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The Planck Surveyor Telescope

History of Planck Surveyor

• Mission was selected in

1996 as the 3rd mission of

ESA in the 2000 Horizon

Space Program

• First named

COBRAS/SAMBA later

renamed Planck after

German Physicist Max

Planck, won Nobel Price

in 1918

History Continued • Planned to launch in

February 2007

• Commenced building

in 1999

• 3rd telescope to be

launched to study

CMB

– 1st telescope-COBE-

launched 1989

– 2nd telescope-WMAP-

launched 2001

Properties of Planck Surveyor

• Designed to detect microwaves

• Has an off axis Gregorian design

• Has a primary mirror of 1.75m x 1.75m

• Contains 2 instruments

– LFI

– HFI

LFI (Low Frequency Instrument)



• Has 22 tuned radio

receivers

• Will be operated at

-256°C

• Radio receivers work like

transistors they amplify

the signal from telescope

and then it is stored for

analysis

• detects wavelengths at 11.1

to 3.0 mm

HFI (High Frequency Instrument)

• Has 52 detectors which

work by converting

radiation to heat, will

do this through 6

wavelength channels

and is operated at

-272.9°C

• Detects at 3.6 to 0.3

mm

Planck Design

• the LFI and HFI

combine their

measurements to yield

a map of the

anisotropies of the

Cosmic Microwave

Background

Design of Planck

• Planck will sit at the L2

point between the Sun and

Earth

• Will continuously face the

anti-sun direction which

will minimize confusing

signals from thermal

fluctuations

Goals of Planck Mission









• Mapping of the anistropies of cosmic microwave

background

• Determination of the Hubble constant

• Testing models of the early universe

Goals continued

• What the dark matter that composes the

universe is made of

• How did the universe evolve into what it is

today?

• How will it continue to evolve? It will it

continue to expand?

Advantages Over Previous Models



• Compared to WMAP and

COBE has higher angular

resolution

• maps it creates of

anisotropies will be

superior to WMAP

because of higher

sensitivity and angular

resolution

Advantages Continued

• Planck will make

measurements over

broader range of

frequencies that will

help get rid of

interfering signals

• Can detect the

slightest variation in

temperature

Technological Advances



• Will have shields that

will cover the focal

plane and telescope

which will reduce

stray light and will

protect the instrument

from thermal radiation

Technological Advances

• Planck’s 2 instruments the LFI

and HFI will be combined to

yield precise map of the

anisotropies of CMB

• Planck will need to overcome the

many different radiations that are

emitted in our universe that are

not actually CMB, will do this by

having different instruments that

measure other wavelengths

Technological Advances

• Planck’s detectors will be

set at a temperature just

slightly above absolute

zero (0 Kelvin) to detect

the slightest fluctuations

• Planck’s off axis-tilt

Gregorian design allows

for no blocking of the

optical path

Pictures from WMAP

Pictures from COBE

For More Information:

• http://www.rssd.esa.int/index.php?project=Planck



• http://aether.lbl.gov/www/projects/cosa/



• http://planck.esa.int/science-e/www/area/index.cfm?fareaid=17



• http://www.rssd.esa.int/SA/PLANCK/images/pictures/brochures/

planck.pdf


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