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SCR 1845−6357
	; Three-colour image of SCR1845−6357AB generated from the SDI filter images (blue=1.575 μm, green=1.600 μm, red=1.625 μm). Because the T-dwarf fades away towards the longer wavelengths, it appears quite blue in this image. It is roughly 50 times fainter than the star and is separated from it by an angle of 1.17″ on the sky (4.5 times the Earth-Sun distance).
Observation data; Epoch J2000.0 Equinox J2000.0 (ICRS)
Constellation	Pavo
Right ascension	18h 45m 05.25325s
Declination	−63° 57′ 47.4501″
Apparent magnitude (V)	17.4
Characteristics
SCR 1845−6357A
Spectral type	M8.5
SCR 1845−6357B
Spectral type	T6
Apparent magnitude (J)	13.26
Astrometry
Proper motion (μ)	RA: 2583.190 mas/yr ; Dec.: 588.504 mas/yr
Parallax (π)	249.6651 ± 0.1330 mas
Distance	13.064 ± 0.007 ly ; (4.005 ± 0.002 pc)
Details
SCR 1845−6357A
Mass	0.0753 M☉
Radius	0.0941 R☉
Luminosity	2.649×10−4 L☉
Temperature	2400 K
SCR 1845−6357B
Mass	0.04 to 0.05 M☉
Radius	0.7±0.1 RJup
Surface gravity (log g)	5.1 cgs
Temperature	950 K
Age	1.8×109 to 3.1×109 years
Position (relative to A)
Epoch of observation	J2006.3
Angular distance	1.064 ± 0.004″
Position angle	177.2 ± 0.06°
Projected separation	4.10 ± 0.04 AU
Other designations
	GJ 12724, SCR J1845-6357, 2MASS J18450541-6357475, DENIS J184504.9-635747, SCR 1845
Database references
SIMBAD	A
	B
	SCR 1845−6357 Location of SCR 1845−6357 in the constellation Pavo;

SCR 1845−6357 is a binary system, 13.1 light-years (4.0 parsecs) away in the constellation Pavo. The primary is a faint red dwarf. It has a brown dwarf companion. The primary red dwarf was discovered in 2004 by Hambly et al.,^[9] while the secondary brown dwarf was later discovered in 2006.^[10]

System

The primary, SCR 1845−6357A, is a faint (apparent magnitude 17.4)^[2] ultra-cool red dwarf with a mass of about 7% of the Sun's. However, the measurements are still preliminary and are subject to change.^[11]

This star has been found to possess a brown dwarf companion, designated SCR 1845-6357B. The companion, classified as a T-dwarf, has an observed projected distance of 4.1 AU, an estimated mass between 40 and 50 times the mass of Jupiter, and an estimated effective temperature of 950 K.^[3]^[7] The brown dwarf has a near-IR J-band magnitude of 13.26.^[4]

References

^ ^a ^b ^c ^d 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 "SCR J1845-6357". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 5 November 2023.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j Kasper, Markus; Biller, Beth A.; Burrows, Adam; Brandner, Wolfgang; Budaj, Jano; Close, Laird M. (August 2007). "The very nearby M/T dwarf binary SCR 1845-6357". Astronomy and Astrophysics. 471 (2): 655–659. arXiv:0706.3824. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881.
^ ^a ^b Chris Gelino; Davy Kirkpatrick; Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Archived from the original on 2013-11-13. Retrieved 2012-06-10. (main page) Archived 2019-05-11 at the Wayback Machine
^ ^a ^b ^c ^d Cifuentes, C.; Caballero, J. A.; Cortés-Contreras, M.; Montes, D.; Abellán, F. J.; Dorda, R.; Holgado, G.; Zapatero Osorio, M. R.; Morales, J. C.; Amado, P. J.; Passegger, V. M.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sanz-Forcada, J. (2020-10-01). "CARMENES input catalogue of M dwarfs. V. Luminosities, colours, and spectral energy distributions". Astronomy and Astrophysics. 642: A115. arXiv:2007.15077. Bibcode:2020A&A...642A.115C. doi:10.1051/0004-6361/202038295. ISSN 0004-6361.
^ Vigan, A.; Bonnefoy, M.; Chauvin, G.; Moutou, C.; Montagnier, G. (2012-04-01). "High-contrast spectroscopy of SCR J1845-6357 B". Astronomy & Astrophysics. 540: A131. arXiv:1204.0241. doi:10.1051/0004-6361/201118426. ISSN 0004-6361.
^ ^a ^b Observed projected distance computed from parallax and observed angular distance.
^ Golovin, Alex; Reffert, Sabine; Just, Andreas; Jordan, Stefan; Vani, Akash; Jahreiß, Hartmut (November 2022). "The Fifth Catalogue of Nearby Stars (CNS5)". Astronomy & Astrophysics. 670: A19. arXiv:2211.01449. Bibcode:2023A&A...670A..19G. doi:10.1051/0004-6361/202244250. S2CID 253264922. Catalogue can be accessed here.
^ Hambly, Nigel C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Jao, Wei-Chun (2004). "The Solar Neighborhood. VIII. Discovery of New High Proper Motion Nearby Stars Using the SuperCOSMOS Sky Survey". The Astronomical Journal. 128 (1): 437–447. arXiv:astro-ph/0404265. Bibcode:2004AJ....128..437H. doi:10.1086/421748. S2CID 9586813.
^ Biller, B. A.; Kasper, M.; et al. (April 2006). "Discovery of a Brown Dwarf Very Close to the Sun: A Methane-rich Brown Dwarf Companion to the Low-Mass Star SCR 1845-6357". The Astrophysical Journal. 641 (2): L141–L144. arXiv:astro-ph/0601440. Bibcode:2006ApJ...641L.141B. doi:10.1086/504256.
^ "THE ONE HUNDRED NEAREST STAR SYSTEMS". Research Consortium On Nearby Stars. Georgia State University. January 1, 2008. Retrieved June 17, 2008.