NGC 4349-127
Observation data
Epoch J2000      Equinox J2000
Constellation Crux
Right ascension 12h 24m 35.47095s[1]
Declination −61° 49′ 11.8614″[1]
Apparent magnitude (V) 10.82[2]
Characteristics
Spectral type M II
Astrometry
Radial velocity (Rv)−11.20±0.21[1] km/s
Proper motion (μ) RA: −7.848(12) mas/yr[1]
Dec.: −0.207(13) mas/yr[1]
Parallax (π)0.5348 ± 0.0143 mas[1]
Distance6,100 ± 200 ly
(1,870 ± 50 pc)
Absolute magnitude (MV)−4.3
Details[3]
Mass3.01±0.24 M☉
Radius37.97±2.56 R☉
Luminosity575.4 L☉
Surface gravity (log g)1.78±0.05 cgs
Temperature4417±12 K
Metallicity [Fe/H]−0.17±0.02 dex
Rotational velocity (v sin i)4.81 km/s
Age0.32 Gyr
Other designations
TIC 450417907, TYC 8975-2606-1, GSC 08975-02606, 2MASS J12243547-6149120, NGC 4349 127, NGC 4349 MMU 127[2]
Database references
SIMBADdata

NGC 4349-127 is a probable red giant star approximately 6,100 light-years away in the constellation of Crux. It is a member of the open cluster NGC 4349 (hence the name NGC 4349-127).[4] Its mass is estimated at 3.9 times Solar, and its age is about 200 million years.[4]

In 2007, this star was found to have a substellar companion. NGC 4349-127 b is a brown dwarf (based on its mass) with nearly 20 times the mass of Jupiter. Within an eccentricity of about 0.19, its orbit is moderately elliptical, about the same as Mercury in the Solar System. It orbits its host star at a distance of 2.38 AU in a period of 677.8 days. This object was discovered by Christophe Lovis and Michel Mayor of the Geneva Observatory using the radial velocity technique.[4]

However, a 2018 study with the same C. Lovis as an author found that the radial velocity signal corresponding to the proposed substellar companion was most likely caused by stellar activity, and thus the companion does not exist.[5] Another study by the same team in 2023 also confirms the stellar origin of the signal.[3]

See also

References

  1. 1 2 3 4 5 6 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. 1 2 "NGC 4349 127". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 November 2023.
  3. 1 2 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. 1 2 3 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 & 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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