One possible explanation is that NGC 474 interacts with a. One possible explanation is that NGC 474 interacts with a. NGC 474 is located at a distance of about 100 million light years in the constellation of Pisces. The image below is an image of NGC 474 from the Digitised Sky Survey 2 (DSS2 – see imprint) taken in the red channel.
Arp 227 floats within the boundaries of the constellation Pisces and consists of the two galaxies that stand out on the left: the strange shell galaxy NGC 474 and its blue, spiral-armed neighbour NGC 470. Alternatively, the shells could look like ripples in a pond, where the ongoing collision with the spiral galaxy directly above NGC 474 is causing density waves to ripple through the galactic giant.
Who discovered NGC 474?
The galaxy NGC 474 is an example of a galaxy that has formed a conspicuous ring structure from stars dispersed by gravitational influences due to collisions with other, smaller galaxies. NGC 474 has an extent of about 250,000 light years and lies about 100 million light years away in the direction of the constellation of Pisces. Although the number of transients in NGC 4449 is small (probably the sample is insufficient), the overall properties of the transient X-ray sources (fraction of HMXBs and SSSs and their luminosity) are consistent with those of the other Magellanic galaxies. Regardless of the actual cause, the image presented dramatically underscores the growing consensus that at least some elliptical galaxies have formed in the recent past, and that the outer halos of most large galaxies are not truly smooth, but have complex structures formed by frequent interactions with – and accretions from – smaller galaxies nearby.
What kind of galaxy is NGC 7479?
NGC 7479 – Barred Spiral Galaxy in Pegasus is classified as a Barred Spiral (Bbc) according to the Hubble and de Vaucouleurs morphological classification. NGC 7479 is a classic barred spiral galaxy in the constellation Pegasus, with a small, bright active galactic core (Seyfert type) fed by gas flowing in along the barred structure. The spiral structure is also unusual in that the arms appear to rotate in the opposite direction to those in the visible and near IR when observed in the radio spectrum. Star formation is rekindled by galactic collisions, and indeed NGC 7479 is experiencing starburst activity, with many bright young stars visible in the spiral arms and in the disk.
What is NGC 428?
The image below is an image of NGC 428 from the Digitised Sky Survey 2 (DSS2 – see imprint), taken in the red channel. Ultimately, cataclysmic events like this are usually triggered when one galaxy gets too close to another and they interact or merge. There also appears to be a significant amount of star formation in NGC 428 – another telltale sign of a merger. The spiral structure of NGC 428 is distorted and deformed, probably due to a collision between two galaxies, and it is still responsible for a healthy amount of star formation – another telltale sign of a merger between two galaxies.
NGC 428 is a barred spiral galaxy in the constellation Cetus (The Sea Monster) whose spiral structure is distorted and deformed, possibly due to the collision of two galaxies.
Which of the following is a major difference between elliptical galaxies and spiral galaxies?
Astronomers have identified more spiral gal axies than elliptical galaxies, but this is simply because spirals are easier to spot. In fact, however, irregular and especially (dwarf) elliptical galaxies probably dominate the universe, but are too faint to be easily seen. At the beginning of the 20th century, Edwin Hubble carried out an extensive study of galaxies and classified them according to their shape and structure. Galaxies classified as E0 appear to be almost perfect circles (remember, a circle is an ellipse), while those classified as E7 appear to be much longer than they are wide.
The so-called Hubble sequence or Hubble tuning fork orders the galaxies according to their shape.