PLATO (spacecraft)

From Wikipedia, the free encyclopedia
Jump to: navigation, search
PLATO
Mission type Space observatory
Operator ESA
Website sci.esa.int/plato/
Mission duration 6 years[1]
Spacecraft properties
Manufacturer To be decided in 2016
Start of mission
Launch date Planned for 2024
Rocket Soyuz-ST
Launch site Kourou ELS
Contractor Arianespace
Orbital parameters
Reference system Sun–Earth L2
Main telescope
Type Multiple refractors[2]
Collecting area 2250 deg2 [4]
Wavelengths Visible spectrum:[3] 390 to 700 nm

Planetary Transits and Oscillations of stars (PLATO) is a space observatory under development by the European Space Agency for launch around 2024. PLATO will use a group of photometers to search for planet transits, to discover and characterize rocky extrasolar planets of all sizes around red dwarf stars, yellow dwarf stars like our Sun, and subgiant stars where water can exist in liquid state.[5] A secondary objective is to study stellar oscillations to measure stellar masses and evolution.

History[edit]

PLATO was proposed in 2007 to European Space Agency (ESA) by a team of scientists in response to the call for ESA Cosmic Vision 2015–2025.[6] The assessment phase was completed during 2009, and in May 2010 it entered the Definition Phase. Following a call for missions in July 2010, ESA selected in February 2011 four candidates for a medium-class mission (M3 mission) for a launch opportunity in 2024.[6][7] PLATO was announced on 19 February 2014 as the selected M3 class science mission for implementation as part of its Cosmic Vision Programme. Other competing concepts that were studied included the four candidate missions EChO, LOFT, MarcoPolo-R and STE-QUEST.[1]

The design of the Telescope Optical Units is by an international team from Italy, Switzerland and Sweden and coordinated by Roberto Ragazzoni at INAF (Istituto Nazionale di Astrofisica) Osservatorio Astronomico di Padova. The design and development is funded by Italian Space Agency, Swiss Space Office and the Swedish National Space Board.[2]

In January 2015 Thales Alenia Space was selected to conduct one out of three phase B1 studies for PLATO, defining the system, subsystem and payload aspects of the observatory.[8]

PLATO is an acronym, but also the name of a philosopher in Classical Greece; Plato (428–348 BC) was looking for a physical law accounting for the orbit of planets (errant stars) and able to satisfy the philosopher's needs for "uniformity" and "regularity".[6]

Objective[edit]

The goal is to find planets like Earth, not just in terms of their size but in their potential for habitability.[5] By using 34 separate small telescopes and cameras, PLATO will search for planets around up to one million stars.[1] The main objective of PLATO is to elucidate the conditions for planet formation and the emergence of life.[3] To achieve this objective, the mission has these goals:[3]

  • Discover and characterise a large number of close-by exoplanetary systems, with a precision in the determination of the planet mass up to 10%, of planet radius of up to 2%, and of stellar age up to 10%.
  • Detect Earth-sized planets in the habitable zone around solar-type stars
  • Detect super-Earths in the habitable zone around solar-type stars
  • Measure solar oscillations in the host stars of exoplanets
  • Measure oscillations of classical pulsators

Optics[edit]

The PLATO payload is based on a multi-telescope approach, involving a set of 32 "normal cameras" working at a readout cadence of 25 sec and monitoring stars fainter than mV = 8 (apparent visual magnitude), plus two "fast cameras" working at a cadence of 2.5 sec, and observing stars in the magnitude range 4 to 8.[4][9] The cameras are based on a fully dioptric telescope including 6 lenses; each camera has an 1100 deg2 field, and a pupil diameter of 120 mm. Each camera is equipped with its own CCD focal plane array, consisting of 4 CCDs with 4510 x 4510 pixels.[4]

The 32 'normal cameras' will be arranged in four groups of 8 cameras with their lines of sight offset by a 9.2° angle from the +ZPLM axis. This particular configuration allows surveying a total field of about 2250 deg2 per pointing. The satellite will be rotated around the mean line of sight by 90° every 3 months, for a continuous survey of exactly the same region of the sky.[4]

PLATO will differ from COROT and Kepler space telescopes in that it will study relatively bright stars (between magnitudes 4 and 10), making it easier to confirm extrasolar planets and measure their masses using follow-up radial velocity measurements on ground-based telescope. It will have a much larger field of view than the Kepler mission (which has 100 deg2) allowing PLATO to study a larger sample and brighter stars.

Launch[edit]

The satellite is planned to launch in 2024 from Guiana Space Centre with a Soyuz rocket to the Earth-Sun L2 Lagrangian point.[1]

See also[edit]

References[edit]

  1. ^ a b c d "ESA selects planet-hunting PLATO mission". European Space Agency. Retrieved 19 February 2014. 
  2. ^ a b "PLATO - Camera Telescope Optical Units". INAF- Osservatorio Astrofisico di Catania. 2014. Retrieved 20 February 2014. 
  3. ^ a b c "PLATO Mission Summary". European Space Agency. ESA. 19 February 2014. Retrieved 19 February 2014. 
  4. ^ a b c d Pagano, Isabella. "The PLATO 2.0 Payload Module". INAF- Osservatorio Astrofisico di Catania. Retrieved 20 February 2014. 
  5. ^ a b Amos, Jonathan (29 January 2014). "Plato planet-hunter in pole position". BBC News. Retrieved 2014-01-29. 
  6. ^ a b c Isabella Pagano (2014). "PLATO 2.0". INAF- Osservatorio Astrofisico di Catania. Retrieved 20 February 2014. 
  7. ^ Cosmic Vision M3 candidate missions presentation event. Announcement and registration. (21 January 2014)
  8. ^ "ESA Selects Thales Alenia Space for PLATO Phase B1 Study". Via Satellite. 12 January 2015. Retrieved 1 August 2015. 
  9. ^ PLATO: detailed design of the telescope optical units. Authors: D. Magrin, Ma. Munari, I. Pagano, D. Piazza, R. Ragazzoni, et al., in Space Telescopes and Instrumentation 2010: Optical, Infrared, and Millimeter Wave, Edited by Oschmann, Jacobus M., Jr.; Clampin, Mark C.; MacEwen, Howard A. Proceedings of the SPIE, Volume 7731, pp. 773124-8 (2010)

External links[edit]