Astronomy:NGC 1570
| NGC 1570 | |
|---|---|
 A legacy surveys image of NGC 1570. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Caelum |
| Right ascension | 04h 22m 08.93282s[1] |
| Declination | −43° 37′ 46.4517″[1] |
| Redshift | 0.014760[2] |
| Helio radial velocity | 4,392±84 km/s[2] |
| Distance | 199 Mly (60.9 Mpc)[3] |
| Group or cluster | LDC 302[3] |
| Apparent magnitude (B) | 13.22[4] |
| Characteristics | |
| Type | S0[5] |
| Mass | 297±149 (black hole)[6] M☉ |
| Size | 108,000 ly (33,113 pc)[7] |
| Apparent size (V) | 1.037′ × 0.809′[8] |
| Other designations | |
| NGC 1571, PGC 14971 | |
NGC 1570, mistakenly called NGC 1571, is a faint galaxy located in the southern constellation Caelum, the chisel. It has a blue magnitude of 13.2,[4] making it visible through a medium sized telescope. Based on a redshift of z = 0.014760,[2] the object is estimated to be 198 million light years (60.9 megaparsecs) away from the Local Group.[3] It appears to be receding with a heliocentric radial velocity of 4,392 km/s.[2]
NGC 1570 has a galaxy morphological classification of S0,[5] indicating that it is a lenticular galaxy. It has also been catalogued as a peculiar elliptical galaxy. The central black hole has a mass 297 times that of the Sun.[9] It is estimated to be 8.9 billion years old, younger than the Milky Way. The average iron abundance of the galaxy is 135% that of the Sun's. NGC 1570 is said to be round in shape, making it more likely to be an elliptical galaxy.[10]
The galaxy was first discovered by Sir John Herschel in November 1835. A month later, he observed NGC 1570 again and mistakenly called it NGC 1571 due to imprecise coordinates. NGC 1570 is part of a small galaxy group called LDC 302.[3] It is the brightest member.
References
- ↑ 1.0 1.1 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Paturel, G.; Dubois, P.; Petit, C.; Woelfel, F. (2002). "Comparison LEDA/SIMBAD octobre 2002. Catalogue to be published in 2003.". LEDA: 0. Bibcode: 2002LEDA.........0P.
- ↑ 3.0 3.1 3.2 3.3 Crook, Aidan C.; Huchra, John P.; Martimbeau, Nathalie; Masters, Karen L.; Jarrett, Tom; Macri, Lucas M. (February 2007). "Groups of Galaxies in the Two Micron All Sky Redshift Survey". The Astrophysical Journal 655 (2): 790–813. doi:10.1086/510201. ISSN 0004-637X. Bibcode: 2007ApJ...655..790C.
- ↑ 4.0 4.1 Lauberts, Andris; Valentijn, Edwin A. (1989). The surface photometry catalogue of the ESO-Uppsala galaxies. Bibcode: 1989spce.book.....L.
- ↑ 5.0 5.1 Lauberts, A. (1982). ESO/Uppsala survey of the ESO(B) atlas. Bibcode: 1982euse.book.....L.
- ↑ Caramete, L. I.; Biermann, P. L. (October 2010). "The mass function of nearby black hole candidates". Astronomy and Astrophysics 521: A55. doi:10.1051/0004-6361/200913146. ISSN 0004-6361. Bibcode: 2010A&A...521A..55C.
- ↑ Casasola, V.; Bettoni, D.; Galletta, G. (16 July 2004). "The gas content of peculiar galaxies: Strongly interacting systems". Astronomy and Astrophysics 422 (3): 941–950. doi:10.1051/0004-6361:20040283. ISSN 0004-6361. Bibcode: 2004A&A...422..941C.
- ↑ Skrutskie, M. F.; Cutri, R. M.; Stiening, R.; Weinberg, M. D.; Schneider, S.; Carpenter, J. M.; Beichman, C.; Capps, R. et al. (February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal 131 (2): 1163–1183. doi:10.1086/498708. ISSN 0004-6256. Bibcode: 2006AJ....131.1163S.
- ↑ Longhetti, M.; Rampazzo, R.; Bressan, A.; Chiosi, C. (June 1998). "Star formation history of early-type galaxies in low density environments". Astronomy and Astrophysics Supplement Series 130 (2): 251–265. doi:10.1051/aas:1998410. ISSN 0365-0138. Bibcode: 1998A&AS..130..251L.
- ↑ Sinnott, Roger W. (1988). NGC 2000.0: The Complete New General Catalogue and Index Catalogues of Nebulae and Star Clusters by J. L. E. Dreyer. Bibcode: 1988cngc.book.....S.
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