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"elliptical galaxy" Definitions
  1. a galaxy that has a generally elliptical shape and that has no apparent internal structure or spiral arms
"elliptical galaxy" Synonyms
galaxy constellation nebula cluster heavens stars trichiliocosm star system Milky Way solar system spiral galaxy Seyfert galaxy irregular galaxy island universe star cluster stellar system heliocentric system planetary system Copernican system Copernican heliocentrism

420 Sentences With "elliptical galaxy"

How to use elliptical galaxy in a sentence? Find typical usage patterns (collocations)/phrases/context for "elliptical galaxy" and check conjugation/comparative form for "elliptical galaxy". Mastering all the usages of "elliptical galaxy" from sentence examples published by news publications.

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M0003 is a supergiant elliptical galaxy in the constellation Virgo.
Eventually the stars will collect themselves into a giant elliptical galaxy.
A zoom-in of an elliptical galaxy showing the FRB pulse detection.
The end-result of the collision will likely yield a giant, elliptical galaxy.
"Shells of Elliptical Galaxy NGC 3923 in Hydra," Winner in the Galaxies category.
The placid appearance of the elliptical galaxy NGC 4889 can fool an unsuspecting observer.
Image: Ross Clark, UK"Shells of Elliptical Galaxy NGC 3923 in Hydra:" Winner of Galaxies category.
M89 Messier 89, an elliptical galaxy pictured at the top right, was first spotted by Messier in 1781.
Holm 15A is a central elliptical galaxy within the Abell 85 cluster, which contains more than 500 galaxies.
"But this will take a long time after the elliptical galaxy has formed," Dr. van der Marel said.
Using multiple telescopes, astronomers pinpointed the location of this FRB to an elliptical galaxy six billion light years away.
M110 Last but not least, Messier 110 is an elliptical galaxy pictured on the lower right of this image.
At first, he thought it was a small, fairly common elliptical galaxy that happened to be more circular than usual.
There's a kind of galaxy called an elliptical galaxy, which are not spheres, but they're not discs or messes, either.
Winner of the galaxies category went to Rolf Wahl Olsen, who snapped a cool pic of elliptical galaxy NHG 3923.
Essentially, researchers followed a breadcrumb trail of lightwaves to the FRB's origin—an elliptical galaxy some 6 billion light years distant.
This supermassive black hole, however, was found in a modestly-sized elliptical galaxy, with only a handful of surrounding galaxies nearby.
NGC 3697 is a product of a collision between two good-sized galaxies, and is slowly evolving to become a giant elliptical galaxy.
DF2 is located about 60 million light years away in a galaxy cluster that is dominated by a massive elliptical galaxy called NGC 1052.
M59 Messier 59, which shines brightly at the upper left of this image, is a large elliptical galaxy located 60 million light years from Earth.
M59Image: NASA, ESA, STScI, and W. Jaffe (Sterrewacht Leiden) and P. Côté (Dominion Astrophysical Observatory) (NASA)Right next to M58 is M59, an enormous elliptical galaxy.
The Milky Way will collide with nearby Andromeda, and form a large, elliptical galaxy, which will die by losing all of its stars to intergalactic space.
Once they collide, the gas is driven out very efficiently, they are compressed to this high density elliptical galaxy, and what's left is a dead system.
Hubble spotted the "Hockey Stick Galaxy," named for its distinctive shape, being stretched by the gravitational forces of nearby elliptical galaxy NGC 4627 and galaxy NGC 4631.
Other evidence, including the afterglow of the elliptical galaxy, supports the idea that we're listening to the cosmic scream of two massive objects smashing into each other.
"Lyman-alpha blob 1 is the site of formation of a massive elliptical galaxy that will one day be the heart of a giant cluster," he told me.
A blazar is a giant elliptical galaxy with two jets emitting light and particles moving close to the speed of light along the axis of the black hole's rotation.
And the object&aposs current shape won&apost last; in a few hundred million years, the cores of the two original galaxies will merge, and NGC 3256 will become a large elliptical galaxy.
But 750 or so million light years away, there's an elliptical galaxy, Galaxy 0003+379, whose two supermassive black holes are orbiting each other from a distance of only 24 or so light years.
The alarm bells really started ringing in 2015, when astronomers published observations of the same phenomenon a third time around Centaurus A, an elliptical galaxy about 10 million light years from the Milky Way.
M1103M2110Image: NASA, ESA, STScI, and M. Franx (Universiteit Leiden) and S. Faber (University of California, Santa Cruz) (NASA)M2110 is a nearly perfectly circular elliptical galaxy in the Virgo cluster, 2110 million light-years away.
The intergalactic gas clouds are literally pouring down toward the supermassive black hole at the center of an elliptical galaxy (named Abell 2597 Brightest Cluster Galaxy), according to a new study in the journal Nature this week.
A team of astronomers from the Carnegie Institution of Science, including Mark Seibert, Barry Madore, Jeff Rich and summer student Lea Hagen, were looking for the evidence of star formation still occurring in a typical "red and dead" elliptical galaxy.
They also wanted to get a better idea of why and how supermassive black holes at the center of some galaxies, like elliptical galaxy M87, seem to propel massive streams of subatomic particles out of the galaxy and into the broader universe.
They detected high-energy neutrinos in pristine ice deep below Antarctica's surface, then traced their source back to a giant elliptical galaxy with a massive, rapidly spinning black hole at its core, called a blazar, located 3.7 billion light years from Earth in the Orion constellation.
You could almost say that an elliptical galaxy, if you left it alone for the longest possible time, might become something like a sphere, but many of them are already practically the age of the universe, so we don't have enough time to know what would happen to them.
Its brightest member is the elliptical galaxy Messier 49; however its most famous member is the elliptical galaxy Messier 87, which is located in the center of the cluster.
The shells and the kinematically decoupled nucleus are the result of the merger of the elliptical galaxy with a small elliptical galaxy. The galaxy has globular clusters that belong in two populations, red and blue.
NGC 4121 is a dwarf elliptical galaxy in the constellation Draco.
NGC 5087 is an elliptical galaxy located in the constellation Virgo.
NGC 4627 is a dwarf elliptical galaxy in the constellation Canes Venatici.
NGC 1600 is an elliptical galaxy in the constellation Eridanus, away from Earth.
NGC 163 is an elliptical galaxy in the constellation Cetus. It was discovered by William Herschel since 1890. It has been found in a faint object but when seeing using an optical telescope was an elliptical galaxy that ranges up to 13 magnitude.
Astronomers have predicted that all five galaxies may eventually merge into one large elliptical galaxy.
Observations and simulations of colliding galaxies suggest that the Antennae Galaxies will eventually form an elliptical galaxy.
NGC 382 is an elliptical galaxy located in Pisces constellation discovered by William Parsons 4 November 1850 .
Elliptical galaxy IC 2006. Elliptical galaxies are characterized by several properties that make them distinct from other classes of galaxy. They are spherical or ovoid masses of stars, starved of star-making gases. The smallest known elliptical galaxy is about one-tenth the size of the Milky Way.
NGC 7317 is an elliptical galaxy that is a member of the Stephan's Quintet in the constellation Pegasus.
NGC 3545B is an elliptical galaxy in the constellation Ursa Major. The object is close to NGC 3545.
Furthermore, the large elliptical galaxy and the edge-on spiral galaxy, both of which have active nuclei, are connected by a stream of stars and dust, indicating that they too are interacting. Astronomers predict that the three galaxies may merge millions of years in the future to form a giant elliptical galaxy.
NGC 467 is an elliptical galaxy in the constellation Pisces. It was discovered on 8 October 1785 by William Herschel.
NGC 4308 is an elliptical galaxy in the constellation Coma Berenices. It is a member of the Coma I Group.
NGC 282 is an elliptical galaxy in the constellation Pisces. It was discovered on October 13, 1879 by Édouard Stephan.
NGC 284 is an elliptical galaxy in the constellation Cetus. It was discovered on October 2, 1886 by Francis Leavenworth.
If Segue 1 is a galaxy it may have been a satellite of Sagittarius Dwarf Elliptical Galaxy in the past.
NGC 297 is an elliptical galaxy in the constellation Cetus. It was discovered on September 27, 1864 by Albert Marth.
NGC 1172 is an elliptical galaxy in the constellation Eridanus. It was discovered by William Herschel on December 30, 1785.
NGC 315 is an elliptical galaxy in the constellation Pisces. It was discovered on September 11, 1784 by William Herschel.
The galaxy, 3C 348, is a supergiant elliptical galaxy. It is classified as type E3 to E4 of the updated Hubble–de Vaucouleurs extended galaxy morphological classification scheme. Little else is known about the galaxy. 3C 348, the galaxy at the image center, appears to be a relatively normal elliptical galaxy in visible light.
NGC 194 is an elliptical galaxy located in the constellation Pisces. It was discovered on December 25, 1790 by William Herschel.
NGC 183 is an elliptical galaxy located in the constellation Andromeda. It was discovered on November 5, 1866 by Truman Safford.
NGC 777 is an elliptical galaxy in the constellation of Triangulum. It was discovered by William Herschel on September 12, 1784.
NGC 57 is an elliptical galaxy in the constellation Pisces. It was discovered on 8 October 1784 by astronomer William Herschel.
NGC 5343 is an elliptical galaxy in the constellation of Virgo. It was discovered on 5 May 1785 by William Herschel.
NGC 233 is an elliptical galaxy located in the constellation Andromeda. It was discovered on September 11, 1784 by William Herschel.
Artist image of a firestorm of star birth deep inside core of young, growing elliptical galaxy. NGC 4676 (Mice Galaxies) is an example of a present merger. Antennae Galaxies are a pair of colliding galaxies – the bright, blue knots are young stars that have recently ignited as a result of the merger. ESO 325-G004, a typical elliptical galaxy.
NGC 1374 is a low-luminosity elliptical galaxy in southern constellation Fornax. It was discovered by John Herschel on November 29, 1837.
The Milky Way galaxy is currently in the process of cannibalizing the Sagittarius Dwarf Elliptical Galaxy and the Canis Major Dwarf Galaxy.
NGC 3268 is an elliptical galaxy in the constellation Antlia. It is a member of the Antlia Cluster, which lies about away.
NGC 3258 is an elliptical galaxy in the constellation Antlia. It is a member of the Antlia Cluster, which lies about away.
NGC 3260 is an elliptical galaxy in the constellation Antlia. It is a member of the Antlia Cluster, which lies about away.
NGC 5223 is an elliptical galaxy in the constellation of Canes Venatici. It was discovered on 1 May 1785 by William Herschel.
NGC 312 is an elliptical galaxy / lenticular galaxy in the constellation Phoenix. It was discovered on September 5, 1836 by John Herschel.
NGC 3357 is an elliptical galaxy located in the constellation of Leo. It was discovered on April 5, 1864 by German astronomer Albert Marth.
3C 273 lies at the center of a giant elliptical galaxy with an apparent magnitude of 16 and an apparent size of 30 arc seconds.
NGC 0154 DSS NGC 154 is an elliptical galaxy in the Cetus constellation. The galaxy was discovered by Frederick William Herschel on November 27, 1785.
MCG+01-02-015 was previously classified as an elliptical galaxy of class E2 although higher-resolution imaging has revealed it to be a barred spiral galaxy.
Elliptical galaxies are thought to form from collisions with spiral galaxies; NGC 3610 is a relatively young elliptical galaxy which has still not lost its disk yet.
The central galaxy in this image is a gigantic elliptical galaxy designated 4C 73.08. The brilliant central object is a supergiant elliptical galaxy, the dominant member of a galaxy cluster with the name MACSJ1423.8+2404. Note the gravitational lensing. Elliptical galaxies vary greatly in both size and mass with diameters ranging from 3000 lightyears to more than 700,000 lightyears, and masses from 105 to nearly 1013 solar masses.
Maffei 1 is a massive elliptical galaxy in the constellation Cassiopeia. Once believed to be a member of the Local Group of galaxies, it is now known to belong to a separate group, the IC 342/Maffei Group. It was named after Paolo Maffei, who discovered it and the neighboring Maffei 2 in 1967 via their infrared emissions. Maffei 1 is a slightly flattened core type elliptical galaxy.
NGC 4150 is an elliptical galaxy located approximately 45 million light years away in the constellation Coma Berenices. It was discovered by William Herschel on March 13, 1785.
NGC 5018 is an elliptical galaxy located in the constellation of Virgo at an approximate distance of 132.51 Mly. NGC 5018 was discovered in 1788 by William Herschel.
NGC 4436 is undergoing a tidal interaction with a nearby dwarf elliptical galaxy known as NGC 4431. The two galaxies are separated by around 58,680 light-years (18 kpc).
Johann Gottfried Koehler (15 December 1745 – 19 September 1801) was a German astronomer who discovered a number of nebulae, star clusters, and galaxies. Koehler is best remembered for his discovery of Open Cluster M67, Elliptical Galaxy M59, and Elliptical Galaxy M60. The latter two were discovered on the same day, 11 April 1779. He worked with the noted astronomer Johann Elert Bode, who refined and published Koehler's proposal for the symbol of Uranus.
NGC 7057 is an elliptical galaxy located about 230 million light-years away in the constellation of Microscopium. NGC 7057 was discovered by astronomer John Herschel on September 2, 1836.
NGC 7061 is an Elliptical galaxy located about 400 million light-years away in the constellation of Indus. NGC 7061 was discovered by astronomer John Herschel on September 30, 1834.
Of the galaxies confirmed to be in orbit, the largest is the Sagittarius Dwarf Elliptical Galaxy, which has a diameter of or roughly a twentieth that of the Milky Way.
NGC 474 is an elliptical galaxy about 100 million light years distant in the constellation Pisces. This large galaxy is known to possess tidal tails, although their origins remain unknown.
NGC 766 is an elliptical galaxy located in the Pisces constellation about 362 million light years from the Milky Way. It was discovered by British astronomer John Herschel in 1828.
NGC 219 is a compact elliptical galaxy located approximately 245 million light-years from the Sun. in the constellation Cetus. It was discovered on September 16, 1863 by George Bond.
NGC 623 is a large elliptical galaxy located in the Sculptor constellation about 400 million light-year from the Milky Way. It was discovered by British astronomer John Herschel in 1837.
The elliptical galaxy is located in the constellation of Hercules at right ascension 16h 53.9m and declination +39° 45'. Its visible size appears to be 1.2 by 1 minute of arc.
IC 3 is a compact elliptical galaxy located approximately 228 million light- years away in the constellation of Pisces. The galaxy was discovered by astronomer Stéphane Javelle on August 27, 1892.
Two members of the Local Group of galaxies are in Cassiopeia. NGC 185 is a magnitude 9.2 elliptical galaxy of type E0, 2 million light-years away. Slightly dimmer and more distant NGC 147 is a magnitude 9.3 elliptical galaxy, like NGC 185 it is an elliptical of type E0; it is 2.3 million light-years from Earth. Though they do not appear in Andromeda, both dwarf galaxies are gravitationally bound to the far larger Andromeda Galaxy.
NGC 4261 is an elliptical galaxy located around 100 million light-years away in the constellation Virgo. It was discovered April 13, 1784 by the German- born astronomer William Herschel. The galaxy is a member of its own somewhat meager galaxy group known as the NGC 4261 group, which is part of the Virgo Cluster. The morphological classification of this galaxy is E2, indicating an elliptical galaxy with a 5:4 ratio between the major and minor axes.
NGC 484 is an elliptical galaxy in the constellation Tucana. It is located approximately 218 million light-years from Earth and was discovered in on October 28, 1834 by astronomer John Herschel.
NGC 990 is an elliptical galaxy located in the constellation Aries about 153 million light-years from the Milky Way. It was discovered by the German - British astronomer William Herschel in 1786.
NGC 7014 is an elliptical galaxy located about 210 million Light-years away from Earth in the constellation Indus. NGC 7014 was discovered by English astronomer John Herschel on October 2, 1834.
NGC 862 is an elliptical galaxy located in the constellation of Phoenix about 241 million light years from the Milky Way. It was discovered by the British astronomer John Herschel in 1834.
Michael J. Irwin is a British astronomer. He is the director of the Cambridge Astronomical Survey Unit and one of the discoverers of the Cetus Dwarf galaxy and the Sagittarius Dwarf Elliptical Galaxy.
NGC 860 is an elliptical galaxy located in the constellation Triangulum. It is about 410 million light-years from the Milky Way. It was discovered by the French astronomer Édouard Stephan in 1871.
NGC 481 is an elliptical galaxy in the constellation Cetus. It is located approximately 229 million light-years from Earth and was discovered in on November 20, 1886 by astronomer Lewis A. Swift.
The sky image is obtained by Sloan Digital Sky Survey, DR14 with SciServer. NGC 6263 is an elliptical galaxy in the constellation Hercules. It was discovered by Albert Marth on June 28, 1864.
Messier 60 or M60, also known as NGC 4649, is an elliptical galaxy approximately 57 million light-years away in the equatorial constellation of Virgo. Together with NGC 4647, it forms a pair known as Arp 116. Messier 60 and the nearby elliptical galaxy Messier 59 were both discovered by Johann Gottfried Koehler in April 1779 during observations of a comet in the same part of the sky. Charles Messier added both to his catalogue about three days after Koehler's discovery.
NGC 636 is an elliptical galaxy in the Cetus constellation. It is located about 96 million light-years from the Milky Way. It was discovered by the German–British astronomer William Herschel in 1785.
NGC 83 is an elliptical galaxy estimated to be about 260 million light-years away in the constellation of Andromeda. It was discovered by John Herschel in 1828 and its apparent magnitude is 14.2.
NGC 97 is an elliptical galaxy estimated to be about 230 million light-years away in the constellation of Andromeda. It was discovered by John Herschel in 1828 and its apparent magnitude is 13.5.
NGC 7075 is an elliptical galaxy with a radio emission located about 290 million light-years away in the constellation of Grus. NGC 7075 was discovered by astronomer John Herschel on September 4, 1834.
NGC 2294 is an elliptical galaxy within the constellation Gemini, discovered by George Johnstone Stoney on February 22, 1849. The visual magnitude is 14, and the apparent size is 0.8 by 0.4 arc minutes.
NGC 79 is an elliptical galaxy estimated to be about 240 million light-years away in the constellation of Andromeda. Its apparent magnitude is 14.9. It was discovered on 14 November 1884 by Guillaume Bigourdan.
NGC 1000 is an elliptical galaxy located in the constellation of Andromeda. It was discovered on December 9, 1871 by Édouard Jean-Marie Stephan. It is the 1,000th object classified by the New General Catalogue.
NGC 1427 is a low-luminosity elliptical galaxy approximately 71 million light- years away from Earth. It is currently traveling toward the Fornax cluster. It was discovered by John Frederick William Herschel on November 28, 1837.
The galaxy is approximately 150,000 light years across. This makes it, in comparison, about 1.5 times as large as the Milky Way. The galaxy also has a satellite elliptical galaxy called PGC (Principal Galaxies Catalogue) 1563523.
NGC 910 is an elliptical galaxy in the constellation of Andromeda. NGC 910 was discovered on October 17, 1786 by the German-British astronomer William Herschel. It is the brightest galaxy in the cluster Abell 347.
NGC 6053 is an elliptical galaxy located about 450 million light-years away in the constellation Hercules. The galaxy was discovered by astronomer Lewis Swift on June 8, 1886 and is member of the Hercules Cluster.
NGC 6158 is an elliptical galaxy located about 400 million light-years away in the constellation Hercules. The galaxy was discovered by astronomer William Herschel on March 17, 1787 and is a member of Abell 2199.
NGC 1404 is an elliptical galaxy in the Southern constellation Eridanus. It lies at a distance of 65 million light years from the Milky Way and it is one of the brightest members of the Fornax Cluster.
NGC 6047 is an elliptical galaxy located about 430 million light-years away in the constellation Hercules. It was discovered by astronomer Lewis Swift on June 27, 1886. NGC 6047 is a member of the Hercules Cluster.
NGC 5886 NED, NGC 5886 (accessed 20-03-2012) (alternatively named ZWG 221.36) is an +14 magnitude elliptical galaxy in the constellation Boötes. It was originally discovered by William Herschel in 1828 with an 18.7 inch reflector.
NGC 4729 is an elliptical galaxy located about 160 million light-years away in the constellation Centaurus. NGC 4729 was discovered by astronomer John Herschel on June 8, 1834 and is a member of the Centaurus Cluster.
The giant elliptical galaxy ESO 325-G004 An elliptical galaxy is a type of galaxy with an approximately ellipsoidal shape and a smooth, nearly featureless image. They are one of the three main classes of galaxy described by Edwin Hubble in his Hubble sequence and 1936 work The Realm of the Nebulae, Alt URL(pp. 124–151) along with spiral and lenticular galaxies. Elliptical (E) galaxies are, together with lenticular galaxies (S0) with their large-scale disks, and ES galaxiesLiller, M.H. (1966), The Distribution of Intensity in Elliptical Galaxies of the Virgo Cluster.
Messier 59 or M59, also known as NGC 4621, is an elliptical galaxy in the equatorial constellation of Virgo. M59 is a member of the Virgo Cluster, with the nearest component being separated from M59 by and around 5 magnitudes fainter. The nearest cluster member of comparable brightness is the lenticular galaxy NGC 4638, which is around away. Messier 59 and the nearby elliptical galaxy Messier 60 were both discovered by Johann Gottfried Koehler in April 1779 during observations of a comet in the same part of the sky.
NGC 1274 is a compact elliptical galaxy located about 280 million light-years away in the constellation Perseus. NGC 1274 was discovered by astronomer Lawrence Parsons on December 4, 1875. It is a member of the Perseus Cluster.
NGC 4478 is an elliptical galaxy located about 50 million light-years away in the constellation Virgo. NGC 4478 was discovered by astronomer William Herschel on April 12, 1784. NGC 4478 is a member of the Virgo Cluster.
NGC 1426 is an elliptical galaxy approximately 59 million light-years away from Earth in the constellation of Eridanus. It was discovered by William Herschel in December 9, 1784. NGC 1426 is a member of the Eridanus Cluster.
Messier 89 (M89 for short, also known as NGC 4552) is an elliptical galaxy in the constellation Virgo. It was discovered by Charles Messier on March 18, 1781. M89 is a member of the Virgo Cluster of galaxies.
NGC 3305 is an elliptical galaxy located about 190 million light-years away in the constellation Hydra. The galaxy was discovered by astronomer John Herschel on March 24, 1835. NGC 3305 is a member of the Hydra Cluster.
NGC 519, also occasionally referred to as PGC 5182 is an elliptical galaxy located approximately 242 million light-years from the Solar System in the constellation Cetus. It was discovered on 20 November 1886 by astronomer Lewis Swift.
NGC 3873 is an elliptical galaxy located about 300 million light-years away in the constellation Leo. The galaxy was discovered by astronomer Heinrich d'Arrest on May 8, 1864. NGC 3873 is a member of the Leo Cluster.
NGC 4564 is an elliptical galaxy located about 57 million light-years away in the constellation Virgo. NGC 4564 was discovered by astronomer William Herschel on March 15, 1784. The galaxy is also a member of the Virgo Cluster.
NGC 4876 is an elliptical galaxy located about 325 million light-years away in the constellation Coma Berenices. NGC 4876 was discovered by astronomer Guillaume Bigourdan on May 16, 1885. NGC 4876 is a member of the Coma Cluster.
ESO 444-46 is a giant elliptical galaxy located about 640 million light-years away in the constellation Centaurus. It is the brightest member of the galaxy cluster Abell 3558 which lies in the center of the Shapley Supercluster.
NGC 4066 is an elliptical galaxy located 340 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 27, 1785. NGC 4066 is a member of the NGC 4065 Group.
NGC 4464 is an elliptical galaxy located about 70 million light-years away in the constellation of Virgo. NGC 4464 was discovered by astronomer William Herschel on December 28, 1785. NGC 4464 is a member of the Virgo Cluster.
NGC 384 is an elliptical galaxy located in the constellation Pisces. It was discovered on November 4, 1850 by Bindon Stoney. It was described by Dreyer as "pretty faint, pretty small, southwestern of 2.", the other being NGC 385.
NGC 3402, also known as NGC 3411, is an elliptical galaxy in the constellation Hydra. The object was discovered on March 25, 1786 by German-British astronomer William Herschel. NGC 3402 is the largest galaxy in the eponymous NGC 3402 cluster.
NGC 4125 is an elliptical galaxy in the constellation Draco. In 2016, the telescope KAIT discovered the super nova SN 2016coj in this galaxy. After detection it became brighter over the course of several days, indicating a Type Ia supernova.
IC 1517 is an elliptical galaxy, of apparent magnitude +13.8, in the constellation Pisces. The galaxy is south and west of Gamma Piscium, just south of the ecliptic, and north of the constellation Aquarius. It has a redshift of 0.02449.
NGC 4468 is a dwarf elliptical galaxy located about 55 million light-years away in the constellation of Coma Berenices. The galaxy was discovered by astronomer William Herschel on January 14, 1787. It is a member of the Virgo Cluster.
NGC 911 is an elliptical galaxy located in the constellation Andromeda about 258 million light years from the Milky Way . It was discovered by French astronomer Édouard Stephan in 1878. It is a member of the galaxy cluster Abell 347.
NGC 938 is an elliptical galaxy located in the constellation Aries, approximately 184 million light years from the Milky Way. It was discovered by the Prussian astronomer Heinrich d'Arrest in 1863. SN 2015ab, a type Ia supernova, occurred within NGC 938.
NGC 4489 is a dwarf elliptical galaxy located about 60 million light-years away in the constellation of Coma Berenices. It was discovered by astronomer William Herschel on March 21, 1784. NGC 4489 is a member of the Virgo Cluster.
There are many types of galaxy mergers, which do not necessarily result in elliptical galaxies, but result in a structural change. For example, a minor merger event is thought to be occurring between the Milky Way and the Magellanic Clouds. Mergers between such large galaxies are regarded as violent, and the frictional interaction of the gas between the two galaxies can cause gravitational shock waves, which are capable of forming new stars in the new elliptical galaxy. By sequencing several images of different galactic collisions, one can observe the timeline of two spiral galaxies merging into a single elliptical galaxy.
NGC 4095 is an elliptical galaxy located 330 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 26, 1785. NGC 4095 is a member of the NGC 4065 Group and is a LINER.
Abell 1146 is a rich galaxy cluster in the constellation Crater. Its richness class is 4, and it is located about 2 billion light-years (630 megaparsecs) away. Its brightest member, PGC 33231, is an elliptical galaxy. It has a redshift of 0.142.
NGC 901 is an elliptical galaxy in the constellation Aries. It is estimated to be 441 million light years from the Milky Way and has a diameter of approximately 50,000 ly. NGC 901 was discovered on September 5, 1864 by Albert Marth.
NGC 904 is an elliptical galaxy in the constellation Aries. It is estimated to be 244 million light years from the Milky Way and has a diameter of approximately 85,000 ly. NGC 904 was on 13 December 1884 by the astronomer Edouard Stephan.
NGC 4436 is a lenticular or dwarf elliptical galaxy located about 60 million light-years away in the constellation of Virgo. NGC 4436 was discovered by astronomer William Herschel on April 17, 1784. The galaxy is a member of the Virgo Cluster.
NGC 323 is an elliptical galaxy located in the constellation Phoenix. It was discovered on October 3, 1834 by John Herschel. It was described by Dreyer as "pretty faint, small, round, brighter middle, preceding (western) of 2", the other being NGC 328.
NGC 6086 is an elliptical galaxy in the constellation of Corona Borealis. It has an apparent magnitude of 12.7. A Type-cD galaxy, it is the brightest cluster galaxy in the cluster Abell 2162. In 2010, a supermassive black hole was discovered in NGC 6086.
NGC 501, also occasionally referred to as PGC 5082 or GC 284, is an elliptical galaxy in the constellation Pisces. It located approximately 224 million light-years from the Solar System and was discovered on 28 October, 1856 by Irish astronomer R. J. Mitchell.
NGC 5011 is an elliptical galaxy in the constellation of Centaurus. It was discovered on 3 June 1834 by John Herschel. It was described as "pretty bright, considerably small, round, among 4 stars" by John Louis Emil Dreyer, the compiler of the New General Catalogue.
NGC 1403 is a lenticular or elliptical galaxy in the constellation Eridanus. It was discovered in 1886 by Francis Preserved Leavenworth. It was thought to be a "very faint, extremely small, nebulous star" by John Louis Emil Dreyer, the compiler of the New General Catalogue.
When galaxies interact through collisions, dynamical friction between stars causes matter to sink toward the center of the galaxy and for the orbits of stars to be randomized. This process is called violent relaxation and can change two spiral galaxies into one larger elliptical galaxy.
NGC 7034 is an elliptical galaxy located about 380 million light-years away in the constellation of Pegasus. It is part of a pair of galaxies that contains the nearby galaxy NGC 7033. NGC 7034 was discovered by astronomer Albert Marth on September 17, 1863.
NGC 939 is a lenticular or elliptical galaxy in the constellation Eridanus. It is estimated to be 241 million light-years from the Milky Way and has a diameter of approximately 80,000 ly. NGC 939 was discovered on October 18, 1835 by astronomer John Herschel.
NGC 821 is an elliptical galaxy in the constellation Aries. It is estimated to be about 80 million light-years from the Milky Way and has a diameter of approximately 55,000 light years. NGC 821 was discovered on September 4, 1786 by astronomer Wilhelm Herschel.
NGC 822 is an elliptical galaxy in the constellation Phoenix. It is estimated to be about 233 million light-years from the Milky Way and has a diameter of approximately 80,000 light-years. NGC 822 was discovered on September 5, 1834 by astronomer John Herschel.
NGC 4089 is an elliptical galaxy located 340 million light-years away in the constellation Coma Berenices. NGC 4089 was discovered by astronomer Heinrich d'Arrest on May 4, 1864 and is a member of the NGC 4065 Group. The galaxy also hosts an AGN.
It has a heterogeneous halo of extremely hot gas, posited to be due to the active galactic nucleus at the core of the central elliptical galaxy. M87 is the largest galaxy in the Virgo cluster, and is at a distance of from Earth (redshift 0.0035).
NGC 533 is an elliptical galaxy in the constellation Cetus. It was discovered on October 8, 1785 by William Herschel. It was described as "pretty bright, pretty large, round, gradually brighter middle" by John Louis Emil Dreyer, the compiler of the New General Catalogue.
NGC 630 is an elliptical galaxy in the constellation Sculptor. It is estimated to be 275 million light years from the Milky Way and has a diameter of approximately 125,000 light years. The object was discovered on October 23, 1835 by the English astronomer John Herschel.
NGC 953 (also PGC 9586, UGC 1991, MCG 5-7-1, GWT GWT 504 104 or 505.1) is an elliptical galaxy in the constellation Triangulum. It has an apparent magnitude of 14.5. It was discovered by the German astronomer Heinrich Louis d'Arrest on September 26, 1865.
HVGC-1 is the first discovered hypervelocity globular cluster. Discovered in 2014, it was found escaping the supergiant elliptical galaxy Messier 87, in the Virgo Cluster. It is one of thousands of globular clusters found in M87. It is the first hypervelocity star cluster so far discovered.
NGC 4467 is an elliptical galaxy located about 78 million light-years away in the constellation of Virgo. NGC 4467 was discovered by astronomer Otto Struve on April 28, 1851. NGC 4467 is a companion of Messier 49 and is a member of the Virgo Cluster.
IC 1101 is a supergiant elliptical galaxy at the center of the Abell 2029 galaxy cluster and is one of the largest known galaxies. Its halo extends about from its core, and it has a mass of about 100 trillion stars. The galaxy is located from Earth.
200px NGC 3818 is an elliptical galaxy in the Constellation Virgo. It is at a distance of about 77 million light-years away from Earth. In the center of NGC 3818 lies a supermassive black hole. NGC 3818 was discovered by William Herschel on March 5, 1785.
Most galaxies are organized into distinct shapes that allow for classification schemes. They are commonly divided into spiral, elliptical and Irregular galaxies. As the name suggests, an elliptical galaxy has the cross-sectional shape of an ellipse. The stars move along random orbits with no preferred direction.
NGC 3610 is an elliptical galaxy in the constellation Ursa Major. It was discovered on 8 April 1793 by William Herschel. NGC 3610 was imaged by the Hubble Space Telescope in 2015. The image shows a prominent disk, a characteristic of spiral galaxies but not elliptical galaxies.
NGC 736 is an elliptical galaxy in the constellation Triangulum. It is an estimated 200 million light years from the Milky Way and has a diameter of approximately 85,000 light years. NGC 736 was discovered on September 12, 1784 by the German-British astronomer William Herschel.
NGC 4860 is an elliptical galaxy in the constellation Coma Berenices. The galaxy was discovered on 21 April 1865 by Heinrich Louis d'Arrest. With its distance from earth being approximately 110 million parsecs, NGC 4860 belongs to the Coma Cluster, which consists of over 1,000 identified galaxies.
NGC 770 is an elliptical galaxy in the constellation Aries. It is around 120 million light years from the Milky Way and has a diameter of around . NGC 770 is gravitationally linked to NGC 772. The galaxy was discovered on November 3, 1855 by RJ Mitchell.
NGC 4660 is an elliptical galaxy located about 63 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster. NGC 4660 forms a tight pair with Messier 59.
NGC 4084 is an elliptical galaxy located 315 million light-years away in the constellation Coma Berenices. NGC 4084 was discovered by astronomer Heinrich d'Arrest on April 26, 1865. NGC 4084 is an isolated member of the Coma Supercluster and is classified as a LINER galaxy.
It is a peculiar elliptical galaxy that orbits 42,000 light-years from the center of NGC 1097. Dwarf galaxy NGC 1097B (5 x 106 solar masses), the outermost one, was discovered by its HI emission, and appears to be a typical dwarf irregular. Little else is known about it.
NGC 1267 is an elliptical galaxy located about 220 million light-years away in the constellation Perseus. NGC 1267 was discovered by astronomer Heinrich d'Arrest on February 14, 1863. NGC 1267 is a member of the Perseus Cluster and is possibly interacting with the spiral galaxy NGC 1268.
NGC 4494 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 45 million light years from Earth, which, given its apparent dimensions, means that NGC 4494 is about 60,000 light years across. It was discovered by William Herschel in 1785.
NGC 810 is an unbarred elliptical galaxy located in the constellation Cetus, approximately 360 million light-years from the Milky Way. It was discovered by the French astronomer Édouard Stephan in 1871. NGC 810 is currently in a merger event. It is interacting with the galaxy SDSS J020529.28+131503.5.
NGC 4055 is an elliptical galaxy located 310 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832. It is listed both as NGC 4061 and NGC 4055.
The outer isophotes of the galaxy appear twisted and feature faint shells. NGC 1549 forms an interacting pair with the lenticular galaxy NGC 1553, which lies 12 arcminutes to the south. It is the largest elliptical galaxy in a moderate size galaxy group known as the Dorado Group.
For example, the giant elliptical galaxy M87 has an absolute magnitude of −22 (i.e. as bright as about 60,000 stars of magnitude −10). Some active galactic nuclei (quasars like CTA-102) can reach absolute magnitudes in excess of −32, making them the most luminous objects in the observable universe.
NGC 823, also known as IC 1782, is an elliptical galaxy in the constellation Fornax. It is estimated to be 196 million light years from the Milky Way and has a diameter of approximately 100,000 light years. NGC 823 was discovered on October 14, 1830 by astronomer John Herschel.
NGC 4696 is an elliptical galaxy. It lies around away in the constellation Centaurus. It is the brightest galaxy in the Centaurus Cluster, a large, rich cluster of galaxies in the constellation of the same name. The galaxy is surrounded by many dwarf elliptical galaxies also located within the cluster.
NGC 3226 is a dwarf elliptical galaxy that is interacting with the spiral galaxy NGC 3227. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo.
276, No. 2, February 1997, pp.40-45, Ken Crosswell, "Malin 1: A Bizarre Galaxy Gets Slightly Less So", 22 January 2007 UGC 1382 was previously thought to be an elliptical galaxy, but low-brightness spiral arms were later detected. UGC 1382 is much closer to Earth than Malin 1.
NGC 1573 is an elliptical galaxy in the constellation of Camelopardalis. It was discovered on 1 August 1883 by Wilhelm Tempel. It was described as "very faint, small" by John Louis Emil Dreyer, the compiler of the New General Catalogue. It is located about 190 million light-years (58 megaparsecs) away.
NGC 7029 is an elliptical galaxy located about 120 million Light-years away from Earth in the constellation Indus. NGC 7029 has an estimated diameter of 129,000 light-years. It was discovered by astronomer John Herschel on October 10, 1834. It is in a pair of galaxies with NGC 7022.
NGC 7674 is the brightest and largest member of the isolated Hickson 96 compact group of galaxies, consisting of four galaxies. NGC 7674 forms a pair with its smaller companion NGC 7674A, which lies 34 arcseconds to the north. NGC 7675, an elliptical galaxy, lies 2.2 arcminutes to the east.
NGC 7002 is a large elliptical galaxy around 320 million Light-years away from Earth in the constellation of Indus. The galaxy was discovered by English astronomer John Herschel on September 30, 1834. NGC 7002 is also part of a group of galaxies that contains the nearby galaxy NGC 7004.
NGC 6375 is a galaxy in the New General Catalog. It is located in the sky near the constellation Hercules. It is an E0 type lenticular, elliptical galaxy. It was discovered by German astronomer Albert Marth in 1864 with a mirror type telescope with a diameter of 121.92 cm (48 inches).
NGC 3842 is an elliptical galaxy in the constellation of Leo. It was discovered by William Herschel. It is notable for containing one of the largest black holes ever detected, reported to have a mass of 9.7 billion solar masses. It is around 330 million light-years distant from Earth.
NGC 3309 is a giant elliptical galaxy located about 200 million light-years away in the constellation Hydra. NGC 3309 was discovered by astronomer John Herschel on March 24, 1835. The galaxy forms a pair with NGC 3311 which lies about away. Both galaxies dominate the center of the Hydra Cluster.
NGC 680 is an elliptical galaxy located in the constellation Aries. It is located at a distance of circa 120 million light years from Earth, which, given its apparent dimensions, means that NGC 680 is about 100,000 light years across. It was discovered by William Herschel on September 15, 1784.
NGC 3640 is an elliptical galaxy with a highly disturbed stellar component. The galaxy features boxy isophotes, and patchy shell-like features. These features indicate a recent merger with a smaller gas-poor galaxy. A dust lane is observed along the minor-axis, spanning 30 arcseconds in a north-south direction.
NGC 543 is an elliptical galaxy in the constellation Cetus. It is estimated to be 239 million light years from the Milky Way and has a diameter of approximately 40,000 ly. NGC 543 was discovered by the German-Danish astronomer Heinrich Louis d'Arrest. It is a member of the galaxy cluster Abell 194.
Abell 3742 is a galaxy cluster located around 200 million light years (61 Mpc) from Earth in the constellation Indus. The cluster's brightest member is the elliptical galaxy NGC 7014. Abell 3742 is located in the Pavo-Indus Supercluster and is one of three major clusters along with Abell 3656 and Abell 3698.
The host galaxy of SN Refsdal is at a redshift of 1.49, corresponding to a comoving distance of 14.4 billion light-years and a lookback time of 9.34 billion years. The multiple images are arranged around the elliptical galaxy at z = 0.54 in a cross-shaped pattern, also known as an "Einstein cross".
M96 is the brightest galaxy within the M96 Group, a group of galaxies in the constellation Leo that includes the Messier objects M95 and M105, as well as at least nine other galaxies. M96 group is the nearest galaxy group to Earth containing both bright spirals and a bright elliptical galaxy (Messier 105).
It was discovered on January 7 of 2006 and took place on the outskirts of this galaxy. On 25th June 2020, the ATLAS telescope in Hawaii spotted a supernova candidate in M85. M85 is interacting with the nearby spiral galaxy NGC 4394, and a small elliptical galaxy called MCG 3-32-38.
Fig. 1. The firehose instability in an N-body simulation of a prolate elliptical galaxy. Time progresses top–down, from upper left to lower right. Initially, the long-to-short axis ratio of the galaxy is 10:1. After the instability has run its course, the axis ratio is approximately 3:1.
NGC 4323 is a lenticular or dwarf elliptical galaxy located about 52.5 million light-years away in the constellation Coma Berenices. The galaxy was discovered in 1882 by astronomer Wilhelm Tempel and is a member of the Virgo Cluster. NGC 4323 is commonly misidentified as NGC 4322, which is a 13th magnitude star.
ESO 146-5 (ESO 146-IG 005) is the designation given to a giant interacting elliptical galaxy in the center of the Abell 3827 cluster. It is well noted due to its strong gravitational lensing effect, measurements of which show the galaxy to be one of the most massive in the known universe.
The jets producing the radio lobes are not particularly powerful, giving the lobes a more diffuse, knotted structure due to interactions with the intergalactic medium. Associated with this peculiar galaxy is an entire cluster of galaxies. NGC 1399 is a large elliptical galaxy in the Southern constellation Fornax, the central galaxy in the Fornax cluster.
NGC 4056 is an elliptical galaxy located about 340 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer Albert Marth on March 18, 1865 and is a member of the NGC 4065 Group. Although NGC 4056 is commonly equated with PGC 38140, there is still uncertainty in its identification.
NGC 4482 is a dwarf elliptical galaxy located about 60 million light-years away in the constellation Virgo. NGC 4482 was discovered by astronomer William Herschel on March 15, 1784. It was rediscovered by astronomer Arnold Schwassmann on September 6, 1900 and was listed as IC 3427. It is a member of the Virgo Cluster.
NGC 1407 is an elliptical galaxy in Eridanus. It is at a distance of 76 million light years from Earth. It is the brightest galaxy in the NGC 1407 Group, part of the Eridanus Group, with NGC 1407 being its brightest member. NGC 1400, the second brightest of the group lies 11.8 arcmin away.
NGC 596 is an elliptical galaxy in the constellation Cetus. The galaxy lies 65 million light years away from Earth, which means, given its apparent dimensions, that NGC 596 is approximately 60,000 light years across. The galaxy shows an outer envelope and is a merger remnant. The surface brightness profil is smooth and featureless.
It is metal- rich with a metallicity of . It has an average luminosity distribution of . Based on proper motion studies, this cluster was first suspected in 2000 to have been captured from the Sagittarius Dwarf Elliptical Galaxy (SagDEG) about 1.7 Ga ago. It is now generally believed to be a member of that galaxy.
NGC 4070 is an elliptical galaxy located 340 million light-years away in the constellation Coma Berenices. NGC 4070 was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832 and was listed as NGC 4059. The galaxy is a member of the NGC 4065 Group.
NGC 811 is an object in the New General Catalogue. It is an elliptical galaxy located in the constellation Cetus about 700 million light-years from the Milky Way. It was discovered by the American astronomer Francis Leavenworth in 1886. However, it is usually misidentified as a different object, the spiral galaxy PGC 7905.
NGC 4886 is an elliptical galaxy located about 327 million light-years away in the constellation Coma Berenices. NGC 4886 was discovered by astronomer Heinrich d'Arrest on April 6, 1864. It was then rediscovered by d'Arrest on April 22, 1865 and was listed as NGC 4882. NGC 4886 is a member of the Coma Cluster.
NGC 4458 is an elliptical galaxy located about 54 million light-years away in the constellation of Virgo. It was discovered by astronomer William Herschel on April 12, 1784. NGC 4458 is a member of Markarian's Chain which is part of the Virgo Cluster. It is in a pair with the galaxy NGC 4461.
IC 1459 (also catalogued as IC 5265) is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light years across. It was discovered by Edward Emerson Barnard in 1892.
NGC 1332 is an almost edge-on elliptical galaxy located in constellation of Eridanus. Situated about 70 million light years away, it is a member of the Eridanus cluster of galaxies, a cluster of about 200 galaxies. It is also the brightest member of the NGC 1332 Group. It was discovered by William Herschel on 9 December 1784.
NGC 1332 has a Hubble classification of E, which indicates it is an elliptical galaxy. It is moving from away from the Milky Way at a rate of 1,553 km/s. Its size on the night sky is 4.5' x 1.4' which is proportional to its real size of 92 000 ly. NGC 1332 is an early-type galaxy.
The giant elliptical galaxy ESO 325-G004. On the left (in the sense that the sequence is usually drawn) lie the ellipticals. Elliptical galaxies have relatively smooth, featureless light distributions and appear as ellipses in photographic images. They are denoted by the letter E, followed by an integer n representing their degree of ellipticity in the sky.
NGC 6041 is a giant elliptical galaxy located about 470 million light-years away in the constellation Hercules. NGC 6041 has an extended envelope that is distorted towards the galaxy pair Arp 122. NGC 6041 is the brightest galaxy (BCG) in the Hercules Cluster. The galaxy was discovered by astronomer Édouard Stephan on June 27, 1870.
NGC 1395 is an elliptical galaxy located in the constellation Eridanus. It is located at a distance of circa 75 million light years from Earth, which, given its apparent dimensions, means that NGC 1395 is about 130,000 light years across. It was discovered by William Herschel on November 17, 1784. It is a member of the Eridanus Cluster.
NGC 720 is an elliptical galaxy located in the constellation Cetus. It is located at a distance of circa 80 million light years from Earth, which, given its apparent dimensions, means that NGC 720 is about 110,000 light years across. It was discovered by William Herschel on October 3, 1785. The galaxy is included in the Herschel 400 Catalogue.
The stars of Segue 2 were probably among the first stars to form in the Universe. Currently, there is no star formation in Segue 2. Segue 2 is located near the edge of Sagittarius Stream and at the same distance. It may once have been a satellite of Sagittarius Dwarf Elliptical Galaxy or its star cluster.
This is a giant elliptical galaxy with a morphological classification of E1, indicating a flattening of 10%. The half-light radius is and the extinction-corrected total luminosity in the visual band is . The central mass-to-light ratio is 6.5, which steadily increases away from the core. The visible galaxy is surrounded by a massive dark matter halo.
GOODS-N-774 also called "Sparky", is a distant early galaxy which is in the process of core formation. The galaxy is massive and extremely compact, forming stars furiously. It is thought to be on its way to becoming a giant elliptical galaxy. This galaxy was discovered in 2014, and is some 11 billion light years distant.
There was another object called "Ursa Major Dwarf", discovered by Edwin Hubble in 1949. It was designated as Palomar 4. Due to its peculiar look, it was temporarily suspected to be either a dwarf spheroidal or elliptical galaxy. However, it has since been found to be a very distant (about 360,000 ly) globular cluster belonging to our galaxy.
NGC 4065 is an elliptical galaxy located 300 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 27, 1785. It was then rediscovered by John Herschel on April 29, 1832 and was listed as NGC 4057. NGC 4065 is the brightest member of the NGC 4065 Group.
NGC 821 is an E6 elliptical galaxy. It is unusual because it has hints of an early spiral structure, which is normally only found in lenticular and spiral galaxies. NGC 821 is 2.6 by 2.0 arcminutes and has a visual magnitude of 11.3. Its diameter is 61,000 light-years and it is 80 million light-years away.
The object had an apparent size up to 50″ in the near infrared but was not visible on the corresponding blue light sensitive plate. Its spectrum lacked any emission or absorption lines. Later it was shown to be radio-quiet as well. In 1970 Hyron Spinrad suggested that Maffei 1 is a nearby heavily obscured giant elliptical galaxy.
Picture of the galaxy taken by Hubble space telescope NGC 4589 is an elliptical galaxy located in the constellation Draco. It is at a distance of about 108 million light-years away from the Earth. It is known as PGC 42139 or UGC 7797. In the center of NGC 4589 lies a supermassive black hole in its center.
Planetary nebula Abell 33 captured using ESO's Very Large Telescope. Elliptical galaxy NGC 3923. Hydra contains three Messier objects. M83, also known as the Southern Pinwheel Galaxy, is located on the border of Hydra and Centaurus, M68 is a globular cluster near M83, and M48 is an open star cluster in the western end of the serpent.
NGC 996 is an elliptical galaxy of the Hubble type E0 in the constellation Andromeda. It is estimated to be 210 million light years from the Milky Way and has a diameter of approximately 75,000 ly. The supernova SN 1996bq occurred in this galaxy. NGC 996 was discovered on December 7, 1871 by astronomer Édouard Stephan.
NGC 4881 is an elliptical galaxy in the northern constellation of Coma Berenices. It was discovered by the German astronomer Heinrich Louis d'Arrest on April 22, 1865. John L. E. Dreyer described it as "faint, small, a little extended, 9th magnitude star to southwest". This object is located at a distance of approximately from the Milky Way.
NGC 7196 is an elliptical galaxy registered in the New General Catalogue. It is located in the direction of the Indus constellation, at a distance of circa 150 million light years. It was discovered by the English astronomer John Herschel in 1834 using a 47.5 cm (18.7 inch) reflector. NGC 7196 appears slightly distorted, with asymmetric outer isophotes.
Small galaxies coalesced with large galaxies more frequently. Note that the Milky Way and the Andromeda Galaxy are predicted to collide in about 4.5 billion years. The expected result of these galaxies merging would be major as they have similar sizes, and will change from two "grand design" spiral galaxies to (probably) a giant elliptical galaxy.
NGC 78 is a pair of galaxies in the constellation Pisces. NGC 78A, which is the more southern galaxy, is a barred spiral galaxy. NGC 78B, which is the more northern galaxy, is an elliptical galaxy. Although the designations NGC 78A and 78B are used today, the designation NGC 78 was formerly used mainly for the northern galaxy.
NGC 3597 is the product of a collision between two galaxies. It is evolving into a giant elliptical galaxy. It is widely accepted that the merging of smaller galaxies due to gravitational attraction plays a major role in shaping the growth and evolution of elliptical galaxies. Such major galactic mergers are thought to have been more common at early times.
NGC 1399 is a large elliptical galaxy in the Southern constellation Fornax, the central galaxy in the Fornax cluster. The galaxy is 66 million light- years away from Earth. With a diameter of 130 000 light-years, it is one of the largest galaxies in the Fornax cluster and slightly larger than Milky Way. William Herschel discovered this galaxy on October 22, 1835.
She is an American Astronomical Society ambassador. During her doctoral studies, Mutlu-Pakdil discovered the galaxy PGC 1000714, which has been nicknamed "Burçin's galaxy". PGC 1000714 is an extremely rare double ringed elliptical galaxy, and her discovery generated extensive media coverage. She worked with the North Carolina Museum of Natural Sciences to create a series of short scientific films for the general public.
The X-ray jets of Centaurus A are thousands of light-years long, while the radio jets are over a million light- years long. Like other starburst galaxies, a collision is suspected to be responsible for the intense burst of star formation. Models have suggested that Centaurus A was a large elliptical galaxy that collided and merged with a smaller spiral galaxy.
NGC 3384 is an elliptical galaxy in the constellation Leo. The galaxy was discovered by William Herschel in 1784 as part of the Herschel 400 Catalogue. The high age of the stars in the central region of NGC 3384 was confirmed after analysis of their color. More than 80% were found to be Population II stars which are over a billion years old.
NGC 3109 is a small barred Magellanic type spiral or irregular galaxy around 4.34 Mly away in the direction of the constellation of Hydra. NGC 3109 is believed to be tidally interacting with the dwarf elliptical galaxy Antlia Dwarf.Grebel, Gallagher, Harbeck, p.7 It was discovered by John Herschel on March 24, 1835 while he was in what is now South Africa.
CGCG 049-033 is an elliptical galaxy, located some 680 million light-years from Earth, in the constellation of Serpens. It is the central galaxy (BCG) of the galaxy cluster Abell 2040. CGCG 049-033 is known for having the longest galactic jet ever discovered. The beam is about 1.5 million light-years long and was discovered in December 2007.
NGC 4093 is an elliptical galaxy located 340 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer Heinrich d'Arrest on May 4, 1864. NGC 4093 is a member of the NGC 4065 Group and is a radio galaxy with a two sided jet. A rotating disk in the galaxy was detected by K. Geréb et al.
NGC 71 is an elliptical galaxy located in the constellation Andromeda. It is in the NGC 68 group. The galaxy was discovered by R. J. Mitchell in 1855, and observed in 1865 by Heinrich d'Arrest, who described it as "extremely faint, very small, round". The galaxy is about 110,000-130,000 light years across, making it just slightly larger than the Milky Way.
NGC 4318 is a small lenticular galaxy located about 72 million light-years away in the constellation Virgo. It was discovered by astronomer John Herschel on January 18, 1828. NGC 4318 is a member of the Virgo W′ group, a group of galaxies in the background of the Virgo Cluster that is centered on the giant elliptical galaxy NGC 4365.
NGC 4473 is an elliptical galaxy located about 50 million light-years away in the constellation of Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784. NGC 4473 has an inclination of about 71°. NGC 4473 is a member of a chain of galaxies called Markarian's Chain which is part of the larger Virgo Cluster of galaxies.
NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across. It was discovered by William Herschel on February 23, 1784. NGC 4636 lies one and a half degrees southwest of Delta Virginis.
NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. It lies near 110 Virginis and is part of the Herschel 400 Catalogue.
NGC 759 is an elliptical galaxy located 230 million light-years away in the constellation Andromeda. NGC 759 was discovered by astronomer by Heinrich d'Arrest on September 17, 1865. It is a member of Abell 262. Despite being classified as a radio galaxy, the radio emission in NGC 759 could be due to star formation rather than an active galactic nucleus.
Abell 569 is a galaxy cluster in the northern constellation of Lynx. It is organized into two primary condensations that are separated by about 1.5 Mpc, and is probably a member of the Perseus Supercluster. The brightest galaxy in the cluster is NGC 2329, a giant elliptical galaxy of type D that is associated with a radio and X-ray source.
NGC 386 is an elliptical galaxy located in the constellation Pisces. It was discovered on November 4, 1850 by Bindon Stoney. It was described by Dreyer as "considerably faint, small, round." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385, NGC 387 and NGC 388, NGC 386 forms a galaxy cluster called Arp 331.
NGC 387 is an elliptical galaxy located in the constellation Pisces. It was discovered on December 10, 1873 by Lawrence Parsons. It was described by Dreyer as "very faint, small, round." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386 and NGC 388, NGC 387 forms a galaxy cluster called Arp 331.
NGC 388 is an elliptical galaxy located in the constellation Pisces. It was discovered on November 4, 1850 by Bindon Stoney. It was described by Dreyer as "very faint, small, round." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386 and NGC 387, NGC 388 forms a galaxy cluster called Arp 331.
An inflow of material toward the central bar of the galaxy causes new stars to be created in the ring. The ring is approximately 5,000 light-years in diameter, the spiral arms of the galaxy extend tens of thousands of light-years beyond the ring. NGC 1097 has two satellite galaxies, NGC 1097A and NGC 1097B. Dwarf elliptical galaxy NGC 1097A is the larger of the two.
Elliptical galaxies have central supermassive black holes, and the masses of these black holes correlate with the galaxy's mass. Elliptical galaxies have two main stages of evolution. The first is due to the supermassive black hole growing by accreting cooling gas. The second stage is marked by the black hole stabilizing by suppressing gas cooling, thus leaving the elliptical galaxy in a stable state.
Though they are visible as fuzzy objects in small telescopes, their structure is only visible in larger instruments. M95 is a barred spiral galaxy. M105 is about a degree away from the M95/M96 pair; it is an elliptical galaxy of the 9th magnitude, also about 20 million light-years from Earth. NGC 2903 is a barred spiral galaxy discovered by William Herschel in 1784.
Once there, the stars, gas, dust and dark matter of the large galaxy and its trailing galaxies will join with those of other galaxies who preceded them in the same fate. A giant or supergiant diffuse or elliptical galaxy will result from this accumulation. The centers of merged or merging galaxies can remain recognizable for long times, appearing as multiple "nuclei" of the cD galaxy.
The Sculptor Dwarf Galaxy (also known as Sculptor Dwarf Elliptical Galaxy or the Sculptor Dwarf Spheroidal Galaxy, and formerly as the Sculptor System) is a dwarf spheroidal galaxy that is a satellite of the Milky Way. The galaxy lies within the constellation Sculptor. It was discovered in 1937 by American astronomer Harlow Shapley using the 24-inch Bruce refractor at Boyden Observatory.Shapley, H., (1938) Harvard Bull. 908.
NGC 4623 is an edge-on lenticular or elliptical galaxy located about 54 million light-years away in the constellation of Virgo. NGC 4623 is classified as an E7, a rare type of "late" elliptical that represents the first stage of transition into a lenticular galaxy. NGC 4623 was discovered by astronomer William Herschel on April 13, 1784. NGC 4623 is a member of the Virgo Cluster.
This galaxy has a morphological classification of E1, indicating a standard elliptical galaxy with a flattening of 10%. The major axis is aligned along a position angle of 71°. Isophotes of the galaxy are near perfect ellipses, twisting no more than 5° out of alignment, with changes in ellipticity of no more than 0.06. There is no fine structure apparent in the isophotes, such as ripples.
ESO 306-17 is a fossil group giant elliptical galaxy in the Columba constellation, about 1 million light-years in diameter, and 493 million light- years away.MSNBC, "A Giant Among Galaxies ?" , Alan Boyle, 4 March 2010 (accessed 5 March 2010) The galaxy is situated alone in a volume of space about it. It is theorized that the galaxy cannibalized its nearest companions, hence, being a fossil group.
This is an elliptical galaxy of type E1/2 (E1.5), although some sources class it as S0 – a lenticular galaxy. An E2 class indicates a flattening of 20%, which has a nearly round appearance. The isophotes of the galaxy are boxy in shape, rather than simple ellipses. The mass-to-light ratio is a near constant 9.5 in the V (visual) band of the UBV system.
NGC 5010 is a lenticular galaxy located about 140 million light years away, in the constellation Virgo. It is considered a LIRG (Luminous Infrared Galaxy). As the galaxy has few young blue stars and mostly red old stars and dust, it is transitioning from being a spiral galaxy to being an elliptical galaxy, with its spiral arms having burned out and become dusty arms.
NGC 375 is an elliptical galaxy located in the constellation Pisces. It was discovered on September 12, 1784 by William Herschel. It was described by Dreyer as "pretty faint, small, round, brighter middle." Along with galaxies NGC 379, NGC 380, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386, NGC 387 and NGC 388, NGC 375 forms a galaxy cluster called Arp 331.
It has a low surface brightness and has a diameter of 4.5 arcminutes. It is not perfectly circular, rather, it is elliptical and oriented on a west-northwest/east-southeast axis. However, it is of fairly uniform brightness throughout. Another notable galaxy is NGC 4993, an elliptical galaxy which was the source of events GW170817, GRB 170817A and SSS17a from the merger of two neutron stars.
These features are commonly associated with many active galaxies. The axial ratio of the elliptical galaxy is 1.4, meaning it is about 1.4 times large along the primary axis than along the perpendicular axis. At the nucleus of this galaxy is a supermassive black hole with an estimated solar masses. The dimensionless ratio of the black hole spin to the black hole mass-energy j is .
IC 2006 is an elliptical galaxy in the constellation Eridanus. The galaxy was discovered on 3 October 1897 by the American astronomer Lewis A. Swift. It is estimated to be around 60 to 70 million light years (20 megaparsecs) away, in the Fornax Cluster. The galaxy is one of the smaller in the Fornax cluster, with a diameter of only 35 000 light-years.
NGC 3640 is an elliptical galaxy located in the constellation Leo. It is located at a distance of circa 75 million light years from Earth, which, given its apparent dimensions, means that NGC 3640 is about 90,000 light years across. It was discovered by William Herschel on February 23, 1784. It lies 2 degrees south of Sigma Leonis and is a member of the Herschel 400 Catalogue.
NGC 380 is an elliptical galaxy located in the constellation Pisces. It was discovered on September 12, 1784 by William Herschel. It was described by Dreyer as "pretty faint, small, round, suddenly brighter middle." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386, NGC 387 and NGC 388, NGC 380 forms a galaxy cluster called Arp 331.
The Hercules Cluster (Abell 2151) is a cluster of about 200 galaxies some 500 million light-years distant in the constellation Hercules. It is rich in spiral galaxies and shows many interacting galaxies. The cluster is part of the larger Hercules Supercluster, which is itself part of the much larger Great Wall super-structure. The cluster's brightest member is the giant elliptical galaxy NGC 6041.
As of 2014, the group is the smallest mass object to exhibit separation between its dark matter and baryonic matter components. The galaxy group is dominated by one elliptical galaxy, situated in one of the two concentrations, while the other node has two large bright galaxies, which do not dominate the group. The group has an apparent radius of 200 arcseconds, and a virial radius of 1 megaparsec.
Another galaxy cluster in the constellation, RX J1532.9+3021, is approximately 3.9 billion light-years from Earth. At the cluster's center is a large elliptical galaxy containing one of the most massive and most powerful supermassive black holes yet discovered. Abell 2065 is a highly concentrated galaxy cluster containing more than 400 members, the brightest of which are 16th magnitude; the cluster is more than one billion light-years from Earth.
NGC 7603 is a spiral Seyfert galaxy in the constellation Pisces. It is listed (as Arp 92) in the Atlas of Peculiar Galaxies. It is interacting with the smaller elliptical galaxy PGC 71041 nearby. This galaxy pair has long been a cornerstone for those who are critical of the view that the universe is expanding, and advocates for Non-standard cosmology such as Halton Arp, Fred Hoyle, and others.
Pegasus is also noted for its more unusual galaxies and exotic objects. Einstein's Cross is a quasar that has been lensed by a foreground galaxy. The elliptical galaxy is 400 million light-years away with a redshift of 0.0394, but the quasar is 8 billion light-years away. The lensed quasar resembles a cross because the gravitational force of the foreground galaxy on its light creates four images of the quasar.
NGC 4555 is a solitary elliptical galaxy about 40,000 parsecs (125,000 light- years) across, and about 310 million light years distant. Observations by the Chandra X-ray Observatory have shown it to be surrounded by a halo of hot gas about 120,000 parsecs across. The hot gas has a temperature of around 10,000,000 kelvins. The galaxy is one of the few elliptical galaxies proven to have significant amounts of dark matter.
Messier 85 (also known as M85 or NGC 4382 or PGC 40515 or ISD 0135852) is a lenticular galaxy, or elliptical galaxy for other authors, in the Coma Berenices constellation. It is 60 million light-years away, and it is estimated to be 125,000 light-years across. It was discovered by Pierre Méchain in 1781. It is the northernmost outlier of the Virgo cluster discovered as of 2004.
This galaxy has a morphological classification of pec dE5, indicating a dwarf elliptical galaxy with a flattening of 50%. M110 is designated peculiar because there are patches of dust and young blue stars located near the center. This is unusual for dwarf elliptical galaxies in general, and the reason for this peculiarity is unclear. Unlike M32, M110 does not show evidence for a supermassive black hole at its center.
An early stage merger in this case can also be identified as a LIRG. After that, it becomes a late stage merger, which is a ULIRG. It then becomes a quasar and in the final stage of the evolution it becomes an elliptical galaxy. This can be evidenced by the fact that stars are much older in elliptical galaxies than those found in the earlier stages of the evolution.
NGC 4278 is an elliptical galaxy. Its nucleus has been found to be active (AGN) and based on its spectrum has been identified as a LINER. The most accepted theory for the power source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. In the centre of NGC 4278 lies a supermassive black hole with an estimated mass based on stellar velocity dispersion.
NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 seyfert galaxy. NGC 708 is surrounded by 4700 globular clusters.
Charles Messier listed both in the Messier Catalogue about three days after Koehler's discovery. This is an elliptical galaxy of type E5 with a position angle of 163.3°, indicating the overall shape shows a flattening of 50%. However, isophotes for this galaxy deviate from a perfect ellipticity, showing pointed shapes instead. These can be decomposed mathematically into a three component model, with each part having a different eccentricity.
NGC 1549 is an elliptical galaxy located in the constellation Dorado. It is located at a distance of circa 50 million light years from Earth, which, given its apparent dimensions, means that NGC 1549 is about 75,000 light years across. NGC 1549 was discovered by John Herschel on 6 December 1835 and may have been observed by James Dunlop in 1826. It is a member of the Dorado Group.
NGC 5090 and NGC 5091 are a set of galaxies approximately away in the constellation Centaurus. They are in the process of colliding and merging with some evidence of tidal disruption of NGC 5091. NGC 5090 is an elliptical galaxy while NGC 5091 is a barred spiral galaxy. The radial velocity of the nucleus of NGC 5090 has been measured at , while NGC 5091 has a radial velocity of .
NGC 1142 and NGC 1141 imaged by the Sloan Digital Sky Survey NGC 1142 (also known as NGC 1144) is a distorted spiral galaxy in the constellation of Cetus. It is located about 370 million light years away from Earth, which means, given its apparent dimensions, that NGC 1142 is approximately 170,000 light years across. It is a type 2 Seyfert galaxy. It interacts with the elliptical galaxy NGC 1141.
When measured in the optical band, this galaxy has a redshift value of z = 0.428, corresponding to a distance of 1.5 Gpc. 3C 244.1 is located within a cluster of other galaxies. Observations with the Hubble Space Telescope show an elliptical galaxy with blobs and a filamentary structure. The radio jets being generated by the active galactic nucleus are interacting with the interstellar medium, producing extended narrow line regions.
X-shaped (or "winged") radio galaxies are a class of extragalactic radio source that exhibit two, low-surface-brightness radio lobes (the "wings") oriented at an angle to the active, or high-surface-brightness, lobes. Both sets of lobes pass symmetrically through the center of the elliptical galaxy that is the source of the lobes, giving the radio galaxy an X-shaped morphology as seen on radio maps.
It is a member of the Coma cluster of galaxies, positioned around to the north of the cluster's center with no nearby galactic neighbors. The morphological class of this galaxy is E0, indicating it is an elliptical galaxy with a spherically symmetric form. It does not display any unusual or peculiar features. A total of 88 globular cluster candidates have been identified orbiting this galaxy, which yields an estimated total of .
NGC 5846 is a giant elliptical galaxy with a round shape. It has a low luminosity active galactic nucleus, whose categorisation is ambiguous, having features that are observed both in LINER and HII regions. The source of nuclear activity in galaxies is suggested to be a supermassive black hole that accretes material. NGC 5846 harbors a supermassive black hole with estimated mass based on the central velocity dispersion.
The publication of their discovery was delayed by 10 years and was published in 1876 with the work Über einige im Cape-Catalog fehlende Nebel. NGC 1381 lies at the core of the Fornax Cluster. It lies within a region with increased density of candidate globular clusters nearly half a degree across that connects the elliptical galaxy NGC 1399 with its surrounding galaxies like NGC 1404, NGC 1387, and NGC 1380B.
Messier 49 (also known as M 49 or NGC 4472) is an elliptical galaxy located about away in the equatorial constellation of Virgo. This galaxy was discovered by French astronomer Charles Messier on February 16, 1777. As an elliptical galaxy, Messier 49 has the physical form of a radio galaxy, but it only has the radio emission of a normal galaxy. From the detected radio emission, the core region has roughly 1053 erg (1046 J or 1022 YJ) of synchrotron energy. The nucleus of this galaxy is emitting X-rays, suggesting the likely presence of a supermassive black hole with an estimated mass of , or 565 million times the mass of the Sun. X-ray emissions shows a structure to the north of Messier 49 that resembles a bow shock. To the southwest of the core, the luminous outline of the galaxy can be traced out to a distance of 260 kpc. The only supernova event observed within this galaxy is SN 1969Q, discovered in June 1969.
Close view with HST NGC 3597 is thought to be the product of the collision of two large galaxies, and it appears to be slowly evolving to become an elliptical galaxy. Because of this, NGC 3597 is interesting to astronomers. Galaxies smashing together pool their available gas and dust, triggering new rounds of star birth. Some of this material ends up in dense pockets initially called proto-globular clusters, dozens of which festoon NGC 3597.
The galaxy has been observed with the InfraRed Spectrograph (IRS) onboard Spitzer Space Telescope, examining the dust features of NGC 4278. Multiphase gas and dust have been observed in the same elongated features. Another uncommon finding for an elliptical galaxy is the detection of emission by polycyclic aromatic hydrocarbons (PAHs) and of strong [Si II] 34.8-μm emission. PAHs in other elliptical galaxies are believed to be destroyed by the hot interstellar medium.
APM 08279+5255 is a very distant, broad absorption line quasar located in the constellation Lynx. It is magnified and split into multiple images by the gravitational lensing effect of a foreground galaxy through which its light passes. It appears to be a giant elliptical galaxy with a supermassive black hole and associated accretion disk. It possesses large regions of hot dust and molecular gas, as well as regions with starburst activity.
It may be the closest giant elliptical galaxy. Maffei 1 lies in the Zone of Avoidance and is heavily obscured by the Milky Way's stars and dust. If it were not obscured, it would be one of the largest (about 3/4 the size of the full moon), brightest, and best-known galaxies in the sky. It can be observed visually, using a 30–35 cm or bigger telescope under a very dark sky.
This interacting galaxy was found 1.4 billion light years away in the center of Abell 3827. A huge halo of stars is surrounding its interacting nuclei. It has immense gravity that holds the cluster together due to its mass. Its unusual shape has led to the conclusion that each one of the nuclei was formed from multiple collisions of smaller galaxies, and now the nuclei are merging to form a single huge elliptical galaxy.
NGC 6045 is very luminous in both X-ray and Infrared light. This high luminosity in both X-ray and Infrared has been suggested to be the result of a starburst event in the galaxy. It is thought that starburst events are caused by interactions or mergers with other galaxies. Also, NGC 6045 has a warped disk which may be due to an interaction with the elliptical galaxy NGC 6047 which lies around ~ from the galaxy.
The stream lies within the Milky Way, approximately 10 kiloparsecs (30,000 light- years) from the Sun, and extending over a region of space at least 10 kpc across in three dimensions. It is close on the plane of the sky to the Sagittarius Dwarf Elliptical Galaxy, which was found in 1994 through a similar photometric analysis of a star survey.Ibata, R. A., et al., 1994, A Dwarf Satellite Galaxy in Sagittarius, Nature, Volume 370, Number 6486, p. 194.
Clusters of galaxies consist of hundreds to thousands of galaxies bound together by gravity. Clusters of galaxies are often dominated by a single giant elliptical galaxy, known as the brightest cluster galaxy, which, over time, tidally destroys its satellite galaxies and adds their mass to its own. Superclusters contain tens of thousands of galaxies, which are found in clusters, groups and sometimes individually. At the supercluster scale, galaxies are arranged into sheets and filaments surrounding vast empty voids.
It measures 7 arcminutes by 1 arcminute. It likely originated as a spiral galaxy and underwent a catastrophic gravitational interaction with Centaurus A around 500 million years ago, stopping its rotation and destroying its structure. NGC 4650A is a polar-ring galaxy 136 million light-years from Earth (redshift 0.01). It has a central core made of older stars that resembles an elliptical galaxy, and an outer ring of young stars that orbits around the core.
NGC 4709 is an elliptical galaxy located in the constellation Centaurus. It is considered to be a member of the Centaurus Cluster and is the dominant member of a small group of galaxies known as "Cen 45" which is currently merging with the main Centaurus Cluster (Cen 30) even though the two subclusters' line of sight redshift velocities differ by about 1500 km/s. NGC 4709 was discovered by astronomer James Dunlop on May 7, 1826.
Arp 147 (also known as IC 298) is an interacting pair of ring galaxies. It lies 430 million to 440 million light years away in the constellation Cetus and does not appear to be part of any significant galaxy group. The system was originally discovered in 1893 by Stephane Javelle and is listed in the Atlas of Peculiar Galaxies. The system was formed when a spiral galaxy (image right) collided with an elliptical galaxy (image left).
This galaxy has a large collection of globular clusters, estimated at about 5,900. By contrast, this count is far more than the roughly 200 orbiting the Milky Way, but is exceeded by the 13,450 globular clusters orbiting the supergiant elliptical galaxy Messier 87. On average, the globular clusters of M 49 are about 10 billion years old. Between 2000 and 2009, strong evidence for a stellar mass black hole was discovered in an M 49 cluster.
A likely outcome of the collision is that the galaxies will merge to form a giant elliptical galaxy or perhaps even a large disc galaxy. Such events are frequent among the galaxies in galaxy groups. The fate of the Earth and the Solar System in the event of a collision is currently unknown. Before the galaxies merge, there is a small chance that the Solar System could be ejected from the Milky Way or join the Andromeda Galaxy.
NGC 2936 is an interacting spiral galaxy located at a distance of 326 million light years, in the constellation Hydra. NGC 2936 is interacting with elliptical galaxy NGC 2937, located just beneath it. They were both discovered by Albert Marth on Mar 3, 1864.. To some astronomers, the galaxy looks like a penguin or a porpoise. NGC 2936, NGC 2937, and PGC 1237172 are included in the Atlas of Peculiar Galaxies as Arp 142 in the category "Galaxy triplet".
Image of the disk of the black hole in the center of the supergiant elliptical galaxy Messier 87 An accretion disk is a structure (often a circumstellar disk) formed by diffuse material in orbital motion around a massive central body. The central body is typically a star. Friction causes orbiting material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material, causing the emission of electromagnetic radiation.
These units are much larger, and are not merely a one-off creation of stars which allows their age to be determined in this fashion. The creation of stars in a galaxy takes place over billions of years, even though star production may long since have ceased (see elliptical galaxy). The oldest stars in a galaxy can only set a minimum age for the galaxy (when star formation began) but by no means determine the actual age.
NGC 680, an elliptical galaxy with an asymmetrical boundary, is the brighter of the two at magnitude 12.9; NGC 678 has a magnitude of 13.35. Both galaxies have bright cores, but NGC 678 is the larger galaxy at a diameter of 171,000 light-years; NGC 680 has a diameter of 72,000 light-years. NGC 678 is further distinguished by its prominent dust lane. NGC 691 itself is a spiral galaxy slightly inclined to our line of sight.
Maffei 1 is mainly made of old metal-rich stars more than 10 billion years in age. As a large elliptical galaxy, Maffei 1 is expected to host a significant population of globular clusters (about 1100). However, due to heavy intervening absorption, ground- based observations for a long time failed to identify any of them. Observations by the Hubble Space Telescope in 2000 revealed about 20 globular cluster candidates in the central region of the galaxy.
M110 is classified as either a dwarf spheroidal galaxy or simply a generic elliptical galaxy. It is far fainter than M31 and M32, but larger than M32 with a surface brightness of 13.2, magnitude of 8.9, and size of 21.9 by 10.9 arcminutes. The Andromeda Galaxy has a total of 15 satellite galaxies, including M32 and M110. Nine of these lie in a plane, which has caused astronomers to infer that they have a common origin.
The Sextans Dwarf Spheroidal is a dwarf spheroidal galaxy that was discovered in 1990 by Mike Irwin as the 8th satellite of the Milky Way, located in the constellation of Sextans. It is also an elliptical galaxy, and displays a redshift because it is receding from the Sun at 224 km/s (72 km/s from the Galaxy). The distance to the galaxy is 320,000 light-years and the diameter is 8,400 light-years along its major axis.
The Sagittarius Dwarf Irregular Galaxy (SagDIG) is a dwarf galaxy in the constellation of Sagittarius. (SagDIG should not be confused with the Sagittarius Dwarf Elliptical Galaxy, SagDEG, a satellite galaxy of the Milky Way discovered decades later in the same constellation.) It lies about 3.4 million light-years away. It was discovered by Cesarsky et al. on a photographic plate taken for the ESO (B) Atlas on 13 June 1977 using the ESO 1 meter Schmidt telescope.
The globular cluster NGC 6584 lies near Theta Arae and is 45,000 light-years distant from Earth. It is an Oosterhoff type I cluster, and contains at least 69 variable stars, most of which are RR Lyrae variables. The planetary nebula IC 4699 is of 13th magnitude and lies midway between Alpha and Epsilon Telescopii. IC 4889 is an elliptical galaxy of apparent magnitude 11.3, which can be found 2 degrees north-north-west of 5.3-magnitude Nu Telescopii.
IC 1101 is a supergiant elliptical galaxy in the Abell 2029 galaxy cluster located about from Earth. At the diameter of 5.5 million light-years or more than 50 times the size of the Milky Way, it was the largest known galaxy in the universe. Virgo is also home to the quasar 3C 273 which was the first quasar ever to be identified. With a magnitude of ~12.9, it is also the optically brightest quasar in the sky.
Under these conditions, enormous bursts of star formation are triggered, so rapid that most of the gas is converted into stars rather than the normal rate of 10% or less. Galaxies undergoing such rapid star formation are known as starburst galaxies. The post-merger elliptical galaxy has a very low gas content, and so H II regions can no longer form. Twenty-first century observations have shown that a very small number of H II regions exist outside galaxies altogether.
The stars of Com were probably among the first stars to form in the Universe and currently there is no star formation in Com. The measurements have so far failed to detect any neutral hydrogen in it—the upper limit is only 46 solar masses. Coma Dwarf is located near the Sagittarius Stream, which is made of stars stripped from the Sagittarius Dwarf Elliptical Galaxy. This association may indicate that Com is a former satellite of star cluster from that galaxy.
In the Local Group, the Milky Way and the Andromeda Galaxy are gravitationally bound, and currently approaching each other at high speed. Simulations show that the Milky Way and Andromeda are on a collision course, and are expected to collide in less than five billion years. During this collision, it is expected that the Sun and the rest of the Solar System will be ejected from its current path around the Milky Way. The remnant could be a giant elliptical galaxy.
Types of galaxies according to the Hubble classification scheme: an E indicates a type of elliptical galaxy; an S is a spiral; and SB is a barred-spiral galaxy.Galaxies to the left side of the Hubble classification scheme are sometimes referred to as "early-type", while those to the right are "late-type". Galaxies come in three main types: ellipticals, spirals, and irregulars. A slightly more extensive description of galaxy types based on their appearance is given by the Hubble sequence.
It is also called "the Coathanger" because of its distinctive star pattern when viewed with binoculars or a low power telescope. Planetary nebula Hen 2-437 is located in the constellation of Vulpecula. NGC 7052 is an elliptical galaxy in Vulpecula at a distance of 214 million light-years from Earth. It has a central dusty disk with a diameter of 3700 light-years; there is a supermassive black hole with a mass of 300 million solar masses in its nucleus.
Corona Australis' location near the Milky Way means that galaxies are uncommonly seen. NGC 6768 is a magnitude 11.2 object 35′ south of IC 1297. It is made up of two galaxies merging, one of which is an elongated elliptical galaxy of classification E4 and the other a lenticular galaxy of classification S0. IC 4808 is a galaxy of apparent magnitude 12.9 located on the border of Corona Australis with the neighbouring constellation of Telescopium and 3.9 degrees west-southwest of Beta Sagittarii.
NGC 5322 is an elliptical galaxy located in the constellation Ursa Major. It is located at a distance of circa 80 million light years from Earth, which, given its apparent dimensions, means that NGC 5322 is about 140,000 light years across. It was discovered by William Herschel on March 19, 1790. The galaxy has been found to possess an inner stellar disc and an edge-on nuclear dust disc across the centre, aligned along the major-axis of the galaxy.
Abell 2218 was used as a gravitational lens to discover the most distant known object in the universe as of 2004. The object, a galaxy some 13 billion years old, is seen from Earth as it would have been just 750 million years after the Big Bang.NBC News: "Galaxy ranks as most distant object in cosmos" The color of the lensed galaxies is a function of their distances and types. The orange arc is an elliptical galaxy at moderate redshift (z=0.7).
NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.
Deep images obtained with the CAFOS instrument at the Calar Alto Observatory reveal that NGC 4070 has some deviation from a perfectly spherical or ellipsoidal shape morphology. This indicates that NGC 4070 has undergone a recent interaction, either with the galaxy 2MASX J12040831+2023280 or with a small knot of material. There also appears to be faint, broad bridge of luminous matter between NGC 4070 and the neighbouring elliptical galaxy NGC 4066. The two galaxies are separated by a projected distance of .
One ultraluminous X-ray source has been detected in NGC 988. NGC 988 is the brightest galaxy in NGC 1052 group (which is also known as NGC 988 group),which also includes the elliptical galaxy NGC 1052, NGC 991, NGC 1022, NGC 1035, NGC 1042, NGC 1047, NGC 1051, NGC 1084, NGC 1110. It belongs in the same galaxy cloud as Messier 77. One supernova has been discovered in NGC 988, SN 2017gmr, a Type II supernova discovered on 4 September 2017.
Individual stars themselves rotate as they orbit, so the side approaching will be blueshifted and the side moving away will be redshifted. Stars also have random (as well as orbital) motion around the galaxy, meaning any individual star may depart significantly from the rest relative to its neighbours in the rotation curve. In spiral galaxies this random motion is small compared to the low-eccentricity orbital motion, but this is not true for an elliptical galaxy. Molecular-scale Doppler broadening will also contribute.
The structure and photometry of LEDA 1000714 was studied with significant detail in 2017. The core of the galaxy appears to be similar to an elliptical galaxy, and is almost perfectly round, not flattened into a disk. Unlike some ring galaxies, the central core shows no signs of a bar structure connecting the outer ring to the center of the galaxy. This is similar to Hoag's Object, and a number of other galaxies have been found that have a perfectly round center.
IC 1459 is a giant elliptical galaxy. In its core has been observed a fast counter-rotating stellar component, with an estimated total mass of . The stars of this component have circular orbits on a flat disk with a radius of less than two arcseconds. It has been suggested that the stars of the counterrotating disk are of external origin, either by the accretion of a stellar satellite or of a dense molecular cloud from which the stars were created.
The galaxy also features multiple shells and disturbed isophotes, which indicate that it has accreted material, probably by the merger of smaller galaxies with the elliptical galaxy. Enhanced photography revealed the presence of a diffuse spiral pattern at the outer regions of IC 1459. It has been suggested that a merger started a starburst event in IC 1459. The total duration of this event has not been well constrained, but it is estimated it lasted less than 80 million years.
NGC 547 is an elliptical galaxy and radio galaxy (identified as 3C 40) located in the constellation Cetus. It is located at a distance of circa 220 million light years from Earth, which, given its apparent dimensions, means that NGC 547 is about 120,000 light years across. It was discovered by William Herschel on October 1, 1785. It is a member of the Abell 194 galaxy cluster and is included along with NGC 547 in the Atlas of Peculiar Galaxies.
This galaxy is small and isolated with a morphological classification of SB(r)0+, which indicates a barred spiral (SB) with a ring around the bar (r). Being a lenticular galaxy, it has the large halo of an elliptical galaxy. The disk is inclined at an angle of to the line of sight from the Earth, with the major axis aligned along a position angle of . The galaxy has an unusually high mass-to-light ratio, much greater than for a typical spiral galaxy.
NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. Sir William Herschel already recognised them as a 'double nebula' and they were jointly listed as Holm 187 in the Catalogue of Double and Multiple Galaxies and as Arp 94 in the Atlas of Peculiar Galaxies.
Astronomers posit that its dust lanes, not common in elliptical galaxies, are due to a previous merger with another galaxy, probably a spiral galaxy. NGC 5128 appears in the optical spectrum as a fairly large elliptical galaxy with a prominent dust lane. Its overall magnitude is 7.0 and it has been seen under perfect conditions with the naked eye, making it one of the most distant objects visible to the unaided observer. In equatorial and southern latitudes, it is easily found by star hopping from Omega Centauri.
NGC 1379 is a low-luminosity elliptical galaxy in southern constellation Fornax. It was discovered by William Herschel on December 25, 1835. At a distance of 60 million light-years, it is one of the closer members of Fornax Cluster. It is a member of Fornax Cluster, and it is located about 24' from central galaxy, NGC 1399, as twice as NGC 1387, the galaxy next to the NGC 1379. NGC 1387 is also the closest galaxy to this, and it is in foreground from NGC 1379.
Centaurus A may be described as having a peculiar morphology. As seen from Earth, the galaxy looks like a lenticular or elliptical galaxy with a superimposed dust lane. The peculiarity of this galaxy was first identified in 1847 by John Herschel, and the galaxy was included in Halton Arp's Atlas of Peculiar Galaxies (published in 1966) as one of the best examples of a "disturbed" galaxy with dust absorption. The galaxy's strange morphology is generally recognized as the result of a merger between two smaller galaxies.
Elliptical galaxy Centaurus A and its globular clusters Centaurus A is located approximately 4° north of Omega Centauri (a globular cluster visible with the naked eye). Because the galaxy has a high surface brightness and relatively large angular size, it is an ideal target for amateur astronomy observations. The bright central bulge and dark dust lane are visible even in finderscopes and large binoculars, and additional structure may be seen in larger telescopes. Centaurus A is visible to the naked eye under exceptionally good conditions.
The Field of Streams is a patch of sky where several stellar streams are visible and crisscross. It was discovered by Vasily Belokurov and Daniel Zucker's team in 2006 by analyzing the Sloan Digital Sky Survey II (SDSS-II) data. The team named the area Field of Streams because of so many crisscrossing trails of stars.SDSS, "Multiple galaxy mergers continue in the Milky Way", 2006 May 8 (accessed 2009 March 29) The Sagittarius Stream of the Sagittarius Dwarf Elliptical Galaxy (SagDEG) dominates the Field.
Radio observations and Hubble Space Telescope images of M84 have revealed two jets of matter shooting out from the galaxy's center as well as a disk of rapidly rotating gas and stars indicating the presence of a supermassive black hole. It also has a few young stars and star clusters, indicating star formation at a very low rate. The number of globular clusters is , which is much lower than expected for an elliptical galaxy. Two supernovae have been observed in M84: SN 1957 and SN 1991bg.
NGC 3311 is a supergiant elliptical galaxy (a type-cD galaxy) located about 190 million light-years away in the constellation Hydra. The galaxy was discovered by astronomer John Herschel on March 30, 1835. NGC 3311 is the brightest member of the Hydra Cluster and forms a pair with NGC 3309 which along with NGC 3311, dominate the central region of the Hydra Cluster. NGC 3311 is surrounded by a rich and extensive globular cluster system rivaling that of Messier 87 in the Virgo Cluster.
This ring lies perpendicular to the plane of NGC 2768 itself, stretching up and out of the galaxy. The dust in NGC 2768 forms an intricate network of knots and filaments.Dusty detail in elliptical galaxy NGC 2768 8 April 2013, ESA/Hubble & NASA In the centre of the galaxy are two tiny, S-shaped symmetric jets. These two flows of material travel outwards from the galactic centre along curved paths, and are masked by the tangle of dark dust lanes that spans the body of the galaxy.
NGC 4631 has a nearby companion dwarf elliptical galaxy, NGC 4627. NGC 4627 and NGC 4631 together were listed in the Atlas of Peculiar Galaxies as an example of a "double galaxy" or a galaxy pair. NGC 4631 and NGC 4627 are part of the NGC 4631 Group, a group of galaxies that also includes the interacting galaxies NGC 4656 and NGC 4657. However, exact group identification is problematic because this galaxy and others lie in a part of the sky that is relatively crowded.
Robert Earl Jackson (born 1949) is a scientist, who, with Sandra M. Faber, in 1976 discovered the Faber–Jackson relation between the luminosity of an elliptical galaxy and the velocity dispersion in its center. Jackson was a graduate student at the University of California at Santa Cruz. As a Research Assistant for Faber, he contributed to the data analysis on the project that led to the Faber–Jackson relation (1976). Jackson received his Ph.D. in 1982 with the thesis titled "The Anisotropy of the Hubble Constant".
A giant galaxy interacting with its satellites is common. A satellite's gravity could attract one of the primary's spiral arms, or the secondary satellite's path could coincide with the position of the primary satellite's and so would dive into the primary galaxy (the Sagittarius Dwarf Elliptical Galaxy into the Milky Way being an example of the latter). That can possibly trigger a small amount of star formation. Such orphaned clusters of stars were sometimes referred to as "blue blobs" before they were recognized as stars.
After a while of dangerous investigating (for instance, sneaking into Mrs. Pearce's attic) they were approached by a man in a suit at a restaurant who told them to leave their teachers alone and then promptly burned a hole through the table they were sitting at with his finger. They disobeyed his order, however, and Charlie was kidnapped and taken to the Sagittarius Dwarf Elliptical Galaxy, where he had to fake happiness or else face certain death. But, Jimbo did not seem to know this.
NGC 7331, also known as Caldwell 30, is an unbarred spiral galaxy about away in the constellation Pegasus. It was discovered by William Herschel in 1784.The NGC/IC Project : NGC Discoverers List by Bob Erdmann. NGC 7331 is the brightest galaxy in the field of a visual grouping known as the NGC 7331 Group of galaxies. The other members of the group are the lenticular or unbarred spirals NGC 7335 and 7336, the barred spiral galaxy NGC 7337 and the elliptical galaxy NGC 7340.
Its size on the night sky is 4.8' x 0.8', indicating a real size of about 90,000 light-years, so PGC 13809 is slightly smaller than the Milky Way. It is also one of the larger galaxies in the Fornax Cluster, a cluster of 200 galaxies. Its magnitude is 12.6. With a redshift of 1838 km/s, it is one of the faster moving galaxies in the Fornax Cluster, but it is close to the central giant elliptical galaxy NGC 1399, so gravitational reaction is possible.
NGC 4889 (also known as Caldwell 35) is an E4 supergiant elliptical galaxy. It was discovered in 1785 by the British astronomer Frederick William Herschel I, who catalogued it as a bright, nebulous patch. The brightest galaxy within the northern Coma Cluster, it is located at a median distance of 94 million parsecs (308 million light years) from Earth. At the core of the galaxy is a supermassive black hole that heats the intracluster medium through the action of friction from infalling gases and dust.
Spindle Galaxy (NGC 5866), a lenticular galaxy with a prominent dust lane in the constellation of Draco. At the centre of the Hubble tuning fork, where the two spiral-galaxy branches and the elliptical branch join, lies an intermediate class of galaxies known as lenticulars and given the symbol S0. These galaxies consist of a bright central bulge, similar in appearance to an elliptical galaxy, surrounded by an extended, disk-like structure. Unlike spiral galaxies, the disks of lenticular galaxies have no visible spiral structure and are not actively forming stars in any significant quantity.
In the late 1970s, François Schweizer studied NGC 1316 extensively and found that the galaxy appeared to look like a small elliptical galaxy with some unusual dust lanes embedded within a much larger envelope of stars. The outer envelope contained many ripples, loops, and arcs. He also identified the presence of a compact disk of gas near the center that appeared inclined relative to the stars and that appeared to rotate faster than the stars. Based on these results, Schweizer considered that NGC 1316 was built up through the merger of several smaller galaxies.
NGC 1316 is located within the Fornax Cluster, a cluster of galaxies in the constellation Fornax. However, in contrast to Messier 87, which is a similar elliptical galaxy that is located in the center of the Virgo Cluster, NGC 1316 is located at the edge of the Fornax Cluster. NGC 1316 appears to be interacting with NGC 1317, a small spiral galaxy to the north. However, that small spiral galaxy does not appear to be sufficiently large enough to cause the distortions seen in the structure of this galaxy.
NGC 3923 Elliptical Shell Galaxy (Hubble photograph) A shell galaxy is a type of elliptical galaxy where the stars in the galaxy's halo are arranged in concentric shells. About one-tenth of elliptical galaxies have a shell-like structure, which has never been observed in spiral galaxies. The shell-like structures are thought to develop when a larger galaxy absorbs a smaller companion galaxy. As the two galaxy centers approach, the centers start to oscillate around a center point, the oscillation creates gravitational ripples forming the shells of stars, similar to ripples spreading on water.
The type-cD galaxySidereal Times, June 2002, page 3 (also cD-type galaxy,Proceedings of PATRAS 2008, page 59 cD galaxyGalaxy Clusters, Jan Hartlap, page 3) is a galaxy morphology classification, a subtype of type-D giant elliptical galaxy. Characterized by a large halo of stars,Surface Photometry and the Structure of Elliptical Galaxies, "Chapter 11. cD and Brightest Cluster Galaxies", John Kormendy, S. Djorgovski, 1989 they can be found near the centres of some rich galaxy clusters.A Dictionary of Astronomy, "cD galaxy" (accessed 14 April 2010) They are also known as supergiant ellipticalsencyclopedia.
PKS 1302-102 is a quasar in the Virgo constellation, located at a distance of approximately 1.1 Gpc (around 3.5 billion light-years). It has an apparent magnitude of about 14.9 mag in the V band with a redshift of 0.2784. The quasar is hosted by a bright elliptical galaxy, with two neighboring companions at distances of 3 kpc and 6 kpc. The light curve of PKS 1302-102 appears to be sinusoidal with an amplitude of 0.14 mag and a period of 1,884 ± 88 days, which suggests evidence of a supermassive black hole binary.
Centaurus A (also known as NGC 5128) is a galaxy in the constellation of Centaurus. It was discovered in 1826 by Scottish astronomer James Dunlop from his home in Parramatta, in New South Wales, Australia. There is considerable debate in the literature regarding the galaxy's fundamental properties such as its Hubble type (lenticular galaxy or a giant elliptical galaxy) and distance (10–16 million light-years). NGC 5128 is one of the closest radio galaxies to Earth, so its active galactic nucleus has been extensively studied by professional astronomers.
At a distance of 30,000 light-years, it has chains of stars extending to the north that are resolvable in small amateur telescopes. One galaxy group located in Capricornus is HCG 87, a group of at least three galaxies located 400 million light-years from Earth (redshift 0.0296). It contains a large elliptical galaxy, a face-on spiral galaxy, and an edge-on spiral galaxy. The face-on spiral galaxy is experiencing abnormally high rates of star formation, indicating that it is interacting with one or both members of the group.
Bootes II is located only 1.5 degrees (~1.6 kpc) away from another dwarf galaxy—Boötes I, although they are unlikely to be physically associated because they move in opposite directions relative to the Milky Way. Their relative velocity—about 200 km/s is too high. It is more likely associated with the Sagittarius Stream and, therefore, with the Sagittarius Dwarf Elliptical Galaxy (SagDEG). Bootes II may be either a satellite galaxy of SagDEG or one of its star clusters torn from the main galaxy 4–7 billion years ago.
NGC 1380 lies in the central part of the Fornax Cluster, 35 arcminutes northwest of the large elliptical galaxy NGC 1399. In the same field of view lie the galaxies NGC 1380A, NGC 1379, NGC 1381, NGC 1382, and NGC 1387. NGC 1380 lies 2 degrees north-northeast of Chi2 Fornacis and because of its high surface brightness can be spotted with a five inch telescope even from bright suburban skies. One supernova has been detected in NGC 1380, SN 1992A, a type Ia supernova with peak magnitude of 12.8.
The number of stars contained in the Andromeda Galaxy is estimated at one trillion (), or roughly twice the number estimated for the Milky Way. The Milky Way and Andromeda galaxies are expected to collide in around 4.5 billion years, merging to form a giant elliptical galaxy or a large lenticular galaxy. With an apparent magnitude of 3.4, the Andromeda Galaxy is among the brightest of the Messier objects, making it visible to the naked eye from Earth on moonless nights, even when viewed from areas with moderate light pollution.
M60 is the third-brightest giant elliptical galaxy of the Virgo cluster of galaxies, and is the dominant member of a subcluster of four galaxies, the M60 group, which is the closest-known isolated compact group of galaxies. It has several satellite galaxies, one of them being the ultracompact dwarf galaxy M60-UCD1, discovered in 2013. The motion of M60 through the intercluster medium is resulting in ram-pressure stripping of gas from the galaxy's outer halo, beyond a radius of 12 kpc. NGC 4647 appears approximately 2′.
NGC 2276 is an intermediate spiral galaxy in the constellation Cepheus. The galaxy lies 105 million light-years away from Earth. NGC 2276 has an asymmetrical appearance, most likely caused by gravitational interactions with its neighbor, elliptical galaxy NGC 2300. One of the many starburst spiral arms contains an intermediate mass black hole with 50,000 times the mass of the Sun, named NGC 2276-3c. NGC 2276-3c has produced two jets: a large-scale radio jet, approximately 2,000 light years long, and an "inner jet" about 6 light years long.
3C 66B is an elliptical Fanaroff and Riley class 1 radio galaxy located in the constellation Andromeda. With an estimated redshift of 0.021258, the galaxy is about 300 million light-years away. The orbital motion of 3C 66B showed supposed evidence for a supermassive black hole binary (SMBHB) with a period of 1.05 ± 0.03 years, but this claim was later proven wrong (at 95% certainty). Messier 87 (M87), about 55 million light years away, is the largest giant elliptical galaxy near the Earth, and also contains an active galactic nucleus.
Observing it through a 40 cm telescope will reveal its central region and halo. The Telescopium group is group of twelve galaxies spanning three degrees in the northeastern part of the constellation, lying around 37 megaparsecs (120 million light-years) from our own galaxy. The brightest member is the elliptical galaxy NGC 6868, and to the west lies the spiral galaxy (or, perhaps, lenticular galaxy) NGC 6861. These are the brightest members of two respective subgroups within the galaxy group, and are heading toward a merger in the future.
NGC 7049 is a lenticular galaxy that spans about 150,000 light-years and lies about 100 million light-years away from Earth in the inconspicuous southern constellation of Indus. NGC 7049's unusual appearance is largely due to a prominent rope-like dust ring which stands out against the starlight behind it. These dust lanes are usually seen in young galaxies with active star- forming regions. NGC 7049 shows the features of both an elliptical galaxy and a spiral galaxy, and has relatively few globular clusters, indicative of its status as a lenticular type.
11 Comae Berenices is a binary star system in the northern constellation of Coma Berenices, located in the sky, east and slightly north of Denebola in Leo, but not nearly as far east as ε Virginis in Virgo. It is about a degree from the elliptical galaxy M85 and two degrees north of the spiral galaxy M100. Based upon an annual parallax shift of , the star is located 305 light years away from the Sun. It is visible to the naked eye as a faint, orange- hued star with an apparent visual magnitude of 4.72.
The ages of the globular clusters in NGC 4636 vary from 2 to 15 billion years, with a bit more than a quarter of the clusters having ages less than 5 billion years. It has been suggested that the younger clusters were formed during the merging of smaller galaxies with the elliptical galaxy. The velocity dispersion of the clusters is km/s, with the velocity dispersion of the blue clusters being slightly larger. This velocity dispersion is similar to that of Messier 60, which is, however, a brighter galaxy.
NGC 3862 is an elliptical galaxy located 300 million light-years away in the constellation Leo. Discovered by astronomer William Herschel on April 27, 1785, NGC 3862 is an outlying member of the Leo Cluster. The galaxy is classified as a FR I radio galaxy and as a Head-tail radio galaxy. It hosts a supermassive black hole that is blasting a jet of plasma that is moving at 98 percent of the speed of light and is one of the few jets that can be seen in visible light.
Minor galactic mergers involve two galaxies of very different masses, and are not limited to giant ellipticals. The Milky Way galaxy, depending upon an unknown tangential component, is on a four- to five-billion-year collision course with the Andromeda Galaxy.Nagamine, Kentaro; Loeb, Abraham (2003), Future evolution of nearby large-scale structures in a universe dominated by a cosmological constant It has been theorized that an elliptical galaxy will result from a merger of the two spirals. It is believed that black holes may play an important role in limiting the growth of elliptical galaxies in the early universe by inhibiting star formation.
X-ray image of galaxy cluster Abell 2142 Corona Borealis contains few galaxies observable with amateur telescopes. NGC 6085 and 6086 are a faint spiral and elliptical galaxy respectively close enough to each other to be seen in the same visual field through a telescope. Abell 2142 is a huge (six million light-year diameter), X-ray luminous galaxy cluster that is the result of an ongoing merger between two galaxy clusters. It has a redshift of 0.0909 (meaning it is moving away from us at 27,250 km/s) and a visual magnitude of 16.0. It is about 1.2 billion light-years away.
Cygnus X is the largest star-forming region in the Solar neighborhood and includes not only some of the brightest and most massive stars known (such as Cygnus OB2-12), but also Cygnus OB2, a massive stellar association classified by some authors as a young globular cluster. More supernovae have been seen in the Fireworks Galaxy (NGC 6946) than in any other galaxy. Cygnus A is the first radio galaxy discovered; at a distance of 730 million light-years from Earth, it is the closest powerful radio galaxy. In the visible spectrum, it appears as an elliptical galaxy in a small cluster.
Several million years ago, it collided with a smaller galaxy, which created a region filled with young, hot, blue stars. Astronomers do not know if the collision was simply a glancing blow or a prelude to a full-on merger, which would end with the two galaxies incorporated into one larger, probably elliptical galaxy. A remarkable long-duration gamma-ray burst was GRB 050525A, which flared in 2005. The afterglow re-brightened at 33 minutes after the original burst, only the third found to exhibit such an effect in the timeframe, and unable to be completely explained by known phenomena.
The Antlia Dwarf is classified alternatively as a dwarf elliptical galaxy of type dE3.5, or either as a dwarf spheroidal galaxy (dSph) or as a transitional galaxy from spheroidal to irregular types (dSph/Irr). The last classification is due to a substantial star formation in this galaxy in the last 0.1 billion years. Antlia Dwarf comprises two components: a core and an old halo. Its half-light radius is about 0.25 kpc. The metallicity is very low, at about <[Fe/H]>=−1.6 to −1.9 meaning that Antlia Dwarf contains 40–80 times less heavy elements than the Sun.
Gravitational tidal effects may also drive gas inward and trigger a star burst in the core of the small galaxy, resulting in the high density of M32 observed today. There is evidence that M32 has a faint outer disk, and as such is not a typical elliptical galaxy. Newer simulations find that an off-centre impact by M32 around 800 million years ago explains the present-day warp in M31's disk. However this feature only occurs during the first orbital passage, whereas it takes many orbits for tides to transform a normal dwarf into M32.
Messier 88 seen by the 24 inch telescope on Mt. Lemmon, USA. M88 is one of the fifteen Messier objects that belong to the nearby Virgo Cluster of galaxies. It is galaxy number 1401 in the Virgo Cluster Catalogue (VCC) of 2096 galaxies that are candidate members of the cluster. M88 may be on a highly elliptical orbit that is carrying it toward the cluster center, which is occupied by the giant elliptical galaxy M87. It is currently 0.3–0.48 million parsecs from the center and will come closest to the core in about 200–300 million years.
1ES 1101-232 is an active galactic nucleus of a distant galaxy known as a blazar. An X-ray source (catalogued as A 1059-22) was first recorded by Maccagni and colleagues in a 1978 paper; they thought the source arose from a galaxy in the Abell 1146 galaxy cluster, which contained many giant elliptical galaxies. In 1989, Remillard and colleagues linked the X-ray source with a visual object and established that the object was surrounded by a large elliptical galaxy. They also discovered that the object (and galaxy) were more distant, with a redshift of 0.186.
HXMM01, known more formally as 1HERMES S250 J022016.5−060143, is a starburst galaxy located in the northwestern portion of the constellation Cetus.Inferred from right ascension and declination of galaxy using the Fourmilab Virtual Telescope. Discovered in 2013 by a team at the University of California, Irvine, it was discovered that HXMM01 is actually still forming from its two parent galaxies as part of the "brightest, most luminous and most gas-rich submillimeter-bright galaxy merger known." When the merger is complete, HXMM01 will rapidly evolve to become a giant elliptical galaxy with a mass about four times that of the Milky Way.
This new class of GRB-like events was first discovered through the detection of GRB 110328A by the Swift Gamma-Ray Burst Mission on 28 March 2011. This event had a gamma-ray duration of about 2 days, much longer than even ultra-long GRBs, and was detected in X-rays for many months. It occurred at the center of a small elliptical galaxy at redshift z = 0.3534. There is an ongoing debate as to whether the explosion was the result of stellar collapse or a tidal disruption event accompanied by a relativistic jet, although the latter explanation has become widely favoured.
After a while of Jimbo investigating Charlie's "Spudvetch!" notebook (their secret notebook for gathering information) he discovered that his best bet to find him would be on the Isle Of Skye, in Scotland. He and his sister, who he had managed to convince to come with him, eventually arrived there, although with much difficulty, and inside an abandoned shack, a mysterious portal opened. Jimbo got sucked into Sagittarius Dwarf Elliptical Galaxy, but his sister stayed on Earth, unaware. He found Charlie but the same guy from the restaurant discovers them and Charlie's fake happiness and imprisons them.
Machacek, et al. (2005), reported on a X-ray trail that exists between and the nearby elliptical galaxy . is moving away from at in approximately the same trajectory as the X-ray trail, suggesting a link between the two galaxies. Four possibilities for the trail's existence were given: gas stripped from the two galaxies during a close fly-by, intergalactic medium that has been gravitationally focused behind as it moves, interstellar medium that was stripped from by ram pressure as it passed through the densest part of the Pavo group, and interstellar medium stripped from by turbulent viscosity as it passes through Pavo.
Many of the brighter galaxies in this cluster, including the giant elliptical galaxy Messier 87, were discovered in the late 1770s and early 1780s and subsequently included in Charles Messier's catalogue of non- cometary fuzzy objects. Described by Messier as nebulae without stars, their true nature was not recognized until the 1920s. The cluster subtends a maximum arc of approximately 8 degrees centered in the constellation Virgo. Although some of the cluster's most prominent members can be seen with smaller instruments, a 6-inch telescope will reveal about 160 of the cluster's galaxies on a clear night.
The galaxy product of the collision has been nicknamed Milkomeda or Milkdromeda. According to simulations, this object will look like a giant elliptical galaxy, but with a centre showing less stellar density than current elliptical galaxies. It is, however, possible the resulting object will be a large lenticular galaxy, depending on the amount of remaining gas in the Milky Way and Andromeda. In the far future, roughly 150 billion years from now, the remaining galaxies of the Local Group will coalesce into this object, that being the next evolutionary stage of the local group of galaxies.
NGC 1142 is a spiral galaxy which interacts with the elliptical galaxy NGC 1141. The linear separation of the two galaxies is 40 arcseconds, which corresponds to about 20 kiloparsecs at the distance of NGC 1142. The closest encounter took place 22 million years before the observed moment and created a density wave across NGC 1142, which resulted in the formation of knots of gas and stars, and led to the distortion of the spiral galaxy, creating a knotty loop or ring that extends towards NGC 1141 and an off-centre nucleus. A stellar bridge connects the two galaxies.
NGC 4639 is a face-on barred spiral galaxy located from Earth (redshift 0.0034). Its outer arms have a high number of Cepheid variables, which are used as standard candles to determine astronomical distances. Because of this, astronomers used several Cepheid variables in NGC 4639 to calibrate type 1a supernovae as standard candles for more distant galaxies. NGC 4981 was discovered on 17 April 1784 by William Herschel. Virgo possesses several galaxy clusters, one of which is HCG 62. A Hickson Compact Group, HCG 62 is at a distance of from Earth (redshift 0.0137) and possesses a large central elliptical galaxy.
Elliptical galaxy NGC 4889 in front of hundreds of background galaxies. Giant elliptical galaxies like NGC 4889 are believed to be the result of multiple mergers of smaller galaxies. There is now little dust remaining to form the diffuse nebulae where new stars are created, so the stellar population is dominated by old, population II stars that contain relatively low abundances of elements other than hydrogen and helium. The egg- like shape of this galaxy is maintained by random orbital motions of its member stars, in contrast to the more orderly rotational motions found in a spiral galaxy such as the Milky Way.
NGC 2974 by GALEX in ultraviolet, where an outer ring becomes visible. NGC 2974 has been categorised by Gérard de Vaucouleurs as an elliptical galaxy, however there is evidence the galaxy has a disk. A rotating disk of neutral hydrogen with axis similar to that of the optical isophotes of the galaxy was detected in 1988 by Kim et al. They estimated the total HI mass to be . The galaxy in ultraviolet, as observed by GALEX, features an outer ring structure that holds about 1% of the total stellar mass of the galaxy and has a population of young stars.
It is a 10th magnitude galaxy associated with the Fornax Cluster. Fornax A is a radio galaxy with extensive radio lobes that corresponds to the optical galaxy NGC 1316, a 9th- magnitude galaxy. One of the closer active galaxies to Earth at a distance of 62 million light-years, Fornax A appears in the optical spectrum as a large elliptical galaxy with dust lanes near its core. These dust lanes have caused astronomers to discern that it recently merged with a small spiral galaxy. Because it has a high rate of type Ia supernovae, NGC 1316 has been used to determine the size of the universe.
NGC 720 is an elliptical galaxy with elongated shape in the northwest to southeast axis as seen from Earth. Observations by the Hubble Space Telescope of the core of NGC 720 did not reveal the presence of dust, disk, or inner spiral. As observed in X-rays by the Chandra X-ray Observatory in 2000, the galaxy features a slightly flattened, or ellipsoidal triaxial halo of hot gas that has an orientation different from that of the optical image of the galaxy. Its shape cannot be accounted for based on the observed mass, even when using the Modified Newtonian dynamics theory of gravity, which excludes the need for dark matter.
X-shaped galaxies are a sub-class of Fanaroff-Riley Type II (FRII) radio galaxies. FRII objects exhibit a pair of large (kiloparsec) scale radio lobes that straddle the parent elliptical galaxy; the lobes are believed to consist of plasma ejected from the center of the galaxy by jets associated with the accretion disk around the supermassive black hole. Unlike the classical FRII sources, the X-shaped galaxies exhibit two, misaligned pairs of radio lobes of comparable extent. One pair of lobes, the "active" lobes, have a relatively high surface brightness and appear to be generated by ongoing emission from the center of the galaxy.
Messier 105 or M105, also known as NGC 3379, is an elliptical galaxy located 36.6 million light years away in the equatorial constellation of Leo. It was discovered by Pierre Méchain on 24 March 1781, just a few days after he discovered the nearby galaxies Messier 95 and Messier 96. This galaxy is one of several that were not originally included in the original Messier Catalogue compiled by Charles Messier. Messier 105 was included in the catalog only when Helen S. Hogg found a letter by Méchain describing Messier 105 and when the object described by Méchain was identified as a galaxy previously named NGC 3379.
The surface brightness profile of Maffei 1 in the blue (B-band) and near infrared (I-band) light Maffei 1 is a massive elliptical galaxy classified as type E3 in the Hubble classification scheme. This means that it is slightly flattened, its semi-minor axis being 70% of its semi-major axis. Maffei 1 has also a boxy shape (E(b)3 type), while its central region (radius ≈ 34 pc) is deficient in light emission as compared to the r1/4 law, meaning that Maffei 1 is a core type elliptical. Both the boxy shape and the presence of an underluminous core are typical of intermediate to massive ellipticals.
Abell 2597 is a galaxy cluster located about a billion light years from Earth in the constellation of Aquarius. It is a giant elliptical galaxy that is surrounded by a sprawling cluster of other galaxies. In 2018, the National Radio Astronomy Observatory (NRAO) captured cosmic weather event using the Atacama Large Millimeter/submillimeter Array (ALMA) that has never been seen before - a cluster of towering intergalactic gas clouds raining in on the supermassive black hole at the center of the huge galaxy. The black hole draws in vast store of cold molecular gas and sprays it back again in an ongoing cycle so that it resembles a gigantic fountain.
While there is evidence to suggest that the environmental damage to the interstellar medium of NGC 4438 may have been caused by an off-center collision with NGC 4435 millions of years ago, a recent discovery of several filaments of ionized gas links NGC 4438 with the large neighboring elliptical galaxy Messier 86, in addition to a discovery of gas and dust within M86 that may have been stripped from NGC 4438 during a past encounter between the two. Given the high density of galaxies in the center of the Virgo galaxy cluster, it is possible that the three galaxies, NGC 4435, NGC 4438, and M86, have had past interactions.
Astronomers initially thought that the halo was small and light, indicative of a spiral galaxy, but the Spitzer Space Telescope found that the dust ring around the Sombrero Galaxy is larger and more massive than previously thought, indicative of a giant elliptical galaxy. Famous Sombrero Galaxy Shows Surprising Side The galaxy has an apparent magnitude of +8.0, making it easily visible with amateur telescopes, and it is considered by some authors to be the galaxy with the highest absolute magnitude within a radius of 10 megaparsecs of the Milky Way. Its large bulge, its central supermassive black hole, and its dust lane all attract the attention of professional astronomers.
NGC 4636 is characterised by its large number of globular clusters, much larger than that of galaxies with similar size located not in the centre of galaxy clusters. The total number of globular clusters within a radius of 14 arcminutes is estimated to be 4,200 ± 120 and within 7 arcminutes is estimated to be 3,500 ± 170. In comparison, globular clusters orbit around Messier 87, the giant elliptical galaxy at the centre of the Virgo Cluster, and 150–200 lie in and around the Milky Way. The number of globular clusters drops abruptly at 7 and 9 arcminutes, probably indicating the edge of the galaxy.
Sargent spent the majority of his career at California Institute of Technology (Caltech), excepting an absence of four years during which he claims to have had to go back to England to find himself a wife, Anneila Sargent. Sargent carried out research in many areas of astronomy including stars, galaxies, quasars and active galactic nuclei, quasar absorption lines, and the intergalactic medium. He pioneered the detection of supermassive black holes in galactic nuclei using stellar dynamics, and published the first dynamical measurement of the mass of the black hole in the elliptical galaxy Messier 87. He supervised the theses of a number of students while at Caltech, including John Huchra, Edwin Turner, Charles C. Steidel, and Alex Filippenko.
20 on the plate between pages 114 and 115. In 1847 John Herschel described the galaxy as "two semi-ovals of elliptically formed nebula appearing to be cut asunder and separated by a broad obscure band parallel to the larger axis of the nebula, in the midst of which a faint streak of light parallel to the sides of the cut appears." In 1949 John Gatenby Bolton, Bruce Slee and Gordon Stanley localized NGC 5128 as one of the first extragalactic radio sources. Five years later, Walter Baade and Rudolph Minkowski suggested that the peculiar structure is the result of a merge event of a giant elliptical galaxy and a small spiral galaxy.
NGC 5982 is an elliptical galaxy located in the constellation Draco. It is located at a distance of circa 130 million light years from Earth, which, given its apparent dimensions, means that NGC 5982 is about 100,000 light years across. It was discovered by William Herschel on May 25, 1788. NGC 5982 has a kinematically decoupled nucleus, with its major axis being nearly perpendicular to the rotation of the galaxy. NGC 5982 features many shells in its envelope, nearly 26. The shells form circular arcs, with the further being located at a radius of 150 arcseconds along the major axis of the galaxy, while the innermost one lies 8 arcseconds off the nucleus.
NGC 4697 (also known as Caldwell 52) is an elliptical galaxy some 40 to 50 million light-years away in the constellation Virgo. It is a member of the NGC 4697 Group, a group of galaxies also containing NGC 4731 and several generally much smaller galaxies This group is about 55 million light-years away; it is one of the many Virgo II Groups, which form a southern extension of the Virgo Supercluster of galaxies. The distance to NGC 4697 is not known with high precision: measurements vary from 28 to 76 million light-years. According to the NASA Extra-galactic Database, the average is about 38 million light-years; according to SIMBAD, about 50 million light-years.
Abell 1201 BGC is a massive elliptical galaxy residing as the brightest cluster galaxy of the Abell 1201 galaxy cluster. At a redshift of 0.169, this system is around 2.7 billion light years from Earth, and offset about 11 kiloparsecs from the X-ray peak of the intracluster gas. With an ellipticity of 0.32±0.02, the stellar distribution is far from spherical. In solar units, the total stellar luminosity is 4×1011 in SDSS r-band, and 1.6×1012 in 2MASS K-band. Half the stars orbit within an effective radius of 15 kpc, and their central velocity dispersion is about 285 km s−1 within 5 kpc rising to 360 km s−1 at 20 kpc distance.
APM 08279+5255 is a bright source at almost all wavelengths and has become one of the most studied of distant sources. Using interferometry it has been mapped in X-ray with the AXAF CCD Imaging Spectrometer on the Chandra X-ray Observatory, in infrared with the Hubble Space Telescope, and in radio with the Very Long Baseline Array. Measurements with the IRAM Plateau de Bure Interferometer and other instruments looked at the distribution of molecules such as CO, CN, HCN, and HCO+ as well as atomic carbon. From these observations APM 08279+5255 is a giant elliptical galaxy with large amounts of gas and dust and an active galactic nucleus (AGN) at its core.
The stream of stars was discovered in the early 21st century by astronomers conducting the Sloan Digital Sky Survey. It was in the course of investigating this ring of stars, and a closely spaced group of globular clusters similar to those associated with the Sagittarius Dwarf Elliptical Galaxy, that the Canis Major Dwarf Galaxy was discovered. Globular clusters thought to be associated with the Canis Major Dwarf galaxy include NGC 1851, NGC 1904, NGC 2298 and NGC 2808, all of which may have been part of the galaxy's globular cluster system before accreting into the Milky Way. NGC 1261 is another nearby cluster, but its velocity differs enough to make its relationship to the system unclear.
Messier 87 (also known as Virgo A or NGC 4486, generally abbreviated to M87) is a supergiant elliptical galaxy with about 1 trillion stars in the constellation Virgo. One of the most massive galaxies in the local universe, it has a large population of globular clusters—about 12,000 compared with the 150–200 orbiting the Milky Way—and a jet of energetic plasma that originates at the core and extends at least , traveling at a relativistic speed. It is one of the brightest radio sources in the sky and a popular target for both amateur and professional astronomers. The French astronomer Charles Messier discovered M87 in 1781, and cataloged it as a nebula.
The distance to the galaxy from Earth, derived by surface brightness fluctuation, is 19±1.7 Mpc. Due to close proximity, it is assumed to be associated with the elliptical galaxy NGC 1052 and to lie at a distance of about from NGC 1052.. On 3 June 2019, however, a separate team used a full observing dataset on the same object to review this claim, and found out that the actual distance of the galaxy was different, and that it may contain dark matter after all. A more recent study on NGC 1052-DF2 suggests the previously reported distance of the galaxy was greatly exaggerated. Consequently, the galaxy now looks "normal" in every way.
In the example on the left (below the image of the Orion Nebula) the telescope took a family photograph of a cluster of galaxies in the constellation of Fornax (the Chemical Furnace). The wide field allows many galaxies to be captured in a single image including the striking barred-spiral NGC 1365 and the big elliptical galaxy NGC 1399. The image was constructed from images taken through Z, J and Ks filters in the near-infrared part of the spectrum and has captured many of the cluster members in a single image. At the lower-right is the elegant barred-spiral galaxy NGC 1365 and to the left the big elliptical NGC 1399, surrounded by a swarm of faint globular clusters.
X-shaped (or "winged") radio galaxies are a class of extragalactic radio source that exhibit two, low-surface-brightness radio lobes (the "wings") oriented at an angle to the active, or high-surface-brightness, lobes. Both sets of lobes pass symmetrically through the center of the elliptical galaxy that is the source of the lobes, giving the radio galaxy an X-shaped morphology as seen on radio maps (see figure). X-shaped sources were first described by J. P. Leahy and P. Parma in 1992, who presented a list of 11 such objects. The X-shaped galaxies have received much attention following the suggestion in 2002 that they might be the sites of spin-flips associated with the recent coalescence of two supermassive black holes.
The chemical composition of Segue 1 indicates no substantial chemical evolution has occurred since the galaxy formed, supporting the idea that it may be a surviving first galaxy that experienced only one burst of star formation, a fossil galaxy from the early universe.SEGUE 1: AN UNEVOLVED FOSSIL GALAXY FROM THE EARLY UNIVERSE Segue 1 is located in the middle of the Sagittarius Stream and at approximately the same distance from the Sun. It may once have been a globular cluster of the Sagittarius Dwarf Elliptical Galaxy, which was later stripped from it by the tidal forces acting from the Milky Way galaxy. However, more recent studies concluded that Segue 1 is not actually associated with the Sagittarius stream and that it is not being tidally disrupted.
Studies from RAVE either concentrate on peculiar stars and objects or overall trends for the different components of our Galaxy, with a main focus of the structure and formation of the Milky Way. For example, RAVE is suited to searching for stellar streams, some of which are remnants of dwarf galaxies that merged with the Milky Way during galaxy formation. A search for a stellar stream from the Sagittarius Dwarf Elliptical Galaxy - which is currently merging with the Milky Way - in the vicinity of the sun yielded a null result, which helps constrain the shape of the Milky Way's dark halo. Another study of the highest velocity stars was used to constrain the local Galactic escape velocity and so the mass of the dark halo.
Velocity dispersion (y-axis) plotted against absolute magnitude (x-axis) for a sample of elliptical galaxies, with the Faber–Jackson relation shown in blue. The Faber–Jackson relation provided the first empirical power-law relation between the luminosity L and the central stellar velocity dispersion \sigma of elliptical galaxy, and was presented by the astronomers Sandra M. Faber and Robert Earl Jackson in 1976. Their relation can be expressed mathematically as: : L \propto \sigma^ \gamma with the index \gamma approximately equal to 4. In 1962, Rudolph Minkowski had discovered and wrote that a "correlation between velocity dispersion and [luminosity] exists, but it is poor" and that "it seems important to extend the observations to more objects, especially at low and medium absolute magnitudes".
NGC 4038 (left) and NGC 4039 (right) Corvus contains no Messier objects. It has several galaxies and a planetary nebula observable with amateur telescopes. The center of Corvus is home to a planetary nebula, NGC 4361. The nebula itself resembles a small elliptical galaxy and has a magnitude of 10.3, but the magnitude 13 star at its centre gives away its true nature. The NGC 4038 Group is a group of galaxies across Corvus and Crater. The group may contain between 13 and 27 galaxies. The best-known member is the Antennae peculiar galaxy, located 0.25 north of 31 Crateris. It consists of two interacting galaxies—NGC 4038 and 4039—that appear to have a heart shape as seen from Earth.
GRB 050509B was a gamma-ray burst (GRB) observed by the NASA Swift satellite on May 9, 2005. It was the first short duration GRB for which an accurate positional measurement was made, accurate enough to locate it near to an elliptical galaxy lying at a redshift of 0.225. The significance of this finding is that it lends support to the theory that short bursts are formed during the catastrophic merger of two neutron stars, or a neutron star and a black hole. The orbital decay (via gravitational radiation) of stellar binaries consisting of these exotic compact objects is believed to take hundreds of millions of years, hence gamma ray bursts produced this way would be expected to be in old (misleadingly called "early type") galaxies.
The luminosity profiles of both elliptical galaxies and bulges are well fit by Sersic's law, and a range of scaling relations between the elliptical galaxies' structural parameters unify the population.Graham, A.W. (2013), Elliptical and Disk Galaxy Structure and Modern Scaling Laws Every massive elliptical galaxy contains a supermassive black hole at its center. Observations of 46 elliptical galaxies, 20 classical bulges, and 22 pseudobulges show that each contain a black hole at the center. The mass of the black hole is tightly correlated with the mass of the galaxy,Graham, A.W. (2016), Galaxy Bulges and Their Massive Black Holes: A Review evidenced through correlations such as the M–sigma relation which relates the velocity dispersion of the surrounding stars to the mass of the black hole at the center.
The Canis Major Overdensity (CMa Overdensity) or Canis Major Dwarf Galaxy (CMa Dwarf) is a disputed dwarf irregular galaxy in the Local Group, located in the same part of the sky as the constellation Canis Major. The supposed small galaxy contains a relatively high percentage of red giants and is thought to contain an estimated one billion stars in all. The Canis Major Dwarf Galaxy is classified as an irregular galaxy and is now thought to be the closest neighboring galaxy to the Earth's location in the Milky Way, being located about away from the Solar System and from the Galactic Center. It has a roughly elliptical shape and is thought to contain as many stars as the Sagittarius Dwarf Elliptical Galaxy, the previous contender for closest galaxy to our location in the Milky Way.
The Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph), also known as the Sagittarius Dwarf Elliptical Galaxy (Sgr dE or Sag DEG), is an elliptical loop-shaped satellite galaxy of the Milky Way. It contains four globular clusters, with the brightest of them – NGC 6715 (M54) – being known well before the discovery of the galaxy itself in 1994. Sgr dSph is roughly 10,000 light-years in diameter, and is currently about 70,000 light-years from Earth, travelling in a polar orbit (an orbit passing over the Milky Way's galactic poles) at a distance of about 50,000 light-years from the core of the Milky Way (about one third of the distance of the Large Magellanic Cloud). In its looping, spiraling path, it has passed through the plane of the Milky Way several times in the past.
Data obtained in optical light with the Magellan I and II telescopes in Las Campanas, Chile, also provides intriguing information about this object, which is found in the elliptical galaxy NGC 1399 in the Fornax galaxy cluster. The spectrum reveals emission from oxygen and nitrogen but no hydrogen, a rare set of signals from within globular clusters. The physical conditions deduced from the spectra suggest that the gas is orbiting a black hole of at least 1,000 solar masses. To explain these observations, researchers suggest that a white dwarf star strayed too close to an intermediate-mass black hole and was ripped apart by tidal forces. The black hole is swallowing material from the white dwarf star, and the material’s velocity implies the size of the black hole.
According to lead author David R. Law: The fact that this galaxy exists is astounding. Current wisdom holds that such grand-design spiral galaxies simply didn't exist at such an early time in the history of the Universe. The presence of a dwarf galaxy in the vicinity of BX442 offers a clue as to how the premature spiral structure may have emerged in what would otherwise be a somewhat chaotic lumpy collection of stars, as is the case with most other early galaxies. A recent study of one of the satellite galaxies of the Milky Way, known as the Sagittarius Dwarf Elliptical Galaxy (SagDEG), suggest that SagDEG may have helped generate some the Milky Way's spiral structure when it passed repeatedly through the plane of our galaxy over the past few hundred million years.
Janz, J. et al. (2017), Implications for the origin of early-type dwarf galaxies - the discovery of rotation in isolated, low-mass early-type galaxies The highly isolated dwarf elliptical galaxy CG 611 possesses the same physical attributes as dE galaxies in clusters - such as rotation and faint spiral arms - attributes that were previously assumed to provide evidence that dE galaxies were once spiral galaxies prior to a transformation process requiring immersion with a cluster of galaxies. CG 611 has a gas disk which counter- rotates to its stellar diskGraham, A.W. et al. (2017), Implications for the Origin of Early-type Dwarf Galaxies: A Detailed Look at the Isolated Rotating Early-type Dwarf Galaxy LEDA 2108986 (CG 611), Ramifications for the Fundamental Plane’s SK2 Kinematic Scaling, and the Spin-Ellipticity Diagram, clearly revealing that this dE galaxy's disk is growing via accretion events.
Hyper luminous Infrared Galaxies (HyLIRG), also referred to as HiLIRGs and HLIRGs, are considered to be some of the most luminous persistent objects in the Universe, exhibiting extremely high star formation rates, and most of which are known to harbour Active Galactic Nuclei (AGN). They are defined as galaxies with luminosities above 1013 L⊙, as distinct from the less luminous population of ULIRGs (L = 1012 – 1013 L⊙). HLIRGs were first identified through follow-up observations of the IRAS mission. IRAS F10214+4724, a HyLIRG being gravitationally lensed by a foreground elliptical galaxy, was considered to be one of the most luminous objects in the Universe having an intrinsic luminosity of ~ 2 × 1013 L⊙. It is believed that the bolometric luminosity of this HLIRG is likely amplified by a factor of ~30 as a result of the gravitational lensing.
In contrast to spirals, an elliptical galaxy loses the cold component of its interstellar medium within roughly a billion years, which hinders the galaxy from forming diffuse nebulae except through mergers with other galaxies. In the dense nebulae where stars are produced, much of the hydrogen is in the molecular (H2) form, so these nebulae are called molecular clouds. Observations indicate that the coldest clouds tend to form low-mass stars, observed first in the infrared inside the clouds, then in visible light at their surface when the clouds dissipate, while giant molecular clouds, which are generally warmer, produce stars of all masses. These giant molecular clouds have typical densities of 100 particles per cm3, diameters of , masses of up to 6 million solar masses (), and an average interior temperature of 10 K. About half the total mass of the galactic ISM is found in molecular clouds and in the Milky Way there are an estimated 6,000 molecular clouds, each with more than .
Previously thought to belong to the Milky Way at a distance from Earth of about 50,000 light-years, it was discovered in 1994 that M54 most likely belongs to the Sagittarius Dwarf Elliptical Galaxy (SagDEG), making it the first globular cluster formerly thought to be part of our galaxy reassigned to extragalactic status, even if not recognized as such for nearly two and a quarter centuries. As it is located on SagDEG's center, some authors think it actually may be its core; however others have proposed that it is a real globular cluster that fell to the center of this galaxy due to decay of its orbit caused by dynamical friction. Modern estimates now place M54 at a distance of some 87,000 light-years, translating into a true radius of 150 light-years across. It is one of the denser of the globulars, being of class III (I being densest and XII being the least dense).
R. Astr. Soc. 179:433-456 (1977). The Blandford-Znajek mechanism has been invoked by the Event Horizon Telescope Collaboration to explain the jet power in the first observation of a black hole shadow in the giant elliptical galaxy M87.The Event Horizon Telescope Collaboration, "First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole" The Astrophysical Journal Letters 875:L1 (2019) Blandford also theorized another mechanism for jet formation through hydromagnetic winds launched from accretion disks.R. D. Blandford and D. G. Payne, "Hydromagnetic flows from accretion disks and the production of radio jets", Mon. Not. R. Astr. Soc. 199:883–903 (1982). In addition to the Blandford-Znajek and Blandford-Payne mechanisms for the formation of relativistic jets, Roger Blandford also helped devise a widely used theoretical model for jet geometric and spectral properties, the Blandford-Königl conical jet model,R. D. Blandford and A. Königl, "Relativistic Jets as Compact Radio Sources", ApJ.
Notably, the giant elliptical galaxy M87 contains a supermassive black hole, whose event horizon was observed by the Event Horizon Telescope Collaboration in 2019. Of all of the subclumps, Virgo A, formed by a mixture of elliptical, lenticular, and (usually) gas-poor spiral galaxies, is the dominant one, with a mass of approximately 1014 , which is approximately an order of magnitude larger than the other two subclumps.The Virgo Super Cluster: home of M87 (with frames) Turbulence may prevent galaxy clusters from cooling (Chandra X-ray). The three subgroups are in the process of merging to form a larger single cluster and are surrounded by other smaller galaxy clouds, mostly composed of spiral galaxies, known as N Cloud, S Cloud, and Virgo E that are in the process of infalling to merge with them, plus other farther isolated galaxies and galaxy groups (like the galaxy cloud Coma I) that are also attracted by the gravity of Virgo to merge with it in the future.
GW 170817 was a gravitational wave (GW) signal observed by the LIGO and Virgo detectors on 17 August 2017, originating from the shell elliptical galaxy . The GW was produced by the last minutes of two neutron stars spiralling closer to each other and finally merging, and is the first GW observation which has been confirmed by non-gravitational means. Unlike the five previous GW detections, which were of merging black holes not expected to produce a detectable electromagnetic signal, the aftermath of this merger was also seen by 70 observatories on 7 continents and in space, across the electromagnetic spectrum, marking a significant breakthrough for multi-messenger astronomy. The discovery and subsequent observations of GW 170817 were given the Breakthrough of the Year award for 2017 by the journal Science. The gravitational wave signal, designated GW 170817, had a duration of approximately 100 seconds, and shows the characteristics in intensity and frequency expected of the inspiral of two neutron stars.
17 August 2017: Gravitational wave (GW170817) detected from merger of two neutron stars (00:23 video; artist concept). On 17 August 2017, LIGO/Virgo collaboration detected a pulse of gravitational waves, named GW170817, associated with the merger of two neutron stars in NGC 4993, an elliptical galaxy in the constellation Hydra. GW170817 also seemed related to a short (≈2 second long) gamma-ray burst, GRB 170817A, first detected 1.7 seconds after the GW merger signal, and a visible light observational event first observed 11 hours afterwards, SSS17a. The association of GW170817 with GRB 170817A in both space and time is strong evidence that neutron star mergers do create short gamma-ray bursts. The subsequent detection of event Swope Supernova Survey 2017a (SSS17a) in the area in which GW170817 and GRB 170817A were known to have occurred and its having the expected characteristics for a kilonova is strong evidence that neutron star mergers do produce kilonovae.
IC 5148, the spare-tyre nebula as imaged by the ESO Faint Object Spectrograph and Camera (EFOSC2) on the New Technology Telescope at La Silla Nicknamed the spare-tyre nebula, IC 5148 is a planetary nebula located around 1 degree west of Lambda Gruis. Around 3000 light-years distant, it is expanding at 50 kilometres a second, one of the fastest rates of expansion of all planetary nebulae. Northeast of Theta Gruis are four interacting galaxies known as the Grus Quartet. These galaxies are NGC 7552, NGC 7590, NGC 7599, and NGC 7582. The latter three galaxies occupy an area of sky only 10 arcminutes across and are sometimes referred to as the "Grus Triplet," although all four are part of a larger loose group of galaxies called the IC 1459 Grus Group. NGC 7552 and 7582 are exhibiting high starburst activity; this is thought to have arisen because of the tidal forces from interacting. Located on the border of Grus with Piscis Austrinus, IC 1459 is a peculiar E3 giant elliptical galaxy. It has a fast counterrotating stellar core, and shells and ripples in its outer region. The galaxy has an apparent magnitude of 11.9 and is around 80 million light-years distant.

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