The Pennsylvanian Period in Alabama: Looking Up Astronomy and
... Few humans would deny that the night sky is one of the most beautiful things in nature. On a clear, dark moonless night unaffected by light pollution, one can see as many as 3000 naked-eye stars. One of the most profound things about the night sky is that it is like a time machine. When we look out ...
... Few humans would deny that the night sky is one of the most beautiful things in nature. On a clear, dark moonless night unaffected by light pollution, one can see as many as 3000 naked-eye stars. One of the most profound things about the night sky is that it is like a time machine. When we look out ...
Chapter 8: The Pennsylvanian Period in Alabama: Looking Up
... Few humans would deny that the night sky is one of the most beautiful things in nature. On a clear, dark moonless night unaffected by light pollution, one can see as many as 3000 naked-eye stars. One of the most profound things about the night sky is that it is like a time machine. When we look out ...
... Few humans would deny that the night sky is one of the most beautiful things in nature. On a clear, dark moonless night unaffected by light pollution, one can see as many as 3000 naked-eye stars. One of the most profound things about the night sky is that it is like a time machine. When we look out ...
Document
... Problems ---(1) Virgo ≠ CMB (2) Hydra-Cen ≠ CMB (3) GA + Virgo ≠ CMB amplitude (4) Honkin’ Pisces-Perseus on the other side (5) Where is Convergence? (6) Biasing ...
... Problems ---(1) Virgo ≠ CMB (2) Hydra-Cen ≠ CMB (3) GA + Virgo ≠ CMB amplitude (4) Honkin’ Pisces-Perseus on the other side (5) Where is Convergence? (6) Biasing ...
Freeman_DM2
... We have had a long controversy over the last few years about whether the rotation curves imply cusped or cored dark halos. This continues to be very illuminating Galaxies of low surface brightness are important in this debate. The normal or high surface brightness spirals have a fairly well defined ...
... We have had a long controversy over the last few years about whether the rotation curves imply cusped or cored dark halos. This continues to be very illuminating Galaxies of low surface brightness are important in this debate. The normal or high surface brightness spirals have a fairly well defined ...
Habitable Zone
... • If Mars were larger and with a thicker atmosphere, Mars could have strong enough greenhouse warming to have surface liquid water. • Calculations show that the outer boundary is ~1.7AU (Mars is at 1.52AU) • However, in cold atmosphere, CO2 could condense on snowflakes and fall onto the ground red ...
... • If Mars were larger and with a thicker atmosphere, Mars could have strong enough greenhouse warming to have surface liquid water. • Calculations show that the outer boundary is ~1.7AU (Mars is at 1.52AU) • However, in cold atmosphere, CO2 could condense on snowflakes and fall onto the ground red ...
Document
... (iv) Early in its formation the cloud was approximately spherical with a diameter of 6 AU and a temperature of 100 K. Show that the gas pressure inside the giant molecular cloud was about 1 Pa. The gas cloud behaves as an ideal gas. ...
... (iv) Early in its formation the cloud was approximately spherical with a diameter of 6 AU and a temperature of 100 K. Show that the gas pressure inside the giant molecular cloud was about 1 Pa. The gas cloud behaves as an ideal gas. ...
Y13 Cosmology HW booklet
... (iv) Early in its formation the cloud was approximately spherical with a diameter of 6 AU and a temperature of 100 K. Show that the gas pressure inside the giant molecular cloud was about 1 Pa. The gas cloud behaves as an ideal gas. ...
... (iv) Early in its formation the cloud was approximately spherical with a diameter of 6 AU and a temperature of 100 K. Show that the gas pressure inside the giant molecular cloud was about 1 Pa. The gas cloud behaves as an ideal gas. ...
7/3 Some stars were found in regions above the main sequence
... main sequence spectra and spectra from giant stars. Giant stars, while much larger than main sequence stars, are no more massive. They are much less dense, and the effect of the low density on the spectrum can be measured. Luminosity Classes: Ia. Bright Supergiants Ib. Supergiants II. Bright Giants ...
... main sequence spectra and spectra from giant stars. Giant stars, while much larger than main sequence stars, are no more massive. They are much less dense, and the effect of the low density on the spectrum can be measured. Luminosity Classes: Ia. Bright Supergiants Ib. Supergiants II. Bright Giants ...
Powerpoint on redshift
... When you look at distant galaxies they don’t actually seem redder. The speed of light is too fast for us to be able to see a colour change. We see red shift as a movement of spectral absorption lines. The dark lines should always appear in the same place, as the atoms can only absorb certain w ...
... When you look at distant galaxies they don’t actually seem redder. The speed of light is too fast for us to be able to see a colour change. We see red shift as a movement of spectral absorption lines. The dark lines should always appear in the same place, as the atoms can only absorb certain w ...
22. The Milky Way Galaxy
... Composition unknown. Probably mostly exotic particles that don't interact with ordinary matter at all (except gravity). Some may be brown dwarfs, cold white dwarfs … Most likely it's a dark halo surrounding the Milky Way. Or we need a new theory of gravity. ...
... Composition unknown. Probably mostly exotic particles that don't interact with ordinary matter at all (except gravity). Some may be brown dwarfs, cold white dwarfs … Most likely it's a dark halo surrounding the Milky Way. Or we need a new theory of gravity. ...
Galaxy interaction and transformation
... The properties of such merger remnants are important to understand. If we know how merger remnants behave, we can look for merger signatures and estimate how many mergers have occurred during the history of the universe. More importantly, the study of the structure of merger remnants can help us to ...
... The properties of such merger remnants are important to understand. If we know how merger remnants behave, we can look for merger signatures and estimate how many mergers have occurred during the history of the universe. More importantly, the study of the structure of merger remnants can help us to ...
Slide 1
... Electrons being ejected out of an atom. Electrons being lifted into an excited state in ...
... Electrons being ejected out of an atom. Electrons being lifted into an excited state in ...
Size and Scale of the Universe
... There are two basic methods for measuring astronomical distances: the standard rulers and the standard candles... ...
... There are two basic methods for measuring astronomical distances: the standard rulers and the standard candles... ...
Star-Galaxy Classification Using Data Mining
... manageable, 5,000 objects were randomly sampled from the entire dataset. After analyzing the ranges of stellarity for the objects within the unknown group in more detail, the results still appeared to be somewhat misleading. First, approximately 290,000 objects fell into the stellarity range above 0 ...
... manageable, 5,000 objects were randomly sampled from the entire dataset. After analyzing the ranges of stellarity for the objects within the unknown group in more detail, the results still appeared to be somewhat misleading. First, approximately 290,000 objects fell into the stellarity range above 0 ...
Size and Scale of the Universe
... There are two basic methods for measuring astronomical distances: the standard rulers and the standard candles... ...
... There are two basic methods for measuring astronomical distances: the standard rulers and the standard candles... ...
Galaxy Evolution in the SDSS Low
... Average of 10 runs per object over factor of 3 improvement in S/N: e.g., at spectroscopic sample limit rP=19.5, median Petrosian mag error is 0.07 mag for an individual run (measured from empirical run-to-run scatter), but only 0.02 mag for catalog coadd Star/galaxy separation criterion rPSF – rmo ...
... Average of 10 runs per object over factor of 3 improvement in S/N: e.g., at spectroscopic sample limit rP=19.5, median Petrosian mag error is 0.07 mag for an individual run (measured from empirical run-to-run scatter), but only 0.02 mag for catalog coadd Star/galaxy separation criterion rPSF – rmo ...
Hubble Diagram Instruction Sheet
... Measuring distances in space is a daunting task. One method is to use an object with a known absolute magnitude (M); we call these Standard Candles. Type Ia supernovae are standard candles. There are two classes of supernovae, Type I and Type II. For this activity we will be using Type Ia supernovae ...
... Measuring distances in space is a daunting task. One method is to use an object with a known absolute magnitude (M); we call these Standard Candles. Type Ia supernovae are standard candles. There are two classes of supernovae, Type I and Type II. For this activity we will be using Type Ia supernovae ...
Leiden Oktober 2005 - Royal Observatory, Edinburgh
... Herschel Open-Time Key-Programme proposal to study the cluster infall region use well-defined rich cluster sample at z≈0.5 map the infall region around these clusters out to around 5 Mpc (depending on cluster mass) measure SFR and LIR for each galaxy measure stellar masses from near-IR (fol ...
... Herschel Open-Time Key-Programme proposal to study the cluster infall region use well-defined rich cluster sample at z≈0.5 map the infall region around these clusters out to around 5 Mpc (depending on cluster mass) measure SFR and LIR for each galaxy measure stellar masses from near-IR (fol ...
Document
... Define Short-term Photometric Resolution (STPR) as s/m for a Gaussian fit to a histogram of several hundred signal measurements for a given star and Long-term Photometric Resolution (LTPR) as s/m for the nightly average signal measure of a given star over an entire campaign. LTPR vs Mean Stellar Si ...
... Define Short-term Photometric Resolution (STPR) as s/m for a Gaussian fit to a histogram of several hundred signal measurements for a given star and Long-term Photometric Resolution (LTPR) as s/m for the nightly average signal measure of a given star over an entire campaign. LTPR vs Mean Stellar Si ...
Astronomy Chapter 17 – Galaxies A. Main Ideas 1. Discovering
... parallax to measure such large distances because the angle by which the galaxy’s position changes as we move around the Sun is too small to be measured. Astronomers use the method of standard candles to measure the distance to distant galaxies. Using the inverse-square law and the known luminosity o ...
... parallax to measure such large distances because the angle by which the galaxy’s position changes as we move around the Sun is too small to be measured. Astronomers use the method of standard candles to measure the distance to distant galaxies. Using the inverse-square law and the known luminosity o ...
Astronomy Final C - Tarleton State University
... 78. It is believed that the Sagittarius Dwarf Elliptical Galaxy collided with the A.Andromeda Galaxy B.Triangulum Galaxy C.Milky Way Galaxy D.Small Magellanic Cloud E.Large Magellanic Cloud 79. The “Strong Force” A.consists of photons B.represents the decay of elementary particles C.binds particles ...
... 78. It is believed that the Sagittarius Dwarf Elliptical Galaxy collided with the A.Andromeda Galaxy B.Triangulum Galaxy C.Milky Way Galaxy D.Small Magellanic Cloud E.Large Magellanic Cloud 79. The “Strong Force” A.consists of photons B.represents the decay of elementary particles C.binds particles ...
Stellar Deaths - Mid
... What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion. Energy is produced. (A small amount of mass = a lot of energy) E = mc2. Sum of mass and energy always conserved in reactions. Mass is just “frozen” ...
... What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion. Energy is produced. (A small amount of mass = a lot of energy) E = mc2. Sum of mass and energy always conserved in reactions. Mass is just “frozen” ...
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.