Observational Astrophysics I
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Transcript of Observational Astrophysics I
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Observational Astrophysics I
Astronomical detectorsKitchin pp. 2-51
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Types of detectors
Integrating detectors Photon counting detectors (PCD)
Accumulate reaction to incoming radiation over time
React to (almost) every incoming photon and produce digital count
Example: photographic plate, CCD
Example: photomultiplier
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Common parameters of detectors Quantum efficiency
(QE) Spectral response Linearity Gain Dynamic range Saturation level Cosmic ray
sensitivity
Modulation Transfer Function (MTF)
Cosmetics Noise
Shot noise Read-out noise Dark current
Memory Flatness
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Charge Coupled Device
Light
Parallel charge transport
Serial charge transport
towards ADC
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Readout sequence
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Cont
inuo
us fl
ow
cryo
stat
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Electron trail
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Critical data flow properties
12 or 16 bits
CCD
Parallel CTE
Serial C
TE
Logarithmicamplifier
Analog signal
Digital signal ADUs
ADC+ bias
Readout
noise
Tem
pera
ture
cont
rol
Voltage on shift register
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Quantum Efficiency
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Improving spectral range QE drops in the blue because the top layer
is too thick and non-transparent. One way to improve it is the remove extra silicon substrate from the back (thinning) and use this side to detect the light (back-illumination).
QE drops in the red because photons have too low energy. Warming up CCD improves response in the red but also increases the noise.
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Dark currentAt T=270 K DC 10 e-/pixel/s
At T=230 K DC 0.1 e-/pixel/s
At T=170 K DC 10 e-/pixel/hour
At T=120 K DC 1 e-/pixel/hour
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Cooling
Liquid N2: 125 150 K
Peltier cooler: -20° -60° C
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Cosmetics
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Fringingλ=650 nm λ=900 nm
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LinearityCCD full well is the number of electrons which can be stored in one pixel (height of energy barrier between pixels).
Typical values are between 30000 and 1000000 which also where the CCD goes non-linear.
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Charge Transfer Efficiency This is examined by measuring the amplitude
of bright points left by a –ray source. Amplitude dependence in the directionof parallel read gives parallelCTE, while the other directionreflects serial CTE. Good CTEis >0.99999.
The same experimentestablishes the relation betweenADU and number of photoelectrons (gain). Same CCD may use more than one gain (e.g. 1.1 and 9).
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CCD noise Shot noise (Poisson distribution σ
≈√N) Dark current is time, depends on
temperature Readout noise, depends on the
temperature, read speed and amplifier(s) used
Cosmic rays destroycontent of a few pixels
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Flatness
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Binning
Step 1
Step 2
Step 3
Step 4
ReadoutExample: 44 binning
Exposure
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Next time… Hybrid detectors IR detectors Photon counting detectors Calibrations