Astronomical Observing Techniques Lecture 3: Eyes to the Skies
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1 Astronomical Observing Techniques Lecture 3: Eyes to the Skies Christoph U. Keller
2 Outline 1. Poin8ng Telescopes on Earth 2. Space Telescope Orbits 3. Op8cal Telescopes 4. Radio Telescopes, Interferometers 5. X-ray and Gamma-Ray Telescopes 6. Neutrino Telescopes 7. Gravita8onal Wave Telescopes Astronomical Observing Techniques 2016: Telescopes 2
3 Early Telescopes Hans Lipperhey 1608: spy glasses Galileo Galilei 1609: first use in astronomy Kepler 1611: improved refractor Newton 1668: first reflector Herschel 1789: 1.22-m diameter, 12-m long Astronomical Observing Techniques 2016: Telescopes 3
4 Telescope Mounts Equatorial mount Azimuthal mount + single moving axis + constant rota8on + no image rota8on - large, heavy - instruments: varying gravity + light and symmetric + fixed gravity on bearings + two fixed-gravity ports - two moving axes - image rota8on Astronomical Observing Techniques 2016: Telescopes 4
5 CTIO 4-m, WIYN 3.5-m Astronomical Observing Techniques 2016: Telescopes 5
6 Azimuthal Telescope Mounts SALT VLT Astronomical Observing Techniques 2016: Telescopes 6
7 Space Telescope Orbits Orbits - low Earth - sun-synchronous - geosta8onary - Earth-trailing - L2 Orbit choice influenced by - communica8ons - thermal background radia8on - space weather - sky coverage - access (servicing) HST : low Earth orbit ~96 minutes Spitzer: Earth-trailing solar orbit ~60 yr Astronomical Observing Techniques 2016: Telescopes 7
8 Lagrangian Points map.gsfc.nasa.gov/mission/observatory_l2.html Astronomical Observing Techniques 2016: Telescopes 8
9 L2 JWST, WMAP, GAIA, Herschel in orbits around L2 + sun-shields - orbit around L2 - radia8on Astronomical Observing Techniques 2016: Telescopes 9
10 Telescope Scale: l tanω = and for smallω : l ωf f Magnifica8on: V = f f 1 2 = D D 1 2 = ω2 ω Astronomical Observing Techniques 2016: Telescopes 10
11 Hollandsche Kijker entrance pupil f1 f2 magnifica8on = f1/f2 limitations: field, chromatic aberrations Astronomical Observing Techniques 2016: Telescopes 11
12 Kepler Refractor larger FOV image upside down f1 f2 magnifica8on = f1/f Astronomical Observing Techniques 2016: Telescopes 12
13 Spherical Lenses Spherical Aberration: Beams away from center have shorter focal lengths Astronomical Observing Techniques 2016: Telescopes 13
14 Spherical Mirrors provide large field of view (FoV) rays more distant from op8cal axis have a different focal point Astronomical Observing Techniques 2016: Telescopes 14
15 Parabolic Mirrors Parabolic primary mirrors focus all rays from the same direc8on to one point. But: different direc8ons have different focal points. v à Field of view limited by aberra8ons: the bigger the mirror the bigger the difference [parabola sphere] near the edge à bigger telescopes have smaller FOVs (~<1 deg) Astronomical Observing Techniques 2016: Telescopes 15
16 Schmidt Telescope Idea: 1. Use spherical primary mirror for maximum field of view (>5 deg) à no offaxis asymmetry but spherical aberra8ons 2. correct spherical aberra8ons with corrector lens. Two meter Alfred-Jensch- Telescope in Tautenburg, the largest Schmidt camera in the world Astronomical Observing Techniques 2016: Telescopes 16
17 Two-Mirror Telescopes Newtonian Cassegrain Gregorian Three Mirror Anastigmat (TMA) Astronomical Observing Techniques 2016: Telescopes 17
18 Modifica8on of Cassegrain configura8on (parabolic primary, ellip8cal secondary): Hyperbolic primary mirror (almost parabola) and hyperbolic secondary mirror eliminates (some) op8cal errors (3 rd order coma and spherical aberra8on). à large field of view & compact design (for a given focal length) Astronomical Observing Techniques 2016: Telescopes 18
19 Ritchey-Chrétien Telescopes VLT (4x) GTC Subaru Keck (2x) Gemini (2x) Astronomical Observing Techniques 2016: Telescopes 19
20 Ritchey-Chrétien Telescope HST Astronomical Observing Techniques 2016: Telescopes 20
21 TMA Wide-Field Telescope Large Synoptic Survey Telescope (LSST) Astronomical Observing Techniques 2016: Telescopes 21
22 Light Gathering Power and Light gathering power For extended objects: D S / N f (see lecture on S/N) For point sources: 2 S / N D 2 Angular resolu8on (given by the Rayleigh criterion) λ sin Θ = 1.22 or Δl = 1.22 D fλ D Astronomical Observing Techniques 2016: Telescopes 22
23 Telescope Foci where to put the instruments Prime focus wide field, fast beam but difficult to access and not suitable for heavy instruments Cassegrain focus moves with telescopes, small field Astronomical Observing Techniques 2016: Telescopes 23
24 Telescope Foci where to put instruments (2) Nasmyth ideal for heavy instruments to put on a stable plarorm, but field rotates Coudé very slow beam, usually for large spectrographs in the basement Astronomical Observing Techniques 2016: Telescopes 24
25 Growth of Telescope Area λ sin Θ =1.22 D Astronomical Observing Techniques 2016: Telescopes 25
26 Mass bigger mirrors require thinner / segmented mirrors ac8ve support Astronomical Observing Techniques 2016: Telescopes 26
27 Segmented, Thin and Honeycomb Mirrors Astronomical Observing Techniques 2016: Telescopes 27
28 Mirror Support Astronomical Observing Techniques 2016: Telescopes 28
29 Telescopes in Comparison Palomar Keck JWST Telescope aperture 5 m 10 m 6.5 m Telescope mass 600 t 300 t 6.5 t # of segments Segment size 5 m 1.8 m 1.3 m Mass / segment kg 400 kg 20 kg Astronomical Observing Techniques 2016: Telescopes 29
30 Radio Telescopes Dishes similar to optical telescopes but with much lower surface accuracy Arecibo, Puerto Rico the largest (305m) single-aperture telescope Effelsberg, Germany 100m fully steerable telescope Greenbank, USA after structural collapse (now rebuilt) Astronomical Observing Techniques 2016: Telescopes 30
31 Arrays and Interferometers VLA in New Mexico 27 antennae (each 25m) in a Y-shape (up to 36 km baseline) WSRT (Westerbork) in Drenthe 14 antennae along 2.7 km line ALMA in Chile 50 dishes (12m each) at 5000m altitude 400µm 3mm (720 GHz 84GHz)
32 LOFAR in the Netherlands LOw Frequency ARray uses two types Arecibo of lowcost antennae: Low Band Antenna (10-90 MHz) High Band Antenna ( MHz). Antennae are organized in 36 sta8ons over ~100 km. Each sta8on contains 96 LBAs and 48 HBAs Baselines: 100m 1500km Main LOFAR subsystems: sensor fields wide area networks central processing systems user interfaces
33 X-ray Telescopes X-rays impinging perpendicular on any material are largely absorbed rather than reflected telescope op8cs based on glancing angle reflec8on (rather than refrac8on or large angle reflec8on) typical reflec8ng materials for X-ray mirrors are gold and iridium (gold has a cri8cal reflec8on angle of 3.7 deg at 1 kev).
34 Gamma-Ray Telescopes FERMI satellite MAGIC Cerenkov telescopes Fig. 1 in arxiv.org/pdf/ v1.pdf magic.mpp.mpg.de/newcomers/introduction/ Astronomical Observing Techniques 2016: Telescopes 34
35 RHESSI Gamma-Ray hesperia.gsfc.nasa.gov/rhessi3/ mission Astronomical Observing Techniques 2016: Telescopes 35
36 Neutrino Telescopes neutrino.kek.jp/figures.html images Super-Kamiokande, 50,000 tons of water Sudbury Neutrino Observatory, 1000 tons of D 2 O Astronomical Observing Techniques 2016: Telescopes 36
37 Neutrino scaxering of neutrinos on electrons: e - + ν e è e - + ν e electron accelerated to v > c è Cerenkov radia8on solar neutrinos neutrino oscilla8ons neutrinos from SN1987A Astronomical Observing Techniques 2016: Telescopes 37
38 Neutrinos in Ice and Water gallery.icecube.wisc.edu antares.in2p3.fr/gallery IceCube at the South Pole ANTARES in Mediterranean Sea Astronomical Observing Techniques 2016: Telescopes 38
39 Wave Detectors ligo.org/multimedia/gallery Astronomical Observing Techniques 2016: Telescopes 39
40 GW Measurement Principle ligo.org/science/gw-overview/images/ifo.jpg Astronomical Observing Techniques 2016: Telescopes 40
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