Right ascension 03 19 48.1 Type cD;pec;NLRG Magnitude 12.6 Apparent magnitude (V) 12.6 | Declination +41° 30′ 42″ Apparent size (V) 2′.2 × 1′.7 Constellation Perseus | |
 | ||
Redshift 5264 ± 11 km/s
z=0.017559 Distance 222 million light-years
68.2 Mpc Similar Perseus cluster, NGC 1261, NGC 4236, NGC 5005, NGC 2775 | ||
Hubble active galaxy ngc 1275 720p
NGC 1275 (also known as Perseus A or Caldwell 24) is a type 1.5 Seyfert galaxy located around 237 million light-years away in the direction of the constellation Perseus. NGC 1275 corresponds to the radio galaxy Perseus A and is situated near the center of the large Perseus Cluster of galaxies.
Contents
- Hubble active galaxy ngc 1275 720p
- Hubble hd zoom into galaxy ngc 1275 within the constellation perseus
- Dynamics
- References
Hubble hd zoom into galaxy ngc 1275 within the constellation perseus
Dynamics
NGC 1275 consists of two galaxies, a central type-cD galaxy in the Perseus Cluster, and a so-called "high velocity system" (HVS) which lies in front of it. The HVS is moving at 3000 km/s towards the dominant system, and is believed to be merging with the Perseus Cluster. The HVS is not affecting the cD galaxy as it lies at least 200 thousand light years from it.; however tidal interactions are disrupting it and ram-pressure stripping produced by its interaction with the intracluster medium of Perseus is stripping its gas as well as producing large amounts of star formation within it
The central cluster galaxy contains a massive network of spectral line emitting filaments, which apparently are being dragged out by rising bubbles of relativistic plasma generated by the central active galactic nucleus. Long gaseous filaments made up of threads of gas stretch out beyond the galaxy, into the multimillion-degree, X-ray–emitting gas that fills the cluster. The amount of gas contained in a typical thread is approximately one million times the mass of the Sun. They are only 200 light-years wide, are often very straight, and extend for up to 20,000 light-years.
The existence of the filaments poses a problem. As they are much cooler than the surrounding intergalactic cloud, it is unclear how they have existed for such a long time, or why they have not warmed, dissipated or collapsed to form stars. One possibility is that weak magnetic fields (about one-ten-thousandth the strength of Earth’s field) exert enough force on the ions within the threads to keep them together.
NGC 1275 contains 13 billion solar masses of molecular hydrogen that seems to be infalling from Perseus' intracluster medium in a cooling flow, both feeding its active nucleus and fueling significant amounts of star formation
A supermassive black hole with a mass 340 million times that the Sun may be present in NGC 1275's center.