Editing SMART-1 (section)

==Instruments==

===AMIE===
The Advanced Moon micro-Imager Experiment was a miniature colour camera for lunar imaging. The CCD camera with three filters of 750, 900 and 950&nbsp;nm was able to take images with an average pixel resolution of 80 m (about 260&nbsp;ft). The camera weighed 2.1&nbsp;kg (about 4.5&nbsp;lb) and had a power consumption of 9 watts.<ref>{{cite journal | title= Science objectives and first results from the SMART-1/AMIE multicolour micro-camera|display-authors= 4|author= Josset J. L.|author2= Beauvivre S.|author3= Cerroni P.|author4= De Sanctis M. C.|author5= Pinet P.|author6= Chevrel S.|author7= Langevin Y.|author8= Barucci M. A.|author9= Plancke P.|author10= Koschny D.|author11= Almeida M.|author12= Sodnik Z.|author13= Mancuso S.|author14= Hoffmann B. A.|author15= Muinonen K.|author16= Shevchenko V.|author17= Shkuratov Y.|author18= Ehrenfreund P.|author19= Foing B. H.|journal= Advances in Space Research|volume=37|pages=14–20|date= 2006|issue= 1|bibcode = 2006AdSpR..37...14J |doi = 10.1016/j.asr.2005.06.078 }}</ref>

===D-CIXS===
The Demonstration of a Compact X-ray Spectrometer was an [[X-ray telescope]] for the identification of chemical elements on the lunar surface. It detected the [[X-ray fluorescence]] (XRF) of crystal compounds created through the interaction of the electron shell with the solar wind particles to measure the abundance of the three main components: [[magnesium]], [[silicon]] and [[aluminium]]. The detection of [[iron]], [[calcium]] and [[titanium]] depended on the solar activity. The detection range for X-rays was 0.5 to 10 keV. The spectrometer and XSM (described below) together weighed 5.2&nbsp;kg and had a power consumption of 18 watts.

===XSM===
The X-ray solar monitor studied the [[solar variation|solar variability]] to complement D-CIXS measurements.

===SIR===
The Smart-1 Infrared Spectrometer was an [[Infrared spectroscopy|infrared spectrometer]] for the identification of mineral spectra of [[olivine]] and [[pyroxene]]. It detected wavelengths from 0.93 to 2.4&nbsp;μm with 256 channels. The package weighed 2.3&nbsp;kg and had a power consumption of 4.1 watts.<ref>{{cite journal| title= Scientific objectives and selection of targets for the SMART-1 Infrared Spectrometer (SIR)|display-authors= 4|author= Basilevsky A. T.|author2= Keller H. U.|author3= Nathues A.|author4= Mall J.|author5= Hiesinger H.|author6= Rosiek M.|journal= Planetary and Space Science|volume= 52|pages= 1261–1285|date= 2004|doi=10.1016/j.pss.2004.09.002|bibcode=2004P&SS...52.1261B| issue= 14}}</ref>

===EPDP===
The Electric Propulsion Diagnostic Package was to acquire data on the new propulsion system on SMART-1. The package weighed 0.8&nbsp;kg and had a power consumption of 1.8 watts.<ref>{{cite journal| author=  Di Cara D. M.| author2=  Estublier D.|title=Smart-1: An analysis of flight data  |journal= Acta Astronautica| volume= 57 |issue= 2–8 |date= 2005| pages= 250–256|doi= 10.1016/j.actaastro.2005.03.036 |bibcode = 2005AcAau..57..250D }}</ref>

===SPEDE===
The Spacecraft Potential, Electron and Dust Experiment. The experiment weighed 0.8&nbsp;kg and had a power consumption of 1.8 watts. Its function was to measure the properties and density of the plasma around the spacecraft, either as a Langmuir probe or as an electric field probe. SPEDE observed the emission of the spacecraft's ion engine and the "wake" the Moon leaves to the [[solar wind]]. Unlike most other instruments that have to be shut down to prevent damage, SPEDE could keep measuring inside radiation belts and in solar storms, such as the [[Halloween solar storms, 2003|Halloween 2003 solar storms]].<ref>{{Cite web |url=http://sci.esa.int/smart-1/31415-instruments/ |website=sci.esa.int |title=ESA Science & Technology - Instruments}}</ref><ref name="Schmidt2014">{{cite journal | bibcode = 2014EGUGA..1613174S | title=SMART-1 SPEDE: Results and Legacy after 10 Years | volume=16 | year=2014 |author1=Schmidt, Walter |author2=Mälkki, Anssi | journal=EGU General Assembly Conference Abstracts | pages=13174 }}</ref> It was built by [[Finnish Meteorological Institute]] and its name was intentionally chosen so that its acronym is the same as the nickname of [[Spede Pasanen]], a famous Finnish movie actor, movie producer, and inventor. The algorithms developed for SPEDE were later used in the [[ESA]] lander [[Philae_(spacecraft)|Philae]].<ref name="Schmidt2014" />

===KATE===
[[Ka band|K<sub>a</sub> band]] TT&C (telemetry, tracking and control) Experiment. The experiment weighed 6.2&nbsp;kg and had a power consumption of 26 watts. The Ka-band transponder was designed as precursor for [[BepiColombo]] to perform radio science investigations and to monitor the dynamical performance of the electric propulsion system.