Science&Program,&Abstracts,& List&of&Participants& · PLATO&2.0!! Science&Conference! Ta♉rmina,’3"5"December"2014!!!!! Science&Program,&Abstracts,& List&of&Participants&!!

PLATO 2.0 Science Conference Ta♉rmina, 3-‐5 December 2014

Science Program, Abstracts, List of Participants

PLATO 2.0 Science Conference, Ta♉rmina, 3-5 December 2014

2

Contents Scientific Program ..................................................................................................................................................... 5 Abstracts ...................................................................................................................................................................... 10 Session A -‐ The PLATO Mission and Current Status ............................................................................... 10 Heras, A. & Colangeli, L. -‐ PLATO as M3 mission in ESA's Cosmic Vision plan ....................... 10 Hatzes, A. -‐ Exoplanets in the 2020’s ........................................................................................................ 10 Rauer, H. -‐ The PLATO Mission -‐ Overview ............................................................................................ 10 Gondoin, P. -‐ PLATO spacecraft, payload and mission operation concept ............................... 10 Gizon, L. -‐ PLATO Data Centre ...................................................................................................................... 10

Session B -‐ Planet formation and evolution ................................................................................................ 11 Alibert, Y. -‐ Planetary system formation and composition: statistics on low mass planets ................................................................................................................................................................................... 11 Nelson, R. P. -‐ Formation and orbital evolution of planetary systems ....................................... 11 Mardling, R. -‐ The star-‐planet tidal link ................................................................................................... 12 Laskar, J. -‐ How to characterize multi-‐planet systems ...................................................................... 12 Nascimbeni, V. -‐ TTVs: from Observations to Understanding ....................................................... 12 Church, R.P. -‐ Deducing inclinations of transiting multi-‐planet systems .................................. 12 Mordasini, C. -‐ Time: a new dimension of constraints for planet formation and evolution theory ..................................................................................................................................................................... 13 Zwintz, K. -‐ Stellar structure across the HR diagram ......................................................................... 13 White, T.R. -‐ What Interferometry will do for PLATO ....................................................................... 13

Session C -‐ PLATO Stars and Planets ............................................................................................................. 14 Piotto, G. -‐ PLATO target and field selection .......................................................................................... 14 Goupil, M. J. -‐ Asteroseismology with Plato ............................................................................................ 14 Cabrera, J. -‐ The planet detection pipeline of PLATO 2.0: overview and challenges ............ 14 Deleuil, M. -‐ PLATO candidates selection and ranking ...................................................................... 14 Udry, S. -‐ PLATO Follow-‐Up challenges ................................................................................................... 15 Santos, N. C. -‐ Deriving stellar parameters ............................................................................................. 15 Gaidos, E. -‐ Properties of Very Cool Stars and their Planets: The Kepler Experience and the PLATO Promise .......................................................................................................................................... 15 Kolb, U. -‐ Binary population models of PLATO 2.0 fields ................................................................. 15 Santerne, A. -‐ Minimising the needs of follow-‐up observations for PLATO : the central role of planet-‐validation tool ................................................................................................................................. 16

Session D -‐ Giant and Terrestrial Planets .................................................................................................... 16 Sohl, F. -‐ Terrestrial planet mass-‐radius and composition ............................................................. 16 Guillot, T. -‐ Giant planet mass radius relationship and their compositions ............................. 17 Deeg, H.J. -‐ Circumbinary Planets ............................................................................................................... 17 Kislyakova, K. -‐ Star-‐planet interaction and planetary characterization methods ............... 17 Ehrenreich, D. -‐ Atmospheres of PLATO planets ................................................................................. 18 Burleigh, M.R. -‐ Eclipses, transits and intrinsic variability of white dwarfs with PLATO 2.0 ................................................................................................................................................................................... 18 Haswell, C.A. -‐ Do extremely close-‐in transiting planets hold the key to learning exoplanet compositions? ..................................................................................................................................................... 19 Noack, L. -‐ Terrestrial planets vs. water worlds: characterization and habitability limitations ............................................................................................................................................................. 19 Szabó, Gy. M. -‐ An occurrence-‐weighted searching strategy for exomoons ............................ 20


3

Rodríguez-‐López, C. -‐ CARMENES: Radial velocity follow-‐up and characterization of PLATO targets ..................................................................................................................................................... 20

Session E -‐ Stellar and Other Science ............................................................................................................. 21 Chaplin, W.J. -‐ Prospects for studies of solar-‐type stars with PLATO ......................................... 21 Miglio, A. -‐ Red-‐Giants and Galactic Structure ...................................................................................... 21 Tkachenko, A. -‐ Binary stars in the era of space-‐based missions ................................................. 22 Campante, T. L. -‐ An ancient extrasolar system with five terrestrial-‐size planets ................ 22 Cassisi, S. -‐ Improving our understanding of stellar evolution with PLATO ........................... 23 Nielsen, M. B. -‐ Constraints on the radial differential rotation for six Sun-‐like stars .......... 23 Reese, D. R. -‐ SpaceInn hare-‐and-‐hounds exercise ............................................................................. 23 Ball, W. H. -‐ A new correction of stellar oscillation frequencies for near-‐surface effects .. 24 Buldgen, G. -‐ Asteroseismic inversions in the context of the Plato mission ............................ 24

Session F -‐ PLATO's Contribution to Exoplanet studies ........................................................................ 24 Pagano, I. -‐ Synergy with other facilities: CHEOPS, TESS, JWST and E-‐ELT ............................. 24 Sozzetti, A. -‐ On the Gaia -‐ PLATO Synergy ............................................................................................. 25

Posters contributions .......................................................................................................................................... 26 (A) Alonso R. -‐ The phase curve of Kepler-‐7b ....................................................................................... 26 (B) Ammler-‐von Eiff, M. -‐ Low-‐resolution spectroscopy in the ground-‐based follow-‐up of planet candidates -‐ lessons learned from CoRoT ................................................................................ 26 (C) Bensmaïa, M.K. -‐ Time-‐Dependent Convection asteroseismic modelling of β Hydri ... 26 (D) Bonfanti, A. -‐ The ages of stars-‐hosting planets ........................................................................... 27 (E) Boué, G. -‐ On the origin of stellar spin-‐orbit angle in extrasolar systems ......................... 27 (F) Cegla, H. M -‐ Disentangling Low-‐mass Planetary Signals and Stellar Surface Magneto-‐convection in Spectroscopic Observations ............................................................................................ 27 (G) Corsaro, E. -‐ Towards an efficient full asteroseismic characterization of a large number of planet-‐host stars ......................................................................................................................... 28 (H) Cosmovici, C. -‐ Search for Water in exoplanetary Systems by means of ground-‐based Radiospectrometry ........................................................................................................................................... 28 (I) Csizmadia, Sz. -‐ Precise planet parameters with PLATO ........................................................... 28 (J) Cunha, M.S. -‐ Oscillations in g-‐mode period spacings in red giants as a way to determine their state of evolution ............................................................................................................. 29 (K) de Jong, Roelof S. -‐ 4MOST spectroscopic host star characterisation for PLATO .......... 29 (L) do Nascimento, J. D. -‐ Rotation Periods and ages of solar Twins revealed by the kepler mission: A roadmap for PLATO ages ........................................................................................................ 29 (M) Debski, B. -‐ Light Curve Morphology: a tool for PLATO 2.0 for studying extreme close binaries .................................................................................................................................................................. 30 (N) Di Mauro, M. P. -‐ A synergic strategy to identify habitable exoplanets ............................. 30 (O) García Muñoz, A. -‐ Steps towards the interpretation of exoplanet phase curves .......... 30 (P) Garrido, R. -‐ An information preserving method for filling gaps in time series ............. 30 (Q) Giuffrida, G. -‐ Gaia and PLATO 2.0 in ASDC .................................................................................... 31 (R) Iro, N. -‐ Exoplanet atmosphere modelling ...................................................................................... 31 (S) Janot-‐Pacheco, E. -‐ Atmospheric Biosignatures on Earth and Exoplanets by Spectroscopic Techniques ............................................................................................................................. 31 (T) Klagyivik, P. -‐ Cluster formation and evolution as will be seen by PLATO: experiences with eclipsing binaries in NGC 2264 ......................................................................................................... 32 (U) Krticka, J. -‐ High precision photometry as a test of stellar model atmospheres and evolution theory ................................................................................................................................................ 32 (V) Mecheri, R. -‐ A convenient system of first order ODEs describing the oscillations of rapidly rotating stars ....................................................................................................................................... 33


4

(W) Morel, T. -‐ Uncertainty in stellar radii for PLATO2.0 targets based on Gaia data ........ 33 (X) Nelson, R. P. -‐ Formation and orbital evolution of planetary systems ............................... 33 (Y) Norton, A. J. -‐ Detecting non-‐transiting planets in transiting planet surveys .................. 34 (Z) Oshagh, M. -‐ Effect of stellar activity on the high-‐precision transmission spectra ....... 34 (AA) Paetzold, M. -‐ Wavelet based filter methods for the detection of small transiting planets: application to Kepler light curves ............................................................................................ 34 (BB) Paparo, M. -‐ Impact of CoRoT asteroseismology to Plato planet-‐hosting stars. Massive sample of large separations in Delta Scuti stars. ............................................................... 35 (CC) Peres, G. -‐ The residual X-‐ray emission in Venus shadow ..................................................... 36 (DD) Ragazzoni, R. -‐ PLATO Telescope Optical Units: design and evolution ........................... 36 (EE) Suran, M. D. -‐ ROMOSC Asteroseismic data interpretation pipeline ................................. 36 (FF) Salmon, S. J. A. J. -‐ What can we learn from the asteroseismology of β Cephei stars through the forward approach .................................................................................................................... 36 (GG) Schou, J. -‐ On the surface effect in Sun-‐like stars ...................................................................... 37 (HH) Sódor, Á. -‐ Studying hybrid delta Scuti-‐gamma Doradus pulsators by space photometry .......................................................................................................................................................... 37 (II) Turck-‐Chièze, S. -‐ Improving stellar modelling ............................................................................ 37 (JJ) Valio, A. -‐ Determination of Stellar Rotation through starspots ........................................... 38 (KK) Voss, H. -‐ Scientific capabilities of the Gaia UB team applicable to PLATO 2.0 ............ 38

List of participants ................................................................................................................................................. 39


5

Scientific Program

3 December 2014

09:15 - 09:30 Welcome and Introduction Session A - The PLATO Mission and Current Status (Chair: Don Pollacco)

Invited talks 09:30 - 09:50 ESA Overview L. Colangeli/A. Heras 09:50 - 10:20 Exoplanets in the 2020's Artie Hatzes 10:20 - 11:00 PLATO Overview Heike Rauer 11:00 – 11:20 Coffee

11:20 - 11:40 PLATO Payload Philippe Gondoin 11:40 - 12:00 PLATO Data Centre Laurent Gizon 12:00 - 12:30 Discussion (lead H. Rauer) 12:30 - 14:00 Lunch Session B - Planet formation and evolution (Chair: Stephane Udry) Invited talks 14.00 - 14:20 Planet population studies Yann Alibert 14:20 - 14:40 Evolution and Migration Richard Nelson 14:40 - 15:00 Short-period planetary systems and their secrets Rosemary Mardling 15:00 - 15:20 How to characterize multi-planet systems Jacques Laskar 15:20 - 15:40 TTVs: from Observations to Understanding Valerio Nascimbeni 15:40 - 16:00 Coffee Contributed talks 16:00 - 16:15 Deducing Inclinations of Transiting Multi-Planet

Systems Ross Church 16:15 - 16:30 Time: A New Dimension of Constraints for Planet

Formation and Evolution History Christoph Mordasini

Invited talks 16:30 - 16:50 Stellar structure across the HR diagram Konstanze Zwintz

Contributed talks 16:50 - 17:05 What Interferometry Will Do for PLATO Timothy White 17:05 - 17:35 Discussion (lead R. Nelson)


6

17:45 - 19:30 PLATO 2.0 Board Meeting

4 December 2014 Session C - PLATO Stars and Planets (Chair: Isabella Pagano) Invited talks 09:00 - 09:20 The PLATO Input Catalogue Giampaolo Piotto 09:20 - 09:40 PLATO Asteroseismology Marie-Jo Goupil 09:40 - 10:10 Stellar Activity and transit Hunting J. Cabrera/A. F. Lanza 10:10 - 10:25 Candidate Selection/Ranking Magali Deleuil 10:25 - 10:45 Follow up of PLATO Planet Candidates Stephane Udry 10:45 - 11:05 Deriving stellar parameters Nuno Santos 11:05 -11:25 Coffee Contributed talks 11:25 - 11:40 Properties of Very Cool Stars and their Planets: The

Kepler Experience and the PLATO Promise Eric Gaidos 11:40 - 11:55 Binary Population Models of PLATO Fields Ulrich Kolb

11:55 - 12:10 Minimizing the Needs of Follow-up Observations for PLATO: The central Role of Planet Validation Tool Alexander Santerne

12:10- 12:40 Discussion (lead S. Udry) 12:40- 13:50 Lunch 13:50 – 15:30 Visit to the Taormina Ancient Greek Theatre Session D - Giant and Terrestrial Planets (Chair: Richard Nelson) Invited talks 15:30 - 15:50 Terrestrial planet mass-radius and composition Frank Sohl 15:50 - 16:10 Giant planet mass-radius and composition Tristan Guillot 16:10 - 16:30 Circumbinary Planets Hans Deeg 16:30 - 16:50 Star-planet interaction Kristina Kislyakova 16:50 - 17:10 Atmospheres of PLATO Planets David Ehrenreich 17:10 - 17:30 Coffee Contributed talks 17:30 - 17:45 Eclipses, Transits and Intrinsic variability of White

Dwarfs with PLATO Matthew Burleigh 17:45 - 18:00 Do extremely Close-in Transiting Planets Hold the Key

to Learning Exoplanet Compositions Carole Haswell 18:00 - 18:15 Terrestrial Planets vs. Water Worlds: Characterisation

and Habitability Limitation Lena Noack

18:15 - 18:30 An Occurrence Weighted Searching Strategy for Exomoons Gyula Szabó


7

18:30 - 19:00 Discussion (lead T. Guillot) 20:30 Social dinner

5 December 2014 Session E - Stellar and Other Science (Chair: Nuno Santos) Invited talks 09:30 - 10:00 Sun-like stars William Chaplin 10:00 - 10:15 Red-Giants and Galactic Structure Andrea Miglio 10:15 - 10:30 Binary Stars Andrew Tkachenko

Contributed talks 10:30 - 10:45 An Ancient extrasolar System with Five Terrestrial sized

planets Tiago Campante 10:45 - 11:05 Coffee 11:05- 11:20 Improving Our Understand of Stellar Evolution with

PLATO Santi Cassisi 11:20- 11:35 Constraints on the Radial Differential Rotation of Six Sun-

Like Stars Martin Bo Nielsen 11:35 -11:50 SpaceInn hare-and-hounds Exercise Daniel Reese 11:50 -12:05 A new Correction for Stellar Oscillation Frequencies for

surface effects Warrick Ball 12:05 -12:20 Asteroseismic Inversions in the Context of PLATO Gaël Buldgen 12:20 -12:50 Discussion (lead N. Santos) 12:50 -14:30 Lunch Session F - PLATO's Contribution to Exoplanet studies (Chair: Heike Rauer) Invited talks 14:30 - 15:10 Synergy with other facilities: CHEOPS, TESS, JWST

and E-ELT Isabella Pagano

Contributed talks 15:10 - 15:30 Synergy with Gaia Alessandro Sozzetti 15:30 - 16:10 Discussion (lead PSAT) 16:10 - 16:30 Coffee 16:30 END


8

Poster Contributions

A. Alonso, R., et al., The phase curve of Kepler-7b

B. Ammler-von Eiff, M., et al., Low-resolution spectroscopy in the ground-based follow-up of planet candidates - lessons learned from CoRoT

C. Bensmaïa, M. K., et al., Time-Dependent Convection asteroseismic modelling of β Hydri

D. Bonfanti, A., et al., Analysis of the ages of the stars with planets

E. Boué, G., On the origin of stellar spin-orbit angle in extrasolar systems

F. Cegla, H. M., et al., Disentangling Low-mass Planetary Signals and Stellar Surface Magneto-convection in Spectroscopic Observations

G. Corsaro, E., et al., Towards an efficient full asteroseismic characterization of a large number of planet-host stars

H. Cosmovici, C., et al., Search for Water in exoplanetary Systems by means of ground-based Radiospectrometry

I. Csizmadia, Sz., Precise planet parameters with PLATO

J. Cunha, M.S., et al., Oscillations in g-mode period spacings in red giants as a way to determine their state of evolution

K. de Jong, Roelof S., et al., 4MOST spectroscopic host star characterisation for PLATO 2.0

L. do Nascimento, J.D., et al., Rotation Periods and ages of solar Twins revealed by the Kepler mission: A roadmap for PLATO ages

M. Debski, B., et al., Light Curve Morphology: a tool for PLATO 2.0 for studying extreme close binaries

N. Di Mauro, M. P., et al., A synergic strategy to identify habitable exoplanets

O. García Muñoz, A., Steps towards the interpretation of exoplanet phase curves

P. Garrido, R., et al., An information preserving method for filling gaps in time series

Q. Giuffrida, G., et al., Gaia and PLATO 2.0 in ASDC

R. (r) Iro, N., Exoplanet atmosphere modelling

S. Janot-Pacheco, E., et al., Atmospheric Biosignatures on Earth and Exoplanets by Spectroscopic Techniques

T. Klagyivik P., et al., Cluster formation and evolution as will be seen by PLATO: experiences with eclipsing binaries in NGC 2264

U. Krticka, J., et al., High precision photometry as a test of stellar model atmospheres and evolution theory

V. Mecheri, R., et al., A convenient system of first order ODEs describing the oscillations of rapidly rotating stars

W. Morel, T., Uncertainty in stellar radii for PLATO 2.0 targets based on Gaia data

X. Nelson R. P. ,et al., Formation and orbital evolution of planetary systems

Y. Norton, A. J,. et al., Detecting non-transiting planets in transiting planet surveys

Z. Oshagh, M., et al., Effect of stellar activity on the high-precision transmission spectra

AA. Paetzold, M., et al., Wavelet based filter methods for the detection of small transiting planets: application to Kepler light curves


9

BB. Paparo, M., Impact of CoRoT asteroseismology to PLATO 2.0 planet-hosting stars. Massive sample of large separations in Delta Scuti stars

CC. Peres, G., et al., The residual X-ray emission in Venus shadow

DD. Ragazzoni, R., et al., PLATO 2.0 Telescope Optical Units: design and evolution

EE. Salmon, S. J. A. J., et al., What can we learn from the asteroseismology of β Cephei stars through the forward approach

FF. Schou, J., On the surface effect in Sun-like stars

GG. Suran, M. D., et al., ROMOSC Asteroseismic data interpretation pipeline

HH. Sódor, Á., et al., Studying hybrid delta Scuti-gamma Doradus pulsators by space photometry

II. Turck-Chièze, S., et al., Improving stellar modelling

JJ. Valio, A., Determination of Stellar Rotation through starspots

KK. Voss H., et al., Scientific capabilities of the Gaia UB team applicable to PLATO 2.0


10

Abstracts Session A -‐ The PLATO Mission and Current Status

Heras, A. & Colangeli, L. -‐ PLATO as M3 mission in ESA's Cosmic Vision plan In February 2014, ESA selected PLATO as the M3 mission in the Cosmic-‐Vision 2015-‐2025

plan for a launch in 2024. Consequently, a Definition study was initiated with the purpose to consolidate the mission requirements, the mission design and the development plan. Conditional upon a successful completion of the Definition phase, the mission will be submitted to the Science Program Committee for adoption in June 2016. A PLATO Science Advisory Team has been appointed by ESA to advise on the scientific aspects of the mission, such as the consolidation of the scientific requirements and the preparation of the Science Management Plan, and to provide the scientific elements of the Definition study report (or Red Book).

Hatzes, A. -‐ Exoplanets in the 2020’s I will look into my crystal ball and try to tell you what the future has in store for

exoplanets in the 2020s.

Rauer, H. -‐ The PLATO Mission -‐ Overview PLATO has been selected as ESA’s M3 mission for launch in 2024. Its science results will

revolutionize our understanding of extra-‐solar planets through its discovery and bulk characterization of planets around hundreds of thousands of stars. In addition, the precise stellar parameters obtained by asteroseismic studies will open new doors to better understand stellar interiors and allow us to constrain poorly-‐understood physical processes.

Gondoin, P. -‐ PLATO spacecraft, payload and mission operation concept The PLATO space mission is described with a particular emphasis on the spacecraft,

payload and mission operation concept.

Gizon, L. -‐ PLATO Data Centre Co-authors: PLATO Consortium

The PLATO Data Centre (PDC) is a core element of the PLATO Mission, and has the major responsibility for the development, implementation and operation of the data processing ground segment for PLATO. The PDC will generate the key science data products (DP) from the PLATO mission, including: DP1 the science-‐ready light curves and centroid curves for each star, corrected for instrumental effects; DP2 transit candidates and their parameters; DP3 asteroseismic mode parameters; DP4 stellar rotation periods and stellar activity; DP5


11

seismically-‐determined stellar masses and ages, and DP6 the list of confirmed planetary systems, fully characterized by combining DP2-‐5 and follow-‐up observations. The PDC is structured into eight main work packages: WP31 system architecture, WP32 data processing algorithms, WP33 data processing development, WP34 input catalogue, WP35 preparatory and follow-‐up database management, WP36 stellar

Session B -‐ Planet formation and evolution

Alibert, Y. -‐ Planetary system formation and composition: statistics on low mass planets We present in this contribution planetary system formation and composition models,

coupled with internal structure models allowing the determination of planetary radius distribution. We focus here on the properties of warm to cold (up to~ AU from their star), core-‐dominated, planets, that are more likely to potentially harbour habitable conditions. The case of massive planets is addressed in a companion abstract by C. Mordasini. Our planetary system formation models include the following effects: planetary growth by capture of solids and gas, protoplanetary disk structure and evolution, planet-‐planet and planet-‐disk interactions. In addition, we compute the composition of the solids and gas in the protoplanetary disk, as well as their evolution with time. The formation and composition models allow therefire the determination of the composition of planets, in term of refractory elements (Mg, Si, Fe, etc…) as well as volatile elements (water, CO2, CO, NH3, etc…), in a way self consistent with the formation process of the different members of the planetary system. Finally, using internal structure models, we compute the radius distribution of planets at different periods, using the planetary composition provided by formation models. We will show in this contribution results of these formation/composition models, and we will demonstrate how the simultaneous determination of mass, radius and period of a statistical number of warm to cold earth to neptune-‐mass planets can be used to constrain the formation track of planets, as well as some important mechanism that may occur during planet formation, like volatile transport in the protoplanetary disk, stellar irradiation, interactions between planets and with the protoplanetary disk. Finally, we will show how the same observations (mass, radius, period), coupled with the knowledge of the central star composition and 2 bands transit observations can be used in order to select planets that are best suited for follow-‐up habitability studies.

Nelson, R. P. -‐ Formation and orbital evolution of planetary systems Co-author: Coleman, G.

The on-‐going discovery of extrasolar planets with highly diverse properties provides a formidable challenge to our ability to explain how planetary systems form and evolve. The core accretion scenario of plant formation is based on a sequential picture in which planetesimals grow into planetary embryos, which in turn accrete to form systems of planets whose properties depend on the detailed formation history. In this talk I will present the results of recent N-‐body simulation of planetary system formation that incorporate the most up-‐to-‐date prescriptions for migration, gas accretion and disc evolution. Among other issues, I will discuss how well these models are able to account


12

for the observed extrasolar planets, and the areas in which our current ideas about planet formation fall short of being able to provide a satisfactory explanation of the observed planetary population.

Mardling, R. -‐ The star-‐planet tidal link The exoplanet revolution is a direct result of Nature’s preference for short-‐period planets

and planetary systems. Without such a bounty we would surely not be attending the PLATO 2.0 Science Conference! I will discuss some of the outstanding questions resulting from these discoveries:

-‐ Why are most planet pairs not in resonance? -‐ How do Hot Jupiters arrive at their orbits? -‐ How do ultra-‐short period low-‐mass planets arrive at their orbits? -‐ What is the main bloating mechanism for Hot Jupiters? -‐ What is the main mechanism for spin-‐orbit misalignment of Hot Jupiters? -‐ Can we distinguish between mechanisms? -‐ How are tidal disturbances dissipated inside stars and planets?

Laskar, J. -‐ How to characterize multi-‐planet systems Co-authors: Correia, A.C.M.,Boué, G., Delisle, J.B.

TBD

Nascimbeni, V. -‐ TTVs: from Observations to Understanding Transit Time Variation (TTV) is a powerful dynamical technique to measure relative

masses within a multiple planetary system, without need of (or in synergy with) radial velocity measurements. It has also been exploited to infer the presence of additional, previously unknown bodies in the same system, even non-‐transiting ones. I will review the basic physical principles behind TTVs, the computational challenges of the inverse problem, the main results achieved so far and how TTVs could help the science case of PLATO.

Church, R.P. -‐ Deducing inclinations of transiting multi-‐planet systems Co-authors: Davies, M.B., Johansen A.

For individual exoplanet systems, PLATO 2.0 will measure directly the orbital periods of the planets but not their inclinations or eccentricities. We discuss how the distribution of exoplanet orbital inclinations can be constrained from transit data alone, by making use of the relative numbers of observed one-‐transit, two-‐transit and three-‐transit systems. Applying the technique to the Kepler sample we find that the observations are inconsistent with a single population of planetary systems. The ratio of observed two-‐planet to three-‐planet systems constrains the average mutual inclinations to be no more than a few degrees. In addition, to explain the observed systems there must be a second population of massive planets that do not have companions within 0.5 AU.


13

Mordasini, C. -‐ Time: a new dimension of constraints for planet formation and evolution theory Co-authors: Jin, S., Molliere, P., Alibert, Y., Benz, W.

A distinctive asset of the PLATO mission compared to other transit missions is its ability to measure reliable ages of the host stars and thus planets. This adds time as a new dimension in the study of exoplanets that was up to now only marginally accessible observationally. I will present how this new dimension opens a window to conceptually new observational constraints for planet formation and evolution theory. First, observing the temporal dimension will allow to directly see how giant planets contract in time. This yields essential constraints for theoretical models of the planetary interior and atmosphere regarding the opacity in the atmosphere, the physics of bloating mechanisms, and the energy transport in the interior. These informations are in turn key constraints for planet formation models regarding the enrichment of giant planets in heavy element by planetesimal impacts or the migration mode of Hot Jupiters (disk migration versus scattering or Kozai). Second, regarding low-‐mass planets it will allow to observe for the first time directly the boundary between gas-‐rich and solid planets, simply because gas-‐rich planets contract in time, while the radii of solid planets are essentially constant. This is a crucial information to understand the nature of the numerous close-‐in low-‐mass planets, and the key to understand the efficiency of H/He accretion during the formation phase as well as its loss due to atmospheric escape during evolution. I will address these points using statistical predictions of combined planet formation and evolution models for the planetary mass-‐mean density or distance-‐radius relationship.

Zwintz, K. -‐ Stellar structure across the HR diagram Based on the analysis of detected stellar oscillations, stellar structure and evolution

models could be improved significantly within the last few decades. We can now study thousands of stars across the HR diagram with precisions on the part-‐per-‐million level. Asteroseismology has also been able to unravel details of the internal structure for different types of stars in all stages of their evolution from the pre-‐main sequence to the final phases. The masses, radii, and ages of stars that were determined through asteroseismic investigations can serve as most valuable input for other scientific communities such as exoplanet, binary, cluster, and galactic archeology research. PLATO's main mission and its complementary science program are expected to advance our knowledge about the interior structure of stars even further by addressing some of the still open questions, such as the role of internal magnetic fields, the mixing of chemical species or internal rotation, with emphasis on stellar clusters of all ages and metallicities.

White, T.R. -‐ What Interferometry will do for PLATO The scientific success of the PLATO Mission depends on being able to accurately and

precisely determine the properties of stars. Planetary properties can only be as well constrained as the properties of their host stars. Many of the methods for determining stellar properties have some dependence on stellar models, and direct measurements of stellar properties are required to verify and calibrate these methods. Long-‐baseline optical


14

interferometry is capable of sub-‐milliarcsecond resolution, allowing for the imaging of stellar discs. The direct measurement of angular diameter with interferometry, in conjunction with measurements of parallax and bolometric flux, allows stellar radii and effective temperatures to be determined with little model dependence. In this talk I will discuss the crucial role these measurements will play in calibrating methods to determine stellar radii, particularly asteroseismic scaling relations. Additionally I will discuss the prospects of using interferometry to test theoretical limb-‐darkening coefficients, a key variable in modelling the light curves of planetary transits.

Session C -‐ PLATO Stars and Planets

Piotto, G. -‐ PLATO target and field selection Co-author: Nascimbeni, V.

TBD

Goupil, M. J. -‐ Asteroseismology with Plato I will first discuss the seismic performances needed to characterize the Plato planet host

stars with the resquested. Some results from CoRoT and Kepler will be used as illustrations of the ability of seismology to reach the expected performances

Cabrera, J. -‐ The planet detection pipeline of PLATO 2.0: overview and challenges Co-author: Lanza, N.

The planet detection pipeline is in charge of detecting planetary candidates in the light curves and classify them according to their properties, before they proceed to further characterization. The PLATO 2.0 planet detection pipeline builds on the expertise of the space borne surveys CoRoT and Kepler, but also on the European expertise from the ground (Super-‐WASP, NGTS). On the one hand, PLATO 2.0 should be able to detect planets with the size of the Earth, around solar-‐like stars, with one year orbital period. The main challenges for this scientific program are the detection of the planetary signal in the presence of stellar activity and its characterization with a reduced number of observations. With the term stellar activity we refer to intrinsic variability of the stellar targets at the time scales characteristic of transits. On the other hand, the PLATO 2.0 pipeline should be able to deal simultaneously with a large number of targets with very different properties, requiring different optimization approaches, for example, planets around eclipsing binaries. In this talk we will give an overview of the pipeline design in the M3 phase and the strategies considered to meet the challenges of PLATO 2.0 from the PSPM point of view.

Deleuil, M. -‐ PLATO candidates selection and ranking From lessons learnt from previous missions, CoRoT and Kepler, I will review what is

foreseen for PLATO candidates selection and ranking. We will see how this process benefits


15

the long duration and high precision light curves but also of all the information available on the candidate’s host star and its neighborhood. For the shallower transits that will challenge follow-‐up observations, statistics will provide valuable complementary information to the ranking process, securing or rejecting its planetary nature.

Udry, S. -‐ PLATO Follow-‐Up challenges TBD

Santos, N. C. -‐ Deriving stellar parameters In this talk I will review the importance of deriving precise spectroscopic stellar

parameters for FGKM type stars in the context of PLATO. A discussion will be done regarding the present day precision as well as some of the challenges in this field.

Gaidos, E. -‐ Properties of Very Cool Stars and their Planets: The Kepler Experience and the PLATO Promise

Although late K and M dwarf stars comprise a mere 3% of the Kepler target star catalog, they yielded a disproportionately large yield of small (Earth-‐size) transiting planet detections, especially planets that experience low stellar irradiances and that may have surface temperatures permissive of liquid water, i.e. "habitable". However, elucidating the precise nature of these objects has proven difficult because the host-‐stars stars are mostly too faint to measure planet masses with the Doppler radial velocity, and mostly too far away for precise parallaxes and other fundamental stellar parameters. I will review recent work in improving the parameters (temperature, radius, luminosity, metallicity) of these stars through spectroscopic methods calibrated on nearby stars, describe the statistical properties of the inferred planet population around these stars, predict the yield of future PLATO discoveries, and speculate on what we can learn about their composition, formation, and evolution of Earth-‐ to-‐ Neptune-‐size planets.

Kolb, U. -‐ Binary population models of PLATO 2.0 fields Co-authors: Rowden, P., Farrell, E., Farmer, R.

Assessing the expected false positive rate caused by blends requires a stellar population model of PLATO fields that takes includes self-‐consistently the evolving binary star content. We conducted exploratory simulations probing the latitude and longitude dependence of the blend signal in one of the proposed long-‐look PLATO fields, using tools we successfully deployed in the past towards modeling the Kepler field. Our analysis reveals the physical nature of the main blend contributors and helps predict and minimize the blend rate. But crucially it also delivers constraints on physical mechanisms driving binary evolution, such as wind and angular momentum loss rates, when the actually observed blend statistics is understood and compared against these population predictions. We present preliminary results and discuss the steps needed to fully exploit the data set PLATO will deliver for the


16

understanding of the binary star physics, including binaries that display an asteroseismic signal.

Santerne, A. -‐ Minimising the needs of follow-‐up observations for PLATO : the central role of planet-‐validation tool Co-authors: Díaz, R.F., Almenara, J.M.

To reach its scientific objectives, the space-‐based photometric observations of PLATO need to be followed up by ground based observations. Those observations are needed to (1) screen out non-‐planetary candidates, and (2) characterise the mass, radius and age of the planet down to a few percent. Given the fact that PLATO will detect thousands of potential planets, the follow-‐up will request a huge amount of telescope time. Fortunately, a new technique has been developed by the community to unveil the uncertain nature of the smallest CoRoT and Kepler candidates: the statistical planet validation. In this presentation, I will first explain the method of validating statistically exoplanet candidates. Then, I will present why this technique should be used prior to ground-‐based observations, (1) to estimate the probability of each false-‐positive scenario, (2) to constrain the parameter space of the most likely false-‐positive scenarios, (3) to define which instrument would be the most efficient to reject all false-‐positive scenarios. By doing that, it would be possible to reduce the list of candidates for intensive ground-‐based observations only to the bona-‐fide exoplanets. I will also discuss how the same tool could be used to optimise the epoch of radial velocity observations to efficiently constrain the orbit and mass of the planet, especially in case of eccentric orbit.

Session D -‐ Giant and Terrestrial Planets

Sohl, F. -‐ Terrestrial planet mass-‐radius and composition Co-authors: Wagner, F.W., Rauer, H.

The characterization of terrestrial-‐type, solid exoplanets in terms of internal structure and atmospheric composition has important implications on their formation, orbital evolution, and possible habitability. Structural models of low-‐mass solid exoplanets transiting their host stars are required to satisfy the planetary masses and radii as provided by radial velocity and photometric observations. These models are constructed by using equations of state for the radial density distribution, which are compliant with the thermodynamics of the high-‐pressure limit, and can be used to derive mass-‐radius relationships for low-‐mass solid exoplanets. Structural models of planetary interiors gain some insight in planet bulk composition but still suffer from inherent degeneracy or non-‐uniqueness problems, mainly due to the incomplete knowledge of the degree of internal separation of light and heavy constituents, the occurrence of pressure-‐induced phase transformations, and/or the possible presence of an optically thick atmosphere. In this paper, we will present an overview of interior models of selected terrestrial planets and confirmed rocky exoplanets.


17

Guillot, T. -‐ Giant planet mass radius relationship and their compositions Inferring the compositions of transiting gaseous planets from their mass and radius is

possible, but hampered by two issues: (1) The inaccurate determination of these parameters; (2) The presence of poorly understood mechanisms to inflate or slow the planetary contraction. By providing very accurate parameters for hot and warm giant planets orbiting bright stars thanks to their asteroseismic signatures, PLATO should enable distinguishing these inflation mechanisms and constraining the compositions of gaseous exoplanets. For the closest hot Jupiters, PLATO should detect the planets' tidal distortion, providing constraints on the inner density profile. Altogether, this will provide a much better understanding of the formation of planetary systems.

Deeg, H.J. -‐ Circumbinary Planets Circumbinary planets (CBP) are planets orbiting both components of a binary star. They

may be detected by a variety of techniques making use of precise photometry. The first successful technique was the precise timing of the binary eclipses, finding several planets with decade-‐long orbital periods. More recently, detections by transits have been successful, all from data of the Kepler mission. Transit detections constitute now the majority of known CBPs, with common features being masses in the Neptune-‐range and periods of a few months that are (with one exception) close to the innermost limit for a stable orbit around the central binary. A few CBPs have also been detected by direct imaging. Circumbinary planets are an interesting test-‐bed for planet formation models, as they need to account for the additional perturbation and stability issues arising from the binaries' orbit. The current sample of such planets is however still very small and the true parameter space for their existence is still poorly known, of note being a likely absence of CBPs around very short-‐periodic binaries. Current CBPs are also mostly on faint stars which impedes good characterisation. An overview over our current knowledge of CBPs will be given and the potential of their detection by PLATO be outlined, which is the subject of its Work Package 112510.

Kislyakova, K. -‐ Star-‐planet interaction and planetary characterization methods Co-authors: Lammer, H., Holmström, M., Johnstone, C.P., Odert, P., Erkaev, N.V.

We study the interactions between stellar winds and the extended hydrogen-‐dominated upper atmospheres of exoplanets. We consider the interaction processes for close-‐in exoplanets (“Hot Jupiters”) as well as for exoplanets in the terrestrial size-‐mass domain (“Super-‐Earths”). As a result of the interaction, the planetary atmosphere is ionized by several mechanisms: ionization by the stellar wind (electron impact ionization) and stellar radiation, and charge-‐exchange between the neutral atoms in the planetary exosphere and the stellar wind protons. The intensity of the interaction depends on the planetary gravity and orbital location and on the presence and strength of the intrinsic magnetic field. By means of numerical modelling, we model the high energetic and thermal particle coronae around the exoplanets which are formed by charge-‐exchange, tidal effects and radiation pressure. We estimate the resulting escape of planetary pick-‐up ions, which are swept away by the stellar wind. The particle code is based on Direct Simulation Monte Carlo (DSMC) method and includes stellar wind protons and atmospheric neutrals presented by metaparticles. We also summarize how one can estimate the Ly-‐alpha attenuation produced by neutral hydrogen


18

clouds around an exoplanet and show on an example of the “Hot Jupiter” HD 209458b how this method can be used as a means to estimate the stellar plasma environment at the orbital location and the planetary magnetic moment. Finally, we discuss how PLATO observations of exoplanets orbiting bright stars can be used to reconstruct stellar wind properties, upper atmosphere structure and escape, as well as to test the magnetosphere hypotheses.

Ehrenreich, D. -‐ Atmospheres of PLATO planets The field of exoplanet atmospheres is now booming thanks to (low-‐resolution) space-‐

borne spectrographs and high-‐resolution (narrow-‐ranged) NIR spectrographs on ground-‐based 8m-‐class telescopes. These instruments allow observers to constrain atmospheric properties on a limited set of objects. In this talk, I will review the current state-‐of-‐the-‐art in exoplanetary atmospheres and the upcoming instrumental and theoretical perspectives that will set the stage for the launch of PLATO. PLATO will act as a game changer, turning a target-‐starved field into a discipline dominated by survey studies, where statistical studies of planetary atmospheres become possible. I will discuss possible paths towards new approaches for target selection and characterisation of planetary atmospheres during the PLATO era.

Burleigh, M.R. -‐ Eclipses, transits and intrinsic variability of white dwarfs with PLATO 2.0 Co-author: Braker, I.

The similar size of a white dwarf (WD) star to Earth implies that any sub-‐stellar or gas giant companion at suitable orbital inclination will completely eclipse it, while terrestrial bodies smaller than the Moon, including asteroids, will still produce transits that are detectable in high signal/noise light-‐curves. Intriguingly, WDs even possess a habitable zone extending from 0.005AU to 0.02AU and periods from 4 -‐ 30 hours. Whether such planets actually exist around WDs is an open question. Those caught within the expanding envelope of an AGB star will be destroyed. But the presence of debris disks around a few % of Wds and accreted metals in the photospheres of a surprisingly large fraction of such stars demonstrates that surviving asteroids and terrestrial planets must be perturbed into orbits that take them close to the central WD, where they are tidally disrupted. Even so, it appears dynamically difficult, though not impossible, to perturb them into stable, circularised orbits within the WD HZ. Alternatively, 2nd generation planets may be created from material ejected after the AGB phase. The PLATO 2.0 mission is an ideal opportunity to search the HZs of a statistically significant (500 -‐ 1000) sample of WDs for terrestrial planets. Any discovery would provide vital data and a significant challenge to dynamicists and theoreticians, just as the unexpected discovery of hot Jupiters did in the 1990s. A single detection would then open the exciting possibility of studying the atmosphere of a nearby terrestrial world through spectroscopy. We will present simulations of the expected signature of transits and eclipses of WDs by nearby planets in PLATO 2.0 data. We will also present exciting data from the few WDs observed by the Kepler mission that shows a surprisingly large fraction appear to be low amplitude, periodically variable. In some cases this may be due to the presence of starspots in the convective atmospheres of WDs with appreciable magnetic fields. But in other stars the origin is less obvious, but may be related to the accretion of circumstellar rocky material.


19

Haswell, C.A. -‐ Do extremely close-‐in transiting planets hold the key to learning exoplanet compositions? Co-authors: Fossati, L, Bochinski, J, Staab, D., Barnes, J., Anglada-Escude, G.

We studied an extremely close-‐in hot Jupiter exoplanet, WASP-‐12b, using HST to detect absorption from dozens of species in the extended exosphere of the planet. Surprisingly, we also discovered that the entire planetary system is shrouded in diffuse gas lost from the heavily irradiated planet. WASP-‐12's gas shroud produces noticeable absorption in the strongest lines of abundant species: we first noted it in Mg II h&k, and found a similar signature in the Ca II H&K lines. Meanwhile, the Kepler mission has revealed evidence for dozens of small rocky bodies orbiting their host stars with sub-‐day periods. In this context we are working on identifying some very interesting close-‐in exoplanetary bodies orbiting nearby stars. Once identified, these systems will permit exquisite quality observations revealing their compositions in unprecedented detail.

Noack, L. -‐ Terrestrial planets vs. water worlds: characterization and habitability limitations Co-authors: Heistracher C., Zimov N., Hoening D., Rivoldini A., Van Hoolst T., Lammer H., Bredehoeft J.-H.

The upcoming PLATO mission will be able to deliver measurements of mass and radius of the detected exoplanets with a high accuracy. It has been calculated that an error in radius of 2% and an error in mass of 4-‐10% can be expected [Rauer et al., in review, "The PLATO 2.0 mission"]. In our study we investigated how well these measurements can constrain the interior of a planet and, assuming that water is present at the surface of the planet, discuss additional habitability constraints typically assumed for water-‐arm and water-‐rich planets. We concentrate only on small-‐mass exoplanets of up to 10 Earth masses or 2 Earth radii. We explore how the radius of a planet depends on the planet's mass and its composition assuming an Earth-‐like iron core, a silicate mantle and a possible water-‐ice layer (hereafter referred to as ocean layer) to investigate how well terrestrial planets without (or with negligible amounts of) water can be distinguished from water worlds with ocean layers several hundreds of kilometers deep. Water-‐arm planets (terrestrial planets) are typically defined to be habitable if they are in the habitable zone and if surface temperatures suitable for liquid water are present. This requires a long-‐term stable atmosphere, and can be constrained by the evolution of volcanic outgassing and the possible plate tectonics history. We have shown that (at least for an Earth-‐size planet) both outgassing and likelihood of plate tectonics strongly depend on the interior structure of terrestrial planets and therefore on their composition [Noack et al., PSS, 2014, "Can the interior structure influence the habitability of a rocky planet?"]. Planets with a small iron core will likely be in the stagnant-‐lid regime and develop a dense, Venus-‐like atmosphere. Planets with a core of approximately half to three quarters of the planet size tend to be in the plate tectonics regime. A larger core, on the other hand, leads to ceasing of outgassing (possibly inhibiting a secondary atmosphere) and again a stagnant lid. A water-‐rich planet on the other hand may be called habitable if the ocean layer is molten directly above the silicate shell. Another factor is the possible delivery of cometary material including pre-‐biotic material to the ocean. However, if a water world contains a large amount


20

of water, a deep ocean layer (containing water and/or ice) forms, which is most likely frozen from a specific depth on. This depth depends mainly on the mass and radius of the planet as well as the ocean surface temperature. We find that local remelting of the high-‐pressure ice at the ocean-‐mantle boundary is possible for ice layers of intermediate thickness (again depending on the mass and radius of the planet). However, such a second ocean layer might freeze out during the thermal evolution of the planet depending on the heat flux out of the silicate mantle [Noack et al., in review, "Water worlds: how life-‐friendly is an ocean deeper than on Earth?"]. Ocean planets, that can be clearly detected as such, contain a large amount of water (to significantly reduce the average density of the planet) and are likely to have a thick high-‐pressure ice layer which cannot be molten from beneath -‐ these planets might therefore not be habitable. When it comes to the detection of a possibly habitable planet, terrestrial planets seem to be more suitable candidates than ocean planets since the classification of the latter would likely imply a thick, partly frozen ocean layer. A planet with a terrestrial-‐like average density can still contain a thin ocean layer, but would still be classified as habitable.

Szabó, Gy. M. -‐ An occurrence-‐weighted searching strategy for exomoons Co-authors: Simon, A. E., Charnoz, S.

In the past decade, the quest for exomoons concerned the detection methods and their performance. The central question was whether the largest exomoons can be somehow detected by photometry or spectroscopy, and which are the most effective tools for such a detection. These tools favoured large moons at large orbital distance. The photometric methods were extensively tested in Kepler data, which led to negative results to date, suggesting that 1) the S/N ratio of Kepler targets (which were fainter stars in the most cases) were suboptimal for such a detection, and 2) the presumed Earth-‐size or even super-‐Earth-‐size moons likely do not exist even around the most massive exoplanets. An alternative to point 2) is that Earth-‐sized exomoons are not likely to survive around planets close to their star or around evolved stars. Therefore, the detection studies must rely BOTH on observability and occurrence considerations -‐ the observation strategy must be pointed to the effective detection of moons that are more likely to exist. In this contribution we will concentrate on this complex issue. Along the recognition that SUCCESS RATE ~ OBSERVABILITY x OCCURRENCE, we propose the unification of satellite formation and stability studies on one side, and instrumentation and evaluation studies on the other side, to estimate and optimize the success rate of an exomoon discovery. We propose and estimator that helps identify the most promising systems hosting an observable exomoon, and demonstrate how the occurrence considerations influence the target selection strategy.

Rodríguez-‐López, C. -‐ CARMENES: Radial velocity follow-‐up and characterization of PLATO targets Co-authors: Amado, R. L., the CARMENES consortium

This contribution will provide an overview of the CARMENES instrument, of the survey that will be carried out with it during the first years of operation and of its potential as a follow-‐up facility for PLATO. CARMENES (Calar Alto high-‐Resolution search for M dwarfs with Exoearths with Near-‐infrared and optical Echelle Spectrographs) is a next-‐generation radial-‐


21

velocity instrument under construction for the 3.5m telescope at the Calar Alto Observatory by a consortium of eleven Spanish and German institutions. The CARMENES instrument consists of two separate Echelle spectrographs covering the wavelength range from 0.55 to 1.7 mum at a spectral resolution of R = 82,000, fed by fibers from the Cassegrain focus of the telescope. The spectrographs are housed in vacuum tanks providing the temperature-‐stabilized environments necessary to enable a 1 m/s radial velocity precision employing a simultaneous calibration with an emission-‐line lamp or with a Fabry-‐Perot etalon. For mid-‐M to late-‐M spectral types, the wavelength range around 1.0 mum (Y band) is the most important wavelength region for radial velocity work. Therefore, the efficiency of CARMENES has been optimized in this range. The CARMENES instrument consists of two spectrographs, one equipped with a 4k x 4k pixel CCD for the range 0.55 -‐ 0.95 mum, and one with two 2k x 2k pixel HgCdTe detectors for the range from 0.95 -‐ 1.7mum. Each spectrograph will be coupled to the 3.5m telescope with two optical fibers, one for the target, and one for calibration light. The front end contains a dichroic beam splitter and an atmospheric dispersion corrector, to feed the light into the fibers leading to the spectrographs. Guiding is performed with a separate camera; on-‐axis as well as off-‐axis guiding modes are implemented. Fibers with octagonal cross-‐section are employed to ensure good stability of the output in the presence of residual guiding errors. The fibers are continually actuated to reduce modal noise. The spectrographs are mounted on benches inside vacuum tanks located in the coudé laboratory of the 3.5m dome. Each vacuum tank is equipped with a temperature stabilization system capable of keeping the temperature constant to within +/-‐0.01°C over 24 hours. The visible-‐light spectrograph will be operated near room temperature, while the near-‐IR spectrograph will be cooled to ~ 140 K. The CARMENES instrument passed its final design review in February 2013. The MAIV phase is currently ongoing. First tests at the telescope are scheduled for early 2015. Completion of the full instrument is planned for the fall of 2015. At least 600 usable nights have been allocated at the Calar Alto 3.5m Telescope in the time frame until 2018 to conduct an exoplanet survey targeting ~ 300 M dwarfs with the completed instrument. A data base of M stars (dubbed CARMENCITA) has been compiled from which the CARMENES sample can be selected. CARMENCITA contains information on all relevant properties of the potential targets. Dedicated imaging, photometric, and spectroscopic observations, as part of the science preparation, are underway to provide crucial data on these stars that are not available in the literature.

Session E -‐ Stellar and Other Science

Chaplin, W.J. -‐ Prospects for studies of solar-‐type stars with PLATO In this talk I will review our current understanding of the internal structure and dynamics

of solar-‐type stars, making reference in particular to results from Kepler and CoRoT. I will then discuss the exciting possibilities for detailed studies that will be made possible by data from PLATO.

Miglio, A. -‐ Red-‐Giants and Galactic Structure In this presentation I will recall why ageing stars and their pulsations are key to the

PLATO mission. The pulsation frequencies of red-‐giant stars may be used to place tight constraints on their fundamental properties, including radius, mass, evolutionary state, and


22

age. Thanks to the early achievements with CoRoT and Kepler, Galactic archeology has now been included as one of the major scientific goals of ESA’s PLATO 2.0, which will supply seismic constraints for stars over a significantly larger fraction of the sky (and volume) compared to CoRoT, Kepler, and K2. By detecting solar-‐like oscillations in ∼85,000 nearby dwarfs and an even larger number of giants, PLATO 2.0 will provide a revolutionary complement to Gaia’s view of the Milky Way. In addition to providing constraints on stellar populations, ageing stars will also play a fundamental role in PLATO's core science.

Planets orbiting red giants have now been detected in a few Kepler targets, and seismic constraints on their host stars were key to the accurate characterisation of planetary systems, including inferences on spin-orbit misalignments. Finally, oscillations modes detected in ageing stars may be used to test stellar models (e.g. transport of angular momentum and of chemical species), leading to a better understanding of stellar evolution in earlier phases as well.

Tkachenko, A. -‐ Binary stars in the era of space-‐based missions Complementary observations of binary stars allow the determination of fundamental

stellar quantities, and are a principal source of stellar masses. As such, binary stars are irreplaceable for probing models of stellar structure and evolution. Besides that, the interactions between two stars within a binary system allow us to test and further develop theories of tidal evolution and angular momentum transport under extreme physical conditions that cannot be reproduced in our labs. Dynamical tides are also known to be effective in resonant excitation of stellar pulsations but magnetic fields in binaries are expected to strongly affect the transfer of mass and angular momentum as well as the global properties of stellar oscillations. The interplay between stellar magnetic fields, binarity, and oscillations has yet to be investigated in detail, and will provide a further insight into the tidal evolution theory. The development of modern instrumentation with high spectral and spatial resolution and the amazing precision of on-‐board detectors operational in space on the one hand, and new modern analysis techniques on the other hand, now make it possible to surpass the barrier of 1% accuracy on the stellar parameters, allowing studies on a much more detailed scale.

Campante, T. L. -‐ An ancient extrasolar system with five terrestrial-‐size planets The chemical composition of stars hosting small exoplanets appears to be more diverse

than that of gas-‐giant hosts, which tend to be metal-‐rich. This implies that small, including Earth-‐size, planets may have readily formed at earlier epochs in the Universe's history when metals were more scarce. We report Kepler observations of KOI-‐3158, a metal-‐poor Sun-‐like star from the old population of the Galactic thick disk, which hosts five planets with sizes between Mercury and Venus. We used asteroseismology to measure an age of 11.2+/-‐1.0 Gyr (~9% precision) for the host star, indicating that KOI-‐3158 formed when the Universe was less than 20% of its current age and making it the oldest known system of terrestrial-‐size planets. We thus show that Earth-‐size planets have formed throughout most of the Universe's 13.8-‐billion-‐year history, leaving open the possibility for the existence of ancient life in the Galaxy. The discovery of such a system encapsulates many of the science goals set for ESA’s future PLATO mission, namely, the precise characterization of a system of terrestrial-‐size


23

planets around a bright Sun-‐like star whose fundamental properties have been tightly constrained by asteroseismology. The interdisciplinary approach adopted in the analysis of this unique system could thus serve as the archetype of the analysis procedure of future PLATO targets.

Cassisi, S. -‐ Improving our understanding of stellar evolution with PLATO Nowadays, the huge improvements in asteroseismic analysis allow us to determine the

mass and radius of large sample of stars with an approach -‐largely-‐ independent of stellar model computations. This notwithstanding, some evolutionary parameters, such as the stellar age -‐ a pivotal information also in planetary system analysis -‐ we need to rely on theoretical model predictions. Depending of the stellar mass range and evolutionary stage, these theoretical predictions can be significantly affected by not negligible uncertainties mainly related to our poor knowledge of some important physical processes such as convection, rotation (and related mixing processes), magnetic fields, mass loss, etc. We will briefly review the most important shortcoming in current generation of stellar models and make some prediction on how PLATO is expected to largely improve the our understanding of stellar evolution.

Nielsen, M. B. -‐ Constraints on the radial differential rotation for six Sun-‐like stars Co-authors: Gizon, L., Schunker, H., Schou, S.

Asteroseismology has the potential to constrain differential rotation in Sun-‐like stars. We have analyzed six high signal-‐to-‐noise Sun-‐like stars in the Kepler field, in order to constrain their radial differential rotation. We measure the rotational frequency splitting from the acoustic oscillation power spectrum. We use a Markov chain Monte Carlo method to fit independent sections of the p-‐mode envelope. This allows us to search for differences in the splittings across a range in frequency, spanning up to 8 radial orders. For all six stars we find that the measured splittings are consistent with solid-‐body rotation, but also that the differential rotation cannot be larger than ~1-‐1.5muHz. Furthermore, we determined the rotation period from the starspot signal and compared this to the mean asteroseismic periods. We find that the periods are consistent, indicating that they both trace rotation in the same region of the star.

Reese, D. R. -‐ SpaceInn hare-‐and-‐hounds exercise Co-authors: Chaplin, W. J., Davies, G. R., Miglio, A., et al.

With the advent of high-‐precision space photometry missions and the forthcoming PLATO mission, different methods have been and are being developed for inferring stellar properties from pulsation frequencies. As described in Gough (1985), these include the so-‐called "forward modelling" approach which consists in searching for an optimal stellar model in a parameter space, analytical methods based on matching patterns in the pulsation spectrum, and inverse methods which seek to correct a reference model so as to reproduce observations. Given this variety of methods, it then becomes crucial to compare them and assess their ability at reproducing stellar properties. In the present talk, I will describe an


24

ongoing SpaceInn hare-‐and-‐hounds exercise which seeks to test how accurately one can retrieve general stellar properties as well as the depth of the convection zone in main-‐sequence solar-‐like pulsators, from a set of individual frequencies. This exercise is also designed to compare convection zone depths obtained from the forward modelling approach with those obtained from an independent analysis based on acoustic glitches. In a future round of exercises, we plan to test how accurately the He ionisation zone can be located, the He abundance determined, and the properties of a small convective core (if present) estimated.

Ball, W. H. -‐ A new correction of stellar oscillation frequencies for near-‐surface effects Co-author: Gizon, L.

A key component of the PLATO mission is to exploit asteroseismology to constrain the properties of planet hosting stars, as is currently possible for a handful of stars observed by CoRoT and Kepler. However, current stellar models have inaccuracies near the surface that introduce systematic differences in the oscillation frequencies. These so-‐called surface effects must be corrected to reduce the amount of error induced on the underlying model parameters. We introduce two parametrizations of the surface effect. We first show that these parametrizations accurately correct model frequencies for two calibrated solar models, and then use them to fit parameters for the planet-‐hosting CoRoT target HD 52265. Our results give similar parameters to the widely-‐used correction by Kjeldsen et al. (2008), but the new parametrizations fit the mode frequencies significantly better. We finally present preliminary results of fits to other stars, consolidating the usefulness of the new parametrizations.

Buldgen, G. -‐ Asteroseismic inversions in the context of the Plato mission Co-‐author: Reese, D., Dupret, M-‐A.

The determination of stellar characteristics such as the mass, the age or the radius, is crucial when studying both stellar evolution and exoplanetary systems. In the context of the Plato mission, the high quality data allows us to reach a new level of accuracy and model-‐independence for stellar characterization by using inversion techniques. In this study, we will use the SOLA method (F. Pijpers and M. J. Thompson 1994), known for its successes in helioseismology, and show how it can offer us new insights into the structure of observed stars. We will present results for the mean density, building on the approach of Reese et al. 2012, and other custom-‐made structural characteristics constraining the outer layers of stars and the chemical content of their cores. We will show that inversions can determine these characteristics within 0.5%, a significant improvement over the capabilities of the classical forward modelling process. Consequently, such inversions lead to better stellar models and help us obtain more accurate fundamental parameters such as the age, mass or radius.

Session F -‐ PLATO's Contribution to Exoplanet studies

Pagano, I. -‐ Synergy with other facilities: CHEOPS, TESS, JWST and E-‐ELT With a launch planned in 2024, PLATO 2.0 will start his survey for small planets around

bright stars at a time when CHEOPS, TESS and JWST will have completed their excellent job


25

discovering and characterising internal structure and atmospheres of an important number of exoplanets orbiting close-‐by stars. What are we expecting more by a mission like PLATO 2.0? This talk is about why we need PLATO2.0 after CHEOPS, TESS and JWST, and about the synergies with them and with E-ELT, the European Extremely-Large telescope that will see the first light when PLATO 2.0 is launched.

Sozzetti, A. -‐ On the Gaia -‐ PLATO Synergy I will discuss Gaia's two-‐tiered, synergistic contribution to PLATO 2.0 in terms of a) its

data products of fundamental importance for the realization of the PLATO 2.0 Input Catalogue and b) the combination of Gaia and PLATO 2.0 data for improved understanding of the architecture of planetary systems.


26

Posters contributions (A) Alonso R. -‐ The phase curve of Kepler-‐7b Co-author: Rebollido-Vázquez, I.

We perform an analysis of the complete Kepler data set for the star Kepler-‐7b, known to host a 5d-‐period, 1.6Rj planet with the highest albedo measured for a giant exoplanet, of about 0.3. We apply different detrending techniques to produce the phase curves, and describe a method to discern properties about the rotation of the planet.

(B) Ammler-‐von Eiff, M. -‐ Low-‐resolution spectroscopy in the ground-‐based follow-‐up of planet candidates -‐ lessons learned from CoRoT Co-author: Sebastian D., Guenther E.W., Stecklum B.

We present results of low-‐resolution spectroscopic observations (R about 1,000) conducted within the ground-‐based follow-‐up of CoRoT planet candidates. We also discuss recent efforts to study the stellar content of CoRoT target fields using multi-‐object spectroscopy. We address the specific requirements of PLATO and discuss the role of Gaia and future multi-‐object spectroscopic facilities. Low-resolution spectroscopy helps to identify eclipses of giant stars due to low-mass stars which can mimick a planetary transit of a Sun-like star. It is important to exclude such false positives before the start of the expensive ground-based radial velocity (RV) measurements. Experience from CoRoT shows that spectral classification based on low-resolution spectra helps to find the giant stars among faint candidates (V=13-16). In addition, early-type targets are identified which are often excluded from further RV follow-up. On the other hand, low-resolution reconnaissance spectroscopy ensures that good planet candidates are kept that would otherwise be discarded based on photometric spectral type alone. Multi-object spectroscopy, in particular, has proven extremely efficient and also allows one to study other stars in the target field in addition to the actual candidates. This way it is possible to study the stellar environment and the frequency of planetary systems in detail and to draw conclusions about the main galactic factors of planet formation.

(C) Bensmaïa, M.K. -‐ Time-‐Dependent Convection asteroseismic modelling of β Hydri Co-author: Grigahcène, A., Damerdji, Y., Dupret, M. A., Scuflaire, R., Garrido, R.

The success of helioseismology in improving our understanding of solar interior had a big impact on stellar physics as well. Conversely, the study of Sun-‐like stars provides a better understanding of the Sun itself. The subgiant star β Hydri, which is considered as probable future Sun, shows solar-‐like oscillations that allow its study using asteroseismology. Recently, it has been shown that Time-‐Dependent Convection models are the most appropriate for this type of investigation. In this work we use TDC models to better constrain structure models and estimate the global parameters of β Hydri using the atmospheric and astroseismic available information. Our best model reproduces the observed frequencies with unprecedented high precision: among the 33 observed modes, 18 frequencies are reproduced with difference < 1 micro


27

Hertz, 10 frequencies with difference < 2 micro Hertz and the rest with < 2.4 micro Hertz. More, the model gives a mass of 1.0710 Msun and an age of 7.6643 Gyr.

(D) Bonfanti, A. -‐ The ages of stars-‐hosting planets Co-author: Ortolani, S.

We determined the age of planet-‐hosting stars (SWP) through stellar tracks and isochrones computed with the Padova & Trieste Stellar Evolutionary Code (PARSEC). We developed algorithms based on two different techniques to determine the ages of field stars: isochrone placement and Bayesian estimation. Their application on a synthetic sample of coeval stars shows that the Bayesian computation of the modal age tends to select the outmost age values in the isochrones grid. Therefore, we used the isochrone placement technique to measure the ages of 317 stars with planets (SWP). We found that ~6% of SWP has an age lower than 0.5 Gyr. The age distribution peaks in the interval [1.5, 2) Gyr, then it decreases. However ~7% of the stars are older than 11 Gyr. The Sun results to be a common star-‐hosting planets regarding its evolutionary stage. Our SWP age distribution is less peaked and slightly shifted towards lower ages if compared with the ages in the literature, based on the isochrone fit. In particular, there are no ages younger than 0.5 Gyr in the literature.

(E) Boué, G. -‐ On the origin of stellar spin-‐orbit angle in extrasolar systems Two different paths may lead to hot Jupiters : migration in the protoplanetary disk and

dynamical interaction with other planets or with a stellar binary companion. These two scenarios predict different stellar spin-‐orbit angle distributions. Hence, several works have been dedicated to the study of spin-‐orbit measurements in order to disentangle the two scenarios. However, other mechanisms like chaotic star formation or magnetic interaction with the disk are also susceptible to produce spin-‐orbit misalignments. In this talk, I will show how PLATO 2.0 can lift the veil on the origin of stellar obliquity and bring valuable information on planetary systems early evolution.

(F) Cegla, H. M -‐ Disentangling Low-‐mass Planetary Signals and Stellar Surface Magneto-‐convection in Spectroscopic Observations Co-authors: Watson, C. A., Shelyag, S., Mathioudakis, M.

Magnetic activity and variability inherent to solar-‐type stars naturally limits the level of precision attainable for radial velocity (RV) measurements. Even magnetically quiet stars, with a convective envelope, still exhibit RV variability on the several tens of cm/s level due to oscillations and stellar surface magneto-‐convection (i.e. granulation). This is especially significant at the Earth-‐analogue level as the astrophysical noise completely swamps the 9 cm/s planet signal. Our aim is to understand the physical processes behind granulation in order to disentangle its effects from observed stellar absorption lines. To do so, we start with a state-‐of-‐the-‐art 3D magnetohydrodynamic simulation of the solar surface. Motivated by computational constraints and a desire to breakdown the physics, we define the parameters the granulation signal from these simulations and use it to construct model Sun-‐as-‐a-‐star observations. We present our granulation parametrisation across the stellar disc (including a quantitative measure of the RV signature due solely to the corrugated nature of granulation),


28

alongside the current results from our Sun-‐as-‐a-‐star simulations. We find several line diagnostics correlate with the induced RV shifts. In particular, our proxy for brightness measurements is one of the best-‐suited diagnostics for reducing convective noise in the simulations. Accordingly, simultaneous space-‐based photometry, from missions such as PLATO 2.0, could be key in reaching a sufficient precision for the RV confirmation of habitable, Earth-‐like worlds.

(G) Corsaro, E. -‐ Towards an efficient full asteroseismic characterization of a large number of planet-‐host stars Co-authors: De Ridder J., Garcia R. A.

Characterizing planet-‐host stars with solar-‐like oscillations is proving to be a key step to improve our understanding about planetary formation and evolution, and about stellar physics in general. However, to fully analyze the asteroseismic properties of individual oscillation modes, several challenges arise in terms of computational power and efficiency. This is mainly related to the high number of parameters involved in the models fitting the observations and to the high quality light curves now available from the NASA Kepler mission. Sophisticated and robust statistical analysis tools are a prerequisite to conduct this type of analysis. In this talk we present a recently developed Bayesian code termed DIAMONDS, which is able to perform a fast inference based on the use of the nested sampling algorithm. We show the potential of DIAMONDS in the asteroseismic analysis of a challenging F-‐type star observed by Kepler for more than four years. Finally, we focus on the possibility to automatize the entire process for a large number of targets thanks to the high capabilities of the method introduced. This advance in data analysis will be greatly needed for the analysis of tens of thousands pulsating stars that are expected to be observed by the ESA PLATO mission.

(H) Cosmovici, C. -‐ Search for Water in exoplanetary Systems by means of ground-‐based Radiospectrometry Co-authors: Pluchino, S., Montebugnoli, S., Pogrebenko, S., Bianchi, G., Schillirò, F., Bartolini, M.

The ITASEL project (Italian Search for Extraterrestrial Life) started 1999 and was supported and financed by ASI with the main purpose to develop a modern technology for the detection of life bearing molecules in Comets and Exoplanetary systems by means of ground-‐based radiospectrometry. In particular the 22 GHz (1.35 cm) water MASER emission was used, after its discovery during the Comet Shoemaker-‐Levy 9 catastrophic impact with Jupiter in July 1994, as a diagnostic tool for the search of water in habitable planets up to 50 light years from Sun. 35 exoplanetary systems were investigated using 2 new FFT spectrometers (SPECTRA-‐1 and-‐2). In 5 of them we could detect, using the Radiotelescopes of Medicina and Noto, the Maser emission with a S/N ratio > 4 in different periods. Special attention was devoted to the Epsilon Eridani exoplanetary system because of its close distance to Sun and the presence of a huge cloud of comets surrounding the hosting star. Here we’ll present the observations carried out up to now and discuss the results and possible future plans.

(I) Csizmadia, Sz. -‐ Precise planet parameters with PLATO PLATO aims at measuring planetary radii with 2% accuracy. In this poster we review what

requirements is needed to reach this ambitious goal and how one can reach it.


29

(J) Cunha, M.S. -‐ Oscillations in g-‐mode period spacings in red giants as a way to determine their state of evolution Co-authors: Stello, D., Avelino, P. P., Christensen-Dalsgaard, J.

Sharp structural variations in the radiative inner layers of red giant stars may influence the stars' oscillation periods, producing a signature in their period spacings. These signatures are expected to be found in the data for a number of red giant stars that will be observed by the PLATO 2.0 mission, revealing not only details of their inner structure, but also their precise evolutionary status. In this work we describe the main characteristics of the signature imprinted in the period spacings by glitches in the buoyancy frequency lying inside the g-‐mode propagation cavity and explain under which conditions that signature is expected to exist. Based on the analysis of the period spacings for a large grid of models, we further identify regions along the red giant evolution where the signature may be found.

(K) de Jong, Roelof S. -‐ 4MOST spectroscopic host star characterisation for PLATO Co-author: the 4MOST collaboration

4MOST is ESO's next generation spectroscopic survey facility for the VISTA telescope with a first light planned in 2020. In its initial 5 year survey 4MOST is expected to deliver spectra for >20 million objects spread over a large fraction of the southern sky. Of particular interest for PLATO will be that 4MOST can obtain resolution R~20,000 spectra for a large fraction of the stars to be observed by PLATO in the 10-‐15th mag range. Such spectroscopic observations would identify double line spectroscopic binaries, provide exo-‐planet host-‐star characterisation yielding birth place information by identifying stellar families in abundance and dynamics space, and support the astro-‐seismology investigations such that much more accurate masses and ages of stars can be obtained. Repeat observations could furthermore yield single line spectroscopic binaries, but would require a modification of the survey strategy as currently planned.

(L) do Nascimento, J. D. -‐ Rotation Periods and ages of solar Twins revealed by the kepler mission: A roadmap for PLATO ages Co-authors: Meibom, S., Barnes, S., Garcia, R., Mathur, S.

The Sun is a benchmark in stellar astrophysics research and establishing a sample of solar analog stars is important to map its past, present and future, and to understand how representative it is for stars with the same mass and age. We present a new sample of solar-‐type field stars that contain at least fifteen solar analogs and possibly even solar twins. Using long-‐cadence (Q0-‐Q16) light curves from NASA's Kepler mission we determine the stellar rotation periods and ages. We analyze the properties of unevolved solar analogs and twin candidates and determine their gyrochronology ages. From our results we present the comparison between the gyro-‐ages and ages from asteroseismology for solar analogs. We summarize that searching for solar twins will be an important roadmap for age determinations in future missions like PLATO.


30

(M) Debski, B. -‐ Light Curve Morphology: a tool for PLATO 2.0 for studying extreme close binaries Co-author: Zola, S.

The continuous high precision photometry is essential for understanding the processes governing the short-‐time scale activity in extreme close binaries. The analysis of the evolution signal of such light curve parameters like the O'Connell effect and the separation of the brightness maxima is a powerful tool for studying the evolution of the activity of the binary system. We present Light Curve Morphology Analysis, which fits perfectly to the outcome data of the PLATO 2.0 mission. The Analysis may offer, inter alia, the most precise and useful description of the observed known and newly discovered binaries.

(N) Di Mauro, M. P. -‐ A synergic strategy to identify habitable exoplanets Co-authors: Ventura, R., Claudi, R., Mura, A., Mangano, V.

We will present a new approach to characterize habitability of exoplanets by using properties of the host-‐star as obtained by Asteroseismology and by modelling conditions of stability of the planetary atmosphere as developed for the planets of our Solar System.

(O) García Muñoz, A. -‐ Steps towards the interpretation of exoplanet phase curves PLATO will enable the investigation of exoplanet atmospheres through the accurate

analysis of planet phase curves. Just as for the Solar System planets, phase curves contain unique yet blended information on the dynamical and thermal state, composition (gas, cloud, haze), and horizontal/vertical structure of the planets’ envelopes. In preparation for the interpretation of PLATO and other space mission phase curves, I have been re-‐visiting the problem of phase curve interpretation in the Solar System, paying special attention to Earth, Titan, and Venus. The observational data are collected from space missions (Messenger, Cassini) and ground-‐based observations. These three objects are vastly different, but together they encompass some of the configurations (broken/continuous cloud/haze cover) that will surely occur on exoplanets. In my presentation, I will summarize these ongoing efforts. Incorporating the lessons learned from decades of Solar System exploration will surely help characterize exoplanet atmospheres and decide what steps are needed next.

(P) Garrido, R. -‐ An information preserving method for filling gaps in time series Co-authors: Pascual-Granado, J., Suárez, J. C.

Invalid flux measurements, introduce aliases in the periodogram and wrong amplitudes. It has been demonstrated that replacing such invalid data with a linear interpolation is not harmless. On the other side, using power spectrum estimators for unevenly sampled time series is not only less computationally efficient but it leads to difficulties in the interpretation of the results. Therefore, even when the gaps are rather small and the duty cycle is high enough the use of gap-‐filling methods is a gain in frequency analysis. However, the method must preserve the information contained in the time series. We present a gap-‐filling method based on autoregressive moving-‐average modelling of the data that make no assumptions about the analyticity of the signal. In this contribution we give a short description of the method and show some results when applying it to CoRoT seismo


31

light curves. We show that this method remove the aliased periodogram making unnecessary any pre whitening technique for asteroseismic analysis. This technique can be extended to the time series supplied by PLATO when necessary.

(Q) Giuffrida, G. -‐ Gaia and PLATO 2.0 in ASDC Co-authors: Marrese, P. M., Marinoni, S., Verrecchia, F., Buonanno, R., Castellani, M.

The number of stars that Plato 2.0 can follow will be limited by telemetry bandwidth, and is considerably smaller than the total number of stars in Plato's field of view (FOV), therefore the selection of the optimal targets (i.e. the preparation on the Plato Input Catalogue) is a fundamental task for the mission. The implementation of Plato Input Catalogue (PIC) is developed and managed at the ASI Science Data Center (ASDC), one of the PLATO Data Processing Centre, following the scientific inputs of the Target/Field Characterization team (leader G. Piotto). ASDC has the responsibility for the delivery and maintenance of the final input catalogue. ASDC is also responsible in DPAC-‐CU9 for the cross match of the Gaia catalog with big Optical/IR surveys. The cross-‐match tables with PPMXL, GSC2.3, AllWISE, 2MASS, SDSS DR10 and UCAC4 will be part of the first official Gaia catalog release (mid-‐2016). Several other catalogs will be added in future releases (Pan-‐STARRS, the ESO-‐surveys ….) This big set of data will constitute the foundation of the Plato Input Catalog. ASDC (www.asdc.asi.it), a facility of the Italian Space Agency (ASI), is a multi-‐mission science operations, data processing and data archiving center that provides support to several scientific space missions such as Plato,Gaia, Herschel, Planck, Swift, AGILE, Fermi and NuSTAR.

(R) Iro, N. -‐ Exoplanet atmosphere modelling With the discovery of an increasing number of planets outside our Solar System, we are

becoming familiar with physical conditions and atmospheric compositions that span a much wider range that what covered by the planets of our solar system. Non-‐exhaustive examples are equilibrium temperatures ranging from 50K (Neptune) to over 3000K (WASP-‐12b, WASP18b); orbital eccentricity, ranging from 0-‐0.1 for solar system planets (except Mercury) and circularized close-‐in hot Jupiters to HD80606b (e=0.93). Other parameters relevant for atmospheric dynamical features are also quite diverse: the Rhines length and Rossby length are, e.g., much smaller than the planet radii for Solar system planets, while they are comparable to the planetary radii for hot Jupiters and Neptunes, meaning that in the latter case typical circulation features are global. It seems timely and urgent to try to frame in a common framework our understanding of such a large variety of atmospheric conditions. Here we present VIPER, the Versatile Interactive PlanetSimulator for Extrasolar Research. This project, under development, aims at developing the Planet Simulator, an already flexible climate model to a new level of modularity.

(S) Janot-‐Pacheco, E. -‐ Atmospheric Biosignatures on Earth and Exoplanets by Spectroscopic Techniques Co-authors: Bendjoya, P., Bernardes, L. Lage, C.


32

The new generation of ground based astronomical instruments (ALMA,VLT-‐SPHERE,VLT-‐MATISSE,E-‐ELT) and the latest and future space missions (e.g. CoRoT, Kepler, PLATO) bring us to a crucial turnover in our knowledge on the exoplanetary science domain. New exoplanetary systems are being detected almost each day and we will in a few years be able to make direct images of the exoplanets and hence to analyze their atmospheres. Since the discovery of the first exoplanet in 1995, this field of research has become a major one in astronomy and astrophysics. This is not surprising since this field is related to a fundamental and ancient question of humanity on the possibility to discover other worlds. Once the existence of these new planetary systems have been proved, the next crucial question is “Is there any life on these new worlds?”. The ultimate subject of this project is to study theoretical and instrumental tools that will help answering these questions. In order to reach these goals we will use the only planet at our disposal on which we know that life is fully developed: Earth. We will consider Earth and life on Earth as the ideal laboratory to experiment strategies for the detection of life signatures by spectroscopic techniques not only qualitatively but also quantitatively. Life-‐related molecules are quite complex. One of the main teaching concerning life on Earth is that biodiversity is a phenomenal reality that has not been quantitatively estimated due to the huge amount of species and individuals in each species. When considering the whole biodiversity (from vegetables to animals, passing through microbes and viruses) it seems obvious that life has “polluted” our atmosphere continuously in a non negligible way since at least 3 Gyr. We intend to systematize the detection of this non negligible part of “pollution” of our atmosphere by the biosphere. From the results it will then be possible to adapt detection strategies and to envisage the instrumental developments for the atmospheric bio-‐signature detection in planets of the solar system and finally in exoplanets as soon as their own spectra will be accessible with the proper resolution.

(T) Klagyivik, P. -‐ Cluster formation and evolution as will be seen by PLATO: experiences with eclipsing binaries in NGC 2264 Co-author: Csizmadia Sz.

Using ground-‐based measurements we found an extremely high fraction of eclipsing binaries in the area of the very young open cluster NGC 2264 (Klagyivik et al. 2013). This observation can be explained only if all the orbital planes are nearly edge-‐on inside the cluster while it is isotropically distributed in the field, which has an implication on cluster formation and evolution. Thanks to its large-‐sky accessibility, PLATO 2.0 will be an excellent instrument for evolutionary tracing of binary systems in open clusters observing a large number of open clusters at different ages of different richness of clusters. Combining these data with the results of the Gaia satellite, the beginning of a new era of binary star and cluster formation studies is foreseen.

(U) Krticka, J. -‐ High precision photometry as a test of stellar model atmospheres and evolution theory Co-authors: Mikulasek, Z., Janik, J., Prvak, M.

Chemically peculiar stars represent a large class of upper main sequence stars. The processes of radiative diffusion and gravitational settling in their atmospheres give rise to pronounced deviations in the chemical composition of these stars from the solar value. Some chemically peculiar stars show inhomogeneous surface distribution of chemical elements on


33

their surface. The uneven surface distribution of various elements, together with radiative flux redistribution and rotation, is the origin of these stars' light variability. The comparison of the predicted light variability (derived from model atmospheres using surface abundance maps) with observed light variability provides a very precise test of model atmospheres. Moreover, the periodical light variability may serve as a very precise clock that is able to detect even very minute changes of rotational period. Therefore, space-‐based photometry may serve as test of internal structure and evolutionary models of the stars with global magnetic field.

(V) Mecheri, R. -‐ A convenient system of first order ODEs describing the oscillations of rapidly rotating stars Co-author: Roxburgh, I. W.

In this contribution we present a new simplified form of the equations of hydrodynamics describing the oscillations of rapidly rotating stars. It is obtained first from an expansion of the perturbation quantities into a multiple summation of spherical harmonics and then a truncation of the equations at a certain order. After lengthy algebraic manipulations of the equations in a surface fitted system of coordinates, the resulting equations consist of a set of first order linear Ordinary Differential Equations (ODEs) representing an eigenvalues problem which can be solved numerically using the appropriate boundary conditions at the center and at the surface of a rotating (non-‐spherical) star. This set of equations is a generalization of the very familiar ODEs system known in the case of a non-‐rotating (spherical) star. This model can be used for the exploitation of the future PLATO asteroseismic data.

(W) Morel, T. -‐ Uncertainty in stellar radii for PLATO2.0 targets based on Gaia data Planets orbiting red giants have now been detected in a few Kepler targets, and seismic

constraints on their host stars were key to the accurate characterisation of planetary systems, including inferences on spin-‐orbit misalignments. Finally, oscillations modes detected in ageing stars may be used to test stellar models (e.g. transport of angular momentum and of chemical species), leading to a better understanding of stellar evolution in earlier phases as well.

(X) Nelson, R. P. -‐ Formation and orbital evolution of planetary systems Co-author: Coleman, G.

The on-‐going discovery of extrasolar planets with highly diverse properties provides a formidable challenge to our ability to explain how planetary systems form and evolve. The core accretion scenario of plant formation is based on a sequential picture in which planetesimals grow into planetary embryos, which in turn accrete to form systems of planets whose properties depend on the detailed formation history. In this talk I will present the results of recent N-‐body simulation of planetary system formation that incorporate the most up-‐to-‐date prescriptions for migration, gas accretion and disc evolution. Among other issues, I will discuss how well these models are able to account for the observed extrasolar planets, and the areas in which our current ideas about planet formation fall short of being able to provide a satisfactory explanation of the observed planetary population.


34

(Y) Norton, A. J. -‐ Detecting non-‐transiting planets in transiting planet surveys Co-author: Lohr, M. E.

Wide field photometric surveys, epitomized by SuperWASP at the present time and by PLATO in the future, detect vast numbers of eclipsing binary stars and pulsating stars as a by-‐product of their main purpose. Any regularly repeating fiducial marker such as an eclipse or a pulse can be used to monitor dynamical changes in a stellar system. So circumbinary planets in eclipsing binaries and planets orbiting pulsating stars can in principle be detected from cyclical eclipse timing variations and pulse timing variations respectively, caused by light travel time delays induced by an orbiting exoplanet. I present some recent work in this area from SuperWASP data and look ahead to the prospects for such detections with PLATO.

(Z) Oshagh, M. -‐ Effect of stellar activity on the high-‐precision transmission spectra Co-authors: Santos, N. C.; Ehrenreich, D.; Haghighipour, N.; Figueira, P.; Santerne, A.; Montalto, M.

Transmission spectroscopy during planetary transits, which is based on the measurements of the variations of planet-to-star radius ratio as a function of wavelength, is a powerful technique to study the atmospheric properties of transiting planets. One of the main limitation of this technique is the effects of stellar activity, which up until now, have been taken into account only by assessing the effect of non-occulted stellar spots on the estimates of planet-to-star radius ratio. In this paper, we study, for the first time, the impact of the occultation of a stellar spot and plage on the transmission spectra of transiting exoplanets. We simulated this effect by generating a large number of transit light curves for different transiting planets, stellar spectral types, and for different wavelengths. Results of our simulations indicate that the anomalies inside the transit light curve can lead to a significant underestimation or overestimation of the planet-to-star radius ratio as a function of wavelength. At short wavelengths, the effect can reach to a difference of up to 10% in the planet-to-star radius ratio, mimicking the signature of light scattering in the planetary atmosphere. Atmospheric scattering has been proposed to interpret the increasing slopes of transmission spectra toward blue for exoplanets HD 189733b and GJ 3470b. Here we show that these signatures can be alternatively interpreted by the occultation of stellar plages. Results also suggest that the best strategy to identify and quantify the effects of stellar activities on the transmission spectrum of a planet is to perform several observations during the transit epoch at the same wavelength. This will allow for identifying the possible variations in transit depth as a function of time due to stellar activity variability.

(AA) Paetzold, M. -‐ Wavelet based filter methods for the detection of small transiting planets: application to Kepler light curves Co-author: Grziwa, S.

The space telescopes CoRoT and Kepler provided a huge number of high-‐resolution stellar light curves. These light curves are searched for transit signals which may be produced by planets when passing in front of the stellar disc. Stellar flux variations caused by star spots, pulsation, flares, glitches, hot pixels etc., however, dominate the stellar light curves and may mask faint transit signals in


35

particular those of small exoplanets. This may lead to missed candidates or a high rate of false detections. The Rheinisches Institut für Umweltforschung (RIU-‐PF) as one of the CoRoT detection teams has developed the two model independent wavelet based filter techniques VARLET and PHALET. These two filters are used to reduce the flux variability in order to improve the search for transits. The VARLET filter separates the large-‐scale variations from the white noise without using a-‐priori information of the target star. The transit feature, however, is not extracted and is still contained in the residual (filtered) time series which makes it now much easier to search for transits by the search routine EXOTRANS (Grziwa et al., 2012). The PHALET filter is used to separate periodic disturbances with well-‐known periods independent of their shape, e.g. disturbances caused by the spacecraft motion in the Earth orbit. The main purpose Of PHALET, however, is to extract already detected transits in order to search for multi-‐planet systems that are transits from additional planets in the stellar light curve. RIU-‐PF searched all publicly available Kepler light curves for planetary transits by including VARLET and PHALET in the detection pipeline. The results of that search are compared with the official Kepler candidate list. About 93% of the 2232 entries in the recent Kepler candidate list could be confirmed; together with a number of newly detected candidates including 20 new multi-‐planet systems. The huge number of available light curves can only be handled and processed with fully automated filtering and detection algorithms running on computer clusters. This will become even more important for future missions like PLATO and TESS.

(BB) Paparo, M. -‐ Impact of CoRoT asteroseismology to Plato planet-‐hosting stars. Massive sample of large separations in Delta Scuti stars.

The detailed investigation of exoplanets needs information on the planet-‐hosting stars. Asteroseismology allows unique information on the stars orbiting by planets. The large separation between the consecutive radial orders and the small separation of modes with different l values are well-‐known and useful parameters for characterizing solar type oscillation. Determinations of large separation in Delta Scuti stars were obtained from ground-‐based data (Handler et al., 1997, Breger et al., 1999, 2009), from space data (Matthews, 2007-‐MOST, Garcia Hernandez et al. 2009, 2013, Mantegazza et al, 2012-‐CoRoT and Hernandez et al. 2013-‐Kepler), but only for limited number of stars. Mostly the Fourier transform technique and the histogram of frequency differences were used. The CoRoT target, 102749568 was a case, where individual frequencies in shifted regular patterns were localized (Paparo et al. 2013). As a continuation of this method, 96 Delta Scuti stars on the first CoRoT long run were checked for regular patterns. 86 Delta Scuti stars showed regular (not equidistant) patterns. The method seems to be robust not only for finding single patterns but shifted patters, too. The distribution of patters: 24 stars showed -‐ single pattern, 32 stars -‐ two, 17 stars -‐ three, 8 stars -‐four, 4 stars -‐ five and 1 star showed -‐ six shifted patters. No more than 60 frequencies per a single star was used, in average 30 frequencies/star. In 50 stars 40-‐60 % of the frequencies were included in one of the patterns. Averaging the individual frequency differences of the patterns, the large separation of 86 Delta Scuti stars were determined with


36

high precision. Two peaks exist:: 33 stars showed large separation between 25-‐30 microHz and 22 stars exhibited separation between 30-‐40 microHz.. The other values distributed around the two peaks. The shifts between the patterns (analogy of the small separation) showed also systematic values. The same "magic numbers" appeared from star to star. The localization of independent frequencies in the shifted patterns allows a relative mode identification. A systematic survey on the other CoRoT runs and Kepler data could give huge improvement in charactherizing of planet-‐hosting stars.

(CC) Peres, G. -‐ The residual X-‐ray emission in Venus shadow Co-authors: Afshari, M., Reale, F., Gambino, A.

We take advantage of Venus transit on the Sun disk to measure the x-‐ray and UV residual emission. We provide evolution and spatial structure of this X-‐ray and UV shadows and comment these preliminary analysis.

(DD) Ragazzoni, R. -‐ PLATO Telescope Optical Units: design and evolution Co-author: the PLATO TOU Team

PLATO (Planetary Transits and Oscillations of stars) is the Cosmic Vision Programme M3 mission selected for launch in January 2024 by ESA. The main goal of the PLATO mission is to detect terrestrial exoplanets in the habitable zone of solar-‐type stars and to characterize their bulk properties. The payload concept is based on a multi-‐Camera approach, involving 34 cameras, looking at 4 partially overlapping areas on the sky. The many eyes of PLATO are based on a fully dioptric design (6-‐lenses), working in an extended visible light range and are able to observe a very large field. Here we highlight the main features of the Telescope Optical Units (TOU), starting from the optical design, through the main analysis which are on-‐going at the moment of this writing, to its prototyping activities, aimed to validate several different aspect of the overall design.

(EE) Suran, M. D. -‐ ROMOSC Asteroseismic data interpretation pipeline Co-author: Pricopi, D.

We present our data interpretation pipeline ROMOSC which will be used for asteroseismic characterization of the stars hosting exoplanetary systems observed by PLATO Mission.

(FF) Salmon, S. J. A. J. -‐ What can we learn from the asteroseismology of β Cephei stars through the forward approach Co-authors: Montalban, J., Miglio, A., Noels, A., Eggenberger, P., Dupret, M-A., Briquet, M.

The beta Cephei pulsating stars present a unique opportunity to test and probe our knowledge on the interior of massive stars. The information we can obtain depends on the quality and number of observational constraints, both seismic and classical ones. The asteroseismology of beta Cephei stars proceeds by a forward approach, which often result in multiple solutions, without clear indication on the level of confidence. We seek a method to derive confidence intervals on stellar parameters obtained by forward


37

approach and investigate how these latter behave depending the seismic data accessible to the observer. We realise forward modelling with help of a grid of pre-‐computed models and use Monte-‐Carlo simulations to build confidence intervals on the inferred stellar parameters. We apply and test this method in a series of hare and hound exercises on a subset of theoretical models simulating observed stars. Results show that a set of 5 frequencies (with knowledge of their associated angular degree) yields good seismic constraints. In particular, presence of mixed modes provides a strong diagnosis on the evolutionary state of the star. Significant errors on the determination of the extent of the central mixed region appear when the theoretical models do not present the same chemical mixture as the observed star.

(GG) Schou, J. -‐ On the surface effect in Sun-‐like stars The so-‐called surface effect continues to be a cause of problems in helio-‐ and astero-‐

seismology, especially for stars with the narrow range of frequencies typically observed in intensity by missions such as CoRoT, Kepler and Plato. Here I will investigate some of the likely causes of the surface effect, in particular the effects of the near surface convection. I will also briefly touch on other observable consequences of near-‐surface convection on the oscillation modes.

(HH) Sódor, Á. -‐ Studying hybrid delta Scuti-‐gamma Doradus pulsators by space photometry Co-authors: Sódor, Á., Bognár, Zs., Paparó, M.

We have the opportunity to study the full interior of the genuine hybrids by asteroseismic means, because both low-‐order p-‐ and high-‐order g-‐modes are self-‐excited at the same time in these objects. Therefore, the asteroseismic importance of such genuine hybrids is very high. However, a few other physical processes can also be responsible for the observed low-‐-‐frequency light variations, e.g., binarity and surface inhomogeneities. The discrimination between the different scenarios is often not straightforward. Usually, ground-‐based follow-‐up spectroscopy is necessary, which will be more affordable and more effective for the bright PLATO hybrid candidates. Our future goal is to devise reliable methods for discriminating between genuine hybrids and other possible objects showing low-‐frequency light variations together with delta Scuti pulsations. Here we present our preliminary results from our ongoing hybrid-‐candidate studies based on space photometry, emphasizing its relevance to the PLATO project.

(II) Turck-‐Chièze, S. -‐ Improving stellar modelling Co-authors: LePennec, M., Ducret, J.E., Ribeyre, X, Salmon, S., Blancard, C., Cosse, P., Faussurier, G., Mondet, G., Colgan, J., Fontes, C., Kilcrease, D.

We present in this poster different activities that we are performing to improve the microscopic description of solar-‐like stars and massive stars in order to better interpret the present asteroseismic observations of stars from KEPLER. This activity will largely benefit also to the future PLATO mission.


38

(JJ) Valio, A. -‐ Determination of Stellar Rotation through starspots During the eclipse of a star by its orbiting planet, spots and other features on the surface

of the host star may be occulted. This will cause small variations in the star light curve. Detailed analysis of these variations during planetary transits provides a wealth of information about starspot properties. If observation of multiple transits is available, it may be possible to detect the same spot on different transits and thus determine the stellar rotation. Assuming a rotation profile of the star with latitude, it may also be possible to estimate stellar differential rotation. This study is performed using a method that simulates the passage of a planet (dark disk) in front of a star with multiple spots of different sizes, intensities, and positions on its surface. The light curves of known planets detected by the CoRoT and Kepler satellite are analyzed and the estimates of stellar rotation and differential rotation presented.

(KK) Voss, H. -‐ Scientific capabilities of the Gaia UB team applicable to PLATO 2.0 Co-authors: Carrasco, J. M., Julbe, F., Jordi, C., Torra, J.

The knowledge and understanding about the character and features of the photometric, spectro-‐photometric and spectroscopic data of the ESA Gaia mission gained during its processing and validation should be applied during the PLATO target star selection process to allow optimal transit search results. Our team at the Universitat de Barcelona currently working on Gaia has an extensive expertise in space-‐based photometry that could be very useful for the preparation and execution of the PLATO2.0 mission. Additional Gaia derived information about stellar parameters, positions, proper motions and parallaxes should be incorporated in the target star selection as well as 2D analysis of crowded regions obtained with Gaia. Gaia data will become available stepwise with the different catalogue releases. Our role in these releases can help to get the maximum profit of the Gaia data to the PLATO2.0 mission as soon as they become available step by step.


39

List of participants Surname Name Affiliation Country

1 Adibekyan Vardan CAUP Portugal 2 Affer Laura INAF - Osservatorio Astronomico di Palermo Italy 3 Alibert Yann University of Bern Switzerland 4 Alonso Roi Instituto de Astrofísica de Canarias Spain

5 Ammler-von Eiff Matthias Max Planck Institute for Solar System Research Germany

6 Appourchaux Thierry Institut d'Astrophysique Spatiale France 7 Baglin Annie LESIA Observatoire de Paris France 8 Ball Warrick Institut für Astrophysik Göttingen Germany 9 Ballot Jérôme IRAP France 10 Barrado David Centro de Astrobiología Spain 11 Baudin Frédéric IAS France 12 Belkacem Kevin LESIA - Paris Observatory France 13 Bellassai Giancarlo INAF OACT Italy 14 Bigot Lionel Lagrange - Observatoire de la Côte d'Azur France 15 Bognar Zsofia MTA CSFK, Konkoly Observatory Hungary 16 Bonfanti Andrea Università degli Studi di Padova Italia 17 Bonomo Aldo Stefano INAF - Osservatorio Astrofisico di Torino Italy 18 Borsa Francesco INAF - Osservatorio Astronomico di Brera Italy 19 Borsato Luca Università degli Studi di Padova - DFA Italy 20 Boué Gwenaël IMCCE France 21 Bourrier Vincent Observatoire de Genève Suisse 22 Brown David University of Warwick / Queen's University Belfast UK 23 Buldgen Gaël University of Liège Belgium 24 Burleigh Matthew University of Leicester UK 25 Burston Raymond MPS Germany 26 Cabrera Juan DLR Germany 27 Camilletti Adam Airbus DS UK UK 28 Campante Tiago University of Birmingham UK 29 Cassisi Santi INAF - Osservatorio Astronomico Teramo Italia

30 Cegla Heather Cegla Queen's University Belfast

United Kingdom

31 Chaplin William University of Birmingham United Kingdom

32 Church Ross Lund Observatory Sweden

33 Colangeli Luigi ESA The Netherlands

34 Corsaro Enrico Service d'Astrophysique, IRFU/DSM/CEA Saclay France 35 Cosentino Rosario INAF-FGG Spagna 36 Cosmovici Cristiano INAF-IAPS Italy 37 Csizmadia Szilard DLR-EPA Germany 38 Cunha Margarida Centro de Astrofísica da Universidade do porto Portugal 39 D'Arrigo Paolo Airbus DS UK


40

Surname Name Affiliation Country 40 Damasso Mario INAF-OATo Italy 41 Davies Guy Rhys University of Birmingham UK 42 de Jong Roelof Leibniz-Institut für Astrophysik Potsdam (AIP) Germany

43 Debski Bartlomiej Astronomical Observatory of the Jagiellonian University Polska

44 Deeg Hans Instituto de Astrofísica Canarias Spain 45 Deleuil Magali LAM France 46 Demangeon Olivier Laboratoire D'Astrophysique de Marseille (LAM) France

47 do Nascimento José-Dias

Harvard-Smithsonian Center for Astrophysics (CfA) & Univ. F. do Rio do Rio Grande do Norte (UFRN) USA

48 Dreyer Claudia DLR Germany 49 Ehrenreich David University of Geneva Switzerland 50 Gaidos Eric University of Hawaii USA

51 Gandolfi Davide Landessternwarte Königstuhl - University of Heidelberg Germany

52 García Muñoz Antonio ESA Netherlands

53 Garrido Rafael IAA-CSIC Spain 54 Giuffrida Giuliano ASDC-INAF Italy 55 Gizon Laurent Max Planck Institute for Solar System Research Germany

56 Gondoin Philippe ESA The Netherlands

57 Goupil Marie-Jo observatoire de Paris France 58 Granata Valentina University of Padova Italy 59 Grenfell John Lee Dept. Exoplanets and Atmospheres, DLR Berlin Germany 60 Guillot Tristan Obs. Cote d'Azur France 61 Hassani Sheida Sharif University of Technology Iran 62 Haswell Carole The Open University UK 63 Hatzes Artie Thueringer Landessternwarte Tautenburg Germany 64 Helled Ravit Tel-Aviv University Israel

65 Heras Ana M. ESA/ESTEC The Netherlands

66 Hodgkin Simon Institute of Astronomy, Cambridge University UK 67 Iro Nicolas Univ. hamburg Germany

68 Janot-Pacheco Eduardo University of São Paulo Brazil

69 Jones Geraint MSSL, University College London, UK UK

70 Kislyakova Kristina Space Research Institute, Austrian Academy of Sciences, Graz Austria

71 Klagyivik Peter Instituto de Astrofísica de Canarias Spain 72 Kolb Ulrich The Open University UK

73 Krticka Jiri Masaryk University Czech Republic

74 Lanza Antonino F. INAF - Osservatorio Astrofisico di Catania Italy 75 Lanzafame Alessandro Università di Catania Itay 76 Laskar Jacques Observatoire de Paris France 77 Leto Giuseppe INAF-OACT Italy


41

Surname Name Affiliation Country 78 Ligi Roxanne Observatoire de la Côte d'Azur France 79 Lignieres Francois IRAP France

80 Lund Mikkel Stellar Astrophysics Centre (SAC), Aarhus University, DK UK

81 Marcadon Frédéric Institut d'astrophysique spatiale France 82 Mardling Rosemary Monash University Australia 83 Martinetti Eugenio INAF OACT Italy 84 Mecheri Redouane CRAAG Algeria 85 Messina Sergio INAF OACT Italy 86 Michel Eric Observatoire de Paris- LESIA France

87 Miglio Andrea University of Birmingham United Kingdom

88 Mordasini Christoph MPIA Germany 89 Morel Thierry ULg, Liege, Belgium Belgium 90 Musella Riccardo Observatoire de Paris France 91 Nascimbeni Valerio INAF-OAPD Italy 92 Nelson Richard Queen Mary University of London U.K. 93 Nielsen Martin Bo Institute for Astrophysics, Goettingen Germany 94 Noack Lena ROB, Royal Observatory of Belgium Belgium 95 Norton Andrew The Open University UK 96 Paetzold Martin RIU-Planetenforschung Germany 97 Pagano Isabella INAF - Catania Astrophysical Observatory Italia 98 Paparo Margit Konkoly Observatory Hungary

99 Peres Giovanni Universita` di Palermo, Dip. FIsica e Chimica - Specola Universitaria Italy

100 Pilbratt Göran ESA The Netherlands

101 Pinçon Charly LESIA (Observatoire de Paris) France 102 Pino Lorenzo Università degli studi di Padova Italy 103 Piotto Giampaolo Universita' di Padova Italia 104 Pollacco Don University of Warwick UK 105 Pricopi Dumitru Astronomical Institute of the Romanian Academy Romania 106 Prisinzano Loredana INAF-OAPA Italy 107 Ragazzoni Roberto INAF - Osservatorio Astronomico di Padova Italia

108 Ramsay Gavin Armagh Observatory United Kingdom

109 Rauer Heike DLR Germany

110 Reese Daniel University of Birmingham United Kingdom

111 Remus Francoise OBSPM-LUTh France 112 Ribas Ignasi ICE (CSIC-IEEC) Spain 113 Salmon Sébastein CEA Saclay France

114 Santerne Alexandre Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto Portugal

115 Santos Nuno Centro de Astrofísica, Univ. Porto Portugal 116 Scandariato Gaetano INAF-OACT Italia


42

Surname Name Affiliation Country 117 Schalinski Cornelius OHB System Germany 118 Schou Jesper Max Planck Institute for Solar System Research Germany 119 Schweitzer Mario OHB System Germany 120 Silva Aguirre Victor Aarhus University Denmark 121 Silvotti Roberto INAF-OATo Italy 122 Sódor Ádám Konkoly Observatory Hungary 123 Sohl Frank DLR Institute of Planetary Research Germany 124 Sozzetti Alessandro INAF - Osservatorio Astrofisico di Torino Italy 125 Spinella Salvatore OACT - INAF Italy

126 Strassmeier Klaus G. AIP Germany

127 Suran Marian Doru Astronomical Institute of the Romanian Academy of the Romanian Academy Romania

128 Szabo Robert MTA CSFK, Konkoly Observatory, Budapest, Hungary Hungary

129 Szabó M. Gyula Konkoly Observatory Hungary 130 Tkachenko Andrew Institute of Astronomy, KU Leuven Belgium 131 Udry Stéphane University of Geneva Switzerland 132 Valio Adriana Mackenzie University Brazil

133 Ventura Rita Inaf - Osservatorio Astrofisico di Catania Italia

134 Voss Holger Institut d'Estudis Espacials de Catalunya (IEEC)/Universitat de Barcelona (UB) Spain

135 Wheatley Peter University of Warwick UK 136 White Timothy University of Göttingen Germany 137 Wuchterl Günther Thüringer Landessternwarte Germany 138 Zwintz Konstanze Institute of Astronomy, KU Leuven Belgium

Documents

Science&Program,&Abstracts,& List&of&Participants& · PLATO&2.0!! Science&Conference! Ta♉rmina,’3"5"December"2014!!!!! Science&Program,&Abstracts,& List&of&Participants&!!