{'fraction_non_alphanumeric': 0.04706308263191239, 'fraction_numerical': 0.04000362023712553, 'mean_word_length': 4.01588742623695, 'pattern_counts': {'":': 0, '<': 3, '<?xml version=': 0, '>': 2, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Transiting hot Jupiters from WASP-South, Euler and TRAPPIST: WASP-95b to WASP-101b

We report the discovery of the transiting exoplanets WASP-95b, WASP-96b, WASP-97b, WASP-98b, WASP-99b, WASP-100b and WASP-101b. All are hot Jupiters with orbital periods in the range 2.1 to 5.7 d, masses of 0.5 to 2.8 Mjup, and radii of 1.1 to 1.4 Rjup. The orbits of all the planets are compatible with zero eccentricity. WASP-99b shows the shallowest transit yet found by WASP-South, at 0.4%. The host stars are of spectral type F2 to G8. Five have metallicities of [Fe/H] from -0.03 to +0.23, while WASP-98 has a metallicity of -0.60, exceptionally low for a star with a transiting exoplanet. Five of the host stars are brighter than V = 10.8, which significantly extends the number of bright transiting systems available for follow-up studies. WASP-95 shows a possible rotational modulation at a period of 20.7 d. We discuss the completeness of WASP survey techniques by comparing to the HAT project.

clear night using an array of 200mm f/1.8 lenses and a cadence of ∼ 10 mins. Transit searching of accumulated lightcurves leads to candidates that are passed to TRAP-PIST (Jehin et al. 2011), a robotic 0.6-m photometric telescope, which can resolve blends and check that the candidate transits are planet-like, and to the 1.2-m Euler/CORALIE spectrograph, for radial-velocity observations. About 1 in 12 candidates turns out to be a planet. Higher-quality transit lightcurves are then obtained with TRAPPIST and Euler-CAM (Lendl et al. 2012). A list of the observations reported here is given in Table 1 while the CORALIE radial velocities  are listed in Table A1.

THE HOST STARS
For each star, the individual CORALIE spectra were coadded to produce a single spectrum with typical S/N of ∼ 100:1 (though the fainter WASP-98, V = 13, had a S/N of only 40:1). Our methods for spectral analysis are described in Doyle et al. (2013). The excitation balance of the Fe i lines was used to determine the effective temperature (T eff ), and spectral type was estimated from T eff using the table in Gray (2008). The surface gravity (log g) was determined from the ionisation balance of Fe i and Fe ii. The Ca i line at 6439Å and the Na i D lines were also used as log g diagnostics. The metallicity was determined from equivalent width measurements of several unblended lines. The projected stellar rotation velocity (v sin i) was determined by fitting the profiles of several unblended Fe i lines. An instrumental FWHM of 0.11 ± 0.01Å was determined from the telluric lines around 6300Å.
For age estimates we use the lithium abundance and the Sestito & Randlich (2005) calibration. We also give a gyrochronological age, from the measured v sin i and assuming that the star's spin is perpendicular to us, so that this is the true equatorial speed. This is then combined with the stellar radius to give a rotational period, to compare with the results of Barnes (2007). The results for each star are listed in the Tables 2 to 10. We also list proper motions from the UCAC4 catalogue of Zacharias et al. (2013). The motions and metallicities are all compatible with the stars being local thin-disc stars.
We searched the WASP photometry of each star for rotational modulations by using a sine-wave fitting algorithm as described by Maxted et al. (2011). We estimated the significance of periodicities by subtracting the fitted transit lightcurve and then repeatedly and randomly permuting the nights of observation. We found a marginally significant modulation in WASP-95 (see Section 4.2) but not in any of the other stars (with 95%-confidence upper limits being typically 1 mmag).

SYSTEM PARAMETERS
The CORALIE radial-velocity measurements were combined with the WASP, EulerCAM and TRAPPIST photometry in a simultaneous Markov-chain Monte-Carlo (MCMC) analysis to find the system parameters. For details of our methods see Collier Cameron et al. (2007b). The limbdarkening parameters are noted in each Table, and are taken from the 4-parameter non-linear law of Claret (2000).
For all of our planets the data are compatible with zero eccentricity and hence we imposed a circular orbit (see Anderson et al. 2012 for the rationale for this). The upper limits on the eccentricity range from 0.02 (for the V = 9.5 WASP-99) to 0.27 (for the fainter, V = 12.2, WASP-96).   Table 1) together with the fitted MCMC model. (Third) The CORALIE radial velocities with the fitted model. (Lowest) The bisector spans; the absence of any correlation with radial velocity is a check against transit mimics. c 0000 RAS, MNRAS 000, range Table 3. System parameters for WASP-96.
Parameters from MCMC analysis.
The transit lightcurves lead directly to stellar density but one additional constraint is required to obtain stellar masses and radii, and hence full parametrisation of the system. Here we use the calibrations presented by Southworth (2011), based on masses and radii of eclipsing binaries.
For each system we list the resulting parameters in Tables 2 to 8, and plot the resulting data and models in Figures 1 to 7. We also refer the reader to Smith et al. (2012) who present an extensive analysis of the effect of red noise in the transit lightcurves on the resulting system parameters.
As in past WASP papers we plot the spectroscopic T eff , and the stellar density from fitting the transit, against the evolutionary tracks from Girardi et al. (2000), as shown in Fig. 8. The upper plot is the periodogram (the y-scale being the fraction of the scatter in the data that is modelled by a sinusoidal variation, weighted by the standard errors); the lower plot is the data folded on the 20.7-d period.

WASP-95
WASP-95 is a V = 10.1, G2 star with an [Fe/H] of +0.14 ± 0.16. It may be slightly evolved, with an age of several billion years. WASP-95 shows a possible rotational modulation at a period of 20.7 d and an amplitude of 2 mmag in the WASP data ( Fig. 9), though this is seen in only one of the two years of data. The values of v sin i from the spectroscopic analysis (assuming that the spin axis is perpendicular to us) and the stellar radius from the transit analysis combine to a rotation period of 19.7 ± 3.9 d, which is compatible with the possible rotational modulation.

WASP-98
At V = 13.0, WASP-98 is at the faint end of the WASP-South/CORALIE survey. The spectral analysis has a lower S/N of only 40 and so is less reliable. It appears to be exceptionally metal poor ([Fe/H] = -0.6 ± 0.19) for a transit host star. The spectral analysis suggests G7, though the transit parameters lead to a lower mass of 0.7 M⊙. The planet is a typical hot Jupiter having a high-impact (b = 0.7) transit.

WASP-99
WASP-99 is the brightest host star reported here, at V = 9.5. Spectral analysis suggests that it is an F8 star with [Fe/H] of +0.21 ± 0.15, though the transit analysis gives a higher mass (M = 1.5 M⊙) and an expanded radius (R = 1.8 R⊙). The planet is relatively massive (M = 2.8 MJup), though its mass and radius are similar to those of many known planets.
The transit of WASP-99b is the shallowest yet found by WASP-South, at 0.0041 ± 0.0002, along with that of WASP-72b at 0.0043 ± 0.0004 (Gillon et al. 2013).

COMPLETENESS
With the WASP survey now passing WASP-100 we can ask how complete the survey methods are and how many planets we are missing. A full discussion of selection effects is a large topic and is not attempted here, but we can use the HAT project as a straightforward check on our techniques. The HAT project (Bakos et al. 2004) is very similar in conception and hardware to WASP, and thus whether a HAT planet is also detected by us gives an indication of how many we are overlooking.   . 11 shows, for each HAT planet (up to HAT-P-46 and HATS-3b), the number of data points it has in the WASP survey and whether we also detect it. There is some level of subjectivity in claiming a detection, since all WASP candidates are scrutinised by eye, and thus two planets are shown as marginal detections. Most non-detections result from there being little or no WASP data (< 6000 data points), but it is worthwhile to review the remaining 7 cases.
HAT-P-1 (Bakos et al. 2007) is bright and has 14 000 points in WASP data. It isn't detected owing to some excess noise in some parts of our automated photometry, which prevents the transit-search algorithm from finding the transits. HAT-P-9b (Shporer et al. 2009) has V = 12.3 and there are 11 000 WASP points. There is excess noise in some of the WASP photometry, preventing the search algorithm finding the transit. These two are the worst failures of the WASP techniques applied to the HAT sample.
HAT-P-37 (Bakos et al. 2012) at V = 13.2 is fainter than any WASP planet, and also has a brighter eclipsing binary 68 ′′ away, which misleads the WASP search algorithms. HAT-P-38 (Sato et al. 2012) is relatively faint (V = 12.6) and there is relatively limited WASP data (9000 points).
Of the two marginal detections, HAT-P-19b (Hartman et al. 2011) has 12 000 WASP points but is faint (V = 12.9) and has an orbital period of 4.008 d. As a single-longitude survey, WASP's sampling hampers the finding of integer-day periods. HAT-P-15b (Kovács et al. 2010) is also below 12th magnitude (V = 12.2), and has relatively sparse coverage by WASP (9000 points), and also has a long orbital of 10.86 d, giving fewer transits than the typical 2-5-d hot Jupiters.
Thus, in summary, at brighter than V = 12.8 and given 10 000 WASP points (roughly two seasons of data) we fail to detect only 2 out of 23 HAT-discovered planets (note that the number 23 doesn't include independent discoveries by HAT of WASP planets). Thus we conclude that, in well-covered regions of sky, the WASP-South survey techniques give fairly complete discoveries for the sort of planets findable by WASP-like surveys. That means hot Jupiters around stars in the magnitude range V = 9-13, and excluding crowded areas of sky such as the galactic plane. It also applies only to stars later than mid F, since hotter stars don't give good RV signals.
The lower period limit of 0.8 d is likely a real cut-off in the distribution of hot Jupiters (e.g., Hellier et al. 2011), since we routinely look for candidates down to periods of 0.5 d. The longer period limit is primarily set by the amount of observational coverage, and our completeness will drop off above P orb ∼ 7 d, though this could increase to 'warm' Jupiters beyond ∼ 10 d as WASP continues to accumulate data.
The upper limit in planetary size is also likely a real feature of hot Jupiters, given the number of systems found with R = 1.8-2.0 RJup, but not above that range. The lower size limit of WASP discoveries is set primarily by red noise and so is harder to evaluate. Fig. 12 shows the transit depths of WASP planets, suggesting that we have a good discovery probability down to depths of ∼ 0.5% in the magnitude range V = 9-12. This is sufficient for R ∼ > 0.9 RJup given R * < 1.3 R ⊙ , and ∼ > 0.7 RJup given < 1.0 R ⊙ , and thus is sufficient for most hot Jupiters.