The TESS-Keck Survey or TKS is an exoplanet search project that uses the Keck I and the Automated Planet Finder (APF) to conduct ground-based follow-up of planet candidates discovered by the Transiting Exoplanet Survey Satellite. [1] The TKS aims to measure the mass for about 100 exoplanets [2] and has been awarded some of the largest time allocations in the histories of Keck I and APF. [1] The program has four main science themes: [2]
Name | Class | Radius (R🜨) | Mass (ME) | Bulk density (g/cm3) | Orbital period (days) | Discovery year | Note | Reference |
---|---|---|---|---|---|---|---|---|
HD 332231 b | warm sub-Saturn | 9.744 | 76.32 | 0.464 | 18.71 | 2020 | [3] | |
TOI-561 b | super-earth | 1.45 | 3.2 | 5.5 | 0.44 | 2021 | old metal-poor host star | [4] |
TOI-561 c | sub-Neptune | 2.90 | 6.5 | 1.6 | 10.8 | 2021 | old metal-poor host star | [4] |
TOI-561 d | sub-Neptune | 2.32 | 2.4 | 1.3 | 16.4 | 2021 | metal-poor host star | [4] |
HD 63935 b | sub-Neptune | 2.99 | 10.8 | 2.2 | 9.06 | 2021 | [5] | |
HD 63935 c | sub-Neptune | 2.90 | 11.1 | 2.5 | 21.40 | 2021 | [5] | |
HIP-97166 b | sub-Neptune | 2.7 | 20 | 5.3 | 10.3 | 2021 | eccentric orbit | [6] |
HIP-97166 c | sub-Neptune | 10 | 16.8 | 2021 | eccentric orbit | [6] | ||
TOI-2180 b | giant planet | 11.3 | 890.4 | 3.32 | 260.8 | 2022 | originally found by citizen scientists of Planet Hunters, planet with eccentric orbit | [7] |
HD 191939 e | warm Saturn | 108 | 101.5 | 2022 | study also announced the mass of the other planets | [8] | ||
HD 191939 f | giant planet | ≥630 | 1700-7200 | 2022 | candidate | [8] | ||
TOI-1444 b | super-earth | 1.4 | 3.87 | 0.47 | 2021 | [9] | ||
TOI-1444 c | 11.8 | 16 | 2021 | candidate | [10] | |||
TOI-1246 e | >25.6 | 93.8 | 2022 | candidate, study also announced the mass of the other planets | [11] | |||
TOI-1272 b | hot Neptune | 4.1 | 25 | 1.9 | 3.3 | 2022 | eccentric orbit | [12] |
TOI-1272 c | 27 | 8.7 | 2022 | [13] | ||||
TOI-1669 c | giant planet | 191 | 501 | 2022 | planet b is a close-in small planet (about 4 ME) | [14] | ||
TOI-1694 c | giant planet | 295 | 393 | 2022 | planet b is a close-in small planet (31 ME) | [14] | ||
HIP 8152 b (TOI-266) | sub-Neptune | 2.6 | 7.8 | 2.5 | 10.75 | 2023 | [15] | |
HIP 8152 c | sub-Neptune | 2.5 | 9.4 | 3.4 | 19.61 | 2023 | [15] | |
HD 42813 b (TOI-469) | sub-Neptune | 3.4 | 5.8 | 0.8 | 13.63 | 2023 | star is metal-rich, planet has relative low density | [15] |
HD 25463 b (TOI-554) | sub-Neptune | 2.6 | 8.5 | 2.6 | 7.05 | 2023 | [15] | |
HD 25463 c | super-Earth | 1.5 | <4.1 | <7.1 | 3.04 | 2023 | [15] | |
TOI-669 b | hot sub-Neptune | 2.6 | 9.8 | 3.0 | 3.95 | 2023 | [15] | |
HD 135694 b (TOI-1247) | warm sub-Neptune | 2.51 | 5.7 | 2.0 | 15.92 | 2023 | [15] | |
HD 6061 b (TOI-1473) | hot sub-Neptune | 2.45 | 10.8 | 4.0 | 5.25 | 2023 | [15] | |
TOI-1736 b | sub-Neptune | 3.1 | 11.9 | 2.3 | 7.07 | 2023 | star is a subgiant | [15] |
TOI-1736 c | temperature super-Jovian | >2477 | 571.3 | 2023 | not transiting, in a moderately eccentric orbit | [15] | ||
TOI-1386 b | warm sub-Saturn | 6.05 | 47 | 1.16 | 25.84 | 2024 | orbits a solar analogue | [16] |
TOI-1386 c | >98 | 227.6 | 2024 | not transiting | [16] | |||
TOI-1347 b | ultra-short period planet | 1.8 | 11.1 | 9.9 | 0.85 | 2024 | possible high molecular weight atmosphere | [17] |
TOI-1347 c | 1.6 | <6.4 | <4.1 | 4.84 | 2024 | [17] | ||
TOI-329 b | Neptune size | 4.72 | 40.8 | 2.13 | 5.70 | 2024 | old subgiant host star; moderate eccentric orbit e=0.39 | [18] |
HD 39688 b (TOI-480) | Earth-density | 2.69 | 15.7 | 4.42 | 6.86 | 2024 | [18] | |
TOI-603 b | 7.93 | 47.5 | 0.52 | 16.17 | 2024 | subgiant host star | [18] | |
TOI-1199 b | giant planet | 10.60 | 69.4 | 0.32 | 3.67 | 2024 | [18] | |
TOI-1294 b | Saturn-sized | 9.19 | 62.2 | 0.44 | 3.91 | 2024 | massive metal-rich host star | [18] |
TOI-1294 c | 148.3 | 160.1 | 2024 | not transiting | [18] | |||
TOI-1439 b | Neptune-sized | 4.15 | 38.4 | 2.94 | 27.64 | 2024 | metal-rich subgiant host star | [18] |
TOI-1605 b | Jupiter-sized | 10.34 | 221.3 | 8.70 | 2024 | solar-like metallicity host star; eccentric orbit e=0.28 | [18] | |
TOI-1828 b | hot Jupiter | 8.62 | 58.5 | 0.50 | 9.09 | 2024 | subgiant host star; eccentric orbit e=0.31 | [18] |
HD 148193 b (TOI-1836) | 8.38 | 28.4 | 0.27 | 20.38 | 2024 | young and hot subgiant host star | [18] | |
TOI-1885 b | giant planet | 13.66 | 516.4 | 1.12 | 6.54 | 2024 | young and hot host star | [18] |
HD 83342 b (TOI-1898) | warm Jupiter | 9.74 | 127.5 | 0.76 | 45.52 | 2024 | CTOI of Planet Hunters: TESS; highly eccentric orbit e=0.48 | [19] [18] |
TOI-2019 b | 5.66 | 34.6 | 1.05 | 15.34 | 2024 | cool metal-rich subgiant host star | [18] | |
TOI-1736 c | 2477 | 571.3 | 2024 | eccentric orbit e=0.37 | [18] | |||
TOI-1751 b | sub-Neptune | 2.77 | 14.5 | 3.6 | 37.47 | 2024 | slightly evolved solar-type metal-poor star | [20] |
Follow-up works by TKS studied the already discovered planets TOI-1726 c [21] and WASP-107b. [22]
14 Herculis or 14 Her is a K-type main-sequence star 58.4 light-years away in the constellation Hercules. It is also known as HD 145675. Because of its apparent magnitude, of 6.61 the star can be very faintly seen with the naked eye. As of 2021, 14 Herculis is known to host two exoplanets in orbit around the star.
Lambda Serpentis, Latinized from λ Serpentis, is a star in the constellation Serpens, in its head. It has an apparent visual magnitude of 4.43, making it visible to the naked eye. Based upon parallax measurements, this star lies at a distance of about 38.9 light-years from Earth. Lambda Serpentis is moving toward the Solar System with a radial velocity of 66.4 km s−1. In about 166,000 years, this system will make its closest approach of the Sun at a distance of 7.371 ± 0.258 light-years, before moving away thereafter.
An ultra-short period (USP) planet is a type of exoplanet with an orbital period of less than one Earth day. At this short distance, tidal interactions lead to relatively rapid orbital and spin evolution. Therefore when there is a USP planet around a mature main-sequence star it is most likely that the planet has a circular orbit and is tidally locked. There are not many USP planets with sizes exceeding 2 Earth radii. About one out of 200 Sun-like stars has an ultra-short-period planet. There is a strong dependence of the occurrence rate on the mass of the host star. The occurrence rate falls from % for M dwarfs to % for F dwarfs. Mostly the USP planets seem consistent with an Earth-like composition of 70% rock and 30% iron, but K2-229b has a higher density suggesting a more massive iron core. WASP-47e and 55 Cnc e have a lower density and are compatible with pure rock, or a rocky-iron body surrounded by a layer of water.
HD 66428 is a G-type main sequence star located approximately 174 light-years away in the constellation of Monoceros. This star is similar to the Sun with an apparent magnitude of 8.25, an effective temperature of 5705 ± 27 K and a solar luminosity 1.28. Its absolute magnitude is 11.1 while its U-V color index is 0.71. It is considered an inactive star and it is metal-rich . This star has a precise mass of 1.14552 solar masses. This precision comes from the Corot mission that measured asteroseismology.
14 Herculis c or 14 Her c is an exoplanet approximately 58.4 light-years away in the constellation of Hercules. The planet was found orbiting the star 14 Herculis, with a mass that would make the planet a gas giant roughly the same size as Jupiter but much more massive. It was discovered on November 17, 2005 and published on November 2, 2006, although its existence was not confirmed until 2021.
HD 68988 is a star in the northern constellation of Ursa Major. It has been given the proper name Násti, which means star in the Northern Sami language. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. HD 68988 is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.20. The star is located at a distance of 199 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −69 km/s and is predicted to come as close as 78 light-years in 617,000 years.
HD 107148 b is a jovian exoplanet with minimum mass of only 70% that of Saturn. Unlike Saturn, it orbits much closer to the star. The planetary orbit was significantly refined in the 2021.
HD 34445 is a star in the equatorial constellation of Orion. With an apparent visual magnitude of 7.31, it is a 7th magnitude star that is too dim to be readily visible to the naked eye. The system is located at a distance of 150.5 light years from the Sun based on parallax measurements, but is drifting closer with a high radial velocity of −79 km/s. It is expected to draw as close as 57.5 light-years in ~492,000 years.
K2-187, also known as EPIC 212157262, is a Sun-like star in K2 Campaign 5. It is very close in size and temperature to the Sun, and has a system of four confirmed exoplanets ranging between 1.4 R🜨 and 3.2 R🜨. The innermost planet takes just 18 hours to orbit its star, while the outermost planet orbits every 2 weeks.
WASP-107b is a super-Neptune exoplanet that orbits the star WASP-107. It lies 200 light-years away from Earth in the constellation Virgo. Its discovery was announced in 2017 by a team led by D. R. Anderson via the WASP-South.
WASP-75 is a F-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 2.9±0.2 billion years. WASP-75 is similar to the Sun in its concentration of heavy elements.