ESA UNCLASSIFIED – For Internal Use

Missione ESA-JAXA BepiColombo

Partecipazione Italiana: Progetti e Opportunità

Stefano Orsini (INAF-IAPS)

SAIt - Società Astronomica Italiana 57° Congresso

Bologna, 7-10 maggio 2013

MMO

MPO

The BepiColombo fleet

MPO Flight Model mechanical and propulsion bus delivered

MPO vacuum bake-out completed

Flight model harness for MPO delivered and ready for integration

MTM Flight Model mechanical and propulsion bus in integration

MPO FM and MTM STM

MPO FM at Phenix facility

MPO FM harness

Spacecraft Status SWG#10, March 6, 2013

MTM STM: mass properties test and thermal balance test at 10 Solar

Constants completed.

System functional tests on Spacecraft Engineering Test Bench

continuing with delivery and integration of the MMO Electrical Model

Payload FM delivery: mid-2013 – beginning 2014.

Delta-CDR: September 2013. LAUNCH: MID-2016 (TBC)

ETB at Friedrichshafen

Spacecraft Status 2 SWG#10, March 6, 2013

BepiColombo Instruments

PI E. Flamini @ ASI

G. Cremonese @ INAF-OAPd

V. Da Deppo @ CNR-IFN UOS

G. Naletto @ UniPd CISAS

M.T. Capria @ INAF-IAPS

P. Palumbo @ Uniparthenope

E. Mazzotta Epifani @ INAF-OAC

F. Capaccioni @ INAF-IAPS

M.C. De Sanctis @ INAF-IAPS

G. Piccioni @ INAF-IAPS

G. Filacchione @ INAF-IAPS

S. Debei @ UniPd CISAS

E. Lorenzini @ UniPd CISAS

M. Zaccariotto @ UniPd CISAS

C. Bettanini @ UniPd CISAS

A. Francesconi @ UniPd CISAS

P. Nicolosi @ UniPd Dip.II

M.G. Pelizzo @ CNR-IFN UOS

V. Iafolla @ INAF-IAPS

F. Santoli @ INAF-IAPS

R. Peron @ INAF-IAPS

D. Lucchesi @ INAF-IAPS

E. Amata @ INAF-IAPS

C. Federico @ UniPg

M. Storini @ INAF-IAPS

M. Laurenza @ INAF-IAPS

BC Italian scientific team

SIMBIO-Sys

Stereo Camera - STC

High Res.Cam. - HRIC

Vis-IR imag.spec.-VIHI

TM & System

ISA

L. Iess @ UniRoma

P. Tortora @ UniBO

A. Milani @ UniPI

MORE

S. Orsini @ INAF-IAPS

A. Milillo @ INAF-IAPS

E. De Angelis @ INAF-IAPS

A. Mura @ INAF-IAPS

S. Selci @ CNR-ISC

R. Leoni @ CNR-IFN

SERENA

PHEBUS

MIXS

MEA

SIXS

ASI science management

Elena

SIMBIO-SYS (PI: Enrico. Flamini, ASI)

The SIMBIO-SYS (Spectrometer and Imagers for MPO BepiColombo –

Integrated Observatory SYStem) instrument architecture is based on 3

different optical channels sharing a common Main Electronics and PDU.

HRIC

Local mapping at high resolution with colour

capabilities.

Spatial resolution 5-10 m/pixel @ periherm

Filters: pan, 550, 750, 880 nm.

STC

Global stereo mapping and DTM

reconstruction.

Spatial resolution 50 m/pixel @ periherm

Filters: pan, 420, 550, 750, 920 nm.

VIHI Global mineralogical mapping;

Spatial resolution 100 m/pixel @ periherm

Spectral coverage 0.4-2.0 µm with 6.25nm

resolution Flamini et al. PSS 58, 2010

SIMBIO-SYS Package

Co-PI Gabriele Cremonese STC overall responsibility

Co-PI Pasquale Palumbo HRIC overall responsibility

Co-PI Fabrizio Capaccioni VIHI overall responsibility

Co-PI Yves Langevin Main Electronics Calibration at package level Co-PI Alain Doressoundiram VIHI proximity electronics FPA procurement & Calibration TM Stefano Debei Instrument architecture Thermal and structural design Scientific Req. Implementation INDUSTRY SELEX GALILEO

IASorsay

Stereo Channel(STC)

1. Global mapping in stereo

mode at spatial resolution of

< 110 m, max resolution of

50 m per pixel at the

periherm (400 km)

2. Mapping in four colours at

spatial resolution of < 110 m

Science goal: Digital Elevation

Model of Mercury Surface

IASorsay

High Resolution Imaging Channel (HRIC)

Science

goal

Acquisition

conditions

Expected

resolution

Coordination

with

Geomorphology

characterization

of selected areas

400 < h < 690 km

Periside

Phase angle < 90°

5 – 8 m STC

VIHI

BELA

Mineralogy

mapping at small

scales

400 < h < 545 km

Periside

Phase angle < 50°

10 – 15 m STC

VIHI

Targeting

operation

mode

on selected

interesting

areas

IASorsay

Visible and Infrared Hyperspectral Imager (VIHI)

MORE • The Mercury Orbiter Radio-science

Experiment (MORE) addresses the mission

scientific goals in geodesy, geophysics and

fundamental physics. It will:

• Provide crucial experimental constrains to

models of the planet’s internal structure,

determine the size of the inner and outer

core, the thickness of the mantle and the

crust.

• Test theories of gravity with unprecedented

accuracy

• Test the novel tracking system in precise orbit

determination and space navigation

Scientific Goals

Gravity Rotation Relativity

Harmonic

coefficients up to

degree 25

Moment of inertia of

the planet and its

mantle

Post-Newtonian

parameters

Love number k2

Rotational state of

the planet

Solar gravitational

oblateness ( J2)

PI: Luciano Iess, Univ. La Sapienza

On board instrumentation

• High gain antenna (diameter = 1 m)

• Two trasponders:

- X/X/Ka Deep Space Transponder (DST)

- Ka/Ka Deep Space Transponder (KaT)

X Ka X Ka

Range rate: ≈ 3 μm/s accuracy @1000 s (two

way)

Range: 20 cm accuracy (two way)

End to end Allan deviation:

1.4e-14 @ 1000s

A system-level experiment

High precision

data

Accurate orbit

determination

Experiment

goals

Ka Transponder Specific Radio Science Ka/Ka link

for precise Doppler and ranging

measurements

TT&C subsystem: -High gain antenna (HGA)

- RF network

-X/X/Ka Deep Space Transponder

(DST)

X/X and X/Ka link for Doppler and

ranging measurements

ISA tri-axial accelerometer Precise measurements of non-

gravitational acceleration

Ground station equipment

and ancillary data

Simultaneous tracking of the

spacecraft by the X/X, X/Ka and

Ka/Ka frequency links and

calibration of the tropospheric

effects

AOCS subsystem Attitude reconstruction

High resolution camera

(SIMBIO-SYS)

Laser altimeter (BELA)

Determination of Mercury’s rotational

state

Geodesy experiment

Participating Institutions

in Italy:

Sapienza Università di Roma

Università di Pisa

Università di Bologna

ISA (Italian Spring Accelerometer) (P.I.: V. Iafolla, IAPS-INAF) is part of the

BepiColombo suite of instruments dedicated to RSE (Radio Science Experiments)

By measuring the non-gravitational perturbations acting on the MPO

spacecraft, it will enable an accurate reconstruction of its gravitational orbit around

Mercury, in order to:

• Constrain the internal structure of the planet (measurement of global gravity field

and of its temporal variations due to solar tides, local gravity anomalies, rotation

state)

• Test Einstein General Relativity theory (improved determination of PNP)

parameters)

ISA performance

Measurement bandwidth 3105 ÷ 1101 Hz

Intrinsic noise 1109 m/s2/Hz

Measurement accuracy 1108 m/s2

Dynamics 300108 m/s2

A/D converter saturation 3000108 m/s2

The instrument is an ensemble of three one-axis sensors arranged in

such a way to measure the acceleration vector acting on it

Courtesy

TAS-I

ISA will be the first among such type of instruments to fly on an interplanetary mission

Control

capacitors

Pick–up

capacitors

Proof–

mass

Decennal experience of the

Experimental Gravitation Group (IAPS-

INAF) in:

• Measurement of small forces

• Fundamental physics tests

• Geophysical instrumentation

Courtesy

TAS-I

Courtesy

TAS-I

Given its high sensitivity, the

instrument pushes the requirements

on the spacecraft in terms of

dynamical environment (mechanical

and thermal noise)

In practice, its proof masses will constitute a

virtual test mass freely falling in the

gravitational field of Mercury

SERENA Search for Exospheric Refilling

and Emitted Natural Abundances Neutral and Ionized Particle Detectors for Hermean Environment Investigations

S. Orsini (PI), S. Livi (CoPI-STROFIO), K. Torkar (CoPI-PICAM), S. Barabash (CoPI-MIPA)

A. Milillo (PI Dep., Sci. Coord.), P. Wurz (Sci. Coord.), A. Olivieri (ASI PM), E. Kallio (SGS),

and the SERENA TEAM

ELENA: Emitted Low Energy Neutral Atoms Neutral particle emission form Mercury’s surface

STROFIO: Exososphere Mass Spectrometer

Exospheric density and composition

PICAM: Planetary Ion CAMera

Planetary ions composition and distribution

MIPA:Miniature Ion Precipitation Analyzer

Solar wind ion precipitation

INDUSTRY: OHB-CGS (Milano) & AMDL (Roma)

SERENA Search for Exospheric Refilling

and Emitted Natural Abundances Neutral and Ionized Particle Detectors for Hermean Environment Investigations

S. Orsini (PI), S. Livi (CoPI-STROFIO), K. Torkar (CoPI-PICAM), S. Barabash (CoPI-MIPA)

A. Milillo (PI Dep., Sci. Coord.), P. Wurz (Sci. Coord.), A. Olivieri (ASI PM), E. Kallio (SGS),

and the SERENA TEAM

ELENA: Emitted Low Energy Neutral Atoms Neutral particle emission form Mercury’s surface

STROFIO: Exososphere Mass Spectrometer

Exospheric density and composition

PICAM: Planetary Ion CAMera

Planetary ions composition and distribution

MIPA:Miniature Ion Precipitation Analyzer

Solar wind ion precipitation

INDUSTRY: OHB-CGS (Milano) & AMDL (Roma)

PICAM

MIPA

ELENA

STROFIO

Soft X-ray shuttering @43kHz

Ion beam_1keV shuttering @43kHz

ELENA is a Time-of-Flight (ToF)

sensor, based on the state-of-the art

of ultra-sonic oscillating shutter

(operated at frequencies of the order

of tens of kHz), mechanical gratings

and Micro-Channel Plate (MCP)

detectors.

The purpose of the shuttering system

is to digitize space and time when

tagging the incoming particles without

introducing “disturbing” detector

elements, which may affect the

particle’s trajectory or the energy. This

is particularly important in this case, in

which neutrals of energies of a few

tens of eVs must be detected.

Parameter Required Actual

Energy range <0.02 – 5 keV <0.01–5keV(mass dependent)

Velocity resolution v/v 10% Down to 10%

Viewing angle 5ox70o 4.5ox76o

Angular resolution 5ox5o 4.5ox4.5o (actual)

4.5°x2.4° (nominal pixel)

Mass resolution M/M H and heavy species H and heavy species

Optimal temporal resolution <5 m 40 s

Geometric factor G 10–5 cm2 sr 3.5 10–5 cm2 sr

Integral Geometric factor 1.1 10–3 cm2 sr

BepiColombo

BC will allow us a step ahead in our understanding

of Mercury and will be the base of our studies for

many years.

Huge Italian community is involved in the effort,

covering many of the technical and scientific fields

of this mission: from this point of view, BC is

certainly an Italy-lead ESA mission.

Next steps: payload FM delivery, system delta-CDR

(September 2013), launch by mid-2016 (or earlier,

TBD)