Eight years of accurate photometric follow-up of transiting giant exoplanets
TTwenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold
Eight years of accurate photometric follow-up oftransiting giant exoplanets
L. Mancini , J. Southworth Max Planck Institute for Astronomy, K¨onigstuhl 17, 69117 – Heidelberg, Germany ( [email protected] ) Astrophysics Group, Keele University, Sta ff ordshire, ST5 5BG, UK ( [email protected] ) Abstract
Since 2008 we have run an observational program to accurately measure the characteristics ofknown exoplanet systems hosting close-in transiting giant planets, i.e. hot Jupiters. Our study is basedon high-quality photometric follow-up observations of transit events with an array of medium-classtelescopes, which are located in both the northern and the southern hemispheres. A high photometricprecision is achieved through the telescope-defocussing technique. The data are then reduced andanalysed in a homogeneous way for estimating the orbital and physical parameters of both the planetsand their parent stars. We also make use of multi-band imaging cameras for probing planetary atmo-spheres via the transmission-photometry technique. In some cases we adopt a two-site observationalstrategy for collecting simultaneous light curves of individual transits, which is the only completelyreliable method for truly distinguishing a real astrophysical signal from systematic noise. In thiscontribution we review the main results of our program.
Transiting extrasolar planets (TEPs) are the most important and interesting planets to study. The particular orbitalconfiguration of these planetary systems, with respect to an Earth-based observer, enables measurement of theirmain physical properties, including the planet’s mass, radius, density, surface gravity and temperature, which areof huge importance for finding Earth twins in habitable zones around normal stars. Specific science cases for thiswork include high-precision measurements of the properties of planetary systems, transmission photometry andspectroscopy to study the atmospheres of giant planets, and transit timing work to study the dynamical propertiesof planetary systems.In August 2008, we began a long-term observational program for measuring the physical properties of knowTEP systems via accurate photometric monitoring of transit events. Our project was conceived considering: ( i ) thepoor quality of the photometric data on which many TEP discoveries were based; and ( ii ) the necessity of analysingthe data in a homogeneous way, so that the properties of di ff erent exoplanets can be reasonably comparable in aglobal picture. Establishing such a homogeneous and trustworthy dataset is fundamental for theoretical studies ofhow exoplanets form and evolve.The scope of our project has inexorably grown alongside the discovery rate of suitable planets for analysis. Thetime-critical nature of transit observations naturally encourages a survey-style project whereby large numbers oftransits are scheduled for observation in order to overcome the di ffi culties of scheduling and losses due to weatherand technical issues. Once a su ffi cient number of transits have been observed for a given planet, these can then beused to characterise the planetary system in detail. The need for a large amount of observing time is best met byusing ground-based medium-class telescopes, which are su ffi cient for the project and more readily available thanlarger facilities. These telescopes are best suited to the study of close-in giant planets, usually termed “hot Jupiters”,orbiting bright stars ( V (cid:46)
14 mag). For these TEPs, the transits are deep (typically 1–2%) and frequent, and a highphotometric precision can be obtained using 1–2 m telescopes. a r X i v : . [ a s t r o - ph . E P ] M a y wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold
Hot Jupiters arguably represent the first class of exoplanets found, and 51 Peg b is their prototype. They are giantgas planets with tight ( ∼ . − .
05 au) and short-period ( ∼ −
10 days) orbits around their parent stars. Theyare strongly irradiated by their host stars, resulting in high equilibrium temperatures (e.g. 2750 K for Kepler-13and 2710 K for WASP-33). Although it appears that they are very uncommon with respect to Neptunian and rockyplanets (e.g. Fressin et al. 2013; Petigura et al. 2013), there are many motivations for studying them. Their relativelylarge mass and radius allows measurement of these quantities to much better precision than smaller planets, theirspin-orbit alignment is directly accessible by observing the Rossiter-McLaughlin e ff ect, transmission spectra canbe obtained of the terminator regions of their atmospheres, and their day-side thermal emission and reflected lightare measurable. It is therefore possible to investigate the properties of their atmospheres and the abundances ofelements and molecules. However, after four lustra from their discovery (Mayor & Queloz 1995), their formationand evolution mechanisms are still unclear and under intriguing investigation and debate. In particular, it is not clearwhat are the physical mechanisms responsible of their migration from the snow line ( ∼ − au from their parent stars. The medium-class telescopes, which we utilise in our program, summarised in Table 1, are equipped with CCDcameras that have fields-of-view (FOVs) of up to several tens of arcmin, allowing the possibility to include inthe scientific images a good number ( ∼ −
10) of reference stars, which are vital for achieving high-qualitydi ff erential photometry. We perform photometric observations of planetary transits through broad-band filters, Table 1: List of the telescopes used in our programTelescope Observatory Aperture Instrument Multi-band ability Transits
Southern hemisphere
MPG 2.2 m La Silla 2.2 m GROND 4 bands 49Danish La Silla 1.54 m DFOSC No 148
Northern hemisphere
INT La Palma 2.5 m WFC No 32CAHA 2.2 m Calar Alto 2.2 m BUSCA 4 bands 33Cassini Loiano 1.52 m BFOSC No 72Zeiss Calar Alto 1.23 m DLR-MKIII No 151 generally Cousins / Bessell R and I or Sloan / Gunn r and i (according to the magnitude and colour of the parentstars). This choice is dictated by several considerations: ( i ) we generally observe cool dwarf stars, which emit moreradiation between 6000 and 8000 Å; ( ii ) limb darkening (LD) is weaker than at bluer wavelengths so the transitlight curves are more box-shaped and thus the transit depth and timings of the four contact points are easier tomeasure; ( iii ) at these wavelengths, the photometry is less a ff ected by extinction from Earth’s atmosphere and fromspot activity on the surfaces of the parent stars. If the target is not too close to nearby stars, the observations are performed using the telescope-defocusing technique(Alonso et al. 2008; Southworth et al. 2009a), which allows us to get light curves with a higher precision than usingtelescopes operated in focus (see Fig. 1). This observational method consists of defocussing the telescope so that According to the definition given by Hatzes & Rauer (2015), giant planets cover the mass range 0 . − M Jup . It is a fairly common strategy to make observations with the telescope in focus and then bin the data points. While this methodcan yield light curves with quite high photometric precision, it is much more strongly a ff ected by red noise from e ff ects such asflat-fielding imperfections. wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold - - - ������� ����� � � � � � �� � � � � � �� Copernico 1.82 m ( focussed ) T exp = rms scatter = - - - ������� ����� Copernico 1.82 m binned ( focussed ) T exp = rms scatter ( after binning ) = - - - ������� ����� Zeiss 1.23 m ( defocussed ) T exp =
120 sec rms scatter = Figure 1: Example light curves of Qatar-1 from Covino et al. (2013).
Left : follow-up light curve froma 1.82 m telescope operated in focus with an exposure time of 7 sec.
Centre : the same light curve afterbinning.
Right : follow-up light curve from a defocussed 1.23 m telescope with an exposure time of120 sec. we can use long exposure times (with a maximum of ∼
120 sec to ensure we get a good sampling of the transitevent) and collect more photons in each point spread function (PSF), which can now cover thousands of pixels. Theimmediate result is that the light from the target and the stars in the FOV show up on the CCD in the particularshape of annuli of di ff erent sizes. Collecting more photons during longer exposures greatly lowers the Poisson andscintillation noise, and systematic noise coming from flat-fielding and focus or seeing variations. We stress thatthere is not a general setting for the exposure time and the amount of defocussing, but they must be chosen caseby case, by considering the brightness of the target and reference stars, the aperture of the telescope and the filterused. Special attention is placed in tuning the defocussing in order to avoid to work in the non-linear regime ofthe CCDs (we usually try to get a maximum counts per pixel around 25000–35000 ADU for 16-bit CCD systems).Once the set-up is established, a changing of the exposure time during the monitoring of planetary-transit events(they generally last several hours) is possible if we need to compensate for variation in seeing, airmass and skytransparency, which a ff ect the count rate of the observations during the sequence.More rarely, the defocus can also be adjusted under particular circumstances. At several observatories, onecould see the telescope going slowly from defocussed to in-focus after tracking past the meridian. This is generallycaused by a gradual shifting of the primary mirror under the changing influence of gravity. This causes the observerto greatly decrease the exposure time, thus losing the benefits of the defocussing technique, and also results in PSFsof very di ff erent sizes between the first and the second part of the observations. One way to solve the problem isto take a note of the number of pixels inside the annulus of the target star at the beginning of the observations, andperiodically check that this number remains constant during the sequence. If it changes (i.e. the size of the annulusbecame smaller), we increase the defocus to have again the same number of pixels. Indeed, what it is importantis to keep the same amount of defocus, i.e. the width of the PSF for each star in the FOV should cover the samenumber of pixels through the full observing sequence. Time series photometry of transit events can be a ff ected by many sources of systematics, which are not always easilyfound and corrected, but also by astrophysical phenomena such as gravity darkening, the presence of exomoonsor Trojan bodies, and the planet crossing irregularities on the stellar photosphere such a starspot or a star-spotcomplex. The question is how we can be completely sure that we have identified all the systematics in our dataand distinguish real astrophysical signals from them? The only way to be completely sure is to observe the sametransit event with two di ff erent telescopes through similar filters, preferably at di ff erent observatories. If we see thesame anomaly / feature occurring at the same time on both light curves, than we can unambiguously claim that it is wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold of astrophysical origin. We adopted this observational strategy in only a few cases (see an example in Fig. 2), astelescope scheduling, technical problems and weather conditions can all frustrate simultaneous observations. ○○○○ ○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○○ ��� ( ��� )- ������� � � � � � �� � � � � � �� ○ Sloan r Bessell R Figure 2: Simultaneous observations of a transit of WASP-103 b taken with the MPG 2.2 m and theDanish 1.54 m telescopes (Southworth et al. 2015a). The same features (probably a starspot bell orgranulation) are very well recorded by the two telescopes during the scanning of the stellar photospherethrough the planetary transit.
The radius of an exoplanet, which we measure from a transit event, can vary as a function of wavelength. Variationsof its atmospheric opacity can cause the absorption of light rays coming from the parent star at specific wavelengths,allowing detection of the presence of atomic (e.g. Na and K) and molecular (e.g. H O and CO) species. Thismeans that by photometrically observing a transit through di ff erent passbands, we can reconstruct the transmissionspectra of TEPs and probe their atmospheres. This technique, also known as transmission photometry , is similarto transmission spectroscopy, with the clear disadvantage of a lower spectral resolution. On the other hand, thereare many benefits to prefer photometry to spectroscopy, mainly the possibility to use ground-based telescopes withsmaller apertures, the possibility to investigate TEPs orbiting faint stars, more relaxed constraints on comparisonstars, and the established fact that photometry is much less a ff ected by telluric absorption and changing airmass andsky conditions. Indeed, the most robust results of planetary-atmosphere investigation come from space observationswith the HST (e.g. Sing et al. 2015; Nikolov et al. 2015). However these studies are limited by the orbital period( ∼
90 min) of the spacecraft around Earth, causing a target star to be unobservable for half of each orbit. Thisimplies that, in order to have data covering a complete transit and part of the out-of-transit light curve, observationswith the HST have to be performed over multiple transits, which are generally spread over many days, duringwhich the telescope su ff ers continual changes in temperature and focus. Moreover, since occulted and un-occultedstarspots can cause a wavelength-dependent variations of the transit depth (Sing et al. 2011), it is also always betterto obtain the observations of complete transits at multiple wavelengths simultaneously. The use of multi-imagingcameras are thus mandatory for performing transmission photometry.We use two instruments that are able to perform simultaneous multi-band photometric observations (see exam-ples in Fig. 3): ( i ) the Gamma-Ray Burst Optical and Near-Infrared Detector (GROND) instrument, mounted onthe MPG 2.2 m telescope, capable of simultaneous observations in four broad optical (similar to Sloan g , r , i , z ) andthree NIR ( J , H , K ) passbands (Greiner et al. 2008); ( ii ) the Bonn University Simultaneous CAmera (BUSCA),mounted on the 2.2 m telescope at Calar Alto, able to simultaneously make photometry in four wavelength bands(from UV to visual IR), with the possibility to use di ff erent sets of filters, both broad and narrow (Reif et al. 1999).Neither instrument was designed for exoplanet work, and they therefore have operational limitations which lowerthe quality of the data obtainable. These limitations include needing to use the same exposure times and focus wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold settings in all passbands, resulting in low count rates in the bluer passbands where the stars are fainter, a small fieldof view which limits the number of comparison stars available, and non-standard passbands which are broad orhave low throughput. - - ������� ����� � � � � � �� � � � � � �� MPG 2.2m / GROND
Sloan g Sloan r Sloan i Sloan z - - - ������� ����� � � � � � �� � � � � � �� CAHA 2.2m / BUSCA
Gunn u Gunn g Gunn r Gunn z Figure 3: Examples of typical light curves obtained with multi-band imagers.
Left-hand panel : lightcurves of a transit of WASP-80 b observed with GROND (Mancini et al. 2014a).
Right-hand panel :light curves of a transit of HAT-P-8 b observed with BUSCA (Mancini et al. 2013a).
Once we have collected photometric observations of planetary transits, they are analysed in three steps followingthe
Homogeneous Studies approach (Southworth 2012, and references therein).( i ) We reduce the photometric data of the observed transits using defot , an idl -based data reduction pipelinedesigned specifically for time-series photometry of defocussed images. After having calibrated the scientificimages, we choose an optimal ensemble of comparison stars and perform standard aperture photometry toextract the light curves. We then remove instrumental and astrophysical trends from our light curves byfitting a straight line or a polynomial to the out-of-transit data.( ii ) We use jktebop (Southworth 2012) for modelling the transit light curves. This code is able to fit the orbitalinclination, i , the transit midpoint, T , the orbital period, P orb , the limb-darkening coe ffi cients, and the sumand ratio of the fractional radii of the star and planet, r (cid:63) + r p and k = r p / r (cid:63) . Here the fractional radii aredefined as r (cid:63) = R (cid:63) / a and r p = R p / a , where a is the orbital semi-major axis, and R (cid:63) and R p are the absoluteradii of the star and the planet, respectively. The uncertainties in the parameters are robustly determined byMonte Carlo simulations, bootstrapping simulations, and / or a residual-permutation algorithm.If anomalies, which are generally caused by starspots occulted by the planet during the transit event, arepresent in the light curves, then we model these with the prism + gemc codes (Tregloan-Reed et al. 2013a, idl is a trademark of the ITT Visual Information Solutions. The source code of jktebop is available at http: // / jkt / codes / jktebop.html wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold jktebop but with additional parameters todescribe the starspots. Each spot is specified using the longitude and colatitude of its centre, its angularradius and its contrast, i.e. the ratio of the surface brightness of the star-spot to that of the surroundingphotosphere.( iii ) The full physical properties of a transiting planetary system are not directly accessible from observationsalone, so the measured parameters from the light curves and spectroscopic observations must be combinedwith an additional constraint. For this we use the jktabsdim code (see Southworth 2009), which can useeither theoretical predictions of the properties of low-mass stars or an empirical calibration from eclipsingbinary stars (see Southworth 2010) as this additional constraint. Five di ff erent sets of theoretical models areimplemented, allowing some idea of the systematic di ff erences between the models to be obtained. jktabsdim takes as input r (cid:63) , r p , i and P orb from the light curve analysis, and the orbital eccentricity, velocity amplitude,e ff ective temperature and metallicity from spectroscopic analysis of the host star. It returns the best-fittingproperties of the star and planet, and the age of the system. We have obtained high-quality light curves for more than 50 known TEPs and, so far, have refined the main physicalparameters of 38 of them, which are summarised in Table 2. In most of the cases and for most of the parameterswe obtained better estimations. In particular, for several TEPs, we found that their measured characteristics aresignificantly di ff erent to previous works based on less data. Some of these cases are highlighted in Fig.4, whichshows large shifts in the measured properties for some planets. The largest changes were seen for WASP-7 andWASP-16, where the measured planetary densities decreased by a factor of two or more.Thanks to the multi-band observations performed with GROND and BUSCA, we have probed the atmosphere,at the terminator region, of 14 TEPs; they are: HAT-P-5 b, HAT-P-8 b, HAT-P-23 b, Qatar-2 b, WASP-19 b, WASP-36 b, WASP-44 b, WASP-45 b, WASP-46 b, WASP-48 b, WASP-57 b, WASP-67 b, WASP-80 b, WASP-103 b. Inseveral cases we have founded larger planet radius at bluer optical wavelengths. In particular, for the hot JupitersWASP-36 b (Mancini et al. 2016) and WASP-103 b (Southworth et al. 2015a) we have determined a large variationbetween blue ( g -band) and red ( z -band) optical wavelengths of roughly 10 atmospheric pressure scaleheight to aconfidence level of more than 5 and 7 σ . In both the cases, this variation is too large to be attributable to Rayleighscattering in the planetary atmosphere, and should be caused by the presence of strong absorber species at bluerwavelengths.The accurate determination of the physical properties of TEPs systems via ground-based photometric follow-up observations will continue until the Transiting Exoplanet Survey Satellite (TESS) will start its operations in late2017. Indeed, this part of our project will superseded by the higher photometric precision of the TESS telescope.However, in the next future, there will be no space missions completely dedicated to the study of planet atmospheres.This means that for still many years, ground-based multi-band photometric observations can play an important rolefor investigating the properties and chemical composition of the TEPs’ atmospheres, especially for those orbitingaround faint stars, strongly cooperating with ground-based spectrometers and observations performed by the HST,the Spitzer and, soon, the JWST spacecrafts. It is then important, as suggested by Southworth et al. (2015b), to havea new multi-band camera, specifically designed for transit observations. This should have a su ffi cient number ofpassbands for covering the entire optical transmission spectrum of a exoplanet and the possibility to set a di ff erentexposure time for each filter, for guaranteeing enough S / N in each band. wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold ●●● ● ●● ●● ●● ●● ●● ● ●● ● ● ●● ●●● ● ●●●● ●●●● ●● ●● ●●● ● ●●● ●● ● ●●● ●● ●●● ● ●●● ●●●● ●● ●●● ● ●●● ●● ●●●● ●●● ● ●●● ●● ●● ●● ●● ●● ● ● ●● ●● ● ●● ● ●● ● ●● ●● ● ● ● ●●● ●● ●●●● ●● ●● ● ●● ●● ● ●● ●● ● ●● ●● ● ●● ●●● ● ● ●● ●●● ● ●● ● ●●● ●● ●● ● ●●●● ●● ●●● ● ●●● ●●● ● ● ●● ●● ● ●● ●● ●● ●●● ●● ● ● ●● ●● ●● ●● ●● ●● ●●●● ●●● ● ●● ●●●● ●●
Planet mass ( M Jup ) P l ane t r ad i u s ( R J up ) ρ jup ρ jup ρ jup ρ jup ρ jup / jkt / tepcat / ; Southworth 2011) and their errorbars havebeen suppressed for clarity. Dotted lines show where density is 2.5, 1.0, 0.5, 0.25 and 0.1 ρ Jup .7 wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold T a b l e : R e v i s e dp a r a m e t e r s o f t h e TE P s y s t e m s t h a t w e h a v e s t ud i e d TE P s y s t e m R e f e r e n ce s M (cid:63) ( M (cid:12) ) R (cid:63) ( R (cid:12) ) l og g (cid:63) ( c g s ) ρ (cid:63) ( ρ (cid:12) ) M p ( M J up ) R p ( R J up ) g p ( m / s ) ρ p ( ρ J up ) a ( a u ) P ( d a y s )) HA T - P - S ou t h w o r t h e t a l . ( ) B a ko s e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) HA T - P - M a n c i n i e t a l . ( a ) L a t h a m e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± .
061 1 . + . − . . ± .
040 1 . + . − . . ± . . ± . . ± . . ± . ± . . ± . . ( ) . ( ) HA T - P - S ou t h w o r t h e t a l . ( a ) B a ko s e t a l . ( ) . ± .
062 1 . + . − . . ± . . ± . . ± . . ± . . ± . ... . ± .
030 0 . + . − . . ± . . ± . . ± . . ± . . ± .
017 0 . + . − . . ± . . + . − . . ( ) . ( ) HA T - P - C i ce r i e t a l . ( ) B u c hh a v ee t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) HA T - P - C i ce r i e t a l . ( a ) B a ko s e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) HA T - P - M a n c i n i e t a l . ( ) B a ko s e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ± . ± . ± . . ± . . ± . . ± . . ( ) . ( ) Q a t a r- M i s li s e t a l . ( ) A l s ub a i e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± .
075 1 . + . − . . ± . . ± . . ± .
70 18 . + . − . . ± .
040 0 . + . − . . ± . . + . − . . ( ) . ( ) Q a t a r- M a n c i n i e t a l . ( c ) B r y a n e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) T r E S - M i s li s e t a l . ( ) M a ndu s h e v e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) T o rr e s e t a l . ( ) . ± .
060 0 . + . − . . ± .
022 0 . + . − . . ± .
018 4 . + . − . . ± .
067 1 . + . − . . ± .
045 0 . + . − . . ± .
033 1 . + . − . . ± .
80 19 . + . − . . ± .
048 0 . + . − . . ± . . + . − . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) W il s on e t a l . ( ) . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( a ) A nd e r s on e t a l . ( ) . ± .
062 0 . + . − . . ± .
041 1 . + . − . . ± .
030 4 . + . − . . ± . ... . ± .
082 1 . + . − . . ± .
057 1 . + . − . . ± . . + . − . . ± .
14 1 . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - T r e g l o a n - R ee d e t a l . ( ) G ill on e t a l . ( ) . ± .
067 0 . + . − . . ± .
025 0 . + . − . . ± . . ± . . ± .
053 1 . + . − . . ± .
027 0 . + . − . . ± .
037 1 . + . − . . ± . . ± . . ± . . ± . . ± . . + . − . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) H e lli e r e t a l . ( a ) . ± .
065 1 . + . − . . ± .
092 1 . + . − . . ± .
047 4 . + . − . . ± . ... . ± .
13 0 . + . − . . ± .
093 0 . + . − . . ± . . + . − . . ± .
10 1 . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - M a n c i n i e t a l . ( ) W e s t e t a l . ( a ) . ± .
040 0 . + . − . . ± .
014 0 . + . − . . ± . . ± . . ± . ... . ± . . ± . . ± .
023 0 . + . − . . ± .
50 14 . + . − . . ± .
026 0 . + . − . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) W e s t e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) L i s t e r e t a l . ( ) . ± .
054 1 . + . − . . ± .
042 0 . + . − . . ± .
022 4 . + . − . . ± .
056 1 . + . − . . ± .
038 0 . + . − . . ± .
040 1 . + . − . . ± .
71 19 . + . − . . ± .
033 0 . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - S ou t h w o r t h e t a l . ( c ) A nd e r s on e t a l . ( ) . ± . . ± . . ± .
041 1 . + . − . . ± . . ± . . ± .
012 0 . + . − . . ± .
033 0 . + . − . . ± .
053 1 . + . − . . ± .
20 3 . + . − . . ± . . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - S ou t h w o r t h e t a l . ( c ) H e lli e r e t a l . ( ) . ± . . ± . . ± .
047 1 . + . − . . ± .
026 4 . + . − . . ± .
062 0 . + . − . . ± . . ± . . ± .
057 1 . + . − . ±
17 194 + − . ± .
90 7 . + . − . . ± . . ± . . ( ) . ( ) W A SP - M a n c i n i e t a l . ( c ) H e bb e t a l . ( ) . ± .
041 0 . + . − . . ± .
015 0 . + . − . . ± . . + . − . . ± . . + . − . . ± .
036 1 . + . − . . ± .
021 1 . + . − . . ± .
18 15 . + . − . . ± . . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - C i ce r i e t a l . ( ) B ou c hy s e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± . . ± . . ± . . + . − . . ( ) . ( + )( − ) W A SP - S ou t h w o r t h e t a l . ( ) M a x t e d e t a l . ( ) . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . + . − . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) S t r ee t e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± .
054 1 . + . − . . ± .
047 1 . + . − . . ± .
99 14 . + . − . . ± .
043 0 . + . − . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) E no c h e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± .
032 1 . + . − . . ± . . ± . . ± .
028 0 . + . − . . ± . . ± . . ( ) . ( ) C o n t i nu e d o nn e x t p ag e wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold T a b l e c o n t i nu e d f r o m p re v i o u s p ag e TE P s y s t e m R e f e r e n ce s M (cid:63) ( M (cid:12) ) R (cid:63) ( R (cid:12) ) l og g (cid:63) ( c g s ) ρ (cid:63) ( ρ (cid:12) ) M p ( M J up ) R p ( R J up ) g p ( m / s ) ρ p ( ρ J up ) a ( a u ) P ( d a y s )) W A SP - S ou t h w o r t h e t a l . ( ) S m a ll e y e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - M a n c i n i e t a l . ( ) S m it h e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) M a x t e d e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) L e nd l e t a l . ( ) . ± .
037 0 . + . − . . ± .
021 0 . + . − . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . ... . ± .
029 0 . + . − . . ± . . ± . . ( ) . ( ) W A SP - M a n c i n i e t a l . ( ) A nd e r s on e t a l . ( ) . ± . . ± . . ± .
030 0 . + . − . . ± .
020 4 . + . − . . ± .
058 1 . + . − . . ± . . ± . . ± . . ± . . ± . . + . − . . ± .
074 0 . + . − . . ± . . ± . . ( ) . ( ) W A SP - C i ce r i e t a l . ( ) A nd e r s on e t a l . ( ) . ± . . ± . . ± .
024 0 . + . − . . ± .
014 4 . + . − . . ± .
047 1 . + . − . . ± . . ± . . ± .
038 1 . + . − . . ± . . + . − . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - C i ce r i e t a l . ( ) A nd e r s on e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . + . − . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - C i ce r i e t a l . ( a ) E no c h e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - T r e g l o a n - R ee d e t a l . ( ) G ill on e t a l . ( ) . ± .
057 0 . + . − . . ± . . ± . . ± . . ± . . ± .
032 1 . + . − . . ± .
068 1 . + . − . . ± . . ± . . ± . . ± . . ± .
033 0 . + . . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) H e lli e r e t a l . ( ) . + . − . . ± . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . + . − . . ± . . + . − . . + . − . . + . − . . ± . . + . − . . + . − . . ± . . ± . . ( ) . ( ) W A SP - S ou t h w o r t h e t a l . ( ) F ae d i e t a l . ( ) . ± . . ± . . ± .
033 0 . + . − . . ± .
025 4 . + . − . . ± .
085 1 . + . − . . ± .
062 0 . + . − . . ± .
053 0 . + . − . . ± . . + . − . . ± .
072 0 . + . − . . ± . . ± . . ( ) . ( ) W A SP - M a n c i n i e t a l . ( ) F ae d i e t a l . ( ) . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± . . ± .
046 1 . + . − . . ± .
83 5 . + . − . . ± . . ± . . ± . . ± . . ( ) . ( ) W A SP - M a n c i n i e t a l . ( a ) T r i a ud e t a l . ( ) . ± .
035 0 . + . − . . ± .
012 0 . + . − . . ± . . + . − . . ± .
050 3 . + . − . . ± .
027 0 . + . − . . ± .
022 0 . + . − . . ± .
46 15 . + . − . . ± .
023 0 . + . − . . ± . . + . − . . ( ) . ( + )( − ) W A SP - S ou t h w o r t h e t a l . ( a ) G ill on e t a l . ( ) . ± .
091 1 . + . − . . ± .
040 1 . + . − . . ± .
014 4 . + . − . . ± .
013 0 . + . − . . ± . . ± . . ± .
045 1 . + . − . . ± . . ± . . ± .
027 0 . + . − . . ± . . ± . . ( ) . ( ) wenty years of giant exoplanets - Proceedings of the Haute Provence Observatory Colloquium, 5-9 October 2015Edited by I. Boisse, O. Demangeon, F. Bouchy & L. Arnold
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