spectrographs. literature: astronomical optics, daniel schneider astronomical observations, gordon...
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Spectrographs
Literature:
Astronomical Optics, Daniel Schneider
Astronomical Observations, Gordon Walker
Stellar Photospheres, David Gray
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
R = 15.000
R = 100.000
R = 500.000
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
R = 3.000
R = 30.000
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:
3000001K
1000003G0
1200025F5
375080F0
2000150A0
R1Vsini (km/s)Sp. T.
4. Rotational Broadening:
1 2 pixel resolution, no other broadening
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.
6 Isotopic shifts:
Example:
Li7 : 6707.76
Li6 : 6707.92
R> 200.000
7 Line shapes (pulsations, spots, convection):
R=100.000 –200.000
Driven by the need to detect subtle distortions in the spectral line profiles.
Line shapes due to Convection
Hot rising cell
Cool sinking lane
•The integrated line profile is distorted.
• Amplitude of distortions ≈ 10s m/s
R = 200.000
R > 500.000
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
collimator
Spectrographs
slit
camera
detector
corrector
From telescope
Anamorphic magnification:
d1 = collimator diameter
d2 = mirror diameter
r = d1/d2
slit
camera
detector
correctorFrom telescope
collimator
Without the grating a spectograph is just an imaging camera
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
Spectrographs are characterized by their angular dispersion
d
d
Dispersing element
ddA =
f
dl
dd
dld = f
In collimated light
S
dd
dld = S
In a convergent beam
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
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 collimator
A = Dispersing element
f2
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
w´ = rw(f2/f1) = rDF2
h´ = h(f2/f1) = ´DF2
F2 = f2/d1r = anamorphic magnification due to dispersing element = d1/d2
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
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
b
The Grating Equation
m = sin + sin b 1/ = grooves/mm
dd =
m cos =
sin + sin cos
Angular Dispersion:
Linear Dispersion:
ddx
dd=
ddx
=1fcam
1
d/d
dx = fcam d
Angstroms/mm
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
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
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
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
F1 < F
d/
1
But R ~ d1/
d1 smaller => must be smaller
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
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
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
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:
collimator
Spectrographs
slit
camera
detector
corrector
From telescope
Cross disperser
y ∞ 2
y
m-2
m-1
m
m+2
m+3
Free Spectral Range m
Grating cross-dispersed echelle spectrographs
Prism cross-dispersed echelle spectrographs
y ∞ –1
y
Cross dispersion
y ∞ · –1 =
Increasing wavelength
grating
prism
grism
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
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
Cross dispersing elements: Pros and Cons
Grisms:
Pros:
• Good spacing of orders from red to blue
Cons:
• Low efficiency (40%)
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
• Chose and , choice depends on – Efficiency– Space constraints– „Picket Fence“ for Littrow configuration
normal
• White Pupil design? – Efficiency– Costs, you require an extra mirror
Tricks to improve efficiency:White Pupil Spectrograph
echelle
Mirror 1
Mirror 2Cross disperser
slit
slit
• 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
• 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
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
• Stability: Mechanical and Thermal?
HARPS
HARPS: 2.000.000 Euros
Conventional: 500.000 Euros
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%
Tricks to improve efficiency:Immersed gratings
Increases resolution by factor of n
n
Allows the length of the illuminated grating to increase yet keeping d1, d2, small
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
Fourier Transform Spectrometer
Interferogram of a monchromatic source:
I() = B()cos(2n)
Interferogram of a two frequency source:
I() = B1()cos(21) + B2(2)cos(22)
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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