B2 0206+35
Radio galaxy in the constellation of Triangulum
From Wikipedia, the free encyclopedia
B2 0206+35 known as UGC 1651 or 4C 35.03, is a low-luminosity Fanaroff Riley class I radio galaxy[1] located in the constellation of Triangulum. It's redshift is (z) 0.037 and it is a member of a galaxy cluster, Zwicky 0216.0+3625.[2][3]
| B2 0206+35 | |
|---|---|
The radio galaxy B2 0206+35. | |
| Observation data (J2000 epoch) | |
| Constellation | Triangulum |
| Right ascension | 02h 09m 38.589s |
| Declination | +35° 47′ 50.34″ |
| Redshift | 0.036572 |
| Heliocentric radial velocity | 10,964 km/s |
| Distance | 534 Mly |
| Apparent magnitude (V) | 13.0 |
| Apparent magnitude (B) | 14.9 |
| Characteristics | |
| Type | FR I |
| Notable features | Radio galaxy |
| Other designations | |
| UGC 1651, PGC 8249, OHIO D 311, 4C 35.03, ZW V 191, BWE 0206+3533, Cul 0206+355 | |
Description
B2 0206+35 is classified as an elliptical galaxy[4] or alternatively, a dumbbell galaxy.[5] It is described as having a distorted appearance with a tidal tail and a dust lane running through its center, indicating the galaxy is interacting with a nearby galaxy located 31 kiloparsecs away at a position angle of 110°.[6]
The galaxy has two-sided radio jets found emerging straight out from the nucleus. They measure 40 kiloparsecs (kpc) northwest to southeast, with observations showing they are embedded in a radio emission halo of low surface brightness.[4][6][7] Very Large Array (VLA) resolved imaging shows the galaxy has a main jet and a counter jet. The main jet is centrally peaked, narrow with a bright base while the counter jet is wider with a limb-brighten structure, found to be the brightest between 2.5 and 6 arcseconds from the nucleus.[8]
The nucleus of the galaxy itself is described as a bright core with a flat spectrum.[9] In addition, the galaxy has radio lobes that are depicted as overlapping and circular in cross-section. One of the lobes located northwest has a circular edge found projecting beyond the emission boundaries, while the other lobe is located within the outer boundary of the source.[10]
Radio mapping by the VLA at 5 GHz, showed both lobes are polarized. Based on results, the northwest lobe has a mean fractional polarization percentage of 23.2% while the mean fractional polarization of the southeast lobe is 27.5%. Because of the difference between frequencies, this might be caused by Faraday depolarization. The polarization in the core is estimated to be either 5.6% or 5.3% according to Capetti who measured it at 1.4 GHz frequencies.[11] A magnetic field surrounds the galaxy along the line of sight, being associated with the largest amplitude band located in the lobe's outer parts.[12]