astro 500mab/education/astro500/lectures/a500... · 2020. 9. 17. · 2.pick up mclean anda basic...
TRANSCRIPT
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Astro 500
A500/L-6
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Find values for WIYN & SALT instr.:
A500/L-6
• Detector gain, read-noise, system efficiency• WIYNØ WHIRCØ Bench SpectrographØ ODIØ NEID• SALTØ SALTCAMØ RSSØ HRS
Assignment: vWork as a teamvTabulate informationvAssess availability, ease of accessvBring to class to present
What did you find?
4A500/L-6
Telescopes & Optics
• Defining the telescope & observatory• Mounts• Foci• Optical designs• Geometric optics• Aberrations
Outline
Conceptually separate
Critical for understanding telescope and instrument capabilities and preliminary instrument design
Essential for detailed instrument design and for evaluating data.
5A500/L-6
Telescopes as Facilities
• The Observatory: far more than telescope
ØOpto-mechanical and thermal controlØAcquisition & guidingØTelemetry and sensingØ Instrumentation and instrument interfaces (ports)ØSoftware for telescope and instrument controlØTechnical support and maintenanceØData storage and transferØSoftware pipelines for data reduction and analysisØEnvironment for observer and operatorØPersonnel management, technical and scientific leadership
6A500/L-6
Telescopes: broader relevance
• Telescopes are examples of optical systems serving as cameras, i.e., producing images from sources at infinity (collimated light).
• Spectrographs and re-imaging systems essentially use variants of these systems as collimators and cameras.
7A500/L-6
Telescopes
• What parameters define telescopes?ØCollecting Area (A)ØFOV (W)Ø Image QualityØCostØThroughputØSpectral rangeØPlate scale/MagnificationØPointing/tracking
highly coupled
We will focus on optical/IR telescopes;Most of this parameter space is relevant for light collection at other wavelengths.
Telescopes as cameras
Telescopes
8A500/L-6
Examples of Telescopes
ØRefractingo Galilean (1609)o Keplerian (1611)
ØReflecting (4x harder to make!)o Newtonian (1672)o Gregorian (1673)o Cassegrain (1668)o Ritchey-Cretien (1927)
ØCatadioptrico Schmidt (1931)o Maksutov (1944)
ØMulti-mirroro MMT (1977)o Keck (1992)o HET (1996), SALT (2005)o all ELT’s (2014+)
Trends to larger collecting area, but more compact in mounting and focal-ratio (speed).
Why?
9A500/L-6Credit: R. Racine
Newton
HerschelParsons
Yerkes
Hale
Galileo
Keck 1&2VLT1-4
ELT’s
SALT
10A500/L-6
Telescope Mounts
Ø Equatorial*o German (Yerkes)o English Yoke or English Crosso Fork (Shane 3m)o Horseshoe (CTIO & KPNO 4m)
Ø Alt-Az (Altitude-Azimuth)o ARC, WIYN, ARC, SOARo Keck, VLT, Subaru, LBT, MMT
MegallanØ Transit
o Arecibo (radio)o LMT - liquid mirror telescope
Ø Transit-Azimutho HET, SALT
Easiest for tracking
Best for flexure, but pointing limitations
Best compromise
Most compact but requires computer control; has field rotation
Cheapest but limited sky coverage (40%)
Cheap and up to 70% sky coverage
First: 1977
3.5-4.5m
6.5-10m
*https://en.wikipedia.org/wiki/Equatorial_mount
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Telescope FociØPrimeØNewtonianØCassegrain
ØFolded CassegrainØNasmythØCoude
What’s the difference?
Where’s prime focus?
12A500/L-6
Types of Telescopes
Category Primary Secondary Corrector Name Principal Aberrations
Singlet lens Spherical refractor spherical + chromatic
Singlet mirror Paraboloid mirror
Newtonian coma + astigmatism
Doublet mirrors Paraboloid Hyperbaloid Cassegrain comaHyperbaloid Hyperbaloid Ritchey-Chertien (RC) astigmatism (twice
Cassegrain field)Parabaloid Ellipsoid Gregorian field curvatureEllipsoid Spherical Dall-KirkhamEllipsoid Ellipsoid Aplonatic Gregorian
(AG)best images but large obstruction
Multiplets Spherical Aspheric lens or achromate doublet
Schmidt v. wide field
Spherical Hyperbaloid Aspheric lens Schmidt-Cassegrain “
Spherical Spherical Spherical meniscus lens
Maksutov “
Spherical 4-mirror asphere HET, SALT Low cost
13A500/L-6
Singlets
14A500/L-6
Doublets*
*with a confusing mixture of labels for telescope types and foci
15A500/L-6
Multiplets: Catadioptrics
Spherical Primary
16A500/L-6
• Trade-offs primarily between cost, desired field of view (at given image-quality) and collecting area.
• Image-quality and field-of-view concern aberrations.• 6 principal aberrations:
Ø ChromaticØ SphericalØ ComaØ AstigmatismØ DistortionØ Field curvature
Why different designs?
Lenses only
The Big 3
Not strictly aberrationsOff-
axis
Rad
ial
17A500/L-6
Optics• Geometric Optics
ØReflectionØRefractionØThin lensØSpherical opticsØConics
ØStopsØPupilsØChief raysØMarginal rayØSystem design
ØTelescope summary
• AberrationsChromaticSphericalComaAstigmatismDistortionField curvature
Whe
re w
e’re
hea
ded
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Reading
• Walker - ok place to start• Schroeder - ferocious, but very rigorous and
remarkably general and complete• McLean - fairly complete, but missing basicsØ Recommend:
1. Start with Walker to get an overview2. Pick up McLean and a basic optics book (e.g.,
Meyer-Arendt, “Introduction to Classical and Modern Optics”) and work out quoted results; return to Walker to reconcile results and nomenclature.
3. Then hit Schroeder’s text running to go to expert level.
A500/L-6
19A500/L-6
Some Everyday Concepts
• Specular and Diffuse Reflection• Refraction
Specular Diffuse
Refraction
20A500/L-6
The Thin Lens
f
f
Object
Image
h’
h
s
s’
€
1f
=1s
+1s'
m =−s's
=h'h
= magnification
f− ratio = f /D, D = clear aperture
€
1f≡ P = optical power
chief ray
focal ray
parallel ray &marginal ray
21A500/L-6
The Thin Lens
f
f€
1f
=1s
+1s'
m =−s's
=h'h
= magnification
f− ratio = f /D, D = clear aperture
Object at ∞
D
22A500/L-6
Spherical OpticsFocal Length Defined
f
Object at Infinity
€
1f
=1s
+1s'
=2R
Rs2
'1=
fs1
'1=
DefinitionC
R
s s’
f = R/2 is referred to as the paraxial focal-length
23A500/L-6
Snell’s Law
Index = n
Index = n’
q’q P
Q
n and n’ depend on l
€
1V
= (nF − nC ) /(nD −1)
= dispersive power
F,D,C: solar-spectrum Fraunhofer lines (486, 589, 656 nm).V vs n is called a glass table.
B
C
Fermat’s principle: least time
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An Aside: Implications of Snell’s Law
qa
z
d
Impact of wedges and and plane parallel plates on an optical beam
n n n
q
q’
€
α ≈ (n −1)θ
€
z ≈ (n −1)tn
€
d ≈ t sinθ 1− cosθncosθ '
%
& '
(
) *
t
If beam is converging, astigmatism introduced. Can be eliminated with wedge.
A500/L-6
25A500/L-6
The Thick Lens
f1Object
h
s
€
n2
f2
=n2 − n1
R= refractive power
f2 /n2 = reduced focal lengthR = radius of curvature
chief ray
focal ray
parallel ray &marginal ray
n1
f2
n2
Image
h’
s’
26A500/L-6
Optical Power, P
Two surfaces• separation d• index n
€
P ≡ 1f
= P1 + P2 −dnP1P2
R1
R2
n
Two-surface spherical lens in air or vacuum• R1, R2 radii of curvature• R>0: center of curvature behind lens
f
€
P =1f
= (n −1) 1R1
−1R2
+d(n −1)nR1R2
#
$ %
&
' (
units : dioptor (m−1)
Lensmaker’s formula: