)
Ichiro Yoshikawa (The University of Tokyo)
Kazuo Yoshioka (The Univertisy of Tokyo)
Team members:
Go Murakami (JAXA)
Masaki Kuwabara (JAXA)
Ichiro Yoshikawa (The University of Tokyo)
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NAC/WAC is a monochromatic camera system composed of a telescopic camera and wide-angle camera onboard the B1 probe to reveal the global shape of the target body, its surface morphology, and the large-scale structure of dust coma.
After the B1 separation, continuous imaging of the target serves as light curve acquisition as well as the source of optical navigation, and at the closest approach, the nucleus will be observed at a pixel resolution < 40 m/pix with high solar incident angle. Instrument PI
Naoya Sakatani (Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Japan) Instrument deputy-PI Shingo Kameda (Rikkyo Univ.) Takahiro Sasaki Eri Tatsumi |
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Probe B2
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On its trajectory past the target body, Optical Periscopic Imager for Comets (OPIC) onboard the B2 probe will image the nucleus and its surrounding gas and dust environment to allow its spatial reconstruction. This allows to pinpoint the activity hotspots and, when combined with instruments on A and B1, generation of 3D models of the fly-by scenario.
OPIC will take monochromatic photos in the visible spectrum. When the B2 probe is far from the nucleus, OPIC will take high exposure photos of the area around the nucleus. At this distance, nucleus is not resolvable and will only be a dot on the image. These images show how much gas and dust is in the viewing direction of OPIC and its spatial distribution. The data can be also used to constrain the trajectory and rotation state of B2 after B2-A separation. When the B2 probe gets closer to the target body, the target body will become resolvable, and images will be taken automatically and analyzed onboard the B2 probe before transmission to spacecraft A and consequently to the Earth. The images will show the low-resolution structure of the nucleus and gas and dust immediately around it, including potential satellites and fragmentation. This can be combined with imagery from A and B1 spacecraft to generate a more detailed and less ambiguous 3D model of the target, as each spacecraft will only travel in a line and so will have a limited range of viewing angles to the Target. |
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PI: Mihkel Pajusalu, Tartu Observatory, University of Tartu, Estonia
Deputy-PI: Aire Olesk, Tartu Observatory, University of Tartu, Estonia
Karin Pai
Reimo Soosaar
Joosep Kivasttik
Iaroslav Iakubivskyi
Hans Teras
Aditya Savio Paul
Karin Kruuse
Artiom Nikolajev
Guillaume Le Bonhomme
Vootele Mets
Uku Kert Paidra
Amal Vinod
Jaan Praks
Árni Þór Þorgeirsson
Eric Brune
Aire Olesk
Timo Väisänen
Michał Porębski
Markus Hiltunen
Gabriel Schwarzkopf
Maximilian Bührer
Deputy-PI: Aire Olesk, Tartu Observatory, University of Tartu, Estonia
Karin Pai
Reimo Soosaar
Joosep Kivasttik
Iaroslav Iakubivskyi
Hans Teras
Aditya Savio Paul
Karin Kruuse
Artiom Nikolajev
Guillaume Le Bonhomme
Vootele Mets
Uku Kert Paidra
Amal Vinod
Jaan Praks
Árni Þór Þorgeirsson
Eric Brune
Aire Olesk
Timo Väisänen
Michał Porębski
Markus Hiltunen
Gabriel Schwarzkopf
Maximilian Bührer
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The EnViss (Entire Visible Sky) camera has been conceived to study the comet dust environment, including its polarimetric properties, in the visible wavelength range. It features a fish-eye lens to image 180° FoV. Thanks to B2 rotation, the full sky view will be re-constructed by stitching the acquired sky-slices.
Scientific measurements The EnVisS camera scientific goal is to measure the radiance and linear polarization (degree of polarization and angle of polarization) of the coma all over the sky in the wavelength range 550-800 nm. Depending on the target object activity, the map of the coma will be taken with different spatial resolution in order to achieve the desired SNR. Minimum resolution element is 0.2°. |
EnVisS instrument present mechanical layout (courtesy of UCL-MSSL, UK, and Leonardo SpA, IT)
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PI: Vania Da Deppo, CNR-Institute for Photonics and Nanotechnologies, Padova, IT
Co-PI: Luisa Lara, Instituto de Astrofísica de Andalucía - CSIC, ES
Vincenzo Della Corte
Claudio Pernechele
Paola Zuppella
Paolo Chioetto
Jose M. Castro-Marin
Jaime Jiménez Ortega
Ignacio Martínez Navajas
Jaan Praks
Andris Slavinskis
Simone Nordera
Stefano Bagnulo
Co-PI: Luisa Lara, Instituto de Astrofísica de Andalucía - CSIC, ES
Vincenzo Della Corte
Claudio Pernechele
Paola Zuppella
Paolo Chioetto
Jose M. Castro-Marin
Jaime Jiménez Ortega
Ignacio Martínez Navajas
Jaan Praks
Andris Slavinskis
Simone Nordera
Stefano Bagnulo
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Dust Impact Sensor and Counter (DISC) is part of the Dust Field Plasma (DFP) suite and will be produced in two units, one on S/C A and one on S/C B2. DISC, devoted to characterize in situ the cometary dust environment, is a monitoring instrument: when a dust particle impacts its sensitive surface the momentum and mass of the particle is measured.
DISC will:
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DISC Unit Co-PI: Vincenzo Della Corte, INAF-IAPS, Rome, Italy
DISC Deputy Unit Co-PI: Alessandra Rotundi, University "Parthenope", Naples, Italy
Giuseppe Sindoni
Andrea Longobardo
Alice Maria Piccirillo
Federico Di Paolo
Ivano Bertini
Laura Inno
DISC Deputy Unit Co-PI: Alessandra Rotundi, University "Parthenope", Naples, Italy
Giuseppe Sindoni
Andrea Longobardo
Alice Maria Piccirillo
Federico Di Paolo
Ivano Bertini
Laura Inno
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FGM-B2 (BFG for short), part of the Dust, Field and Plasma (DFP) consortium, is a dual-sensor fluxgate magnetometer on the B2 probe. It will measure the 3D magnetic field vector. Its dataset will be used to identify plasma/field boundaries and regions. A magnetometer is the only instrument present on all three spacecraft. This multi-point capability will allow to assess the 3D structure of these boundaries and energy transfer through the coma and across boundaries. The two BFG sensors are mounted on a rigid boom. The front-end electronics has been optimised for B2: light weight (408 g total) and low power consumption (1.8 W total). The BFG magnetometer is based on a strong heritage, including Rosetta/Philae and THEMIS, MMS and GEO-KOMPSAT-2A/SOSMAG.
FGM (B) Unit Co-PI: Marina Galand, Imperial College London, UK.
FGM (B) Deputy Unit Co-PI: Martin Volwerk, Space Research Institute, Austrian Academy of Sciences, Graz, Austria Uli Auster Chris Carr Charlotte Götz Ingo Richter Emanuele Cupido Gunter Laky Aris Valavanoglou Werner Magnes Gerhard Berghofer |
One fluxgate magnetometer sensor on the left, with its harness, and its cover on the right.
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