MPS-Participation in SWI

PI (Principal Investigator) responsibility of SWI

SWI-Team @ MPS


Paul Hartogh (Principal Investigator)
Christopher Jarchow
Miriam Rengel
Ladislav Rezac
Norbert Krupp
Johannes Wicht
Alexander Medvedev
Uli Christensen
Markus Fränz
Richard Larsson

Engineers and Technicians:

Büttner, Irene
Börner, Peter
Chares, Bernd
Danneberg, Arne 
Frahm, Sophie
Erd, Christian
Franz, Sven
Garcia, Juan Pablo (Project Manager)
Heeke, Günter
Hellmann, David
Höfner, Sebastian
John, Hendrik
Levitina, Tatiana
Loose, Alexander
Meierdierks, Thimo
Miettinen, Esa-Pekka
Pasko, Pawel
Perplies, Henry
Schirmer, Oskar 
Stämm, Stefan
Sved, Daniel
Ulrich, Jan
Wagenknecht, Malte
Winkelmann, Felix

Team Assistants

Strotseva-Feinschmidt, Anna
Rezacova, Petra


SWI - Submillimetre Wave Instrument

The Submillimetre Wave Instrument (SWI) will investigate the Galilean moons of the giant planet Jupiter, the chemistry, meteorology, and structure of Jupiter’s middle atmosphere as well as atmospheric and magnetospheric coupling processes. By characterising Jupiter as a planet and possible habitat, and the investigation of more recent active areas within Europa’s ice crust, SWI will provide data for further investigations of habitable on the Galilean moons Ganymede, Europa and Callisto. Furthermore, the instrument will investigate the Jupiter system as an archetype of a gas giant planet and characterise Jupiter’s atmosphere as well as its rings and moons.

SWI is a spectrometer and radiometer, which has two identical channels that measure spectra in the range of 530 µm. It is desirable to reduce the measurable signal wavelength within one channel to 250 µm.

In this way, SWI will be able to

  • perform a detailed characterisation of the dynamics and composition of Jupiter’s stratosphere as well as its coupling to the underlying and overlying atmosphere,
  • perform in a unique and unprecedented characterisation of the thin atmospheres and exospheres of the Galilean moons; determine their sources and sinks; investigate the interaction with Jupiter’s magnetosphere,
  • determine the dominant isotopic ratios in the atmospheres of Jupiter and the Galilean moons, and therefore the origin and evolution of the entire Jupiter system,
  • measure the characteristics of the icy moons’ surfaces and subsurface and their composition.
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