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NGC 1535

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NGC 1535
Emission nebula
Planetary nebula
NGC 1535 using the 0.8m Schulman Telescope from the Mount Lemmon SkyCenter
Observation data: J2000 epoch
Right ascension04h 14m 15.782s[1]
Declination−12° 44′ 21.68″[1]
Distance5500–7500 ly   (1740–2310[2] pc)
Apparent magnitude (V)10.5[1]
Apparent dimensions (V)0.650′ × 0.611′[1]
ConstellationEridanus
Designations2MASX J04141578-1244216, IRAS 04119-1251, PN G 206.4-40.5, PK 206-40.1, dML87 112, UITBOC 627, VERA J0414-1244

NGC 1535, also known as Cleopatra's Eye,[3] is a planetary nebula located around 5500-7500 light years away from Earth in the constellation of Eridanus.

It was discovered by William Herschel on February 1, 1785.[4] The object is included in the Astronomical League's Herschel 400 Observing Program.[5]

Characteristics

It is very similar to the Eskimo Nebula in both color and structure. It has a round exhibiting moderate ellipticity.[6] The dust distribution inside NGC 1535 is uniform and nearly round in shape. It displays a dust halo with a noticeable inner ring of increased intensity.[7][8] Outside this ring is a faint oval disk, note quite symmetrical with the main nebula. This region shows faint traces of ring formation in the southeastern region.[6][9] The nebula seems to have formed in a somewhat metal-poor region having undergone little or no enhancement of elements mixing with nuclear-processed material.[10]

NGC 1536 is a bright, high-excitatory nebula.[11] Spectra of NGC 1535 from ROSAT reveal of “double hump” shape with approximately one-third of the photons are within the high energy range with more than 0.5 keV. These high energies could not simply have been produced by a stellar photosphere, even with the central star having a temperature of 250,000 Kelvin.[12]

Observations by Leahy et al. using ROSAT reported X-ray emissions from NGC 3587 and NGC 1535. However comparisons between optical and X-ray images shows that these X-ray emissions coincide with a star that was outside the optical boundary of the nebula. This would make previous reports of X-ray emission from NGC 1535 likely false. Observations were taken using ROSAT High Resolution Imager which clearly confirms that the X-ray emissions contain three peaks that are point sources (RX J111447.9+550106, RX J111450.9+550208, and RX J111504.9+550141). Only the first of these sources are projected to be from the central star.[13]

Central star

At the center of NGC 1535, there is a O-type star with a spectral type of O(H)5. It is difficult to visually observe with a magnitude of 10. This star has a mass of 0.59☉ and a temperature of 66,000 Kelvin.[14][15] The star produces stellar winds with a terminal velocity of about 200 km/sec. These stellar winds are suspected to be the dominant force, shaping the morphology of the nebula to a round shape.[16][17]

References

  1. "NGC 1535". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 11 July 2015.
  2. Smith, H. (9 April 2015). "On the distances of planetary nebulae". Monthly Notices of the Royal Astronomical Society. 449 (3): 2980–3005. arXiv:1409.3422. Bibcode:2015MNRAS.449.2980S. doi:10.1093/mnras/stv456.
  3. Stoyan, Ronald; Schurig, Stephan (2014). interstellarum Deep Sky Atlas. Erlangen: Cambridge University Press; Oculum-Verlag GmbH. ISBN 978-1-107-50338-0. OCLC 920437579.
  4. Seligman, Courtney. "Celestial Atlas: NGC Objects: NGC 1500 - 1549". cseligman.com. Archived from the original on 1 January 2016. Retrieved 11 July 2015.
  5. "The Herschel 400 Club Observing List in New General Catalog (N.G.C.) Number Order" (PDF). The Astronomical League. Retrieved 2024-03-05.
  6. "The planetary nebulae NGC 1535 and NGC 2022". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
  7. "Best of AOP - Planetary Nebulae: NGC 1535". Caelum Observatory (mirror of NOAO/AOP. NOAO. Archived from the original on 13 July 2015. Retrieved 11 July 2015.
  8. R A Pignata, W A Weidmann, E O Schmidt, A Mudrik, D Mast, Dust distribution in planetary nebulae, Monthly Notices of the Royal Astronomical Society, Volume 528, Issue 1, February 2024, Pages 459–480, https://doi.org/10.1093/mnras/stad3568
  9. "Part III. The Planetary Nebulae". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
  10. Barker, Timothy (1989-05-15). "The ionization structure of planetary nebulae. IX - NGC 1535". Astrophysical Journal, Part 1. 340. ISSN 0004-637X.
  11. Louise, R. & Pascoli, G.. (1985). Study of three high excitation planetary nebulae in the Southern Hemisphere - NGC 1535, NGC 2440, NGC 2452. Astronomy and Astrophysics. 150. 285-297.
  12. "ROSAT X-Ray Observations of Four Planetary Nebulae". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
  13. "ROSAT X-Ray Observations of Two Planetary Nebulae: NGC 1535 and NGC 3587". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
  14. González-Santamaría, I.; Manteiga, M.; Manchado, A.; Ulla, A.; Dafonte, C.; López Varela, P. (2021). "Planetary nebulae in Gaia EDR3: Central star identification, properties, and binarity". Astronomy & Astrophysics. 656: A51. arXiv:2109.12114. Bibcode:2021A&A...656A..51G. doi:10.1051/0004-6361/202141916. S2CID 237940344.
  15. Pottasch, S. R.; Surendiranath, R.; Bernard-Salas, J. (2011-07-01). "Abundances in planetary nebulae: NGC 1535, NGC 6629, He2-108, and Tc1". Astronomy & Astrophysics. 531: A23. arXiv:1107.4041. doi:10.1051/0004-6361/201116669. ISSN 0004-6361.
  16. Adam, J. & Köppen, J.. (2017). Influence of the Stellar Wind on the Nebular Ionization in NGC 1535 and 4361. Symposium - International Astronomical Union. 103. 338-339. 10.1017/S0074180900093888.
  17. "Unexpected bi-polar motions in the planetary nebula NGC 1535". ui.adsabs.harvard.edu. Retrieved 2026-05-26.