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WASP-121 / Dilmun
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Puppis
Right ascension	07h 10m 24.06046s
Declination	−39° 05′ 50.5712″
Apparent magnitude (V)	10.4
Characteristics
Spectral type	F6V
Apparent magnitude (B)	11.00
Apparent magnitude (V)	10.51
Apparent magnitude (J)	9.625
Apparent magnitude (H)	9.439
Apparent magnitude (K)	9.374
Astrometry
Radial velocity (Rv)	38.25±0.22 km/s
Proper motion (μ)	RA: −3.735 mas/yr ; Dec.: 25.663 mas/yr
Parallax (π)	3.7996 ± 0.0104 mas
Distance	858 ± 2 ly ; (263.2 ± 0.7 pc)
Details
Mass	1.330±0.019 M☉
Radius	1.461±0.015 R☉
Surface gravity (log g)	4.251±0.003 cgs
Temperature	6,628±66 K
Metallicity [Fe/H]	+0.17±0.05 dex
Rotational velocity (v sin i)	11.90±0.31 km/s
Age	1.11±0.14 Gyr
Other designations
	Dilmun, CD−38 3220, TOI-495, WASP-121, TYC 7630-352-1, 2MASS J07102406-3905506
Database references
SIMBAD	data

WASP-121, also known as CD-38 3220 and formally named Dilmun,^[8] is a magnitude 10.4 star located approximately 858 light-years (263 parsecs) away in the constellation Puppis.^[1] WASP-121 has a mass and radius similar to the Sun's. It hosts one known exoplanet.

The star, although metal-rich in terms of overall contents of heavy elements, is depleted of carbon. The carbon to oxygen molar ratio of 0.23±0.05 for WASP-121 is well below the solar ratio of 0.55.^[9]

Nomenclature

The designation WASP-121 indicates that this was the 121st star found to have a planet by the Wide Angle Search for Planets.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project.^[10] The approved names, proposed by a team from Bahrain, were announced in June 2023. WASP-121 is named Dilmun after the ancient civilization, and its planet is named Tylos after the ancient Greek name for Bahrain.^[11]

Planetary system

In 2015, the exoplanet WASP-121b was discovered orbiting WASP-121 by the transit method.^[3]^[12] WASP-121b is a hot Jupiter with a mass about 1.18 times that of Jupiter and a radius about 1.81 times that of Jupiter.^[4]^[13] The exoplanet orbits WASP-121, its host star, every 1.27 days.^[4]^[13] Hot water molecules have been found in the stratosphere of WASP-121b (i.e., the atmospheric layer in which temperatures increase as the altitude increases).^[3]^[13]^[14]^[15]

The WASP-121 planetary system^[6]
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
b / Tylos	1.170±0.043 $M$ _J	0.02571±0.00010	1.275^[3]	0.0^[3]	87.6^[3]°	1.742±0.006 $R$ _J

Gallery

WASP-121b – computer-simulated views (August 2018)
An artist's impression of a hot Jupiter planet

References

^ ^a ^b Staff. "Finding the constellation which contains given sky coordinates". djm.cc. Retrieved 3 August 2017.
^ ^a ^b ^c ^d ^e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ ^a ^b ^c ^d ^e ^f Staff (2015). "Planet WASP-121 b". Extrasolar Planets Encyclopaedia. Retrieved 3 August 2017.
^ ^a ^b ^c Staff (2017). "WASP Planets". wasp-planets.net. Retrieved 3 August 2017.
^ ^a ^b ^c ^d ^e ^f "WASP-121". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 3 August 2017.
^ ^a ^b Sing, David K.; Evans-Soma, Thomas M.; Rustamkulov, Zafar; Lothringer, Joshua D.; Mayne, Nathan J.; Schlaufman, Kevin C. (November 2024). "An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve". The Astronomical Journal. 168 (6): 231. doi:10.3847/1538-3881/ad7fe7. ISSN 1538-3881.
^ Borsa, F.; Allart, R.; Casasayas-Barris, N.; Tabernero, H.; Zapatero Osorio, M. R.; Cristiani, S.; Pepe, F.; Rebolo, R.; Santos, N. C.; Adibekyan, V.; Bourrier, V.; Demangeon, O. D. S.; Ehrenreich, D.; Pallé, E.; Sousa, S.; Lillo-Box, J.; Lovis, C.; Micela, G.; Oshagh, M.; Poretti, E.; Sozzetti, A.; Allende Prieto, C.; Alibert, Y.; Amate, M.; Benz, W.; Bouchy, F.; Cabral, A.; Dekker, H.; D'Odorico, V.; et al. (2021), "Atmospheric Rossiter–Mc Laughlin effect and transmission spectroscopy of WASP-121b with ESPRESSO", Astronomy & Astrophysics, 645: A24, arXiv:2011.01245, Bibcode:2021A&A...645A..24B, doi:10.1051/0004-6361/202039344, S2CID 226237425
^ "2022 Approved Names". NameExoworlds. Retrieved 22 July 2024.
^ Polanski, Alex S.; Crossfield, Ian J. M.; Howard, Andrew W.; Isaacson, Howard; Rice, Malena (2022), "Chemical Abundances for 25 JWST Exoplanet Host Stars with KeckSpec", Research Notes of the American Astronomical Society, 6 (8): 155, arXiv:2207.13662, Bibcode:2022RNAAS...6..155P, doi:10.3847/2515-5172/ac8676
^ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
^ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
^ Delrez, L.; Santerne, A.; Almenara, J.-M.; Anderson, D. R.; Collier-Cameron, A.; Díaz, R. F.; Gillon, M.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Neveu-Vanmalle, M.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Smith, A. M. S.; Triaud, A. H. M. J.; Udry, S.; Van Grootel, V.; West, R. G. (2015), "WASP-121 b: A hot Jupiter close to tidal disruption transiting an active F star", Monthly Notices of the Royal Astronomical Society, 458 (4): 4025–4043, arXiv:1506.02471, doi:10.1093/mnras/stw522
^ ^a ^b ^c Landau, Elizabeth; Villard, Ray (2 August 2017). "Hubble Detects Exoplanet with Glowing Water Atmosphere". NASA. Retrieved 2 August 2017.
^ Evans, Thomas M.; et al. (2 August 2017). "An ultrahot gas-giant exoplanet with a stratosphere". Nature. 548 (7665): 58–61. arXiv:1708.01076. Bibcode:2017Natur.548...58E. doi:10.1038/nature23266. PMID 28770846. S2CID 205258293.
^ Mikal-Evans, Thomas; Sing, David K.; Kataria, Tiffany; Wakeford, Hannah R.; Mayne, Nathan J.; Lewis, Nikole K.; Barstow, Joanna K.; Spake, Jessica J. (2020). "Confirmation of water emission in the dayside spectrum of the ultrahot Jupiter WASP-121b". Monthly Notices of the Royal Astronomical Society. 496 (2): 1638–1644. arXiv:2005.09631. doi:10.1093/mnras/staa1628. S2CID 218684532.