4C +41.26
Galaxy in the constellation Canes Venatici
From Wikipedia, the free encyclopedia
4C +41.26 known as PGC 2174167, is a massive elliptical galaxy of type E[1] located in the constellation of Canes Venatici. Its redshift is 0.228324, estimating the galaxy to be located 3 billion light years away from Earth.[2] It is the brightest cluster galaxy of Abell 1763 (ACO 1763).[3][4]
| 4C +41.26 | |
|---|---|
4C +41.26 captured by SDSS | |
| Observation data (J2000.0 epoch) | |
| Constellation | Canes Venatici |
| Right ascension | 13h 35m 20.095s |
| Declination | +41d 00m 04.13s |
| Redshift | 0.228324 |
| Heliocentric radial velocity | 68,450 km/s |
| Distance | 3.15 Gly (965.8 Mpc) |
| Group or cluster | Abell 1763 |
| Apparent magnitude (V) | 0.033 |
| Apparent magnitude (B) | 0.025 |
| Surface brightness | 16.0 |
| Characteristics | |
| Type | BrClG |
| Size | 862,300 light-years (264.4 kiloparsecs) |
| Apparent size (V) | 0.24' x 0.19' |
| Other designations | |
| B3 1333+412, PGC 2174167, TXS 1333+412, RX J1335.2+410, OGC 0110, 7C 1333+4115, 2MASX J13352009+4100041, NVSS J133519+410004 | |
Characteristics
4C +41.26 is one of the largest galaxies. Spanning at least 862,300 light-years across in diameter, it is classified as a Type-cD galaxy.[5] Not to mention, the galaxy has a high line-of-sight peculiar velocity reaching up to vpec ~ 650 km s−1. It has an active galactic nucleus, containing a powerful P1.4 ~ 1026 W Hz−1 bended double-lobed radio source, suggesting 4C +41.26 is likely shaped through its relative bulk intracluster medium (ICM) flow caused by one or several galaxy mergers.[6][7] The galaxy is estimated to have span MK = −25.7 to −27.8 mag, with the cluster halo masses of M500 up to 1.7×1015 M☉.[8]
4C +41.26 is part of the rich galaxy cluster[9] with at least 181 identified galaxy members, fitted through the integrated spectral energy distributions (SEDs)[10] utilized with a set of templates built with GRASIL 3d model,[11] by astronomers.[12] The members in the cluster consists of elliptical, spiral, starburst, and poststarburst galaxies.[13] It is suggested according to observations from Spitzler MIPS Data, researchers have found traces of increased starburst activity in filament galaxies inside ACO 1763.[9]
The cluster hosts two galaxy filaments which stretches towards another neighboring galaxy cluster, Abell 1770 (ACO 1770) located ~ 13 Mpc away. The intracluster gas of ACO 1770 is elongated in the same direction, as indicated by its X-ray morphology. As the cluster is fed by the filaments, it causes 4C +41.26 to be displaced from its original location from center of the cluster (0.1 Mpc off the X-ray peak emission) by the subcluster-cluster collisions and pressure of the intracluster gas. This results the galaxy falling towards Abell 1770.[14]