Observational astrophysics i
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Observational Astrophysics I. Astronomical detectors Kitchin pp. 2-51. Types 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

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Observational Astrophysics I

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Observational astrophysics i

Observational Astrophysics I

Astronomical detectors

Kitchin pp. 2-51


Types of detectors

Types of detectors


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

Common parameters of detectors


Charge coupled device

Light

Serial charge transport

towards ADC

Parallel charge transport

Charge Coupled Device


Readout sequence

Readout sequence


Observational astrophysics i

Continuous flow cryostat


Electron trail

Electron trail


Critical data flow properties

Parallel CTE

Digital signal ADUs

Voltage on shift register

Temperaturecontrol

CCD

Serial CTE

Readoutnoise

+ bias

ADC

Logarithmicamplifier

Analog signal

Critical data flow properties

12 or 16 bits


Quantum efficiency

Quantum Efficiency


Improving spectral range

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.


Dark current

Dark current

At 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


Cooling

Cooling

Peltier cooler: -20°  -60° C

Liquid N2: 125  150 K


Cosmetics

Cosmetics


Fringing

Fringing

λ=650 nm

λ=900 nm


Linearity

Linearity

CCD 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.


Charge transfer efficiency

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).


Ccd noise

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


Flatness

Flatness


Binning

Binning

Example: 44 binning

Readout

Exposure

Step 1

Step 2

Step 3

Step 4


Next time

Next time…

  • Hybrid detectors

  • IR detectors

  • Photon counting detectors

  • Calibrations


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