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Next Generation Extremely Large Telescopes

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Presentation on theme: "Next Generation Extremely Large Telescopes"— Presentation transcript:

1 Next Generation Extremely Large Telescopes

2 Outline What are we looking for? Telescope types
Telescope style Mirror types Size comparison – Existing vs New New Ground Based Telescopes Electromagnetic Spectrum New Space Based Telescopes

3 What are we looking for? More distant and fainter objects:
discover new stars, galaxies, black holes, exoplanets first objects to emit light in the Universe Investigate dark energy and dark matter Determine if there is life elsewhere in the galaxy identify potentially habitable planets Measure quasars, pulsars, gravitational waves Mapping small objects in the solar system near-Earth asteroids, Kuiper belt objects Detecting transient optical events novae and supernovae

4 What are the objects? Stars, starlike objects Galaxies
Pulsars – Pulsing stars Quasars – Quasi Stellar radio sources novae and supernovae – exploding stars Galaxies Exoplanets – planets around other stars Invisible items – don’t emit light Black holes – location of intense gravity Dark Energy Dark Matter Gravitational waves

5 How do we find them? Images of objects Object motion
Effect on motion or image of nearby matter (other objects) Exoplanets – transit and movement of star Dark energy – expansion of universe dark matter – attraction of objects

6 Extremely Large Telescopes
Why is “bigger”/larger is better? Greater resolving power see more detail More light gathering power See dimmer objects Space based vs Ground based No atmospheric interference Adaptive Optics Removes effects of atmospheric distortion Adaptive Optics Corrects the distortions of an incoming wavefront by measuring the distortions and deforming a mirror in order to compensate for the distortion

7 Resolution Low resolution High resolution

8 Telescope Styles Refracting Reflecting Multiple Mirror Lenses Mirrors
Aberration Correction

9 Refracting telescope:
Objective lens

10 Cassegrain Reflecting telescope Ritchey-Cretien Hyperbolic Parabolic
Objective Mirror Hyperbolic Secondary Mirror Ritchey-Cretien

11 Multiple Mirror Telescopes
Aberration any disturbance of the rays of a pencil of light such that they can no longer be brought to a sharp focus or form a clear image. A telescope with only 1 curved mirror will always have aberrations Spherical aberration Coma Astigmatism Aberration correction Multiple mirrors Mirror Shapes Parabolic hyperbolic

12 Spherical Aberration How a spherical mirror creates spherical aberration A parabolic mirror focus all light to a single point

13 Coma Aberration Stars in the center of the field are not affected by coma, but the effect grows stronger toward the edge of the field.  Stars affected by pure coma are shaped like little comets (hence the name) pointed toward the center of the field.  Spot diagram of a star at the edge of the field affected by coma

14 Astigmatism Spot diagram of a star at the edge of the field affected by astigmatism Two distinct focal surfaces exist in the presence of astigmatism a Tangential focal surface Sagittal focal surface

15 Gregorian Telescope hyperbolical secondary ellipsoidal primary
Final Focus hyperbolical secondary ellipsoidal primary Two-mirror 3-reflection system. Concave secondary mirror (S) reflects light back to the primary (P), which then forms the final focus through an opening on the secondary. Correction of all three aberrations, spherical, coma and astigmatism The only remaining aberration is relatively strong field curvature.

16 Multiple Mirror Telescopes
parabolic mirrors eliminates spherical aberration from spherical mirror Two curved mirrors - Ritchey–Chrétien telescope eliminates coma Gregorian Eliminates spherical, coma, astigmatism 3 curved mirrors Anastigmat telescope also cancels astigmatism. Korsch Corrects astigmatism and field curvature Larger field of view than one or two mirrors

17 Telescope Styles Gregorian Three-mirror anastigmat Ritchey-Chretien
Giant Magellan Telescope Three-mirror anastigmat European Extremely Large Telescope (EELT) Large Synoptic Survey Telescope (LSST) Ritchey-Chretien Thirty Meter Telescope Korsch James Webb Space Telescope (JWST) Radio Telescope Deformable Fixed primary - FAST

18 Segmented Mirror Telescopes
an array of smaller mirrors designed to act as segments of a single large curved mirror. used as objectives for large reflecting telescopes. mirror segments have to be polished to a precise shape actively aligned by a computer-controlled active optics future large optical telescopes essentially all plan to use segmented mirrors.

19 Existing Large Telescopes
Ground Based

20 Ground Based Telescope Size Comparsion
Human 39.3 m EXISTING NEW

21 Basketball court tennis court New Ground Based Telescopes Existing

22 New Large Ground Based Telescopes
500 M Aperture Spherical Telescope (FAST) 30 Meter Telescope Giant Magellan Telescope European Extremely Large Telescope (EELT) Large Synoptic Survey Telescope (LSST)

23 Electromagnetic Spectrum
Interstellar Communication 10 GHz 1 GHz FAST telescope microwave GHz MHz Radio astronomy Study of celestial objects at radio frequencies FAST telescope - 70 MHz – 3 GHz Interstellar communication (1 GHz to 10 GHz) radiation coming from the Milky Way stars and galaxies radio galaxies, quasars, pulsars Cosmic microwave background radiation

24 Electromagnetic Spectrum
wavelength Larger diameter Telescope diameter for same resolving power smaller diameter

25 Five Hundred Meter Aperture Spherical Telescope FAST China – Sept 25, 2016

26 Five Hundred Meter Aperture Spherical Telescope FAST
Features Single dish - Can shift its 4450 reflectors for pointing and focusing Collecting area – almost 450 basketball courts – world’s largest Type – Deformable Fixed primary Radio telescope - 70 MHz to 3.0 GHz Potential to search for more strange objects to better understand the origin of the universe boost the global hunt for extraterrestrial life 169% larger than next largest – Arecibo Twice as sensitive

27 Ground Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective FAST 500 M Aperture Spherical Telescope Sept 25, 2016 China 500 meters (30 soccer fields) radio See below An astrophysical maser is a naturally occurring source of stimulated spectral line emission, typically in the microwave portion of the electromagnetic spectrum. This emission may arise in molecular clouds, comets, planetary atmospheres, stellar atmospheres, or various other conditions in interstellar space.For interstellar communication, a particular range of radio frequencies, “microwaves” from 1 GHz to 10 GHz, are particularly good choices FAST wavelength 10 cm to 4.3 m 70 MHz to 3.0 GHz Objectives quasars pulsars gravitational waves extra-terrestrial life

28 Electromagnetic Spectrum
Hubble Near UV, visible, Near IR James Webb Visible (orange) – Mid IR Infrared astronomy detect objects such as planets view highly red-shifted objects from the early days of the universe caused by expansion of the universe penetrates dusty regions of space such as molecular clouds

29 Galaxy motion vs Electromagnetic Spectrum
Stationary galaxy No shift Receding galaxy Red shift Approaching galaxy Blue shift

30 Planet rotation around star effect on Electromagnetic Spectrum
Blue Shift Red Shift Locates exoplanets that cannot be seen visually

31 Thirty Meter Telescope TMT International Observatory Hawaii ?? - 2022
Consortium: United States, Canada, Japan, China, and India. Alternate Locations: Baja California in Mexico, Canary Islands, Chile, India and China

32 Thirty Meter Telescope Hawaii -?? - 2022

33 Thirty Meter Telescope
Features Telescope style: Ritchey-Chretien 9 x light gathering power of Keck telescope Highest altitude of all proposed Extremely Large Telescopes (ELT’s) Adaptive optics to correct image blur due to earth’s atmosphere Delayed due to islanders

34 Ground Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective 30 Meter Telescope 2022? Hawaii?? Altitude 13,287 ft Blue Canyon 4695 ft 30 meters 492 segmented mirrors Near UltraViolet Visible Mid Infrared See below Objectives More distant and fainter objects exoplanets black holes clues left from early universe

35 Giant Magellan Telescope GMT Consortium Chile 2021 1st light
US-led in partnership with Australia, Brazil, and Korea, with Chile as the host country

36 Giant Magellan Telescope
Features Telescope style - Gregorian Resolving power 10 x Hubble Space Telescope Advanced adaptive optics to correct atmosphere distortion Largest optical observatory in world at first light

37 Ground Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective Notes Giant Magellan 1st light 2021 Completion 2025 Chile Altitude 8225 ft Palomar San Diego 5617 ft m Mirrors Resolving power of 25 meter primary Visible light Near Infrared See below Objectives It should be able to probe the first objects to emit light in the Universe To investigate dark energy and dark matter To identify potentially habitable planets

38 European Extremely Large Telescope (EELT) European Southern Observatory (ESO) Chile – first light 2024

39 European Extremely Large Telescope (EELT)
Features Telescope type Three mirror anastigmat with two flat folding mirrors providing the adaptive optics. Adaptive optics to correct image blur due to earth’s atmosphere Images 16 times sharper than Hubble Will be largest “light” telescope in the world

40 Ground Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective Notes European Extremely Large Telescope 2024 Atacama desert Chile Altitude 10,039 ft 39.3 meters 798 hexagonal segments Visible light Near IR See below Objectives Detailed studies of: planets around other stars, first galaxies in the Universe, super-massive black holes, nature of the Universe’s dark sector, water and organic molecules in protoplanetary disks around other stars

41 Large Synoptic Survey Telescope (LSST) LSST Corporation Chile – first light 2019

42 Large Synoptic Survey Telescope (LSST)
Features Telescope type three-mirror anastigmat Advance in speed – not size Photograph entire sky every 3 nights movies

43 Ground Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective Large Synoptic Survey Telescope (LSST) Chile Altitude 8739 ft James Lick 4209 ft 8.4 m Visible light See below Objectives Measuring weak gravitational lensing in the deep sky to detect signatures of dark energy and dark matter Mapping small objects in the Solar System, particularly near-Earth asteroids and Kuiper belt objects Detecting transient optical events such as novae and supernovae Mapping the Milky Way Our use of the word derives from the greek word “Synopsis” and refers to looking at all aspects of something. The LSST is a synoptic survey in several ways: billions of objects will be imaged in six colors in an unprecedented large volume of our universe. This survey over half the sky also records the time evolution of these sources: the first motion picture of our universe

44 FAST China 30 Meter Telescope Hawaii ?? EELT GIANT MAGELLAN LSST Chile
LSST Cerro Pachón Chile NW coastThe location is exceedingly dry, making it suitable for infrared observations. The air overhead is very stable, yielding excellent seeing. During the summer months, Cerro Pachón is often above the haze layer that can envelop lower altitudes. EELT GIANT MAGELLAN LSST Chile

45 Existing Space Based Telescopes New Space Based Telescopes Hubble
basketball court tennis court

46 Space Telescope Orbit Location
Earth Lagrange points, L-points, or libration points) are positions in an orbital configuration of two large bodies where a small object affected only by gravity can maintain a stable position relative to the two large bodies. Lagrange points, L-points, or libration points) positions in an orbital configuration of two large bodies where a small object affected only by gravity can maintain a stable position relative to the two large bodies.

47 New Large Space Telescopes
James Webb Space Telescope Advanced Technology Larger Aperture Space Telescope (ATLAST) 3. Wide Field Infrared Survey Telescope (WFIRST)

48 James Webb Space Telescope (JWST) NASA Launch – Oct 2018

49 James Webb Space Telescope
Features Type Korsch - Corrects astigmatism and field curvature Unprecedented resolution and sensitivity from : long-wavelength (orange – red) visible light through near-infrared to the mid-infrared 3 X Hubble IR spectrum Aperture 6.5 m vs Hubble 2.4 m Can View high-redshift objects have their visible emissions shifted into the infrared, cold objects such as debris disks and planets emit most strongly in the infrared this band is difficult to study from the ground or by existing space telescopes such as Hubble.

50 Space Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective James Webb Space Telescope Oct 2018 Orbit L2 Lagrange point 6.5m Visible (orange) to Infrared See below Objectives Observing some of the most distant objects in the universe Very first stars Epoch of reionization, formation of the first galaxies Understanding the formation of stars and planets Imaging molecular clouds and star-forming clusters Studying the debris disks around stars Direct imaging of exoplanets Spectroscopic examination of planetary transits

51 Advanced Technology Larger Aperture Space Telescope ATLAST Space Telescope Science Institute Launch – Oct m Telescope

52 The architectures are:
a telescope with a monolithic primary mirror two variations of a telescope with a large segmented primary mirror

53 Advanced Technology Larger Aperture Space Telescope ATLAST
Features 5 – 10 times better resolution than Hubble or James Webb Space Telescope Sensitivity limit 2000 times better than Hubble Hubble Replacement (2.4 m)

54 Space Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective Notes Advanced Technology Larger Aperture Space Telescope (ATLAST) Concept Orbit L2 Lagrange point 3 concepts: 8 m 9.2 m 16.8 UV, Visible Near IR See below Objectives Determine if there is life elsewhere in the galaxy By searching the spectra of terrestrial exoplanets for “biosignatures” molecular oxygen, ozone, water. methane Hubble NearUV , visiblem Near IR 2.4 M

55 Wide-Field Infrared Survey Telescope WFIRST NASA Launch Mid 2020’s

56 Wide-Field Infrared Survey Telescope WFIRST
Features Telescope type -Three-mirror anastigmat Wider FOV than Hubble due to shorter focal length Hubble-quality imaging over an area of sky 100x larger than Hubble Hubble Space Telescope/WFC3/IR PHAT Survey required 432 pointings to cover M31 while only 2 WFIRST pointings are required. NASA repurposed spy telescope HST/WFC3/IR PHAT survey HST Wide Field Camera 3 / Infrared /Panchromatic Hubble Andromeda Treasury

57 Space Based Telescopes Key Characteristics
Operational Location Aperture (ft/m) Signal type (visible, IR, etc Primary objective Notes WFIRST Wide Field Infrared Survey Mid 2020’s Orbit Sun-Earth L2 Lagrange point 2.4m Infrared See below Objectives Settle fundamental questions about the nature of dark energy Could reveal all kinds of new information about the evolution of the universe Discover new exoplanets and entire galaxies Wider FOV than Hubble because of shorter focal length

58 Telescope “First Light” Schedule
Ground Based Space Based Sept Oct Mid FAST James WFIRST Giant Large Meter European ATLAST 500 m Webb Magellan Synoptic Extremely Survey Large LSST EELT FAST – 500 Meter Aperture Spherical Telescope WFIRST – Wide Field Infrared Survey Telescope ATLAST – Advanced Technology Larger Aperture Space Telescope

59 END

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