SuperWASP Results

http://www.astronomynow.com/nam09/2009/04/transiting-planets-galore.html
WASP-20b is the 0.3 mass of Jupiter at 5 days orbit.

Borislav wrote:

http://www.astronomynow.com/nam09/2009/04/transiting-planets-galore.html
WASP-20b is the 0.3 mass of Jupiter at 5 days orbit.

I'm not convinced it is the same candidate, since WASP-21b has very similar parameters.

A search for transit timing variation
http://arxiv.org/abs/1010.3122

Quote :

Photometric follow-ups of transiting exoplanets (TEPs) may lead to discoveries of additional, less massive bodies in extrasolar systems. This is possible by detecting and then analysing variations in transit timing of transiting exoplanets. In 2009 we launched an international observing campaign, the aim of which is to detect and characterise signals of transit timing variation (TTV) in selected TEPs. The programme is realised by collecting data from 0.6--2.2-m telescopes spread worldwide at different longitudes. We present our observing strategy and summarise first results for WASP-3b with evidence for a 15 Earth-mass perturber in an outer 2:1 orbital resonance.

Doesn't seem to say anything we didn't already know.

Just checked http://www.astro.keele.ac.uk/~ch/wasps.html, Lists blank entries up to WASP-47! (Other than most of them are WASP-S)

http://iaus276.oato.inaf.it/IAUS_276/Program/Oral/session2/Faedi.pdf

Quote :

WASP-35b
Enoch et al. in prep.
Period = 1.5 days
Mpl ≈ 2.3 MJup
Rpl ≈ 1.6 RJup
The first joint WASP North/South planet

Quote :

WASP-39b
Faedi et al. 2010 in prep
P = 4d
Mpl ~ 0.3 Mjup
Rpl ~ 1.3 RJup
highly bloated planet around a late G8 star (~5Gyr)
- radius is 1.55 Lmes Saturn radius
- The least dense Saturn-mass planet from WASP-N
ρ≈0.13ρJ

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WASP-40b
West et al. in prep.
Need more data to solve the system
2 planets? (P≈3d and P≈26d)

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HAT-P-14b=WASP-27b independent discovery

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WASP detecIon rate is 1 planet every 8 candidates
To date we have 158 candidates in the archive

sky coverage in 2008



sky coverage in 2010

Gotta love those descriptions of 6-day planets as "long-period"...

In general, it remains to determine the nature of only three systems (among the first four dozen) - WASP-20, WASP-23 and WASP-34. Although it is possible they can actually be brown dwarfs.

WASP-31b: a low-density planet transiting a late-F-type star
http://arxiv.org/abs/1011.5882

Quote :

We report the discovery of the low-density, transiting giant planet WASP-31b. The planet is 0.47 Jupiter masses and 1.56 Jupiter radii. It is in a 3.4-day orbit around a 1-Gyr-old, late-F-type, V = 11.7 star, which is a member of a common proper motion pair. In terms of its low density, WASP-31b is second only to WASP-17b, which is a more highly irradiated planet of similar mass.

Finally. Now there's WASP-36 left to announce. As well as the other candidates left, of course.

WASP-34b: a near-grazing transiting sub-Jupiter-mass exoplanet in a hierarchical triple system
http://arxiv.org/abs/1012.2278

Quote :

We report the discovery of WASP-34b, a sub-Jupiter-mass exoplanet transiting its 10.4-magnitude solar-type host star (1SWASP J110135.89-235138.4; TYC 6636-540-1) every 4.3177 days in a slightly eccentric orbit (e = 0.038 +/- 0.012). We find a planetary mass of 0.59 +/- 0.01 M_Jup and radius of 1.22 ^{+0.11}_{-0.08} R_Jup. There is a linear trend in the radial velocities of 55+/-4 m/s/y indicating the presence of a long-period third body in the system with a mass > 0.45 M_Jup at a distance of >1.2 AU from the host star. This third-body is either a low-mass star, white dwarf, or another planet. The transit depth ((R_P/R_*)^2 = 0.0126) and high impact parameter (b = 0.90) suggest that this could be the first known transiting exoplanet expected to undergo grazing transits, but with a confidence of only ~80%.

Also, this paper is a bit of candy.
The WASP-South search for transiting exoplanets
http://arxiv.org/abs/1012.2286

Quote :

Since 2006 WASP-South has been scanning the Southern sky for transiting exoplanets. Combined with Geneva Observatory radial velocities we have so far found over 30 transiting exoplanets around relatively bright stars of magnitude 9--13. We present a status report for this ongoing survey.

Another planet with no coordinates

http://exoplanet.eu/star.php?st=WASP-41

EDIT* - Maybe Hydra. See approximate coordinates in Hellier et al. (2010) arxiv paper. There is also WASP-23, likely in Puppis.

http://exoplanet.eu/star.php?st=WASP-23

I guess the large yield of the SuperWASP survey as compared to the space-based missions just goes to show the advantage of targeting relatively bright stars.

Pity TESS lost out in the mission selection process.

maybe still hope about TESS:

http://www.centauri-dreams.org/?p=11098#comments

http://www.popsci.com/technology/article/2010-01/mit-space-telescope-could-find-thousands-exoplanets-just-two-years

the observatory it's not totally dead yet

Borislav wrote:

In general, it remains to determine the nature of only three systems (among the first four dozen) - WASP-20, WASP-23 and WASP-34. Although it is possible they can actually be brown dwarfs.

Now it remains to find a mass of WASP-20b. (V=10.7, T=2.4 days)

WASP-41b: A transiting hot Jupiter planet orbiting a magnetically-active G8V star
http://arxiv.org/abs/1012.2977

Quote :

We report the discovery of a transiting planet with an orbital period of 3.05d orbiting the star TYC 7247-587-1. The star, WASP-41, is a moderately bright G8V star (V=11.6) with a metallicity close to solar ([Fe/H]=-0.08+-0.09). The star shows evidence of moderate chromospheric activity, both from emission in the cores of the CaII H and K lines and photometric variability with a period of 18.3d and an amplitude of about 1%. The rotation period of the star implies a gyrochronological age for WASP-41 of 1.8Gyr with an error of about 15%. We have used a combined analysis of the available photometric and spectroscopic data to derive the mass and radius of the planet (0.93+-0.06M_Jup, 1.21+-0.06R_Jup). Further observations of WASP-41 can be used to explore the connections between the properties of hot Jupiter planets and the level of chromospheric activity in their host stars.

WASP-40b: independent discovery of the 0.6-Mjup transiting exoplanet HAT-P-27b
http://arxiv.org/abs/1101.4643

Quote :

From WASP photometry and SOPHIE radial velocities we report the discovery of WASP-40b (= HAT-P-27b), a 0.6-Mjup planet that transits its 12th magnitude host star every 3.04 d. The host star is of late-G or early-K type and likely has an above-Solar metallicity, with [Fe/H] = 0.14 +/- 0.11. The planet's mass and radius are typical of the known hot Jupiters, thus adding another system to the apparent pileup of transiting planets with periods near 3 to 4 d. Our parameters match those of the recent HATnet announcement of the same planet, thus giving confidence in the techniques used. We report a possible indication of stellar activity in the host star.

two new planets on EPE:

WASP-35b http://exoplanet.eu/star.php?st=WASP-35

WASP-39 http://exoplanet.eu/star.php?st=WASP-39

no preprint yet

Wasp 39b up herehttp://arxiv.org/pdf/1102.1375

I wonder why so much time for WASP-36. It has been announced in July 2010!

High-precision photometry of WASP-12 b transits

Quote :

The transiting extrasolar planet WASP-12 b was found to be one of the most intensely irradiated exoplanets. It is unexpectedly bloated and is losing mass that may accrete into the host star. Our aim was to refine the parameters of this intriguing system and search for signs of transit timing variations. We gathered high-precision light curves for two transits of WASP-12 b. Assuming various limb-darkening laws, we generated best-fitting models and redetermined parameters of the system. Error estimates were derived by the prayer bead method and Monte Carlo simulations. System parameters obtained by us are found to agree with previous studies within one sigma. Use of the non-linear limb-darkening laws results in the best-fitting models. With two new mid-transit times, the ephemeris was refined to BJD(TDB)=(2454508.97682 +/- 0.00020) + (1.09142245 +/- 0.00000033) E. Interestingly, indications of transit timing variation are detected at the level of 3.4 sigma. This signal can be induced by an additional planet in the system. Simplified numerical simulations shows that a perturber could be a terrestrial-type planet if both planets are in a low-order orbital resonance. However, we emphasise that further observations are needed to confirm variation and to constrain properties of the perturber.

WASP-23 b paper.
http://arxiv.org/abs/1103.2603

Notable for discussion of degeneracies between the projected stellar rotation velocity and the projected spin-orbit angle. Wonder how many of the rest of the transiting planets sample may be similarly affected.

Starspots and spin-orbit alignment in the WASP-4 exoplanetary system
http://arxiv.org/abs/1103.4859

They observed the planet transit a starspot on two consecutive orbits, allowing for better constraints on the spin-orbit angle than was given by the Rossiter-McLaughlin effect observations due to it's low impact parameter.

A ground-based Ks-band detection of the thermal emission from the transiting exoplanet WASP-4b
http://arxiv.org/abs/1104.0041

Quote :

Secondary eclipses are a powerful tool to measure directly the thermal emission from extrasolar planets, and to constrain their type and physical parameters. We started a project to obtain reliable broad-band measurements of the thermal emission of transiting exoplanets. Ground-based high-cadence near-infrared relative photometry was used to obtain sub-millimagnitude precision light curve of a secondary eclipse of WASP-4b -- a 1.12 M_J hot Jupiter on a 1.34 day orbit around G7V star. The data show a clear ~10-\sigma detection of the planet's thermal emission at 2.2 \mu m. The calculated thermal emission corresponds to a fractional eclipse depth of 0.185^{+0.014}_{-0.013}%, with a related brightness temperature in Ks of T_B = 1995 \pm 40 K, centered at T_C = 2455102.61162^{+0.00071}_{-0.00077} HJD. We could set a limit on the eccentricity of e cos \omega=0.0027 \pm 0.0018, compatible with a near-circular orbit. The calculated brightness temperature, as well as the specific models suggest a highly inefficient redistribution of heat from the day-side to the night-side of the planet, and a consequent emission mainly from the day-side. The high-cadence ground-based technique is capable of detecting the faint signal of the secondary eclipse of extrasolar planets, making it a valuable complement to space-based mid-IR observations.