Rafael Rodrigo - La misión Rosetta al cometa 67P

Instrumentos OSIRIS y GIADA:
Contribución científica y tecnológica española a la misión
ROSETTA
Rafael Rodrigo
CAB (INTA-CSIC and ISSI, Bern)
M.D. Sabau (INTA)
Fundación Areces
Madrid, 5 Mayo, 2015

Rosetta’s objectives
- Bringing a lab to a comet !
- Determine the physical properties and
the chemical composition of a comet
by in-situ investigations.
- Study the evolution of the cometary
phenomena (coma and tail) while the
comet approaches the Sun.
- Observe at least two asteroids from close
by, so to study another class of primitive
members of the solar system to
understand better how it was formed.

Scientific instruments
- Remote Sensing
OSIRIS (Imaging)
ALICE (UV spectroscopy, 70-205 nm)
VIRTIS (VIS and IR mapping spectr., 0.25-5 m)
MIRO (Microwave spectroscopy)
- Composition analysis
ROSINA (neutral gas and ion mass spectrometer
12-200 amu)
COSIMA (Dust mass spectrometer)
MIDAS (Grain morphology)

Scientific instruments
- Nucleus large-scale structure
CONSERT (Radio sounding, nucleus tomography)
- Dust flux, Dust mass distribution
GIADA (Dust velocity and impact momentum)
- Comet plasma environment, solar wind interaction
RPC (Langmuir probe, ion and electron sensor,
fluxgate magnetometer, ion composition
analyser, mutual impedance probe)
RSI (Radio Science)

NAC – Narrow Angle Camera
FOV 2.2°, IFOV 18.6 µrad/px
SiC, 2k x 2k BI E2V CCD, AB
3-mirror off-axis, f/8, 717mm
WAC – Wide Angle Camera
FOV 12°, IFOV 101 µrad/px
Al bench, 2k x 2k BI E2V CCD, AB
2-mirror off-axis, f/5.6, 140mm
NAC
WAC
2 cm px res @ 1 km
10 cm px res @ 1 km
OSIRIS
Scientific Imaging System

Two high performance cameras
- NAC and WAC.
- Optimized for comet observations.
- 32 filters from 250 to 1000 nm
(UV to IR).
Built by European consortium from:
- Germany, Italy, France, Spain,
Sweden and ESA.
Max Planck Institut für Sonnensystemforschung (MPS),
Università di Padova (UPD), Laboratoire d’Astrophysique de Marseille (LAM),
Instituto de Astrofísica de Andalucía (IAA-CSIC), Scientific Support Office-ESA (SSO),
Instituto Nacional de Técnica Aeroespacial (INTA), Univ. Politécnica de Madrid (UPM),
Dept. of Astronomy and Space Physics, Uppsala Univ (DASP),
Institut für Datentechnik und Kommunikationsnetze der TU Braunschweig (IDA).
OSIRIS
Scientific Imaging System
Osiris

El Consorcio OSIRIS
- Max-Planck Institut für Solarsystemforschung, Alemania
- Laboratoire d’Astrophysique de Marseille, Francia
- Università di Padova, Italia
- Instituto de Astrofísica de Andalucía, España
- Astronomical Observatory, Suecia
- Scientific Support Office-ESA,ESTEC
- Dept. of Astronomy and Space Physics, Uppsala Univ, Suecia
- Institut für Datentechnik und Kommunikationsnetze der TU
Braunschweig, Alemania
Contribución Española
- IAA: MCB
- INTA: FWM y PCM
- UPM: Modelos Térmicos y Análisis de Elementos Finitos
- Industrias: Sener, Casa, Crisa y Tecnológica

IDR-UPM
Mantas Térmicas
Diseño Estructural
Diseño Térmico
INTA
Ruedas de Filtros
Fuentes de
Alimentación
UDIT - IAA
Controladora de
Mecanismos
Gestión General
El IAA es Co-Investigador del Instrumento y lidera el
Consorcio Español

Las cámaras van dotadas de diversos filtros que permiten la
obtención de datos mineralógicos y el estudio de la coma del
cometa desde su origen nuclear
Cámara NAC Modelo
Proto-Flight
LAM - Marsella
Cámara WAC Modelo
Vuelo
UPD - Padua
Rueda de Filtros
Modelo Vuelo
INTA - Madrid

Módulo Convertidor de potencia en la E-Box

Mechanism Controller Board
El diseño físico consiste en dos circuitos impresos cuyos
componentes están localizados en el interior de un sandwich
formado por los PCBs, e interconectado por dos conectores
flexibles.
Las funciones a realizar por MCB son el control de los
dispositivos electro-mecánicos del instrumento, y el control de la
adquisición de datos (housekeeping).

La tarjeta superior
está destinada a alojar
los circuitos de drivers
de motores
El núcleo de MCB
está compuesto por
dos FPGAs una
dedicada al control
de los drivers y la
otra a las
comunicaciones con
la DPU y al
housekeeping. Existe
una redundancia
completa de estos
dispositivos
La inferior se encarga
de la electrónica
digital de control.

GIADA (Grain Impact
Analyser and Dust
Accumulator)
Estudiar las propiedades
mecánicas de las partículas de
polvo cometario en los
alrededores del núcleo. Tres
tipos de sensores miden la masa,
la velocidad, el momento y el
flujo de estas partículas.

El Consorcio GIADA
- GIADA ha sido construido por un Consorcio liderado por la
Univ.Napoli “Parthenope” e INAF-Oss.Astr. Capodimonte,
en colaboración con el
Instituto de Astrofísica de Andalucía (CSIC),
Selex-ES,FI y SENER.
GIADA está en la actualidad gestionado y operado por:
Istituto di Astrofisica e Planetologia Spaziali‐INAF (Italia).

Prototipo. Detalle de la electrónica digital

Modelo de calificación electromagnética.
Vista frontal de la fuente de alimentación y la CPU.

Modelo de vuelo.
Vista trasera de la fuente de alimentación y la CPU.

Modelo de vuelo. Vista frontal de la tarjeta analógica.

Giada2 – GIADA - ROSETTA
Funcionalidades: Adquisición de datos de los diferentes
sensores, pre-procesado y procesado de datos, interfaces S/C,
conversión de datos y fuente de alimentación, housekeeping del
instrumento.

Rosetta’s journey to
67P/Churyumov-Gerasimenko
- Launch (2 March 2004, from Kourou, French Guyana).
- Deep-space Maneuver, 1st Earth swig-by (4 Mar 2005).
- Deep-space Maneuver, Mars swing-by (25 Feb 2007).
- 2nd Earth swing-by (13 Nov 2007).
- Steins fly-by (5 Sept 2008) – 800 km distance, 5 km diameter.
- Deep space Maneuver, 3rd Earth swing-by (13 Nov 2009).
- Lutetia fly-by (10 July 2010) – 3000 km distance, 100 km diameter.
- Deep space Maneuver and start hibernation (8 June 2011).
– within 4.5 AU from Sun.
- Exit from hibernation and Deep space Maneuver (20 Jan 2014).
prime Science missions begins
- Comet r-v (6 Aug 2014) 4.5-4 AU from Sun.
- Philae Lander deployment (12 Nov 2014)
at 3.25-3 AU from Sun.
- Comet closest approach to the Sun (Aug 2015).
- End of Mission (31 Dec 2015).

Asteroid (2867) Steins (5.9x4 km). Rosetta, Sept 5, 2008
Credits:ESA/Rosetta/MPSforOSIRISTeamMPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

Cometas
Asteroid 21 Lutetia (r eff=100 km) Rosetta, July 10, 2010
- 462 images at 3,170 km. Relative speed: 15 km/s.
- Asteroid Type-M with one of the highest densities measured: 3.4 ± 0.3 g cm-3
- Surface covered by a thick layer of regolith, with a central crater of 55 km.

Albedo (visible) 0.19 ± 0.01. Typical spectra of surfaces composed by primitive material.
Absence of absorption bands, associated to silicates as olivine or pyroxene.

2°x2° NAC Image Close-up. Rosetta at approx. 5 Mio km of the comet and
660 Mio km from Earth.
Comet in NAC View on March 21, 2014
M107
67P/C-G

Comet Wake-up
27/3, 3/4, 7/4, 14/4, 17/4, 20/4, 27/4, 30/4, 4/5
(exposure time: 720 s)
5 Mio km to 2 Mio km distance to the comet

Credits: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

NAC F22, July 7, 2014. Nucleus started to be resolved.

1P/Halley 81P/Wild 2 9P/Tempel 1
19P/Borelly 103P/Hartley 2

SHAP1
14 July, 2014
12.000 km
220m/px

A Close Binary? The result of a soft impact of two small cometesimals.

03 August 2014
285 km 5.5 m/px
1 km

Thomas et al., Science, 2015.
19 different morphological regions based upon large scale unit boundaries.

Hathor
Hapi
Set

Dynamic - The Crack
Justification: Crack structure in area of activity.

Crack Detail
• Crack is not uniform along
length.
• Small slope or composition
change within region.
– The smooth area is not
uniform
• Crack formation through a
thermal contraction
mechanism in frozen soils.
Thomas et al., Science, 2015

El-Maary et al., GRL, 2015.
First ever observations of meter-scale fractures on a surface of a comet, some forming polygonal networks.
a) Polygonal fractures on the edge of the Apis region on the body lobe, patterns are composed of irregular 2-5m-wide polygons.
b) Fractured region at the edge of the Atum regions close to the neck. Fractures vary greatly in length and mode of intersection forming highly
irregular polygons. The longest visible facture is ~250 m. Within this irregular pattern, a more regular pattern of 2–6 m-wide polygons is visible.
c) Regular patterns in at the edge of Nut depression creating ~15 m-wide polygons with orthogonal fracture intersections.
d) Polygonal patterns on the edge the ridge separating Anubis/Atum from Ash and Seth regions.
Image has been overexposed to highlight the shadowed features. Smaller embedded polygons are 2–5 m-wide.

a) NAC image of the Ash region in the foreground and the regions of Hathor and Anuket in the background.
b) Close-up of the fractures scarp showing what appears to be a new fracture cross-cutting two previous fractures.
The new fracture is 100–125 cm-wide and is expected to lead to mass wasting of the fractured scarp.
c) Small fracture that appears to cut though the scarp edge and the smooth coating on the top (morphologic characteristic of the Ash region).
d) Cropped NAC image of another mesa in the Ash region showing a similarly fractured scarp and a debris field in at the foot of the cliff,
suggesting a progressive process of mass-wasting.
El-Maary et al. GRL, 2015.

NAC_2014‐09‐05T06.31.16.575Z_ID10_1397549600_F22 (Imhotep region)
Smooth terrain
Layering of material
Smooth material on topo higher surfaces
Circular structures
Layered consolidated material
Fracturing of the consolidated material
650 m diameter raised semi‐circular structure

NAC at 130 km; Aug 6. Resol.: 2.4m/px

Boulder Cheops. NAC, 19 Sept: distance= 28.5 km. Maximum dimension of about 45 m.

NAC_2014‐09‐02T21.44.22.575Z_ID10_1397549800_F22
Circular depression in Set, partially eroded
Surface deflation

NAC_2014‐08‐22T03.42.53.641Z_ID30_1397549000_F22 Alcove at the Hathor-Anuket boundary

NAC_2014‐09‐18T08.07.20.370Z_ID10_1397549000_F22 Tectonic feature in the Aker region

NAC_2014‐09‐12T05.09.04.388Z_ID10_1397549600_F22 Fracturing and layering at Hapi

Boulders. Cauliflower. Growing out of the cliff faces? Erosion? Highly porous icy wall?

Max-Planck-Institut für
Sonnenystemforschung
EuroPlanet Science Congress
Cascais, Portugal
08-12/09/14 Jean-Baptiste Vincent
OSIRIS team
Comets might be primordial objects at their core, but they have experienced
significant surface processing. We need to understand this evolution if we want
to link current observations to the origin of the Solar System.
Fundamental questions:
• What is cometary activity ?
• Why is only a small fraction of the surface active ?
• Is there a link between coma and surface features ?
1P/Halley, GIOTTO 1986
19P/Borelly,
Deep Space 1 2001 103P/Hartley 2, EPOXI 2010
Cometary Evolution and Activity

Rosetta
SWT#38
25/09/14 Jean-Baptiste Vincent
OSIRIS team
05Aug_23:20 06Aug_00:20 06Aug_01:20 06Aug_02:20
06Aug_03:20 06Aug_04:20 06Aug_05:20 06Aug_06:20
WAC images, August 05-06 2014, 3.60 AU, 175 km, 12 m/px
One large feature visible, focused in a narrow jet some time during the rotation. Combination of
projection effect and temporal variation as the illumination conditions are changing with the
rotation.
By observing the activity from different angles, we can link dust features in the coma to specific
regions on the surface, and morphologic/color information.
63/14

NAC , August 8

NAC , August 28

WAC , August 8 Chunks: dust clouds embedded in the jet
Lara et al., A&A, 2015

Ash starts to
become active
very recently
Gutiérrez et al.WAC, September 16

WAC, September 16 Gutiérrez et al.
Ash starts to
become active
very recently

WAC Sept 23

VLT August 11. Dusty coma extending at least 19,000 km from the nucleus.
Rosetta was deep inside the “atmosphere”, coma (100 km from the nucleus).

Outburst: 12 March 2015

Activity found before Sunrise
(S/C~80km, rh~2.12 AU, 7.85m/px)

• Dust travel 400-500m in 130s: vd ~ 3-4 m/s
• Slope changed within 100m
-> fast sublimation or fragmentation
• Source of Imhotep outburst
-> Cliffs or changes Sunrise Jet or in its surface
2015-03-12T12.43.55.838
There are also other new jet activities looking
like coming from Imhotep ?
Z.-Y. Lin, J.-C. Lee and W.-H. Ip

Illumination is not accurate because no ray tracing was using to calculate shadows.
J.B. Vincent, 2015

One of the most recent images, the source is somewhere in the yellow circle.
No obvious surface changes.
NAC_2015-04-15T13.06.03.556Z_ID30_1397549001_F24
J.B. Vincent, 2015

MTP007/SHAP4S – September 2014
J.B. Vincent, 2015
No obvious changes are found. Given the very short duration of the outburst, and the very low
brightness of the associated plume, it could be concluded that very low dust masses are involved.

Rosetta
SWT#38
OSIRIS team
82/14
Active pits
Most of the activity comes from the transition region, probably from several
sources (cliffs on both sides, outcrops, boulders, cracks…) yet to be determined
unambiguously.
Some jets can be consistently traced down the inner walls of a pit, across several
Vincentetal.,Nature,2015

Rosetta
SWT#38
OSIRIS team
The pit has a very peculiar morphology, with horizontal layers, but
also vertical striations and pebble-like features yet to be explained.
Many jets can be linked to this hole, apparently starting from the
bright walls on both sides. There is almost continuous activity
during a comet day as each side gets illuminated.
There are other pits with similar morphologies and hints of activity.
83/14Sierks et al., Science, 2015. (NAC Aug. 28; at 60 km; Resol.: 1m/px)

Rosetta
SWT#38
OSIRIS team
Pit formation mechanism by sinkhole collapse:
- A sub surface heat source sublimes surrounding ices (left).
- This gas then escapes or redeposit, thus forming a cavity.
- When the ceiling gets too thin to support its own weight it collapses,
creating a deep, circular pit with a smooth bottom.
Newly exposed material in the pit’s walls can start to sublime.
84/14Vincent et al., Nature, 2015.

Rosetta
SWT#38
OSIRIS team
85/14Recently observed crater in Siberia, believed to be formed by a sudden methane release from the permafrost.

• 67P is active.
• We see large temporal and spatial variations.
• Most of the activity is located in the transition region between the two lobes.
• Work ongoing on determining precise source locations, and modeling dust features.
• Several "active pits" detected, geomorphological study and continuous monitoring in
progress.
• Existing models of activity still valid for the jets and their sources.
Summary

Della Corte et al., A&A, 2015
GIADA working principle (top panel).
Dust particles quantities measured by
GIADA and derived ones (bottom panel).

Credit: ESA/Rosetta for GIADA Team
Giada

Rotundietal.,Science,2015

Fulle et al., ApJL, 2015.
Shower of fluffy agglomerates detected by OSIRIS-WAC on 29th Jan. 2015
GIADA collected particles belonging to two families:
(i) compact particles (ranging in size from 0.03 to 1mm),
(ii) fluffy aggregates (ranging in size from 0.2 to 2.5 mm) of sub-micron grains. Fluffy aggregates detections are
a factor of 10 higher than compact particles.
The dynamics of the fluffy aggregates is biased by an electrostatic interaction with the spacecraft.
The fluffy aggregates are actually the products of fragmentation of bigger and charged parent aggregates
that interact with the spacecraft negative potential.
They thus enter in GIADA as “showers” of fragments at speeds <1m s−1.
The equivalent bulk density of such optically thick aggregates is constrained to <1 kg m−3.

Credit: ESA/Rosetta/MPS for COSIMA Team MPS/CSNSM/UNIBW/TUORLA/IWF/IAS/ESA/
BUW/MPE/LPC2E/LCM/FMI/UTU/LISA/UOFC/vH&S Schulz et al., Nature, 2015.

Fulle et al., ApJL, 2015.Credit: ESA/Rosetta for GIADA Team
Number of fluffy particles as a function of comet distance.
The number of detections is normalized to the time spent by the spacecraft at specific distances (Feb-March 2015).
- Detections at < 25 km correspond to the Close Flybys (the trajectory during which the STRs undergone to a malfunctioning.
- Detections to distances > 55 km are relative to the Far Flybys, when the STRs worked nominally.
- Conclusion: “the concentration of fluffy particles should be acceptable for the STRs at distances > 70 km.”
- The trajectory geometry could represent an issue, but a pyramid trajectory, being similar to the Far Flybys,
at distances > 70 km, should be safe.

NAVCAM at 26.8 km; Oct. 30. Resol.: 2.27m/px

NAC at 15.5 km from the surface; resol.: 28 cm/px; the enlarged insets are 17 x 17 m.
First Touchdown: 15:34
Second: 17:25
Third: 17:32

GIADA Team: A. Rotundi, V. Della Corte, J.J. López-Moreno, M. Accolla, N. Altobelli, E. Bussoletti, L.
Colangeli, M. Cosi, J.F. Crifo, F. Esposito, M. Ferrari, M. Fulle, F. Giovane, S. F. Green, E. Gruen, B.
Gustafson, M. L. Herranz, S. Ivanovski, J. M. Jerónimo, P. L. Lamy, M. R. Leese, A. C. López-Jiménez, F.
Lucarelli, E. Mazzotta Epifani, M. McDonnell, V. Mennella, A. Molina, R. Morales, F. Moreno, J. L. Ortiz, E.
Palomba, P. Palumbo, J. M. Perrin, F. J. M. Rietmeijer, R. Rodrigo, J. Rodríguez, J. A. R. Sordini, P. Weissman,
V. Zakharov, J. C. Zarnecki.
Special thanks: A. Rotundi and V. Della Corte (IAPS and Univ Napoli)
M. Fulle (INAF-Obs. Astronomico Trieste)
Rosetta Science Ground Segment at ESAC, the Rosetta Mission
Operations Centre at ESOC and the Rosetta Project at ESTEC for their
outstanding work, overcoming all the technological challenges and
enabling the science return of the Rosetta Mission.

OSIRIS Team: H. Sierks, C. Barbieri, P. Lamy, R. Rodrigo, D. Koschny, H. Rickman, J. Agarwal, M. A'Hearn,
I. Bertini, F. Angrilli, M. A. Barucci, J. L. Bertaux, G. Cremonese, V. Da Deppo, B. Davidsson, S. Debei,
M. De Cecco, S. Fornasier, M. Fulle, O. Groussin, C. Güttler, P. Gutiérrez, S. Hviid, W. Ip, L. Jorda,
H. U. Keller, J. Knollenberg, R. Kramm, E. Kührt, M. Küppers, L. Lara, M. Lazzarin, J. J. López, S. Lowry,
S. Marchi, F. Marzari, H. Michalik, S. Mottola, G. Naletto, N. Oklay, L. Sabau, C. Snodgrass, N. Thomas,
C. Tubiana, J-B. Vincent, P. Wenzel, all Associate Scientists & Assistants.
Special thanks: P.J. Gutiérrez and L.M. Lara (IAA-CSIC)
N. Thomas (UBe), H.U. Keller (TU Braunschweig)
H. Sierks and J.B. Vincent (MPS)
Rosetta Science Ground Segment at ESAC, the Rosetta Mission
Operations Centre at ESOC and the Rosetta Project at ESTEC for
their outstanding work, overcoming all the technological challenges
and enabling the science return of the Rosetta Mission.

Rafael Rodrigo - La misión Rosetta al cometa 67P

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Rafael Rodrigo - La misión Rosetta al cometa 67P