NGC 3489
NGC 3489 by Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationLeo
Right ascension11h 00m 18.6s[1]
Declination+13° 54′ 04″[1]
Redshift0.002258 ± 0.000006 [1]
Heliocentric radial velocity677 ± 2 km/s[1]
Distance29 ± 8.4 Mly (8.9 ± 2.6 Mpc)[1]
Apparent magnitude (V)10.2 [2]
Characteristics
TypeSAB(rs)0+ [1]
Apparent size (V)3.5′ × 2.0′
Other designations
UGC 6082, CGCG 066-084, MCG +02-28-039, PGC 33160[1]

NGC 3489 is a lenticular galaxy located in the constellation Leo. It is located at a distance of circa 30 million light years from Earth, which, given its apparent dimensions, means that NGC 3489 is about 30,000 light years across. It was discovered by William Herschel on April 8, 1784.[3] NGC 3489 is a member of the Leo Group.[4]

NGC 3489 has a weak bar, seen along the minor axis, and a small bulge.[5] The age of the stellar population in NGC 3489 shows a gradient, with the younger stars lying closer to the core. When observed in H-beta, the central arcsecond of NGC 3489 shows a peak, indicating the presence of younger stars at the core, whose age is estimated to be about 1.7 Gys.[6] Although currently NGC 3489 is considered a post-starburst galaxy, there is still molecular gas in the nucleus that can lead to star formation, although its mass is less than what is found in galaxies with active star formation.[7] In the nuclear region of NGC 3489 has been observed dust with an open spiral pattern.[6] The galaxy has an outer ring structure, with a diameter of 1.54 arcminutes along the major axis.[8]

NGC 3489 has an active galactic nucleus, which has been categorised based on its spectrum as a type 2 Seyfert galaxy or, based on the nuclear [O I] emission strength, which lies between that of H II nuclei and LINER, a transition object.[9] This kind of transition emission could be attributed to post AGB stars located in the core.[7] A supermassive black hole which accretes material in the centre of the galaxy is believed to be the cause of nuclear activity. In the centre of NGC 3489 lies a black hole with estimated mass (6±0.54)×106 M☉ based on velocity dispersion.[5]

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 3489. Retrieved 2016-01-18.
  2. ↑ "Revised NGC Data for NGC 3489". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 3489". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Stierwalt, Sabrina; Haynes, Martha P.; Giovanelli, Riccardo; Kent, Brian R.; Martin, Ann M.; Saintonge, Amélie; Karachentsev, Igor D.; Karachentseva, Valentina E. (1 August 2009). "The Arecibo Legacy Fast Alfa Survey. IX. The Leo Region H I Catalog, Group Membership, and the H I Mass Function for the Leo I Group". The Astronomical Journal. 138 (2): 338–361. arXiv:0906.2178. Bibcode:2009AJ....138..338S. doi:10.1088/0004-6256/138/2/338. S2CID 15537435.
  5. 1 2 Nowak, N.; Thomas, J.; Erwin, P.; Saglia, R. P.; Bender, R.; Davies, R. I. (1 February 2010). "Do black hole masses scale with classical bulge luminosities only? The case of the two composite pseudo-bulge galaxies NGC 3368 and NGC 3489". Monthly Notices of the Royal Astronomical Society. 403 (2): 646–672. arXiv:0912.2511. Bibcode:2010MNRAS.403..646N. doi:10.1111/j.1365-2966.2009.16167.x. S2CID 59580555.
  6. 1 2 McDermid, Richard M.; Emsellem, Eric; Shapiro, Kristen L.; Bacon, Roland; Bureau, Martin; Cappellari, Michele; Davies, Roger L.; De Zeeuw, Tim; Falcón-Barroso, Jesús; Krajnović, Davor; Kuntschner, Harald; Peletier, Reynier F.; Sarzi, Marc (December 2006). "The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres*". Monthly Notices of the Royal Astronomical Society. 373 (3): 906–958. arXiv:astro-ph/0609452. Bibcode:2006MNRAS.373..906M. doi:10.1111/j.1365-2966.2006.11065.x. S2CID 14930637.
  7. 1 2 Sarzi, Marc; Shields, Joseph C.; Schawinski, Kevin; Jeong, Hyunjin; Shapiro, Kristen; Bacon, Roland; Bureau, Martin; Cappellari, Michele; Davies, Roger L.; Tim de Zeeuw, P.; Emsellem, Eric; Falcón-Barroso, Jesús; Krajnović, Davor; Kuntschner, Harald; McDermid, Richard M.; Peletier, Reynier F.; van den Bosch, Remco C. E.; van de Ven, Glen; Yi, Sukyoung K. (March 2010). "The SAURON project - XVI. On the sources of ionization for the gas in elliptical and lenticular galaxies". Monthly Notices of the Royal Astronomical Society. 402 (4): 2187–2210. arXiv:0912.0275. Bibcode:2010MNRAS.402.2187S. doi:10.1111/j.1365-2966.2009.16039.x. S2CID 15107933.
  8. ↑ Comerón, S.; Salo, H.; Laurikainen, E.; Knapen, J. H.; Buta, R. J.; Herrera-Endoqui, M.; Laine, J.; Holwerda, B. W.; Sheth, K.; Regan, M. W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Gil de Paz, A.; Menéndez-Delmestre, K.; Seibert, M.; Mizusawa, T.; Kim, T.; Erroz-Ferrer, S.; Gadotti, D. A.; Athanassoula, E.; Bosma, A.; Ho, L. C. (19 February 2014). "ARRAKIS: atlas of resonance rings as known in the S4G". Astronomy & Astrophysics. 562: A121. arXiv:1312.0866. Bibcode:2014A&A...562A.121C. doi:10.1051/0004-6361/201321633. S2CID 119295831.
  9. ↑ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search for "Dwarf Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". The Astrophysical Journal Supplement Series. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.
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