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Hot Jupiters with Relatives: Discovery of Additional Planets in Orbit Around WASP-41 and WASP-47 ∗ M Astronomy & Astrophysics manuscript no. W41c_W47c_corr c ESO 2018 October 1, 2018 Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47 ∗ M. Neveu-VanMalle1; 2, D. Queloz2; 1, D. R. Anderson3, D. J. A. Brown4, A. Collier Cameron5, L. Delrez6, R. F. Díaz1, M. Gillon6, C. Hellier3, E. Jehin6, T. Lister7, F. Pepe1, P. Rojo8, D. Ségransan1, A. H. M. J. Triaud9; 10; 1, O. D. Turner3, and S. Udry1 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland 2 Cavendish Laboratory, J J Thomson Avenue, Cambridge, CB3 0HE, UK 3 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 4 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 5 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK 6 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bat. B5C, Liège 1, Belgium 7 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr. Suite 102, Goleta, CA 93117, USA 8 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 9 Centre for Planetary Sciences, University of Toronto at Scarborough, 1265 Military Trail, Toronto, ON, M1C 1A4, Canada 10 Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, Canada e-mail: [email protected] Received July 15, 2015; accepted September 30, 2015 ABSTRACT We report the discovery of two additional planetary companions to WASP-41 and WASP-47. WASP-41 c is a planet of minimum mass 3.18 ± 0.20 MJup and eccentricity 0.29 ± 0.02, and it orbits in 421 ± 2 days. WASP-47 c is a planet of minimum mass 1.24 ± 0.22 MJup and eccentricity 0.13 ± 0.10, and it orbits in 572 ± 7 days. Unlike most of the planetary systems that include a hot Jupiter, these two systems with a hot Jupiter have a long-period planet located at only ∼1 au from their host star. WASP-41 is a rather young star known to be chromospherically active. To differentiate its magnetic cycle from the radial velocity effect induced by the second planet, we used the emission in the Hα line and find this indicator well suited to detecting the stellar activity pattern and the magnetic cycle. The analysis of the Rossiter–McLaughlin effect induced by WASP-41 b suggests that the planet could be misaligned, though an aligned orbit cannot be excluded. WASP-47 has recently been found to host two additional transiting super Earths. With such an unprecedented architecture, the WASP-47 system will be very important for understanding planetary migration. Key words. planetary systems – stars: individual: WASP-41 – stars: individual: WASP-47 – Techniques: photometric – Techniques: radial velocities – Techniques: spectroscopic 1. Introduction locity surveys, Feng et al. (2015) recently constrained the orbits of the distant (P > 9 years) giant planets in orbit around the hot- In contrast to the large number of multiple planetary systems, Jupiter hosts HD 187123 and HD 217107. Among all systems stars with hot-Jupiter planets have long been thought to lack ad- with a close-in giant planet discovered by transit surveys, only ditional planets. Recent studies suggest that this statement may HAT-P-13 (Bakos et al. 2009), HAT-P-46 (Hartman et al. 2014), not be true (e.g. Knutson et al. 2014). However the existence of and Kepler-424 (Endl et al. 2014) have an additional planetary those additional planets was revealed by nothing more than ra- companion detected by Doppler surveys with a fully measured dial velocity trends. Only seven outer planetary companions of orbit. close-in (a < 0.1 AU) giant planets have a full orbital period that The Wide Angle Search for Planets (WASP, Pollacco et al. has been observed. 2006) has discovered more than 100 hot Jupiters. While some The multiple planetary system around υ Andromedae (But- of them clearly have a very distant companion (e.g. WASP-8, arXiv:1509.07750v2 [astro-ph.EP] 20 Oct 2015 ler et al. 1997) was the first to be found with a hot Jupiter. This Queloz et al. 2010), none of them were previously known to have planet is surrounded by three more massive giant planets orbiting a fully resolved orbit. between 0.8 and 5 au (Curiel et al. 2011). Ten years later, the dis- covery of the planetary system around HIP 14810 (Wright et al. The radial velocity follow-up observations of WASP initi- 2007, 2009) revealed that a hot Jupiter can be found in a system ated in 2008 with the fibre-fed echelle spectrograph CORALIE with smaller planets on wider orbits. From 15 years of radial ve- (mounted on the 1.2-m Euler Swiss telescope at La Silla) has identified new multiple systems including a hot Jupiter. We re- ∗ Using data collected at ESO’s La Silla Observatory, Chile: HARPS port here the detection of additional planets around WASP-41 on the ESO 3.6m (Prog ID 087.C-0649 & 089.C-0151), the Swiss Euler (Maxted et al. 2011) and WASP-47 (Hellier et al. 2012). These Telescope, TRAPPIST, the 1.54-m Danish telescope (Prog CN2013A- new planets are both located only ∼1 au of their parent star. 159), and at the LCOGT’s Faulkes Telescope South. The data is publicly When searching for long-period companions using the radial ve- available at the CDS Strasbourg and on demand to the main author. locities technique, the effects of stellar activity should be care- Article number, page 1 of 18 A&A proofs: manuscript no. W41c_W47c_corr fully considered to avoid misdetections. A stellar magnetic cycle used in our analysis to characterise the transiting planet WASP- may mimic the signal of a planetary companion (e.g. Lovis et al. 47b were 2011). WASP-41 is known to be active (Maxted et al. 2011), which makes it important to recognise the temporal structure of – the transit depth defined as the planet/star area ratio (dF = 2 its magnetic cycle. Since the photospheric Ca (H & K) emission (Rp=R?) ), where Rp and R? are the planetary and stellar ra- lines cannot be extracted from single CORALIE spectra (insuffi- dius, respectively; cient signal-to-noise ratio), we alternatively use the emission in – the transit impact parameter in the case of a circular orbit 0 the Hα band to characterise activity. We find that this indicator (b = ab cos ip;b=R?), where ab and ip;b are the semi-major is very well suited to WASP-41, though it may not be true in axis and the inclination of the planetary orbit, respectively; general (Cincunegui et al. 2007). – the transit duration T14, from first to last contact; Section 2 reports the observations, analysis, and results for – the orbital period Pb; WASP-47. Section 3 similarly addresses the case of WASP-41 – the time of inferior conjunctionp T0;b; p with a description of the various additional observations, a study – the two parameters eb cos !b and eb sin !b, where eb is the eccentricity and ! the argument of periastron; of the stellar activity, and an analysis that includes the Rossiter– b q 2 1=3 McLaughlin effect followed by the results. In section 4, after – the parameter K2;b = Kb 1 − e P , where Kb is the radial discussing the importance of considering magnetic cycles when b b velocity semi-amplitude. searching for long-period planets, we compare our two multi- ple planetary systems, including a hot Jupiter, to the five previ- For the period Pb and time of inferior conjunction T0;b, we im- ously known ones. We discuss the biases induced by the observ- posed Gaussian priors defined by the values derived in Hellier ing strategies of Doppler and transit surveys in finding multiple et al. (2012), since we did not include the WASP photometry planetary systems including a hot Jupiter. Finally we check the in our analysis. Uniform priors were assumed for the probabil- transit probabilities of WASP-47c and WASP-41c. ity distribution functions of all the other jump parameters. The During the process of revision of this paper, (Becker et al. choices of jump parameters were optimised to reduce the depen- 2015) reported the presence of two additional super-Earths tran- dencies between the parametersp and thus to minimisep the corre- siting WASP-47 every ∼0.8 and 9 days. This remarkable discov- lations. We checked that using e cos ! and e sin ! as jump ery brings strong constraints on the migration of this system and parameters translates into a uniform prior on e and does not in- will be discussed in the last section. fluence the results. We modelled the limb-darkening with a quadratic law, where instead of the coefficients u and u , we used the combinations 2. WASP-47 c 1 2 c1 = 2×u1 +u2 and c2 = u1 −2×u2 as jump parameters in order to 2.1. Observations minimise the correlation of the obtained uncertainties (Holman et al. 2006). We assumed normal priors on u1 and u2 with the WASP-47 is a G9V star hosting a giant planet with a mass of values deduced from the tables by Claret & Bloemen (2011). As 1.14 MJup and a period of 4.16 days (Hellier et al. 2012). The described in Gillon et al. (2012), we applied a correction factor discovery paper includes 19 radial velocity measurements taken CF = 1:32 to the error bars of the photometric data to account with CORALIE during two observing seasons. Ongoing moni- for the red noise.
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