basic principles of ccd imaging in astronomy

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Basic Principles of CCD Imaging in Astronomy Based on Slides by Simon Tulloch available from http://www.ing.iac.es/~smt/CCD_Primer/CCD_Primer.htm

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Basic Principles of CCD Imaging in Astronomy. Based on Slides by Simon Tulloch available from http://www.ing.iac.es/~smt/CCD_Primer/CCD_Primer.htm. What is a CCD?. “CCD” = “Charge-Coupled Device” Invented in 1970s, originally for: Memory Devices Arithmetic Processing of Data - PowerPoint PPT Presentation

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Page 1: Basic Principles of CCD Imaging in Astronomy

Basic Principles of CCD Imaging in Astronomy

Based on Slides by Simon Tulloch available from

http://www.ing.iac.es/~smt/CCD_Primer/CCD_Primer.htm

Page 2: Basic Principles of CCD Imaging in Astronomy

• “CCD” = “Charge-Coupled Device”• Invented in 1970s, originally for:

– Memory Devices – Arithmetic Processing of Data

• When Made of Silicon (Si), has same Light-Sensitive Properties as Light Meters– Use them to “Measure” Light

• Applied to Imaging as Sensor

What is a CCD?

Page 3: Basic Principles of CCD Imaging in Astronomy

• Revolutionized Astronomical Imaging– More Sensitive than Photographic Emulsions

• Factor of 100 Measure Light only 0.01 as Bright– Improved Light-Gathering Power of Telescopes by nearly 100

• Amateur w/ 15-cm (6") Telescope + CCD can get similar performance as 1960s Professional with 1-m (40") Telescope + Photography

• Now Considered to be “Standard” Sensor in Astronomical Imaging– Special Arrangements with Observatory Now Necessary to use

Photographic Plates or Film

CCDs in Astronomy

Page 4: Basic Principles of CCD Imaging in Astronomy

• Made from Crystalline Material– Typically Silicon (Si)

• CCD Converts “Light” to “Electronic Charge”– Spatial Pattern of Light Produces a Spatial Pattern of

Charge = “Image”1. “Digitized”

– Analog Measurements (“Voltages”) Converted to Integer Values at Discrete Locations

2. Stored as Computer File

What is a CCD?

Page 5: Basic Principles of CCD Imaging in Astronomy

Si Crystal Structure• Regular Pattern of Si

atoms– Fixed Separations

Between Atoms• Atomic Structure Pattern

“Perturbs” Electron Orbitals– Changes Layout of

Available Electron States from Model of Bohr Atom

http://www.webelements.com/webelements/elements/text/Si/xtal.html

Page 6: Basic Principles of CCD Imaging in Astronomy

Electron States in Si Crystal• Available States in Crystal Arranged in

Discrete “Bands” of Energies– Lower Band Valence Band

• More electrons– Upper Band Conduction Band

• Fewer electrons

• No States Exist in “Gap” Between Bands

Incr

easi

ng e

nerg

y

Valence Band of Electron States

Conduction Band of Electron States

“Gap” = 1.12 electron-volts(eV) - - -

-“Gap”

Page 7: Basic Principles of CCD Imaging in Astronomy

Comparison of State Structure in Crystal with Bohr Model

Orbitals

Discrete Transition

Isolated Atom (as in Gas)

Conduction Band

Valence Band

Single Atom in Crystal

“Gap”

States “Blur” Together To Form “Bands”

Page 8: Basic Principles of CCD Imaging in Astronomy

Action of Light on Electron States• Incoming Photon w/ Energy 1.12 eV

Excites Electrons From “Valence Band” to “Conduction Band”

• Electron in Conduction Band Moves in the Crystal “Lattice”

• Excited Electron e- leaves “Hole” (Lack of Electron = h+) in Valence Band– Hole = “Carrier” of Positive Charge

Page 9: Basic Principles of CCD Imaging in Astronomy

Action of “Charge Carriers”

• Carriers are “Free” to Move in the Band– Electron e- in Conduction Band– Hole h+ in Valence Band

• Charge Carriers may be “Counted” – Measurement of Number of Absorbed Photons

Page 10: Basic Principles of CCD Imaging in Astronomy

Maximum to “Jump” Si Band Gap

• 1 eV = 1.602 10-12 erg = 1.602 10-12 Joule

To Energize Electron in Si Lattice Requires < 1.1 m

27 8

12

6

6.624 10 sec 3 10sec

1.12 1.602 10

1.107 10 1107

merghc

ergE eVeV

m nm

Page 11: Basic Principles of CCD Imaging in Astronomy

Energy and Wavelength

• Incident Wavelength > 1.1 m Photon CANNOT be Absorbed!– Insufficient Energy to “Kick” Electron to

Conduction Band

Silicon is “Transparent” to long CCDs constructed from Silicon are Not

Sensitive to Long Wavelengths

Page 12: Basic Principles of CCD Imaging in Astronomy

After Electron is Excited into Conduction Band….

• Electron and Hole Usually “Recombine” Quickly– Charge Carriers are “Lost”

• Apply External Electric Field to “Separate” Electrons from Holes

• “Sweeps” Electrons Away from Holes– Maintains Population of “Free” Electrons– Allows Electrons to be “Counted”

Page 13: Basic Principles of CCD Imaging in Astronomy

photon

phot

on

Hole

Electron

Conduction Band

Valence Band

Generation of CCD Carriers

Page 14: Basic Principles of CCD Imaging in Astronomy

photon

phot

on

Conduction Band

Valence Band

Spontaneous Recombination

Page 15: Basic Principles of CCD Imaging in Astronomy

Prevent Spontaneous Recombination by Applying

Voltage to “Sweep” Electrons

+Ammeter

++++

Page 16: Basic Principles of CCD Imaging in Astronomy

Prevent Spontaneous Recombination by Applying

Voltage to “Sweep” Electrons

+

++++

Ammeter

Page 17: Basic Principles of CCD Imaging in Astronomy

Thermal “Noise”• Big BUT: Other Kinds of Energy Have Identical

Effect• Thermally Generated Electrons are

Indistinguishable from Photon-Generated Electrons – Heat Energy can “Kick” e- into Conduction Band– Thermal Electrons appear as “Noise” in Images

• “Dark Current”– Keep CCDs COLD to Reduce Number of Thermally

Generated Carriers (Dark Current)

Page 18: Basic Principles of CCD Imaging in Astronomy

How Do We “Count” Charge Carriers (“Photoelectrons”)?

• Must “Move” Charges to an “Amplifier”• Astronomical CCDs: Amplifier Located at

“Edge” of Light-Sensitive Region of CCD– Charge Transfer is “Slow”– Most of CCD Area “Sensitive” to Light

• Video and Amateur Camera CCDs: Must Transfer Charge QUICKLY– Less Area Available to Collect Light

Page 19: Basic Principles of CCD Imaging in Astronomy

“Bucket Brigade” CCD Analogy

• Electron Charge Generated by Photons is “Transferred” from Pixel to “Edge” of Array

• Transferred Charges are “Counted” to Measure Number of Photons

Page 20: Basic Principles of CCD Imaging in Astronomy

BUCKETS (PIXELS)

VERTICALCOLUMNS of PIXELS

CONVEYOR BELT

(SERIAL REGISTER)

MEASURING CYLINDER(OUTPUT

AMPLIFIER)

Rain of Photons

Page 21: Basic Principles of CCD Imaging in Astronomy

Shutter

Rain of Photons

Page 22: Basic Principles of CCD Imaging in Astronomy

CONVEYOR BELT

(SERIAL REGISTER)

MEASURING CYLINDER(OUTPUT AMPLIFIER)

Empty First Buckets in Column Into Buckets in Conveyor Belt

Page 23: Basic Principles of CCD Imaging in Astronomy

CONVEYOR BELT

(SERIAL REGISTER)

MEASURING CYLINDER(OUTPUT AMPLIFIER)

Page 24: Basic Principles of CCD Imaging in Astronomy

Empty Second Buckets in Column Into First Buckets

Page 25: Basic Principles of CCD Imaging in Astronomy
Page 26: Basic Principles of CCD Imaging in Astronomy

Empty Third Buckets in Column Into Second Buckets

Page 27: Basic Principles of CCD Imaging in Astronomy

Start Conveyor Belt

Page 28: Basic Principles of CCD Imaging in Astronomy
Page 29: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

After each bucket has been measured,the measuring cylinder is emptied,

ready for the next bucket load.

Page 30: Basic Principles of CCD Imaging in Astronomy
Page 31: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 32: Basic Principles of CCD Imaging in Astronomy
Page 33: Basic Principles of CCD Imaging in Astronomy
Page 34: Basic Principles of CCD Imaging in Astronomy

Empty First Buckets in Column Into Buckets in Conveyor Belt

Now Empty

Page 35: Basic Principles of CCD Imaging in Astronomy
Page 36: Basic Principles of CCD Imaging in Astronomy

Empty Second Buckets in Column Into First Buckets

Page 37: Basic Principles of CCD Imaging in Astronomy
Page 38: Basic Principles of CCD Imaging in Astronomy

Start Conveyor Belt

Page 39: Basic Principles of CCD Imaging in Astronomy
Page 40: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 41: Basic Principles of CCD Imaging in Astronomy
Page 42: Basic Principles of CCD Imaging in Astronomy
Page 43: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 44: Basic Principles of CCD Imaging in Astronomy
Page 45: Basic Principles of CCD Imaging in Astronomy
Page 46: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 47: Basic Principles of CCD Imaging in Astronomy

Empty First Buckets in Column Into Buckets in Conveyor Belt

Page 48: Basic Principles of CCD Imaging in Astronomy
Page 49: Basic Principles of CCD Imaging in Astronomy

Start Conveyor Belt

Page 50: Basic Principles of CCD Imaging in Astronomy
Page 51: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 52: Basic Principles of CCD Imaging in Astronomy
Page 53: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 54: Basic Principles of CCD Imaging in Astronomy
Page 55: Basic Principles of CCD Imaging in Astronomy

Measure& Drain

Page 56: Basic Principles of CCD Imaging in Astronomy

Ready for New Exposure

Page 57: Basic Principles of CCD Imaging in Astronomy

Features of CCD Readout

• Pixels are Counted in Sequence– Number of Electrons in One Pixel Measured at

One Time– Takes a While to Read Entire Array

• Condition of an Individual Pixel Affects Measurements of ALL Following Pixels– A “Leaky” Bucket Affects Other Measurements

in Same Column

Page 58: Basic Principles of CCD Imaging in Astronomy

for this Pixel

“Leaky” Bucket Loses Water (Charge)

AND following Pixel

Less Charge Measuredfor This Column

Page 59: Basic Principles of CCD Imaging in Astronomy

Structure of Astronomical CCDs• Image Area of

CCD Located at Focal Plane of Telescope

• Image Builds Up During Exposure

• Image Transferred, pixel-by-pixel to Output Amplifier

Connection pins

Gold bond wires

Bond pads

Silicon chip

PackageImage Area

Serial register(Conveyor Belt)

Output amplifier

Page 60: Basic Principles of CCD Imaging in Astronomy

CCD Manufacture

Don Groom LBNL

Page 61: Basic Principles of CCD Imaging in Astronomy

Fabricated CCD

Kodak KAF1401 1317 1035 pixels (1,363,095 pixels)

Page 62: Basic Principles of CCD Imaging in Astronomy

Charges (“Buckets” are Moved by Changing Voltage Pattern

123

Apply VoltagesHere

Page 63: Basic Principles of CCD Imaging in Astronomy

123

Charge Transfer

Page 64: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

Time-slice shown in diagram

1

2

3

Charge Transfer - 1

Page 65: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 2

Page 66: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 3

Page 67: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 4

Page 68: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 5

Page 69: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 6

Page 70: Basic Principles of CCD Imaging in Astronomy

123

+5V

0V

-5V

+5V

0V

-5V

+5V

0V

-5V

1

2

3

Charge Transfer - 7

Page 71: Basic Principles of CCD Imaging in Astronomy

pixe

l bo

unda

ry

Phot

ons

Charge Capacity of CCD pixel is Finite (Up to 300,000 Electrons)

After Pixel Fills, Charge Leaks into adjacent pixels.

Phot

ons

Overflowingcharge packet

Spillage Spillagepi

xel

boun

dary

CCD “Blooming” - 1

Page 72: Basic Principles of CCD Imaging in Astronomy

Flow of bloomed

charge

Channel “Stops” (Charge Barrier)

Charge Spreads in Column• Up AND Down

CCD “Blooming” - 2

ChargeTransferDirection

Page 73: Basic Principles of CCD Imaging in Astronomy

Bloomed Star Imageswith “Streaks”

M42

CCD “Blooming” - 3

• Long Exposure for Faint Nebulosity

Star Images are Overexposed

Page 74: Basic Principles of CCD Imaging in Astronomy

CCD Image Defects

• “Dark” Columns– Charge “Traps” Block Charge

Transfer– “Charge Bucket” with a

VERY LARGE Leak• Not Much of a Problem in

Astronomy– 7 Bad Columns out of 2048 Little Loss of Data

Page 75: Basic Principles of CCD Imaging in Astronomy

1. Bright Columns– Electron “Traps”

2. Hot Spots– Pixels with Larger Dark Current– Caused by Fabrication Problems

3. Cosmic Rays ()– Unavoidable– Ionization of e- in Si– Can Damage CCD if High

Energy (HST)

CCD Image Defects

Cosmic rays

Cluster ofHot Spots

BrightColumn

Page 76: Basic Principles of CCD Imaging in Astronomy

M51

Dark Column

Hot Spots, Bright Columns

Bright First Row • incorrect operation of signal processing electronics

CCD Image Defects

Negative Image

Page 77: Basic Principles of CCD Imaging in Astronomy

CCD Image Processing

• “Raw” CCD Image Must Be Processed to Correct for Image Errors

• CCD Image is Combination of 4 Images:1. “Raw” Image of Scene2. “Bias” Image3. “Dark Field” Image with Shutter Closed4. “Flat Field” Image of Uniformly Lit Scene

Page 78: Basic Principles of CCD Imaging in Astronomy

Bias Frame• Exposure of Zero Duration with Shutter Closed

– “Zero Point” or “Baseline” Signal from CCD– Resulting Structure in Image from Image Defects

and/or Electronic “Noise”• Record 5 Bias Frames Before Observing

– Calculate Average to Reduce Camera Readout Noise by 1/5 45%

Page 79: Basic Principles of CCD Imaging in Astronomy

“Dark Field” Image• Dark Current Minimized by

Cooling• Effect of Dark Current is

“Compensated” Using Exposures of Same Duration Taken with Shutter Closed.

• Dark Frames are Subtracted from Raw Frames

Dark Frame

Page 80: Basic Principles of CCD Imaging in Astronomy

“Flat Field” Image• Sensitivity to Light Varies from Pixel to Pixel

– Fabrication Problems– Dust Spots– Lens Vignetting– …

• Image of “Uniform” (“Flat”) Field– Twilight Sky at High Magnification– Inside of Closed Dome

Page 81: Basic Principles of CCD Imaging in Astronomy

, ,r x y d x y

Correction of Raw Imagewith Bias, Dark, Flat Images

Flat Field Image

Bias Image

OutputImage

Dark Frame

Raw File ,r x y

,d x y

,f x y

,b x y

, ,f x y b x y

“Flat” “Bias”

“Raw” “Dark”

, ,, ,

r x y d x yf x y b x y

“Raw” “Dark”“Flat” “Bias”

Page 82: Basic Principles of CCD Imaging in Astronomy

, ,r x y b x y

Correction of Raw Imagew/ Flat Image, w/o Dark Image

Flat Field Image

Bias Image

OutputImage

Raw File

,r x y

,f x y

,b x y , ,f x y b x y

“Flat” “Bias”

, ,, ,

r x y b x yf x y b x y

“Raw” “Bias”“Flat” “Bias”

“Raw” “Bias”

Assumes Small Dark Current(Cooled Camera)