Class 4 Galaxies Galaxy Classification Formation of Galaxies
... The rotation curve for the Milky Way Galaxy plots rotation speed against distance from the Galactic center. We can use this curve to compute the mass of the Galaxy. The dashed curve is the expectation if the Galaxy “ended” at a radius of 15 kpc, the limit of most of the known spiral structure and th ...
... The rotation curve for the Milky Way Galaxy plots rotation speed against distance from the Galactic center. We can use this curve to compute the mass of the Galaxy. The dashed curve is the expectation if the Galaxy “ended” at a radius of 15 kpc, the limit of most of the known spiral structure and th ...
10 meters
... At this tremendous distance we could see all the Milky Way & other galaxies too... ...
... At this tremendous distance we could see all the Milky Way & other galaxies too... ...
Galaxy3
... the luminosity of the galaxy is the same as if there where 3 x 1011 Suns in this galaxy. That means it has about 3 x 1011 times the mass of the Sun. • To do a better estimate, you look at the luminosity function, which tells you how many high mass stars, medium mass stars and low mass stars make up ...
... the luminosity of the galaxy is the same as if there where 3 x 1011 Suns in this galaxy. That means it has about 3 x 1011 times the mass of the Sun. • To do a better estimate, you look at the luminosity function, which tells you how many high mass stars, medium mass stars and low mass stars make up ...
5X_Measuring_galaxy_redshifts
... To do this, the spectrum is first re-binned into channels of equal width in ‘log wavelength’, such that the Doppler shift is the same for all channels. Largescale variations are then filtered out (i.e. only spectral lines left). The spectrum is then ‘slid’ against a template prepared from a known br ...
... To do this, the spectrum is first re-binned into channels of equal width in ‘log wavelength’, such that the Doppler shift is the same for all channels. Largescale variations are then filtered out (i.e. only spectral lines left). The spectrum is then ‘slid’ against a template prepared from a known br ...
Lab 4
... Photometry is the determination and use of the color spectrum of astronomical objects to determine the objects’ properties. Two properties you will investigate later are distance and age. The objects you will use are stars in various clusters in the Milky Way galaxy and beyond. This is known as the ...
... Photometry is the determination and use of the color spectrum of astronomical objects to determine the objects’ properties. Two properties you will investigate later are distance and age. The objects you will use are stars in various clusters in the Milky Way galaxy and beyond. This is known as the ...
Stars M. R. W. Masheder Room 4.15
... accuracy of better than a milliarcsec (mas). Its final catalogue (1997) contained about 120,000 stars, including 20,000 with d≤100 pc measured to better than 10% accuracy. In the next decade this will be surpassed by the GAIA mission which will measure distances accurately out to several kpc. (The G ...
... accuracy of better than a milliarcsec (mas). Its final catalogue (1997) contained about 120,000 stars, including 20,000 with d≤100 pc measured to better than 10% accuracy. In the next decade this will be surpassed by the GAIA mission which will measure distances accurately out to several kpc. (The G ...
File - Flipped Out Science with Mrs. Thomas!
... Unit (AU) and is sometimes used to denote large distances that are less than a light year • Distances within our universe are measured in light years and ...
... Unit (AU) and is sometimes used to denote large distances that are less than a light year • Distances within our universe are measured in light years and ...
lab 11 only - Penn State University
... The celestial sphere is divided up in a system like the \longitude-latitude" system on the Earth's surface. The latitude of an object in the sky is called the declination; an object (like Polaris) whose position is over the Earth's north pole has a declination of +90 degrees; an object over the sout ...
... The celestial sphere is divided up in a system like the \longitude-latitude" system on the Earth's surface. The latitude of an object in the sky is called the declination; an object (like Polaris) whose position is over the Earth's north pole has a declination of +90 degrees; an object over the sout ...
Scales This is a 16 meter by 16 meter scene. A meter is close in size
... Moving outward still, at 1700 light years across, we see the extended solar neighborhood. You can see our nearest stellar neighbors! Moving outward, we would be able to see the Milky Way galaxy. Since we are inside the Milky Way, we can’t take a picture from the outside, but our galaxy is a grand de ...
... Moving outward still, at 1700 light years across, we see the extended solar neighborhood. You can see our nearest stellar neighbors! Moving outward, we would be able to see the Milky Way galaxy. Since we are inside the Milky Way, we can’t take a picture from the outside, but our galaxy is a grand de ...
... the finite speed of light to measure distances. However, stars are so far away and such poor reflectors that this approach is impractical (though it is used to determine distances to planets in our solar system). The question of measuring star distances has occupied astronomers at least since the ti ...
Chapter 9 / Adobe Acrobat Document
... to those aboard the shuttle—seven astronauts died during the Challenger launch disaster and another seven astronauts died when Columbia broke up on re-entry. 28. Hubble and Humason’s distance-redshift relationship: the universe’s expansion has been confirmed by observations at very large distances a ...
... to those aboard the shuttle—seven astronauts died during the Challenger launch disaster and another seven astronauts died when Columbia broke up on re-entry. 28. Hubble and Humason’s distance-redshift relationship: the universe’s expansion has been confirmed by observations at very large distances a ...
Properties of Stars - Mr. Carter`s Earth
... The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were all the same distance away. Rather than speak of the brightness of ...
... The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were all the same distance away. Rather than speak of the brightness of ...
Cosmology Unit – FINAL EXAM PRACTICE TEST
... 10. According to the _____ law, a galaxy two times as far away from Earth as a second galaxy will be moving away approximately twice as fast. a. Sagan b. Hubble c. dark matter d. cosmological 11. In the raisin bread analogy for the universe, what do the raisins represent? a. stars b. galaxies c. bl ...
... 10. According to the _____ law, a galaxy two times as far away from Earth as a second galaxy will be moving away approximately twice as fast. a. Sagan b. Hubble c. dark matter d. cosmological 11. In the raisin bread analogy for the universe, what do the raisins represent? a. stars b. galaxies c. bl ...
Phobos
... gravitational field of a foreground star amplifies the light of a background star that momentarily aligns with it. The particular character of the light magnification can reveal clues to the nature of the foreground star and any associated planets. However, without identification and characterizatio ...
... gravitational field of a foreground star amplifies the light of a background star that momentarily aligns with it. The particular character of the light magnification can reveal clues to the nature of the foreground star and any associated planets. However, without identification and characterizatio ...
The Milky Way - Midlandstech
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer three ...
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer three ...
Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... • After eliminating any possible manmade sources she realized this emission must be coming from space. • The regularity of these pulses at first made her and her co-workers think they had discovered alien life. Jocelyn Bell Burnell in front • Later they realized these must be of the radio telescope ...
... • After eliminating any possible manmade sources she realized this emission must be coming from space. • The regularity of these pulses at first made her and her co-workers think they had discovered alien life. Jocelyn Bell Burnell in front • Later they realized these must be of the radio telescope ...
Goal: To understand how Saturn formed and
... • If the planet exerts the same force on the star as the star exerts on the planet, what will happen to the star (which is thousands to millions times more massive than the planet)? ...
... • If the planet exerts the same force on the star as the star exerts on the planet, what will happen to the star (which is thousands to millions times more massive than the planet)? ...
Light Years Away
... diameter. The Oort cloud, is a spherical cloud of comets situated about 50,000 AU from the Sun. This is approximately 1000 times the distance from the Sun to Pluto ...
... diameter. The Oort cloud, is a spherical cloud of comets situated about 50,000 AU from the Sun. This is approximately 1000 times the distance from the Sun to Pluto ...
Light Years Away
... diameter. The Oort cloud, is a spherical cloud of comets situated about 50,000 AU from the Sun. This is approximately 1000 times the distance from the Sun to Pluto ...
... diameter. The Oort cloud, is a spherical cloud of comets situated about 50,000 AU from the Sun. This is approximately 1000 times the distance from the Sun to Pluto ...
Review for Midterm 1
... How are emission, absorption, and continuous spectra created? What can the spectrum of a star tell us about the star? What else can we learn from spectra? What does the energy of a photon depend on? What is the sun mostly made of; how do we know? What are the different types of light? 3. Births of s ...
... How are emission, absorption, and continuous spectra created? What can the spectrum of a star tell us about the star? What else can we learn from spectra? What does the energy of a photon depend on? What is the sun mostly made of; how do we know? What are the different types of light? 3. Births of s ...
Ch 11a (Measuring Stars 10-28-10)
... you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent brightness is proportional to 1/d2). If we know the appare ...
... you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent brightness is proportional to 1/d2). If we know the appare ...
ISP 205 Final Exam Seating Chart SIT IN CORRECT ROW
... Slide 3: You must work your way out rung by rung, starting with the parallax method. How does the parallax method work? Pulsating variables used to get position of center of our galaxy + distance to M31, etc. What are pulsating variables and how are they used? Hubble’s law: v is measured from Dopple ...
... Slide 3: You must work your way out rung by rung, starting with the parallax method. How does the parallax method work? Pulsating variables used to get position of center of our galaxy + distance to M31, etc. What are pulsating variables and how are they used? Hubble’s law: v is measured from Dopple ...
Chapter 5. Determining Masses of Astronomical Objects
... their Synodic period (S) as described in an earlier chapter. As an example, the mass of the Sun might be found from this equation by using the data for the Earth’s orbit. We know that the period is 1 year (or 3.16 × 107 sec) and we know that the AU is 150 million km (or 1.5 × 101 1 cm). Therefore, w ...
... their Synodic period (S) as described in an earlier chapter. As an example, the mass of the Sun might be found from this equation by using the data for the Earth’s orbit. We know that the period is 1 year (or 3.16 × 107 sec) and we know that the AU is 150 million km (or 1.5 × 101 1 cm). Therefore, w ...
–1– 2. Milky Way We know a great deal, perhaps more than any
... • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is about 10 kpc, and the MW is flattened with an axial ratio of 1/5. The Sun is abo ...
... • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is about 10 kpc, and the MW is flattened with an axial ratio of 1/5. The Sun is abo ...
The Magnitude System
... It turns out that our eyes read out light signals logarithmically (this means that brightness and magnitudes have some type of logarithmic relation). The relationship was originally determined empirically and now it is used as a definition. It was found that a difference in 5 magnitudes corresponds ...
... It turns out that our eyes read out light signals logarithmically (this means that brightness and magnitudes have some type of logarithmic relation). The relationship was originally determined empirically and now it is used as a definition. It was found that a difference in 5 magnitudes corresponds ...
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.