GAPS2: the origin of planetary systems diversity

Transcription

1 ETAEARTH European Union Seventh Framework Programme (FP7/ ) grant agreement GAPS2: the origin of planetary systems diversity Luca Malavolta 1,2 & GAPS2 Collabora6on 1: INAF - Osservatorio Astronomico di Padova 2: Dipar6mento di Fisica e Astronomia Galileo Galilei - Universita di Padova HoRSE 02/10/2018 Nice

2 HARPS-N TNG Telescopio Nazionale Galileo La Palma

3 Global Architecture of Planetary Systems GAPS: 30 to 40 nights/semester from AOT32 Nearly 8000 spectra for more than 300 objects 78 INAF/associates + 19 foreigners Regular meetings to keep track of advancements Strong involvement of young researchers 25 refereed papers + submitted / in preparation Detection of low-mass planets around M dwarfs (Affer+2016, ) The first multi-planet system in an open cluster (Malavolta+2016) Rossiter-McLaughlin for a large sample of planets (Covino+2013, ) Detection of a giant planet around a red giant (Gonzalez Alvarez+2017) Search for low mass planets orbiting M dwarfs Search for low mass companions in known planetary systems Frequency of Neptune-mass companions around Low [Fe/H] stars Search for GP orbiting stars in crowded environments Characterization of planetary orbits through RML effect Asteroseismology Star-Planet Interaction The first wide binary in which both components host planets (Desidera+2014) Giant planet migration history via improved parameters for 231 planets (Bonomo+2017)

4 HARPS-N and GIANO-B + HARPS-N Luca Malavolta GIANO-B HoRSE 02/10/2018 Nice

5 HARPS-N + GIANO-B = GIARPS + = HARPS-N Luca Malavolta GIANO-B HoRSE 02/10/2018 Nice

6 HARPS-N + GIANO-B = GIARPS + = HARPS-N Luca Malavolta GIANO-B d n a i t t e Por o i n n E See lks a t y u l l i u Gloria G, Lorenzo Pino o m o n o B + Aldo HoRSE 02/10/2018 Nice

7 GAPS2: The origin of planetary diversity Phenomenon Site of planet formation and migration path towards their host star Hot and warm Neptunes formation and migration; similarity or difference from Jovian or small-size planets Migration path: disc and/or high eccentricity migration Giant planets effects on formation of small planets, especially in the HZ

8 GAPS2: The origin of planetary diversity GAPS2: Large Program status 306 hours / semester allocated PI: Giusi Micela (INAF-OAPa) Phenomenon Site of planet formation and migration path towards their host star Hot and warm Neptunes formation and migration; similarity or difference from Jovian or small-size planets Migration path: disc and/or high eccentricity migration Giant planets effects on formation of small planets, especially in the HZ

9 Chemical composition of protoplanetary disk Phenomenon Site of planet formation and migration path towards their host star Effects Atmospheric composition enriched by the chemical elements at the formation site and encountered during migration High C/O low O/C

10 Planetary atmospheres as proxy of formation environment Phenomenon Effects Observables Site of planet formation and migration path towards their host star Atmospheric composition enriched by the chemical elements at the formation site and encountered during migration Atmospheric composition: C/O and O/H ratios, Na, TiO, CH 4 and CO 2 abunudances HARPS-N GIANO-B Wasp-39b, Wakeford+2018

11 Cross-correlation function to detect water Water on HD using GIANO, Brogi+2018 HARPS-N GIANO Pino+2018

12 Planetary atmospheres as proxy of formation environment 26 hot Jupiters in a wide range of masses, radii, and irradiation conditions 4 hot- and sub- Neptunes Observables Identify the individual contributions from species such as Na, TiO (VIS) and H 2 O, CO, CH 4* and CO 2* (NIR) Presence of hazes/clouds Determine atmospheric Temperature-Pressure profiles Constraints on fundamental proxies of the HJs formation location and migration history, e.g. the C/O and O/H ratios (HiRes GIARPS + LowRes HST/JWST data) *very high S/N required Large Program Plan We need to observe the full transit, several times. Scheduling limitations requires nights across severalsemesters

13 Observing the origin of planetary architecture Phenomenon Effects Observables Migration path: disc and/or high eccentricity migration of gas giants Hot and warm Neptunes formation and migration; similarity or difference from Jovian planets or small-size ones Low vs. high eccentricity and/or obliquity. Differentmigration timescales Different orbital parameters (eccentricity and/or obliquity); different mass-radius relations Orbital parameters of hot/warm Jupiters as a function of age. Frequency of young hot/warm planets Orbital and physical (mass, radius, density) parameters of hot and warm Neptunes as a function of stellar age Young planets in young clusters: Cepheus (10 Myr) Upper Scorpius (11 Myr) Taurus (15 Myr) Columba (42 Myr) Hercules-Lyrae (250 Myr) Ursa Mayor (450 Myr) Coma Berenices (590 Myr)

14 Observing the origin of planetary architecture Phenomenon Effects Observables Giant planets effects on formation of small planets, especially in the HZ Different architectures of planetary systems in the presence or absence of giants Occurrence of small (HZ) planets in the presence of long-period giants High frequency of Super- Earth around M dwarfs (50%) without gas giants Search for Super-Earth around M dwarfs with gas giants Large Program Plan Around 10 M0-M2 dwarfs with V 11 mag not included in the CARMENES input catalog. First half of the project: known long-period giant planet observable with GIARPS Second half of the project: targets from bright, slowly rotating, inactive M dwarfs candidates from TESS and Gaia, to be observed with HARPS-N

15 The Spectral Lines Of Planets with Python (SLOPpy) pipeline Developed by Daniela Sicilia (UniPD & INAF-OACt) and LM Automatic and homogeneous extraction and analysis of transmission spectra for HARPS and HARPS-N (for now ) Telluric correction and transmission spectrum in the full wavelength range Wyttenbach et al. 2015

16 Philosophy behind SLOPpy Modularity The user can easily change or remove every reduction step or dataset Reproducibility For a given configuration file, the user always get the same result

17 Philosophy behind SLOPpy Modularity The user can easily change or remove every reduction step or dataset Reproducibility For a given configuration file, the user always get the same result Separate computing/plotting blocks Batch execution on large datasets

18 Philosophy behind SLOPpy Modularity The user can easily change or remove every reduction step or dataset Reproducibility For a given configuration file, the user always get the same result Separate computing/plotting blocks Batch execution on large datasets Data persistence User can easily retrieve results from a previous steps WORK IN PROGRESS

19 PyORBIT a code for exoplanet orbital parameters and stellar activity. github.com/lucamalavolta/pyorbit Wide selection of models: Gaussian Processes for RV or photometry (shared or independent hyperparameter) Polynomial trends Correlation with activity indexes Sinusoids (independent or shared amplitudes and periods) Celeritesupport (untested) Friendly human documentation! Featured: Malavolta+2016, Benatti+2017, Malavolta+2017, Malavolta+2018, Lanza+2018, Kosiarek+(sub), Rice+(sub) Priors: Uniform / Gaussian / (Modified) Jeffrey / Truncated Rayleigh / Beta Distribution they can be applied to any parameter Bayesian model selection with nested sampling (MultiNest/PolyChord) More stuff that doesn t fit in the page Global exploration of parameter space: PyDifferentialEvolution -> emcee Parameter exploration in Linear/Logarithmic space (your choice) YAML interface, no need to know Python!

20 Hot/Warm Jupiters and Neptunes around young stars GAPS2 Atmosphere of Hot Jupiters and Neptunes Super-Earths with giant companions in M dwarfs The Spectral Lines Of Planets with Python (SLOPpy) pipeline: automatic and homogeneous extraction and analysis of transmission spectra Thank you for your attention