Editing Rosetta (spacecraft) (section)

== Instruments ==
[[File:Rosetta Instrument Inventory.png|thumb|Rosetta instrument inventory|400x400px]]
{{For|the instruments on ''Philae''|Philae (spacecraft)#Instruments}}

=== Nucleus ===
The investigation of the nucleus was done by three [[optical spectrometer]]s, one [[microwave]] radio antenna and one [[radar]]:
* '''[[Alice (spacecraft instrument)|Alice]]''' (an ultraviolet imaging spectrograph). The [[ultraviolet]] [[spectroscopy|spectrograph]] searched for and quantified the [[noble gas]] content in the comet nucleus, from which the temperature during the comet creation could be estimated. The detection was done by an array of [[potassium bromide]] and [[caesium iodide]] [[photocathode]]s. The {{convert|3.1|kg|abbr=on}} instrument used 2.9 watts, with an improved version onboard [[New Horizons]]. It operated in the extreme and far ultraviolet spectrum, from {{convert|700|-|2050|Å|nm|abbr=on}}.<ref>{{cite journal|title=''Alice'': The Rosetta Ultraviolet Imaging Spectrograph |journal=Space Science Reviews |first1=S. A. |last1=Stern |first2=D. C. |last2=Slater |first3=J. |last3=Scherrer |first4=J. |last4=Stone |first5=M. |last5=Versteeg |first6=M. F. |last6=A'Hearn |first7=J. L. |last7=Bertaux |first8=P. D. |last8=Feldman |first9=M. C. |last9=Festou |first10=Joel Wm. |last10=Parker |first11=O. H. W. |last11=Siegmund |display-authors=5 |volume=128 |issue=1–4 |pages=507–527 |date=February 2007 |doi=10.1007/s11214-006-9035-8 |bibcode=2007SSRv..128..507S |arxiv=astro-ph/0603585|s2cid=44273197}}</ref><ref>{{cite journal |title=Alice—An Ultraviolet Imaging Spectrometer for the Rosetta Orbiter |journal=Advances in Space Research |first1=S. A. |last1=Stern |first2=D. C. |last2=Slater |first3=W. |last3=Gibson |first4=J. |last4=Scherrer |first5=M. |last5=A'Hearn |first6=J. L. |last6=Bertaux |first7=P. D. |last7=Feldman |first8=M. C. |last8=Festou |display-authors=5 |volume=21 |issue=11 |pages=1517–1525 |year=1998 |doi=10.1016/S0273-1177(97)00944-7 |bibcode=1998AdSpR..21.1517S |citeseerx=10.1.1.42.8623}}</ref> ALICE was built and operated by the [[Southwest Research Institute]] for NASA's Jet Propulsion Laboratory.<ref name="swri20140610">{{cite web |url=http://www.swri.org/9what/releases/2014/rosetta-alice.htm |title=Rosetta-Alice spectrograph to begin first-ever close up ultraviolet studies of comet surface and atmosphere |publisher=Southwest Research Institute |date=10 June 2014 |access-date=28 December 2016}}</ref>
* '''[[Optical, Spectroscopic, and Infrared Remote Imaging System|OSIRIS]]''' (Optical, Spectroscopic, and Infrared Remote Imaging System). The camera system had a [[Telephoto lens|narrow-angle]] lens (700&nbsp;mm) and a [[wide-angle lens]] (140&nbsp;mm), with a 2048×2048 pixel [[Charge-coupled device|CCD]] chip. The instrument was constructed in Germany. Development and construction of the instrument was led by the [[Max Planck Institute for Solar System Research]] (MPS).<ref>{{cite journal |title=Osiris—The optical, spectroscopic and infrared remote imaging system for the Rosetta Orbiter |journal=Advances in Space Research |first1=N. |last1=Thomas |first2=H. U. |last2=Keller |first3=E. |last3=Arijs |first4=C. |last4=Barbieri |first5=M. |last5=Grande |first6=P. |last6=Lamy |first7=H. |last7=Rickman |first8=R. |last8=Rodrigo |first9=K.-P. |last9=Wenzel |first10=M. F. |last10=A'Hearn |first11=F. |last11=Angrilli |first12=M. |last12=Bailey |first13=M. A. |last13=Barucci |first14=J.-L. |last14=Bertaux |first15=K. |last15=Brieβ |first16=J. A. |last16=Burns |first17=G. |last17=Cremonese |first18=W. |last18=Curdt |first19=H. |last19=Deceuninck |first20=R. |last20=Emery |first21=M. |last21=Festou |first22=M. |last22=Fulle |first23=W.-H. |last23=Ip |first24=L. |last24=Jorda |first25=A. |last25=Korth |first26=D. |last26=Koschny |first27=J.-R. |last27=Kramm |first28=E. |last28=Kührt |first29=L. M. |last29=Lara |first30=A. |last30=Llebaria |first31=J. J. |last31=Lopez-Moreno |first32=F. |last32=Marzari |first33=D. |last33=Moreau |first34=C. |last34=Muller |first35=C. |last35=Murray |first36=G. |last36=Naletto |first37=D. |last37=Nevejans |first38=R. |last38=Ragazzoni |first39=L. |last39=Sabau |first40=A. |last40=Sanz |first41=J.-P. |last41=Sivan |first42=G. |last42=Tondello |display-authors=5 |volume=21 |issue=11 |pages=1505–1515 |year=1998 |doi=10.1016/S0273-1177(97)00943-5 |bibcode=1998AdSpR..21.1505T |hdl=11577/2517967 |url=http://oa.upm.es/39904/|hdl-access=free }}</ref>
* '''VIRTIS''' (Visible and Infrared Thermal Imaging Spectrometer). The Visible and [[Infrared spectroscopy|IR spectrometer]] was able to make pictures of the nucleus in the IR and also search for IR spectra of molecules in the [[Coma (cometary)|coma]]. The detection was done by a mercury cadmium telluride array for IR and with a CCD chip for the [[Visible spectrum|visible wavelength]] range. The instrument was produced in Italy, and improved versions were used for [[Dawn (spacecraft)|Dawn]] and [[Venus Express]].<ref name="1995-igarss-virtis">{{Cite conference |last1=Coradini |first1=A. |last2=Capaccioni |first2=F. |last3=Capria |first3=M. T. |last4=Cerroni |first4=P. |last5=de Sanctis |first5=M. C. |last6=Magni |first6=G. |last7=Reininger |first7=F. |last8=Drossart |first8=P. |last9=Barucci |first9=M. A. |last10=Bockelee-Morvan |first10=D. |last11=Combes |first11=M. |last12=Crovisier |first12=J. |last13=Encrenaz |first13=T. |last14=Tiphene |first14=D. |last15=Arnold |first15=G. |last16=Carsenty |first16=U. |last17=Michaelis |first17=H. |last18=Mottola |first18=S. |first19=G. |last19=Neukum |last20=Schade |first20=U. |first21=F. |last21=Taylor |last22=Calcutt |first22=S. |first23=T. |last23=Vellacott |last24=Venters |first24=P. |first25=R. E. |last25=Watkins |last26=Bellucci |first26=G. |first27=V. |last27=Formisano |last28=Angrilli |first28=F. |last29=Bianchini |first29=G. |last30=Saggin |first30=B. |first31=E. |last31=Bussoletti |first32=L. |last32=Colangeli |last33=Mennella |first33=V. |last34=Fonti |first34=S. |first35=G. |last35=Tozzi |last36=Bibring |first36=J. P. |last37=Langevin |first37=Y. |last38=Schmitt |first38=B. |last39=Combi |first39=M. |last40=Fink |first40=U. |last41=McCord |first41=T. |first42=W. |last42=Ip |first43=R. W. |last43=Carlson |last44=Jennings |first44=D. E. |date=July 1995 |title=VIRTIS, visible infrared thermal imaging spectrometer for the ROSETTA mission |conference=1995 International Geoscience and Remote Sensing Symposium, IGARSS '95. Quantitative Remote Sensing for Science and Applications |location=Firenze, Italy |publisher=[[Institute of Electrical and Electronics Engineers|IEEE]] |volume=27 |page=253 |bibcode=1996LPI....27..253C |doi=10.1109/igarss.1995.521822 |isbn=978-0-7803-2567-8 |display-authors=5 |s2cid=119978931 }}</ref>
* '''MIRO''' (Microwave Instrument for the Rosetta Orbiter). The abundance and temperature of volatile substances like water, ammonia and carbon dioxide could be detected by MIRO via their [[microwave]] emissions. The {{convert|30|cm|in|abbr=on}} radio antenna along with the rest of the {{convert|18.5|kg|lb|abbr=on}} instrument was built by NASA's Jet Propulsion Laboratory with international contributions by the Max Planck Institute for Solar System Research (MPS), among others.<ref name="mps.miro">{{cite web|url=http://www.mps.mpg.de/1979612/MIRO |title=MIRO — Microwave Instrument for the Rosetta Orbiter |publisher=Max Planck Institute |access-date=28 December 2016}}</ref>
* '''[[CONSERT]]''' (Comet Nucleus Sounding Experiment by Radiowave Transmission). The CONSERT experiment provided information about the deep interior of the comet using [[radar]]. The radar performed [[tomography]] of the nucleus by measuring electromagnetic wave propagation between the ''[[Philae (spacecraft)|Philae]]'' lander and the ''Rosetta'' orbiter through the comet nucleus. This allowed it to determine the comet's internal structure and deduce information on its composition. The electronics were developed by France and both antennas were constructed in Germany. Development was led by the Laboratoire de Planétologie de Grenoble with contributions by the Ruhr-Universität Boch and the Max Planck Institute for Solar System Research (MPS).<ref>{{cite web |title=CONSERT — COmet Nucleus Sounding Experiment by Radio-wave Transmission |date= |work=MPS-Beteiligungen an der Mission Rosetta |publisher=Max-Planck-Institut für Sonnensystemforschung (MPS) |url=https://www.mps.mpg.de/2244587/CONSERT |language=de}}</ref><ref>{{cite journal |title=The Comet Nucleus Sounding Experiment by Radiowave Transmission (CONSERT): A Short Description of the Instrument and of the Commissioning Stages |journal=Space Science Reviews |first1=W. |last1=Kofman |first2=A. |last2=Herique |first3=J.-P. |last3=Goutail |first4=T. |last4=Hagfors |first5=I. P. |last5=Williams |first6=E. |last6=Nielsen |first7=J.-P. |last7=Barriot |first8=Y. |last8=Barbin |first9=C. |last9=Elachi |first10=P. |last10=Edenhofer |first11=A.-C. |last11=Levasseur-Regourd |first12=D. |last12=Plettemeier |first13=G. |last13=Picardi |first14=R. |last14=Seu |first15=V. |last15=Svedhem |display-authors=5 |volume=128 |issue=1–4 |pages=414–432 |date=February 2007 |doi=10.1007/s11214-006-9034-9 |bibcode=2007SSRv..128..413K|s2cid=122123636 }}</ref>
*'''RSI''' (Radio Science Investigation). RSI made use of the probe's communication system for physical investigation of the nucleus and the inner [[Coma (cometary)|coma]] of the comet.<ref>{{cite web |url=http://sci.esa.int/rosetta/35061-instruments/?fbodylongid=1645 |title=RSI: Radio Science Investigation |publisher=European Space Agency |access-date=26 November 2014}}</ref>

=== Gas and particles ===
* '''ROSINA''' (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis). The instrument consisted of a double-focus [[Sector instrument|magnetic mass spectrometer]] (DFMS) and a [[reflectron]] type [[Time of flight|time of flight mass spectrometer]] (RTOF). The DFMS had a high resolution (could resolve [[nitrogen|N<sub>2</sub>]] from [[carbon monoxide|CO]]) for molecules up to 300 [[Atomic mass unit|amu]]. The RTOF was highly sensitive for neutral molecules and for ions. The Max Planck Institute for Solar System Research (MPS) has contributed to the development and construction of the instrument.<ref>{{cite journal |title=Rosetta Orbiter Spectrometer for Ion and Neutral Analysis—ROSINA |journal=Advances in Space Research |first1=H. |last1=Balsiger |first2=K. |last2=Altwegg|author2-link=Kathrin Altwegg |first3=E. |last3=Arijs |first4=J.-L. |last4=Bertaux |first5=J.-J. |last5=Berthelier |first6=P. |last6=Bochsler |first7=G. R. |last7=Carignan |first8=P. |last8=Eberhardt |first9=L. A. |last9=Fisk |first10=S. A. |last10=Fuselier |first11=A. G. |last11=Ghielmetti |first12=F. |last12=Gliem |first13=T. I. |last13=Gombosi |first14=E. |last14=Kopp |first15=A. |last15=Korth |first16=S. |last16=Livi |first17=C. |last17=Mazelle |first18=H. |last18=Rème |first19=J. A. |last19=Sauvaud |first20=E. G. |last20=Shelley |first21=J. H. |last21=Waite |first22=B. |last22=Wilken |first23=J. |last23=Woch |first24=H. |last24=Wollnik |first25=P. |last25=Wurz |first26=D. T. |last26=Young |display-authors=5 |volume=21 |issue=11 |pages=1527–1535 |year=1998 |doi=10.1016/S0273-1177(97)00945-9 |bibcode=1998AdSpR..21.1527B}}</ref> ROSINA was developed at the University of Bern in Switzerland.
* '''[[Micro-Imaging Dust Analysis System|MIDAS]]''' (Micro-Imaging Dust Analysis System). The high-resolution [[atomic force microscopy|atomic force microscope]] investigated several physical aspects of the dust particles which are deposited on a silicon plate.<ref>{{cite journal |title=The MIDAS experiment for the Rosetta mission |journal=Advances in Space Research |first1=W. |last1=Riedler |first2=K. |last2=Torkar |first3=F. |last3=Rüdenauer |first4=M. |last4=Fehringer |first5=R. |last5=Schmidt |first6=H. |last6=Arends |first7=R. J. L. |last7=Grard |first8=E. K. |last8=Jessberger |first9=R. |last9=Kassing |first10=H. St. C. |last10=Alleyne |first11=P. |last11=Ehrenfreund |first12=A. C. |last12=Levasseur-Regourd |first13=C. |last13=Koeberl |first14=O. |last14=Havnes |first15=W. |last15=Klöck |first16=E. |last16=Zinner |first17=M. |last17=Rott |display-authors=5 |volume=21 |issue=11 |pages=1547–1556 |year=1998 |doi=10.1016/S0273-1177(97)00947-2 |bibcode=1998AdSpR..21.1547R}}</ref>
* '''COSIMA''' (Cometary Secondary Ion Mass Analyser). COSIMA analysed the composition of dust particles by [[secondary ion mass spectrometry]], using [[indium]] ions. It could detect ions up to a mass of 6500&nbsp;amu. COSIMA was built by the Max Planck Institute for Extraterrestrial Physics (MPE, Germany) with international contributions. The COSIMA team is led by the Max Planck Institute for Solar System Research (MPS, Germany).<ref>{{cite journal |title=Chemometric evaluation of time-of-flight secondary ion mass spectrometry data of minerals in the frame of future ''in situ'' analyses of cometary material by COSIMA onboard ROSETTA |journal=Rapid Communications in Mass Spectrometry |first1=Cecile |last1=Engrand |first2=Jochen |last2=Kissel |first3=Franz R. |last3=Krueger |first4=Philippe |last4=Martin |first5=Johan |last5=Silén |first6=Laurent |last6=Thirkell |first7=Roger |last7=Thomas |first8=Kurt |last8=Varmuza |display-authors=5 |volume=20 |issue=8 |pages=1361–1368 |date=April 2006 |doi=10.1002/rcm.2448 |pmid=16555371|bibcode=2006RCMS...20.1361E }}</ref>
* '''GIADA''' (Grain Impact Analyser and Dust Accumulator). GIADA analysed the dust environment of the [[Coma (cometary)|comet coma]] by measuring the optical cross section, momentum, speed and mass of each grain entering inside the instrument.<ref>{{cite journal |title=The Grain Impact Analyser and Dust Accumulator (GIADA) experiment for the Rosetta mission: design, performances and first results |journal=Space Science Reviews |first1=L. |last1=Colangeli |first2=J. J. |last2=Lopez-Moreno |first3=P. |last3=Palumbo |first4=J. |last4=Rodriguez |first5=M. |last5=Cosi |first6=V. |last6=Della Corte |first7=F. |last7=Esposito |first8=M. |last8=Fulle |first9=M. |last9=Herranz |first10=J. M. |last10=Jeronimo |first11=A. |last11=Lopez-Jimenez |first12=E. |last12=Mazzotta Epifani |first13=R. |last13=Morales |first14=F. |last14=Moreno |first15=E. |last15=Palomba |first16=A. |last16=Rotundi |display-authors=5 |volume=128 |issue=1–4 |pages=803–821 |date=February 2007 |doi=10.1007/s11214-006-9038-5 |bibcode=2007SSRv..128..803C|s2cid=123232721 }}</ref><ref>{{cite journal |title=GIADA: its status after the Rosetta cruise phase and on-ground activity in support of the encounter with comet 67P/Churyumov-Gerasimenko |journal=[[Journal of Astronomical Instrumentation]] |first1=V. |last1=Della Corte |first2=A. |last2=Rotundi |first3=M. |last3=Accolla |first4=R. |last4=Sordini |first5=P. |last5=Palumbo |first6=L. |last6=Colangeli |first7=J. J. |last7=Lopez-Moreno |first8=J. |last8=Rodriguez |first9=F. J. M. |last9=Rietmeijer |first10=E. |last10=Mazzotta Epifani |first11=S. |last11=Ivanovski |first12=A. |last12=Aronica |first13=M. |last13=Cosi |first14=E. |last14=Bussoletti |first15=J. F. |last15=Crifo |first16=F. |last16=Esposito |first17=M. |last17=Fulle |first18=S. F. |last18=Green |first19=E. |last19=Gruen |first20=M. L. |last20=Herranz |first21=J. M. |last21=Jeronimo |first22=P. |last22=Lamy |first23=A. |last23=Lopez-Jimenez |first24=J. A. M.. |last24=McDonnell |first25=V. |last25=Mennella |first26=A. |last26=Molina |first27=R. |last27=Morales |first28=F. |last28=Moreno |first29=E. |last29=Palomba |first30=J. M. |last30=Perrin |first31=R. |last31=Rodrigo |first32=P. |last32=Weissman |first33=V. |last33=Zakharov |first34=J. C. |last34=Zarnecki |display-authors=5 |volume=3 |issue=1 |pages=1350011–110 |date=March 2014 |doi=10.1142/S2251171713500116 |bibcode=2014JAI.....350011D |url=http://oro.open.ac.uk/39545/1/2014_DellaCorte_et_al_JAI_1350011.pdf}}</ref>

=== Solar wind interaction ===
* '''RPC''' (Rosetta Plasma Consortium).<ref>{{cite journal |title=The Rosetta plasma consortium: Technical realization and scientific aims |journal=Advances in Space Research |first1=J. G. |last1=Trotignon |first2=R. |last2=Boström |first3=J. L. |last3=Burch |first4=K.-H. |last4=Glassmeier |first5=R. |last5=Lundin |first6=O. |last6=Norberg |first7=A. |last7=Balogh |first8=K. |last8=Szegö |first9=G. |last9=Musmann |first10=A. |last10=Coates |first11=A. |last11=Åhlén |first12=C. |last12=Carr |first13=A. |last13=Eriksson |first14=W. |last14=Gibson |first15=F. |last15=Kuhnke |first16=K. |last16=Lundin |first17=J. L. |last17=Michau |first18=S. |last18=Szalai |display-authors=5 |volume=24 |issue=9 |pages=1149–1158 |date=January 1999 |doi=10.1016/S0273-1177(99)80208-7 |bibcode=1999AdSpR..24.1149T}}</ref><ref>{{cite journal |title=RPC-MAG The Fluxgate Magnetometer in the ROSETTA Plasma Consortium |journal=Space Science Reviews |first1=Karl-Heinz |last1=Glassmeier |first2=Ingo |last2=Richter |first3=Andrea |last3=Diedrich |first4=Günter |last4=Musmann |first5=Uli |last5=Auster |first6=Uwe |last6=Motschmann |first7=Andre |last7=Balogh |first8=Chris |last8=Carr |first9=Emanuele |last9=Cupido |first10=Andrew |last10=Coates |first11=Martin |last11=Rother |first12=Konrad |last12=Schwingenschuh |first13=Karoly |last13=Szegö |first14=Bruce |last14=Tsurutani |display-authors=5 |volume=128 |issue=1–4 |pages=649–670 |date=February 2007 |doi=10.1007/s11214-006-9114-x |bibcode=2007SSRv..128..649G|s2cid=121047896 }}</ref>