NearInfrared
... Step 4: We can perform photometry on the target and measure the total counts per second, by identifying the area of interest. This can be done directly using IRAF as it has been shown in other exercises or within ATV. We start ATV, change the mouse mode to “ImExam” and the left click on the position ...
... Step 4: We can perform photometry on the target and measure the total counts per second, by identifying the area of interest. This can be done directly using IRAF as it has been shown in other exercises or within ATV. We start ATV, change the mouse mode to “ImExam” and the left click on the position ...
NGC 1569 A Dwarf galaxy with a Giant Starburst Stefanie Mhhle1,2
... hydrogen in NGC 1569 using a high-resolution HI data cube complemented with single-dish observations. The velocity structure is ...
... hydrogen in NGC 1569 using a high-resolution HI data cube complemented with single-dish observations. The velocity structure is ...
Chapter 15
... By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 2.6 million solar masses ...
... By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 2.6 million solar masses ...
Astro-MilkyWay
... By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 2.6 million solar masses ...
... By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 2.6 million solar masses ...
Galaxies
... Black Holes Most galaxies seem to harbor supermassive black holes in their centers. They are fed and fueled by stars and gas from the nearcentral environment ...
... Black Holes Most galaxies seem to harbor supermassive black holes in their centers. They are fed and fueled by stars and gas from the nearcentral environment ...
Galaxies - SD43 Teacher Sites
... could live. We now know there is life beneath the frozen land mass of Antarctica, inside sulphur deposits several kilometres underground, and even in the superheated water in the cracks of rock surrounding volcanic magma chambers. The ingredients that create organic molecules on Earth have recently ...
... could live. We now know there is life beneath the frozen land mass of Antarctica, inside sulphur deposits several kilometres underground, and even in the superheated water in the cracks of rock surrounding volcanic magma chambers. The ingredients that create organic molecules on Earth have recently ...
The Dynamics of the Galaxies in the Local Group
... • Necessary to determine the complete 3D velocity of an object • “Easy” to measure for stars close to the Sun • Very small and difficult to measure for distant objects • Never measured for Andromeda (tried since 1898) • Now finally measured with Hubble Space Telescope ...
... • Necessary to determine the complete 3D velocity of an object • “Easy” to measure for stars close to the Sun • Very small and difficult to measure for distant objects • Never measured for Andromeda (tried since 1898) • Now finally measured with Hubble Space Telescope ...
Clusters
... it is currently thought that the very large amounts of expected cooling are in reality much smaller, as there is little evidence for cool X-ray emitting gas in many of these systems = the cooling flow problem theories for why there is little evidence of cooling include ◦ heating by the central AGN p ...
... it is currently thought that the very large amounts of expected cooling are in reality much smaller, as there is little evidence for cool X-ray emitting gas in many of these systems = the cooling flow problem theories for why there is little evidence of cooling include ◦ heating by the central AGN p ...
CHP 15
... b. indicates that the material they formed from had been enriched with material from supernovae. c. indicates that they contain very few heavy metals compared to halo stars. d. depends on the temperature of the star. e. depends on the mass of the star. ____ 17. The center of our galaxy lies in the d ...
... b. indicates that the material they formed from had been enriched with material from supernovae. c. indicates that they contain very few heavy metals compared to halo stars. d. depends on the temperature of the star. e. depends on the mass of the star. ____ 17. The center of our galaxy lies in the d ...
Lecture 18, Structure of spiral galaxies
... • Stars in the disk are relatively young. • fraction of heavy elements same as or greater than the Sun • plenty of high and lowmass stars, blue and red • Stars in the halo are old. • fraction of heavy elements much less than the Sun • mostly lowmass, red stars • Stars in the halo must have forme ...
... • Stars in the disk are relatively young. • fraction of heavy elements same as or greater than the Sun • plenty of high and lowmass stars, blue and red • Stars in the halo are old. • fraction of heavy elements much less than the Sun • mostly lowmass, red stars • Stars in the halo must have forme ...
Messier 87
Messier 87 (also known as Virgo A or NGC 4486, and generally abbreviated to M87) is a supergiant elliptical galaxy in the constellation Virgo. One of the most massive galaxies in the local universe, it is notable for its large population of globular clusters—M87 contains about 12,000 compared to the 150-200 orbiting the Milky Way—and its jet of energetic plasma that originates at the core and extends outward at least 1,500 parsecs (4,900 light-years), travelling at relativistic speed. It is one of the brightest radio sources in the sky, and is a popular target for both amateur astronomy observations and professional astronomy study.French astronomer Charles Messier discovered M87 in 1781, cataloguing it as a nebulous feature while searching for objects that would confuse comet hunters. The second brightest galaxy within the northern Virgo Cluster, M87 is located about 16.4 million parsecs (53.5 million light-years) from Earth. Unlike a disk-shaped spiral galaxy, M87 has no distinctive dust lanes. Instead, it has an almost featureless, ellipsoidal shape typical of most giant elliptical galaxies, diminishing in luminosity with distance from the centre. Forming around one sixth of M87's mass, the stars in this galaxy have a nearly spherically symmetric distribution, their density decreasing with increasing distance from the core. At the core is a supermassive black hole, which forms the primary component of an active galactic nucleus. This object is a strong source of multiwavelength radiation, particularly radio waves. M87's galactic envelope extends out to a radius of about 150 kiloparsecs (490,000 light-years), where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse interstellar medium of gas that has been chemically enriched by elements emitted from evolved stars.