@ CFHT Isabelle Boisse (LAM) and the SPIRou team France, Canada, CFHT, Brazil, Hawaii, Taiwan, Switzerland & Portugal
Consortium PIs Jean-François Donati (IRAP, France) - René Doyon (Canada) Project scientists System Engineer Management SPIRou Science Consortium Xavier Delfosse (IPAG, France) - Etienne Artigau (Canada) Sebastien Baratchart (IRAP, France) Driss Kouach (IRAP, France) French institutes : IRAP, IPAG, LAM, IAP + 8 labos franciliens + data opened to all CFH community 100+ scientists from 10+ institutes in France, Canada, Brazil, Taiwan, Switzerland and Portugal Structured in 20 Working groups
Search of planets around M dwarfs Throughput Wavelength domain Spectral resolution RV stability Polarimetric capacities HARPS / SOPHIE SPIRou SPIRou optimized for accurate RV on M dwarfs
Technical details Simultaneous wavelength coverage: 0.98-2.35 μm (YJHK bands) Spectral resolution: 75 000 - RV precision 1m/s Circular and linear achromatic polarimetry SNR env. 100 (per 2.3 km/s/pix) @ H=11 in 1 hour Throughput (optics) > 50% Science array H4RG-15 (4096 x 4096 pix - 15 μm pixel)
Technical details Cassegrain unit with polarimeter (heritage from Espadons and HARPS) Fluoride optical fibers (circular & octogonal) & pupil slicer Cryogenic spectrograph cooled down @ 80 K and stable @ 2mK 2 cryocoolers - 1500 kg - 1.7 x 3.3 m No moving part in the spectrograph
Technical details
Instrument IRAP (Toulouse, Fr) Cassegrain unit, Slicer, Polarimeter, Management, Integration IPAG (Grenoble, Fr) Spectrograph optics LAM/OHP (Marseille, Fr) Data reduction Calibration module Geneva (Switzerland) Velocity reference module Univ. de Montréal/Laval Spectrograph camera, Data simulation & reduction, Optical design HIA (Canada) Cryostat & Optical bench, Management, Integration CFHT (Hawaii) Instrument control, Detector, Management ASIAA (Taiwan) Guiding camera
Schedule Ongoing construction optical bench @ NRC-H 2016 Integration in France Fall 2017 first light guiding camera @ ASIAA & CFHT Cass mechanics @ IRAP spectrograph collimator @ SESO
Science drivers Earth-mass planets around M-dwarfs Extension of the large programs on HARPS/SOPHIE Follow-up of transiting surveys Synergies with TESS, JWST, ALMA, PLATO & E-ELT M-Earth, APACHE, EXTRA, SPECULoOS Formation of stars and planets Magnetic topologies of young protostars (class I, ctts, wtts) Young hot Jupiters And Weather patterns on brown dwarfs Properties and formation of massive stars Exoplanet & Solar System planet atmospheres.
Observations 500-night SPIRou legacy survey Concept approved by CFHT board of directors in 2014 Dec Final proposal to be submitted to TAC by 2017 v1.0 du SPIRou Legacy Survey (SLS) https://spirou.irap.omp.eu/obser vations/the-spirou-legacy-sur vey 3 main components : env. 300 M dwarfs and 140 PMS stars SLS-PS: env. 275 nights (planet search) SLS-TF: env. 100 nights (transit follow-up) SLS-MP: env. 125 nights (magnetic protostars & planets) 100 nights / yr all observed in polarimetric mode Open time PI proposals 30 % of SPIRou time
WP1 : detecting low-mass planets WP1.1 : Input catalog Determine the input catalog before the observation and optimize it during the survey to optimize planets detection list all relevant parameters (mass, age, temperature, rotation period, [Fe/H] ) conduct preparatory observations as needed WP2 : RV follow-up of transiting pl. WP1.2 : Planets detection Organize / optimize SPIRou RV Survey to detect low-mass planets at short orbital periods (<150 d) (in particular in HZ) Organize / optimize SPIRou RV Survey to detect planets at larger period and multi-system Search for planets and determine orbital elements WP1.3 : Detection limits and statistics Determine detection limits of RV survey Determine frequency occurrence of planets around M dwarfs Compare with theoretical model of planetary formation WP5 : Study common to all SPIRou Legacy Survey WP4 : common studies of planetary system WP1.4 : Photometric follow up of SPIRou Planets Organize photometric follow up by ground (ExTrA, ) Organize photometric follow up by space (CHEOPS, ) WP3 : Exploring stars and planets formation WP2.1 : target selection Establish criteria for target selection to optimize scientific return with SPIRou Collect data from : WP2.1.1 : TESS WP2.1.2 : K2 WP2.1.3 : ExTrA WP2.1.4 : NGTS list all relevant parameters (mass, age, temperature, rotation period, [Fe/H] ) WP3.1 : Input catalog Determine the input catalog before the observation and optimize it during the survey Select embedded class-i protostars, ctts, wtts list all relevant parameters (mass, age, temperature, veiling, accretion, rate, rotation period, ) conduct preparatory observations as needed WP2.2 : Planet characterization Organize / optimize SPIRou RV survey to identify planets among transiting candidates and measure the planetary mass /Determine orbital parameters Identify planetary candidate and adapt strategy for planet mass characterization Search for another planets in the system Model fitting to analyse RV and photometric data Study exoplanet internal structures & compare w/ observations WP3.3 : Characterize inner accretion disc Organize complementary SPIRou observations Detect emission lines from innermost regions of accretion disc in class-i protostars & cttss characterize disc large-scale fields using zeeman signatures monitor best target reassess origin of disc field & impact on planet formation WP2.3 : Complementary observations Target selection from WP1.4 and WP2.2 Target selection from others surveys Organize complementary observation on sources detected (from WP1.2) or confirmed (from WP2.2) with SPIrou : SPIRou measurement of Rossiter SPIRou measurement of transmission and emission spectrum Organize complementary obs with JWST Organize complementary obs with ELT Organize complementary obs with CHEOPS.. Compare planetary spectrum with theoretical models of planet atmospheres WP4.1 : RV optimization Optimize RV extraction Telluric line subtraction linked to the Data processing center WP5.1 : Spectral analysis Analyse SPIRou spectra Determine or Redetermine stellar parameters for all stars (Teff, logg, [Fe/H], activity, rotation) Locate them accurately in HR diagram WP4.2 : filtering activity filter activity jitter from RV curves Use simultaneous spectropolarimetry Look for correlations between spot distributions and largescale magnetic topologies; WP4.3 : Dynamics Study stability of multi-planets system Study evolution of the system Compare w/ observation WP5.2 : Stellar magnetic properties of Mdwarfs Monitor rotational modulation & reconstruct large scale magnetic field Investigate how large-scale fields vary with stellar parameters among M dwarfs and lowmass protostars; compare w/ theoretical dynamo models of fullyconvective and non-fully-convective stars; Investigate the link between magnetic properties and stellar activity WP3.2 : Large-scale fields of low-mass protostars Organize / optimize SPIRou Zeeman Survey Monitor rotational modulation & reconstruct large scale magnetic field Study how magnetic topology & accretion patterns depend on stellar parameter compare w/ dynamo models of PMS stars WP3.4 : Search for hot Jupiter Search for hot jupiter in RV curves of wtts Derive statistics Compare to formation model WP3.5 : Complementary observations & modeling organize complementaty observations : photometry, optical spectroscopy, X-rays (Chandra, XMM), radio (ALMA, NOEMA) Model corona winds & magnetospheric accretion Model properties of accretion funnels, shock & post-shock region, improve accretion model observe and model jets WP4.4 : Star-planet interaction Study tidal effect (synchronization, ) Study magnetic interaction WP4.5 : Habitable zone Determine habitable zone for planetary system detected Model planetary climate The SLS Data available to all registered users i.e. CFHT community + SPIRou partners (limited number) + scientists bringing expertise to the SLS (limited number) Agreement on data access & Publication policy Publication involve all sub-wp members WP5.3 : Earth atmosphere Model telluric lines in reduced spectra and derive atmospheric properties (e.g., column densities of atmospheric molecules, wind speeds) and their evolution with time compare with similar data obtained at other sites (e.g., CSO, ESO).
Data center At LAM The DRS will be improved to correct : instrumental noise (background light,.) telluric line corrections Provide ultimate version of processed data raw/reduced data available to all registered user via password proprietary period (12 + 12 months) user support Archive At CFHT data processed with latest version of the DRS free access to the DRS
PLATO mission M3 ESA Select to flight in 2024 Search for planets in transit Preparation work Selection of the fields - and finalise the observational strategy Collect all available spectra on the possible targets of the field Data center of complementary data spectra, RV, imaging,. at LAM
Resume spirou.irap.omp.eu 0.9-2.5 μm - RV accuracy 1m/s First light fall 2017 Polarimetric mode 2 major science goals Habitable Earth like planets around M dwarfs Formation of stars and planets via magnetic topologies of young protostars