NGC 2423-3

NGC 2423-3
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension 07h 37m 09.23325s[1]
Declination −13° 54′ 23.9569″[1]
Apparent magnitude (V) 10.04[2]
Characteristics
Spectral type G5IV-V/K2III[2]
Astrometry
Radial velocity (Rv)18.23±0.15[1] km/s
Proper motion (μ) RA: -0.601 mas/yr[1]
Dec.: -3.625 mas/yr[1]
Parallax (π)1.0746 ± 0.0140 mas[1]
Distance3,040 ± 40 ly
(930 ± 10 pc)
Absolute magnitude (MV)0.03[citation needed]
Details[3]
Mass2.03±0.14 M☉
Radius17.71±1.04 R☉
Luminosity131.8 L☉
Surface gravity (log g)2.23±0.04 cgs
Temperature4534±12 K
Metallicity [Fe/H]−0.08±0.01 dex
Rotational velocity (v sin i)2.19 km/s
Age1.02 Gyr
Other designations
BD−13 2130, TIC 288474555, TYC 5409-2156-1, GSC 05409-02156, 2MASS J07370922-1354239, NGC 2423 3, NGC 2423 MMU 3, NGC 2423 SN 4[2]
Database references
SIMBADdata

NGC 2423-3 is a red giant star approximately 3,040 light-years away in the constellation of Puppis. The star is part of the NGC 2423 open cluster (hence the name NGC 2423-3). The star has an apparent magnitude of 10 and an absolute magnitude of zero, with a mass of 2.4 times the Sun. In 2007, it was proposed that an exoplanet orbits the star, but this is now doubtful.

Planetary system

NGC 2423-3 b is an exoplanet 10.6 times more massive than Jupiter. Only the minimum mass is known since the orbital inclination is not known, so it is likely to be a brown dwarf instead. The planet orbits at 2.1 AU, taking 1.956 years to orbit eccentrically around the star. Its eccentricity is about the same as Mercury, but less than Pluto. The planet has a semi-amplitude of 71.5 m/s.[4]

This planet was discovered by Christophe Lovis and Michel Mayor in July 2007 by the radial velocity method.[4] Lovis had also found three Neptune-mass planets orbiting HD 69830 in May 2006, also in Puppis.

However, a 2018 study with the same C. Lovis as an author found evidence that the radial velocity signal corresponding to the proposed planetary companion could be caused by stellar activity or stellar pulsations, and so the planet may not exist.[5] Another study by the same team in 2023 confirms evidence for a stellar origin of the signal.[3]

The NGC 2423-3 planetary system[4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b (dubious) >10.6 MJ 2.10 714.3 ± 5.3 0.21 ± 0.07 — —

See also

References

  1. ^ 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.
  2. ^ a b c "BD-13 2130". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 November 2023.
  3. ^ a b Delgado Mena, E.; Gomes da Silva, J.; et al. (November 2023). "Planets around evolved intermediate-mass stars. III. Planet candidates and long-term activity signals in six open clusters". Astronomy & Astrophysics. 679: A94. arXiv:2309.13589. Bibcode:2023A&A...679A..94D. doi:10.1051/0004-6361/202346890.
  4. ^ a b c C. Lovis & M. Mayor (2007). "Planets around evolved intermediate-mass stars I. Two substellar companions in the open clusters NGC 2423 and NGC 4349". Astronomy and Astrophysics. 472 (2): 657–664. arXiv:0706.2174. Bibcode:2007A&A...472..657L. doi:10.1051/0004-6361:20077375. S2CID 15173677.
  5. ^ Delgado Mena, E.; Lovis, C.; et al. (November 2018). "Planets around evolved intermediate-mass stars. II. Are there really planets around IC 4651 No. 9122, NGC 2423 No. 3, and NGC 4349 No. 127?". Astronomy & Astrophysics. 619: A2. arXiv:1807.09608. Bibcode:2018A&A...619A...2D. doi:10.1051/0004-6361/201833152. S2CID 119483881.


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