Extrasolar Planet Science with High-Precision Astrometry Johannes Sahlmann

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1 Extrasolar Planet Science with High-Precision Astrometry Johannes Sahlmann Geneva Observatory The First Years Of ESO, Garching,

2 high-precision astrometry is powerful yields complete information, sensitive to orbit inclination -> ideal tool to determine the accurate planet mass distribution does not require spectral lines -> possible to target faint objects, e.g. brown dwarfs less sensitive to activity than radial velocity & transit method -> adapted to the search for planets around young/active stars

3 high-precision astrometry is powerful, but yet limited by the achievable precision a 1,min (mas) e 6 HIPPARCOS Period (years) exoplanet.eu

4 astrometry constrains the true companion mass of RV companions radial velocities yield P, T, e, ω, K1 J. Sahlmann et HIPPARCOS astrometry (van Leeuwen, 27) CORALIE + HIPPARCOS 1 i and Ω from astrometry rch for brown-dwarf companions of stars.. IE 1. CORALIE 1!!1!!1!1 1.1 E ! HD43848 M2 sin i = 49 ± 2 MJup!2 Brown dwarf?. CORALIE+MIKE. i 2 = ±. deg!!1!1 M2 =.2 ±. M 1!1 Sahlmann et al., 211, A&A, 2!4 1!"* (mas) 2!2! N M-dwarf! 1 O C (mas) RV [m/s] 1!# (mas)!# (mas) 1 O C (mas) IE HD RV [m/s] 2 HD17289!!1

5 the upper mass limit for planets orbiting Sun-like stars revealed with astrometry RV: 2 candidate brown dwarf companions in uniform sample (CORALIE) Astrometry: 1 companions have true masses > 8 M Jup, thus are M-dwarfs 1 BD companions remain in the sample of 1647 stars..6 ±.2 % of Sun-like stars have a brown dwarf companion within 1 AU. Norm. fraction M 2 sin i (M Jup ) true masses? µas astrometry Cumulative distribution Sahlmann et al., 211, A&A, 2 1 Planets void BDs M 2 sin i (M J ) upper planet mass limit at ~2-3 M Jup Sahlmann et al., 211, IAUS 276

6 an IR-interferometer can realise 1 µas astrometry Ref. Target Target 3 arcsec T2 Baseline Beam combination T1 Reference K-band image of an ESPRI target. single-reference relative astrometry within a narrow field (~3 ) in K-band interference fringe separation in delay space is proportional to angular separation atmospheric limit: 1 µas for 3 min integration and a 1 m baseline (Shao & Colavita, 1992) sufficient for exoplanet detection around one of the stars

7 Exoplanet search with PRIMA PRIMA is the dual-feed facility of the VLTI Delplancke et al., 26 ESPRI = MPIA Heidelberg + LSW Heidelberg + Observatoire de Genève targets: hosts of RV planets, young stars, nearby main-sequence stars ESO/ G. Hüdepohl accuracy requirement: 1-1 µas under commissioning at Paranal observatory Launhardt et al., 28

8 binary star observations with PRIMA Δδ (arcsec) HD136 NACO Δ α* (arcsec) Δα * (arcsec) HD WDS PRIMA Δ δ (arcsec) Nov 211 Jul 211 NACO Δ α* (arcsec) Nov 21 WDS PRIMA O C (arcsec). 24(18) µas! Δα* (mas) Years 2(23) since (24) 23(12) 2(6) Δδ (mas) (18) (18) (23) (24) (6) 2Δα* (mas) 4 Δα* (mas) 2(23) 2(24) 23(12) 2(6) (12) (24) (18) (6) (23) precision is sufficient but biases are yet too large for the planet search 2 4 Δα* (mas) (12) work in progress Sahlmann et al., in prep.

9 A FORS2/VLT search for planets around late-m and L dwarfs Are the conditions for planet formation met around ultra-cool dwarfs? 4.1 Data reduction ESO 81

10 FORS2/VLT is capable of 1 micro-arcsec astrometry Principles Lazorenko & Lazorenko 24, Lazorenko 26 - optical imaging with an exquisite camera + large telescope - large number of reference stars - detailed modelling of PSF distortions and atmospheric image motion Performance Lazorenko et al. 27, 29, precision of ~ µas on time scales of days-years - refuted planet around VB1 Planet search survey of 2 targets (ongoing) 2 late-m and early-l dwarfs close to the galactic plane within 3 pc 2-year programme: 1 epochs per target 1 nights of FORS2 (21-212) Detection limit ( M Neptune ) 2 1 at 3 pc 2 at 1 pc Orbital Period (days)

11 measuring parallax and proper motion 2 Dwarf 4 1 Δ δ (mas) 1 average epoch uncertainty: 11 µas residual dispersion: 14 µas Δ δ (mas) Δ α* (mas) parallax /-.6 mas (relative) proper motion RA /-.9 mas/yr proper motion DE /-.7 mas/yr Δ α* (mas) Δ α* (mas) 177

12 preliminary results Frequency epochs median precision: 11 µas residual dispersion: 134 µas Modulus (milli arcsec) 1. The long-term accuracy is < 13 µas per epoch. Better than GAIA for faint targets! 2. Exclude planets more massive than Jupiter in intermediate periods (~-4 days) for several targets. Sahlmann et al., in prep.

13 Conclusions High-precision astrometry is powerful: revealed upper-mass limit for planets around Sun-like stars Better than 1 milli-arcsec astrometry is required to reach into the Jupiter-mass domain: 1. PRIMA/VLTI has the potential: 3 micro-arcsec precision demonstrated, but ESPRI planet search inhibited by systematic errors limiting the astrometric accuracy to > 3 mas (so far!) 2. FORS2/VLT realises 13 micro-arcsec accuracy -> exploring the population of planets around ultra-cool dwarfs (+ ultra-precise distances + BD binaries) General-user ground-based facilities for high-precision astrometry can deliver great science. Synergies (e.g. preparation + follow up) with fixed-duration space missions (GAIA). Unique capabilities present at ESO: Imaging with (extremely) large telescopes + Interferometer

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