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

Gaudi & Winn (2007)

The shape of the RM anomalydepends on the trajectory of the transiting planet.

What can we learn from RM effect observations?

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

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).

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

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<13, DEC>-30 and VsinI>1km/s

spanning a range of stellar and planet properties

Excluded objects with:

RM effect already measured

Kepler targets

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

RVC from Alsubai (2010)

Observed R-M effect

Qatar-1 spectroscopic orbit

New orbital solution based on HARPS-N data consistent with a circular orbit

P=1.42002449±0.0000010 d

Qatar-1 spectroscopic characterization

Results from MOOG:

Teff

=4820±50 KLogg=4.43±0.10

ξ=0.90±0.05 km/s logn(FeI)=7.68±0.09logn(FeII)=7.68±0.06[FeI/H]=0.25±0.10[FeII/H]=0.25±0.12

vsini=2.5±0.5 km/s

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

Asiago CA Alsubai ETD

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 profileThe model considers the actual area of the disc that is occulted during an exposureand the phase smearing due to the planet's displacement.

Qatar-1 RM effect model

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

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

Orbit Star Planet

P = 1.4200239 ± 0.0000010 days M* = 0.85 ± 0.03 M

SunM

pl = 1.33 ± 0.05 M

Jup

a = 0.0023 ± 0.0002 AU R* = 0.80 ± 0.12 R

SunR

pl = 1.21 ± 0.19 R

Jup

e = 0.020 ± 0.010 Teff

= 4820 ± 50 K ρpl

= 0.75 ± 0.42 ρJup

i = 83.82 ± 0.25 deg log(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

T14

= 0.067491 ± 0.000018 days ξ = 0.90±0.05 km/s

TC

= 2455518.41131 ± 0.00039 BJD

±deg

Qatar-1 system properties

Qatar-1 system properties

New RVC solution consistent with a circular orbit

Orbit well aligned within uncertainties with star spin axis

Determination of star Teff, log g, [Fe/H], vsinI from

Estimated star Prot ~20 days yields agegyro of ~1.3 Gyr (for B-V=0.9, using Eq. 3 of Barnes 2007)

Porb much shorter than stellar Prot implies that tidal interaction is causing angular momentum to be tranferred from planet orbit to the star, and planet is going to be engulfed.

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

THANK YOUTHANK YOU

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