NGC 3859

NGC 3859 is a spiral galaxy[2] located about 295 million light-years away in the constellation Leo.[3] It was discovered by astronomer Édouard Stephan on March 23, 1884.[4] The galaxy is a member of the Leo Cluster.[5][6]

NGC 3859
SDSS image of NGC 3859.
Observation data (J2000 epoch)
ConstellationLeo
Right ascension 11h 44m 52.2s[1]
Declination19° 27′ 15″[1]
Redshift0.018239[1]
Helio radial velocity5468 km/s[1]
Distance295 Mly (90.4 Mpc)[1]
Group or clusterLeo Cluster
Apparent magnitude (V)14.76[1]
Characteristics
TypeS? pec[1]
Size~135,000 ly (41.5 kpc) (estimated)[1]
Apparent size (V)1.2 x 0.3[1]
Other designations
CGCG 97-122, IRAS 11423+1943, MCG 3-30-91, PGC 36582, UGC 6721[1]

Physical characteristics

Deep imaging of NGC 3859 by Yagi et al.have revealed a distorted faint halo which is elongated toward the northeast along the major axis of the galaxy. On the southwestern side of the galaxy, the halo is extends about ~33,000 ly (10 kpc) above the disk of the galaxy. To the north, there is a small dwarf galaxy which is possibly an interacting companion. A part of the extended halo of NGC 3859 may be the result of an interaction between the dwarf and NGC 3859.[5]

Hα emission

The bright disk Hα emission in the disk together with the very blue color of the galaxy and the emission line dominated nuclear spectrum indicate that NGC 3859 is a starburst galaxy. The morphology of the Hα emission of NGC 3859 is peculiar is characterized by two narrow spurs which extend to the northwest and the southeast from the galaxy disk and whose widths are ~6,500 ly (2 kpc) and ~33,000 ly (10 kpc) respectively. The morphology and size of the two spurs of NGC 3859 are quite similar to the Hα nebula and extended ionized gas cloud which suggest that the spurs originated in a starburst superbubble or superwind. The northern part of an Hα nebula of NGC 3859 seems to be flowing toward the northeast. Also, the two spurs of the galaxy also are bending in the same direction. These morphological characteristics suggest that the hot gas of the galaxy is being affected by ram pressure from the southwest. However, there is no indication of one-sided elongation of ionized gas within the galaxy. There is also no sharp cutoff at the southwest edge of the Hα nebula, and no extended part of the Hα emission out of the galaxy to the northeast, but shows an extension toward east-southeast. In addition, the northern faint flowing part of the nebular continuum is overlapped by the dwarf companion galaxy suggesting that this part of the Hα nebula could have been formed by a galaxy interaction rather than ram pressure. Therefore, ram pressure stripping may not be strong enough to create the overall structure of the extended ionized gas cloud (EIG) around NGC 3859.[5]

SN 2014U

On February 23, 2014, a type II supernova designated as SN 2014U was discovered in NGC 3859.[7][8][9]

gollark: Just download a JAR from the releases.
gollark: https://github.com/Vazkii/CMPDL
gollark: Or use CMPDL.
gollark: MultiMC has `add instance → import from ZIP`.
gollark: I think MultiMC has the ability to install from zips.

See also

References
  1. "NASA/IPAC Extragalactic Database". Results for NGC 3859. Retrieved 2018-07-19.
  2. "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2018-07-21.
  3. "Revised NGC Data for NGC 3859". spider.seds.org. Retrieved 2018-07-21.
  4. "New General Catalog Objects: NGC 3850 - 3899". cseligman.com. Retrieved 2018-07-17.
  5. Yagi, Masafumi; Yoshida, Michitoshi; Gavazzi, Giuseppe; Komiyama, Yutaka; Kashikawa, Nobunari; Sadanori Okamura (2017). "Extended Ionized Gas Clouds in the Abell 1367 Cluster". The Astrophysical Journal. 839 (1): 65. arXiv:1703.10301. Bibcode:2017ApJ...839...65Y. doi:10.3847/1538-4357/aa68e3. ISSN 0004-637X.
  6. "NGC 3859". Retrieved 2018-07-21.
  7. dbishopx@gmail.com. "Bright Supernovae - 2014". rochesterastronomy.org. Retrieved 2018-07-22.
  8. "SN 2014U | Transient Name Server". wis-tns.weizmann.ac.il. Retrieved 2018-07-22.
  9. "2014U - The Open Supernova Catalog". sne.space. Retrieved 2018-07-22.


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