| NGC 5775 | |
|---|---|
Hubble Space Telescope image of NGC 5775, taken using the Advanced Camera for Surveys
| |
| Observation data (J2000 epoch) | |
| Constellation | Virgo |
| Right ascension | 14h53m 57.653s[1] |
| Declination | +03° 32′ 40.10″[1] |
| Redshift | 0.005607[2] |
| Heliocentric radial velocity | 1681[2] |
| Distance | 66.33 ± 13.31 Mly (20.338 ± 4.081 Mpc)[2] |
| Grouporcluster | Virgo Cluster |
| Apparent magnitude (V) | 11.34 |
| Apparent magnitude (B) | 13.0 |
| Characteristics | |
| Type | Sbc[3] |
| Apparent size (V) | 3.967' × 0.793'[1] |
| Other designations | |
| UGC 9579, MCG+01-38-014, PGC 53247[3] | |
NGC 5775 is a spiral galaxy, a member of the Virgo Cluster, that lies at a distance of about 70 million light-years. Although the spiral is tilted away from us, with only a thin sliver in view, such a perspective can be advantageous for astronomers. For instance, astronomers have previously used the high inclination of this spiral to study the properties of the halo of hot gas[4] that is visible when the galaxy is observed at X-ray wavelengths. It is a member of the NGC 5775 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.[5]
One supernova has been observed in NGC 5775: SN 1996ae (type IIn, mag. 16.5).[6]
NGC 5775 is interacting with the nearby galaxy NGC 5774 in the form of two connecting H I bridges through which the gas is travelling from NGC 5774 to NGC 5775.[7] Faint optical emission as well as radio continuum emission are also present along the bridges.[8] It is possible that star formation is occurring between the galaxies.[7]
This system may be in the early stages of a merger.[8]
Media related to NGC 5775 at Wikimedia Commons
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