PoS(FRAPWS2016)069 , I. , A. 3 7 http://pos.sissa.it/ , G. Micela , E. Covino 2 6 ], a system of Super-Earths 2 , A.F. Lanza and the GAPS Team 1 9 , R. Cosentino 1 , R. Gratton 1 , R. Smareglia , C. Boccato 8 5 ]. 3 , S. Desidera 1 , E. Poretti 6 , A. Sozzetti 4 , R.Claudi 1† ∗ ], the first planetary system around a in an open cluster [ , G. Piotto , E. Molinari 2 1 3 [email protected] Speaker. SB acknowledges the support from INAF trough the "Progetti Premiali" funding scheme of the Italian Ministry of orbiting an M-dwarf star [ The GAPS programme is an Italian projectsystems aiming around to search and with characterize extra-solar differentborn planetary characteristics in (mass, 2012, , when environment). singleobserving research GAPS program groups for was joined the in exploitation order oftrograph, the to mounted extraordinary at propose performances the a of Telescopio Nazionale long-term the Galileo. multi-purpose in HARPS-N Now spec- which this group wide is range a concerted ofrole community expertise in the and wider capabilities international are context.radial shared We present velocity in the order survey: results to achieved they up reachplanet to were a detection now more obtained from and the important in the GAPS we both characterization detected, the of for already two instance, the known main firstets exoplanetary objectives confirmed [ systems. of binary system the in With project, which GAPS both the components host plan- ∗ † Copyright owned by the author(s) under the terms of the Creative Commons INAF - Astronomical Observatory of Padova INAF - Astrophysical Observatory of Catania INAF - Astronomical Observatory of Palermo University of Padova, Dep. of PhysicsINAF and - Astronomy Astronomical Observatory of Torino INAF - TNG, Fundación Galileo Galilei INAF - Astronomical Observatory of Capodimonte INAF - Astronomical Observatory of Brera INAF - Astronomical Observatory of Trieste c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Education, University, and Research. Frontier Research in Astrophysics – II 23-28 May 2016 Mondello (Palermo), Italy S. Benatti 1 2 3 4 5 6 7 8 9 E-mail: The GAPS Project: First Results Pagano Maggio PoS(FRAPWS2016)069 , ], K 4 the e , of the i S. Benatti the and , and a semiamplitude, ? P M 2 / 1 ) 2 e 1 − 1 ( 3 / 2 ) i ? M sin p + 1 M p M ( 3 / 1  G P π 2  = K 100 RV epochs) in order to separate the single signals. Moreover, the RV ∼ , while an Earth-like planet at the same distance induces a RV modulation of only 1 − ]. The improvements in the technological capabilities, together with the complemen- 8 ]). In particular, low-mass planets (in the range between Super-Earths and Neptunes) 7 . The detection of multiple systems with low-mass components requires a particular 1 ], [ − 6 The main purpose of GAPS is the study and the characterization of the architectural proper- The results of the NASA-Kepler mission show that our Solar System is not a model for other The of the star orbiting the barycenter of the planet - star system changes as a Since 2012, after the installation of the high resolution echelle spectrograph HARPS-N [ being the planetary mass (since the real mass depends on the unknown inclination, ], [ p 5 M orbit, the RV technique only provides a value for the minimum mass), orbital eccentricity of the planet.orbital period: This a method Jupiter-like is planet orbiting more atof sensitive 1 about to AU 30 from high m its s host planetary star mass produces9 and a RV cm short semiamplitude s observational effort ( modulation due to thecompanion, contribution hampering of the the interpretation of stellar the activity time series. can mimic the presence of a planetary appear to be ubiquitous andcentral are star generally [ found in multiple systems, tightly packed close to their ties of planetary systems throughplanetary the parameters and radial their velocity correlations technique,our with by knowledge those analyzing of of the the the distributions host planetaryexoplanet of star. research, systems such will The as opportunity help their to formation to and extend understand evolution. the most debated1.1 aspects of Scientific scenario the exoplanetary systems, but a large variety of planetary([ sizes and systems architectures actually exists function of time with a period equal to the orbital period of the planet, the Italian telescope TNG (La Palma, Canaryof Islands) the became extrasolar planets. one of The the opportunity key toaged facilities exploit a for the the large great study capabilities fraction of of thisand instrument Italian to encour- scientists propose working a in long-term theArchitecture observing of program field Planetary with to Systems" specific set-up (GAPS)more themes a Project than and collaboration 60 is objectives. astronomers the The from result "Global (INAF) several of and institutes Italian of this Universities the collaboration. (Padova, Italian Torino National andalso It Milano). Institute provided gathers by for A a Astrophysics technical few and collaborators scientific from support European is and American Institutions. tarity of the techniques, played athe crucial detection role limits in toward the planets discoverydial with of velocity lower such (RV) masses technique, a which and diversity, allowing measures wider to theprovided orbits. push reflex a motion large In of number this the of framework star discoveries thecandidates. induced and ra- by represents a an planet, essential has tool for the follow-up of transit The GAPS Project 1. Introduction defined as follows: PoS(FRAPWS2016)069 S. Benatti 2500 observing ∼ , metal poor stars and 2 2 . In the framework of the GAPS project, HARPS-N spectra 1 − (Serra la Nave Observatory) surveys, from the INAF–Astrophysical 1 ]. 12 ]) and in the collaboration with the HARPS-N GTO program, allowing a preliminary http://chiantitopics.it/wp-content/uploads/2016/05/Leto.pdf determination of the frequencystars of in exoplanets open clusters; around M stars search for additional low mass companions in systems that already host giant planets. Rossiter-McLaughlin effect; 11 , ]) and EXORAP ] for a description of the M dwarf sub-program. – – – 13 10 e.g. Planet detection: System characterization: See See [ The scientific objectives of GAPS, which are pursued by six sub-programs focused on different Thanks to the wide expertise of the GAPS members (high-resolution spectroscopy, stellar An accurate observing strategy, focused on an intensive monitoring, the adoption of new so- The GAPS observing programme started in September 2012. Since then 1 2 • • 300 stars). For 16 interesting objects we have obtained 90 or more RV data points. The GAPS ] and the extreme instrumental stability, ensured by a series of control systems, they can reach ∼ 9 mass estimate for the first transitingM0 dwarf habitable-zone K2-3 Super-Earth [ (in a multiple system) around the type of stars, can be separated into two main aspects: hours were allocated and( about 7000 spectra haveobservations been are collected performed for with theHARPS HARPS-N, at targets the the 3.6m of twin ESO-La our Silla instrument telescope.the sample in visible These range two the spectrographs (400-600 are northern nm) fiber-fed with hemispherethe and a work measure of resolution in of of the 114,000. high They precision[ represent radial the state velocities: of thanks the art toa for the RV accuracy simultaneous calibration better technique thanare also 1 supported m by s aformed coordinated through photometric the monitoring, APACHE (Astronomical in Observatory particular ofValley, [ for the Autonomous M Region dwarf of stars, the per- Aosta activity and pulsations, crowded stellarnamics, environments, data planetary handling) systems our data formation, are planetary carefullyto dy- analyzed produce and scientific discussed within results the with community, aanalysis aiming quality tools as (DE-MCMC, high Gaussian as processes) possible.astrophysical which noise We are have and in developed to robust use RV enable totools data the analyze showed detection their RV data effectiveness of also affected very in by ment small the (see amplitude international [ planetary context, as signals. in These the "RV challenge" experi- Observatory of Asiago and by a number of amateur astronomers. phisticated techniques for proper treatment andof high mitigation resolution of spectrographs activity-induced are signals, the andof key the low points mass use to planetary successfully companions detect in and a confirm multi-planet the system. presence 2. The contribution of GAPS The GAPS Project PoS(FRAPWS2016)069 ± 04 . 0 , left 2 ∼ (RML) 3 R S. Benatti ∆ ] has shown a (right panel). In 16 2 ], as an additional 17 ]), see Figure 03 days and a Jupiter-like planet . 19 ) with an orbital period of 1276 0 11 degrees. ± Jup ± 16 36 ]. This is the first confirmed case of a bi- . 7 M 1 . − ], around the F star Kelt-6 (see Figure 3 > 3500 days) around the target Pr 0211 in the 18 = , of i λ 3 orb ). In order to investigate and explain such a config- P 1 ]), including the analysis of the Rossiter-McLaughlin ] report the RV monitoring with HARPS-N in addition to TRES 15 2 34 days, as presented by [ . 0 ± 80 . > 0.60) and long period ( ], besides the refinement of the orbital solution, the analysis of the RML effect e 120 ] claimed the presence of a transiting Hot Jupiter around the northern component 17 . = 14 3.2 orb Asteroseismology; star-planet interaction; orbital refinement of already known planetary systems. P – – – 74 days has been detected with GAPS observations, as reported by [ M44 open cluster, already known to host a Hot Jupiter ([ uration, a dedicated study ([ significant difference of the chemical abundancethe between condensation the temperature. stars A probably further correlated analysis with of this systemKelt-6 is c ongoing. A moderately eccentric giant planet (Msin panel). In [ data available in literature, whicheccentricity allowed ( to detect a massive planet characterized by high this case a deep analysis of the stellar activity has been performed through a dedicated code for the inner transiting planetthe is orbit, also with presented, a projected Kelt-6 spin-orbit b, angle, showing a slight misalignment of Pr 0211 c The search for planetary companions aroundtive stars of in the crowded GAPS environment project. is [ another objec- of the XO-2 binary system, composed bymag, two K0 both stars with super-metal-rich similar in characteristics ( composition).southern component We performed with an HARPS-N intensive andby monitoring found a of evidence Saturn-mass the of planet a withwith planetary orbital system period composed of 18 nary system in which both theis components present host in planets. the Moreover, RV acompanion residuals linear in long-term of wide trend orbit. XO-2 S, Thisevolution, revealing system since the is the possible an two interesting presence stellartwo laboratory of companions different planetary for an show systems planet very (see additional formation Fig. similar and characteristics but they host effect of XO-2 N b,to showed the that companion, XO-2 perhaps N due has to a the larger presence level of of the stellar Hot activity Jupiter, with while respect [ companion to the Hot Jupiter, discovered by [ XO-2 S b and c In 2007 [ see Section 3 • • • The GAPS Project In the following Sections we summarize the first results of the GAPS3. survey. GAPS Results 3.1 Planet detections PoS(FRAPWS2016)069 S. Benatti , while the outer shows a . ⊕ ⊕ 27 M 77 M . . 0 0 ± ± 47 26 . . ). The inner planet shows an orbital period ] 3 01) has been determined for the inner planet. 15 . 0 4 ± 02 . 0 = e ] presented the detection of a planetary system composed by two 3 0008 days and a minimum mass of 2 . 0 02 days period and a minimum mass of 6 ± . 0 ± 6498 . 74 . Super-Earths around the early M dwarf starcan GJ be 3998. confused As with for the Pr RV 0211 modulation theanalysis induced stellar was by activity carried the signal on presence in of low-mass order planets,both to so the properly the treat stellar this and phenomenon. the As differentialaddition a rotation to result, were the signatures identified ones of in of the the periodogram two of planets the (Figure RV, in of 2 aiming to exclude a stellarsystem cause discovered for around the an additional open RVvalue cluster signal. of star. the This orbital Moreover, is a eccentricity the ( significant first improvement multi-planet of the 13 GJ 3998 b and c Within GAPS a parallelprogram and and fruitful some scientists collaboration of has theIAC started ICE (Instituto (Institut between de de the Ciències Astrofísica de M de l’Espai/CSIC-IEEC)Survey), dwarfs and since Canarias), they the sub- called have similar HADES objectives in (HArps-nof the red study this of Dwarf this collaboration type of [ stars. In the framework Rossiter-McLaughlin effect The Rossiter-McLaughlin (RML) effect occurs whenits a host planet star, transits producing in an frontof anomaly of a in the fraction disk the of of radial the velocities. blue-shifted region Due or to a the fraction temporary of blocking the red-shifted region of the star, the • • Figure 1: Comparison betweenchitecture the of planetary the systems orbiting innerrepresented the Solar in XO-2 System. the binary right stars Left one.of and panel Mercury, The the Venus shows and orbits ar- the the of Earth system the areThe XO-2 indicated of cross with planets symbol XO-2N, black, indicates are blue while the traced and star XO-2S by green location. dotted is red From lines ellipses; [ respectively. the orbits The GAPS Project 3.2 System characterization PoS(FRAPWS2016)069 ] and for S. Benatti the retro- 21 e.g. ] 3 , left panel). The very last result of 4 ]. 23 5 ] (see Figure 22 7200 7200 ] 2 7000 7000 ] and the good degree of alignment for Qatar-1 b [ 20 6800 6800 6600 6600 between the star spin axis and the planet orbital axis. With a dedicated : Radial velocity time series of KELT-6 (obtained from HARPS-N, λ Time [BJD TDB-2,450,000][BJD Time 6400 6400 : Orbital solution and RV residuals for Pr 0211 b (upper panel) & c (lower panel). 6200 6200 TRES HIRES HARPS-N Left panel confidence regions. From [ σ 6000 6000 0 0 75 25 50 50 100 150 100

−25 −75 −50 −50

the RML sub-program reports theplanets orbital around obliquity WASP-43, HAT-P-20 and of Qatar-2 the [ three very massive close-in giant resulting spectrum appears to befect slightly is red-shifted useful and to blue-shifted characterize respectively. theprojected orbit This angle of ef- the planet companion, allowing to measure the sky grade orbit of HAT-P-18 b [ HAT-P-36 and WASP-11/HAT-P-10 [ program of GAPS we observed the RML effect for several systems, showing −100 −150 −200 [m/s] O-C Residuals

Right panel RV [m/s] RV ]. 17 Figure 3: GLS periodograms of theare radial velocities marked of GJ with 3998: a the periodicitiesdifferential blue of rotation (13.74 the (42.5 two days) planets days) and arelines a indicated indicate cyan by 0.1%, dot 1% red and (2.65 and 10% days), magenta level of dots, the false respectively. stellar alarm probability. (30.7 The From dashed days) [ and the Figure 2: [email protected] telescope and HIRES@Keck), over-plotted tomodel the (orange best line), two-planet are Keplerian shown in[ the upper panel, whileRed the and residuals blue are dots in represent the HARPS-Nsent lower and the one. TRES 3 data, From respectively. The gray shaded areas repre- The GAPS Project PoS(FRAPWS2016)069 ], 27 ] the fre- S. Benatti 24 ] determined a 28 for a review), are Boo. In [ τ , two quantities which are ν ∆ Di Mauro : Phase-folded RV measurements of TrES-4 , right panel). This result opens several questions 6 4 ), making TrES-4 b the transiting Hot Jupiter with the ] and the large separation Boo. 28 Jup 0.04 Right panel τ max ν ]. ç ç ç ç ç ç 04 M 22 . ç ç ç ç 0 ç ç 0.02 ç ç ]), with a further support of photometric data. [ ç ç ± ç ç ç ç ç ç 27 ç ç 49 ç ç . ç ç ç ç ç ç ç ç 0.00 ç ç ç ç ], red squares). The lower panel shows the residuals from the best-fit model ç ç Orbital phase ç ç ç ç : Phase-folded RV data of the Rossiter-McLaughlin effect of WASP-11 b 29 ç ç ç ç ç ç ç ç 0.02 ç ç - ç ç ç ç ç ç ç ç ç ç ] a clear indication of star-planet interaction between the G-star HD 17156 and the Left panel 26 0.04 5 0 0 5

10 15 30 20 10 10 20 30 10 - -

- - - - -

s m RV s m C O Γ - - L  H L  H directly connected with the mean properties of the star (see about the formation of such highly inflated bodies. In [ quency of the maximum power measured. This result encourages the applicationing of the exoplanets, asteroseismic in approach to order starsactivity to host- indicators constrain have been their performed ages in orderwhich and to still masses. detect remain the ambiguous possible Finally, for star-planet a interaction, full analysis of the value of the RV semiamplitudepreviously compatible reported (0 with a planetarysecond-lowest density mass known significantly (see lower Figure than hosted Hot Jupiter has beentions. found, A thanks significant X-ray to detection a andindex coordinated a occurred strong HARPS-N near increasing and of the XMM the periastron Ca visit observa- II of H&K this chromospheric planet, characterized byThe a curious high case eccentricity. of TrES-4 b Within GAPS we performed aHot RV monitoring Jupiter to TrES-4 refine b the ([ orbital solution of the transiting Asteroseismology and star-planet interaction The synergy between Asteroseismology and the exoplanets searcherful, is since acknowledged the and pow- planet parameters arewith strictly higher correlated accuracy with thanks the to stellar theperformed ones, seismic available within analysis today GAPS, of aiming stellar to oscillations. search A for pilot stellar study was oscillations in • • green diamonds and [ observed with HARPS-N over-plotted toplotted the in best-fitting the model. lower The panel.obtained corresponding with residuals From HARPS-N are [ (blueThe circles) comparison and with the previous studies best-fit clearly Keplerian shows a orbit discrepancy model of the (black RVto solid semiamplitude the ([ line). HARPS-N radial velocities. From [ Figure 4: The GAPS Project PoS(FRAPWS2016)069 S. Benatti ], whose data were ]. New planet detec- 31 ] presented a study on 36 , the Bayesian homoge- 33 e.g. ] investigated the chromospheric emission of ] we show that our radial velocities scatter is (this proceeding) for details. The extension of ]), providing simultaneous observations in the 34 30 37 7 Claudi ] to obtain temperature-sensitive ratios of spectral features from a 32 for low-activity early-M dwarfs, with the contribution of the HADES The GAPS programme with HARPS-N at TNG. IV. A planetary system around α , A&A, 567, L6. incompatible with the presence ofaffected by the the two lower giant sensibility of planets thea claimed instrumentation. very by metal This poor [ result star, dismissed generally planets excluded around by theStellar planet parameters formation and theory. activity for MThe stars HARPS-N spectra usedin to a obtain parallel high study precision by radial [ velocities were also exploited the relationship between activity-rotation andship of stellar different parameters chromospheric lines, and while theCa [ flux-flux II relation- H&K and H collaborators. large sample of M0-M4.5 dwarf stars.and They gravities provide empirical as calibrations a for function masses,also radii, paid of on effective the temperature characteristics and of the metallicity. stellar activity Particular of attention M is dwarfs: [ HARPS-N spectra also allowed tocase confirm of or the rule-out metal previous poor planet star detections, HIP 11952. as in In the [ XO-2S GAPS has coagulated a large number of Italian scientists involved in the exoplanets field, Other studies involved in particular the system characterization, ]), and the full analysis of the HD 108874 planetary system, reported in [ • 35 [1] S. Desidera et al. 2014 resulting in a strong andto coordinated now collaboration. and Several even interesting morecandidates results papers were has are published been in up preparation identifiedwe or but plan close in further to some the observations. cases submission.developed After an we A four optimized need number observing more of strategy ofwhich planet and data HARPS-N require new for observations many analysis data their and tools, and analysis confirmation, inare specific we particular foreseen so treatment for have for of GAPS, those the since objects RV GIARPSexoplanetary time is research. series. expected to In Anyway, new be fact perspectives available GIARPSspectrograph at will TNG of combine with TNG HARPS-N high and in impact GIANO, on the the the near high infrared resolution (see [ tions will be soon presented indata dedicated for papers, a while robust the confirmation. identified planet candidates still require 4. Conclusions and future perspectives the wavelength range will open toof the the GAPS extrasolar community planets. new scenarios and objectives in the study References 3.3 Further works neous determination of orbital and physical parameters([ for a large sample of giant transiting planets visible and in the near infrared bands, see The GAPS Project PoS(FRAPWS2016)069 , , ApJ, S. Benatti , ApJS, 201, , A&A, 554, A28. ˘ A¸S53,Ed. Seager, S. , PNAS, Vol. 111, Nr. pp. 27â , SPIE Conf. Ser., Vol. 8446, 1. , Sci, 340, 572. 8 , Hot Planets and Cool Stars, ed. R. Saglia, EPJ Web of A&A, 575, A111. , A&A, 588, A118. , A&A, 593A, 117. , A&A, 598, 133. Radial Velocity Techniques for Exoplanets , A&A, 583, A135. , ApJ, 790, 146. The GAPS programme with HARPS-N at TNG. IX. The multi-planet system The GAPS programme with HARPS-N at TNG. V. A comprehensive analysis Harps-N: the new planet hunter at TNG , AJ, 147, 39. The GAPS programme with HARPS-N at TNG. XI. Pr 0211 in M 44: the first Architecture of Kepler’s Multi-transiting Systems. II. New Investigations with The APACHE Project A Nearby M Star with Three Transiting Super-Earths Discovered by K2 The GAPS Programme with HARPS-N at TNG. III: The retrograde orbit of Planet Occurrence within 0.25 AU of Solar-type Stars from Kepler KELT-6b: A P 7.9 Day Hot Saturn Transiting a Metal-poor Star with a The GAPS programme with HARPS-N at TNG. I. Observations of the The HADES RV Programme with HARPS-N@TNG. II. Data treatment and The GAPS programme with HARPS-N at TNG. X. Differential abundances in the XO-2b: Transiting Hot Jupiter in a Metal-rich Common Binary Two "b"s in the Beehive: The Discovery of the First Hot Jupiters in an Open Radial Velocity Fitting Challenge. I. Simulating the data set including realistic The HADES RV Programme with HARPS-N@TNG - GJ 3998: An early M-dwarf Observed Properties of Extrasolar Planets Exploring exoplanet populations with NASA’s Kepler Mission , A&A, 598A, 26. , A&A, 564, L13. , A&A, 581, L6. , ApJ, 756, L33. simulations 35, 12647. 804, 10. ApJ, 671, 2115. of the XO-2 stellar and planetary systems Long-period Companion University of Arizona Press Tucson, AZ. XO-2 planet-hosting binary KELT-6: Detection of the planet KELT-6KELT-6 c b and measurement of the Rossiter-McLaughlin effect for Cluster HAT-P-18b Rossiter-McLaughlin effect and characterisation of the transiting system Qatar-1 stellar radial-velocity signals Conferences 47, id. 03006. 15. Twice as Many Candidates multi-planet system in an open cluster hosting a system of Super-Earths [8] A. Howard 2013 [9] C. Lovis & D. Fischer 2010 [5] A. Howard et al. 2012 [7] N. Batalha 2014 [6] D. Fabrycky et al. 2014 [2] L. Malavolta et al. 2016 [3] L. Affer et al. 2016 [4] R. Cosentino et al. 2012, [13] M. Perger et al. 2017 [14] C. Burke et al. 2007 [15] M. Damasso et al. 2015a The GAPS Project [10] Sozzetti, A., et al. 2013 [16] K. Biazzo et al. 2015 [18] K. Collins et al. 2014 [19] S. Quinn et al. 2012 [20] M. Esposito et al. 2014 [21] E. Covino et al. 2013 [11] X. Dumusque 2017 [12] I. Crossfield et al. 2015 [17] M. Damasso et al. 2015b PoS(FRAPWS2016)069 , , A&A, S. Benatti , A&A, , this , A&A, 540, , ApJ, 667, L195 , SPIE Conf. Ser., Vol. , A&A, 578, A64. Bootis A τ , ApJ, 785, 126. , this proceeding, [arXiv170307604D]. , A&A, 598A, 27. 9 , A&A, 599A, 90. chromospheric emission of low-activity early-M dwarfs α , A&A, 554, A29. Friends of Hot Jupiters. I. A Radial Velocity Search for Massive, The HADES RV Programme with HARPS-N@TNG. IV. Time resolved TrES-4: A Transiting Hot Jupiter of Very Low Density The GAPS Programme with HARPS-N at TNG. XIV: Investigating giant Stellar parameters of early-M dwarfs from ratios of spectral features at The HArps-n red Dwarf Exoplanet Survey (HADES) III. Flux-flux and The GAPS Programme with HARPS-N at TNG. XX. The orbital obliquity of Planetary companions around the metal-poor star HIP 11952 The GAPS programme with HARPS-N at TNG. VI. The curious case of The GAPS Programme with HARPS-N at TNG. VIII. Observations of the The GAPS programme with HARPS-N at TNG. II. No giant planets around the Coordinated X-Ray and Optical Observations of Star-Planet Interaction in HD Asteroseismology – A Review The GAPS programme with HARPS-N at TNG. XII: Characterization of the High resolution near IR spectroscopy with GIANO-TNG GIARPS: the VIS-NIR high precision radial velocity facility TNG , A&A, 579, A136. The GAPS programme with HARPS-N at TNG. VII. Putting exoplanets in the , A&A, 577, A132. , A&A, 575, L15. , ApJ, 811, L2. A141. optical wavelengths activity-rotation relationships of early-M dwarfs 17156 TrES-4b Long-period Companions to Close-in Gas Giant Planets analysis of the Ca II H&K and H metal-poor star HIP 11952 planetary system around HD 108874 three close-in massive planets hosted by601A, dwarf 53. K-type stars: WASP-43, HAT-P-20 and Qatar-2 stellar context: magnetic activity and asteroseismology of 598A, 28. planet migration history via improved eccentricityA&A, and 602A, mass 107. determination for 231 transiting planets 9147, 91471E. proceeding. Rossiter-McLaughlin effect and characterisation of theWASP-11/HAT-P-10 transiting planetary systems HAT-P-36 and [32] J. Maldonado et al. 2015 [33] J. Maldonado et al. 2017 [26] A. Maggio et al. 2015 [27] G. Mandushev et al. 2007 [28] A. Sozzetti et al. 2015 [29] H. A. Knutson et al. 2014, [34] G. Scandariato et al. 2017 [23] M. Esposito et al. 2017 [30] S. Desidera et al 2013 [31] J. Setiawan et al. 2012 [37] L. Origlia et al. 2014 [24] F. Borsa et al. 2015 [35] A. S. Bonomo et al. 2017 [36] S. Benatti et al. 2017 [38] R. Claudi et al. 2017 The GAPS Project [22] L. Mancini et al. 2015 [25] M. P. Di Mauro 2017