Gliese 588

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Gliese 588
Lupus constellation map.svg
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Gliese 588     
Location of Gliese 588 in the constellation Lupus

Observation data
Epoch J2000       Equinox J2000
Constellation Lupus
Right ascension 15h 32m 12.93231s [1]
Declination −41° 16′ 32.1304″ [1]
Apparent magnitude  (V)9.311 [2]
Characteristics
Spectral type M2.5V [2]
U−B color index +1.14 [3]
B−V color index +1.51 [3]
Astrometry
Radial velocity (Rv)21.06±0.12 [1] km/s
Proper motion (μ)RA: -1176.447 mas/yr [1]
Dec.: -1030.970 mas/yr [1]
Parallax (π)168.9965±0.0270  mas [1]
Distance 19.300 ± 0.003  ly
(5.9173 ± 0.0009  pc)
Absolute magnitude  (MV)10.44 [4]
Details [5]
Mass 0.43±0.05  M☉
Radius 0.42±0.03  R☉
Surface gravity (log g)4.82±0.08  cgs
Temperature 3555±41  K
Metallicity [Fe/H]0.06±0.08  dex
Rotation 61.3±6.5 d [6]
Other designations
CD−40 9712, GJ 588, HIP 76074, LHS 397, LTT 6210, TYC 7844-1976-1, 2MASS J15321302-4116314 [2]
Database references
SIMBAD data

Gliese 588 is a nearby red dwarf star of spectral type M2.5, located in the constellation Lupus at 19.30 light-years from Earth. [1] It emits a very stable light flux, with no detectable pulsations. [5]

Contents

History of observations

According to Luyten's (1979) (catalogue LHS, as well as NLTT), this object was discovered by Innes. [7] [8] In 1903–1927 Innes was the director of the Union Observatory (UO), South Africa.

However, in the Ci 20 catalogue (see number 934) this star was designated as "CD -40 7021", not "UO". [9] This may indicate that GJ 588 was first catalogued earlier, in the Cordoba Durchmusterung by John M. Thome in 1894. [10] [11] Note: the real CD designation of Gliese 588 is "CD-40 9712", [12] not "CD -40 7021": [9] GJ 588 has a RA of 15 hours, but the real CD -40 7021 has a RA of 11 hours. [13] [10]

Search for planets

In 2019, two planet candidates detected by radial velocity around Gliese 588 were reported in a preprint, among 118 planets around M dwarf stars. These would have minimum masses about 2.4 and 10.3 times that of Earth, and orbit with periods of 5.8 and 206 days. [14] A 2024 study did not find evidence for planets around this star; radial velocity signals with different periods were detected and attributed to intrinsic stellar variability. [15]

References

  1. 1 2 3 4 5 6 7 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 3 "GJ 588". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 25 December 2016.
  3. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  4. ↑ "The One Hundred Nearest Star Systems". 2012. Archived from the original on 26 March 2012. Retrieved 25 December 2016.
  5. 1 2 Berdiñas, Z. M.; Rodríguez-López, C.; Amado, P. J.; Anglada-Escudé, G.; Barnes, J. R.; MacDonald, J.; Zechmeister, M.; Sarmiento, L. F. (2017), "High-cadence spectroscopy of M-dwarfs – II. Searching for stellar pulsations with HARPS", Monthly Notices of the Royal Astronomical Society, 469 (4): 4268–4282, arXiv: 1705.04690 , doi: 10.1093/mnras/stx1140
  6. ↑ Suárez Mascareño, A.; Rebolo, R.; González Hernández, J. I.; Esposito, M. (2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society, 452 (3): 2745–2756, arXiv: 1506.08039 , Bibcode:2015MNRAS.452.2745S, doi: 10.1093/mnras/stv1441
  7. ↑ Luyten, Willem Jacob (1979). "LHS 397". LHS Catalogue, 2nd Edition. Archived from the original on 4 March 2016. Retrieved 15 October 2015.
  8. ↑ Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amy K.; Burgasser, Adam J.; Tinney, Chris G.; Parker, Stephen; Salter, Graeme (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal . 753 (2): 156. arXiv: 1205.2122 . Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. S2CID   119279752.
  9. 1 2 Porter, J. G.; Yowell, E. J.; Smith, E. S. (1930). "A catalogue of 1474 stars with proper motion exceeding four-tenths year". Publications of the Cincinnati Observatory. 20: 1–32. Bibcode:1930PCinO..20....1P. Page 21 (Ci 20 934). Archived 20 January 2015 at the Wayback Machine
  10. 1 2 Thome, J. M. (1894). "Cordoba Durchmusterung declination -32 to -42". Resultados del Observatorio Nacional Argentino. 17: 1–538. Bibcode:1894RNAO...17....1T. Page 468 (CD -40 9712) Archived 20 January 2015 at the Wayback Machine ; page 459 (CD -40 7021) Archived 20 January 2015 at the Wayback Machine
  11. ↑ Dictionary of Nomenclature of Celestial Objects. CD entry Archived 25 September 2015 at the Wayback Machine . SIMBAD . Centre de Données astronomiques de Strasbourg.
  12. ↑ Luyten, Willem Jacob (1979). "NLTT 40449". NLTT Catalogue. Archived from the original on 4 March 2016. Retrieved 15 October 2015.
  13. ↑ Thome, John Macon (1892–1932). "CD -40 7021". Cordoba Durchmusterung. Archived from the original on 4 March 2016. Retrieved 15 October 2015.
  14. ↑ Barnes, J. R.; Kiraga, M.; Diaz, M.; Berdiñas, Z.; Jenkins, J. S.; Keiser, S.; Thompson, I.; Crane, J. D.; Shectman, S. A. (11 June 2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv: 1906.04644 [astro-ph.EP].
  15. ↑ Mignon, L.; Delfosse, X.; et al. (September 2024). "Radial velocity homogeneous analysis of M dwarfs observed with HARPS". Astronomy & Astrophysics . 689: A32. arXiv: 2502.06513 . doi: 10.1051/0004-6361/202346570 .
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