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NGC 266
NGC 266
	NGC 266 is the galaxy in the center-left of this photo. The bright star in the center is SAO 54174.
Observation data (J2000 epoch)
Constellation	Pisces
Right ascension	00h 49m 47.81400s
Declination	+32° 16′ 39.8067″
Redshift	0.015547
Heliocentric radial velocity	4,565.3±15.3 km/s
Distance	197 Mly (60.3 Mpc)
Group or cluster	NGC 315 Group
Apparent magnitude (V)	12.54
Characteristics
Type	SB(rs)ab
Apparent size (V)	3.0' × 2.9'
Other designations
	IRAS 00471+3200, 2MASX J00494779+3216398, UGC 508, MCG +05-03-009, PGC 2901, CGCG 501-022

NGC 266 is a massive^[4] barred spiral galaxy in the constellation Pisces. NGC 266 is located at a distance of 197 megalight-years from the Milky Way.^[4] It was discovered on September 12, 1784, by William Herschel.^[5] The form of this barred galaxy is described by its morphological classification of SB(rs)ab,^[4] which indicates a quasi-ring-like structure (rs) and moderate-to-tightly wound spiral arms (ab).

According to A.M. Garcia, NGC 266 is a member of the NGC 315 Group (also known as LGG 14). This group contains 42 galaxies, including NGC 226, NGC 243, NGC 262, NGC 311, NGC 315, NGC 338, IC 43, IC 66, AND IC 69, among others.^[6] Also, a 2013 paper lists NGC 266 as the dominant member of a small group with six low-mass galaxies.^[4]

NGC 266 is an LINER-type active galaxy.^[7] It has a moderate star formation rate estimated at 2.4 M_☉·yr⁻¹.^[4] A diffuse X-ray emission from hot gas has been detected around this galaxy, extending out to a radius of at least 70,000 light years. This emission not being driven by winds from a starburst region, so the root cause is unknown.^[4]

One supernova has been observed in NGC 266. On 5 October 2005, Tim Puckett, Peter Ceravolo, and Yasuo Sano discovered SN 2005gl (type IIn, mag. 18.2).^[8] It was positioned 29.8″ east and 16.7″ north of the galactic nucleus. An image of the galaxy taken on September 10 showed no supernova event, so this explosion occurred after that date.^[9] The progenitor was identified as a massive hypergiant star that was most likely a luminous blue variable.^[10]

Image gallery

NGC 266 (SDSS)

References

^ ^a ^b 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.
^ ^a ^b ^c ^d "NASA/IPAC Extragalactic Database". Results for NGC 0266. Retrieved September 2, 2016.
^ van den Bosch, Remco C. E.; et al. (May 2015). "Hunting for Supermassive Black Holes in Nearby Galaxies With the Hobby-Eberly Telescope". The Astrophysical Journal Supplement Series. 218 (1): 13. arXiv:1502.00632. Bibcode:2015ApJS..218...10V. doi:10.1088/0067-0049/218/1/10. S2CID 117876537. 10.
^ ^a ^b ^c ^d ^e ^f ^g ^h Bogdán, Ákos; et al. (August 2013). "Detection of a Luminous Hot X-Ray Corona around the Massive Spiral Galaxy NGC 266". The Astrophysical Journal. 772 (2): 5. arXiv:1306.0643. Bibcode:2013ApJ...772...98B. doi:10.1088/0004-637X/772/2/98. S2CID 119206613. 98.
^ "New General Catalog Objects: NGC 250 - 299". Cseligman. Retrieved October 2, 2016.
^ Garcia, A. M. (1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47. Bibcode:1993A&AS..100...47G.
^ "NGC 266". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved December 31, 2016.
^ "SN 2005gl". Transient Name Server. IAU. Retrieved November 20, 2024.
^ Puckett, T.; et al. (October 2005). D. W. E., Green (ed.). "Supernova 2005gl in NGC 266". Central Bureau Electronic Telegrams. 250: 1. Bibcode:2005CBET..250....1P.
^ Gal-Yam, A.; Leonard, D. C. (April 2009). "A massive hypergiant star as the progenitor of the supernova SN 2005gl". Nature. 458 (7240): 865–867. Bibcode:2009Natur.458..865G. doi:10.1038/nature07934. PMID 19305392. S2CID 4392537.