NGC 5102

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NGC 5102
NGC 5102 hst 05400 R569B450.png
NGC 5102 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Centaurus
Right ascension 13h 21m 57.6s [1]
Declination −36° 37′ 49″ [1]
Redshift 468 ± 2 km/s [1]
Distance 12.1 ± 0.7 Mly (3.70 ± 0.23 Mpc) [2] [3] [4] [5]
Apparent magnitude  (V)10.4 [1]
Characteristics
Type SA0− [1]
Apparent size  (V)8.7′ × 2.8′ [1]
Other designations
PGC 46674 [1]

NGC 5102 is a lenticular galaxy in the Centaurus A/M83 Group of galaxies. It was discovered by John Herschel in 1835.

Contents

Distance measurements

At least two techniques have been used to measure the distance to NGC 5102. The surface brightness fluctuations distance measurement technique estimates distances to spiral galaxies based on the graininess of the appearance of their bulges. The distance measured to NGC 5102 using this technique is 13.0 ± 0.8 Mly (4.0 ± 0.2 Mpc). [2] However, NGC 5102 is close enough that the tip of the red giant branch (TRGB) method may be used to estimate its distance. The estimated distance to NGC 5102 using this technique is 11.1 ± 1.3 Mly (3.40 ± 0.39 Mpc). [3] Averaged together, these distance measurements give a distance estimate of 12.1 ± 0.7 Mly (3.70 ± 0.23 Mpc). [5]

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Large, quite faint, irregularly round; it brightens in the middle to a stellar nucleus.

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<span class="mw-page-title-main">NGC 2683</span> Galaxy in the constellation Lynx

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<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

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<span class="mw-page-title-main">NGC 4526</span> Lenticular galaxy in the constellation Virgo

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<span class="mw-page-title-main">NGC 3077</span> Galaxy in the constellation Ursa Major

NGC 3077 is a small disrupted elliptical galaxy, a member of the M81 Group, which is located in the northern constellation Ursa Major. Despite being similar to an elliptical galaxy in appearance, it is peculiar for two reasons. First, it shows wispy edges and scattered dust clouds that are probably a result of gravitational interaction with its larger neighbors, similar to the galaxy M82. Second, this galaxy has an active nucleus. This caused Carl Seyfert in 1943 to include it in his list of galaxies, which are now called Seyfert Galaxies. However, NGC 3077, though an emission line galaxy, is today no longer classified as a Seyfert galaxy.

<span class="mw-page-title-main">Bubble Nebula (NGC 6822)</span> Nebula in Barnards Galaxy in the constellation Sagittarius

The Bubble Nebula in Barnard's Galaxy has the official designation of Hubble 1925 I as it was the first object recorded in a paper by Hubble 1925. It includes areas of bright H II emission. It is located north-west of the larger Hubble 1925 III.

Surface brightness fluctuation (SBF) is a secondary distance indicator used to estimate distances to galaxies. It is useful to 100 Mpc (parsec). The method measures the variance in a galaxy's light distribution arising from fluctuations in the numbers of and luminosities of individual stars per resolution element.

<span class="mw-page-title-main">Dorado Group</span> Galaxy cluster in the constellation Dorado

The Dorado Group is a loose concentration of galaxies containing both spirals and ellipticals. It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'. It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere. Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region, designating it as G16.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 5102. Retrieved 2006-12-15.
  2. 1 2 J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". Astrophysical Journal. 546 (2): 681–693. arXiv: astro-ph/0011223 . Bibcode:2001ApJ...546..681T. doi:10.1086/318301. S2CID   17628238.
  3. 1 2 I. D. Karachentsev; V. E. Karachentseva; W. K. Hutchmeier; D. I. Makarov (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi: 10.1086/382905 .
  4. ↑ Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics. 49 (1): 3–18. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6. S2CID   120973010.
  5. 1 2 average(4.0 ± 0.2, 3.40 ± 0.39) = ((870 + 760) / 2) ± ((602 + 802)0.5 / 2) = 820 ± 50


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