Astronomy:NGC 5170

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Short description: Edge-on spiral galaxy in the constellation Virgo
NGC 5170
NGC 5170 HST 9766 R814B435.png
NGC 5170 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationVirgo
Right ascension 13h 29m 48.769s[1]
Declination−17° 57′ 59.39″[1]
Redshift0.005006[2]
Helio radial velocity1,502 km/s[3]
Galactocentric velocity1,386 km/s[3]
Distance83.5 Mly (25.59 Mpc)[3]
Apparent magnitude (V)12.4[2]
Apparent magnitude (B)12.07[3]
Absolute magnitude (V)−21.6[4]
Characteristics
TypeSA(s)c: sp[2]
Apparent size (V)9′.9 × 1′.2[2]
Other designations
IRAS 13271-1742, NGC 5170, MCG-03-34-084, PGC 47394[3][5]

NGC 5170 is a large, nearby,[6] edge-on spiral galaxy in the equatorial constellation of Virgo. It was discovered on February 7, 1785 by William Herschel. This galaxy is located at a distance of 83.5 million light years and is receding at a heliocentric radial velocity of 1,502 km/s.[3] It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster.[7]

The inclination of the galactic plane of NGC 5170 is tilted at an angle of ~86° to the line of sight from the Earth, which means the disk is significantly obscured. It is estimated to have a morphological class of type Sb to Sc, meaning the spiral arms are moderate to loosely wound. The bulge-to-disk ratio of 0.5 is more consistent with an Sb galaxy.[4] It has an estimated star formation rate of 1.37±0.23 M☉·yr−1, which is more than double the rate in the Milky Way.[4]

The galactic latitude of this star is 43°, making the field relatively free of stars in the Milky Way. Combined with the proximity and edge-on view of NGC 5170, this makes galaxy useful for studies of its globular cluster population. It is estimated to have a total of 600±100 globulars, which is much higher than for the Milky Way. A candidate ultra-compact dwarf galaxy has been identified that is associated with NGC 5170.[4]

Numerical modeling of this galaxy indicates it has a massive dark halo with a thin, low surface brightness disk.[6] The halo mass of NGC 5170 is 3.4×1012 M☉.[4] Examination of the galaxy with the Chandra X-ray Observatory showed there is no diffuse X-ray emission from hot gas in the extended galactic halo.[8]

References

  1. ↑ 1.0 1.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 "NASA/IPAC Extragalactic Database". Results for NGC 5170. http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+5170&img_stamp=yes&extend=no. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Tully, R. Brent et al. (2016). "Cosmicflows-3". The Astronomical Journal 152 (2): 21. doi:10.3847/0004-6256/152/2/50. 50. Bibcode: 2016AJ....152...50T. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 Forbes, Duncan A. et al. (March 2010). "A blue tilt in the globular cluster system of the Milky Way-like galaxy NGC 5170". Monthly Notices of the Royal Astronomical Society 403 (1): 429–438. doi:10.1111/j.1365-2966.2009.16130.x. Bibcode: 2010MNRAS.403..429F. 
  5. ↑ "NGC 5170". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NGC+5170. 
  6. ↑ 6.0 6.1 Khoperskov, A. et al. (July 2010). "Numerical modelling of the vertical structure and dark halo parameters in disc galaxies". Astronomische Nachrichten 331 (7): 731. doi:10.1002/asna.200911402. Bibcode: 2010AN....331..731K. 
  7. ↑ "The Virgo III Groups". Atlas of the Universe. http://www.atlasoftheuniverse.com/galgrps/viriii.html. 
  8. ↑ Pedersen, Kristian et al. (May 2006). "Discovery of a very extended X-ray halo around a quiescent spiral galaxy The "missing link" of galaxy formation". New Astronomy 11 (7): 465–470. doi:10.1016/j.newast.2005.11.004. Bibcode: 2006NewA...11..465P. 

External links

Coordinates: Sky map 13h 29m 48.8s, −17° 57′ 59″



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