COSIMA for the ESA Mission ROSETTA - vh-s.de

vH&SRAUMFAHRT • FORSCHUNG • INDUSTRIE

COmetary Secondary Ion Mass AnalyserCOSIMA for the ESA Mission ROSETTAH. Henkel q, H. Hofner w, J. Kissel e, A. Koch q, M. Hilchenbach e— q von Hoerner & Sulger GmbH (vH&S), Schwetzingen,

w Max-Planck-Institut fur extraterrestrische Physik (MPE), Garching, e Max-Planck-Institut fur Aeronomie (MPAe), Katlenburg-Lindau

The COSIMA Instrument

Electronics Box

Dust Inlet

Target Manip. Unit

COSISCOPE

Ion Source (Clean)

Ion Source (Analyse)

Primary Ion Optics

Drift Tube

Ion Reflector

COSIMA’s Scientific ObjectivesTarget: Comet 67P/Churyumov-Gerasimenko

• Analysis of the elemental composition (and isotopiccomposition of some key elements) of cometary grains.

• Chemical characterisation of the main organic compo-nents, present homologuous and functional groups.

• Mineralic and petrographic characterisation of the inor-ganic phases—all related to solar system chemistry.

COSIMA SpecificationsAtomic mass range 1. . . 4000DaRelative atomic mass resolution m/dm at m=300 >2500COSIMA instrument mass 19.8 kgIndium ion pulse duration ≈5nsIndium ion energy 8 keVPower consumption from 28V DC 20.4W

The COSIMA Team

vH&S The von Hoerner & Sulger GmbH is prime con-tractor and responsible for the overall design, man-agement, production, and qualification testing.

The Max-Planck-Institut fur extraterrestrischePhysik (MPE), Garching, Germany, then with Di-rector Prof. G. Haerendel, hosted the PI Dr. JochenKissel, contributed TMU and mechanical systems.

The Bergische Universitat und Gesamthoch-schule Wuppertal (BUGH) participated in devel-opment of the data acquisition unit TDC.

The Finnish Meteorological Institute (FMI),Helsinki, Finland, provided the GSE and theCOSIMA flight software.

The Ingenieurburo Dr. Franz Krueger, Darm-stadt, Germany, provided cleanliness analyses, sci-entific methods for spectra interpretation, and de-velopmental effort for collector targets.

The Institut d’ Astrophysique Spatiale (IAS), Or-say, France, developed the COSISCOPE cameraand the power converters.

The Osterreichisches Forschungszentrum Sei-bersdorf Ges.m.b.H. (ARCS), Austria, providedthe Primary Ion Sources (PIS).

The Institut fur Weltraumforschung (IWF),Graz, Austria, developed the HV supply for the PIS.

The Laboratoire de Physique & Chimie del’Environnement (LPCE), Orleans, France, pro-vided the primary ion optics (PIBS).

The Universitat der Bundeswehr, Neubiberg,Germany, provided collector targets.

Nyle Utterback, Santa Barbara, CA, did the ionoptics design.

The Institut fur Planetologie, Munster, Germany,performed TOF-SIMS analysis of analogs for scien-tific and instrumental comparison.

The Max-Planck-Institut fur Aeronomie(MPAe), Katlenburg-Lindau, provides scienceoperations.

The ROSETTA Spacecraft

ROSETTA at Comet

—Artist’s view

COSIMA Timeline

1992 ESA performs Pre-Study for newCometary Mission “ROSETTA”.

Dr. J. Kissel, MPK Heidelberg,presents dust mass spectrometerconcept based on CoMA/CRAF(NASA mission, canceled).

Sep. 1993 ESA selects ROSETTA asnew “Cornerstone Mission.”

June 1994 Dr. Kissel contacts insti-tutes for contributions, preparesexp. proposal “COSIMA” to ESA.

Dec. 1995 ESA selects COSIMA forthe ROSETTA mission.

Summer 1996 vH&S starts develop-ment of COSIMA eng. model.

1998 vH&S receives contract for theCOSIMA flight model.

July 2002 vH&S delivers the COSIMAflight model (XM) to ESTEC.

Jan. 2003 ROSETTA launch (Kourou)postponed by ESA.

July 2003 COSIMA emitter mainte-nance session at GSC, Kourou.

26 Feb. 2004 Planned launch date.

Aug. 2014 Arrival (prelim.) at comet67P/Churyumov-Gerasimenko.

COSIMA Functional Principle

Target

Target

Target

Indium

Camera(Camera Pos.)

Ion Optics Ion Source

Ion Reflector

Ion Detector

Electronics

Robotic Arm with Target(Spectrometer Pos.)

(Collect Position)

Cometary Dust

Target Store

(Chemistry Station)

Tungsten Needle

Secondary Ion Beam

Primary Ion Beam

cosima−func−en.fig

ROSETTASpacecraft

Drift Tube

COSIMA Block Diagram

Divider Chain

Power

Data

KAL

Data

Amp.

Sensors

Motors

Start

Poi

nt to

Tar

get

PIBS

Camera

GND

COSISCOPE

TMU

PIS ControlPIBS ControlDeflection Cntl.InterfaceControl

Deflection Cntl. ControlHK−Unit

S/C−Interface

Casc.Supply HVC

Cascade Cascade

Chain

(DET−CASC)(PA−CASC)

(TOF1/2−HVC)

(D−, A−CNTL)(D−CNTL, A−CNTL)(D−CNTL, A−CNTL)

(Board Names in Brackets)

Chop. HVCBunch. HVC

GeneratorPIBS TimingPIBSCameraTMU

Primary Ion

Divider

DetectorPost−Accel.

(SERIF)

Low−VoltageTOF−HVCTOF

Secondary Ion Reflector

(D−, A−CNTL) (D−, A−CNTL)(HK1, HK2)

Switch Unit(LVS)(D−CNTL)

(SERIF)(TMUC, TMUD−A, −B)

BootPROM SRAM

Program WatchDog

Latch−Up−Cntl.

CPU21020

DataSRAMEEPROM

ProgramBusI/F LVC

(LVC)

(TDC−TDC)

CO

SIM

A E

xper

imen

t Bus

Cam

era

TM

U

TD

C

PIS

, PIB

S, T

OF

Sta

tuse

s

Tem

pera

ture

s

Cur

rent

s

Vol

tage

s

Sta

rt

COSIMA Experiment Bus

CC

D

(DET−NW)

Ion Path

Extr. Lens

Reflector

Ion Detector

Target

Emitter AChopper

3−Stage Buncher

Emitter CLC1

LA1

Analyze Beam

Clean Beam

HVCU_px

U_peHVC

Beam Switch

Drift Tube

$Revision: 1.15 $

HVCHVC Dual−HVCDeflection Unit

Deflection UnitTOF−HVC

PA−HVC(PA/DET−HVC) (PA/DET−HVC)

(PIBS/TOF−DU)(TOF3−HVC)

(PIBS/TOF−DU) (L1/2−HVC) (L1/2−HVC)(CB−HVC)(CB−HVC)

Lenses 2 Lenses 1Beam Switch

TDC(TDC−TDC, −DAC,

−PTC, −TRIG) (CPU)

DET−HVC

(BS−HVC)

Hea

ter

Sup

ply

cosimablk.fig

LA2

LC2

COSIMA Measurement Principle

• Cometary dust is collected on targets, which are stored in Target ManipulationUnit (TMU).

• The dust grains are located by microscopic camera COSISCOPE.• A pulsed primary Indium ion beam partially ionises the dust grains.• The secondary ions (pos. or neg., selectable) are accelerated by electrical fields,and travel well-defined distance through drift tube and ion reflector.

• A multisphere plate with dedicated amplifier is used to detect the ions.• The arrival times of the ions are digitised and accumulated into 2ns bins.• The mass spectra are calculated from the time-of-flight spectra.

The COSIMA InvestigationCOSIMA has been proposed, developed, and delivered by an international teamof 39 investigators. The PI Jochen Kissel (MPAe) and 4 CoPIs Yves Langevin (IAS),Rita Schulz (ESTEC), Johan Silen (FMI), and Hanna von Hoerner (vH&S) areleading the investigation. Funding comes from DARA/DLR and the respectiveother national agencies. The special support by ESTEC in a critical situationbefore delivery is gratefully acknowledged.

COSIMA Contact, Links

COSIMA Info von Hoerner & Sulger GmbH, Schlossplatz 8, D-68723 Schwet-zingen, Germany, http://www.vh-s.de, Tel.: (+49) 6202 / 5756-16,E-mail: henkel@vh-s.de. This poster is available at:http://www.vh-s.de/projects/cosima/press/a4poster.pdf

MPAe Homepage http://www.linmpi.mpg.de

MPE Homepage http://www.mpe.mpg.de

FMI COSIMA Homepage http://www.geo.fmi.fi/PLANETS/Cosima.html

ROSETTA Homepage http://rosetta.esa.int

Poster first presented at EGS-AGU-EUG joint assembly, Nice, France, 10 April 2003. Revised and extended 22 April 2004, Rev. 1.106. Poster by pdfTEX.