Lacaille 8760 är en ensam stjärna i mellersta delen av stjärnbildenMikroskopet som också har variabelbeteckningen AX Microscopii. Den har en skenbar magnitud av ca 6,67[2] och kräver åtminstone en handkikare för att kunna observeras. Baserat på parallax enligt Gaia Data Release 3 på ca 251,9 mas,[6] beräknas den befinna sig på ett avstånd på ca 12,9 ljusår (ca 4,0 parsek) från solen. Den rör sig bort från solen med en heliocentriskradialhastighet på ca 21 km/s.[4]
^ [abcd] Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ [abcde] "The One Hundred Nearest Star Systems", RECONS, Georgia State University, hämtad 2015-06-25.
^ [abcde] "V* AX Mic -- Flare Star", SIMBAD, Centre de Données astronomiques de Strasbourg, hämtad 2011-02-18.
^ [abcd] Torres, C. A. O.; et al. (December 2006), "Search for associations containing young stars (SACY). I. Sample and searching method", Astronomy and Astrophysics, 460 (3): 695–708, arXiv:astro-ph/0609258, Bibcode:2006A&A...460..695T, doi:10.1051/0004-6361:20065602, S2CID 16080025. See the online data.
^ [ab] HIP 105090 (unistra.fr). Hämtad 2023-02-21.
^ [ab] Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ [ab] Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763, S2CID 18775378, hämtad 2011-08-26.
^ [ab] Moro-Martín, A.; et al. (March 2015). "Does the Presence of Planets Affect the Frequency and Properties of Extrasolar Kuiper Belts? Results from the Herschel Debris and Dunes Surveys". The Astrophysical Journal. 801 (2): 28. arXiv:1501.03813. Bibcode:2015ApJ...801..143M. doi:10.1088/0004-637X/801/2/143. S2CID 55170390.Vizier catalog entry
^ [ab] Gautier, Thomas N., III; et al. (September 2007), "Far-Infrared Properties of M Dwarfs", The Astrophysical Journal, 667 (1): 527–536, arXiv:0707.0464, Bibcode:2007ApJ...667..527G, doi:10.1086/520667, S2CID 15732144.
^Lindgren, Sara; Heiter, Ulrike (2017). "Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature". Astronomy and Astrophysics. 604: A97. arXiv:1705.08785. Bibcode:2017A&A...604A..97L. doi:10.1051/0004-6361/201730715. S2CID 119216828.
^Boehle, A.; et al. (October 2019), "Combining high-contrast imaging and radial velocities to constrain the planetary architectures of nearby stars", Astronomy & Astrophysics, 630: 17, arXiv:1907.04334, Bibcode:2019A&A...630A..50B, doi:10.1051/0004-6361/201935733, A50.
^Byrne, P. B. (April 1981), "Gliese 825 - A new flare star", Monthly Notices of the Royal Astronomical Society, 195 (2): 143–147, Bibcode:1981MNRAS.195..143B, doi:10.1093/mnras/195.2.143.
^Carson, J. C.; et al. (December 2011), "Low-mass evolution - Zero-age main sequence to asymptotic giant branch", The Astrophysical Journal, 743 (2): 141, arXiv:1110.2191, Bibcode:2011ApJ...743..141C, doi:10.1088/0004-637X/743/2/141, S2CID 119270911.
^e-rara.ch. Johann Elert Bode. Uranographia star atlas (1801), Tabula XVI
^Johann Elert Bode. Allgemeine Beschreibung und Nachweisung der Gestirne (1801), Page 67
^Croswell, Ken (July 2003), "The Brightest Red Dwarf", Sky & Telescope: 32, hämtad 2011-02-18.
^Francis Baily. A Catalogue of 9766 Stars (1847), Page 219