19. Our Galaxy 19.1 The Milky Way Revealed Our goals for learning
... • What is the significance of a rotation curve that is flat at large distances from the galactic center? • The Milky Way’s flat rotation curve implies that the matter associated with our galaxy extends to large distances from the center. A rotation curve is a plot of the orbital speed of stars or ga ...
... • What is the significance of a rotation curve that is flat at large distances from the galactic center? • The Milky Way’s flat rotation curve implies that the matter associated with our galaxy extends to large distances from the center. A rotation curve is a plot of the orbital speed of stars or ga ...
February 2004
... Mars is still in the evening sky in the north west, perhaps almost forgotten after its showing last August, it could be mistaken for a star like Betelgeuse, (it nearly was!) but it is still in a part of the sky where there are not many other bright objects. It showed a small disc in Michael’s 3 inch ...
... Mars is still in the evening sky in the north west, perhaps almost forgotten after its showing last August, it could be mistaken for a star like Betelgeuse, (it nearly was!) but it is still in a part of the sky where there are not many other bright objects. It showed a small disc in Michael’s 3 inch ...
An Updated Ultraviolet Calibration for the Swift/UVOT
... bands in the optical (v, b and u) and ultraviolet (uvw1, uvm2 and uvw2) ranges. There are also two grisms for low resolution spectroscopy. Details about the instrument design and performance can be found in [4] and [5]. The in-orbit photometric calibration given in [5] was based on the ground calibr ...
... bands in the optical (v, b and u) and ultraviolet (uvw1, uvm2 and uvw2) ranges. There are also two grisms for low resolution spectroscopy. Details about the instrument design and performance can be found in [4] and [5]. The in-orbit photometric calibration given in [5] was based on the ground calibr ...
Stars and the Milky Way
... • the Milky Way is one of billions of galaxies in the universe • the Milky Way is made up of over 200 billion stars Other facts about the Milky Way • The Sun is just one of the stars in the Milky Way. • It is called the Milky Way because when astronomers looked up at the sky, they saw a line of ligh ...
... • the Milky Way is one of billions of galaxies in the universe • the Milky Way is made up of over 200 billion stars Other facts about the Milky Way • The Sun is just one of the stars in the Milky Way. • It is called the Milky Way because when astronomers looked up at the sky, they saw a line of ligh ...
DTU 8e Chap 17 Quasars and Other Active Galaxies
... radio emissions from Cygnus A come from the radio lobes located on either side of the peculiar galaxy seen in the inset, a Hubble Space Telescope image. Each of the two radio lobes extend about 160,000 light-years from the optical galaxy and contain a brilliant, condensed region of radio emission. I ...
... radio emissions from Cygnus A come from the radio lobes located on either side of the peculiar galaxy seen in the inset, a Hubble Space Telescope image. Each of the two radio lobes extend about 160,000 light-years from the optical galaxy and contain a brilliant, condensed region of radio emission. I ...
Project Haystack: The Search for Life in the Galaxy
... brainstorm together. The only clue that they have to work with is their ability to rank the modes of travel from slowest to fastest! You may be surprised at their choices! Teacher Information: The speed of the Voyager spacecraft is actually variable. It left Earth with a velocity of about 97,000 km/ ...
... brainstorm together. The only clue that they have to work with is their ability to rank the modes of travel from slowest to fastest! You may be surprised at their choices! Teacher Information: The speed of the Voyager spacecraft is actually variable. It left Earth with a velocity of about 97,000 km/ ...
$doc.title
... achieved in physics laboratories on the Earth, and hence by studying the properties of stars we probe regimes of physical parameters that cannot be reached any other way. The opposite extreme is often reached in the interstellar medium, same idea. Temperature T(ISM) ∼ 3 − 10K, T(Sun, center) ∼ 20 × ...
... achieved in physics laboratories on the Earth, and hence by studying the properties of stars we probe regimes of physical parameters that cannot be reached any other way. The opposite extreme is often reached in the interstellar medium, same idea. Temperature T(ISM) ∼ 3 − 10K, T(Sun, center) ∼ 20 × ...
Salpeter Mass Function
... Most important unsolved problem in star formation. Many theories but no consensus. Observationally, known that dense cores in molecular clouds have a power-law mass function rather similar to the IMF. So the IMF may be determined in part by how such cores form from turbulent molecular gas. Is the IM ...
... Most important unsolved problem in star formation. Many theories but no consensus. Observationally, known that dense cores in molecular clouds have a power-law mass function rather similar to the IMF. So the IMF may be determined in part by how such cores form from turbulent molecular gas. Is the IM ...
constellation.
... color. (Your project should include: the H-R diagram and the different size, temperature and colors of stars) c. How are astronomical units and light years use to measure the distances between the Sun, stars, and Earth. (Your project should include: how many kilometers there are in 1 AU and 1 light ...
... color. (Your project should include: the H-R diagram and the different size, temperature and colors of stars) c. How are astronomical units and light years use to measure the distances between the Sun, stars, and Earth. (Your project should include: how many kilometers there are in 1 AU and 1 light ...
MB mirror - Institute of Astronomy
... The relation between galaxies and the IGM Constrain dark energy from cluster counts and Alcock-Paczsynki test – Accurately measure luminosity functions & starformation rate densities with redshift & environment – Detailed studies of local low-luminosity galaxies ...
... The relation between galaxies and the IGM Constrain dark energy from cluster counts and Alcock-Paczsynki test – Accurately measure luminosity functions & starformation rate densities with redshift & environment – Detailed studies of local low-luminosity galaxies ...
Tasks - ESA Science
... Astronomy is an accessible and visual science, making it ideal for educational purposes. Over the last few years the NASA/ESA Hubble Space Telescope and the ESO telescopes at the La Silla and Paranal Observatories in Chile have presented ever deeper and more spectacular views of the Universe. Howeve ...
... Astronomy is an accessible and visual science, making it ideal for educational purposes. Over the last few years the NASA/ESA Hubble Space Telescope and the ESO telescopes at the La Silla and Paranal Observatories in Chile have presented ever deeper and more spectacular views of the Universe. Howeve ...
First Light Sources at the End of the Dark Ages: Direct
... expected (e.g., at 1.44 µm or H-band, for the z~7.7 window). With GSMTs, the likely sensitivity to unresolved emission at R > 3000 is ~1.5 x 10-19 erg/s/cm2 for a half-night exposure. If a HeII (1640 Å) feature is discovered that is strong relative to the UV continuum limits from JWST and the Lyman ...
... expected (e.g., at 1.44 µm or H-band, for the z~7.7 window). With GSMTs, the likely sensitivity to unresolved emission at R > 3000 is ~1.5 x 10-19 erg/s/cm2 for a half-night exposure. If a HeII (1640 Å) feature is discovered that is strong relative to the UV continuum limits from JWST and the Lyman ...
Skill Sheet 32-B Doppler Shift
... not moving. Use an arrow to indicate the direction that the spectrum would appear to shift if the object was moving toward you. 2. The graphic to the right shows the spectral lines emitted by four moving objects. The spectral lines for when the object is stationary are shown as dotted lines on each ...
... not moving. Use an arrow to indicate the direction that the spectrum would appear to shift if the object was moving toward you. 2. The graphic to the right shows the spectral lines emitted by four moving objects. The spectral lines for when the object is stationary are shown as dotted lines on each ...
SIMULATIONS
... (evolutionary history, SFRH ..) Subresolution PDF formalism to describe MC/cirrus density field ...
... (evolutionary history, SFRH ..) Subresolution PDF formalism to describe MC/cirrus density field ...
Stellar Evolution
... • all the stars are at about the same distance from the Earth • all the stars formed at about the same time Determining the distance and age to a globular cluster is much easier than trying to find the distances and ages of a million random stars! Laboratories for understanding how stars of differen ...
... • all the stars are at about the same distance from the Earth • all the stars formed at about the same time Determining the distance and age to a globular cluster is much easier than trying to find the distances and ages of a million random stars! Laboratories for understanding how stars of differen ...
Laboratory Title: The Glittery Milky Way
... arms of the galaxy, and appears as a hazy band of white light in the night sky arching across the entire celestial sphere and originating from stars and other material that lie within the galactic plane. The stellar disk of the Milky Way galaxy is approximately 100,000 light-years (9.5×1017 km) in d ...
... arms of the galaxy, and appears as a hazy band of white light in the night sky arching across the entire celestial sphere and originating from stars and other material that lie within the galactic plane. The stellar disk of the Milky Way galaxy is approximately 100,000 light-years (9.5×1017 km) in d ...
Quasars
... Quasars and QSOs Not all quasars emit strong radio waves → radio-loud quasars & radio-quiet quasars → alternate name for radio-quiet: Quasi-Stellar Objects (QSOs) The brightness of the nucleus and the distance mask the host galaxy → appear as point sources unless observed at very high angular resolu ...
... Quasars and QSOs Not all quasars emit strong radio waves → radio-loud quasars & radio-quiet quasars → alternate name for radio-quiet: Quasi-Stellar Objects (QSOs) The brightness of the nucleus and the distance mask the host galaxy → appear as point sources unless observed at very high angular resolu ...
ASTR 001 Introduction to the Cosmos
... A) The cosmic background radiation is expected to have a temperature just a few degrees above absolute zero, and its actual temperature turns out to be about 3 K (actually 2.7 K). B) The cosmic background radiation is expected to have a blackbody(continuous) spectrum, and observations from the COBE ...
... A) The cosmic background radiation is expected to have a temperature just a few degrees above absolute zero, and its actual temperature turns out to be about 3 K (actually 2.7 K). B) The cosmic background radiation is expected to have a blackbody(continuous) spectrum, and observations from the COBE ...
Lec09_ch11_lifecycleofstars
... • An H-R census of the Globular cluster stars reveals the age of the cluster – since the globular cluster stars are gravitationally bound close together, they are the same distance from us • use apparent magnitude ...
... • An H-R census of the Globular cluster stars reveals the age of the cluster – since the globular cluster stars are gravitationally bound close together, they are the same distance from us • use apparent magnitude ...
Getting to Know: Evidence for the Big Bang Theory
... One type of evidence that has been used to support the Big Bang Theory is spectrum analysis. Spectrum analysis involves studying the wavelengths of light in the universe. We can study the wavelength of light from distant stars and galaxies to draw conclusions about their movement. For example, if ob ...
... One type of evidence that has been used to support the Big Bang Theory is spectrum analysis. Spectrum analysis involves studying the wavelengths of light in the universe. We can study the wavelength of light from distant stars and galaxies to draw conclusions about their movement. For example, if ob ...
3919 - newmanlib.ibri.org
... kkb, Akk. kakkabu, Aram. kôkb', Syr. kaukeb, Arab. kaukab. Etymologies have been proposed from kbb, burn (Akk., Aram. and Arab.) and from kabba, roll, revolve (Arab.). Unlike modern Eng. usage but parallel to ancient G, the Sem. word probably includes planets, comets, meteors, or any bright object ...
... kkb, Akk. kakkabu, Aram. kôkb', Syr. kaukeb, Arab. kaukab. Etymologies have been proposed from kbb, burn (Akk., Aram. and Arab.) and from kabba, roll, revolve (Arab.). Unlike modern Eng. usage but parallel to ancient G, the Sem. word probably includes planets, comets, meteors, or any bright object ...
PPT Slides - Center for Computational Sciences
... Star Formation in the Universe • Efficiency and speed of star formation in galaxies determined by the supersonic turbulent motions in the interstellar gas • Turbulence likely driven by combination of supernova explosions and galactic shear • Efficient star formation in young galaxies drives winds t ...
... Star Formation in the Universe • Efficiency and speed of star formation in galaxies determined by the supersonic turbulent motions in the interstellar gas • Turbulence likely driven by combination of supernova explosions and galactic shear • Efficient star formation in young galaxies drives winds t ...
10 Astrophysics (Option E)
... As people began to travel they would have noticed that the motion of these bodies depended on where they were. At the equator, the Sun’s path does not change very much from day to day, but close to the North and South Poles, the Sun doesn’t go down in the summer but describes a big circle in the sky ...
... As people began to travel they would have noticed that the motion of these bodies depended on where they were. At the equator, the Sun’s path does not change very much from day to day, but close to the North and South Poles, the Sun doesn’t go down in the summer but describes a big circle in the sky ...
Cosmology with GMRT
... Radio spectral lines from redshifted absorbers provide very competitive constraints on the cosmic variation of fundamental constants – Can be applied to a single object – Are not subject to the same systematics as optical lines – Probe a complementary redshift range ...
... Radio spectral lines from redshifted absorbers provide very competitive constraints on the cosmic variation of fundamental constants – Can be applied to a single object – Are not subject to the same systematics as optical lines – Probe a complementary redshift range ...
ppt - WISH
... Why do we want to find high-z galaxy clusters? 1. Growth of structures: the measurement of cosmological parameters. - independent of the geometric methods such as SNe distance, CMB, BAO - One of the very few ways to test GR at very large scale. 2. Galaxy evolution, cluster formation: effects of env ...
... Why do we want to find high-z galaxy clusters? 1. Growth of structures: the measurement of cosmological parameters. - independent of the geometric methods such as SNe distance, CMB, BAO - One of the very few ways to test GR at very large scale. 2. Galaxy evolution, cluster formation: effects of env ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.