NGC 1832
| NGC 1832 | |
|---|---|
 NGC 1832 by the Hubble Space Telescope | |
| Observation data (J2000 epoch) | |
| Constellation | Lepus |
| Right ascension | 05h 12m 03.4s[1] |
| Declination | −15° 41′ 16″[1] |
| Redshift | 0.006468 ± 0.000017 [1] |
| Heliocentric radial velocity | 1,939 ± 5 km/s[1] |
| Distance | 78.8 ± 19.0 Mly (24.15 ± 5.8 Mpc)[1] |
| Apparent magnitude (V) | 11.3[2] |
| Characteristics | |
| Type | SB(r)bc [1] |
| Apparent size (V) | 2.6′ × 1.7′[1] |
| Other designations | |
| MCG -3-14-10, IRAS 05098-1544, PGC 16906 | |
NGC 1832 is a barred spiral galaxy in the constellation Lepus. The galaxy lies about 80 million light years away from Earth, which means, given its apparent dimensions, that NGC 1832 is approximately 55,000 light years across.[1] It was discovered by William Herschel on February 4, 1785.[3]
Characteristics
[edit]The galaxy has a bright nucleus. The bar has bright ansae at its ends[4] and two loosely wounded arms in a nearly grand design pattern emanate from there. The arms form a nearly complete inner ring at the end of the bar.[5] The ring has a radius of 13 arcseconds and has an estimated star formation rate of 0.70 ± 0.20 M☉.[6] The ring appears as a pseudoring in H-alpha. There is also Hα emission from the nucleus not between the nucleus and the inner ring.[7] The west arm appears diffuse and resembles more like narrow spiral arm fragments. The east arm is better defined. Both arms complete less than half of revolution before fading.[4] There are many HII regions along both arms, the largest of which are more than two arcseconds across.[5] The star formation doesn't appear to be due to a leading density wave causing a pressure shock to the arms of the galaxy.[8]
Supernovae
[edit]Two supernovae have been observed in NGC 1832:
- SN 2004gq (type Ib,[9] peak visual magnitude 15.3[10]) was discovered independently on 11 December 2004 by H. Pugh and W. Li, using the Katzman Automatic Imaging Telescope, and by F. Manzini, as part of the Stazione Astronomica di Sozzago Supernova Search.[11]
- SN 2009kr (type II-L[12]) was discovered by Koichi Itagaki on 6 November 2009 at an apparent magnitude of 16.[13] The progenitor star was identified in images by the Hubble Space Telescope as a luminous supergiant with a mass over 18 M☉, the first time a progenitor of a type II-L supernova was identified.[12]
Nearby galaxies
[edit]NGC 1832 is the foremost galaxy of the NGC 1832 Group,[14] also known as LGG 129. Other members of the group include spiral galaxies MCG-3-14-1, MCG-3-14-4, MCG-2-14-2, and MCG-2-14-4.[15]
References
[edit]- ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 1832. Retrieved 6 February 2025.
- ^ "Revised NGC Data for NGC 1832". spider.seds.org. Retrieved 30 March 2024.
- ^ Seligman, Courtney. "NGC 1832 (= PGC 16906)". Celestial Atlas. Retrieved 19 November 2018.
- ^ a b Eskridge, 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. doi:10.1086/342340.
- ^ a b Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
- ^ Grouchy, R. D.; Buta, R. J.; Salo, H.; Laurikainen, E. (1 June 2010). "RING STAR FORMATION RATES IN BARRED AND NONBARRED GALAXIES". The Astronomical Journal. 139 (6): 2465–2493. doi:10.1088/0004-6256/139/6/2465.
- ^ Crocker, Deborah A.; Baugus, Pamela D.; Buta, R. (August 1996). "The Distribution and Properties of H II Regions in Early-to-Intermediate Hubble Type Ringed Galaxies". The Astrophysical Journal Supplement Series. 105: 353. doi:10.1086/192318.
- ^ Beckman, J. E.; Cepa, J. (1 March 1990). "The nature of arms in spiral galaxies. I. Azimuthal colour profiles of NGC 7479 and NGC 1832". Astronomy and Astrophysics. 229: 37–46. ISSN 0004-6361.
- ^ Modjaz, M.; Kirshner, R.; Challis, P.; Falco, E. (1 January 2005). "Supernovae 2004gq and 2005A". International Astronomical Union Circular. 8461: 3. ISSN 0081-0304.
- ^ Drout, Maria R.; Soderberg, Alicia M.; Gal-Yam, Avishay; Cenko, S. Bradley; Fox, Derek B.; Leonard, Douglas C.; Sand, David J.; Moon, Dae-Sik; Arcavi, Iair; Green, Yoav (10 November 2011). "THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES". The Astrophysical Journal. 741 (2): 97. doi:10.1088/0004-637X/741/2/97.
- ^ Green, Daniel (12 December 2004). "IAUC 8452: TRANSIENT IN Lyn; 2004gq, 2004gr". www.cbat.eps.harvard.edu. 8452.
- ^ a b Elias-Rosa, Nancy; Van Dyk, Schuyler D.; Li, Weidong; Miller, Adam A.; Silverman, Jeffrey M.; Ganeshalingam, Mohan; Boden, Andrew F.; Kasliwal, Mansi M.; Vinkó, József; Cuillandre, Jean-Charles; Filippenko, Alexei V.; Steele, Thea N.; Bloom, Joshua S.; Griffith, Christopher V.; Kleiser, Io K. W.; Foley, Ryan J. (10 May 2010). "THE MASSIVE PROGENITOR OF THE TYPE II-LINEAR SUPERNOVA 2009kr". The Astrophysical Journal. 714 (2): L254 – L259. doi:10.1088/2041-8205/714/2/L254.
- ^ Nakano, S.; Yusa, T.; Kadota, K. (8 November 2009). "Supernova 2009kr in NGC 1832". Central Bureau Electronic Telegrams. 2006: 1.
- ^ 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. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025.
- ^ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN 0365-0138.
External links
[edit]
- NGC 1832 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
