Astronomy:NGC 1535

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Short description: Planetary nebula in the constellation of Eridanus
NGC 1535
Emission nebula
Planetary nebula
File:280px
NGC 1535 using the 0.8m Schulman Telescope from the Mount Lemmon SkyCenter
Credit: Adam Block/Mount Lemmon SkyCenter/University of Arizona
Observation data: J2000 epoch
Right ascension 04h 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
See also: Lists of nebulae

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 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. ↑ 1.0 1.1 1.2 1.3 "NGC 1535". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NGC+1535. 
  2. ↑ Smith, H. (9 April 2015). "On the distances of planetary nebulae". Monthly Notices of the Royal Astronomical Society 449 (3): 2980–3005. doi:10.1093/mnras/stv456. Bibcode: 2015MNRAS.449.2980S. 
  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. http://www.deep-sky-atlas.com/. 
  4. ↑ Seligman, Courtney. "Celestial Atlas: NGC Objects: NGC 1500 - 1549". http://cseligman.com/text/atlas/ngc15.htm#1535. 
  5. ↑ "The Herschel 400 Club Observing List in New General Catalog (N.G.C.) Number Order.". https://www.astroleague.org//wp-content/uploads/2022/02/h400lstn.pdf. 
  6. ↑ 6.0 6.1 "The planetary nebulae NGC 1535 and NGC 2022.". https://ui.adsabs.harvard.edu/abs/1984A&A...136..193S/abstract. 
  7. ↑ "Best of AOP - Planetary Nebulae: NGC 1535". NOAO. http://www.caelumobservatory.com/obs/n1535.html. 
  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". https://ui.adsabs.harvard.edu/scan/manifest/1918PLicO..13...55C. 
  10. ↑ Barker, Timothy (1989-05-15). "The ionization structure of planetary nebulae. IX - NGC 1535" (in en). Astrophysical Journal, Part 1 340. ISSN 0004-637X. https://ntrs.nasa.gov/citations/19890053000. 
  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". https://ui.adsabs.harvard.edu/abs/1996ApJ...466..352L/abstract. 
  13. ↑ "ROSAT X-Ray Observations of Two Planetary Nebulae: NGC 1535 and NGC 3587". https://ui.adsabs.harvard.edu/abs/1998AJ....116.1882C/abstract. 
  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. doi:10.1051/0004-6361/202141916. Bibcode: 2021A&A...656A..51G. 
  15. ↑ Pottasch, S. R.; Surendiranath, R.; Bernard-Salas, J. (2011-07-01). "Abundances in planetary nebulae: NGC 1535, NGC 6629, He2-108, and Tc1" (in en). Astronomy & Astrophysics 531: A23. doi:10.1051/0004-6361/201116669. ISSN 0004-6361. https://www.aanda.org/articles/aa/abs/2011/07/aa16669-11/aa16669-11.html. 
  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.". https://ui.adsabs.harvard.edu/abs/1988A&A...195..263C/abstract. 

Template:NGC objects:1500-1999



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