IAU Symp. 276, Torino, october 2010 R. Gratton 1, M. Kasper 2, C. Verinaud 3, M. Bonavita 1,4 + EPICS Science team Science with EPICS The E-ELT Planet

IAU Symp. 276, Torino, october 2010

R. Gratton1, M. Kasper2, C. Verinaud3, M. Bonavita1,4 + EPICS Science team

Science with EPICSThe E-ELT Planet Finder

1INAF-Osservatorio Astronomico di Padova2ESO3LAOG4Un. of Toronto


EPICS Phase-A study

22

ESOESO: Markus Kasper, Emmanuel Aller-Carpentier, Norbert Hubin, Florian Kerber, Natalia Yaitskova, Patrice Martinez, : Markus Kasper, Emmanuel Aller-Carpentier, Norbert Hubin, Florian Kerber, Natalia Yaitskova, Patrice Martinez, Enrico FedrigoEnrico Fedrigo

LAOGLAOG: : Jean-Luc Beuzit, Christophe Verinaud, Visa Korkiaskoski, Patrick Rabou, Jacopo Antichi, Olivier Jean-Luc Beuzit, Christophe Verinaud, Visa Korkiaskoski, Patrick Rabou, Jacopo Antichi, Olivier Preis Preis

Padova ObservatoryPadova Observatory: Raffaele G. Gratton, Mariangela Bonavita, Dino Mesa: Raffaele G. Gratton, Mariangela Bonavita, Dino Mesa

ASTRONASTRON: : Lars Venema, Lars Venema, Ronald Roelfsema, Rieks Jager, Hiddo HanenburgRonald Roelfsema, Rieks Jager, Hiddo Hanenburg

University of OxfordUniversity of Oxford: : Niranjan Thatte, Mattias Tecza, Graeme SalterNiranjan Thatte, Mattias Tecza, Graeme Salter

LESIALESIA: Pierre Baudoz, Anthony Boccaletti: Pierre Baudoz, Anthony Boccaletti

NOVANOVA: Christoph Keller: Christoph Keller

ETH ZürichETH Zürich: : Hans Martin Schmid Hans Martin Schmid

FIZEAUFIZEAU: Lyu Abe: Lyu Abe

LAMLAM: Kjetil Dohlen: Kjetil Dohlen


Concept

33

Top view Nasmyth implementation


Concept

44

1. E-ELT: 42 m telescope λ/D=4.9 mas at 1 μm

2. Superb XAO and wavefront control• Turbulence residual halo ~10-5 at 30 mas <10-6 close to the AO correction radius• Quasi-static speckles at a similar level than AO residuals through phase-diversity

2. Excellent temporal stability• All moving or rotating optics are in the common path.• Cover providing thermal inertia and dust protection.

3. Efficient calibration of PSF residuals• Well behaved and known chromaticity for spectral deconvolution • Small instrumental polarization and efficient calibration for differential polarimetry

=> EPICS is photon noise limited


Separation (arcsec)X (arcsec)

Y

(arc

sec)

Y

(arc

sec)

EXPECTED PERFORMANCES


Three Driving Science Cases

• Young self-luminous gas planets in star forming regions and young associations

• Mature planets in the solar neighbourhood– Giant planets– Neptune-like & Rocky Planets

• Planets discovered by RV, astrometry and transit searches


Young self-luminous gas planets in star forming regions and

young associations

• Determine the initial frequency and distribution with mass and separation of giant planets

• This will allow extensive comparisons with models of planetary system formation and evolution


Limiting detectable mass of planets as a function of physical separation around a 10 Myr old

G2V star at a distance 120 pc

Uranus Neptune


Mature planets in the solar neighbourhood

• Frequency and mass distribution of giant planets at old ages, once dynamic evolution have cleaned systems from planets in unstable orbits, can be compared with the results obtained in star forming regions and young associations

• Systems may be studied in regions much closer to the central star with respect to the snow line, allowing exploring the HZ and even inner regions

• These observations are important forerunner for spatial missions for spectroscopy of Earth-like planets, clarifying which systems are most likely to host rocky planets in the HZ


• The expected frequency of low-mass planets at various separations from the central star is a basic parameter for models of planet formation.

Model by Mordasini et al.


Even low resolution and low S/N spectra of such objects would allow a first characterization of their atmosphere. This is extremely important because little is known about the range of possible variations for the atmospheres of low-mass planets, and moreover about the incidence of Earth-like (O2-dominated) atmospheres.


IFS & Pol. Analyzer

Monte Carlo simulations using MESS by M. Bonavita

SPHERE @VLT/GPI@Gemini

EPICS-IFS @E-ELT

EPICS-EPOL @E-ELT

1.5m space coronagraphs


IFS

E-POL

(Simu’s made using MESS By MBo)


Planets discovered by RV, astrometry and transit searches

• Breakthrough:– planet masses and even radii (transits)– stellar ages are (isochrones, magnetic

activity and rotation, kinematics, etc.). ideal benchmarks for the calibration of

models for sub-stellar objects.


Gl581d

RV Planets in the separation-contrast plane (J-band)


RV signal of detectable planets


~2012




~2014




~2020




~2022


SIM(Beichman et al. 2008)

Astrometric signal of detectable planets


~2012


SIM(Beichman et al. 2008)



~2014


SIM-LITE(Beichman et al. 2008)



~2020





~2022





~2020


• PLATO: ESA Cosmic Vison proposed mission for the search of transiting planets• Planets down to about 10 MEarth around K and M dwarfs with V=8.5-10 (bright end of

PLATO) can be detected also with EPICS• For K dwarfs, planets in the HZ are detectable• Availability of planet spectrum from EPICS and planet radius from PLATO will be

relevant for the physical study of the planets.• For G and F stars (and K and M dwarfs as well) planets at separation larger than that

accessible to PLATO can be detected, allowing to study the outer planetary system of PLATO targets

Synergy with PLATO


Documents

IAU Symp. 276, Torino, october 2010 R. Gratton 1, M. Kasper 2, C. Verinaud 3, M. Bonavita 1,4 + EPICS Science team Science with EPICS The E-ELT Planet