1. Results of HARPS-N observations of the transiting system Qatar-1 in GAPS E. Covino M. Esposito, M. Barbieri, S. Desidera, L. Mancini, V. Nascimbeni, J. Southworth, A. Sozzetti, R.Claudi, K. Biazzo, N. Lanza, G. Piotto, & GAPS team GREAT-ESF Gaia and Exoplanets Workshop – Turin 5-7/Nov/2012 GREAT-ESF Gaia and Exoplanets Workshop

2. Gaudi & Winn (2007) The shape of the RM anomaly depends on the trajectory of the transiting planet. What can we learn from RM effect observations?

3. Why is the RM effect interesting? Type II migration: disk-planet interaction small eccentricity and inclination  roughly explains semi-major axis distribution (Ida & Lin 2004)  cannot explain eccentric planets Jumping Jupiter model: multiple-planet interaction + scattering Kozai migration: perturbation by off-plane massive companion possible large eccentricity and inclination  explain eccentricity distribution when combined with Type II migration models is connected with the planet migration mechanism

4. Observational panorama ~60 systems with RM effect measured Most planets are aligned (| |<30º). Misaligned planets seem more frequent around slightly more evolved stars or hotter than ~6000K (Winn et al. 2010), though still an open issue (Moutou et al. 2011).

5. Motivation of the GAPS RM effect subprogram derived via the RM effect is an important constraint on spin-orbit alignment and a basic parameter to characterize planetary orbits and test planet migration models Study tidal interaction with host star of close-in GPs Confirmation of transiting planet candidates Study of RM effect for transiting planets provides clues on architecture and orbital evolution of planetary systems

6. The GAPS RM-effect subprogram: targets This sub-program of GAPS is aimed to determine/improve fundamental orbital parameters for transiting planets, i.e. derive the spin-orbit misalignement through observation of the Rossiter-McLaughlin (RM) effect Selected Targets include stars with: V -30 and VsinI>1km/s spanning a range of stellar and planet properties Excluded objects with: RM effect already measured Kepler targets

7. HARPS-N observations of the transiting system Qatar-1 Hot Jupiter orbiting a (V~12.8mag) metal-rich K-dwarf star in about 2.4 days (Alsubai 2010) Obtained 11 spectra (exp-time=900s, S/N~30 at 6000Å, σ RV ~4.5m/s) covering transit on September 3: RM effect successfully detected Out-of-transit data gathered in six following nights (Sep 5, 6, 7, 8, 9, 11): new RVC solution

8. RVC from Alsubai (2010) Observed R-M effect

9. Qatar-1 spectroscopic orbit New orbital solution based on HARPS-N data consistent with a circular orbit P=1.42002449±0.0000010 d

10. Qatar-1 spectroscopic characterization Results from MOOG: T eff =4820±50 K Logg=4.43±0.10 ξ=0.90±0.05 km/s logn(FeI)=7.68±0.09 logn(FeII)=7.68±0.06 [FeI/H]=0.25±0.10 [FeII/H]=0.25±0.12 vsini=2.5±0.5 km/s

11. Ancillary data: transit R-band photometry Asiago 1.82m tel.: Date RMS (mmag) 29/05/2011 3.4 (0.95) 24/08/2012 2.6 (1.04) Calar Alto 1.23m tel.: Date RMS (mmag) 25/08/2011 1.62 21/07/2012 0.82 10/09/2012 0.87 Asiago CA Alsubai ETD

12. Adopted model as in Queloz et al. (2000), based on the following assumptions: average line profile as from CCF; stellar disc modelled by a 2000x2000 matrix, each element contributing with a Gaussian line profile (macroturbulence), characterized by a given velocity along the line-of-sight due to stellar rotation and limb-darkening coefficients (Claret 2004). Total profile resulting from convolution with HARPS-N instrumental profile The model considers the actual area of the disc that is occulted during an exposure and the phase smearing due to the planet's displacement. Qatar-1 RM effect model

13. Qatar-1 phase-smearing in RM effect The model takes into account the actual area of the disc that is occulted during each (900s) exposure and the phase smearing due to the planet's displacement. Total transit duration ~1.62 hours

14. Qatar-1 phase-smearing in RM effect The model takes into account the actual area of the disc that is occulted during each (900s) exposure and the phase smearing due to the planet's displacement. Total transit duration ~1.62 hours

15. Orbit Star Planet P = 1.4200239 ± 0.0000010 daysM * = 0.85 ± 0.03 M Sun M pl = 1.33 ± 0.05 M Jup a = 0.0023 ± 0.0002 AUR * = 0.80 ± 0.12 R Sun R pl = 1.21 ± 0.19 R Jup e = 0.020 ± 0.010T eff = 4820 ± 50 Kρ pl = 0.75 ± 0.42 ρ Jup i = 83.82 ± 0.25 deglog(g) = 4.43 ± 0.10 b = 0.675 ± 0.016[FeI/H] = 0.25 ± 0.10 K = 266 ± 4 m/s VsinI = 2.5 ± 0.5 km/s = 1.5 ± 0.6 km/s T 14 = 0.067491 ± 0.000018 daysξ = 0.90±0.05 km/s T C = 2455518.41131 ± 0.00039 BJD    ±  deg Qatar-1 system properties

16.  New RVC solution consistent with a circular orbit  Orbit well aligned within uncertainties with star spin axis  Determination of star T eff, log g, [Fe/H], vsinI from  Estimated star P rot ~20 days yields age gyro of ~1.3 Gyr (for B-V=0.9, using Eq. 3 of Barnes 2007)  P orb much shorter than stellar P rot implies that tidal interaction is causing angular momentum to be tranferred from planet orbit to the star, and planet is going to be engulfed.

17. Conclusions  New RVC solution consistent with a circular orbit  Orbit aligned within the uncertainties with spin axis  System properties derived  Planet is going to be engulfed by the star  Test of HARPS-N performances

18. THANK YOU

20. Ancillary data: transit R-band photometry Asiago 1.82m tel.: Date RMS (mmag) 29/05/2011 3.4 (0.95) 24/08/2012 2.6 (1.04) Calar Alto 1.23m tel.: Date RMS (mmag) 25/08/2011 1.62 21/07/2012 0.82 10/09/2012 0.87 Asiago CA Alsubai ETD