IC 1297

Last updated
IC 1297
Emission nebula
Planetary nebula
IC 1297 legacy dr10.jpg
An image of IC 1297
Observation data: J2000 epoch
Right ascension 19h 17m 23.4475188000s
Declination −39° 36′ 46.253665872″ [1]
Distance16007.755  ly    (4908  pc)
Apparent magnitude (V)10.7 [1]
Constellation Corona Australis
Physical characteristics
Radius 0.27 ly
Designations ESO 99-1, IRAS 15064-6429, IC 1297, AN 18.1907, PN Sa 2-386 [1]
See also: Lists of nebulae

IC 1297 (also known as Gaia DR3 6714803311390242048) [2] is a small planetary nebula in the constellation Corona Australis. It was initially discovered by Scottish astronomer Williamina Fleming in 1894. [3] IC 1297 is situated south of the celestial equator so it is more easily visible from the southern hemisphere. Given its visual magnitude of 10.7, IC 1297 is visible with the help of a telescope having an aperture of 6 inches (150mm) or more. [4] The object is located approximately 16,007.76 light years (4908pc) away from the Earth [5] , and is moving away from the Sun at a radial velocity of +19.0 km/s. [1] [6]

Contents

Physical characteristics

A paper from 2004 classified the central star of the planetary nebula as a hot Wolf–Rayet type star, with spectral type [WC3/4] or [WO3], indicating strong carbon and oxygen emission lines typical of very evolved stars. [7] Its proper motion has been measured as −1.672 mas/yr in right ascension and −5.191 mas/yr in declination in the 2020 Gaia EDR3 catalog, corresponding to a tangential motion across the sky. [8]

References

  1. 1 2 3 4 "IC 1297". simbad.u-strasbg.fr. Retrieved 2025-10-10.
  2. ↑ "Gaia Archive". gea.esac.esa.int. Retrieved 2025-10-10.
  3. ↑ "Index Catalog Objects: IC 1250 - 1299". cseligman.com. Retrieved 2025-10-10.
  4. ↑ "IC 1297 - Planetary Nebula in Corona Australis | TheSkyLive". theskylive.com. Retrieved 2025-10-10.
  5. ↑ Stanghellini, Letizia; Haywood, Misha (2010-04-16). (Macintosh; Intel Mac OS X 10_15_7) AppleWebKit/537.36 (KHTML, like Gecko) Chrome/110.0.0.0 Safari/537.36 Citoid/WMF (mailto:noc@wikimedia.org)&ssu=&ssv=&ssw=&ssx=eyJfX3V6bWYiOiI3ZjkwMDA4OTg3MGJlZC1mMjcwLTRhNGUtYjQ3NC03OTZiNjRjMTQzZGMxLTE3NjAxMDMwODc5NjQwLTAwMTk0MGFlOTI0M2M5NTFkNDQxMCIsInV6bXgiOiI3ZjkwMDBlZmM3NjkxOS0yNzJiLTQ5NDUtYmEwOC02MGI0OTY4NDMyYjcxLTE3NjAxMDMwODc5NjQwLTRjNDI0YjkzMmJlMzU2ZWExMCIsInJkIjoiaW9wLm9yZyJ9 "The Galactic Structure and Chemical Evolution Traced by the Population of Planetary Nebulae". The Astrophysical Journal. 714 (2): 1096–1107. arXiv: 1003.0759 . Bibcode:2010ApJ...714.1096S. doi:10.1088/0004-637x/714/2/1096. ISSN   0004-637X.{{cite journal}}: Check |url= value (help)
  6. ↑ Duflot, M.; Figon, P.; Meyssonnier, N. (December 1995). "Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue". Astronomy and Astrophysics Supplement Series. 114: 269. Bibcode:1995A&AS..114..269D. ISSN   0365-0138.
  7. ↑ Górny, S. K.; Stasińska, G.; Escudero, A. V.; Costa, R. D. D. (2004-11-01). "The populations of planetary nebulae in the direction of the Galactic bulge - Chemical abundances and Wolf-Rayet central stars". Astronomy & Astrophysics. 427 (1): 231–244. arXiv: astro-ph/0409532 . Bibcode:2004A&A...427..231G. doi:10.1051/0004-6361:20047064. ISSN   0004-6361.
  8. ↑ Collaboration, Gaia (November 2020). "VizieR Online Data Catalog: Gaia EDR3 (Gaia Collaboration, 2020)". VizieR Online Data Catalog. 1350: I/350. Bibcode:2020yCat.1350....0G. doi:10.26093/cds/vizier.1350.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.