Star-Formation in Close Pairs Selected from the Sloan Digital Sky
... The ratio of these radii is the (inverse) concentration index: C = 50% light radius / 90% light radius and correlates with morphological type (e.g. Morgan 1958) Low values of concentration index = systems with centrally condensed light profiles – de Vaucouleurs profiles – galaxies of early morpholog ...
... The ratio of these radii is the (inverse) concentration index: C = 50% light radius / 90% light radius and correlates with morphological type (e.g. Morgan 1958) Low values of concentration index = systems with centrally condensed light profiles – de Vaucouleurs profiles – galaxies of early morpholog ...
The Milky Way Galaxy Chapter 15 Guidepost Guidepost
... Many absorption lines also from heavier elements (metals): Population At the time of formation, the gases forming the Milky Way consisted exclusively of hydrogen and helium. Heavier elements (“metals”) were later only produced in stars. ...
... Many absorption lines also from heavier elements (metals): Population At the time of formation, the gases forming the Milky Way consisted exclusively of hydrogen and helium. Heavier elements (“metals”) were later only produced in stars. ...
Watching Galaxies Form Near the Beginning of Time
... chemical makeup until late in its lifespan • Stars’ orbits change only very slowly over time • Makeup and motions of stars preserve a detailed record of our galaxy’s history • Early stars formed with low heavy-element abundances and in a nearly spherical system ...
... chemical makeup until late in its lifespan • Stars’ orbits change only very slowly over time • Makeup and motions of stars preserve a detailed record of our galaxy’s history • Early stars formed with low heavy-element abundances and in a nearly spherical system ...
Question 1
... b) The rotation of the bulge and disk components c) The Sun’s age and age of the globular cluster stars d) The motion of spiral arms and the mass of the central black hole e) The orbital period and distance from the Galactic center of objects near the edge of the Galaxy Explanation: Use the modified ...
... b) The rotation of the bulge and disk components c) The Sun’s age and age of the globular cluster stars d) The motion of spiral arms and the mass of the central black hole e) The orbital period and distance from the Galactic center of objects near the edge of the Galaxy Explanation: Use the modified ...
The Milky Way
... birth in clouds of gas and dust, to their deaths as white dwarfs, neutron stars, or black holes. Now you are ready to see stars in their vast communities called galaxies. This chapter discusses our home galaxy, the Milky Way Galaxy, and attempts to answer four ...
... birth in clouds of gas and dust, to their deaths as white dwarfs, neutron stars, or black holes. Now you are ready to see stars in their vast communities called galaxies. This chapter discusses our home galaxy, the Milky Way Galaxy, and attempts to answer four ...
Spiral Galaxies - Astronomy Centre
... Due to this large size, Shapley believed our Galaxy to contain the observed nebulae In 1920 the Great Debate took place between Shapley and Heber Curtis, who argued for the island universe hypothesis ...
... Due to this large size, Shapley believed our Galaxy to contain the observed nebulae In 1920 the Great Debate took place between Shapley and Heber Curtis, who argued for the island universe hypothesis ...
1” “Sky-Notes” of the Open University Astronomy Club. April 2005
... NGC3226 (11.4) and NGC3227 (10.8) about 1o east of form a close interacting pair of galaxies. NGC3351 (M95) (9.7) sg, NGC 3368 (M96) (9.2) sg and NGC 3379 (M105) (9.3) eg. An excellent trio in the same low power field located about 3o south of 52 Leo. Close to M105 is NGC 3384 (10.0) eg. NGC3623 ( ...
... NGC3226 (11.4) and NGC3227 (10.8) about 1o east of form a close interacting pair of galaxies. NGC3351 (M95) (9.7) sg, NGC 3368 (M96) (9.2) sg and NGC 3379 (M105) (9.3) eg. An excellent trio in the same low power field located about 3o south of 52 Leo. Close to M105 is NGC 3384 (10.0) eg. NGC3623 ( ...
The Milky Way Galaxy
... Our Galaxy is a collection of stellar and interstellar matter – stars, gas, dust, neutron stars, black holes – held together by gravity. Our view of the Galaxy…. ...
... Our Galaxy is a collection of stellar and interstellar matter – stars, gas, dust, neutron stars, black holes – held together by gravity. Our view of the Galaxy…. ...
MilkyWay
... Our Galaxy is a collection of stellar and interstellar matter – stars, gas, dust, neutron stars, black holes – held together by gravity. Our view of the Galaxy…. ...
... Our Galaxy is a collection of stellar and interstellar matter – stars, gas, dust, neutron stars, black holes – held together by gravity. Our view of the Galaxy…. ...
Unit 1
... fusion reactions of massive stars. Yet, the Sun has iron in its atmosphere, as well as gold, silver and other elements much heavier than iron. Why? ...
... fusion reactions of massive stars. Yet, the Sun has iron in its atmosphere, as well as gold, silver and other elements much heavier than iron. Why? ...
Teaching Text Structure with Understanding the Scale of the Universe
... By 1920, many scientists began to think that some of the objects they were seeing must be other galaxies like the Milky Way but separate from the Milky Way. They spoke of these separate clusters of stars as island universes. ...
... By 1920, many scientists began to think that some of the objects they were seeing must be other galaxies like the Milky Way but separate from the Milky Way. They spoke of these separate clusters of stars as island universes. ...
GAIA Composition, Formation and Evolution of our Galaxy
... – 10 µas ≡ 10% at 10 kpc ≡ 1 AU at 100 kpc – 10 µas/yr at 20 kpc ≡ 1 km/s ⇒ every star in the Galaxy and Local Group will be seen to move ⇒ GAIA will quantify 6-D phase space for over 300 million stars, and 5-D phase-space for over 109 stars And an interesting data reduction challenge…. ...
... – 10 µas ≡ 10% at 10 kpc ≡ 1 AU at 100 kpc – 10 µas/yr at 20 kpc ≡ 1 km/s ⇒ every star in the Galaxy and Local Group will be seen to move ⇒ GAIA will quantify 6-D phase space for over 300 million stars, and 5-D phase-space for over 109 stars And an interesting data reduction challenge…. ...
Universe 8e Lecture Chapter 24 Galaxies
... Elliptical galaxies are nearly devoid of interstellar gas and dust, and so star formation is severely inhibited. Lenticular galaxies are intermediate between spiral and elliptical galaxies. Irregular galaxies have ill-defined, asymmetrical shapes. They are often found associated with other galaxies. ...
... Elliptical galaxies are nearly devoid of interstellar gas and dust, and so star formation is severely inhibited. Lenticular galaxies are intermediate between spiral and elliptical galaxies. Irregular galaxies have ill-defined, asymmetrical shapes. They are often found associated with other galaxies. ...
The Moon
... galaxy, outside our solar system. Between 100,000 and 1,000,000 light years away are no other large galaxies like ours, but there are a few small galaxies. Other large galaxies would be more than a meter away. The next closest galaxy is actually 2.5 meters away, about 2.5 million light years. ...
... galaxy, outside our solar system. Between 100,000 and 1,000,000 light years away are no other large galaxies like ours, but there are a few small galaxies. Other large galaxies would be more than a meter away. The next closest galaxy is actually 2.5 meters away, about 2.5 million light years. ...
Andromeda Galaxy
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The Andromeda Galaxy (/ænˈdrɒmɨdə/), also known as Messier 31, M31, or NGC 224, is a spiral galaxy approximately 780 kiloparsecs (2.5 million light-years) from Earth. It is the nearest major galaxy to the Milky Way and was often referred to as the Great Andromeda Nebula in older texts. It received its name from the area of the sky in which it appears, the constellation of Andromeda, which was named after the mythological princess Andromeda. Being approximately 220,000 light years across, it is the largest galaxy of the Local Group, which also contains the Milky Way, the Triangulum Galaxy, and about 44 other smaller galaxies.The Andromeda Galaxy is the most massive galaxy in the Local Group as well. Despite earlier findings that suggested that the Milky Way contains more dark matter and could be the most massive in the grouping, the 2006 observations by the Spitzer Space Telescope revealed that Andromeda contains one trillion (1012) stars: at least twice the number of stars in the Milky Way, which is estimated to be 200–400 billion.The Andromeda Galaxy is estimated to be 1.5×1012 solar masses, while the mass of the Milky Way is estimated to be 8.5×1011 solar masses. In comparison, a 2009 study estimated that the Milky Way and M31 are about equal in mass, while a 2006 study put the mass of the Milky Way at ~80% of the mass of the Andromeda Galaxy. The Milky Way and Andromeda are expected to collide in 3.75 billion years, eventually merging to form a giant elliptical galaxy or perhaps a large disk galaxy.At 3.4, the apparent magnitude of the Andromeda Galaxy is one of the brightest of any of the Messier objects, making it visible to the naked eye on moonless nights even when viewed from areas with moderate light pollution. Although it appears more than six times as wide as the full Moon when photographed through a larger telescope, only the brighter central region is visible to the naked eye or when viewed using binoculars or a small telescope and would it hence appear to be but another star.