NGC 4772 is aspiral galaxy in the constellationVirgo. The galaxy lies about 90 millionlight 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 byWilliam Herschel on January 24, 1784.[3]
NGC 4772 has a bright circulargalactic 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 minormerger.[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 beactive and based on its spectrum it has been characterised as a type 1.9LINER.[9]
The galaxy has two faint, narrowarms which wrap around the galaxy and form aring.[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 featuresH-alpha andhydrogen 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 differentposition 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 0.03M☉ per year.[8]
SN 1988E was discovered on 20 January 1988 by Yoshiaki Taniguchi at an apparent magnitude of 17.[10] It was initially identified as atype 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 byKoichi Itagaki at an apparent magnitude of 16.3. Its spectrum revealed it was atype Ia supernova near maximum light.[13] The supernova was highly reddened due toextinction by dust.[14]
^abEskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies".The Astrophysical Journal Supplement Series.143 (1):73–111.arXiv:astro-ph/0206320.Bibcode:2002ApJS..143...73E.doi:10.1086/342340.
^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.arXiv:1108.3662.Bibcode:2011AJ....142..145G.doi:10.1088/0004-6256/142/5/145.
^abcdefHaynes, 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.arXiv:astro-ph/0004340.doi:10.1086/301457.
^Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search forDwarf Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies".The Astrophysical Journal Supplement Series.112 (2):315–390.arXiv:astro-ph/9704107.Bibcode:1997ApJS..112..315H.doi:10.1086/313041.
^Murdin, P.; Green, D. W. E. (1 February 1988)."Supernovae".International Astronomical Union Circular (4546): 1.ISSN0081-0304.
^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.
