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WASP-6 is a type-G yellow dwarf star located about 600 light-years away in the Aquarius constellation. Dim at magnitude 12, it is visible through a moderate sized amateur telescope. The star is about 80% of the size and mass of the Sun and it is a little cooler. Starspots in the WASP-6 system helped to refine the measurements of the mass and the radius of the planet WASP-6b.
WASP-56 is a sun-like star of spectral type G6 in the constellation of Coma Berenices. It has an apparent magnitude of 11.48. Observations at the Calar Alto Observatory using the lucky imaging technique detected a candidate companion star located 3.4 arc seconds away, however it is not known if this is an actual binary companion or an optical double.
WASP-21 is a G-type star that is reaching the end of its main sequence lifetime approximately 850 light years from Earth in the constellation of Pegasus that is relatively metal-poor, having 40% of heavy elements compared to the Sun. Kinematically, WASP-21 belongs to the thick disk of the Milky Way.
Qatar 1 is an orange main sequence star in the constellation of Draco.
HAT-P-23 is a G-type main-sequence star about 1200 light-years away. It has a rapid rotation for its advanced age of 4 billion years, and exhibits a strong starspot activity. The star may be in the process of being spun up by the giant planet on close orbit. The star is enriched in heavy elements, having about 140% amount of metals compared to solar abundance.
WASP-50 is a G-type main-sequence star about 610 light-years away. The star is older than Sun and slightly depleted in heavy elements compared to Sun, and have a close to average starspot activity. Despite of advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.
WASP-48 is a subgiant star about 1400 light-years away. The star is likely older than Sun and slightly depleted in heavy elements. It shows an infrared excess noise of unknown origin, yet has no detectable ultraviolet emissions associated with the starspot activity. The discrepancy may be due to large interstellar absorption of light in interstellar medium for WASP-48. The measurements are compounded by the emission from eclipsing contact binary NSVS-3071474 projected on sky plane nearby, although no true stellar companions were detected by survey in 2015.
WASP-35 is a G-type main-sequence star about 660 light-years away. The star age cannot be well constrained, but it is probably older than the Sun. WASP-35 is similar in concentration of heavy elements compared to the Sun.
Qatar-2 is a K-type main-sequence star about 595 light-years away. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.
WASP-78, is a single F-type main-sequence star about 2500 light-years away. It is likely to be younger than the Sun at 3.4+1.5
−0.8 billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.
BD-07 436, also known as WASP-77 since 2012, is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares.
BD+00 316, also known as WASP-71 since 2012, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.
WASP-64 is a single star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. The age of WASP-64 is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.
WASP-67 is a K-type main-sequence star about 620 light-years away. The stars age is poorly constrained, but is likely older than the Sun`s at approximately 8.7+5.5
−8.6 billion years. WASP-67 is slightly depleted in heavy elements, having 85% of the solar abundance of iron.
WASP-55 is a G-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 1.1+0.8
−0.6 billion years. WASP-55 is similar to the Sun in concentration of heavy elements.
WASP-54, also known as BD+00 3088, is a binary star system about 825 light-years away. The primary, WASP-54A, is a F-type main-sequence star, accompanied by the red dwarf WASP-54B on a wide orbit. WASP-54 is depleted in heavy elements, having 55% of the solar abundance of iron. The age of WASP-54 is slightly older than the Sun's at 6.9+1.0
−1.9 billion years.
WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.
WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8 billion years. The star does exhibit starspot activity as is typical for its spectral class.
WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.
WASP-69 is a K-type main-sequence star. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.
References
- 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
- 1 2 3 Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2017), "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics, 602: A107, arXiv: 1704.00373 , doi:10.1051/0004-6361/201629882, S2CID 118923163
- ↑ "WASP-59". SIMBAD . Centre de données astronomiques de Strasbourg.
- ↑ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal, 766: 9, arXiv: 1301.6192 , doi:10.1088/0004-637X/766/1/9, S2CID 118415788
- ↑ Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics, 575: A23, arXiv: 1507.01938 , doi:10.1051/0004-6361/201424091, S2CID 119250579
- 1 2 Hébrard, G.; Collier Cameron, A.; Brown, D. J. A.; Díaz, R. F.; Faedi, F.; Smalley, B.; Anderson, D. R.; Armstrong, D.; Barros, S. C. C.; Bento, J.; Bouchy, F.; Doyle, A. P.; Enoch, B.; Gómez Maqueo Chew, Y.; Hébrard, É. M.; Hellier, C.; Lendl, M.; Lister, T. A.; Maxted, P. F. L.; McCormac, J.; Moutou, C.; Pollacco, D.; Queloz, D.; Santerne, A.; Skillen, I.; Southworth, J.; Tregloan-Reed, J.; Triaud, A. H. M. J.; Udry, S.; et al. (2012), "WASP-52b, WASP-58b, WASP-59b, and WASP-60b: four new transiting close-in giant planets", Astronomy & Astrophysics, 549: A134, arXiv: 1211.0810 , doi:10.1051/0004-6361/201220363, S2CID 54502046
- ↑ Southworth, J.; Mancini, L.; Browne, P.; Burgdorf, M.; Calchi Novati, S.; Dominik, M.; Gerner, T.; Hinse, T. C.; Jorgensen, U. G.; Kains, N.; Ricci, D.; Schafer, S.; Schonebeck, F.; Tregloan-Reed, J.; Alsubai, K. A.; Bozza, V.; Chen, G.; Dodds, P.; Dreizler, S.; Fang, X. -S.; Finet, F.; Gu, S. -H.; Hardis, S.; Harpsoe, K.; Henning, Th.; Hundertmark, M.; Jessen-Hansen, J.; Kerins, E.; Kjeldsen, H.; et al. (2013), High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16, arXiv: 1306.3509 , doi:10.1093/mnras/stt1089, S2CID 53645606
Coordinates: 
23h 18m 29.5475s, +24° 53′ 21.4364″
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