SuperWASP Results

No evidence for an additional planet in the WASP-3 system:

A new analysis of the WASP-3 system: no evidence for an additional companion
http://arxiv.org/abs/1211.0218

WASP-52b, WASP-58b, WASP-59b, and WASP-60b: four new transiting close-in giant planets
http://arxiv.org/abs/1211.0810

Transits and starspots in the WASP-19 planetary system
http://arxiv.org/abs/1211.0864

WASP-19 is found to be reasonably well aligned, whereas WASP-52 seems to have a slight misalignment.

Great. SuperWASP is a true inventory of transiting hot Jupiters, better than Kepler or Corot. In a few years of further discoveries it could start to draw statistics on its own about characteristics of this particular class of planetary population.

WASP-71b: a bloated hot Jupiter in an 2.9-day, prograde orbit around an evolved F8 star
http://arxiv.org/abs/1211.3045

Quote :

We report the discovery by the WASP transit survey of a highly-irradiated, massive (2.258 +/- 0.072 MJup) planet which transits a bright (V = 10.6), evolved F8 star every 2.9 days. The planet, WASP-71b, is larger than Jupiter (1.50 +/- 0.11 RJup), but less dense (0.67 +/- 0.14 {\rho}Jup). We also report spectroscopic observations made during transit with the CORALIE spectrograph, which allow us to detect the Rossiter-McLaughlin effect. We determine the sky-projected angle between the stellar-spin and planetary-orbit axes to be {\lambda} = 19.8 +/- 9.9 degrees.

A growing number of transiting planets in double systems: WASP-77 Ab (Cetus).

WASP-77 Ab: A transiting hot Jupiter planet in a wide binary system

Quote :

We report the discovery of a transiting planet with an orbital period of 1.36d orbiting the brighter component of the visual binary star BD -07 436. The host star, WASP-77A, is a moderately bright G8V star (V=10.3) with a metallicity close to solar ([Fe/H]= 0.0 +- 0.1). The companion star, WASP-77B, is a K-dwarf approximately 2 magnitudes fainter at a separation of approximately 3arcsec. The spectrum of WASP-77A shows emission in the cores of the Ca II H and K lines indicative of moderate chromospheric activity. The WASP lightcurves show photometric variability with a period of 15.3 days and an amplitude of about 0.3% that is probably due to the magnetic activity of the host star. We use an analysis of the combined photometric and spectroscopic data to derive the mass and radius of the planet (1.76+-0.06MJup, 1.21+-0.02RJup). The age of WASP-77A estimated from its rotation rate (~1 Gyr) agrees with the age estimated in a similar way for WASP-77B (~0.6 Gyr) but is in poor agreement with the age inferred by comparing its effective temperature and density to stellar models (~8 Gyr). Follow-up observations of WASP-77 Ab will make a useful contribution to our understanding of the influence of binarity and host star activity on the properties of hot Jupiters.

WASP-33b has a very high brightness temperature suggesting rapid re-radiation of absorbed insolation as expected.
http://arxiv.org/abs/1301.3380

No evidence of TTVs at WASP-10.
http://arxiv.org/abs/1301.3760

Observations of the WASP-2 System by the APOSTLE Program
http://arxiv.org/abs/1301.3955

No TTVs for WASP-2. Seems to be a generic property of hot Jupiter systems, which means that the systems most easily observed from the ground are those which are least likely to exhibit TTV:

Quote :

It is likely that the lack of TTVs being detected from the ground is due to a fundamental property of the systems that are being studied. The vast majority of ground–based follow–up is focused on hot–Jupiter systems, since resolving their transit depths is achievable even with modest aperture telescopes and non photometric observing conditions. However, as outlined by Steffen et al. (2012b), hot–Jupiter systems observed by Kepler also fail to show detectable TTVs, or any evidence for being in a multi–planet system. Their neighbors in exoplanet parameter space, loosely termed warm-Jupiters and hot–Neptunes, do show evidence for both TTVs and transiting companions. What this suggests is a unique dynamical pathway for the formation of contemporary hot–Jupiters, such as multi–planet scattering (e.g. Beaugé & Nesvorný 2012) leading to the ejection of lesser bodies from the system.

So has SuperWASP team gotten its own hot Jupiter around a late-K/M-dwarf: WASP-80 b.

Found in A&A forthcoming free PDF papers.

Oooh nice, looks like it might be a good target to follow-up for studying warm Jupiter atmospheres:

Quote :

WASP-80b’s equilibrium temperature will be around 800K (for an albedo of 0.1). The planet-to-star contrast is favourable for future observation of the emission spectrum of the planet, because it is hosted by a star ~1500K colder than the usual targets. Furthermore, the near 3% depth of the transit makes this gas giant one of the most suitable targets for transmission spectroscopy.

Now on EPE
http://voparis-exoplanet-new.obspm.fr/catalog/wasp-80_b/

WASP-80b on arXiv :
http://arxiv.org/abs/1303.0254

WASP-80b: a gas giant transiting a cool dwarf

Absorbing gas around the WASP-12 planetary system
http://arxiv.org/abs/1303.3375

Something seems to be absorbing the Mg II h&k lines, perhaps material evaporating from the hot Jupiter.

Secondary Eclipse Photometry of the Exoplanet WASP-5b with Warm Spitzer
http://arxiv.org/abs/1303.3886

Orbit consistent with circular, no evidence for eclipse timing variations.

Spin-orbit alignments for three more WASP systems.
http://arxiv.org/abs/1303.5649

Discovery of WASP-65b and WASP-75b: Two Hot Jupiters Without Highly Inflated Radii

Quote :

We report the discovery of two transiting hot Jupiters, WASP-65b (M_pl = 1.55 +/- 0.16 M_J; R_pl = 1.11 +/- 0.06 R_J), and WASP-75b (M_pl = 1.07 +/- 0.05 M_J; R_pl = 1.27 +/- 0.05 R_J). They orbit their host star every 2.311, and 2.484 days, respectively. The planet host WASP-65 is a G6 star (T_eff = 5600 K, [Fe/H] = -0.07 +/- 0.07, age > 8 Gyr); WASP-75 is an F9 star (T_eff = 6100 K, [Fe/H] = 0.07 +/- 0.09, age of 3 Gyr). The mean density of WASP-65b is similar to that of Jupiter (rho_pl = 1.13 +/- 0.08 rho_J), and in fact, WASP-65b is one of the densest planets with a mass between 0.1 and 2.0 M_J, a mass range in which a large fraction of the known planets have been found to be inflated with respect to theoretical planet models. WASP-65b is one of only a handful of planets with masses of around 1.5 M_J, a mass regime surprisingly underrepresented among the currently known hot Jupiters. The radius of Jupiter-mass WASP-75b is slightly inflated (< 10%) as compared to theoretical planet models with no core, and has a density similar to that of Saturn (rho_pl = 0.52 +/- 0.06 rho_J).

Hot Jupiter party.

WASP-76b, WASP-82b, WASP-90b
WASP-95b, WASP-96b, WASP-97b, WASP-98b, WASP-99b, WASP-100b, WASP-101b
WASP-69b, WASP-84b, WASP-70 Ab

WASP-69 and 70 are already known but the third paper provides updated system characterisation.

Quote :

Hot Jupiter party.

 

Let's celebrate broken record: more than 1,000 exoplanets!


http://exoplanet.eu/catalog/wasp-76_b/
http://exoplanet.eu/catalog/wasp-82_b/
http://exoplanet.eu/catalog/wasp-84_b/
http://exoplanet.eu/catalog/wasp-90_b/
http://exoplanet.eu/catalog/wasp-95_b/
http://exoplanet.eu/catalog/wasp-96_b/
http://exoplanet.eu/catalog/wasp-97_b/
http://exoplanet.eu/catalog/wasp-98_b/
http://exoplanet.eu/catalog/wasp-99_b/
http://exoplanet.eu/catalog/wasp-100_b/
http://exoplanet.eu/catalog/wasp-101_b/

Tantalizing update... Up to WASP-112.

http://www.astro.keele.ac.uk/~ch/wasps.html

Trawling for transits in a sea of noise: A Search for Exoplanets by Analysis of WASP Optical Lightcurves and Follow-up (SEAWOLF)
http://arxiv.org/abs/1310.7586

No confirmed detections but a handful of candidates and some odd discrepancies in statistics.

WASP-68 b, as well as two new ones: WASP-73 b and WASP-88 b.
http://arxiv.org/abs/1312.1827

The stars are all fairly evolved.

Of the old bunch WASP-20 and WASP-53 b are left. Now we have a new transiting planet in Capricornus and 2 more in Indus. Up to date there was a dearth of planets in the latter sky field.

New WASP planet. Something recalling WASP-18 b, I guess.

WASP-103b: a new planet at the edge of tidal disruption

Quote :

We report the discovery of WASP-103b, a new ultra-short-period planet (P=22.2 hr) transiting a 12.1 V-magnitude F8-type main-sequence star (1.22+-0.04 Msun, 1.44-0.03+0.05 Rsun, Teff = 6110+-160 K). WASP-103b is significantly more massive (1.49+-0.09 Mjup) and larger (1.53-0.07+0.05 Rjup) than Jupiter. Its large size and extreme irradiation (around 9 10^9 erg/s/cm^2) make it an exquisite target for a thorough atmospheric characterization with existing facilities. Furthermore, its orbital distance is less than 20% larger than its Roche radius, meaning that it might be significantly distorted by tides and might experience mass loss through Roche-lobe overflow. It thus represents a new key object for understanding the last stage of the tidal evolution of hot Jupiters.

Oldie but goldie. Official publication of WASP-20 and 28 b. About time!

WASP-20b and WASP-28b: a hot Saturn and a hot Jupiter in near-aligned orbits around solar-type stars

Quote :

We report the discovery of the planets WASP-20b and WASP-28b along with measurements of their sky-projected orbital obliquities. WASP-20b is an inflated, Saturn-mass planet (0.31 M_Jup  ; 1.46 R_Jup  ) in a 4.9-day, near-aligned (λ=8.1±3.6°) orbit around CD-24 102 (V =10.7; F9). WASP-28b is an inflated, Jupiter-mass planet (0.91 M_Jup  ; 1.21 R_Jup  ) in a 3.4-day, near-aligned (λ=8±18°) orbit around a V =12, F8 star. As intermediate-mass planets in short orbits around aged, cool stars (7_-1⁺² Gyr for WASP-20 and 5_-2⁺³   Gyr for WASP-28; both with T eff   < 6250 K), their orbital alignment is consistent with the hypothesis that close-in giant planets are scattered into eccentric orbits with random alignments, which are then circularised and aligned with their stars' spins via tidal dissipation.

So what's going on with the discovery of WASP-28b? I take it then that the West et al. preprint that's been on the SuperWASP website since 2010 never got accepted in a refereed journal (was it ever submitted I wonder)?