Planck Surveyor
Encyclopedia
Planck is a space observatory
of the European Space Agency (ESA) and designed to observe the anisotropies
of the cosmic microwave background
(CMB) over the entire sky, at a high sensitivity and angular resolution
. Planck was built in the Cannes Mandelieu Space Center
by Thales Alenia Space
and created as the third Medium-Sized Mission (M3) of the European Space Agency's
Horizon 2000 Scientific Programme. The project, initially called COBRAS/SAMBA, is named in honour of the German physicist Max Planck
(1858–1947), who won the Nobel Prize for Physics in 1918.
Planck was launched in May 2009, reaching the Earth/Sun's L2 Lagrangian point
in July, and by February 2010 had successfully started a second all-sky survey. Preliminary data from these surveys have been released, and results are said to indicate that the data quality is excellent. Planck is expected to yield definitive data on a number of astronomical issues by 2012. The mission will complement and improve upon observations made by the NASA
Wilkinson Microwave Anisotropy Probe
(WMAP), which has measured the anisotropies at larger angular scales and lower sensitivity than Planck. Planck will provide a major source of information relevant to several cosmological and astrophysical issues, such as testing theories of the early universe and the origin of cosmic structure.
Planck represents an advance over WMAP in several respects.
It is expected that most Planck measurements will be limited by how well foregrounds can be subtracted, rather than by the detector performance or length of the mission. This is particularly important for the polarization measurements. The dominant foreground depends on frequency, but examples include synchrotron radiation
from the Milky Way Galaxy at low frequencies, and dust at high frequencies.
The LFI has three frequency bands, covering the range of 30–70 GHz. The detectors use High Electron Mobility Transistors
.
The HFI has six frequency bands, between 100 and 857 GHz. They use bolometer
s to detect photons. The four lower frequency bands have sensitivity to linear polarization; the two higher bands do not. The HFI instrument uses 48 bolometric detectors (manufactured by JPL–Caltech) optically coupled to the telescope through cold optics (manufactured by Cardiff University's School of Physics and Astronomy) consisting of a triple horn configuration and optical filters (similar concept used in Archeops ). These detection assemblies are divided into 6 frequency bands (centred at 100, 143, 217, 353, 545 and 857 GHz) with a bandwidth of 33%. Out of these 6 bands, 4 will have the capability to measure the polarisation of the incoming radiation (100, 143, 217 and 353-GHz bands).
design is an off-axis tilted
Gregorian system
, offering the advantages of no blocking of the optical path
combined with compactness. Both the primary mirror
and the secondary mirror
are off-axis
. The eccentricity and tilt angle
of the secondary mirror and the off-axis angle obey the Dragone-Mizuguchi condition, which allows the system to operate without significant degradation over a large focal plane array, while simultaneously minimizing the polarization effects introduced by the telescope.
The baffling system is composed of two elements. The shield
element is a large, self-supporting and roughly conical structure
covered with multi-layer insulation
(MLI), which surrounds the telescope and focal plane instruments. Together with the optical bench, it defines the optical enclosure. It has two important functions, reducing the level of stray light
(which at the chosen orbit
is in large part due to the spacecraft itself) and promoting the radiative cooling
of the optical enclosure towards deep space. The baffle element consists of one half of a conically shaped surface that links the focal plane instruments to the bottom edge of the sub-reflector. The function of the baffle is to shield the detectors from thermal radiation
originating within the optical enclosure.
Telescope characteristics
Type: Off-axis tilted Gregorian
Primary mirror: 1.9 × 1.5 m, off-axis paraboloid
Secondary mirror: 1.1 × 1.0 m, off-axis paraboloid
built components of the science instruments, including bolometer
s for the high-frequency instrument, a 20 Kelvin cryocooler
for both the low- and high-frequency instruments, and amplifier technology for the low-frequency instrument.
(SVM) was designed and built by Thales Alenia Space in its Turin
plant, for both the Herschel Space Observatory
and Planck missions, combined into one single program.
Structurally the Herschel and Planck SVM's are very similar. Both SVM's are of octagonal shape and for both, each panel is dedicated to accommodate a designated set of warm units, while taking into account the dissipation requirements of the different warm units, of the instruments as well as the spacecraft.
Furthermore, on both spacecraft a common design for the avionics
, the attitude control and measurement system (ACMS) and the command and data management system (CDMS), and power subsystem and the tracking, telemetry and command subsystem (TT&C) has been achieved.
All spacecraft units on the SVM are redundant.
, employing triple-junction solar cell
s, a battery
and the power control unit (PCU). It is designed to interface with the 30 sections of each solar array, provide a regulated 28 V bus, distribute this power via protected outputs and to handle the battery charging and discharging.
For Planck, the circular solar array is fixed on the bottom part of the satellite, facing always the sun, as the satellite is spinning around its vertical axis.
The Planck satellite is spun
at one revolution per minute, the absolute pointing error needs to be less than 37 arc min. For Planck being a survey platform, there is also a requirement to be met on pointing reproducibility error to be less than 2.5 arc min over 20 days.
The main sensor of the line of sight in both spacecraft is the star tracker.
, at 13:12:02 on 14 May 2009 aboard an Ariane 5 ECA
heavy launch vehicle. The launch placed the craft into a very elliptical orbit (perigee: 270 km, apogee: more than 1,120,000 km), bringing it near the Lagrangian point of the Earth-Sun system, 1.5 million kilometers from the Earth.
The maneuver to inject Planck into its final orbit around was successfully completed on July 3, 2009, when it entered a Lissajous orbit
of 400,000 km radius around the Lagrangian point. The temperature of the High Frequency Instrument reached just a tenth of a degree above absolute zero (0.1 K) on July 3, 2009, placing both the Low Frequency and High Frequency Instruments within their cryogenic operational parameters, making Planck fully operational.
announced the preliminary results from the Planck First Light Survey (performed to demonstrate the stability of the instruments and the ability to calibrate them over long periods). The results indicated that the data quality is excellent.
On 15 January 2010 the mission was extended by 12 months, with observation continuing until at least the end of 2011. After the successful conclusion of the First Survey, the spacecraft started its Second All Sky Survey on 14 February 2010, with more than 95% of the sky observed already and 100% sky coverage being expected by mid-June 2010.
Some planned pointing list data from 2009 have been released publicly, along with a video visualization of the surveyed sky. The first results are scheduled for release during a conference in Paris from the 10–14 January 2011, and the final results (with all processed data) are expected to be delivered to the worldwide community towards the end of 2012.
On 17 March 2010 the first Planck photos were published, showing dust concentration within 500 light years from the Sun.
On 5 July 2010, the Planck mission delivered its first all-sky image.
Space observatory
A space observatory is any instrument in outer space which is used for observation of distant planets, galaxies, and other outer space objects...
of the European Space Agency (ESA) and designed to observe the anisotropies
Anisotropy
Anisotropy is the property of being directionally dependent, as opposed to isotropy, which implies identical properties in all directions. It can be defined as a difference, when measured along different axes, in a material's physical or mechanical properties An example of anisotropy is the light...
of the cosmic microwave background
Cosmic microwave background radiation
In cosmology, cosmic microwave background radiation is thermal radiation filling the observable universe almost uniformly....
(CMB) over the entire sky, at a high sensitivity and angular resolution
Angular resolution
Angular resolution, or spatial resolution, describes the ability of any image-forming device such as an optical or radio telescope, a microscope, a camera, or an eye, to distinguish small details of an object...
. Planck was built in the Cannes Mandelieu Space Center
Cannes Mandelieu Space Center
The Cannes Mandelieu Space Center is an industrial plant dedicated to spacecraft manufacturing, located in both the towns of Cannes and Mandelieu in France...
by Thales Alenia Space
Thales Alenia Space
Thales Alenia Space is an aerospace company born after the Thales Group bought the participation of Alcatel in the two joint-ventures between Alcatel and Finmeccanica, Alcatel Alenia Space and Telespazio.-History:...
and created as the third Medium-Sized Mission (M3) of the European Space Agency's
European Space Agency
The European Space Agency , established in 1975, is an intergovernmental organisation dedicated to the exploration of space, currently with 18 member states...
Horizon 2000 Scientific Programme. The project, initially called COBRAS/SAMBA, is named in honour of the German physicist Max Planck
Max Planck
Max Karl Ernst Ludwig Planck, ForMemRS, was a German physicist who actualized the quantum physics, initiating a revolution in natural science and philosophy. He is regarded as the founder of the quantum theory, for which he received the Nobel Prize in Physics in 1918.-Life and career:Planck came...
(1858–1947), who won the Nobel Prize for Physics in 1918.
Planck was launched in May 2009, reaching the Earth/Sun's L2 Lagrangian point
Lagrangian point
The Lagrangian points are the five positions in an orbital configuration where a small object affected only by gravity can theoretically be stationary relative to two larger objects...
in July, and by February 2010 had successfully started a second all-sky survey. Preliminary data from these surveys have been released, and results are said to indicate that the data quality is excellent. Planck is expected to yield definitive data on a number of astronomical issues by 2012. The mission will complement and improve upon observations made by the NASA
NASA
The National Aeronautics and Space Administration is the agency of the United States government that is responsible for the nation's civilian space program and for aeronautics and aerospace research...
Wilkinson Microwave Anisotropy Probe
Wilkinson Microwave Anisotropy Probe
The Wilkinson Microwave Anisotropy Probe — also known as the Microwave Anisotropy Probe , and Explorer 80 — is a spacecraft which measures differences in the temperature of the Big Bang's remnant radiant heat — the Cosmic Microwave Background Radiation — across the full sky. Headed by Professor...
(WMAP), which has measured the anisotropies at larger angular scales and lower sensitivity than Planck. Planck will provide a major source of information relevant to several cosmological and astrophysical issues, such as testing theories of the early universe and the origin of cosmic structure.
Objectives
The mission has a wide variety of scientific aims, including:- High resolution detections of both the total intensity and polarization of the primordial CMBCosmic microwave background radiationIn cosmology, cosmic microwave background radiation is thermal radiation filling the observable universe almost uniformly....
anisotropies - Creation of a catalogue of galaxy clusters through the Sunyaev-Zel'dovich effectSunyaev-Zel'dovich effectThe Sunyaev–Zel'dovich effect is the result of high energy electrons distorting the cosmic microwave background radiation through inverse Compton scattering, in which the low energy CMB photons receive energy boost during collision with the high energy cluster electrons...
- Observations of the gravitational lensing of the CMB, as well as the integrated Sachs–Wolfe effect
- Observations of bright extragalactic radio (active galactic nucleiActive galactic nucleusAn active galactic nucleus is a compact region at the centre of a galaxy that has a much higher than normal luminosity over at least some portion, and possibly all, of the electromagnetic spectrum. Such excess emission has been observed in the radio, infrared, optical, ultra-violet, X-ray and...
) and infrared (dusty galaxy) sources - Observations of the Milky WayMilky WayThe Milky Way is the galaxy that contains the Solar System. This name derives from its appearance as a dim un-resolved "milky" glowing band arching across the night sky...
, including the local interstellar mediumInterstellar mediumIn astronomy, the interstellar medium is the matter that exists in the space between the star systems in a galaxy. This matter includes gas in ionic, atomic, and molecular form, dust, and cosmic rays. It fills interstellar space and blends smoothly into the surrounding intergalactic space...
, distributed synchrotronSynchrotronA synchrotron is a particular type of cyclic particle accelerator in which the magnetic field and the electric field are carefully synchronised with the travelling particle beam. The proton synchrotron was originally conceived by Sir Marcus Oliphant...
emission and measurements of the galactic magnetic fieldMagnetic fieldA magnetic field is a mathematical description of the magnetic influence of electric currents and magnetic materials. The magnetic field at any given point is specified by both a direction and a magnitude ; as such it is a vector field.Technically, a magnetic field is a pseudo vector;...
. - Studies of the local Solar System, including planetPlanetA planet is a celestial body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science,...
s, asteroidAsteroidAsteroids are a class of small Solar System bodies in orbit around the Sun. They have also been called planetoids, especially the larger ones...
s, cometCometA comet is an icy small Solar System body that, when close enough to the Sun, displays a visible coma and sometimes also a tail. These phenomena are both due to the effects of solar radiation and the solar wind upon the nucleus of the comet...
s and the zodiacal lightZodiacal lightZodiacal light is a faint, roughly triangular, whitish glow seen in the night sky which appears to extend up from the vicinity of the sun along the ecliptic or zodiac. Caused by sunlight scattered by space dust in the zodiacal cloud, it is so faint that either moonlight or light pollution renders...
.
Planck represents an advance over WMAP in several respects.
- It has higher resolution, allowing it to probe the power spectrum of the CMB to much smaller scales (x3).
- It has higher sensitivity (x10).
- It observes in 9 frequency bands rather than 5, with the goal of improving the astrophysical foreground models.
It is expected that most Planck measurements will be limited by how well foregrounds can be subtracted, rather than by the detector performance or length of the mission. This is particularly important for the polarization measurements. The dominant foreground depends on frequency, but examples include synchrotron radiation
Synchrotron radiation
The electromagnetic radiation emitted when charged particles are accelerated radially is called synchrotron radiation. It is produced in synchrotrons using bending magnets, undulators and/or wigglers...
from the Milky Way Galaxy at low frequencies, and dust at high frequencies.
Instruments
The spacecraft carries two instruments; the Low Frequency Instrument (LFI) and the High Frequency Instrument (HFI). Both instruments can detect both the total intensity and polarization of photons, and together cover a frequency range of 30 to 857 GHz. The cosmic microwave background spectrum peaks at a frequency of 160.2 GHzLow Frequency Instrument
| Frequency (GHz) |
Bandwidth (  ) |
Resolution (arcmin) |
Sensitivity (total intensity) , 14 month observation(10−6) |
Sensitivity (polarization) , 14 month observation(10−6) |
|---|---|---|---|---|
| 30 | 0.2 | 33 | 2.0 | 2.8 |
| 44 | 0.2 | 24 | 2.7 | 3.9 |
| 70 | 0.2 | 14 | 4.7 | 6.7 |
The LFI has three frequency bands, covering the range of 30–70 GHz. The detectors use High Electron Mobility Transistors
HEMT
High electron mobility transistor , also known as heterostructure FET or modulation-doped FET , is a field effect transistor incorporating a junction between two materials with different band gaps as the channel instead of a doped region, as is generally the case for MOSFET...
.
High Frequency Instrument
| Frequency (GHz) |
Bandwidth (  ) |
Resolution (arcmin) |
Sensitivity (total intensity) , 14 month observation(10−6) |
Sensitivity (polarization) , 14 month observation(10−6) |
|---|---|---|---|---|
| 100 | 0.33 | 10 | 2.5 | 4.0 |
| 143 | 0.33 | 7.1 | 2.2 | 4.2 |
| 217 | 0.33 | 5.5 | 4.8 | 9.8 |
| 353 | 0.33 | 5.0 | 14.7 | 29.8 |
| 545 | 0.33 | 5.0 | 147 | N/A |
| 857 | 0.33 | 5.0 | 6700 | N/A |
The HFI has six frequency bands, between 100 and 857 GHz. They use bolometer
Bolometer
A bolometer is a device for measuring the power of incident electromagnetic radiation via the heating of a material with a temperature-dependent electrical resistance. It was invented in 1878 by the American astronomer Samuel Pierpont Langley...
s to detect photons. The four lower frequency bands have sensitivity to linear polarization; the two higher bands do not. The HFI instrument uses 48 bolometric detectors (manufactured by JPL–Caltech) optically coupled to the telescope through cold optics (manufactured by Cardiff University's School of Physics and Astronomy) consisting of a triple horn configuration and optical filters (similar concept used in Archeops ). These detection assemblies are divided into 6 frequency bands (centred at 100, 143, 217, 353, 545 and 857 GHz) with a bandwidth of 33%. Out of these 6 bands, 4 will have the capability to measure the polarisation of the incoming radiation (100, 143, 217 and 353-GHz bands).
Telescope
The telescopeTelescope
A telescope is an instrument that aids in the observation of remote objects by collecting electromagnetic radiation . The first known practical telescopes were invented in the Netherlands at the beginning of the 1600s , using glass lenses...
design is an off-axis tilted
Tilt (optics)
In optics, tilt is a deviation in the direction a beam of light propagates. Tilt quantifies the average slope in both the X and Y directions of a wavefront or phase profile across the pupil of an optical system...
Gregorian system
Gregorian telescope
The Gregorian telescope is a type of reflecting telescope designed by Scottish mathematician and astronomer James Gregory in the 17th century, and first built in 1673 by Robert Hooke...
, offering the advantages of no blocking of the optical path
Optical path
The path that light takes in traversing an optical system is often called the optical path. The physical length of an optical device can be reduced to less than the length of the optical path by using folded optics. The optical path length as defined in optics is the length of the path multiplied...
combined with compactness. Both the primary mirror
Primary mirror
A primary mirror is the principal light-gathering surface of a reflecting telescope.-Description:The primary mirror of a reflecting telescope is a spherical or parabolic shaped disks of polished reflective metal , or in later telescopes, glass or other material coated with a reflective layer...
and the secondary mirror
Secondary mirror
A secondary mirror is the second deflecting or focusing mirror element in a reflecting telescope. Light gathered by the primary mirror is directed towards a focal point typically past the location of the secondary. Secondary mirrors in the form of an optically flat diagonal mirror are used to...
are off-axis
Off-axis optical system
An off-axis optical system is an optical system in which the optical axis of the aperture is not coincident with the mechanical center of the aperture. An optical system in which the optical axis of the aperture is not coincident with the mechanical center of the aperture...
. The eccentricity and tilt angle
Angle
In geometry, an angle is the figure formed by two rays sharing a common endpoint, called the vertex of the angle.Angles are usually presumed to be in a Euclidean plane with the circle taken for standard with regard to direction. In fact, an angle is frequently viewed as a measure of an circular arc...
of the secondary mirror and the off-axis angle obey the Dragone-Mizuguchi condition, which allows the system to operate without significant degradation over a large focal plane array, while simultaneously minimizing the polarization effects introduced by the telescope.
The baffling system is composed of two elements. The shield
Cold shield
A cold shield is a device to protect an object from unwanted heating by thermal radiation or light. Usually it is a cooled object with low absorption and high reflectivity....
element is a large, self-supporting and roughly conical structure
Conical surface
In geometry, a conical surface is the unbounded surface formed by the union of all the straight lines that pass through a fixed point — the apex or vertex — and any point of some fixed space curve — the directrix — that does not contain the apex...
covered with multi-layer insulation
Multi-layer insulation
Multi-layer insulation, or MLI, is thermal insulation composed of multiple layers of thin sheets often used on spacecraft. It one of the main items of the spacecraft thermal design, mainly intended to reduce heat loss by thermal radiation. In its basic form, it does not appreciably insulate...
(MLI), which surrounds the telescope and focal plane instruments. Together with the optical bench, it defines the optical enclosure. It has two important functions, reducing the level of stray light
Stray light
Stray light is light in an optical system, which was not intended in the design. The light may be from the intended source, but follow paths other than intended, or it may be from a source other than the intended source...
(which at the chosen orbit
Orbit
In physics, an orbit is the gravitationally curved path of an object around a point in space, for example the orbit of a planet around the center of a star system, such as the Solar System...
is in large part due to the spacecraft itself) and promoting the radiative cooling
Radiative cooling
Radiative cooling is the process by which a body loses heat by thermal radiation.- Earth's energy budget :In the case of the earth-atmosphere system it refers to the process by which long-wave radiation is emitted to balance the absorption of short-wave energy from the sun.The exact process by...
of the optical enclosure towards deep space. The baffle element consists of one half of a conically shaped surface that links the focal plane instruments to the bottom edge of the sub-reflector. The function of the baffle is to shield the detectors from thermal radiation
Thermal radiation
Thermal radiation is electromagnetic radiation generated by the thermal motion of charged particles in matter. All matter with a temperature greater than absolute zero emits thermal radiation....
originating within the optical enclosure.
Telescope characteristics
Type: Off-axis tilted Gregorian
Gregorian telescope
The Gregorian telescope is a type of reflecting telescope designed by Scottish mathematician and astronomer James Gregory in the 17th century, and first built in 1673 by Robert Hooke...
Primary mirror: 1.9 × 1.5 m, off-axis paraboloid
Paraboloid
In mathematics, a paraboloid is a quadric surface of special kind. There are two kinds of paraboloids: elliptic and hyperbolic. The elliptic paraboloid is shaped like an oval cup and can have a maximum or minimum point....
Secondary mirror: 1.1 × 1.0 m, off-axis paraboloid
NASA
NASA played a role in the development of the mission and will contribute to the analysis of science data. Its Jet Propulsion LaboratoryJet Propulsion Laboratory
Jet Propulsion Laboratory is a federally funded research and development center and NASA field center located in the San Gabriel Valley area of Los Angeles County, California, United States. The facility is headquartered in the city of Pasadena on the border of La Cañada Flintridge and Pasadena...
built components of the science instruments, including bolometer
Bolometer
A bolometer is a device for measuring the power of incident electromagnetic radiation via the heating of a material with a temperature-dependent electrical resistance. It was invented in 1878 by the American astronomer Samuel Pierpont Langley...
s for the high-frequency instrument, a 20 Kelvin cryocooler
Cryocooler
Cryocoolers are the devices used to reach cryogenic temperatures by cycling certain gases.A cryostat is likely to be used to reach and/or maintain similar conditions or keep some environment in cryogenic stasis...
for both the low- and high-frequency instruments, and amplifier technology for the low-frequency instrument.
Service Module – a common development for Herschel and Planck
A common service moduleService module
A service module is a spacecraft compartment containing a variety of support systems used for spacecraft operations. Usually located in the uninhabited area of the spacecraft, the service module is jettisoned upon the completion of the mission, and usually burns up during atmospheric reentry...
(SVM) was designed and built by Thales Alenia Space in its Turin
Turin
Turin is a city and major business and cultural centre in northern Italy, capital of the Piedmont region, located mainly on the left bank of the Po River and surrounded by the Alpine arch. The population of the city proper is 909,193 while the population of the urban area is estimated by Eurostat...
plant, for both the Herschel Space Observatory
Herschel Space Observatory
The Herschel Space Observatory is a European Space Agency space observatory sensitive to the far infrared and submillimetre wavebands. It is the largest space telescope ever launched, carrying a single mirror of in diameter....
and Planck missions, combined into one single program.
Structurally the Herschel and Planck SVM's are very similar. Both SVM's are of octagonal shape and for both, each panel is dedicated to accommodate a designated set of warm units, while taking into account the dissipation requirements of the different warm units, of the instruments as well as the spacecraft.
Furthermore, on both spacecraft a common design for the avionics
Avionics
Avionics are electronic systems used on aircraft, artificial satellites and spacecraft.Avionic systems include communications, navigation, the display and management of multiple systems and the hundreds of systems that are fitted to aircraft to meet individual roles...
, the attitude control and measurement system (ACMS) and the command and data management system (CDMS), and power subsystem and the tracking, telemetry and command subsystem (TT&C) has been achieved.
All spacecraft units on the SVM are redundant.
Power Subsystem
On each spacecraft, the power subsystem consists of the solar arraySolar panels on spacecraft
Spacecraft operating in the inner solar system usually rely on the use of photovoltaic solar panels to derive electricity from sunlight. In the outer solar system, where the sunlight is too weak to produce sufficient power, radioisotope thermal generators are used as a power source.-History:The...
, employing triple-junction solar cell
Solar cell
A solar cell is a solid state electrical device that converts the energy of light directly into electricity by the photovoltaic effect....
s, a battery
Battery (electricity)
An electrical battery is one or more electrochemical cells that convert stored chemical energy into electrical energy. Since the invention of the first battery in 1800 by Alessandro Volta and especially since the technically improved Daniell cell in 1836, batteries have become a common power...
and the power control unit (PCU). It is designed to interface with the 30 sections of each solar array, provide a regulated 28 V bus, distribute this power via protected outputs and to handle the battery charging and discharging.
For Planck, the circular solar array is fixed on the bottom part of the satellite, facing always the sun, as the satellite is spinning around its vertical axis.
Attitude and Orbit Control
This function is performed by the attitude control computer (ACC) which is the platform for the ACMS. It is designed to fulfil the pointing and slewing requirements of the Herschel and Planck payload.The Planck satellite is spun
Rotation
A rotation is a circular movement of an object around a center of rotation. A three-dimensional object rotates always around an imaginary line called a rotation axis. If the axis is within the body, and passes through its center of mass the body is said to rotate upon itself, or spin. A rotation...
at one revolution per minute, the absolute pointing error needs to be less than 37 arc min. For Planck being a survey platform, there is also a requirement to be met on pointing reproducibility error to be less than 2.5 arc min over 20 days.
The main sensor of the line of sight in both spacecraft is the star tracker.
Launch and orbit
The satellite was successfully launched, along with the Herschel Space ObservatoryHerschel Space Observatory
The Herschel Space Observatory is a European Space Agency space observatory sensitive to the far infrared and submillimetre wavebands. It is the largest space telescope ever launched, carrying a single mirror of in diameter....
, at 13:12:02 on 14 May 2009 aboard an Ariane 5 ECA
Ariane 5
Ariane 5 is, as a part of Ariane rocket family, an expendable launch system used to deliver payloads into geostationary transfer orbit or low Earth orbit . Ariane 5 rockets are manufactured under the authority of the European Space Agency and the Centre National d'Etudes Spatiales...
heavy launch vehicle. The launch placed the craft into a very elliptical orbit (perigee: 270 km, apogee: more than 1,120,000 km), bringing it near the Lagrangian point of the Earth-Sun system, 1.5 million kilometers from the Earth.
The maneuver to inject Planck into its final orbit around was successfully completed on July 3, 2009, when it entered a Lissajous orbit
Lissajous orbit
In orbital mechanics, a Lissajous orbit, , named after Jules Antoine Lissajous, is a quasi-periodic orbital trajectory that an object can follow around a Lagrangian point of a three-body system without requiring any propulsion. Lyapunov orbits around a libration point are curved paths that lie...
of 400,000 km radius around the Lagrangian point. The temperature of the High Frequency Instrument reached just a tenth of a degree above absolute zero (0.1 K) on July 3, 2009, placing both the Low Frequency and High Frequency Instruments within their cryogenic operational parameters, making Planck fully operational.
Results
Planck started its First All-Sky Survey on 13 August 2009. In September 2009, the European Space AgencyEuropean Space Agency
The European Space Agency , established in 1975, is an intergovernmental organisation dedicated to the exploration of space, currently with 18 member states...
announced the preliminary results from the Planck First Light Survey (performed to demonstrate the stability of the instruments and the ability to calibrate them over long periods). The results indicated that the data quality is excellent.
On 15 January 2010 the mission was extended by 12 months, with observation continuing until at least the end of 2011. After the successful conclusion of the First Survey, the spacecraft started its Second All Sky Survey on 14 February 2010, with more than 95% of the sky observed already and 100% sky coverage being expected by mid-June 2010.
Some planned pointing list data from 2009 have been released publicly, along with a video visualization of the surveyed sky. The first results are scheduled for release during a conference in Paris from the 10–14 January 2011, and the final results (with all processed data) are expected to be delivered to the worldwide community towards the end of 2012.
On 17 March 2010 the first Planck photos were published, showing dust concentration within 500 light years from the Sun.
On 5 July 2010, the Planck mission delivered its first all-sky image.
