Innovación tecnológica en la Agencia Espacial Europea

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 - 2000 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

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

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

XMM-Newton

Grazing incidence optics

Large fast X-ray CCDs

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

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

ESAC

Cebreros

Cebreros

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

Ground-based Astronomy

Por que astronomia espacial ?

XMM-Newton: primera luz

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

Simbol-X

Corot lanzamiento: dec. 2006

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

M16 – the ‘Eagle Nebula’

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

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.

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

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

Galactic survey

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

14.5”

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

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

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’

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