Jump to content

NGC 2787

From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Rodw (talk | contribs) at 09:37, 24 November 2020 (Disambiguating links to AURA (link changed to Association of Universities for Research in Astronomy) using DisamAssist.). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

NGC 2787
NGC 2787 as observed by the Hubble Space Telescope (HST).
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension09h 19m 18.60430s[1]
Declination+69° 12′ 11.6429″[1]
Heliocentric radial velocity627.3±13.2 km/s[2]
Distance24.17 ± 0.46 Mly (7.41 ± 0.14 Mpc)[3]
Apparent magnitude (V)11.79[4]
Apparent magnitude (B)12.92[4]
Absolute magnitude (B)−18.84[5]
Characteristics
TypeSB(r)0+[6]
Mass/Light ratio50[5] M☉/L☉
Size5.5 kpc[5]
Apparent size (V)2′.530 × 1′.518[7] (NIR)
Notable featuresBarred lenticular; LINER
Other designations
PGC 26341, UGC 4914[8]

NGC 2787 is a barred lenticular galaxy approximately 24[3] million light-years away in the northern circumpolar constellation of Ursa Major. It was discovered on December 3, 1788 by German-born astronomer William Herschel. J. L. E. Dreyer described it as, "bright, pretty large, a little extended 90°, much brighter middle, mottled but not resolved, very small (faint) star involved to the southeast".[9] The visible galaxy has an angular size of 2′.5 × 1′.5[7] and an apparent visual magnitude of 11.8.[4]

This galaxy is small and isolated[5] with a morphological classification of SB(r)0+,[6] which indicates a barred spiral (SB) with a ring around the bar (r). Being a lenticular galaxy, it has the large halo of an elliptical galaxy. The disk is inclined at an angle of 58°±3° to the line of sight from the Earth, with the major axis aligned along a position angle of 110°±3°.[5] The galaxy has an unusually high mass-to-light ratio, much greater than for a typical spiral galaxy.[5] The distribution of the galaxy's neutral hydrogen forms a clumpy ring with a radius of 10.3 kpc, double that of the visible galaxy, with a mass of 5.5×108 M☉.[5] This ring appears misaligned with the central disk.[10]

NGC 2787 contains a low-ionization nuclear emission-line region (LINER) at its core, which is a type of region that is characterized by spectral line emission from weakly ionized atoms.[11] LINERs are very common within lenticular galaxies, with approximately one-fifth of nearby lenticular galaxies containing LINERs.[12] The supermassive black hole at the center has a mass of 4.1+0.4
−0.5×107 M☉.[13] The central region of the galaxy contains dust rings that are tilted with respect to the disk, which may be the result of an encounter with another galaxy.[10]

References

  1. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ van den Bosch, Remco C. E.; et al. (May 2015). "Hunting for Supermassive Black Holes in Nearby Galaxies With the Hobby-Eberly Telescope". The Astrophysical Journal Supplement Series. 218 (1): 13. arXiv:1502.00632. Bibcode:2015ApJS..218...10V. doi:10.1088/0067-0049/218/1/10. S2CID 117876537. 10.
  3. ^ a b Tully, R. Brent; et al. (October 2013). "Cosmicflows-2: The Data". The Astronomical Journal. 146 (4): 25. arXiv:1307.7213. Bibcode:2013AJ....146...86T. doi:10.1088/0004-6256/146/4/86. S2CID 118494842. 86.
  4. ^ a b c Véron-Cetty, M.-P.; Véron, P. (2010). "A catalogue of quasars and active nuclei". Astronomy & Astrophysics. 13th. 518. Bibcode:2010A&A...518A..10V. doi:10.1051/0004-6361/201014188. A10.
  5. ^ a b c d e f g Shostak, G. S. (March 1987). "The distribution of HI in the lenticular galaxy NGC 2787". Astronomy and Astrophysics. 175: 4–8. Bibcode:1987A&A...175....4S.
  6. ^ a b Erwin, Peter; Debattista, Victor P. (June 2013). "Peanuts at an angle: detecting and measuring the three-dimensional structure of bars in moderately inclined galaxies". Monthly Notices of the Royal Astronomical Society. 431 (4): 3060–3086. arXiv:1301.0638. Bibcode:2013MNRAS.431.3060E. doi:10.1093/mnras/stt385. S2CID 54653263.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ 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.
  8. ^ "NASA/IPAC Extragalactic Database". Results for NGC 2787. Retrieved 2006-12-13.
  9. ^ Seligman, Courtney. "NGC Objects: NGC 2750 - 2799". Celestial Atlas. Retrieved 2020-09-09.
  10. ^ a b Erwin, Peter; et al. (November 2003). "When Is a Bulge Not a Bulge? Inner Disks Masquerading as Bulges in NGC 2787 and NGC 3945". The Astrophysical Journal. 597 (2): 929–947. arXiv:astro-ph/0310791. Bibcode:2003ApJ...597..929E. doi:10.1086/378189. S2CID 16032205.
  11. ^ Ho, L. C.; et al. (1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". Astrophysical Journal Supplement. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.
  12. ^ Ho, L. C.; et al. (1997). "A Search for "Dwarf" Seyfert Nuclei. V. Demographics of Nuclear Activity in Nearby Galaxies". Astrophysical Journal. 487 (2): 568–578. arXiv:astro-ph/9704108. Bibcode:1997ApJ...487..568H. doi:10.1086/304638. S2CID 16742031.
  13. ^ 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.


Retrieved from "https://en.wikipedia.org/w/index.php?title=NGC_2787&oldid=990410144"