PLATO (PLAnetary Transits and Oscillations of stars) was proposed as an M-class candidate mission for the Cosmic Vision 2015-2025 programme in response to the Call for Proposals issued by ESA in March 2007. The proposal was submitted by Claude Catala (Observatoire de Paris, France) on behalf of a large consortium comprising scientists from across Europe. In October of that year it was selected for further assessment and consideration by ESA.

PLATO timeline

Phase 0 – November 2007 - April 2008

The ESA internal assessment phase, or phase 0, for all candidate missions began in November 2007. The CDF study, part of the phase 0 process, for PLATO ran from December 2007 to January 2008. This led to a design that was suitable for a feasibility assessment and production of an Invitation to Tender to Industry.

Study Assessment Phase – November 2008 – December 2009

In April 2008 the Invitation to Tender was issued to Industry. Following a competitive assessment Astrium (France) and Thales Alenia Space (Italy) were selected to run parallel industrial assessment studies lasting approximately one year. At the same time a consortium of ESA Member State scientists, the PLATO Payload Consortium (PPLC), was formed to carry out an independent study of the payload, under the leadership of Claude Catala. All three studies ran in parallel and were completed at the end of summer 2009. A PLATO Science Consortium (PSC), formed in 2008 under the leadership of Don Pollacco (Queen’s University Belfast, United Kingdom), worked on the scientific preparation of the mission during this period.

The report of the assessment study, which includes the PLATO science case together with a synthesis of the industrial and instrument consortium studies, was presented to the scientific community in December 2009. In addition, an independent technical review of the assessment study was conducted by ESA. The recommendations of the review board were presented to the scientific community also in December 2009.

Definition Phase – June 2010 – mid-2011

In early 2010 the advisory body structure of ESA’s Science and Robotic Exploration Directorate met to consider the outcome of the studies of all M-class missions. Taking account of the scientific priorities of the Cosmic Vision plan and the technical feasibility of the candidate missions (as determined by the studies conducted by ESA and industry) the Science Programme Committee recommended that PLATO, along with Euclid and Solar Orbiter proceed to the next phase: a more detailed definition phase, with a decision point by mid-2011 on the (up to two) missions that will proceed further to implementation. During this time the cost and implementation schedule for the mission must be firmly established.

Advanced Composition Explorer (ACE) is a NASA space exploration mission being conducted as part of the Explorer program to study matter in situ, comprising energetic particles from the solar wind, the interplanetary medium, and other sources. Real-time data from ACE is used by the Space Weather Prediction Center to improve forecasts and warnings of solar storms. The ACE robotic spacecraft was launched August 25, 1997 and is currently operating in a Lissajous orbit close to the L1 Lagrange point (which lies between the Sun and the Earth at a distance of some 1.5 million km from the latter). The spacecraft is still in generally good condition, and has enough fuel to maintain its orbit until 2024. NASA Goddard Space Flight Center managed the development and integration of the ACE spacecraft. 

Instrumentation

• Cosmic Ray Isotope Spectrometer (CRIS): CRIS determines the isotope composition of galactic cosmic rays. It is designed to be sensitive enough to detect isotopes up to the range of zinc (Z-30).
• ACE Real Time Solar Wind (RTSW).
• Solar Wind Ion Mass Spectrometer (SWIMS) and Solar Wind Ion Composition Spectrometer (SWICS): These two instruments are time-of-flight mass spectrometers, each tuned for a different set of measurements. They analyze the chemical and isotopic composition of solar wind and interstellar matter.
• Ultra-Low Energy Isotope Spectrometer (ULEIS): ULEIS measures ion flux and is sensitive to a range from helium through nickel to determine the makeup of solar energetic particles and the mechanism by which the particles become charged by the sun.
• Solar Energetic Particle Ionic Charge Analyzer (SEPICA): As of 2008, this instrument is no longer functioning due to failed gas valves.
• Solar Isotope Spectrometer (SIS).
• Solar Wind Electron, Proton and Alpha Monitor (SWEPAM).
• Electron, Proton, and Alpha-particle Monitor (EPAM).
• Magnetometer (MAG).

Terra (EOS AM-1) is a multi-national NASA scientific research satellite in a sun-synchronous orbit around the Earth.^[1] It is the flagship of the Earth Observing System (EOS). The name "Terra" comes from the Latin word for Earth.

Launch

The satellite was launched from Vandenberg Air Force Base on December 18, 1999, aboard an Atlas IIAS vehicle and began collecting data on February 24, 2000.

 Mission

Terra carries a payload of five remote sensors designed to monitor the state of Earth's environment and ongoing changes in its climate system:

• ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer)
• CERES (Clouds and the Earth's Radiant Energy System)
• MISR (Multi-angle Imaging SpectroRadiometer)
• MODIS (Moderate-resolution Imaging Spectroradiometer)
• MOPITT (Measurements of Pollution in the Troposphere)

Data from the satellite helps scientists better understand the spread of pollution around the globe. Studies have used instruments on Terra to examine trends in global carbon monoxide and aerosol pollution. The data collected by Terra will ultimately become a new, 15-year global data set.

The Multi-angle Imaging SpectroRadiometer (MISR) is a scientific instrument on the Terra satellite launched by NASA on December 18, 1999. This device is designed to measure the intensity of solar radiation reflected by the Earth system (planetary surface and atmosphere) in various directions and spectral bands; it became operational in February 2000. Data generated by this sensor have been proven useful in a variety of applications including atmospheric sciences, climatology and monitoring terrestrial processes.

The MISR instrument consists of an innovative configuration of nine separate digital cameras that gather data in four different spectral bands of the solar spectrum. One camera points toward the nadir, while the others provide forward and aftward view angles at 26.1°, 45.6°, 60.0°, and 70.5°. As the instrument flies overhead, each region of the Earth's surface is successively imaged by all nine cameras in each of four wavelengths (blue, green, red, and near-infrared).

The data gathered by MISR are useful in climatological studies concerning the disposition of the solar radiation flux in the Earth's system. MISR is specifically designed to monitor the monthly, seasonal, and long-term trends of atmospheric aerosol particle concentrations including those formed by natural sources and by human activities, upper air winds and cloud cover, type, height, as well as the characterization of land surface properties, including the structure of vegetation canopies, the distribution of land cover types, or the properties of snow and ice fields, amongst many other biogeophysical variables.

The High Energy Transient Explorer (abbreviated HETE; also known as Explorer 79) was an American astronomical satellite with international participation (mainly Japan and France). The prime objective of HETE was to carry out the first multiwavelength study of gamma-ray bursts with UV, X-ray, and gamma-ray instruments mounted on a single, compact spacecraft. A unique feature of the HETE mission was its capability to localize GRBs with ~10 arc second accuracy in near real time aboard the spacecraft, and to transmit these positions directly to a network of receivers at existing ground-based observatories enabling rapid, sensitive follow-up studies in the radio, IR, and optical bands. The satellite bus for the first HETE was designed and built by AeroAstro, Inc. of Herndon, VA; the replacement satellite, HETE-2, was built by MIT based on the original HETE design.

Launch attempts

The first HETE was lost during the launch on Nov.4, 1996. The Pegasus rocket achieved a good orbit, but explosive bolts releasing HETE from another satellite (Argentina's SAC-B) and from its DPAF envelope failed to charge, dooming both satellites. A battery on the third stage of the rocket and responsible for these bolts cracked during the ascent.

A second HETE satellite, HETE-2, was launched on October 9, 2000 in a follow-up mission. It was similar to the first HETE, but replaced the UV camera with an additional X-ray camera (Soft X-ray Camera or SXC) capable of higher localization accuracy than the original X-ray instrument (Wide-Field X-ray Monitor or WXM).

The Robotic Optical Transient Search Experiment (ROTSE) is an multi-telescope experiment designed to observe the optical afterglow of gamma-ray bursts. The experiment currently consists of four telescopes located in Australia, Namibia, Turkey, and at the McDonald Observatory near Fort Davis, Texas.

The ROTSE project is a collaboration of astrophysicists from the University of Michigan, Los Alamos National Laboratory, Lawrence Livermore National Laboratory, the University of New South Wales (Australia) and the Max Planck Institute for Nuclear Physics (Germany).

The original ROTSE-I had 4 telephoto lenses of 11 cm aperture, covering a 16x16 degree field of view. This detected the first afterglow of a GRB while the burst was still ongoing, but this was the only burst detected by ROTSE or the very similar Livermore Optical Transient Imaging System. Therefore ROTSE-II was designed, also featuring a large field of view, but it was never built, since new satellites such as HETE-2 and SWIFT could provide smaller error boxes, making a huge field of view unnecessary. This led to the design of ROTSE-III, a more or less conventional telescope designed for fast slewing and operation at multiple locations around the world.

Venus Express (VEX) is the first Venus exploration mission of the European Space Agency. Launched in November 2005, it arrived at Venus in April 2006 and has been continuously sending back science data from its polar orbit around Venus. Equipped with seven science instruments, the main objective of the mission is the long term observation of the Venusian atmosphere. The observation over such long periods of time has never been done in previous missions to Venus, and is key to a better understanding of the atmospheric dynamics. It is hoped that such studies can contribute to an understanding of atmospheric dynamics in general, while also contributing to an understanding of climate change on Earth. The mission is currently funded by ESA through 31 December 2014.

Rosetta is a robotic spacecraft of the European Space Agency on a mission to study the comet 67P/Churyumov–Gerasimenko. Rosetta consists of two main elements:

• the Rosetta space probe;
• the Philae lander.

The spacecraft was launched on 2 March 2004 on an Ariane 5 rocket and will reach the comet by mid 2014. The space probe is intended to orbit and perform long-term exploration of the comet at close quarters. On 10 November 2014 the Philae lander will attempt to land and perform detailed investigations on the comet's surface. Both the probe and the lander carry a large complement of scientific experiments designed to complete the most detailed study of a comet ever attempted.

The probe is named after the Rosetta Stone, as it is hoped the mission will help form an idea of how the solar system looked before planets formed. The lander is named after the Nile island Philae where an obelisk was found that helped decipher the Rosetta Stone. The spacecraft has already performed two successful asteroid flyby missions on its way to the comet. In 2007 performed a Mars swingby (flyby), and returned images. The craft completed its fly-by of asteroid 2867 Šteins in September 2008 and of 21 Lutetia in July 2010, and is presently (2013) in hibernation and on-target for its final destination as of June 2013.

SMOS — the second Earth Explorer mission launched on November 2009 designed to measure Soil Moisture and Ocean Salinity.

The Soil Moisture and Ocean Salinity Satellite (SMOS) is a part of ESA's Living Planet Programme intended to provide new insights into Earth's water cycle and climate. In addition, it will provide better weather forecasting and will also monitor snow and ice accumulation.

Planck —  a  Cosmic Microwave Background explorer, after COBE & WMAP. launched in may 2009.

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.

The mission has a wide variety of scientific aims, including:

• High resolution detections of both the total intensity and polarization of the primordial CMB anisotropies
• Creation of a catalogue of galaxy clusters through the Sunyaev-Zel'dovich effect
• Observations of the gravitational lensing of the CMB, as well as the integrated Sachs–Wolfe effect
• Observations of bright extragalactic radio (active galactic nuclei) and infrared (dusty galaxy) sources
• Observations of the Milky Way, including the local interstellar medium, distributed synchrotron emission and measurements of the galactic magnetic field.
• Studies of the local Solar System, including planets, asteroids, comets and the zodiacal light.