The Science Working Team has selected the first PLATO Long-duration Observation Phase (LOP) field. The name of the field is LOPS2 and its centre coordinates in the equatorial, galactic, and ecliptic reference frames are given in the Table below. LOPS2 field centre coordinates α [hms] 06:21:14.5 ICRS (J2000) δ [dms] -47:53:13 ICRS (J2000) l [deg] 255.9375 IAU 1958 b [deg]…
Download PLATO and the search for planets in the habitable zone as pdf document.
With the imminent launch of the Transiting Exoplanet Survey Satellite (TESS), it is useful to remind ourselves of the similarities…
Planet detection and characterisation R-SCI-L0-01 PLATO shall detect and characterise hundreds of planets around dwarf and subgiant stars of spectral…
These requirements provide the specification of the mission capabilities, and are derived from the high-level science requirements. R-SCI-035 The capability…
R-SCI-290 The payload shall provide high precision photometric time series in the wavelength band of 500 nm to 1000 nm….
“Gaps” are defined as time during which science observations are suspended while other spacecraft operations are performed. R-SCI-400 During nominal…
PLATO is a transit survey mission with the goal of detecting and providing bulk characterisation for new planets and planetary…
Since the discovery of the first extrasolar planet orbiting a solar type star in 1995 (Mayor & Queloz 1995), just…
A prime goal of PLATO will be to detect a large number of planets, down to the terrestrial regime in…
Habitability is defined as the potential of an environment to sustain life of any kind (e.g. Steele et al. 2006)….
PLATO will answer fundamental questions about planetary formation such as: What is the bulk density distribution of low-mass, terrestrial planets?…
PLATO will explore the diversity of planetary system by accurately determining their bulk properties, by constraining planet formation models, and…
One of the major findings of Kepler is the catalogue of multiple-planet transiting systems (see Lissauer et al. 2014). Multiple systems…
What can be learned from accurate radii and masses of terrestrial exoplanets, in spite of the limitations in observables compared…
PLATO will address the following questions regarding gas and ice planets: Up to which orbital distance do we find inflated…
It is now well established that planets form within a few million years from the dusty, circumstellar disk of young…
Several ground-based Doppler planet searches target sub-giant and giant stars instead of main-sequence stars. The number of planets known to…
To date not a single bona fide planet has been identified orbiting an isolated white dwarf (e.g. Hogan et al….
Planets that orbit around both components of a stellar binary were suggested as favourable targets for transit surveys (Borucki 1984)…
The ability to derive the age of planetary systems is one of the key assets of PLATO. The age of…
Numerous studies have been published on the use of wavelength-dependent primary transits and secondary eclipses to characterise the atmospheres of…
Transit observations of exoplanets around bright host stars, together with advanced numerical modelling techniques and known astrophysical parameters (such as…
The combination of high-precision photometry, large number of planets, and well-characterised host stars that will be provided by PLATO will…
Asteroseismology is the study of the global oscillations of stars (see Aerts et al. 2010, Chaplin & Miglio 2013). These oscillations…
The main focus of the asteroseismology programme of PLATO will be to support exoplanet science by providing: stellar masses with…
With sufficiently good data, the asteroseismic determination of mass and radius can be essentially independent of stellar models. For other…
All stars rotate and many exhibit complex surface magnetic fields and activity. Coupled with the presence of turbulent convective envelopes…
In addition to its focus on relatively bright stars, one major advantage of PLATO over the CoRoT and Kepler space missions…
The PLATO’s catalogue of thousands of characterised planets and between 300,000 and ~1,000,000 high precision stellar light curves (depending on…
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