The PLATO 2.0 mission

Rauer, H.; Catala, C.; Aerts, C.; Appourchaux, T.; Benz, W.; Brandeker, Alexis; Christensen‐Dalsgaard, J.; Deleuil, M.; Gizon, Laurent; Goupil, M. J.; Güdel, M.; Janot-Pacheco, E.; Mas-Hesse, J. M.; Pagano, I.; Piotto, G.; Pollacco, D.; Santos, Carlos A.; Smith, Alan M.; Suárez, J. C.; Szabo, Robert M.; Udry, S.; Adibekyan, V.; Alibert, Yann; Almenara, J. M.; Amaro-Seoane, Pau; Eiff, M. Ammler‐von; Asplund, Martin; Antonello, E.; Barnes, Stuart; Baudin, F.; Belkacem, K.; Bergemann, M.; Bihain, G.; Birch, A. C.; Bonfils, X.; Boisse, I.; Bonomo, A. S.; Borsa, F.; Brandão, I. M.; Brocato, E.; Brun, S.; Burleigh, M. R.; Burston, Raymond; Cabrera, J.; Cassisi, S.; Chaplin, W. J.; Charpinet, S.; Chiappini, Cristina; Church, Ross P.; Csizmadia, Sz.; Cunha, M. S.; Damasso, M.; Davies, Melvyn B.; Deeg, H. J.; Díaz, R. F.; Dreizler, S.; Dreyer, C.; Eggenberger, P.; Ehrenreich, D.; Eigmüller, Philipp; Erikson, A.; Farmer, Robert; Feltzing, Sofia; Fialho, Fábio; Figueira, P.; Forveille, T.; Fridlund, M.; García, R. A.; Giommi, P.; Giuffrida, G.; Godolt, M.; Silva, J. Gomes da; Granzer, T.; Grenfell, John Lee; Grötsch-Noels, A.; Günther, E.; Haswell, C. A.; Hatzes, A. P.; Hébrard, G.; Hekker, S.; Helled, Ravit; Heng, Kevin; Jenkins, Jon M.; Johansen, Anders; Khodachenko, M. L.; Kislyakova, K. G.; Kley, W.; Kolb, U.; Krivova, N. A.; Kupka, F.; Lämmer, H.; Lanza, A. F.; Lebreton, Y.; Magrin, Demetrio; Marcos-Arenal, P.; Marrese, P. M.; Marques, J. P.; Martins, J. H. C.; Mathis, S.; Mathur, S.; Messina, S.; Miglio, A.; Montalbán, J.; Montalto, M.; Monteiro, M. J. P. F. G.; Moradi, Hamed; Moravveji, E.; Mordasini, C.; Morel, Thierry; Mortier, A.; Nascimbeni, V.; Nelson, Richard P.; Nielsen, M. B.; Noack, Lena; Norton, A. J.; Ofir, A.; Oshagh, M.; Ouazzani, R. M.; Pápics, P. I.; Parro, Vanderlei Cunha; Petit, P.; Plez, B.; Poretti, E.; Quirrenbach, A.; Ragazzoni, Roberto; Raimondo, Gabriella; Rainer, M.; Reese, D. R.; Redmer, R.; Reffert, S.; Rojas-Ayala, Bárbara; Roxburgh, I. W.; Salmon, Sébastien; Santerne, A.; Schneider, Jean; Schou, J.; Schuh, S.; Schunker, Hannah; Válio, Adriana; Silvotti, R.; Skillen, I.; Snellen, I. A. G.; Sohl, F.; Sousa, S. G.; Sozzetti, A.; Stello, Dennis; Strassmeier, K. G.; Švanda, Michal; Szabó, Gy. M.; Tkachenko, A.; Valencia, Diana; Grootel, V. Van; Vauclair, S.; Ventura, P.; Wagner, F.W.; Walton, N. A.; Weingrill, J.; Werner, Stéphanie C.; Wheatley, P. J.; Zwintz, K.

doi:10.1007/s10686-014-9383-4

Cited by 1,051 publications

(622 citation statements)

References 359 publications

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“…Looking to the future, neither the upcoming NASA TESS Mission (Ricker et al 2014) nor the ESA PLATO Mission (Rauer et al 2014) are optimized for the study of densely populated stellar clusters. A space mission dedicated to the detection and study of oscillations in globular clusters should be considered.…”

Section: Summary and Future Prospectsmentioning

confidence: 99%

Detection of solar-like oscillations in relics of the Milky Way: asteroseismology of K giants in M4 using data from the NASA K2 mission

Miglio

Chaplin

Brogaard

et al. 2016

Mon. Not. R. Astron. Soc.

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116

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Asteroseismic constraints on K giants make it possible to infer radii, masses and ages of tens of thousands of field stars. Tests against independent estimates of these properties are however scarce, especially in the metal-poor regime. Here, we report the detection of solar-like oscillations in 8 stars belonging to the red-giant branch and red-horizontal branch of the globular cluster M4. The detections were made in photometric observations from the K2 Mission during its Campaign 2. Making use of independent constraints on the distance, we estimate masses of the 8 stars by utilising different combinations of seismic and non-seismic inputs. When introducing a correction to the ∆ν scaling relation as suggested by stellar models, for RGB stars we find excellent agreement with the expected masses from isochrone fitting, and with a distance modulus derived using independent methods. The offset with respect to independent masses is lower, or comparable with, the uncertainties on the average RGB mass (4 − 10%, depending on the combination of constraints used). Our results lend confidence to asteroseismic masses in the metal poor regime. We note that a larger sample will be needed to allow more stringent tests to be made of systematic uncertainties in all the observables (both seismic and non-seismic), and to explore the properties of RHB stars, and of different populations in the cluster.

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Section: Summary and Future Prospectsmentioning

confidence: 99%

Detection of solar-like oscillations in relics of the Milky Way: asteroseismology of K giants in M4 using data from the NASA K2 mission

Miglio

Chaplin

Brogaard

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

116

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“…Our ability to measure the internal rotation of Sun-like stars is limited by the S /N in the Kepler observations. The PLATO mission (Rauer et al 2014) promises to change this. Currently the selection of bright Sun-like stars observed in short cadence by Kepler number in the few tens.…”

Section: Resultsmentioning

confidence: 99%

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

Nielsen

2017

Springer Theses

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“…In addition, eclipses can be used to spatially resolve the day-side hemisphere. During ingress and egress, the partial occultation effectively maps the photospheric emission region of the planet [128]. Figure 12 illustrates the results from eclipse mapping observations [107].…”

Section: Transits Eclipses and Phase-curvesmentioning

confidence: 97%

The EChO science case

et al. 2015

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The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune-all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10 −4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R~300 for wavelengths less than 5 μm and R~30 for wavelengths greater than this. spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m 2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m 2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate tha...

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The PLATO 2.0 mission

Abstract: International audienc

Cited by 1,051 publications

References 359 publications

Detection of solar-like oscillations in relics of the Milky Way: asteroseismology of K giants in M4 using data from the NASA K2 mission

Detection of solar-like oscillations in relics of the Milky Way: asteroseismology of K giants in M4 using data from the NASA K2 mission

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

The EChO science case

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