Technology for Telescopes | ESO Deutschland - Eso.org
Seit der Erfindung vor 400 Jahren haben sich astronomische Teleskope von kleinen, manuell auszurichtenden Geräten für visuelle Beobachtungen hin zu großen, ...
Aktiven Optik
Die ESO hat die Technik der <anchor>Aktiven Optik</anchor> entwickelt, die mittlerweile in den meisten modernen Großteleskopen verwendet wird. Die Technik erlaubt die Erhaltung der optimalen Bildqualität durch die Paarung flexibler Spiegel mit Aktuatoren, die aktiv die Spiegelform während Beobachtungen anpassen.
Aktive Optik | ESO Deutschland
Aktive Optik \| ESO Deutschland


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      - [Der VISTA-Spiegel](/public/teles-instr/paranal-observatory/surveytelescopes/vista/mirror/)
      - [VIRCAM](/public/teles-instr/paranal-observatory/surveytelescopes/vista/camera/)
      - [4MOST](/public/teles-instr/paranal-observatory/surveytelescopes/vista/4most/)
      - [Die VISTA-Durchmusterung](/public/teles-instr/paranal-observatory/surveytelescopes/vista/surveys/)
      - [Das VISTA-Konsortium](/public/teles-instr/paranal-observatory/surveytelescopes/vista/consortium/)
    - [VST](/public/teles-instr/paranal-observatory/surveytelescopes/vst/)
      - [The VST mirrors](/public/teles-instr/paranal-observatory/surveytelescopes/vst/mirror/)
      - [OmegaCAM](/public/teles-instr/paranal-observatory/surveytelescopes/vst/camera/)
      - [Die VST-Durchmusterungen](/public/teles-instr/paranal-observatory/surveytelescopes/vst/surveys/)
  - [SPECULOOS](/public/teles-instr/paranal-observatory/speculoos/)
  - [NGTS](/public/teles-instr/paranal-observatory/ngts/)
  - [Cherenkov Telescope Array Observatory](/public/teles-instr/paranal-observatory/ctao/)
- [La Silla Observatory](/public/teles-instr/lasilla/)
  - [Schwedisch–ESO Submillimetre Telescope](/public/teles-instr/lasilla/swedish/)
    - [SIMBA](/public/teles-instr/lasilla/swedish/simba/)
  - [New Technology Telescope](/public/teles-instr/lasilla/ntt/)
    - [EFOSC2](/public/teles-instr/lasilla/ntt/efosc2/)
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    - [SUSI and SUSI2](/public/teles-instr/lasilla/ntt/susi2/)
  - [3,6-Meter-Teleskop der ESO](/public/teles-instr/lasilla/36/)
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# Aktive Optik

## Eine bahnbrechende Erfindung

Es kommt eben doch auf die Größe an, aber auch auf die Form. Beide sind wichtig
für die Konstruktion noch leistungsfähigerer Teleskope. Größere
Hauptspiegel erlauben es den Astronomen, mehr Licht einzufangen, und
einen perfekt geformten Spiegel braucht man, um Verzerrungen zu
vermeiden; die Kombination aus beidem macht es möglich, noch
schwächere Objekte zu beobachten. Leider ist das leichter gesagt
als getan, da es mit zunehmender Spiegelgröße immer schwieriger
wird,  den Spiegel in der perfekten Form zu halten.

Diese Hürde wurde in den sechziger und
siebziger Jahren immer bedeutsamer. Die damalige Technologie erlaubte es Astronomen und
Ingenieuren nicht, Teleskope mit einem Hauptspiegel größer als 5
Meter Durchmesser zu bauen. Darüber hinaus nahm die Bildqualität deutlich
ab, da die Schwerkraft an der Form des Spiegels zerrte. Um mit der
damaligen Technologie Teleskope mit über 5 Metern Durchmesser
zu bauen, hätte man riesige Stützstrukturen für den Spiegel
benötigt, was die Baukosten in die Höhe getrieben und zu einer
untragbar schweren Konstruktion ohne Garantie einer besseren
Bildqualität geführt hätte. Es musste ein neuer Weg gefunden
werden, die optische Genauigkeit zu gewährleisten.

Da hatte der Ingenieur Raymond Wilson von der ESO eine
brilliante und „einfache“ Idee, die man heute als Aktive Optik
bezeichnet. Man müsste einen dünnen und deformierbaren
Hauptspiegel auf ein steuerbares Tragsystem betten, das die jeweils
erforderlichen Korrekturkräfte auf den Spiegel ausübt, um beim
Schwenken des Teleskops die schwerkraftbedingte Verformung
auszugleichen (mehr dazu im kostenlosen Buch [Jewel on the Mountaintop](/public/products/books/book_0050/) von Claus Madsen).

Als das [3,6-Meter\
Teleskop der ESO](http://www.eso.org/public/teles-instr/lasilla/36/) im Jahr 1976 eingeweiht wurde, war die Aktive
Optik noch eine Idee in Wilsons Kopf. Darum ist der Haupspiegel noch
einen halben Meter dick und wiegt unglaubliche 11 Tonnen.

Das neue Konzept wurde zunächst an einem dünnen 1-Meter-Spiegel
mit Aktiver Optik und 75 verstellbaren Stützen in der Nähe der
ESO-Zentrale getestet. Die Stützen sind mit Motoren ausgestattet,
die sehr genau bewegt und sehr präzise gesteuert werden können:
Durch Druck auf den Spiegel korrigieren sie seine Form und
kompensieren die Verformungen durch die Schwerkraft. Wenn das
Teleskop bewegt wird, kann dieses aktive System die korrekte Form des
Spiegels beibehalten. Die Korrekturen durch die Stellmotoren werden
laufend durch einen Computer berechnet, der an einen Bildanalysator
angeschlossen ist, welcher selbst die kleinsten Abweichungen von der
Idealform des Spiegels detektiert. Die Technik der Aktiven Optik
wurde intern bei der ESO entwickelt und wurde nach diesem
erfolgreichen Versuch zu einem der hervorstechenden Merkmale des [New\
Technology Telescope (NTT)](http://www.eso.org/public/teles-instr/lasilla/ntt/). Dank der Aktiven Optik ist der 3,58
Meter große Hauptspiegel des NTT nur 24 Zentimeter dick und wiegt 6
Tonnen.

[![1-metre telescope supports for the active optics experiment at the ESO headquarters in Garching in 1987](http://www.eso.org/public/archives/images/thumb300y/1-m.jpg)](http://www.eso.org/public/images/1-m/)

_Die Stützen für das Experiment mit Aktiver Optik am 1-Meter-Teleskop im ESO-Hauptsitz in Garching im Jahr 1987. Herkunftsnachweis: ESO_

[![The New Technology Telescope (NTT) pioneered the Active Optics.](http://www.eso.org/public/archives/images/thumb300y/esopia00042teles.jpg)](http://www.eso.org/public/images/esopia00042teles/)

_Das New Technology Telescope (NTT) war das erste mit Aktiver Optik._

_Herkunftsnachweis: ESO/C.Madsen. Bacon_

Seit das NTT im Jahre 1990 seinen Betrieb aufnahm, wurde die
Aktive Optik bei fast allen Großteleskopen eingesetzt,
einschließlich des [Very Large\
Telescope (VLT)](http://www.eso.org/paranal/) der ESO. Wilson wurde mit mehreren
Auszeichnungen für seine Erfindung geehrt, die die Astronomie
revolutioniert hat.

Jedes der vier [VLT-Hauptteleskope](http://www.eso.org/public/teles-instr/paranal/)
(engl. Unit Telescopes, kurz UTs) ist mit dem besten System Aktiver Optik
ausgestattet, das bisher gebaut wurde. Das System steuert sowohl den
8,2-Meter-Hauptspiegel aus [Zerodur](http://www.eso.org/public/images/eso9952a/)
als auch den 1,1 Meter großen Sekundärspiegel aus Beryllium am
oberen Ende des Teleskops. Durch die Korrektursignale dieses Systems
werden die Teleskopspiegel automatisch in regelmäßigen Abständen
nachjustiert.

Dank dieser Technik wiegt der Hauptspiegel der vier UTs jeweils 22
Tonnen, bei einem Durchmesser von 8,2 Metern und einer Dicke von nur
17 Zentimetern – die Form eines großen Pfannkuchens. Jeder der
Spiegel ruht auf 150 computergesteuerten Stützen (den
Stellelementen), die in einer äußerst steifen Spiegelzelle mit
einem Gewicht von 11 Tonnen angebracht sind. Das System Aktiver Optik des
VLT garantiert, dass diese großen Spiegel stets die optimale Form
haben und immer erstklassige Bilder des Universums liefern.

[![VLT Active Optics System](http://www.eso.org/public/archives/images/thumb300y/eso9940b.jpg)](http://www.eso.org/public/images/eso9940b/)

_Die Aktive Optik des VLT_

_Herkunftsnachweis: ESO_

[![The prestigious Kavli Prize in Astrophysics for 2010 was awarded to Jerry Nelson, Raymond Wilson and Roger Angel for their contribution to the development of giant telescopes.](http://www.eso.org/public/archives/images/thumb300y/wilson_kavli_2.jpg)](http://www.eso.org/public/images/wilson_kavli_2/)

_Der prestigeträchtige Kavlipreis für Astrophysik wurde im Jahre 2010 an  Jerry Nelson, Raymond Wilson und Roger Angel für ihren Beitrag zur Entwicklung von Großteleskopen verliehen. Herkunftsnachweis: ESO. Bacon_

Jetzt steht der Aktiven Optik die nächste große Herausforderung
bevor, der 39-Meter-Hauptpiegel des geplanten European Extremely
Large Telescope (ELT). Der ELT-Hauptspiegel wird aus 798
einzelnen Segmenten bestehen. Jedes dieser Segmente kann mittels
eines Kolbens und einem Kipp/Schwenkmechanismus bewegt werden, was
dieses Mosaik von Segmenten zu einem einzigen gigantischen Spiegel
machen und sowohl Temperaturschwankungen als auch
Schwerkrafteinflüsse kompensieren wird.

Mehr über die Aktive Optik erfahren Sie in dieser Folge von
ESOcast: [Seeing\
Sharp — Special 50th anniversary episode #3](http://www.eso.org/public/videos/esocast43a/).

### Wissenschaftliche Highlights

Die Aktive Optik an mehreren ESO-Teleskopen hat zu folgenden
herausragenden Entdeckungen beigetragen:

- [VLT und Hubble zeigen, wie große Galaxien von innen nach\
außen sterben](http://www.eso.org/public/news/eso1516/)
- [Die\
Explosion eines Sterns in 3D](http://www.eso.org/public/news/eso1032/)
- [Ein Stern\
umläuft das massereiche Zentrum der Milchstraße in nur 17 Lichtstunden\
Abstand](http://www.eso.org/public/news/eso0226/)

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