Innovación tecnológica en la Agencia Espacial Europea

Presentación del tema: "Innovación tecnológica en la Agencia Espacial Europea"— Transcripción de la presentación:

1 Innovación tecnológica en la Agencia Espacial Europea

2 Centros de la ESA HEADQUARTERS - Paris, France
ESA headquarters houses the Director General’s office, general administration and the main programme directorates. (including Brussels, Kourou liaison, Moscow, Toulouse, Washington and Houston offices). ~500 people ESTEC - Noordwijk, the Netherlands European Space Research & Technology Centre Staff EAC - Cologne, Germany European Astronaut Centre Staff - 60 ESAC - Villafranca del Castillo, Spain Satellite Tracking Station ~120 people ESOC - Darmstadt, Germany European Space Operations Centre Staff - 600 ESRIN - Frascati, Italy European Space Research Institute Staff - 400

3 Lisboa 2000: Hacer de Europea la economia y la sociedad basada en conocimiento mas avanzada del mundo

4 Por que Europa tiene que invertir en tecnologia espacial
1. el desafio de independencia 2. el deasfio del control del planeta 3. el desafio del mas alla Como no podemos ser mas baratos que China o India, tenemos que ser mejores: mejor tecnologia

5 XMM-Newton

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7 Grazing incidence optics

8 Large fast X-ray CCDs

9 XMM-Newton operations
Data Processing Leicester, UK Processed Data Raw Data Spacecraft Operations ESOC, Germany Mission Planning Science Operations ESAC, Spain Command Preparation Instrument Monitoring Instrument Calibration Data Archiving Data Distribution Community Support Processed Data Mission Planning Raw Data Raw Data Satellite Tracking Perth, Australia Kourou, French Guyana Telemetry XMM-Newton TeleCommands

10 ESAC activities Created in 1978 Satellite tracking station
Science Operations Centre Science archive centre and science data distribution centre Created in 1978 25 years of expérience Operations of satellites IUE, ISO, XMM-Newton Support to other missions

11 ESAC

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13 Cebreros

14 Cebreros

15 Por que la Astronomia ? Parte de nuestra cultura
Curiosidad natural del Hombre Ciencia de las condiciones extremas Exploracion del Espacio Voluntad de entender el universo que nos rodea Contribuir a una mejor comprension de nuestro medio ambiante y su fragilidad Nos da conciencia de la casualidad extraordinaria de la vida sobre la tierra

16 Ground-based Astronomy

17 Por que astronomia espacial ?

18 XMM-Newton: primera luz

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20 Las inversiones de hoy son las ganancias de mañana y los empleos de pasado mañana Helmut Schmidt

21 Simbol-X

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23 Corot lanzamiento: dec. 2006

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25 Infrared ‘light’ – what is it?
Infrared ‘light’ – why?

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27 M16 – the ‘Eagle Nebula’

28 The Cool Universe Herschel spectral coverage Herschel emphasis
black-bodies 5-50 K continuum radiation dust grains (re-)radiating gases 10-few100 K brightest atomic/molecular lines Herschel emphasis formation and evolution of galaxies & stars ISM physics & chemistry solar system bodies Herschel strengths covers ISM SED peaks wide area mapping spectral scans, water lines

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30 SPIRE & PACS extragalactic survey(s)
100 sq.deg. to confusion limit Multi-l survey near peak of SED => Lbol & phot z SPIRE confusion limit is ~15-20 mJy Cover 1 sq.deg. in 2-4 days PACS can provide additional colours and higher resolution and follow-up for brighter sources SPIRE FTS => SED PACS line diagnostics possibly HIFI C+ MRR model 1300/660/320 sources/sq.deg.

31 FIR bridges the submm-NIR/optical gap
STOP PRESS !! Spitzer results: 24 μm – 70% 70 μm – 23% 160 μm – 7%

32 Galactic star formation
0.1Lsun protostar at 300 pc =>>

33 Galactic survey

34 Star formation & evolution
Solar System: Water in Giant Planets Atmospheric chemistry Water activity and composition of comets ISM in Galaxies: Normal galaxies Physical properties of star-forming ISM Dense cores and star-formation: Temperature, density structure Dust properties Stellar IMF ISM in the Milky Way: Structure Dynamics (pressure) Composition (gradients) Late stages of stellar evolution: Winds Shells Asymmetries Composition

35 14.5”

36 HIFI spectral line surveys
Spectral survey of Orion-KL showing hundreds of molecular lines with atmospheric transmission overlaid. HIFI will be able to survey outside of the atmospheric windows and at frequencies never probed before, allowing for searches of new molecules. CSO Spectrum of Orion: 8 nights HIFI: expected less than 1 hour Total HIFI range in 12 hours

37 Chemistry - also diagnostic tool
14.5” Ph.D. Thesis, Boonman (2003)

38 HIFI water line observations
Observations by ISO and SWAS/Odin have shown: Water is present in a variety of objects all over the Galaxy. The high resolving power, high sensitivity and large frequency coverage of HIFI, combined with Herschel’s smaller beam ‘will extend our knowledge by orders of magnitude’

39 Herschel Main Scientific Objectives
Formation and evolution of galaxies and structure – Star formation history of the Universe – History of element production – Understanding the Cosmic Infrared Background – Formation of galaxies Formation of stars; physics and chemistry of the interstellar medium – Structure, dynamics, composition of the ISM – Pre-stellar cores to young stellar systems – Circulation/enrichment of the interstellar medium - astrochemistry – Detailed studies of nearby resolvable galaxies Cometary, planetary, and satellite atmospheres – Composition of giant planets – Pristine material in comets – Water activity