HST image of NGC 326
|Observation data (J2000 epoch)|
|Right ascension||00h 58m 22.7s|
|Declination||+26° 51′ 55″|
|Helio radial velocity||14,210 km/s|
|Apparent magnitude (V)||14.33|
|Apparent size (V)||1.4' × 1.4'|
|UGC 00601, CGCG 480-026, MCG +04-03-025, 4C +26.03, B2 0055+26, PGC 3326, PKS B0055+265, TXS 0055+265.|
NGC 326 is a dumbbell galaxy in the constellation Pisces. It was discovered on August 24, 1865 by Heinrich d'Arrest. It was described by Dreyer as "faint, a little extended, 9th or 10th magnitude star to southeast."
X-shaped (or "winged") radio galaxies are a class of extragalactic radio source that exhibit two, low-surface-brightness radio lobes (the "wings") oriented at an angle to the active, or high-surface-brightness, lobes. Both sets of lobes pass symmetrically through the center of the elliptical galaxy that is the source of the lobes, giving the radio galaxy an X-shaped morphology as seen on radio maps.
Study of the galaxy
NGC 326 is a radio galaxy; in fact, it is one of the most prominent X-shaped galaxies ever observed. Several studies have been conducted to try to explain its morphology through either fluid motion or reorientation of the jet axis. The Chandra X-ray Observatory examined the emissions of the galaxy. The study revealed several features, including a high-temperature front that might indicate a shock, high-temperate knots around the rim of the radio emission, and a cavity associated with the eastern wing.
- "NASA/IPAC Extragalactic Database". Results for NGC 0326. Retrieved September 2, 2016.
- "New General Catalog Objects: NGC 300 - 349". Cseligman. Retrieved October 30, 2016.
- "Study of X-Shaped Radio Galaxy NGC 326 Shows Outburst History and Active Galactic Nucleus Feedback". Scitechdaily. February 6, 2012. Retrieved October 30, 2016.
- Hodges-Kluck, Edmund; Reynolds, Christopher S (December 12, 2011). "A Chandra Study of the Radio Galaxy NGC 326: Wings, Outburst History, and AGN Feedback". The Astrophysical Journal. 746 (2): 167. arXiv:1112.2707. Bibcode:2012ApJ...746..167H. doi:10.1088/0004-637X/746/2/167.
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