Download Desarrollo de instrumentación espacial para misiones de la agencia

DESARROLLO DE
INSTRUMENTACION ESPACIAL
PARA LA ESA
Alvaro Giménez
Research and Scientific Support Department
ESA, ESTEC
Los primeros pasos
• La definición de las misiones se hace con un
plan a largo plazo a través de un Call for Ideas
(cada década).
¿Cuáles son los temas preferidos?
150 propuestas recibidas
Una llamada a la comunidad científica europea
Hubble
Newton
Ulysses
Integral
Corot
Smart 1
SOHO
Hinode
Venus Express
Akari
Rosetta
Cluster
Cassini/Huygens
Mars Express
Still to come
Mars
The Moon
Chandrayaan
Sun
Chang’E
Mercury
Stars +
our Galaxy
Infrared + Sub-millimetre
Observatory
Vis-IR observatory
μscope
Gravitational
Waves
Cosmic Microwave
Background
Cosmic Vision 2015-2025
+
Aurora
LISA
SOLAR
F3
ORBITER
GAIA
LISAPF
μSCOPE
BEPI
COLOMBO
JWST
PLANCK
HERSCHEL
ROSETTA
COROT
Hinode
SMART
1
MARS
EXPRESS
HUYGENS
INTEGRAL
Double Star
SOHO
CLUSTER
ULYSSES
Akari
CLUSTER II
XMM
NEWTON
ISO
HST
Time →
VENUS
F2
EXPRESS
Los primeros pasos
• La selección de las misiones se hace con un
Call for Proposals
• Se cuenta con unos 3.5 millardos de euros para 10
años. Es decir unas 3 misiones L y 5 misiones M.
• Esto implica una llamada cada 3-4 años por unos
1000 millones de euros en cada una (2007, 2010 y
2013?)
• Las misiones volarán unos 10 años después (entre
2017 y 2025)
• Hay un proceso de selección en marcha con
propuestas recibidas hasta el 29 de junio.
• Dos tipos de propuestas (se seleccionarán 3 + 3):
Misiones medias (300 M) y misiones grandes (650 M)
CV 2015-2025 Proposals received
Mission Outline
Discipline/Class/Profile
Heritage
In-situ observation of the isotopic ratio and cloud layers of Venus in order to understand the evolution of
Venus and its climate.
Venus
M-class
Balloon, Decent probe
Orbiter
VEP-TRS
Investigation of physical processes leading to acceleration, transport and loss of relativistic electrons in
Earth's radiation belt.
Earth
M-class
Cluster like , 4 S/C
Cross Scale TRS, but only 4
S/C, closer at Earth
Investigate the origin and evolution of the Moon as well as the astrobiologically important possibilities
associated with polar ice by placing scientifically instrumented penetrators into the Lunar surface.
Moon
M-class
hard penetrators (10.000g!)
+ Carrier S/C
EMPIE & EMP (Europa
penetrators) studies, lunar
lander mission analysis
Mission to characterise the very early geological evolution of Mars and the context in which life
potentially arose, to search for traces of the transition from a prebiotic world to life, and to trace the
early evolution of life and its fate as conditions on Mars changed.
Mars
M-class
ExoMars style mission,
complex scenario, expensive
(ExoMars)
Remote sensing and in-situ measurements from orbit of the Mars atmosphere, internal structure and
magnetic field and its interaction with the solar wind in order to understand planetary evolution, the
appearance of life and its sustainability
Mars
M-class
Mars Atmospheric Orbiter +
1 Microsat
Mars studies (lander,
Deimos TRS). Mission
analysis for Mars
In-situ measurements and sample return from a primitive Near-Earth Object (Asteroid or dormant
comet) in order to reveal information about the early formation processes of the solar system and the
role of minor bodies in the origin and evolution of life on Earth.
Asteroid
M-class
JAXA lead mission with ESA
support, to a challenging
NEA
NEA-SR TRS, Deimos TRS,
(Don Quixote)
In-situ measurements and sample return from an active Near-Earth Comet in order to reveal information
about the early formation processes of the solar system and the role of minor bodies in the origin and
evolution of life on Earth.
Comet
M-class
ESA mission to perform
sample return
Comet but similar
problems as NEA-SR TRS,
Deimos TRS (Rosetta)
In-depth, quantitative study of the Jupiter system and its moons, which focuses on the formation of the
Jupiter System, the way how the Jupiter system works, and whether Europa is habitable.
Jupiter
L-class
Europa/Jupiter mission, up
to 3 S/C , 2 launcher
JME-TRS, JSE-TRS &
various CDF's
In-situ measurements of the chemical and isotopic composition of the Saturn atmosphere with two
probes and remote sensing in order to understand the origin, formation and evolution of giant planets,
including extrasolar planets.
Saturn
M-class
ESA contribution to NASA
mission, 2 entry probes to 10
bar
Mission analysis to Saturn.
Strong similarity with Jovian
Entry Probe CDF
In-situ exploration of the two Saturn moons: Titan and Enceladus in order to gain knowledge on their
geological, chemical and evolutionary history and possibly understand their astrobiological potential
Saturn&Encl.
Titan
L-class
NASA mission with ESA
support, 2 S/C, Titanaerobot and Enceladus hard
penetrators.
Aerobot - VEP/TRS (but
Venus), mission analysis
(outer planets)
Dust
M-class
dust observatory at L2,
simple mission, electric
propulsion to L2, Conex
platform
no - but simple
In-situ measurements of interstellar and interplanetary dust particles in order to help characterizing the
physical conditions during the planetary formation process.
CV 2015-2025 Proposals received
Mission Outline
Sample return and in-situ measurements of interstellar and interplanetary dust particles in order to help
characterizing the physical conditions during the planetary formation process.
Discipline/Class/Profile
Heritage
Astrophysics/
Dust
M-class
dust observatory at L2 +
sample return
all sample return TRS
(mainly re-entry problem)
Quantifying the coupling in plasmas between different physical scales in order to address fundamental
questions such as how shocks accelerate and heat particles or how reconnection converts magnetic
energy.
Space Plasma
M-class
up to 10 S/C - 3 tetrahedron
Cross Scale TRS
In-situ mapping of the heliosphere and its boundaries and reveal the nature of the hydrogen wall, the
bow-shock and the local interstellar medium
Interst. Heliop.
L-class
Solar Sail based mission to
leave Solar System, (200AU)
IHP-TRS
Probing and understanding the dynamics the Solar inner core, the radiative/convective zone interface
layer, the photosphere/chromosphere layer and the low corona in order to understand space weather,
space climate and for stellar and fundamental physics.
Sun
M-class
Formation Flying
Coronagraph @ L1, 170 kg
P/L per S/C
(Proba-3)
Perform high spatial, spectral and temporal resolution observations of the Solar atmosphere, from the
photosphere to the corona, and of new insights of the Solar interior and convective zone.
Sun
M-class
Formation Flying
Coronagraph @ L1, HP and
Proteus platform
(Proba-3)
Understanding the origin and evolution of the Sun's magnetic field and its interaction with the
heliospheric plasma by mapping the magnetic field in the solar transition region and corona, both on the
solar disk and above the solar limb.
Sun
M-class
Formation Flying
Coronagraph @ L1
(Proba-3)
Observations of the heliosphere very close to the Sun's surface in order to determine how magnetic
field and plasma dynamics in the outer solar atmosphere give rise to the corona, the solar wind and the
heliosphere.
Sun
exceeding
L-class
Solar Probe style, very close
to the sun (@ 4 Rs) =
extreme hot environment
(Solar Probe)
Determination of the relation between the magnetism and dynamics of the Sun's polar regions and the
solar cycle.
Sun
L-class
Solar Sail based high
inclination Sun observatory
Solar Polar Orbiter TRS
M-class
Multiple hard penetrators
(max 500g), with
meteorological and seismic
instrumentation, inflatable
technology
MetNet national led mission
proposal evaluation (2005/6)
Meteorological, seismic and magnetic network measurements on the Mars surface and from orbit in
order to investigate the planetary interior and better understand the dynamics and general behavior of
the Mars atmosphere as well as providing weather forecast
Mars
CV 2015-2025 Proposals received
Mission Outline
Large multiaperture interferometer based on a large number of spacecrafts and
dedicated to high resolution Visible and near Infrared astronomy.
European contribution to the Japanese SPICA mission, dedicated to Medium and
Far Infrared astronomy and to investigations on the origins of galaxies and
planets.
Class Heritage
?
<M
(EPICURUS)
NA (FIRI)
New generation, space based x-ray observatory dedicated to investigations on
the evolution of the universe at higher energies and based on a 2 spacecraft
formation concept.
L
XEUS (SymbolX)
A space based, near Infrared interferometer dedicated to the study of the
interplanetary environment around young stars and solar-type stars, based on a 3
spacecraft formation concept.
M
Darwin, Pegase
study CNES
Ultra-high precision, visible and near-infrared photometry mission, dedicated to
investigations on exo-planets transiting in front of a large sample of stars as well
as to investigations on the seismic oscillations of these parent stars.
M
(Eddington,
Corot, Kepler)
Visible and near-Infrared telescope dedicated to the direct detection of Giant or
super-Earth extra solar planets.
M
No
Hard X-ray and gamma-ray space based observatory dedicated to the study of
the universe wit respect to high phenomena dominated by high energy and
extreme density.
M
GRL-TRS
(MAX-CNES)
A far-infrared interferometer, capable of achieving high resolution imaging and
spectroscopy and dedicated to the study of the early stages of the galaxies, stars
and planets formation.
L
FIRI-TRS
A wide field, visible and near-infrared space imager, with the primary goal of
studying dark energy and dark matter with unprecedented precision by using
weak gravitational lensing.
M
WFI-TRS
(CNES Dune)
An all-sky gamma-ray and X-ray observatory dedicated to the study of the early
universe, using investigations of the gamma ray bursts.
M
no
(SWIFT, GRL)
A medium-infrared nulling interferometer, dedicated to the study of terrestrial
extra-solar planets and based on a formation of 5 spacecrafts.
L
Darwin
CV 2015-2025 Proposals received
Mission Outline
An experiment dedicated to the measurement of the speed of radio signal
between spacecrafts and Earth.
Class Heritage
?
Theoretical proposal dedicated to investigations on the space and time relation.
No (Pioneer 10)
No
Mission dedicated to the verification of Einstein's general relativity theory, via
deep space laser ranging experiments and atomic clock measurements.
M
No
Experiment dedicated to test the nature of gravitation and the general reality
theory via interplanetary laser ranging experiments.
M
No
Mission dedicated to the verification of the laws of gravity at the largest possible
distances. The mission would entail a probe reaching heliospheric distances
larger than 10 AU and performing radio-tracking and laser ranging experiments.
M
No
Drag-free spacecraft platform hosting a number of experiments dedicated to the
investigation of the gravitation laws and their link to other forces of nature.
M
FPE-B TRS
(STEP, HYPER,
Space mission devoted to a precise measurement of the properties of space-time
using atomic clocks (e.g. modification of time in presence of gravity).
M
FPE-A TRS
Space mission dedicated to the test of the equivalence principle via atom based
interferometry.
M
FPE-B/C TRS
(STEP, HYPER)
A space based observatory dedicated to the study of ultra-high energy cosmic
particles interacting with the earth atmosphere.
?
EUSO studies
SAGAS is a mission dedicated to the study of all aspects of large scale
gravitational phenomena in the solar system, based on an interplanetary travel to
large heliospheric distances.
L
No
FPE / Pioneer 10
Space mission dedicated to investigations of critical physical phenomena
occurring in microgravity conditions.
Space mission dedicated to the test of the equivalence principle via ultra-accurate
displacement measurements.
No
M
GG study by ASI
CV 2015-2025 Proposals received
Mission Outline
Class Heritage
A near-infrared surveyor dedicated to an all-sky, spectroscopic survey of a large
number of galaxies, aiming to obtain information on the evolution of galaxies in
the universe.
M
? WFI, JWST
A space mission aimed at detecting the primordial gravitational waves generated
during the universe inflation by detecting the B-polarisation of the Cosmic
Microwave Background.
M
CMPM-TRS
(CNES SAMPAN,
COFIS)
European contribution to the Russian Millimetron mission dedicated to the
investigation of the universe in sub-millimeter and far-infrared, with extremely high
spatial resolution.
M
no
(FIRI, Herschel,
Planck)
Space based, high angular resolution, near-UV, visible and near IR interferometer
based on a 2 spacecraft formation and used for the detection of extra-solar
planets as well as of stellar systems and proto-planetary disks.
L
no
(Darwin, JWST)
High resolution soft X-ray and extreme ultraviolet (EUV) spectroscopy mission to
carry out a survey of stellar and galactic environments.
M
NASA SR, WSO?
X-ray and gamma-ray observatory dedicated to investigations on the evolution of
different scale structures, from the early universe to present time, tracing the
history of baryons.
M
No
H2EX is an infrared telescope allowing imaging and spectroscopy and dedicated
to the formation of galaxies, stars and giant planets from molecular hydrogen.
M
Previous H2EX
based on Planck
design
+ additional experts
Fase de viabilidad
• Mostrar para las misiones: valor científico, viabilidad
técnica y que son realistas dentro del programa.
• Se forma un Study Science Team con científicos externos,
incluyendo a los proponentes.
• Se confirman objetivos científicos y requerimientos.
• Definir el perfil de la misión (lanzador, plataforma, órbita,
programa tecnológico y operaciones) y el modelo de
carga útil.
• Definir el escenario de implementación y posibles
cooperaciones.
• Estimación del calendario y costo de la misión
• Duración de unos 2 años.
Programas Tecnológicos
La ESA tiene 3 programas tecnológicos:
• GSTP (opcional para los países)
• TRP (financiado por el presupuesto general)
• CTP (financiado por el programa de ciencia)
GSTP = General Support Technology Programme
TRP = Technology Research Programme
CTP = Core technology Programme
Fase de viabilidad
• Las misiones grandes inician un programa tecnológico
hasta asegurar la necesaria madurez en la que se basa
la selección final.
• Producción de un informe final
• Evaluación de las misiones en Noviembre de 2009
• El SSAC (finalmente el SPC) recomienda dos por clase
para la fase de definición.
Fase de Viabilidad
Evaluate
Proposals
Issue Call for
Proposals
Set up
Peer Review
SSAC
approval
Select missions
for assessment
Definition
Phase
Select Mission
for Definition
Noviembre de 2009
Assessment
Studies
Fase de definición
• 2 estudios industriales paralelos iniciados para la
definición de cada misión
• La industria incorpora los desarrollos tecnológicos (en
marcha o planificados) en el diseño del sistema.
• Selección de la carga útil a través de un Announcement of
Opportunity.
• Al final de la fase de definición, se acuerdan las interfaces
con la carga útil (PI) y se hacen propuestas vinculantes
para la fase de implementación en respuesta a una ITT
• Esta fase dura generalmente unos 3 años pero se
propone de sólo 2
• El Study Science Team, para vigilar los objetivos
científicos, pasa a un Science Working Team.
Fase de definición
Carga útil:
• Se aprueba el Science Management Plan (SMP) por el
SPC definiendo las responsabilidades de los que
respondan al AO de la carga útil
• Se hace un Announcement of Opportunity (AO) para
seleccionar la carga útil científica
• Las propuestas se someten a peer review siguiendo tres
criterios:
• Calidad científica
• Viabilidad y madurez tecnológica
• Plan de gestión y financiero
• Los resultados son apoyados en su caso por el SPC y
confirmados por las agencias financiadoras.
Fase de definición
Carga útil:
• En el nuevo plan se propone mantener el desarrollo de
cargas útiles, con fondos nacionales, para dos misiones
en paralelo.
• Los PIs acuerdan con la ESA y la industria el programa
de entrega de instrumentos (a través de acuerdos EID)
• También se seleccionan mission scientists, o
multidisciplinary scientists, a la vez que la carga útil.
• Esta prevista la publicación del próximo Announcement of
Opportunity para 2010 !
Fase de definición
Approve
SMP
Issue
Payload AO
Study mission
w model P/L
Select
Payload
Payload
Peer Review
Study mission
w selected P/L
P/L Funding
Commitment
Implementation
Phase
Noviembre de 2011
Select C/D
Contractor
Fase de implementación
• El SPC debe decidir ahora sobre el inicio de la
implementación o no, con:
• Una carga útil seleccionada y comprometida.
• Una ITT publicada para el contratista principal de la plataforma.
• Un CaC evaluado adecuadamente.
• Problemas posibles encontrados en la fase de
definición:
•
•
•
•
•
La ciencia no se cubre adecuadamente.
La carga útil no tiene la financiación necesaria.
El CaC necesario es mayor que lo inicialmente previsto.
Existen retrasos graves e inevitables.
Algunas cargas útiles tienen que ser conseguidas directamente
por la ESA con la industria o se tiene que formar un consorcio
no competitivo.
Fase de implementación
• Solo una de las misiones en definición pasa a
implementación.
• El comienzo de esta fase implica “no retorno”.
• Hay un contratista principal seleccionado entre los
involucrados en la fase de definición.
• La duración de esta fase es de unos 5 años.
Fase de implementación
• Las operaciones científicas se definen mediante un
Science Implementation Requirements Document
(SIRD) y su respuesta como Science Implementation
Plan (SIP).
• Los PIs dedican la mayor parte del tiempo al desarrollo
de su contribución a la carga útil (con todos los
problemas clásicos de financiación, ESA, industria, etc.)
Fase de explotación
• Para las nuevas misiones se estima el inicio a mediados
de 2017 (M) o el otoño de 2018 (L)
• En el caso de misiones tipo observatorio se publican
nuevos Announcement of Oportunity para la distribución
de tiempo de observación.
Resumen
• El diseño de instrumentos científicos es una etapa necesaria
después de haber demostrado ser buenos usuarios.
• La mejor ciencia requiere nuevas tecnologías y no una
simple repetición, es decir, innovación.
• Hacer instrumentos es enormemente gratificante.
• Hay que ser consciente que el numero de papers disminuye.
• Trabajar con ingenieros es también una gran experiencia. El
intercambio de conocimientos y culturas enriquece a ambos.
• La interacción de culturas diferentes exige procedimientos
sólidos y documentación detallada.
• El traspaso de ideas a otros campos es posible con
programas de instrumentación