NGC 4535

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NGC 4535
NGC 4535.jpg
NGC 4535 imaged with the Very Large Telescope at the Paranal Observatory in Chile
Observation data (J2000 epoch)
Right ascension12h 34m 20.310s[1]
Declination+08° 11′ 51.94″[1]
Helio radial velocity+1,962[2] km/s
Distance54.14 ± 1.76 Mly (16.60 ± 0.54 Mpc)[3]
Group or clusterVirgo Cluster
Apparent magnitude (B)10.73[4]
Absolute magnitude (V)–21.42 ± 0.09[3]
Size117,000 ly
Apparent size (V)11′.8 × 11′.0[6]
Other designations
CGCG 42-159, IRAS 12318+0828, MCG 1-32-104, PGC 41812, UGC 7727, VCC 1555

NGC 4535 is a barred spiral galaxy located some 54[3] million light years from Earth in the constellation Virgo. It is a member of the Virgo Cluster of galaxies and is located 4.3° from Messier 87. The galactic plane of NGC 4535 is inclined by an angle of 43° to the line of sight from the Earth.[4] The morphological classification of NGC 4535 in the De Vaucouleurs system is SAB(s)c,[5] which indicates a bar structure across the core (SAB), no ring (s), and loosely wound spiral arms (c). The inner part of the galaxy has two spiral arms, which branch into multiple arms further away. The small[6] nucleus is of type HII, meaning the spectrum resembles that of an H II region.[5]

During 1999, the Hubble Space Telescope was used to observe Cepheid variable stars in NGC 4535. The period-luminosity relationship for these objects yielded a distance modulus of 31.02 ± 0.26 magnitude. This corresponded to a physical distance estimate of 52.2 ± 6.2 Mly (16.0 ± 1.9) Mpc, which was consistent with distance estimates for other members of the Virgo Cluster.[7]


  1. ^ a b Skrutskie, M. F.; et al. (February 2006), "The Two Micron All Sky Survey (2MASS)", The Astronomical Journal, 131 (2): 1163–1183, Bibcode:2006AJ....131.1163S, doi:10.1086/498708.
  2. ^ Crook, Aidan C.; et al. (February 2007), "Groups of Galaxies in the Two Micron All Sky Redshift Survey", The Astrophysical Journal, 655 (2): 790–813, arXiv:astro-ph/0610732, Bibcode:2007ApJ...655..790C, doi:10.1086/510201.
  3. ^ a b c Gurovich, Sebastián; et al. (September 2010), "The Slope of the Baryonic Tully-Fisher Relation", The Astronomical Journal, 140 (3): 663–676, arXiv:1004.4365, Bibcode:2010AJ....140..663G, doi:10.1088/0004-6256/140/3/663. See Table 2.
  4. ^ a b Vollmer, B.; et al. (March 2010), "The influence of the cluster environment on the large-scale radio continuum emission of 8 Virgo cluster spirals", Astronomy and Astrophysics, 512: A36, arXiv:1001.3597, Bibcode:2010A&A...512A..36V, doi:10.1051/0004-6361/200913591.
  5. ^ a b c Boquien, M.; et al. (March 2012), "The IRX-β relation on subgalactic scales in star-forming galaxies of the Herschel Reference Survey", Astronomy & Astrophysics, 539: A145, arXiv:1201.2405, Bibcode:2012A&A...539A.145B, doi:10.1051/0004-6361/201118624, hdl:1854/LU-3001157.
  6. ^ a b Buta, Ronald J.; et al. (2007), Atlas of Galaxies, Cambridge University Press, pp. 13–17, 232, ISBN 978-0521820486.
  7. ^ Macri, L. M.; et al. (August 1999), "The Extragalactic Distance Scale Key Project. XVIII. The Discovery of Cepheids and a New Distance to NGC 4535 Using the Hubble Space Telescope", The Astrophysical Journal, 521 (1): 155–178, arXiv:astro-ph/9901332, Bibcode:1999ApJ...521..155M, doi:10.1086/307541.
NGC 4535 imaged with a 24-inch telescope

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