|content long||19-June-2013 23:19:49|
Instruments in Brief
The instrument comprises four sensors:
|Summary of MAG Characteristics|
|Smallest range||Default range||Maximum range|
|Magnetic field measurement range (each axis)||± 32.8 nT||± 262 nT||± 8338.6 nT|
|Magnetic field resolution||1 pT||8 pT||128 pT|
|Static magnetic field compensation||± 10 µT||± 10 µT||± 10 µT|
The fluxgate sensors are the same as the ROMAP sensor flown on Rosetta. The design of the MAG electronics is derived from that used for ROMAP, adapted for the two sensor configuration.
PFS (Planetary Fourier Spectrometer) is an infrared spectrometer that operates in the 0.9 μm to 45 μm wavelength range and is designed to perform vertical optical sounding of the Venus atmosphere. The instrument is designed to:
|Summary of PFS Characteristics|
|Short Wavelength Channel||Long Wavelength Channel|
|Spectral range (µm)||0.9 - 5.5||5.0 - 45|
|Spectral resolution (cm-1)||2||2|
|Spectral resolving power (λ/Δλ)||5500 - 1500||1000 - 100|
|Field of view (mrad)||35||70|
The PFS instrument design is based on that flown on Mars Express, modified to optimise performance for the Venus Express mission.
SPICAV (Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus) is an imaging spectrometer for ultraviolet and infrared radiation. SPICAV is derived from the SPICAM instrument flown on Mars Express, which was equipped with two channels, one for ultraviolet wavelengths and one for infrared. An additional channel (SOIR, Solar Occultation at Infrared) has been added for Venus Express, to observe the Sun through Venus's atmosphere at infrared wavelengths.
|Ultraviolet Channel||Infrared Channel||SOIR Channel|
|Spectral range (µm)||0.11 - 0.31||0.7 - 1.7||2.3 - 4.2|
|Spectral resolution||0.8nm||0.5 - 1nm||0.2 - 0.5cm-1|
|Spectral resolving power (λ/Δλ)||~300||~1300||~15 000|
|Field of View (rad)||55 × 8.7||0.2 / pixel||0.3 - 3|
VeRa (Venus Radio Science) is a radio sounding experiment that is used to examine the ionosphere, atmosphere and surface of Venus by means of radio waves transmitted from the spacecraft, passed directly through the atmosphere or reflected off the planet surface and received by a ground station on Earth.
The instrument is designed to:
VeRa uses the spacecraft's transponder for radio transmission and reception, but generates the transmitted signal using its own Ultra Stable Oscillator (USO). The design of the VeRa USO is derived from that used for the Radio Science Investigation instrument flown on Rosetta.
VIRTIS (Visible and Infrared Thermal Imaging Spectrometer) is an imaging spectrometer that operates in the near ultraviolet, visible and infrared parts of the electromagnetic spectrum (0.25 to 5µm wavelength range). The instrument has a variety of operating modes that cover a range of observations from pure, high-resolution spectrometry to spectro-imaging.
|Summary of VIRTIS Characteristics|
|Mapping Spectrometer||High Resolution Spectrometer|
|Visible Channel||Infrared Channel||Infrared Channel|
|Spectral range (µm)||0.25 - 1.0||1 - 5||2 - 5|
|Maximum Spectral resolution (nm)||~2||~10||~3|
|Spectral resolving power (λ/Δλ)||100 - 200||100 - 200||1000 - 2000|
|Field of view (mrad)||0.25||0.25||0.5 - 1.5|
VIRTIS allows the analysis of all layers of the atmosphere and the clouds therein, the making of surface temperature measurements and the study of surface / atmosphere interaction phenomena.
VMC (Venus Monitoring Camera) is a wide angle, multi-channel CCD camera that, using four narrow band filters, operates in the ultraviolet, visible and near infrared spectral ranges. VMC fulfils the following goals:
In addition, VMC images and movies will make a significant contribution to the public outreach program.
|Summary of VMC Characteristics|
|Spectral range (µm)|| |
|Spectral resolution (nm)||~5|
|Field of view (mrad)||300 (total), 0.74 (mrad per pixel)|
The VMC design is derived in part from the Mars Express High/Super Resolution Stereo Colour Imager (HRSC) and partly from the Rosetta Optical, Spectroscopic and Infrared Remote Imaging System (OSIRIS) design.
Last Update: 14 December 2012For further information please contact: SciTech.firstname.lastname@example.org