Andromeda galaxy data

Andromeda galaxy

An important member of this galaxy group, also called M3 1.

Andromeda galaxy is a huge spiral galaxy in Andromeda, visible to the naked eye, with an apparent magnitude of 3.5. Is a close neighbor of our galaxy. Apparent magnitude 3.5. Visible to the naked eye, like a faint oval spot. Astronomers discovered it a long time ago, and messier numbered it August 3rd, 1764.

Andromeda galaxy is the largest galaxy nearest to our galaxy. It is generally believed that the appearance of the Milky Way galaxy is very similar to that of Andromeda galaxy, and both dominate the local galaxy group. The diffuse light of Andromeda galaxy is composed of hundreds of billions of star members. The bright stars around the Andromeda galaxy image are actually stars in our galaxy, which are much closer than the background objects. Andromeda galaxy is also called M3 1 because it is the No.31dispersoid in the list of the famous messier cluster nebulae. M3 1 is quite far away, and its light will take 2 million years to reach the earth. The stars in the nebula can be divided into about 20 communities, which means that they may come from smaller galaxies "swallowed up" by Andromeda.

The number in messier catalog is M3 1, and the editor in the new catalog of nebula clusters is NGC224, which was previously called Andromeda Nebula.

The diameter of Andromeda galaxy is 50,000 parsec (160,000 light years), which is twice the diameter of the Milky Way. It is the largest galaxy in this cluster, about 2.2 million light years away. Andromeda galaxy has many similarities with the Milky Way. A comparative study of them can provide important clues for understanding the movement, structure and evolution of the Milky Way.

1786, F.W. Herschel first listed it as a nebula that can be decomposed into stars. 1924, Hubble recognized Cepheid variable on the spiral arm of Andromeda galaxy on photographic film, and calculated the distance according to the period-luminosity relationship, confirming that it is a star system outside the Milky Way. 1944, Budd distinguished the celestial bodies in the core of Andromeda galaxy and determined the clusters and stars in it.

M3 1 occupies an important position in the history of astronomy. 1786, Herschel was the first to include it in a nebula that can be decomposed into stars. 1924, Hubble recognized Cepheid variable on M3 1 spiral arm on photographic film, and calculated the distance according to the period-luminosity relationship, confirming that it is a star system outside the Milky Way. The modern distance is 670,000 parsec (2.2 million light years). Its diameter is 50,000 parsec (654.38+0.6 million light years), twice that of the Milky Way and the largest in this galaxy group. In 1944, Budd determined the core celestial bodies of M3/kloc-0, determined the clusters and stars in them, and pointed out the spatial distribution of the clusters and the phase of the Milky Way. On the spiral arm of M3 1 is the extreme constellation I, including O-B star, bright Supergiant star, OB star and ionized hydrogen region. Classical Cepheid Variables, novas, Red Giant Stars, Planetary Nebulae and other diskpopulation celestial bodies were observed on the silver disk. In the central area, there is Cepheid Variable Star II. The globular clusters of halo members can reach 30,000 parsec from the main plane of the galaxy. In recent years, it is also found that the heavy element content of M3 1 member gradually increases from the periphery to the center. This phenomenon shows that the process of heavy elements in interstellar matter caused by stellar ejection is much more frequent in the central region of the galaxy than in the peripheral region. 19 14, pease found that M3 1 has rotating motion. Starting from 1939, through the research of babcock and others, the rotation speed curve from the center to the edge was measured, and the mass of the Milky Way was known from this. According to the current estimation, the mass of M3 1 is not less than 3.1×1kloc-0/solar mass, which is more than twice that of the Milky Way and the largest one in this galaxy group. M3 1 has a star-like core with a diameter of only 25 light years, and its mass is equivalent to 107 suns, that is, 1500 stars gather in a cubic parsec. The infrared radiation of the star-like core is very strong, which is about equal to the radiation of the whole core area of the Milky Way. But the radio there is only 1/20 of Silver Heart Radio. Radio observation shows that neutral hydrogen is mostly concentrated in a wide ring with a radius of 10 kiloparsec. The content of hydrogen is 1% of the total mass, which is less than 1.4 ~ 7% of the Milky Way. It can be considered that most of the gases in M3 1 have formed stars. M3 1 is similar to the Milky Way. A comparative study of the two can provide important clues for understanding the movement, structure and evolution of the Milky Way.

Because humans are in the Milky Way, it is impossible to observe the whole picture of the Milky Way, but astronomers imagine that the Milky Way is also a spiral galaxy similar to Andromeda. Andromeda, the Milky Way and more than 30 other galaxies * * * form a larger galaxy group-the local galaxy group.

Our Milky Way and Andromeda galaxy are approaching each other, and they may collide in about 3 billion years, and in the process of fusion, they will temporarily form a bright and complex hybrid galaxy. A series of stars will be scattered, and most of the free gas in the galaxy will be compressed to produce new stars. After several billion years, the spiral arms of galaxies will disappear, and two spiral galaxies will merge into a huge elliptical galaxy.

But the collision and fusion of the two galaxies will only happen in the distant future, and human beings need not worry about it.

The giant spiral galaxy in Andromeda (M3 1). The celestial coordinates of 1950.0 epoch are right ascension 0400 and declination +4 1 00. The apparent magnitude m is 3.5. Visible to the naked eye, it looks like a faint oval spot. In the photo, it appears as an Sb-type galaxy with an inclination of 77 (see classification of galaxies), with a size of160 ′× 40 ′, and two thin and tight spiral arms extending from the bright nucleus, with a range of 245 ′× 75 ′. The serial number in the messier catalog is M3 1, and the serial number in the new catalog of nebula clusters is NGC224, which is called Andromeda Nebula and now Andromeda Galaxy. In 1786, F.W. Herschel was the first to list it in a nebula that can be decomposed into stars. 1924, Hubble recognized Cepheid variable on M3 1 spiral arm on photographic film, and calculated the distance according to the period-luminosity relationship, confirming that it is a star system outside the Milky Way. The modern distance is 670,000 parsec (2.2 million light years). Its diameter is 50,000 parsec (654.38+0.6 million light years), twice that of the Milky Way and the largest in this galaxy group. In 1944, Budd determined the core celestial bodies of M3/kloc-0, and determined the star clusters and stars in it, and pointed out that the spatial distribution of star clusters was similar to that of the Milky Way. On the spiral arm of M3 1 is the extreme star group I, including O-B star (see stellar spectral classification), bright Supergiant star, OB star concordance and ionized hydrogen region. Diskpopulation celestial bodies such as classical Cepheid variable stars, nova, red giant stars and planetary nebulae were observed on the silver disk. In the central area, there is Cepheid Variable Star II. The globular clusters of halo members can reach 30,000 parsec from the main plane of the galaxy. In recent years, it has also been found that the content of heavy elements in M3 1 member gradually increases from the periphery to the center. This phenomenon shows that the process of heavy elements in interstellar matter caused by stellar ejection is much more frequent in the central region of the galaxy than in the peripheral region. 19 14, pease found that M3 1 has rotating motion. Since 1939, through the research of H.D. babcock and others, the rotation speed curve from the center to the edge has been measured, and the mass of the Milky Way has been known from this. According to current estimates, the mass of M3 1 is not less than 3. 1× 10, which is more than twice that of the Milky Way and the largest in this galaxy group.

The absolute magnitude of M3 1, M =-2 1. 1, is the brightest member of this galaxy group. According to the surface brightness distribution, M3 1 has a star-like core in its center, with an absolute magnitude of M =- 1 1, a diameter of only 8 parsec (25 light years) and a mass equivalent to 10 sun, that is, 1500 stars are gathered in a cubic parsec. The infrared radiation of the star-like core is very strong, which is about equal to the radiation of the whole core area of the Milky Way. But the radio there is only 1/20 of Silver Heart Radio. Radio observation shows that neutral hydrogen is mostly concentrated in a wide ring with a radius of 10 kiloparsec. The content of hydrogen is 1% of the total mass, which is less than 1.4 ~ 7% of the Milky Way. It can be considered that most of the gases in M3 1 have formed stars. M3 1 has two dwarf galaxies ──M32(NGC22 1) and NGC 205 \\, which are morphologically classified as E2 and E5p respectively. The latter is a special elliptical galaxy with a large number of young blue stars. In this galaxy group, M3 1 and other galaxies-NGC147, NGC 185, M33 (NGC598) and ι, and II, and III, and IV-form the so-called Andromeda galaxy subgroup.

M3 1 is similar to the Milky Way. A comparative study of them can provide important clues for understanding the movement, structure and evolution of the Milky Way.