ally be hidden by a cloud in front of the nebula, estimated at perhaps 12 to 30 million miles across. This lasted until 1985 when the star's brightness recovered. In 1996 the star experienced another such dimming though to be caused for similar reasons that lasted for around 400 days. Yet another such dimming occurred in 2004.
- NGC 2346. Simbad Astronomical Database. simbad.u-strasbg.fr. Retrieved on 2019-08-25.
- Gaia Colaboration. VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018). (2018). VizieR Online Data Catalog. bibcode: 2018yCat.1345....0G
- Stanghellini, L.; Shaw, R. A.; Villaver, E. (2008). "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale". The Astrophysical Journal 689 (1): 194-202. doi:10.1086/592395. Bibcode: 2008ApJ...689..194S. arXiv:0807.1129
- Høg, E.; Fabricius, C.; Makarov, V. V. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27-L30. Bibcode: 2000A&A...355L..27H.
- From direct calculation using distance of 2,300 ly and apparent magnitude of +11.58.
- NGC 2346. spacetelescope.org (1999-10-07). Retrieved on 2019-08-25.
- Barbier-Brossat, M.; Petit, M.; Figon, P. (1994). "Third bibliographic catalogue of stellar radial velocities". Astronomy and Astrophysics Supplementary Series 108: 603-609. Bibcode: 1994A&AS..108..603B.
- NGC 2346: A Butterfly-Shaped Planetary Nebula. apod.nasa.gov (2001-10-28). Retrieved on 2019-08-25.
- Bob King (2016-03-02). NGC 2346: A Cosmic Butterfly Plays Peekaboo. Retrieved on 2019-08-25.
- Manchado, L.; Stanghellini, E.; Villaver, E. et al. (2015). "High resolution imaging of NGC 2346 with GSAOI/GeMS: disentangling the planetary nebula molecular structure to understand its origin and evolution". The Astrophysical Journal 808 (2). doi:10.1088/0004-637X/808/2/115. Bibcode: 2015ApJ...808..115M. arXiv:1506.03712
- Kato, T.; Nogami, D.; Baba, H. (2001). "The 1996-1997 Fading of V651 Mon, the Binary Central Star of the Planetary Nebula NGC 2346". Publications of the Astronomical Society of Japan 53 (5): 901–904. doi:10.1093/pasj/53.5.901. arXiv:astro-ph/0112304