Next Generation VLA Science White Paper
... active regions. Though still revolutionary at ν ∼ 70–115 GHz, ALMA in its current (nearly final) form would still require ∼ 15 hours to produce a 100 CO map of a nearby galaxy (σ = 0.2 K, ∆v = 5 km s−1 ). To work with lines 10× fainter at matched signal to noise and resolution would require ∼ 1000 h ...
... active regions. Though still revolutionary at ν ∼ 70–115 GHz, ALMA in its current (nearly final) form would still require ∼ 15 hours to produce a 100 CO map of a nearby galaxy (σ = 0.2 K, ∆v = 5 km s−1 ). To work with lines 10× fainter at matched signal to noise and resolution would require ∼ 1000 h ...
20_Testbank
... 1) Explain how we estimate that there are about 50-100 billion galaxies in the observable universe. Answer: Obviously it's impossible to count so many galaxies one by one, but by observing a small part in detail, we can extrapolate to get the total number. As an example, the Hubble deep field shows ...
... 1) Explain how we estimate that there are about 50-100 billion galaxies in the observable universe. Answer: Obviously it's impossible to count so many galaxies one by one, but by observing a small part in detail, we can extrapolate to get the total number. As an example, the Hubble deep field shows ...
Galaxies
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
Galaxy Sorting
... · While the 20 images picked for this activity show a good variety of galaxy characteristics, there is nothing sacred about this list. If you already have images of galaxies from another unrestricted source, such as the Space Telescope Science Institute, feel free to substitute some of them. P ...
... · While the 20 images picked for this activity show a good variety of galaxy characteristics, there is nothing sacred about this list. If you already have images of galaxies from another unrestricted source, such as the Space Telescope Science Institute, feel free to substitute some of them. P ...
Document
... Since young, massive stars heat the dusty clouds from which they formed, resulting in the emission of much infrared radiation, the current rate of star formation in a galaxy can be estimated by measuring its infrared power. Space telescopes such as the Infrared Astronomical Satellite (IRAS, in the m ...
... Since young, massive stars heat the dusty clouds from which they formed, resulting in the emission of much infrared radiation, the current rate of star formation in a galaxy can be estimated by measuring its infrared power. Space telescopes such as the Infrared Astronomical Satellite (IRAS, in the m ...
A Zoo of Galaxies - Portsmouth Research Portal
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
A Zoo of Galaxies
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
Chapter 15 THE MILKY WAY IN RELATION TO OTHER GALAXIES
... Figure 15.2: Radial light and color distributions along the major axis of M31 in U, B, V and R. The profiles of the SW side have been shifted upwards by 3 mag. Colors have not been corrected for foreground reddening. From Walterbos and Kennicutt (1987. The SMC much more resembles dwarf irregulars, s ...
... Figure 15.2: Radial light and color distributions along the major axis of M31 in U, B, V and R. The profiles of the SW side have been shifted upwards by 3 mag. Colors have not been corrected for foreground reddening. From Walterbos and Kennicutt (1987. The SMC much more resembles dwarf irregulars, s ...
Living Things - Fairfield-Suisun Unified School District
... Universe What is the big bang theory? How did the solar system form? What do astronomers predict about the future of the universe? ...
... Universe What is the big bang theory? How did the solar system form? What do astronomers predict about the future of the universe? ...
Formation of Globular Clusters: In and Out of Dwarf Galaxies
... progenitor galaxies at intermediate redshifts • Model explains observed sizes, masses, ages, metallicities • Dynamical evolution explains the present mass function and may be important for metallicity bimodality • Red clusters in the Galaxy are due to massive late gas-rich ...
... progenitor galaxies at intermediate redshifts • Model explains observed sizes, masses, ages, metallicities • Dynamical evolution explains the present mass function and may be important for metallicity bimodality • Red clusters in the Galaxy are due to massive late gas-rich ...
dark matter - University of Texas Astronomy Home Page
... 1. One way to estimate the amount of mass in a spiral galaxy is by looking at how much light it emits. Where there is more light, there must be more stars and hence more mass. When we measure amount of light at different regions in the galaxy, more is emitted at the center and less on the outskirts. ...
... 1. One way to estimate the amount of mass in a spiral galaxy is by looking at how much light it emits. Where there is more light, there must be more stars and hence more mass. When we measure amount of light at different regions in the galaxy, more is emitted at the center and less on the outskirts. ...
16 Hubble s Law and Dark Matter
... Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with e ...
... Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with e ...
Extragalactic Distances from Planetary Nebulae
... many (any?) 2 M main sequence stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is about equal to the ratio of the ...
... many (any?) 2 M main sequence stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is about equal to the ratio of the ...
21_Testbank
... 1) Give examples demonstrating the role of "nature" and "nurture" in galaxy evolution. Answer: Galaxies come in a wide variety of shapes and sizes. Protogalactic clouds that had low angular momentum may have formed spheroidal stellar systems (elliptical galaxies), while clouds with higher angular mo ...
... 1) Give examples demonstrating the role of "nature" and "nurture" in galaxy evolution. Answer: Galaxies come in a wide variety of shapes and sizes. Protogalactic clouds that had low angular momentum may have formed spheroidal stellar systems (elliptical galaxies), while clouds with higher angular mo ...
Galaxy Evolution
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
Introduction
... fraction of quenched late-type galaxies are, however, not gas deficient, and form a more heterogeneous class of objects with probably more complex evolutionary histories. In contrast to the case of star formation, the chemical evolution of star-forming galaxies, as traced by the stellar mass-metalli ...
... fraction of quenched late-type galaxies are, however, not gas deficient, and form a more heterogeneous class of objects with probably more complex evolutionary histories. In contrast to the case of star formation, the chemical evolution of star-forming galaxies, as traced by the stellar mass-metalli ...
Baryons at Low Densities: The Stellar Halos around Galaxies
... Only a half dozen luminous early-type galaxies are close enough to resolve individual stars in the halos and study their properties. Marina Rejkuba summarised the previous studies, most of which concentrated on the nearest giant elliptical galaxy NGC 5128, known also as Centaurus A. The bulk of the ...
... Only a half dozen luminous early-type galaxies are close enough to resolve individual stars in the halos and study their properties. Marina Rejkuba summarised the previous studies, most of which concentrated on the nearest giant elliptical galaxy NGC 5128, known also as Centaurus A. The bulk of the ...
Exploring Neutral Hydrogen and Galaxy Evolution with the SKA
... distribution in galaxies, as well as insight into the relationship between star formation and the interstellar medium, have been limited to the local universe. Ongoing and upcoming H I surveys on SKA pathfinder instruments will extend these measurements beyond the local universe to intermediate reds ...
... distribution in galaxies, as well as insight into the relationship between star formation and the interstellar medium, have been limited to the local universe. Ongoing and upcoming H I surveys on SKA pathfinder instruments will extend these measurements beyond the local universe to intermediate reds ...
Chapter 31
... wavelengths than they do in wavelengths of visible light. • The radio emission usually comes from two huge lobes of very hot gas located on opposite sides of the visible galaxy, linked by jets of gas. • Active galactic nuclei, or AGNs, in some unusual galaxies, contain a highly energetic object or a ...
... wavelengths than they do in wavelengths of visible light. • The radio emission usually comes from two huge lobes of very hot gas located on opposite sides of the visible galaxy, linked by jets of gas. • Active galactic nuclei, or AGNs, in some unusual galaxies, contain a highly energetic object or a ...
The Submillimeter Frontier: A Space Science Imperative
... luminosity of a typical spiral galaxy (the Milky Way, Figure 1) has just two large bumps, one from 0.2 to 2 µm from the luminosity of stars, and one nearly as large from 50 - 400 µm, from the energy absorbed and reradiated by dust. These two terms dwarf all the others, but only one has been widely o ...
... luminosity of a typical spiral galaxy (the Milky Way, Figure 1) has just two large bumps, one from 0.2 to 2 µm from the luminosity of stars, and one nearly as large from 50 - 400 µm, from the energy absorbed and reradiated by dust. These two terms dwarf all the others, but only one has been widely o ...
Finnish Centre for Astronomy with ESO
... a world leading astronomical research and technology organization, with 15 member states, headquarters in Garching, Germany, and three world-class observatories in Chile. Finnish Centre for Astronomy with ESO (FINCA) is a national research institute for astronomical and astrophysical research in Fin ...
... a world leading astronomical research and technology organization, with 15 member states, headquarters in Garching, Germany, and three world-class observatories in Chile. Finnish Centre for Astronomy with ESO (FINCA) is a national research institute for astronomical and astrophysical research in Fin ...
THREE INTRIGUER NEBULAE IN CONSTELLATION CARINA
... Astronomical Twilight. The first step was to identify constellation Antlia whose stars, although faint, were clearly visible to the naked eye. Once the constellation was identified I focused on the region where the cluster lies. To make this possible it is necessary to fix our view on the eastern pa ...
... Astronomical Twilight. The first step was to identify constellation Antlia whose stars, although faint, were clearly visible to the naked eye. Once the constellation was identified I focused on the region where the cluster lies. To make this possible it is necessary to fix our view on the eastern pa ...
13.1 Galaxy Evolution: Introduction
... spectra would look like as a composite of these evolving stellar populations. And, there are also hybrid semi-analytical schemes that combine these. [slide 5] On the observational side, there again are three approaches. First, we can take deep images, the deeper the better, if you want t ...
... spectra would look like as a composite of these evolving stellar populations. And, there are also hybrid semi-analytical schemes that combine these. [slide 5] On the observational side, there again are three approaches. First, we can take deep images, the deeper the better, if you want t ...
Pea galaxy
A Pea galaxy, also referred to as a Pea or Green Pea, might be a type of Luminous Blue Compact Galaxy which is undergoing very high rates of star formation. Pea galaxies are so-named because of their small size and greenish appearance in the images taken by the Sloan Digital Sky Survey (SDSS).Pea Galaxies were first discovered in 2007 by the volunteer users within the forum section of the online astronomy project Galaxy Zoo (GZ).