|Observation data (J2000 epoch)|
|Right ascension||13h 29m 59.6s|
|Declination||+47° 15′ 58″|
|Redshift||465 ± 10 km/s|
|Distance||25 ± 3 Mly (7.7 ± 1.0 Mpc)|
|Type||Amorphous or SB0 pec|
|Apparent dimensions (V)||5′.8 × 4′.6|
|Apparent magnitude (V)||10.5|
|Messier 51b, UGC 8494, PGC 47413, Arp 85|
NGC 5195 (also known as Messier 51b or M51b) is a dwarf galaxy that is interacting with the Whirlpool Galaxy (also known as M51a or NGC 5194). Both galaxies are located approximately 25 million light-years away in the constellation Canes Venatici. Together, the two galaxies are one of the most famous interacting galaxy pairs.
Interaction with the Whirlpool Galaxy
NGC 5195 and the Whirlpool Galaxy comprise one of the most noted interacting galaxy pairs in astronomy. The two galaxies are listed in the Atlas of Peculiar Galaxies as one of several prominent examples of a spiral galaxy with a companion galaxy. The system was also the subject of very early theoretical investigations into galaxy interactions. The two galaxies are connected by a dust-rich tidal bridge. The dust in this tidal bridge can be seen silhouetted against the center of NGC 5195. This demonstrates that NGC 5195 appears to lie behind the Whirlpool Galaxy. The encounter has significantly enhanced the spiral structure of M51.
In January 2016, BBC science reporter Jonathan Webb said, "Astronomers have spotted two huge waves of gas being 'burped' by the black hole at the heart of a nearby galaxy. The swathes of hot gas, detected in X-ray images from Nasa's Chandra space telescope, appear to be sweeping cooler hydrogen gas ahead of them. This vast, rippling belch is taking place in NGC 5195 - a small, neglected sibling of the 'Whirlpool Galaxy', 26 million light years away. That makes it one of the closest black holes blasting gas in this way". He added, "The findings, presented at the 227th meeting of the American Astronomical Society (AAS) in Florida, are a dramatic example of 'feedback' between a supermassive black hole and its host galaxy". Webb's report cited Marie Machacek, co-author of the study from the Harvard–Smithsonian Center for Astrophysics (CFA), as saying, "We think that feedback keeps galaxies from becoming too large […] But at the same time, it can be responsible for how some stars form. This shows that black holes can create, not just destroy."
As a consequence of the gravitational interaction with the Whirlpool Galaxy, NGC 5195 is highly distorted. Classification of its morphology is difficult, as it is sometimes identified as a lenticular galaxy or as an amorphous or irregular galaxy. It has been described as falling outside the standard morphological classification system.
Supernova 1945A is the only supernova that has been detected within NGC 5195. The supernova was found 10″ northwest of the nucleus on April 6, 1945 by Milton L. Humason using the 100-inch (2.5 m) telescope at Mount Wilson Observatory. The supernova, classified as a Type I supernova, reached a peak apparent magnitude of 14.0.
|Wikimedia Commons has media related to Whirlpool Galaxy.|
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- "NASA/IPAC Extragalactic Database". Results for extended name search on NGC 5195. Retrieved 2006-12-07.
- J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". Astrophysical Journal. 546 (2): 681–693. arXiv:. Bibcode:2001ApJ...546..681T. doi:10.1086/318301.
- A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Washington, D.C.: Carnegie Institution of Washington. ISBN 0-87279-667-1.
- "SEDS: NGC 5195". Retrieved 2007-10-13.
- H. Arp (1966). "Atlas of Peculiar Galaxies". Astrophysical Journal Supplement. 14: 1–20. Bibcode:1966ApJS...14....1A. doi:10.1086/190147.
- A. Toomre; J. Toomre (1972). "Galactic Bridges and Tails". Astrophysical Journal. 178: 623–666. Bibcode:1972ApJ...178..623T. doi:10.1086/151823.
- Webb, Jonathan (5 January 2016). "Black hole caught 'burping' galactic gas supply". BBC News Online. Retrieved 6 January 2016.
- M. L. Humason (1945). "Supernova in NGC 5195". Publications of the Astronomical Society of the Pacific. 57: 174–175. Bibcode:1945PASP...57..174H. doi:10.1086/125712.