Flight 188 - uppsagd

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Data relating to Flight 188The PLANCK missionThe Planck satellite has been designed to analyse andmeasure, with unequalled precision, the very low temperaturevariations, or “anisotropies”, of the of the firstlight which filled the Universe after the Big Bang, namelyCosmic Microwave Background (CMB) radiation. Planckwill cover the whole sky with an angular resolution of 5minutes of arc, improving by a factor of about 15 on theinformation delivered by its predecessor WMAP. With the data collected by Planck, thescientists hope to obtain a better understanding of the origin, evolution and geometryof the Universe, and the nature of black energy and the minute matter density fluctuationsat the origin of the galaxies.1 billion years afterthe Big Bang: thegalaxies300,000 yearsafter the BigBang: CMBemission5.5 billion years after theBig Bang: Earth1 s to 3 mn afterthe Big BangPlanck is taking over from the COBE and WMAP satellites (launched by NASA in 1992and 2003 respectively) and will provide very substantially enhanced measurementprecision.Sky maps as seen by COBE: the first image presentsthe temperature of the sky: we observe theimpact of movement of the Sun (dipole form) andthe Milky Way (weak horizontal smudge).With these two effects eliminated, the seconddiagram presents a wideband associated with theresidual emission of the galaxy, and a backgroundfilled with hot and cold points due largely to mixtureof the CMB with the measurement noiseinduced by the instrument.22
Data relating to Flight 188Sky map as seen by WMAP: this image presents a marked enhancement of the clarityand acuity of the sky map resulting from WMAP resolution. It shows minuscule CMBtemperature irregularities.The rotational speed of the satellite, separatedunder slow spin, will stabilise at 1 rotation perminute, making it possible to scan the entire skyin 6 months. Planck will acquire data coveringfour to five times the complete Universe in thespace of 21 months.The 1.5 m-diameter Planck telescope will focus radiation ontwo instruments:• The HFI (High Frequency Instrument) comprises 50bolometers and will be used to convert radiation (from awavelength of 1 cm to 1/3 mm) into heat. The focal planeof this instrument operates at a temperature of 0.1°K;• The LFI (Low Frequency Instrument) comprises a numberof radio receivers operating at a temperature of -253°C.The two instruments will be kept permanently chilled by acooling system operating in the cascade mode (passive systemto 50°K, Sorption Cooler to 18°K, 4°K Cooler to 4°K andDilution Cooler to 0.1°K).23
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Flight 188 - uppsagd

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