SuperWASP Results

Three Hot-Jupiters on the upper edge of the mass-radius distribution: WASP-177, WASP-181 and WASP-183
https://arxiv.org/abs/1903.06622

Quote :

We present the discovery of 3 transiting planets from the WASP survey, two hot-Jupiters: WASP-177b (~0.5 M_Jup, ~1.6 R_Jup) in a 3.07-d orbit of a V = 12.6 K2 star, WASP-183b (~0.5 M_Jup, ~1.5 R_Jup) in a 4.11-d orbit of a V = 12.8 G9/K0 star; and one hot-Saturn planet WASP-181b (~0.3 M_Jup, ~1.2 R_Jup) in a 4.52-d orbit of a V = 12.9 G2 star. Each planet is close to the upper bound of mass-radius space and has a scaled semi-major axis, a/R_star, between 9.6 and 12.1. These lie in the transition between systems that tend to be in orbits that are well aligned with their host-star's spin and those that show a higher dispersion.

WASP-180Ab: Doppler tomography of an hot Jupiter orbiting the primary star in a visual binary
https://arxiv.org/abs/1903.08002

Quote :

We report the discovery and parametrisation of WASP-180Ab, a hot Jupiter confirmed by the detection of its Doppler shadow and by measuring its mass using radial velocities. We find the 0.8 ± 0.1 MJup, 1.29 ± 0.07 RJup planet to be in a misaligned, retrograde orbit around an F7 star with Teff = 6500K and a moderate rotation speed of vsini = 21 km s−1. The host star is the primary of a V = 10.7 binary, where a secondary separated by 5′′ contributes ∼30% of the light. WASP-180Ab therefore adds to a small sample of transiting hot Jupiters known in binary systems. A 4.6-day modulation seen in the WASP data is likely to be the rotational modulation of the companion star, WASP-180B.

WASP-169, WASP-171, WASP-175 and WASP-182: One bloated sub-Saturn and three hot Jupiters discovered by WASP-south
https://arxiv.org/abs/1904.10388#

Quote :

We present the discovery of four giant WASP-south planets, three hot Jupiters and one bloated sub-Saturn; WASP-169b, WASP-171b, WASP-175b and WASP-182b. Besides the discovery photometry from WASP-south we use follow-up observations from CORALIE, HARPS, EulerCam, TRAPPIST-North and -South and SPECULOOS. WASP-169b is a low density Jupiter (M=0.561±0.061 MJup,R=1.304+0.150−0.073 RJup) orbiting a V=12.17 F8 sub-giant in a 5.611~day orbit. WASP-171b is a typical hot Jupiter (M=1.084±0.094 MJup,R=0.98+0.07−0.04 RJup, P=3.82 days) around a V=13.05 G0 star. We find a linear drift in the radial velocities of WASP-171 spanning 3.5 years, indicating the possibility of an additional outer planet. WASP-175b is an inflated hot Jupiter (M=0.99±0.13 MJup,R=1.208±0.081 RJup, P=3.07 days) around a V=12.04 F7 star, which possibly is part of a binary system with a star 7.9\arcsec\ away. WASP-182b is a bloated sub-Saturn (M=0.148±0.011 MJup,R=0.850±0.030 RJup) around a metal rich V=11.98 G5 star ([Fe/H]=0.27±0.11). With a orbital period of P=3.377 days, it sits right in the apex of the sub-Jovian desert, bordering the upper- and lower edge of the desert in both the mass-period and radius-period plane. WASP-169b, WASP-175b and WASP-182b are promising targets for atmospheric characterisation through transmission spectroscopy, with expected transmission signals of 121, 150 and 264 ppm respectively.

WASP-South hot Jupiters: WASP-178b, WASP-184b, WASP-185b & WASP-192b
https://arxiv.org/abs/1907.11667

Quote :

We report on four new transiting hot Jupiters discovered by the WASP-South survey. WASP-178b transits a V = 9.9, A1V star with Teff = 9350 +/- 150 K, the second-hottest transit host known. It has a highly bloated radius of 1.81 +/- 0.09 Rjup, in line with the known correlation between high irradiation and large size. With an estimated temperature of 2470 +/- 60 K, the planet is one of the best targets for studying ultra-hot Jupiters that is visible from the Southern hemisphere. The three host stars WASP-184, WASP-185 and WASP-192 are all post-main-sequence G0 stars of ages 4-8 Gyr. The larger stellar radii (1.3-1.7 Msun) mean that the transits are relatively shallow (0.7-0.9%) even though the planets have moderately inflated radii of 1.2-1.3 Rjup. WASP-185b has an eccentric orbit (e = 0.24) and a relatively long orbital period of 9.4 d. A star that is 4.6 arcsec from WASP-185 and 4.4 mag fainter might be physically associated.

I checked the TESS ExoFOP and despite being in the southern hemisphere, none of these four planets have assigned TOIs, and the paper doesn't really mention TESS beyond a quick blurb in the intro.  I'll be keeping an eye on it though.

WASP-178 = HD 134004 = TIC 160708862
WASP-184 = 2MASS J13580408-3020532 = TIC 112099249
WASP-185 = 2MASS J14161431-1932321 = TIC 46020827
WASP-192 = 2MASS J14543809-3844403 = TIC 160578764

The intro also contains this interestng bit:

Quote :

WASP-South transit candidates proved well matched to follow-up with the 1.2-m Euler telescope and CORALIE spectrograph, teamed with the TRAPPIST-South and (more recently) TRAPPIST-North photometric telescopes, which together observed 1600 planet candidates.

Is this the first we've heard about general TRAPPIST results? (aside of course from TRAPPIST-1)

Signs of an outer companion at WASP-4:

Bouma et al. "WASP-4 is Accelerating Toward the Earth"
https://arxiv.org/abs/2004.00637

The companion is estimated as being in the range 10–300 Jupiter masses at a distance of 10–100 AU.

Two transiting hot Jupiters from the WASP survey: WASP-150b and WASP-176b
https://arxiv.org/abs/2004.06622

Lazarus wrote:

Signs of an outer companion at WASP-4:

Or maybe not...

Baluev et al. "WASP-4 transit timing variation from a comprehensive set of 129 transits"
https://arxiv.org/abs/2004.09109

Quote :

While this Letter was in review, Bouma et al. (2020) reported a radial acceleration of WASP-4 of −15 m s⁻¹ yr⁻¹ based on new Keck data. This would explain the observed TTV through the light arrival delay, but they did not use full CORALIE and HARPS data from Baluev et al. (2019). This full dataset appears strongly inconsistent with their value for c₁, see Fig. 2 in the online-only supplement. The RV trend is only supported by a few recent Keck observations made after a long pause. This indicates that the RV variation they captured looks like a severely nonlinear RV variation rather than constant radial acceleration. This makes their conclusions that RV variation can explain the TTV disputable. RV was nearly constant at least until 2014, while only recently accumulating observable bias. Such a nonlinear RV variation may induce a much smaller TTV than constant acceleration. We believe that results by Bouma et al. (2020) need to be reassessed in view of complete RV data, but this is a work for separate investigation.

Discovery and characterization of the exoplanets WASP-148b and c. A transiting system with two interacting giant planets
https://arxiv.org/abs/2004.14645

Quote :

We present the discovery and characterization of WASP-148, a new extrasolar system including at least two giant planets. The host star is a slowly rotating, inactive late-G dwarf with a V=12 magnitude. The planet WASP-148b is a hot Jupiter of 0.72 RJup and 0.29 MJup transiting its host with an orbital period of 8.80 days. We found the planetary candidate with the SuperWASP photometric survey then characterized it with the SOPHIE spectrograph. Our radial velocity measurements subsequently revealed the presence of a second planet in the system, WASP-148c, with an orbital period of 34.5 days and a minimum mass of 0.40 MJup. No transits of that outer planet were detected. The orbits of both planets are eccentric and fall near the 4:1 mean-motion resonances. That configuration is stable on long time scales but induces dynamical interactions so the orbits slightly differ from purely Keplerian orbits. In particular, WASP-148b shows transit timing variations of typically 15 minutes making it one of the few cases with TTVs detected on ground-based light curves. We establish the orbital plane of both planets could not have a mutual inclination larger than 35 degrees, and the true mass of WASP-148c is below 0.60 MJup. We present photometric and spectroscopic observations of that system covering a time span of ten years, and their Keplerian and Newtonian analyses; they should be significantly improved thanks to future TESS observations.

A second planet at WASP-107, and a lower density for the b planet.

WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration
https://arxiv.org/abs/2011.13444

An update on WASP-148

A Newtonian model for the WASP-148 exoplanetary system enhanced with TESS and ground-based photometric observations
https://arxiv.org/abs/2012.02602

Additional planet in WASP-107 system, beyond the snowline:

WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration

Quote :

With a mass in the Neptune regime and a radius of Jupiter, WASP-107b presents a challenge to planet formation theories. Meanwhile, the planet's low surface gravity and the star's brightness also make it one of the most favorable targets for atmospheric characterization. Here, we present the results of an extensive 4-year Keck/HIRES radial-velocity (RV) follow-up program of the WASP-107 system and provide a detailed study of the physics governing the accretion of its gas envelope. We reveal that WASP-107b's mass is only 1.8 Neptune masses (M_b=30.5±1.7 M_⊕). The resulting extraordinarily low density suggests that WASP-107b has a H/He envelope mass fraction of >85% unless it is substantially inflated. The corresponding core mass of <4.6 M_⊕ at 3σ is significantly lower than what is traditionally assumed to be necessary to trigger massive gas envelope accretion. We demonstrate that this large gas-to-core mass ratio most plausibly results from the onset of accretion at ≳1 AU onto a low-opacity, dust-free atmosphere and subsequent migration to the present-day a_b=0.0566±0.0017 AU. Beyond WASP-107b, we also detect a second more massive planet (M_c sin i=0.36±0.04 M_J) on a wide eccentric orbit (e_c=0.28±0.07) which may have influenced the orbital migration and spin-orbit misalignment of WASP-107b. Overall, our new RV observations and envelope accretion modeling provide crucial insights into the intriguing nature of WASP-107b and the system's formation history. Looking ahead, WASP-107b will be a keystone planet to understand the physics of gas envelope accretion.

Also featuring at NASA Exoplanet Archive with a dedicated NASA page too.

Additional planet in WASP-107 system, beyond the snowline:

WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration

Quote :

With a mass in the Neptune regime and a radius of Jupiter, WASP-107b presents a challenge to planet formation theories. Meanwhile, the planet's low surface gravity and the star's brightness also make it one of the most favorable targets for atmospheric characterization. Here, we present the results of an extensive 4-year Keck/HIRES radial-velocity (RV) follow-up program of the WASP-107 system and provide a detailed study of the physics governing the accretion of its gas envelope. We reveal that WASP-107b's mass is only 1.8 Neptune masses (M_b=30.5±1.7 M_⊕). The resulting extraordinarily low density suggests that WASP-107b has a H/He envelope mass fraction of >85% unless it is substantially inflated. The corresponding core mass of <4.6 M_⊕ at 3σ is significantly lower than what is traditionally assumed to be necessary to trigger massive gas envelope accretion. We demonstrate that this large gas-to-core mass ratio most plausibly results from the onset of accretion at ≳1 AU onto a low-opacity, dust-free atmosphere and subsequent migration to the present-day a_b=0.0566±0.0017 AU. Beyond WASP-107b, we also detect a second more massive planet (M_c sin i=0.36±0.04 M_J) on a wide eccentric orbit (e_c=0.28±0.07) which may have influenced the orbital migration and spin-orbit misalignment of WASP-107b. Overall, our new RV observations and envelope accretion modeling provide crucial insights into the intriguing nature of WASP-107b and the system's formation history. Looking ahead, WASP-107b will be a keystone planet to understand the physics of gas envelope accretion.

Also featuring at NASA Exoplanet Archive with a dedicated NASA page too.

Uncertain whether updating "WASP" or "KELT results", I choose the former and post here the case of this "1SWASP J1407-analogue":

Periodic Eclipses of the Young Star PDS 110 Discovered with WASP and KELT Photometry

Quote :

We report the discovery of eclipses by circumstellar disc material associated with the young star PDS 110 in the Ori OB1a association using the SuperWASP and KELT surveys. PDS 110 (HD 290380, IRAS 05209-0107) is a rare Fe/Ge-type star, a ~10 Myr-old accreting intermediate-mass star showing strong infrared excess (L_IR/L_bol ~ 0.25). Two extremely similar eclipses with a depth of ~30% and duration ~25 days were observed in November 2008 and January 2011. We interpret the eclipses as caused by the same structure with an orbital period of 808±2 days. Shearing over a single orbit rules out diffuse dust clumps as the cause, favouring the hypothesis of a companion at ~2AU. The characteristics of the eclipses are consistent with transits by an unseen low-mass (1.8-70M_Jup) planet or brown dwarf with a circum-secondary disc of diameter ~0.3 AU. The next eclipse event is predicted to take place in September 2017 and could be monitored by amateur and professional observatories across the world.

Doubts have been cast about the presence of a substellar companion...

The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic

Quote :

PDS 110 is a young disk-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in September 2017. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for RV oscillations caused by any hypothetical companion and can rule out close binaries to 0.1 M_⊙. A search of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 years, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and shorter-duration than those of UX Ori variables, but may have a similar mechanism.

However the latest paper explicitly mentions a "PDS 110 b", seemingly a ringed brown dwarf.

Constraining the nature of the possible extrasolar PDS110b ring system

Quote :

The young star PDS110 in the Ori OB1a association underwent two similar eclipses in 2008 and 2011, each of which lasted for a period of at least 25 days. One plausible explanation for these events is that the star was eclipsed by an unseen giant planet (named PDS110b) circled by a ring system that fills a large fraction of its Hill sphere. Through thousands of numerical simulations of the three-body problem, we constrain the mass and eccentricity of this planet as well the size and inclination of its ring, parameters that are not well determined by the observational data alone. We carried out a broad range of different configurations for the PDS110b ring system and ruled out all that did not match with the observations. The result shows that the ring system could be prograde or retrograde; the preferred solution is that the ring has an inclination lower than 60∘ and a radius between 0.1 and 0.2 au and that the planet is more massive than 35M_Jup and has a low eccentricity (<0.05).

Albeit related to TESS research, this concerns WASP planets...

WASP-35 and HAT-P-30/WASP-51: re-analysis using TESS and ground-based transit photometry

Quote :

High-precision transit observations provide excellent opportunities for characterizing the physical properties of exoplanetary systems. These physical properties supply many pieces of information for unvealing the internal structure, external atmosphere, and dynamical history of the planets. We present revised properties of transiting systems WASP-35 and HAT-P-30/WASP-51 through analyzing newly available TESS photometry and ground-based observations obtained at 1m telescope of Yunnan Observatories as well as from the literature. The improved system parameters are consistent with the previous results. Furthermore, we find that HAT-P-30b/WASP-51b's transits show significant timing variation which cannot be explained by decaying orbit due to tidal dissipation and the Rømer effect, while both apsidal precession and an additional perturbing body could reproduce this signal through our comprehensive dynamical simulations. Because both of them are valuable targets which are suitable for transmission spectroscopy, we make some predictions for atmospheric properties of WASP-35b and HAT-P-30b/WASP-51b based on newly derived system parameters.

Something at 1SWASP J182438.34+302546.0, spotted by a Zooniverse user:

Norton et al. "A SuperWASP Light Curve Displaying a Single Long-duration Transit: A Jupiter Size Exoplanet in a Very Distant Orbit?"
https://iopscience.iop.org/article/10.3847/2515-5172/ac6811

If it's a transit, it would be a ~1.8 Rj object at ~205 au from a slightly evolved A7V star. Not sure if 1.8 Rj is a plausible radius for a planet though?

Lazarus wrote:

Something at 1SWASP J182438.34+302546.0, spotted by a Zooniverse user:

Norton et al. "A SuperWASP Light Curve Displaying a Single Long-duration Transit: A Jupiter Size Exoplanet in a Very Distant Orbit?"
https://iopscience.iop.org/article/10.3847/2515-5172/ac6811

If it's a transit, it would be a ~1.8 Rj object at ~205 au from a slightly evolved A7V star. Not sure if 1.8 Rj is a plausible radius for a planet though?

Unless newly, newly formed, likely. But if the host star is "slightly evolved", some doubts are raised and the M dwarf option is more likely.

Quote :

Norton et al. "A SuperWASP Light Curve Displaying a Single Long-duration Transit: A Jupiter Size Exoplanet in a Very Distant Orbit?"

Jupiter size? This one is almost twice Jupiter's radius!

Better relying on imaging techniques for the follow-up rather than waiting for other transits in next... centuries

By the way, nice find!

Lazarus wrote:

Something at 1SWASP J182438.34+302546.0, spotted by a Zooniverse user:

Norton et al. "A SuperWASP Light Curve Displaying a Single Long-duration Transit: A Jupiter Size Exoplanet in a Very Distant Orbit?"
https://iopscience.iop.org/article/10.3847/2515-5172/ac6811

If it's a transit, it would be a ~1.8 Rj object at ~205 au from a slightly evolved A7V star. Not sure if 1.8 Rj is a plausible radius for a planet though?

A comment to the discovery claim...

WASP Lightcurves: Red Noise and a Cautionary Tale

Indeed it did sound a little unrealistic as detection but I liked having hopes

Something has got to be there by the way.

I love detections of this kind

A hot super-Earth planet in the WASP-84 planetary system

Quote :

Hot Jupiters have been perceived as loners devoid of planetary companions in close orbital proximity. However, recent discoveries based on space-borne precise photometry have revealed that at least some fraction of giant planets coexists with low-mass planets in compact orbital architectures. We report detecting a 1.446-day transit-like signal in the photometric time series acquired with the Transiting Exoplanet Survey Satellite (TESS) for the WASP-84 system, which is known to contain a hot Jupiter on a circular 8.5-day orbit. The planet was validated based on TESS photometry, and its signal was distilled in radial velocity measurements. The joint analysis of photometric and Doppler data resulted in a multi-planetary model of the system. With a mass of 15M⊕, radius of 2R⊕, and orbital distance of 0.024 au, the new planet WASP-84 c was classified as a hot super-Earth with the equilibrium temperature of 1300 K. A growing number of companions to hot Jupiters indicates that a non-negligible part of them must have formed under a quiescent scenario such as disc migration or in-situ formation.

WASP-193b: An extremely low-density super-Neptune
https://arxiv.org/abs/2307.08350

Quote :

Gas giants transiting bright nearby stars are stepping stones for our understanding of planetary system formation and evolution mechanisms. This paper presents a particularly interesting new specimen of this kind of exoplanet discovered by the WASP-South transit survey, WASP-193b. This planet completes an orbit around its Vmag = 12.2 F9 main-sequence host star every 6.25 d. Our analyses found that WASP-193b has a mass of Mp = 0.139 +/- 0.029 M_Jup and a radius of Rp = 1.464 +/- 0.058 R_ Jup, translating into an extremely low density of rhop = 0.059 +\- 0.014 g/cm^3. The planet was confirmed photometrically by the 0.6-m TRAPPIST-South, the 1.0-m SPECULOOS-South telescopes, and the TESS mission, and spectroscopically by the ESO-3.6-m/HARPS and Euler-1.2-m/CORALIE spectrographs. The combination of its large transit depth (dF~1.4 %), its extremely-low density, its high-equilibrium temperature (Teq = 1254 +/- 31 K), and the infrared brightness of its host star (magnitude Kmag=10.7) makes WASP-193b an exquisite target for characterization by transmission spectroscopy (transmission spectroscopy metric: TSM ~ 600). One single JWST transit observation would yield detailed insights into its atmospheric properties and planetary mass, within ~0.1 dex and ~1% (vs ~20% currently with radial velocity data) respectively.