Local Group of Galaxies
The MW subgroup has a linear size of about 140 kpc, and the radial velocity dispersion of galaxies in it is 68 km/s.
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| Subgroups of the Community Group |
The Andromeda nebula galaxy system, visible from the outside, is grouped around its main galaxy M31, containing the closest galaxies with high surface brightness M32 and M110, as well as fainter and more distant NGC147 and NGC185, very faint systems And I, And II, And III .
In the summer of 1998, two groups of observers(I.D. Karachentsev and V.E. Karachentseva; T. Armandroff, J. Davies and G. Jacoby) at least 3 more dwarf spheroidal galaxies were discovered - possibly distant members of the subgroup M31(one of these galaxies was discovered independently by both groups): Pegasus DEG (And VI), Cassiopea Dw and And V. The third largest galaxy in the Local Group, M33 (Triangulum), which may or may not be a distant gravitationally bound companion to M31, itself has a dwarf companion LGS 3.
Galaxies NGC3109, Antlia,Sextans A And Sextans B, apparently, form a separate subgroup with V r=+114+-12 km/s, which is located outside the so-called “zero Local Group distance” of 1.7 Mpc from the Local Group centroid (van den Bergh, 1999).
Other members cannot be assigned to any main subgroup and move completely isolated in the gravitational field of the members of giant groups. The substructures in the group are probably not stable. Observations and calculations suggest that the groups are very dynamic and have changed significantly in the past: the galaxies around the large elliptical galaxy Maffei 1 were likely once members of the group of our galaxy.
All of the above shows that the MG is not isolated, but is in gravitational interaction and exchange of members with the nearest surrounding groups of galaxies. Particularly noticeable is the interaction with:
| Galaxy | Alto. Name | RA (2000.0) | Dec (2000.0) | Type | V_r | Dist. | Diam. | V B tot | A B |
|---|---|---|---|---|---|---|---|---|---|
| WLM | DDO221 | 00:01:58 | -15:27:51 | IB(s)m IV-V | - 116 | 950 | 11.5x4.0 | 11.03 | 0.09 |
| IC 10 | UGC192 | 00:20:24 | +59:17:30 | IBM? | -344 | 660 | 6.3x5.1 | 11.80 | |
| Cetus | dSph | 775 | |||||||
| NGC 147 | DDO 3 | 00:33:12 | +48:30:29 | dE5 pec | -193 | 660 | 13.2x7.8 | 10.47 | 0.70 |
| And III | A0032+36 | 00:35:17 | +36:30:31 | dSph | 760 | 4.5x3.0 | 15.00 | 0.19 | |
| NGC 185 | UGC396 | 00:38:58 | +48:20:12 | dE3 pec + Sy | -202 | 620 | 11.7x10.0 | 10.10 | 0.78 |
| NGC205 | M 110 | 00:40:22 | +41:41:26 | E5 pec | - 241 | 725 | 21.9x11.0 | 8.92 | 0.14 |
| M32 | NGC 221 | 00:42:42 | +40:51:52 | E2 (cE2) | -205 | 725 | 8.7x6.5 | 9.03 | 0.31 |
| M31 | NGC 224 | 00:42:44 | +41:16:09 | SA(s)b Liner | -300 | 725 | 190x60 | 4.36 | 0.10 |
| And I | A0043+37 | 00:45:44 | +38:00:23 | dE3 pec ? | 810 | 2.5x2.5 | 13.6 | 0.20 | |
| SMC | NGC292 | 00:52:45 | -72:49:43 | SB(s)m pec | +158 | 58 | 320x185 | 2.7 | 0.17 |
| Scl dw Irr | E349-G31 | 00:08:13 | -34:34:42 | dIBm | +207 | 1.1x0.9 | 15.48 | ||
| Scl dSph | E351-G30 | 01:00:09 | -33:42:33 | dE3 pec | +110 | 84 | 39.8x30.9 | 10.50 | |
| LGS 3 | Psc dw | 01:03:53 | +21:53:05 | dIr/dSph | -277 | 810 | 2x2 | 18.00 | 0.10 |
| IC1613 | DDO 8 | 01:04:54 | +02:08:00 | IAB(s)m V | -234 | 720 | 16.2x14.5 | 9.88 | 0.02 |
| And V | 01:10:17 | +47:37:41 | dSph | 810 | |||||
| And II | 01:16:11 | +33:21:43 | E? | 680 | 3.6x2.52 | 13.5 | 0.14 | ||
| M33 | NGC 598 | 01:33:51 | +30:39:37 | SA(s)cd II-III | -179 | 795 | 70.8x41.7 | 6.27 | 0.18 |
| Phe dw | E245-G07 | 01:51:06 | -44:26:41 | IAm | +56 | 417 | 4.9x4.1 | 13.07 | |
| For dw | E356-G04 | 02:39:59 | -34:26:57 | dE4 | +53 | 140 | 17.0x12.6 | 9.04 | |
| LMC | E056-G115 | 05:23:34 | -69:45:22 | SB(s)m | +278 | 55 | 645x550 | 0.9 | 0.25 |
| Car dw | E206-G220 | 06:41:37 | -50:57:58 | dE3 | +229 | 100 | 23.4x15.5 | 22.14 | 0.10 |
| Leo A | DDO 69 | 09:59:24 | +30:44:42 | IBm V | +20 | 690 | 5.1x3.1 | 12.92 | 0.07 |
| Sex B | DDO 70 | 10:00:00 | +05:19:42 | Im+ IV-V | +301 | 1370 | 5.1x3.5 | 11.85 | 0.05 |
| NGC 3109 | DDO 236 | 10:03:07 | -26:09:32 | SB(s)m | +403 | 1260 | 19.1x3.7 | 10.39 | 0.14 |
| Antlia | A1001-27 | 10:01.8* | -27:05* | dE3 | +361 | 1320 | 1 | ||
| Leo I | Regulus G. | 10:08:27 | +12:18:27 | dE3 | +168 | 270 | 9.8x7.4 | 11.8 | 0.09 |
| Sex A | DDO 75 | 10:11:06 | -04:42:28 | IBm+ V | +324 | 1420 | 5.9x4.9 | 11.86 | 0.06 |
| Sex dw | 10:13:03 | -01:36:53 | dE3 | +230 | 87 | 0.07 | |||
| Leo II | DDO 93 | 11:13:29 | +22:09:17 | dE0 pec | +90 | 215 | 12.0x11.0 | 12.6 | 0.00 |
| GR 8 | DDO 155 | 12:58:39 | +14:13:02 | I'm V | +214 | 1700 | 1.1x1.0 | 14.68 | 0.04 |
| E269-G70 | 13:10.6* | -43:07* | -8 | ||||||
| IC 4247 | 13:24.0* | -30:06* | +274 | ||||||
| UMi dw | DDO 199 | 15:09:11 | +67:12:52 | dE4 | -209 | 60 | 30.2x19.1 | 11.9 | 0.04 |
| Dra dw | DDO 208 | 17:20:19 | +57:54:48 | dE0 pec | -281 | 76 | 35.5x24.4 | 10.9 | 0.08 |
| Milky Way | 17:45.6 | -28:56 | SAB(s)bc I-II ? | 0 | 10 | 30 | |||
| SagDEG | 18:55 | -30:30 | dE7 | 24 | |||||
Most galaxies are collected into certain associations - groups, clusters and superclusters. If we build a three-dimensional model of the part of the Universe known to us, it turns out that the distribution of galaxies resembles the structure of a honeycomb or a fishing net - relatively thin “walls” and “fibers” surround large “bubbles” of almost empty space, the so-called voids. Clusters of galaxies are “nodes” of this “grid”. The lowest level of association is the group. Typically, groups consist of a small (no more than 50) number of galaxies of all kinds and have a size from 1 to 2 Mpc. The mass of a group of galaxies, as a rule, does not exceed 13 solar masses, and the individual speed of galaxies in the group is approximately 150 km/s. Clusters are groups of galaxies larger than a group, although there is no clear distinction between these two classes. A cluster may include hundreds or tens of thousands of galaxies. There are many known galaxy clusters; Astronomers still use their catalog, compiled by J. Abel. In turn, clusters of galaxies unite into galactic superclusters. Back in the second half of the 50s of the last century, it was discovered that most of the brightest galaxies visible from Earth form an integral structure, in the center of which is a cluster in the constellation Virgo, and on its periphery is our Local Group of galaxies. This structure was called the Local Supercluster of Galaxies. Local supercluster covers an area in space several tens of megaparsecs in size, which is 10 times the size of the cluster in the constellation Virgo.
LOCAL GALAXIES GROUP is a collection of several dozen nearby galaxies surrounding our star system - the Milky Way galaxy. Members of the Local Group move relative to each other, but are connected by mutual gravity and therefore occupy a long time limited space about 6 million light years in size and exist separately from other similar groups of galaxies. All members of the Local Group are believed to have a common origin and have been coevolving for about 13 billion years.
The Local Group includes more than 50 galaxies. This number is constantly increasing with the discovery of new galaxies. The local group can be divided into several subgroups:
Milky Way Group consists of the giant spiral Milky Way galaxy and its 14 known satellites (as of 2005), which are dwarf and mostly irregular galaxies;
Andromeda group very similar to the Milky Way group: at the center of the group is the giant spiral galaxy Andromeda. Its 18 known (as of 2005) satellites are also mostly dwarf galaxies;
Triangle Group- the Triangulum galaxy and its possible satellites;
Other dwarf galaxies that cannot be classified into any of the above groups.
The diameter of the Local Group is about one megaparsec. The local group is part of a local supercluster - the Virgo supercluster, main role in which the Virgo cluster plays.
Milky Way- the galaxy in which ours is located solar system. The galaxy got its name because the Earth is in the plane of the galaxy and therefore it is visible in the sky as a hazy streak (in fact, all the stars visible to the naked eye in the sky lie in the Milky Way). The fact that this haze is a cluster of many stars was proven by Galileo in 1610. Edwin Hubble showed that the Milky Way is just one of many galaxies. The Milky Way is a barred spiral galaxy, 100-120 thousand light-years in diameter and about 1000 light-years thick, containing 200-400 billion stars. It has recently been proven that, on average, all star systems in the Milky Way have at least one planet. The density of stars in the Milky Way drops sharply when moving 40,000 light-years from the center of the galaxy. The reason for this phenomenon is not yet known. The orbital period of the entire galaxy is between 15 and 20 million years. The Milky Way is about 13.2 billion years old, so it is one of the first galaxies. In the center of the galaxy there is a bridge, from which four arms extend (perhaps only two of them are full-fledged arms), consisting of stars, gas and dust, although until the early 90s it was believed that the Milky Way was an ordinary spiral galaxy. At the center of the galaxy is a small but very massive source of powerful radiation, Sagittarius A*. Most likely it is a black hole.
Magellanic Clouds- The Large Magellanic Cloud and the Small Magellanic Cloud are satellite galaxies of the Milky Way. Both Clouds were previously considered irregular galaxies, but subsequently discovered structural features of barred spiral galaxies. They are located relatively close to each other and form a gravitationally bound (double) system. Visible to the naked eye in the southern hemisphere. Both Clouds “float” in a common hydrogen shell.
The Magellanic Clouds are located at high galactic latitudes, so little light is absorbed from them Milky Way, moreover, the plane of the Large Magellanic Cloud is almost perpendicular to the line of sight, so for objects visible nearby it will often be true to say that they are close spatially. These features of the Magellanic Clouds made it possible to study the patterns of distribution of stars and star clusters using their example.
The Magellanic Clouds have a number of features that distinguish them from the Milky Way. For example, star clusters with ages of 10 7 -10 8 years have been discovered there, while clusters in the Milky Way are usually older than 10 9 years.
The Magellanic Clouds were familiar to sailors in the southern hemisphere and were called the "Cape Clouds" in the 15th century. Ferdinand Magellan used them for navigation, as an alternative to the North Star, during his trip around the world in 1519-1521. When, after the death of Magellan, his ship returned to Europe, Antonio Pigafetta (Magellan's companion and official chronicler of the trip) proposed calling the Cape Clouds Magellan's Clouds as a kind of perpetuation of his memory.
Stars are massive luminous balls of gas (plasma). They are formed from a gas-dust environment (mainly hydrogen and helium) as a result of gravitational compression. The temperature of matter in the interior of stars is measured in millions of kelvins, and on their surface - in thousands of kelvins. The energy of the vast majority of stars is released as a result of thermonuclear reactions converting hydrogen into helium, which occurs when high temperatures in the interior areas. Stars are often called the main bodies of the Universe, since they contain the bulk of luminous matter in nature. It is also noteworthy that stars have negative heat capacity. 3stars are newborn, young, middle-aged and old. New stars are constantly being formed, and old ones are constantly dying. The youngest, called T Tauri stars (after one of the stars in the constellation Taurus), are similar to the Sun, but much younger than it. In fact, they are still in the process of formation and are examples of protostars (primary stars). This variable stars, their luminosity changes, since they have not yet reached a stationary mode of existence. Many Taurus stars have rotating disks of material around them; Powerful winds emanate from such stars. The energy of the matter that falls on the protostar under the influence of gravity is converted into heat. As a result, the temperature inside the protostar increases all the time. When its central part becomes so hot that nuclear fusion begins, the protostar turns into a normal star. As soon as they start nuclear reactions, the star has a source of energy that can support its existence for a very long time. How long depends on the size of the star at the beginning of this process, but a star the size of our Sun will have enough fuel to survive stable for about 10 billion years. However, it happens that stars much more massive than the Sun last only a few million years; the reason is that they compress their nuclear fuel at a much faster rate. All stars are fundamentally similar to our Sun: they are huge balls of very hot glowing gas, in the very depths of which nuclear energy is generated. But not all stars are exactly like the Sun. The most obvious difference is the color. In addition, stars differ in both brightness and brilliance. How bright a star appears in the sky depends not only on its true luminosity, but also on the distance separating it from us. Taking into account distances, the brightness of stars changes in wide range: from one ten thousandth the brightness of the Sun to the brightness of more than a million Suns. The vast majority of stars appear to be located closer to the dim end of this scale. The Sun, which is in many ways a typical star, is much more luminous than most other stars. With the naked eye you can see very a small amount of weak stars by nature. In the constellations of our sky, the main attention is drawn to the “signal lights” of unusual stars, those that have a very high luminosity. Why do stars vary so much in their brightness? It turns out that this does not depend on the mass of the star. The amount of matter contained in a particular star determines its color and brightness, as well as how the brightness changes over time. The most massive stars are also the hottest and the brightest. They appear white or bluish. Despite their huge size, these stars produce such a colossal amount of energy that all their nuclear fuel reserves burn out in just a few million years. In contrast, stars with low mass are always dim and their color is reddish. They can exist for many billions of years. However, among very bright stars There are reds and oranges in our sky. These include Aldebaran - the eye of the bull in the constellation Taurus, and Antares in Scorpio. These stars have expanded greatly and are now much larger in size than normal red stars. For this reason they are called giants, or even supergiants. Due to their enormous surface area, giants emit immeasurably more energy than normal stars like the Sun, despite the fact that their surface temperature is much lower. The diameter of a red supergiant - for example, Betelgeuse in Orion - is several hundred times greater than the diameter of the Sun. In contrast, the size of a normal red star is typically no more than one-tenth the size of the Sun. In contrast to the giants, they are called "dwarfs". Stars become giants and dwarfs at different stages of their lives, and a giant may eventually become a dwarf when it reaches "old age." A star has two parameters that determine all internal processes - mass and chemical composition. If you set them for a single star, then at any moment in time you can predict all the others physical characteristics stars such as brilliance, spectrum, size, internal structure.
Weight
The mass of a star can only be reliably determined if it is a component of a binary star. In this case, the mass can be calculated using Kepler's generalized third law. But even so, the estimated error ranges from 20% to 60% and largely depends on the error in determining the distance to the star. In all other cases, it is necessary to determine the mass indirectly, for example, from the mass-luminosity relationship. Apparent magnitudes say nothing about the total energy emitted by the star or the brightness of its surface. Indeed, due to differences in distances, a small, relatively cool star, only because of its relatively great proximity to us, can have a significantly lower apparent magnitude (i.e., appear brighter) than a distant hot giant. If the distances to two stars are known, then based on their apparent magnitudes it is easy to find the ratio of the actual light fluxes emitted by them. To do this, it is enough to refer the illumination created by these stars to the standard distance common to all stars. This distance is taken to be 10 parsecs. The magnitude that a star would have if observed from a distance of 10 parsecs is called absolute magnitude. Like visible magnitudes, absolute magnitudes can be visual, photographic, etc.
Another significant characteristic of a star is its radius. The radii of stars vary over a very wide range. There are stars no larger in size than Earth(the so-called “white dwarfs”), there are huge “bubbles” inside which the orbit of Mars could easily fit. It is no coincidence that we called such giant stars “bubbles.” From the fact that stars differ relatively little in their masses, it follows that at a very large radius the average density of matter should be negligibly small. If the average density of solar matter is 1.4 g/cm3, then in such “bubbles” it can be millions of times less than that of air. At the same time, white dwarfs have a huge average density, reaching tens and even hundreds of thousands of grams per cubic centimeter.
The Local Group of Galaxies is a system that gravitationally connects over 50 galaxies, one of which is the Milky Way.
The Local Group of galaxies is one of those cosmic objects that can capture our imagination. People still can't really comprehend how enormous the cosmic scale can be. Meanwhile, looking at the starry sky and reading popular books on astronomy, we never cease to be amazed by them. Objects in space can be so huge that we simply cannot understand the true magnitude of their size. Among these huge objects in space is the Local Group of galaxies.
As of 2015, the local group includes over 50 galaxies various sizes. The largest objects in this system are the Andromeda and Triangulum galaxies. These three largest galaxies have their own subgroups of galaxies that are associated with them gravitational forces. The large galaxies themselves: , and the Milky Way are also connected by gravitational forces and turn around in outer space general center wt.
In addition to large galaxies and their subgroups, the local group includes other dwarf galaxies, which, due to their location, cannot be classified into any of the indicated subgroups. The Local Group of galaxies includes: spiral, elliptical, dwarf elliptical, dwarf spheroidal and irregular galaxies. Perhaps scientists will be able to discover new types of galaxies that are currently unknown before the end of the century. This is quite possible, since serious observations and research by the local group are actively carried out by astronomers around the world to this day.
The Local Group of galaxies consists of more than 50 objects, each of which is a galaxy of varying sizes. These galaxies are gravitationally connected to each other - they all revolve in outer space around a common center of mass. It is believed that almost all local group galaxies are approximately the same age - about 13 billion years. In addition, they are united by composition, which may indicate that these objects have a common origin.
Observations of galaxies included in the local group showed that they have a certain structure, that is, they are not randomly located, but for the most part meaningful. Almost all galaxies of the local group are located along a line that can be roughly drawn between the Milky Way and the Andromeda Nebula. Smaller galaxies are mainly concentrated around three large galaxies: the Milky Way, Andromeda and Triangulum.
The Milky Way Galaxy is far from the largest galaxy in the observable Universe, but for us it is extremely important for the simple reason that this is where the Solar System is located, and therefore we are. The Milky Way Galaxy is part of the local group of galaxies, forming in it something like its own district center. Here in the middle is the Milky Way itself, around which its satellites orbit. Today there are fourteen of them. Among them: Ursa Major, Ursa Minor, Canis Major, Sagittarius, Dragon, Sculptor, Leo, Keel and others.
Clusters and superclusters of galaxies. Local group. Milky Way Galaxy
The Milky Way Galaxy is part of a family of neighboring galaxies known as Local group and forms with them cluster of galaxies. Our Galaxy is one of the largest in the Local Group. The Andromeda Galaxy, part of the Local Group, is the most distant object visible to the naked eye. The 25 galaxies of the Local Group are scattered over 3 million light years. A cluster of galaxies is held together by gravitational forces. Larger galaxy clusters are the Virgo Cluster (several thousand objects) and the Coma Cluster (about 1000 bright elliptical galaxies and several thousand smaller objects). Our Galaxy and its neighbors in the Local Group are slowly moving towards the Virgo Cluster.
Clusters of galaxies, in turn, are grouped into families. Local cluster clusters known as the Local Supercluster, is a formation that includes both the Local Group and the Virgo Cluster. The center of mass is located in the Virgo Cluster. Another supercluster is located in the constellation Hercules. It is 700 million light years away. Superclusters are separated from each other by giant empty spaces and form a spongy structure in the Universe.
Characteristics of galaxies included in the Local Group
Milky Way Galaxy
Milky Way- this is our Galaxy, consisting of 100 billion stars. Our Galaxy has 4 spiral arms, stars, gas and dust. Within 1000 light years of the galactic center, stars are very densely packed. In the very center of the Galaxy there is a mysterious source of colossal energy. There may be a black hole at the center of the Galaxy. The galaxy is spinning. Its internal parts rotate faster than its external parts. The Galaxy's disk is surrounded by a halo cloud of invisible matter.
9/10 The Milky Way galaxies are invisible. Our neighboring two galaxies - the Large and Small Magellanic Clouds - are attracted by an invisible halo and are absorbed by the Milky Way Galaxy.
Characteristics of the Milky Way Galaxy
* More distant flat component stars have longer orbital periods; those located closer to the center of the star have shorter periods. The central part of the Galaxy rotates like a rigid body.
Subsystems of the Galaxy
Average distance of subsystem objects from the galactic plane, kps; T is the age of the stars included in the subsystem, years; M is the mass of the subsystem (in% of the total mass of the Galaxy); N is the estimated total number of objects.
The galactic core is elliptical in shape, dimensions 4.8? 3.1 kps; number of stars?3·E10 7 .
The central core of the Galaxy is elliptical in shape, dimensions ~ 15? 30 ps; number of stars ~ 3·E10 6.
Nucleolus of the Galaxy - diameter ~ 1 ps; in its center there is a compact object (a black hole with a mass of 108-09 solar masses).
Star clusters (relatively close groups of stars):
scattered - diameter from 1.5 to 15 ps; age from several million to several billion years; the number of stars from several tens to several thousand; belong to the subsystem of the galactic plane;
ball - diameter from 15 to 200 ps; age 8-10 billion years; number of stars 10 5 -10 7 ; belong to the intermediate and extreme spherical subsystems.
The total number of stars in the Galaxy is 1.2-10 11.
From the book Everything about everything. Volume 1 author Likum ArkadyWhat is the Milky Way? The most mysterious and beautiful thing in the sky, apparently, is the Milky Way, stretching out like a necklace of precious stones from one end of the sky to the other. In ancient times, people, looking at this picture, like us, were surprised and delighted by this beauty.
From the book Big Soviet Encyclopedia(GA) of the author TSB From the book Great Soviet Encyclopedia (ML) by the author TSB From the book Great Soviet Encyclopedia (ME) by the author TSB From the book Russian Rock. Small encyclopedia author Bushueva Svetlana From the book The Newest Book of Facts. Volume 1 [Astronomy and astrophysics. Geography and other earth sciences. Biology and Medicine] authorWhat is the Local Group of Galaxies? Our Galaxy (the Milky Way), together with the Andromeda galaxy, is part of a small group of 30–40 galaxies that astronomers call the Local Group of galaxies. The most distant of the Local Group galaxies is farther from the Sun
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The gravity of the Local Group affects their movement in space, but their relationships are not limited to this.
Many of them exchange matter, and, as a rule, flows from smaller galaxies to larger ones. Such an exchange occurs between Magellanic and. The gas coming from the planet fuels the formation of new ones in the Milky Way.
Matter flows into our star system and from the galaxy into the Sculptor. This is a faint nebulous object that is visible in the southern night sky only at , although the galaxy itself is 6 times closer to us than
.
She looks like a big one globular cluster and belongs to the class of dwarf spheroidal galaxies with a diameter approximately 50 times smaller than the Milky Way. There are no giant stars, of which there are many in the Magellanic Clouds, or nebulae.
Astronomers have no doubt that many more members of the Local Group remain undiscovered. This is hampered by the own radiation of the equatorial part of the Milky Way, which “overlaps” large areas of the sky.
Recently, another dwarf spheroidal galaxy was discovered in this area - it is located in the constellation Pegasus. It is possible that this “crumb” is also a satellite of spiral Andromeda, which dominates the Local Group.
The new galaxy hides behind the bright glow of the Milky Way and is a cluster of faint blue stars 2 thousand light years across.
Astronomers believe that dwarf galaxies are " building blocks", from which large star systems eventually form.
After the exact location in the Milky Way galaxy was established, astronomers were faced with the task of determining the place of our Galaxy itself in the hierarchy of the Universe.
First of all, it turned out that it is not part of any of the large clusters of galaxies, although the irregular cluster in the constellation Virgo, well known to astronomers, is located relatively nearby.
Further research confirmed that the Milky Way is part of a smaller structure called the Local Group of galaxies.
The Local Group includes galaxies whose distance does not exceed 5 million light years; more than fifty of them have been discovered so far. At this distance they are clearly visible gravitational interactions between them, and their center of mass is on the line connecting the Milky Way and the Andromeda Galaxy.
It is well known that ours is not at rest - it moves around the Sun. moves around the center of the Milky Way. The Milky Way, in turn, moves in the Local Group of galaxies. And the Local Group itself is moving towards large cluster galaxies in the constellation Virgo.
Recently, researchers were able to measure the speed of the Local Group, and it turned out to be unusually high - approximately 600 km/s.
This result came as a complete surprise to astronomers and astrophysicists - there is still no explanation for such a rapid “fall” into the Virgo cluster.
