Astronomy:NGC 4772

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NGC 4772
NGC 4772 imaged by SDSS
Observation data (J2000 epoch)
ConstellationVirgo
Right ascension 12h 53m 29.1613s[1]
Declination+02° 10′ 06.157″[1]
Redshift0.003469 ± 0.000017 [1]
Helio radial velocity1,040 ± 5 km/s[1]
Distance88.2 ± 30.1 Mly (27.0 ± 9.2 Mpc)[1]
Group or clusterNGC 4753 Group
Apparent magnitude (V)10.7[2]
Characteristics
TypeSA(s)a [1]
Size~87,000 ly (26.6 kpc) (estimated)[1]
Apparent size (V)3.4′ × 1.7′ [1]
Other designations
UGC 8021, MCG+00-33-018, PGC 43798[1]

NGC 4772 is a spiral galaxy in the constellation Virgo. The galaxy lies about 90 million light years away from Earth based on redshift-independent methods, which means, given its apparent dimensions, that NGC 4772 is approximately 85,000 light years across. Based on redshift the galaxy lies at a distance of 13.3 Mpc (43.4 Mly).[1] It was discovered by William Herschel on January 24, 1784.[3]

Characteristics

NGC 4772 has a bright circular galactic bulge. The galaxy has a long and broad low-surface-brightness bar in the bulge.[4][5] The kinematics of the central region indicate the presence of a misaligned bar or disk.[6] However it could also indicate the presence of counter-rotating gas,[7] with the galaxy being at the late stages of a minor merger.[6] The central region of the galaxy is depleted in hydrogen[6] and also has low carbon monoxide emission.[8] The nucleus of the galaxy has been found to be active and based on its spectrum it has been characterised as a type 1.9 LINER.[9]

The galaxy has two faint, narrow arms which wrap around the galaxy and form a ring.[4] An outer ring is visible, but appears segmented on its northern and southern part. A dust lane surrounds the bulge. The dust lane has some filaments which resemble a spiral structure.[6] The dust lane region also features H-alpha and hydrogen line emission. The hydrogen emission is distributed in two rings around the nucleus. The inner ring has a radius of 60 arcseconds and the outer ring a radius of 200 arcseconds. There is a faint blue stellar location at the outer ring, while the inner ring coincides with active star formation regions. The two rings have slightly different position angles.[6] Carbon monoxide emission is asymmetric and is distributed along the inner hydrogen ring.[8] The star formation rate of the galaxy is about 0.03 M☉ per year.[8]

Supernovae

Two supernovae have been observed in NGC 4772:

  • SN 1988E was discovered on 20 January 1988 by Yoshiaki Taniguchi at an apparent magnitude of 17.[10] It was initially identified as a type II supernova well past maximum,[11] but further observations found it was depleted in hydrogen and was thus reclassified as a type I supernova about 300 days post maximum light.[12]
  • SN 2012cu was discovered on 14 June 2012 by Koichi Itagaki at an apparent magnitude of 16.3. Its spectrum revealed it was a type Ia supernova near maximum light.[13] The supernova was highly reddened due to extinction by dust.[14]

Nearby galaxies

NGC 4772 is a member of the NGC 4753 Group, along with NGC 4629, NGC 4691, NGC 4753, NGC 4771, NGC 4845, and NGC 4904.[15] It is part of a Virgo II Groups, a chain of groups extending from the Virgo Cluster.[16] NGC 4772 lies near the outer regions of the Virgo Cluster and has been considered an outlying member of it. The high-surface brightness galaxy CGCG 015-036 lies 18.5 arcminutes away, while the galaxy pair of NGC 4809 and NGC 4810 lies 35 arcminutes to the northeast and at a similar redshift.[6]

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 "Results for object NGC 4772". NASA and Caltech. https://ned.ipac.caltech.edu/byname?objname=NGC+4772. 
  2. ↑ "Revised NGC Data for NGC 4772". https://spider.seds.org/ngc/revngcic.cgi?NGC4772. 
  3. ↑ Seligman, Courtney. "NGC 4772 (= PGC 43798)". https://cseligman.com/text/atlas/ngc47a.htm#4772. 
  4. ↑ 4.0 4.1 Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M. et al. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series 143 (1): 73–111. doi:10.1086/342340. Bibcode: 2002ApJS..143...73E. 
  5. ↑ Gutiérrez, Leonel; Erwin, Peter; Aladro, Rebeca; Beckman, John E. (1 November 2011). "The Outer Disks of Early-Type Galaxies. Ii. Surface-Brightness Profiles of Unbarred Galaxies and Trends with Hubble Type". The Astronomical Journal 142 (5): 145. doi:10.1088/0004-6256/142/5/145. Bibcode: 2011AJ....142..145G. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Haynes, Martha P.; Jore, Katherine P.; Barrett, Elizabeth A.; Broeils, Adrick H.; Murray, Brian M. (August 2000). "Kinematic Evidence of Minor Mergers in Normal S[CLC]a[/CLC] Galaxies: NGC 3626, NGC 3900, NGC 4772, and NGC 5854". The Astronomical Journal 120 (2): 703–727. doi:10.1086/301457. 
  7. ↑ Bettoni, D.; Galletta, G.; García-Burillo, S.; Rodríguez-Franco, A. (August 2001). "The gas content of peculiar galaxies: Counterrotators and polar rings". Astronomy & Astrophysics 374 (2): 421–434. doi:10.1051/0004-6361:20010717. Bibcode: 2001A&A...374..421B. 
  8. ↑ 8.0 8.1 8.2 Lee, Bumhyun; Wang, Jing; Chung, Aeree et al. (1 September 2022). "ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies". The Astrophysical Journal Supplement Series 262 (1): 31. doi:10.3847/1538-4365/ac7eba. Bibcode: 2022ApJS..262...31L. 
  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. doi:10.1086/313041. Bibcode: 1997ApJS..112..315H. 
  10. ↑ Kosai, H.; Taniguchi, Y.; Hamabe, M.; Nakamura, T. (1 February 1988). "Possible Supernova in NGC 4772". International Astronomical Union Circular (4543): 1. ISSN 0081-0304. Bibcode: 1988IAUC.4543....1K. http://www.cbat.eps.harvard.edu/iauc/04500/04543.html#Item0. 
  11. ↑ Murdin, P.; Green, D. W. E. (1 February 1988). "Supernovae". International Astronomical Union Circular (4546): 1. ISSN 0081-0304. http://www.cbat.eps.harvard.edu/iauc/04500/04546.html#Item0. 
  12. ↑ Pearce, Gillian; Patchett, Bruce; Murdin, Paul; Allington-Smith, Jeremy (1990). "Observations of SN1988e: A mature supernova". Astrophysics and Space Science 164 (1): 59–62. doi:10.1007/BF00653549. 
  13. ↑ Itagaki, K.; Howerton, S.; Noguchi, T.; Nakano, S.; Elenin, L.; Molotov, I.; Marion, G. H.; Milisavljevic, D. et al. (1 June 2012). "Supernova 2012cu in NGC 4772 = Psn J12532935+0209390". Central Bureau Electronic Telegrams (3146): 1. Bibcode: 2012CBET.3146....1I. https://ui.adsabs.harvard.edu/abs/2012CBET.3146....1I/abstract. 
  14. ↑ Huang, X. et al. (20 February 2017). "The Extinction Properties of and Distance to the Highly Reddened Type IA Supernova 2012cu". The Astrophysical Journal 836 (2): 157. doi:10.3847/1538-4357/836/2/157. Bibcode: 2017ApJ...836..157H. 
  15. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society 412 (4): 2498–2520. doi:10.1111/j.1365-2966.2010.18071.x. Bibcode: 2011MNRAS.412.2498M. http://www.sao.ru/hq/dim/groups/galaxies.dat. Retrieved 1 February 2025. 
  16. ↑ "The Virgo II Groups". http://www.atlasoftheuniverse.com/galgrps/virii.html. 

Template:NGC objects: 4001-5000



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