HATSouth Results

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Re: HATSouth Results

Post by Sirius_Alpha on 12th December 2017, 9:26 pm

HATS-50b through HATS-53b: four transiting hot Jupiters orbiting G-type stars discovered by the HATSouth survey
https://arxiv.org/abs/1712.04324

We report the discovery of four close-in transiting exoplanets, HATS-50 through HATS-53, discovered using the HATSouth three-continent network of homogeneous and automated telescopes. These new exoplanets belong to the class of hot Jupiters and orbit G-type dwarf stars, with brightness in the range V=12.5-14.0 mag. While HATS-53 has many physical characteristics similar to the Sun, the other three stars appear to be metal rich, larger and more massive. Three of the new exoplanets, namely HATS-50, HATS-51 and HATS-53, have low density and similar orbital period. Instead, HATS-52 is more dense and has a shorter orbital period. It also receives an intensive radiation from its parent star and, consequently, presents a high equilibrium temperature. HATS-50 shows a marginal additional transit feature consistent with an ultra-short period hot super Neptune, which will be able to be confirmed with TESS photometry.

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Re: HATSouth Results

Post by Sirius_Alpha on 5th April 2018, 8:48 pm

HATS-39b, HATS-40b, HATS-41b, and HATS-42b: Three Inflated Hot Jupiters and a Super-Jupiter Transiting F Stars
https://arxiv.org/abs/1804.01623

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Re: HATSouth Results

Post by Sirius_Alpha on 15th May 2018, 9:41 pm

HATS-59b,c: A Transiting Hot Jupiter and a Cold Massive Giant Planet Around a Sun-Like Star
https://arxiv.org/abs/1805.05925

We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an eccentric orbit with e=0.1290.049, orbiting a V=13.9510.030 mag solar-like star (M∗=1.0380.039M⊙, and R∗=1.0360.067R⊙) with a period of 5.4160770.000017 days. The outer companion, HATS-59c is on a circular orbit with msini=12.81.1MJ, and a period of 142214 days. The inner planet has a mass of 0.8060.069MJ and a radius of 1.1260.077MJ, yielding a density of 0.700.16gcm−3. Unlike most of the planetary systems that include only a single hot Jupiter, HATS-59b,c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.

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Re: HATSouth Results

Post by Lazarus on 16th May 2018, 5:47 pm

Interesting that HATS-59c is on a near-circular orbit. Not sure how well that fits with the idea that it scattered HATS-59b into the inner system, although the mass ratio is quite high.
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Re: HATSouth Results

Post by Sirius_Alpha on 4th September 2018, 10:09 pm

HATS-60b - HATS-69b: Ten Transiting Planets From HATSouth
https://arxiv.org/abs/1809.01048

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Re: HATSouth Results

Post by Sirius_Alpha on 18th November 2018, 9:34 pm

HATS-70b: A 13 Mjup brown dwarf transiting an A star
https://arxiv.org/abs/1811.06925


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Re: HATSouth Results

Post by Sirius_Alpha on 19th December 2018, 9:35 pm

HATS-54b-HATS-58Ab: five new transiting hot Jupiters including one with a possible temperate companion
https://arxiv.org/abs/1812.07668

We report the discovery by the HATSouth project of 5 new transiting hot Jupiters (HATS-54b through HATS-58Ab). HATS-54b, HATS-55b and HATS-58Ab are prototypical short period (P=2.5−4.2 days, Rp∼1.1−1.2 RJ) hot-Jupiters that span effective temperatures from 1350 K to 1750 K, putting them in the proposed region of maximum radius inflation efficiency. The HATS-58 system is composed of two stars, HATS-58A and HATS-58B, which are detected thanks to Gaia DR2 data and which we account for in the joint modelling of the available data --- with this, we are led to conclude that the hot jupiter orbits the brighter HATS-58A star. HATS-57b is a short-period (2.35-day) massive (3.15 MJ) 1.14 RJ, dense (2.650.21 g cm−3) hot-Jupiter, orbiting a very active star (2% peak-to-peak flux variability). Finally, HATS-56b is a short period (4.32-day) highly inflated hot-Jupiter (1.7 RJ, 0.6 MJ), which is an excellent target for future atmospheric follow-up, especially considering the relatively bright nature (V=11.6) of its F dwarf host star. This latter exoplanet has another very interesting feature: the radial velocities show a significant quadratic trend. If we interpret this quadratic trend as arising from the pull of an additional planet in the system, we obtain a period of Pc=815+253−143 days for the possible planet HATS-56c, and a minimum mass of Mcsinic=5.110.94 MJ. The candidate planet HATS-56c would have a zero-albedo equilibrium temperature of Teq=33250 K, and thus would be orbiting close to the habitable zone of HATS-56. Further radial-velocity follow-up, especially over the next two years, is needed to confirm the nature of HATS-56c.

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Re: HATSouth Results

Post by Sirius_Alpha on 27th December 2018, 12:58 pm

HATS-71b: A giant planet transiting an M3 dwarf star in TESS Sector 1
https://arxiv.org/abs/1812.09406

We report the discovery of HATS-71b, a transiting gas giant planet on a P = 3.7955 day orbit around a G = 15.35 mag M3 dwarf star. HATS-71 is the coolest M dwarf star known to host a hot Jupiter. The loss of light during transits is 4.7%, more than any other confirmed transiting planet system. The planet was identified as a candidate by the ground-based HATSouth transit survey. It was confirmed using ground-based photometry, spectroscopy, and imaging, as well as space-based photometry from the NASA TESS mission (TIC 234523599). Combining all of these data, and utilizing Gaia DR2, we find that the planet has a radius of 1.0800.016RJ and mass of 0.450.24MJ (95% confidence upper limit of 0.81MJ ), while the star has a mass of 0.5690.0420.069M⊙ and a radius of 0.51610.00530.0099R⊙. The Gaia DR2 data show that HATS-71 lies near the binary main sequence in the Hertzsprung-Russell diagram, suggesting that there may be an unresolved stellar binary companion. All of the available data is well fitted by a model in which there is a secondary star of mass 0.24M⊙, although we caution that at present there is no direct spectroscopic or imaging evidence for such a companion. Even if there does exist such a stellar companion, the radius and mass of the planet would be only marginally different from the values we have calculated under the assumption that the star is single.

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Re: HATSouth Results

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