NGC 4293
| NGC 4293 | |
|---|---|
| File:Ngc4293-hst-606.png
Partial image of NGC 4293 taken by the Hubble Space Telescope
|
|
| Observation data (J2000 epoch) | |
| Constellation | Coma Berenices |
| Right ascension | 12h 21m 12.891s[1] |
| Declination | +18° 22′ 56.64″[1] |
| Redshift | 0.002977[2] |
| Helio radial velocity | 893[3] |
| Distance | 54 Mly (16.5 Mpc)[4] |
| Group or cluster | Virgo Cluster |
| Type | (R)SB(s)0/a[5] |
| Apparent dimensions (V) | 5.293′ × 1.800′[1] |
| Apparent magnitude (V) | 10.4[6] |
| Other designations | |
| 2MASX J12211289+1822566, IRAS 12186+1839, LEDA 39907, UGC 7405, UZC J122112.6+182256, Z 99-23.[7] | |
NGC 4293 is the New General Catalogue identifier for a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered by English astronomer William Herschel on March 14, 1784, who described it as "large, extended, resolvable, 6 or 7′ long". This galaxy is positioned to the north-northwest of the star 11 Comae Berenices and is a member of the Virgo Cluster of galaxies.[6] It is assumed to lie at the same distance as the Virgo Cluster itself: around 54 million light years away.[4] The galaxy spans an apparent area of 5.3 × 3.1 arc minutes.[6]
The morphological classification of NGC 4293 is (R)SB(s)0/a, with the SB0/a indicating this has just distinguishable tightly wound spiral arms with a bar structure at the nucleus. An '(s)' notation means that this galaxy does not have a ring-like structure around the nucleus.[5][8] Star formation within NGC 4293 is only taking place within a confined region at the center of the galaxy.[9] The outer stellar disk of the galaxy appears disturbed, suggesting some form of gravitational interaction.[10]
This is a common type of active galaxy known as a LINER, which means that the optical spectrum is dominated by emission lines from gases in low energy ionization states. The activity may be the result of a supermassive black hole (SMBH) in the nucleus that is undergoing a low rate of matter accretion. The estimated mass of such an SMBH is 5.9×107 M⊙.[11] Radio emission from thermal activity has been detected from the proximity of this object.[12]
References
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