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NGC 3384

Coordinates: Sky map 10h 48m 16.9s, 12° 37′ 46″
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NGC 3384
NGC 3384 taken by Hubble.[1]
Observation data (J2000 epoch)
ConstellationLeo[2]
Right ascension10h 48m 16.9s[3]
Declination 12° 37′ 46″[3]
Redshift704 ± 2 km/s[3]
Distance35.1 ± 2.3 Mly (10.8 ± 0.7 Mpc)[4]
Apparent magnitude (V)10.9[3]
Characteristics
TypeE7[3]
Apparent size (V)5′.5 × 2′.5[3]
Other designations
NGC 3371,[3] UGC 5911,[3] PGC 32292[3]

NGC 3384 is an elliptical galaxy in the constellation Leo. The galaxy was discovered by William Herschel in 1784 as part of the Herschel 400 Catalogue. The high age of the stars in the central region of NGC 3384 was confirmed after analysis of their color. More than 80% were found to be Population II stars which are over a billion years old.[5] The supermassive black hole at the core has a mass of 1.6 0.1
−0.2×107 M☉.[6]

Galaxy group information

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SDSS image of NGC 3384 in upper left with M105 (mid right), and NGC 3389 (lower left)

NGC 3384 is a member of the M96 Group, a group of galaxies in the constellation Leo that is sometimes referred to as the Leo I Group.[5] This group also includes the Messier objects M95, M96, and M105. All of these objects are conspicuously close to each other in the sky.[7][8][9][10]

References

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  1. ^ "Settling into old age". spacetelescope.org. Retrieved 13 May 2019.
  2. ^ R. W. Sinnott, ed. (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 978-0-933346-51-2.
  3. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for NGC 3384. Retrieved 2006-10-12.
  4. ^ Jensen, Joseph B.; Tonry, John L.; Barris, Brian J.; Thompson, Rodger I.; et al. (February 2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". Astrophysical Journal. 583 (2): 712–726. arXiv:astro-ph/0210129. Bibcode:2003ApJ...583..712J. doi:10.1086/345430. S2CID 551714.
  5. ^ a b Attia, Abdel-Fattah; Ismail, H. A.; Selim, I. M.; Osman, A. M.; et al. (August 2005). "Stellar Population Analysis of Galaxies based on Genetic Algorithms". Chinese Journal of Astronomy and Astrophysics. 5 (4): 347–355. Bibcode:2005ChJAA...5..347A. doi:10.1088/1009-9271/5/4/002.
  6. ^ Graham, Alister W. (November 2008), "Populating the Galaxy Velocity Dispersion – Supermassive Black Hole Mass Diagram: A Catalogue of (Mbh, σ) Values", Publications of the Astronomical Society of Australia, 25 (4): 167–175, arXiv:0807.2549, Bibcode:2008PASA...25..167G, doi:10.1071/AS08013, S2CID 89905.
  7. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 978-0-521-35299-4.
  8. ^ P. Fouque; E. Gourgoulhon; P. Chamaraux; G. Paturel (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy and Astrophysics Supplement. 93: 211–233. Bibcode:1992A&AS...93..211F.
  9. ^ A. Garcia (1993). "General study of group membership. II – Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
  10. ^ G. Giuricin; C. Marinoni; L. Ceriani; A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. S2CID 9618325.
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