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![Page 1: Spectrographs. Literature: Astronomical Optics, Daniel Schroeder Astronomical Observations, Gordon Walker Stellar Photospheres, David Gray.](https://reader035.fdocuments.in/reader035/viewer/2022062301/56649ece5503460f94bdb7f6/html5/thumbnails/1.jpg)
Spectrographs
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Literature:
Astronomical Optics, Daniel Schroeder
Astronomical Observations, Gordon Walker
Stellar Photospheres, David Gray
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Spectral Resolution
d
1 2
Consider two monochromatic beams
They will just be resolved when they have a wavelength separation of d
Resolving power:
d = full width of half maximum of calibration lamp emission lines
R = d
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R = 15.000
= 0.73 Å
R = 100.000
= 0.11 Å
R = 500.000
= 0.022 Å
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Spectral Resolution
The resolution depends on the science:
1. Active Galaxies, Quasars, high redshift (faint) objects:
R = 500 – 1000
2. Supernova explosions:
Expansion velocities of ~ 3000 km/s
d/ = v/c = 3000/3x105 = 0.01
R > 100
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R = 3.000
R = 30.000
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35.0000.160100000
60.0000.09130000
100.0000.05310000
140.0000.046000
200.0000.0283000
Rth (Ang)T (K)
3. Thermal Broadening of Spectral lines:
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3000001K
1000003G0
1200025F5
375080F0
2000150A0
R1Vsini (km/s)Sp. T.
4. Rotational Broadening:
1 2 pixel resolution, no other broadening
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5. Chemical Abundances:
Hot Stars: R = 30.000
Cool Stars: R = 60.000 – 100.000
Driven by the need to resolve spectral lines and blends, and to accurately set the continuum.
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6 Isotopic shifts:
Example:
Li7 : 6707.76
Li6 : 6707.92
R> 200.000
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7 Line shapes (pulsations, spots, convection):
R=100.000 –200.000
Driven by the need to detect subtle distortions in the spectral line profiles.
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Line shapes due to Convection
Hot rising cell
Cool sinking lane
•The integrated line profile is distorted.
• Amplitude of distortions ≈ 10s m/s
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R = 200.000
R > 500.000
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8 Stellar Radial Velocities:
RV(m/s) ~ R–3/2 ()–1/2 wavelength coverage
R (m/s)100 000 1 60 000 3 30 000 7 10 000 40 1 000 1200
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collimator
Spectrographs
slit
camera
detector
corrector
From telescope
Anamorphic magnification:
d1 = collimator diameter
d2 = mirror diameter
r = d1/d2
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slit
camera
detector
correctorFrom telescope
collimator
Without the grating a spectograph is just an imaging camera
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A spectrograph is just a camera which produces an image of the slit at the detector. The dispersing element produces images as a function of wavelength
without disperser
without disperser
with disperser
with disperser
slit
fiber
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Spectrographs are characterized by their angular dispersion
d
d
Dispersing element
ddA =
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f
dl
dd
dld = f
In collimated light
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S
dd
dld = S
In a convergent beam
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Plate Factor
P = ( f A)–1
= ( f )–1
dd
P = ( f A)–1
= (S )–1
dd
P is in Angstroms/mm
P x CCD pixel size = Ang/pixel
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w
h
f1
d1
A
D
f
d2
w´
h´
D = Diameter of telescope
d1 = Diameter of collimator
d2 = Diameter of camera
f = Focal length of telescope
f1 = Focal length of collimator
f2 = Focal length of camera
A = Dispersing element
f2
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w
h
f1
d1
A
D
d2
f
w´
h´
f2
w = slit width
h = slit height
Entrance slit subtends an
angle and ´on the sky:= w/f
´= h/f
Entrance slit subtends an angle
and ´on the collimator:= w/f1
´= h/f1
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w´ = rw(f2/f1) = rDF2
h´ = h(f2/f1) = ´DF2
F2 = f2/d1r = anamorphic magnification due to dispersing element = d1/d2
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w´ = rw(f2/f1) = rDF2
This expression is important for matching slit to detector:2 = rDF2 for Nyquist sampling (2 pixel projection of slit).1 CCD pixel () typically 15 – 20 m
Example 1:
= 1 arcsec, D = 2m, = 15m => rF2 = 3.1
Example 2:
= 1 arcsec, D = 4m, = 15m => rF2 = 1.5
Example 3:
= 0.5 arcsec, D = 10m, = 15m => rF2 = 1.2
Example 4:
= 0.1 arcsec, D = 100m, = 15m => rF2 = 0.6
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5000 A
4000 An = –1
5000 A
4000 An = –2
4000 A
5000 An = 2
4000 A
5000 An = 1
Most of light is in n=0
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b
The Grating Equation
m = sin + sin b 1/ = grooves/mm
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dd =
m cos =
sin + sin cos
Angular Dispersion:
Linear Dispersion:
ddx
dd=
ddx
=1fcam
1
d/d
dx = fcam d
Angstroms/mm
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Resolving Power:
w´ = rw(f2/f1) = rDF2
dx = f2 dd
f2 dd
rDF2
R = /d = Ar
1
d1
D
=rA
D
d1
For a given telescope depends only on collimator diameter
Recall: F2 = f2/d1
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D(m) (arcsec) d1 (cm)
2 1 10
4 1 20
10 1 52
10 0.5 26
30 0.5 77
30 0.25 38
R = 100.000 A = 1.7 x 10–3
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Adaptive Optics corrects for the atmospheric motion and allows one to achieve near
diffraction limit
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What if adaptive optics can get us to the diffraction limit?
Slit width is set by the diffraction limit:
=
D
R = r
A D
d1
D=
Ar
d1
R d1
100000 0.6 cm
1000000 5.8 cm
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For Peak efficiency the F-ratio (Focal Length / Diameter) of the telescope/collimator should be the same
collimator
1/F 1/F1
F1 = F
F1 > F
1/f is often called the numerical aperture NA
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F1 < F
d/
1
But R ~ d1/
d1 smaller => must be smaller
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Normal gratings:
• ruling 600-1200 grooves/mm
• Used at low blaze angle (~10-20 degrees)
• orders m=1-3
Echelle gratings:
• ruling 32-80 grooves/mm
• Used at high blaze angle (~65 degrees)
• orders m=50-120
Both satisfy grating equation for = 5000 A
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Grating normal
Relation between blaze angle , grating normal, and angles of incidence and diffraction
Littrow configuration:
= 0, = =
m = 2 sin
A = 2 sin
R = 2d1 tan D
A increases for increasing blaze angle
R2 echelle, tan = 2, = 63.4○
R4 echelle tan = 4, = 76○
At blaze peak + = 2
mb = 2 sin cos
b = blaze wavelength
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3000
m=3
5000
m=2
4000 9000
m=1
6000 14000Schematic: orders separated in the vertical direction for clarity
1200 gr/mm grating
2
1
You want to observe 1 in order m=1, but light 2 at order m=2, where 1 ≠ 2 contaminates your spectra
Order blocking filters must be used
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4000
m=99
m=100
m=101 5000
5000 9000
9000 14000
Schematic: orders separated in the vertical direction for clarity
79 gr/mm grating
30002000
Need interference filters but why throw away light?
In reality:
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collimator
Spectrographs
slit
camera
detector
corrector
From telescope
Cross disperser
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y ∞ 2
y
m-2
m-1
m
m+2
m+3
Free Spectral Range m
Grating cross-dispersed echelle spectrographs
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Prism cross-dispersed echelle spectrographs
y ∞ –1
y
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Cross dispersion
y ∞ · –1 =
Increasing wavelength
grating
prism
grism
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Cross dispersing elements: Pros and Cons
Prisms:
Pros:
• Good order spacing in blue
• Well packed orders (good use of CCD area)
• Efficient
• Good for 2-4 m telescopes
Cons:
• Poor order spacing in red
• Order crowding
• Need lots of prisms for large telescopes
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Cross dispersing elements: Pros and Cons
Grating:
Pros:
• Good order spacing in red
• Only choice for high resolution spectrographs on large (8m) telescopes
Cons:
• Lower efficiency than prisms (60-80%)
• Inefficient packing of orders
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Cross dispersing elements: Pros and Cons
Grisms:
Pros:
• Good spacing of orders from red to blue
Cons:
• Low efficiency (40%)
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Important Data reduction issues:
1. Blaze function
2. Scattered Light
3. Reflections
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• „Picket Fence“ or reflected light for Littrow configuration
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Spectrum of a White Light Source (Flat Lamp)
Picket fence:
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Scattered light
Scattered light is light that is scattered into the interorder spacing of echelle spectrographs. All instruments have scattered light at some level or another. This must be removed in the reduction process. Why?
A cross section across rows of the spectrum of the white light source
Bias level of CCD
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To determine the abundance of an element in the stellar spectrum you need to measure the equivalent width
w
Id
Ic
w =Ic – I
Ic
d∫
w
Id + Is
Ic + Is
Is
w =Ic + Is – (I +Is)
Ic + Is
w =Ic – I Ic + Is
Scattered light reduces equivalent width
∫
∫
d
d
Width of a perfectly black line of rectangular profile that would remove the same amount of flux
I
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So you want to build a spectrograph: things to consider
• Chose R product– R is determined by the science you want to do– is determined by your site (i.e. seeing)
If you want high resolution you will need a narrow slit, at a bad site this results in light losses
Major consideration: Costs, the higher R, the more expensive
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normal
Do I need to tilt the grating to make it fit in my room?
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• Reflective or Refractive Camera? Is it fed with a fiber optic?
Camera pupil is image of telescope mirror. For reflective camera:
Image of Cassegrain hole of Telescope
camera
detector
slit
Camera hole
Iumination pattern
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• Reflective or Refractive Camera? Is it fed with a fiber optic?
Camera pupil is image of telescope mirror. For reflective camera:
Image of Cassegrain hole
camera
detector
A fiber scrambles the telescope pupil
Camera hole
ilIumination pattern
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Cross-cut of illumination pattern
For fiber fed spectrograph a refractive camera is the only intelligent option
fiber
e.g. HRS Spectrograph on HET:
Mirror camera: 60.000 USD
Lens camera (choice): 1.000.000 USD
Reason: many elements (due to color terms), anti reflection coatings, etc.
Lost light due to hole in mirror
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• Stability: Mechanical and Thermal?
HARPS
HARPS: 2.000.000 Euros
Conventional: 500.000 Euros
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Tricks to improve efficiency:Overfill the Echelle
d1
d1
R ~ d1/
w´ ~ /d1
For the same resolution you can increase the slit width and increase efficiency by 10-20%
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Atmospheric Seeing Blurs the Image on Slit
slit
Lost light
R = /d = Ar
1
d1
D
But…
You catch more photons, but a wider slit means lower resolution
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Need to turn this
Into this
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Tricks to improve efficiency:Image slicing
The slit or fiber is often smaller than the seeing disk:
Image slicers reformat a circular image into a line
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A modern Image slicer
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Fourier Transform Spectrometer
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Interferogram of a monchromatic source:
I() = B()cos(2n)
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Interferogram of a two frequency source:
I() = B1()cos(21) + B2(2)cos(22)
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Interferogram of a two frequency source:
I() = Bi(i)cos(2i) = B()cos(2)d–∞
+∞
Inteferogram is just the Fourier transform of the brightness versus frequency, i.e spectrum
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Words of Advice
If it is too good to be true it probably isn‘t
Lessons learned:
1. „The Phosphorus Stars“
2. „The Lithium Stars“
3. „The non-pulsating, pulsating A stars“
„You have to be careful that you do not fool yourself and unfortunately, you are the easiest person to fool“
- Richard Feynman