NGC 1535
| Emission nebula | |
|---|---|
| Planetary nebula | |
 NGC 1535 using the 0.8m Schulman Telescope from the Mount Lemmon SkyCenter | |
| Observation data: J2000 epoch | |
| Right ascension | 04h 14m 15.782s[1] |
| Declination | −12° 44′ 21.68″[1] |
| Distance | 5500–7500 ly (1740–2310[2] pc) |
| Apparent magnitude (V) | 10.5[1] |
| Apparent dimensions (V) | 0.650′ × 0.611′[1] |
| Constellation | Eridanus |
| Designations | 2MASX 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
[edit]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 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
[edit]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
[edit]- ^ a b c d "NGC 1535". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 11 July 2015.
- ^ 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.
- ^ Stoyan, Ronald; Schurig, Stephan (2014). interstellarum Deep Sky Atlas. Erlangen: Cambridge University Press; Oculum-Verlag GmbH. ISBN 978-1-107-50338-0. OCLC 920437579.
- ^ Seligman, Courtney. "Celestial Atlas: NGC Objects: NGC 1500 - 1549". cseligman.com. Archived from the original on 1 January 2016. Retrieved 11 July 2015.
- ^ "The Herschel 400 Club Observing List in New General Catalog (N.G.C.) Number Order" (PDF). The Astronomical League. Retrieved 2024-03-05.
- ^ a b "The planetary nebulae NGC 1535 and NGC 2022". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
- ^ "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.
- ^ 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
- ^ "Part III. The Planetary Nebulae". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
- ^ Barker, Timothy (1989-05-15). "The ionization structure of planetary nebulae. IX - NGC 1535". Astrophysical Journal, Part 1. 340. ISSN 0004-637X.
- ^ 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.
- ^ "ROSAT X-Ray Observations of Four Planetary Nebulae". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
- ^ "ROSAT X-Ray Observations of Two Planetary Nebulae: NGC 1535 and NGC 3587". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
- ^ 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.
- ^ 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. doi:10.1051/0004-6361/201116669. ISSN 0004-6361.
- ^ 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.
- ^ "Unexpected bi-polar motions in the planetary nebula NGC 1535". ui.adsabs.harvard.edu. Retrieved 2026-05-26.
External links
[edit]
Media related to NGC 1535 at Wikimedia Commons- "NGC 1535". Mt. Lemmon SkyCenter. University of Arizona. Archived from the original on 2016-08-26. Retrieved 2015-12-26.
- "Cleopatra's Eye (NGC 1535)". Observing at Skyhound.
