Advanced

The PLATO 2.0 mission

Rauer, H.; Catala, C.; Aerts, C.; Appourchaux, T.; Benz, W.; Brandeker, A.; Christensen-Dalsgaard, J.; Deleuil, M.; Gizon, L. and Goupil, M. -J., et al. (2014) In Experimental Astronomy 38(1-2). p.249-330
Abstract
PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 s readout cadence and 2 with 2.5 s cadence) providing a wide field-of-view (2232 deg(2)) and a large photometric magnitude range (4-16 mag). It focuses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by... (More)
PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 s readout cadence and 2 with 2.5 s cadence) providing a wide field-of-view (2232 deg(2)) and a large photometric magnitude range (4-16 mag). It focuses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2 %, 4-10 % and 10 % for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50 % of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0. The PLATO 2.0 catalogue allows us to e. g.: - complete our knowledge of planet diversity for low-mass objects, - correlate the planet mean density-orbital distance distribution with predictions from planet formation theories,- constrain the influence of planet migration and scattering on the architecture of multiple systems, and - specify how planet and system parameters change with host star characteristics, such as type, metallicity and age. The catalogue will allow us to study planets and planetary systems at different evolutionary phases. It will further provide a census for small, low-mass planets. This will serve to identify objects which retained their primordial hydrogen atmosphere and in general the typical characteristics of planets in such a low-mass, low-density range. Planets detected by PLATO 2.0 will orbit bright stars and many of them will be targets for future atmosphere spectroscopy exploring their atmospheres. Furthermore, the mission has the potential to detect exomoons, planetary rings, binary and Trojan planets. The planetary science possible with PLATO 2.0 is complemented by its impact on stellar and galactic science via asteroseismology as well as light curves of all kinds of variable stars, together with observations of stellar clusters of different ages. This will allow us to improve stellar models and study stellar activity. A large number of well-known ages from red giant stars will probe the structure and evolution of our Galaxy. Asteroseismic ages of bright stars for different phases of stellar evolution allow calibrating stellar age-rotation relationships. Together with the results of ESA's Gaia mission, the results of PLATO 2.0 will provide a huge legacy to planetary, stellar and galactic science. (Less)
Please use this url to cite or link to this publication:
author
, et al. (More)
(Less)
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
Exoplanets, Asteroseismology, Transit survey, Stellar science, Exoplanetary science
in
Experimental Astronomy
volume
38
issue
1-2
pages
249 - 330
publisher
Springer
external identifiers
  • wos:000345385300010
  • scopus:84943014904
ISSN
0922-6435
DOI
10.1007/s10686-014-9383-4
language
English
LU publication?
yes
id
7c00bab0-37e5-44ae-8844-6956a07b4a25 (old id 4979450)
date added to LUP
2015-01-27 13:48:55
date last changed
2017-11-19 03:17:33
@article{7c00bab0-37e5-44ae-8844-6956a07b4a25,
  abstract     = {PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 s readout cadence and 2 with 2.5 s cadence) providing a wide field-of-view (2232 deg(2)) and a large photometric magnitude range (4-16 mag). It focuses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2 %, 4-10 % and 10 % for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50 % of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0. The PLATO 2.0 catalogue allows us to e. g.: - complete our knowledge of planet diversity for low-mass objects, - correlate the planet mean density-orbital distance distribution with predictions from planet formation theories,- constrain the influence of planet migration and scattering on the architecture of multiple systems, and - specify how planet and system parameters change with host star characteristics, such as type, metallicity and age. The catalogue will allow us to study planets and planetary systems at different evolutionary phases. It will further provide a census for small, low-mass planets. This will serve to identify objects which retained their primordial hydrogen atmosphere and in general the typical characteristics of planets in such a low-mass, low-density range. Planets detected by PLATO 2.0 will orbit bright stars and many of them will be targets for future atmosphere spectroscopy exploring their atmospheres. Furthermore, the mission has the potential to detect exomoons, planetary rings, binary and Trojan planets. The planetary science possible with PLATO 2.0 is complemented by its impact on stellar and galactic science via asteroseismology as well as light curves of all kinds of variable stars, together with observations of stellar clusters of different ages. This will allow us to improve stellar models and study stellar activity. A large number of well-known ages from red giant stars will probe the structure and evolution of our Galaxy. Asteroseismic ages of bright stars for different phases of stellar evolution allow calibrating stellar age-rotation relationships. Together with the results of ESA's Gaia mission, the results of PLATO 2.0 will provide a huge legacy to planetary, stellar and galactic science.},
  author       = {Rauer, H. and Catala, C. and Aerts, C. and Appourchaux, T. and Benz, W. and Brandeker, A. and Christensen-Dalsgaard, J. and Deleuil, M. and Gizon, L. and Goupil, M. -J. and Guedel, M. and Janot-Pacheco, E. and Mas-Hesse, M. and Pagano, I. and Piotto, G. and Pollacco, D. and Santos, N. C. and Smith, A. and Suarez, J. -C. and Szabo, R. and Udry, S. and Adibekyan, V. and Alibert, Y. and Almenara, J. -M. and Maro-Seoane, P. A. and Ammler-von Eiff, M. and Asplund, M. and Antonello, E. and Barnes, S. and Baudin, F. and Belkacem, K. and Bergemann, M. and Bihain, G. and Birch, A. C. and Bonfils, X. and Boisse, I. and Bonomo, A. S. and Borsa, F. and Brandao, I. M. and Brocato, E. and Brun, S. and Burleigh, M. and Burston, R. and Cabrera, J. and Cassisi, S. and Chaplin, W. and Charpinet, S. and Chiappini, C. and Church, Ross and Csizmadia, Sz. and Cunha, M. and Damasso, M. and Davies, Melvyn B and Deeg, H. J. and Diaz, R. F. and Dreizler, S. and Dreyer, C. and Eggenberger, P. and Ehrenreich, D. and Eigmueller, P. and Erikson, A. and Farmer, R. and Feltzing, Sofia and de Oliveira Fialho, F. and Figueira, P. and Forveille, T. and Fridlund, M. and Garcia, R. A. and Giommi, P. and Giuffrida, G. and Godolt, M. and Gomes da Silva, J. and Granzer, T. and Grenfell, J. L. and Grotsch-Noels, A. and Guenther, E. and Haswell, C. A. and Hatzes, A. P. and Hebrard, G. and Hekker, S. and Helled, R. and Heng, K. and Jenkins, J. M. and Johansen, Anders and Khodachenko, M. L. and Kislyakova, K. G. and Kley, W. and Kolb, U. and Krivova, N. and Kupka, F. and Lammer, H. and Lanza, A. F. and Lebreton, Y. and Magrin, D. and Marcos-Arenal, P. and Marrese, P. M. and Marques, J. P. and Martins, J. and Mathis, S. and Mathur, S. and Messina, S. and Miglio, A. and Montalban, J. and Montalto, M. and Monteiro, M. J. P. F. G. and Moradi, H. and Moravveji, E. and Mordasini, C. and Morel, T. and Mortier, A. and Nascimbeni, V. and Nelson, R. P. and Nielsen, M. B. and Noack, L. and Norton, A. J. and Ofir, A. and Oshagh, M. and Ouazzani, R. -M. and Papics, P. and Parro, V. C. and Petit, P. and Plez, B. and Poretti, E. and Quirrenbach, A. and Ragazzoni, R. and Raimondo, G. and Rainer, M. and Reese, D. R. and Redmer, R. and Reffert, S. and Rojas-Ayala, B. and Roxburgh, I. W. and Salmon, S. and Santerne, A. and Schneider, J. and Schou, J. and Schuh, S. and Schunker, H. and Silva-Valio, A. and Silvotti, R. and Skillen, I. and Snellen, I. and Sohl, F. and Sousa, S. G. and Sozzetti, A. and Stello, D. and Strassmeier, K. G. and Svanda, M. and Szabo, Gy. M. and Tkachenko, A. and Valencia, D. and Van Grootel, V. and Vauclair, S. D. and Ventura, P. and Wagner, F. W. and Walton, N. A. and Weingrill, J. and Werner, S. C. and Wheatley, P. J. and Zwintz, K.},
  issn         = {0922-6435},
  keyword      = {Exoplanets,Asteroseismology,Transit survey,Stellar science,Exoplanetary science},
  language     = {eng},
  number       = {1-2},
  pages        = {249--330},
  publisher    = {Springer},
  series       = {Experimental Astronomy},
  title        = {The PLATO 2.0 mission},
  url          = {http://dx.doi.org/10.1007/s10686-014-9383-4},
  volume       = {38},
  year         = {2014},
}