4U 1543-475

Last updated
IL Lupi
ILLupLightCurve.png
Light curves for the 2002 outburst of IL Lupi, adapted from Buxton & Bailyn (2004). [1] The top panel shows the X-ray flux, while the lower three panels show the magnitude change in the visible, and two near-infrared bands.
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Lupus
Right ascension 15h 47m 08.27687s [2]
Declination −47° 40′ 10.2846″ [2]
Apparent magnitude  (V)11.96 [3] (14.6 - 16.7) [4]
Characteristics
Evolutionary stage main sequence [5]
Spectral type A2 V + black hole [6]
Variable type XNG [4]
Astrometry
Proper motion (μ)RA: −7.543 mas/yr [2]
Dec.: −5.356 mas/yr [2]
Parallax (π)0.1909±0.0551  mas [2]
Distance approx. 17,000  ly
(approx. 5,000  pc)
Details
donor star
Mass 2.45±0.15 [7]   M☉
Radius 2.84±0.11 [6]   R☉
Luminosity 48±11 [6]   L☉
Surface gravity (log g)3.82 [8]   cgs
Temperature 9,000±500 [6]   K
Metallicity [Fe/H]−0.11 [9]   dex
black hole
Mass 9.4±2.0 [10]   M☉
Other designations
4U 1543-47, IL Lup, TIC 254732447, 2MASS J15470829-4740103 [11]
Database references
SIMBAD data

4U 1543-475 is a recurrent X-ray transient [12] located in the southern constellation Lupus, the wolf. IL Lupi is its variable star designation. It has an apparent magnitude that fluctuates between 14.6 and 16.7, making it readily visible in large telescopes but not to the naked eye. The object is located relatively far at a distance of approximately 17,000 light years based on Gaia DR3 parallax measurements.

4U 1543-475 was first observed by Uhuru in 1971. [13] In 1976, 4U 1543-475's spectrum was observed. However, its status as a black hole binary had not been confirmed until 1984 by astronomer S. Kiamoto and colleagues. [14] After subsequent observations, it was given the variable star designation IL Lupi in 1995. 4U 1543-475 erupted three times.[ citation needed ]

See also

References

  1. ↑ Buxton, M. M.; Bailyn, C. D. (November 2004). "The 2002 Outburst of the Black Hole X-Ray Binary 4U 1543-47: Optical and Infrared Light Curves". The Astrophysical Journal. 615 (2): 880–886. doi:10.1086/424503 . Retrieved 31 March 2025.
  2. 1 2 3 4 5 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.
  3. ↑ Alfonso-Garzón, J.; Domingo, A.; Mas-Hesse, J. M.; Giménez, A. (26 November 2012). "The first INTEGRAL-OMC catalogue of optically variable sources". Astronomy & Astrophysics. 548: A79. arXiv: 1210.0821 . Bibcode:2012A&A...548A..79A. doi: 10.1051/0004-6361/201220095 . eISSN   1432-0746. ISSN   0004-6361. S2CID   118428054.
  4. 1 2 Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. eISSN   1562-6881. ISSN   1063-7729. S2CID   125853869.
  5. ↑ Kolb, U. (21 June 1998). "Soft X-ray transients in the Hertzsprung gap". Monthly Notices of the Royal Astronomical Society. 297 (2): 419–426. arXiv: astro-ph/9801283 . Bibcode:1998MNRAS.297..419K. doi: 10.1046/j.1365-8711.1998.01489.x . eISSN   1365-2966. ISSN   0035-8711. S2CID   18862109.
  6. 1 2 3 4 Orosz, Jerome A.; Jain, Raj K.; Bailyn, Charles D.; McClintock, Jeffrey E.; Remillard, Ronald A. (20 May 1998). "Orbital Parameters for the Soft X-Ray Transient 4U 1543−47: Evidence for a Black Hole". The Astrophysical Journal. 499 (1): 375–384. arXiv: astro-ph/9712018 . Bibcode:1998ApJ...499..375O. doi: 10.1086/305620 . eISSN   1538-4357. ISSN   0004-637X. S2CID   16991861.
  7. ↑ Ritter, H.; Kolb, U. (26 May 2003). "Catalogue of cataclysmic binaries, low–mass X-ray binaries and related objects (Seventh edition)". Astronomy & Astrophysics. 404 (1): 301–303. arXiv: astro-ph/0301444 . Bibcode:2003A&A...404..301R. doi: 10.1051/0004-6361:20030330 . eISSN   1432-0746. ISSN   0004-6361. S2CID   61117701.
  8. ↑ Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . eISSN   1538-3881. hdl: 1721.1/124721 . S2CID   166227927.
  9. ↑ Anders, F.; et al. (February 2022). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5". Astronomy & Astrophysics. 658: A91. arXiv: 2111.01860 . Bibcode:2022A&A...658A..91A. doi: 10.1051/0004-6361/202142369 . eISSN   1432-0746. ISSN   0004-6361.
  10. ↑ Özel, Feryal; Psaltis, Dimitrios; Narayan, Ramesh; McClintock, Jeffrey E. (2 December 2010). "The Black Hole Mass Distribution in the Galaxy". The Astrophysical Journal. 725 (2): 1918–1927. arXiv: 1006.2834 . Bibcode:2010ApJ...725.1918O. doi: 10.1088/0004-637X/725/2/1918 . eISSN   1538-4357. ISSN   0004-637X. S2CID   46933635.
  11. ↑ "V* IL Lup". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved April 13, 2023.
  12. ↑ Palombara, Nicola La; Mereghetti, Sandro (2 February 2008). "XMM-Newton observation of 4U 1543–475: The X-ray spectrum of a stellar-mass black-hole at low luminosity". Astronomy & Astrophysics . 430 (2005): L53 –L56. arXiv: astro-ph/0412209 . Bibcode:2005A&A...430L..53L. CiteSeerX   10.1.1.316.7094 . doi:10.1051/0004-6361:200400123. S2CID   865125.
  13. ↑ MATiLSKY, T. A.; Giacconi, R.; Gursky, H.; Kellogg, E. M.; Tananbaum, H. D. (15 May 1972). "A New Transient Source Observed by UHURU". The Astrophysical Journal . 174: L53 –L55. Bibcode:1972ApJ...174L..53M. doi: 10.1086/180947 .
  14. ↑ Kitamoto, S.; Miyamoto, S.; Tsunemi, H; Makishima, K; Nakagawa, M (1 June 1984). "The transient X-ray source 4U 1543-47 observed from TENMA". Publications of the Astronomical Society of Japan. 36 (4): 799–806. Bibcode:1984PASJ...36..799K.
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