The Cosmic Distance Ladder. Hubble s Law and the Expansion of the Universe!
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1 The Cosmic Distance Ladder Hubble s Law and the Expansion of the Universe!
2 Last time: looked at Cepheid Variable stars as standard candles.
3 Massive, off-main sequence stars: at a certain stage between main sequence and red supergiant they are unstable and pulsate. It turns out that pulsation is dependent on the underlying luminosity of the star (outward pressure) What ARE cepheid variables?
4 Massive, off-main sequence stars: at a certain stage between main sequence and red supergiant they are unstable and pulsate. It turns out that pulsation is dependent on the underlying luminosity of the star (outward pressure) What ARE cepheid variables?
5 Cepheid Variable stars show a period luminosity relationship. If we observe a cepheid variable with a 4 day pulsing period and a flux of x W/m 2, how far away is it in parsecs? (Recall L = W and 1 pc = m ) pc
6 Cepheid Variable stars show a period luminosity relationship. If we observe a cepheid variable with a 4 day pulsing period and a flux of x W/m 2, how far away is it in parsecs? (Recall L = W and 1 pc = m ) 4000 pc
7 Cepheid Variables aren t the only standard candles in the Universe: Meet the MUCH brighter and much more rare Type Ia supernovae / White Dwarf Supernovae
8 Cepheid Variables aren t the only standard candles in the Universe: Meet the MUCH brighter and much more rare Type Ia supernovae / White Dwarf Supernovae There s a binary star system
9 Cepheid Variables aren t the only standard candles in the Universe: Meet the MUCH brighter and much more rare Type Ia supernovae / White Dwarf Supernovae There s a binary star system One of those stars turns into a white dwarf! The other could be quite close start feeding the white dwarf material as it goes into a giant phase
10 Cepheid Variables aren t the only standard candles in the Universe: Meet the MUCH brighter and much more rare Type Ia supernovae / White Dwarf Supernovae There s a binary star system One of those stars turns into a white dwarf! The other could be quite close start feeding the white dwarf material as it goes into a giant phase Once the white dwarf exceeds ~1.4 solar masses, SUPERNOVA!
11 Cepheid Variables aren t the only standard candles in the Universe: Meet the MUCH brighter and much more rare Type Ia supernovae / White Dwarf Supernovae There s a binary star system One of those stars turns into a white dwarf! The other could be quite close start feeding the white dwarf material as it goes into a giant phase Once the white dwarf exceeds ~1.4 solar masses, SUPERNOVA! As a result of us figuring out this is what s happening, it is also a standard candle (fixed mass when it explodes) and is visible from the edge of the Universe!
12 Overview of the the Cosmic Distance Ladder Distant Galaxies, Edge of Universe (FARTHER) The Milky Way Galaxy and some very nearby galaxies The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
13 Overview of the the Cosmic Distance Ladder Distant Galaxies, Edge of Universe (FARTHER) The Milky Way Galaxy and some very nearby galaxies RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
14 Overview of the the Cosmic Distance Ladder Distant Galaxies, Edge of Universe (FARTHER) The Milky Way Galaxy and some very nearby galaxies STELLAR PARALLAX RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
15 Overview of the the Cosmic Distance Ladder Distant Galaxies, Edge of Universe (FARTHER) The Milky Way Galaxy and some very nearby galaxies M.S. Fitting STELLAR PARALLAX RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
16 Overview of the the Cosmic Distance Ladder Distant Galaxies, Edge of Universe (FARTHER) CEPHEID VARIABLES The Milky Way Galaxy and some very nearby galaxies M.S. Fitting STELLAR PARALLAX RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
17 Overview of the the Cosmic Distance Ladder TYPE 1A SUPERNOVAE Distant Galaxies, Edge of Universe (FARTHER) CEPHEID VARIABLES The Milky Way Galaxy and some very nearby galaxies M.S. Fitting STELLAR PARALLAX RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
18 Overview of the the Cosmic Distance Ladder TYPE 1A SUPERNOVAE (homework calls this white dwarf supernovae ) Distant Galaxies, Edge of Universe (FARTHER) CEPHEID VARIABLES The Milky Way Galaxy and some very nearby galaxies M.S. Fitting STELLAR PARALLAX RADAR The Solar Neighborhood (nearby stars) The Solar System (CLOSER)
19 Overview of the the Cosmic Distance Ladder TYPE 1A SUPERNOVAE (homework calls this white dwarf supernovae ) CEPHEID VARIABLES M.S. Fitting Key points about the cosmic distance ladder: STELLAR PARALLAX RADAR Distant Galaxies, ** Each step is reliant Edge upon good of Universe calibration of the step below (on smaller scales). For example, we couldn t use cepheid variables at all if we couldn t first measure parallax distances to a few cepheids. ** Overlap is needed The Milky Way Galaxy and some very nearby galaxies ** Any distance measurement made far away is only as good as the worst The distance Solar Neighborhood measurement it relies on lower in the chain. (nearby stars) The Solar System (FARTHER) (CLOSER)
20 Hubble s Law and the Expansion of the Universe!
21 Let s take another look at the Universe as we last left it: ly ly
22 Let s take another look at the Universe as we last left it: ly Edwin Hubble ly Milton Humason In the 1920s, these guys were busy trying to measure the distance to nearish galaxies using variable stars.
23 Let s take another look at the Universe as we last left it: How BIG is the Universe?! ly Edwin Hubble ly Milton Humason In the 1920s, these guys were busy trying to measure the distance to nearish galaxies using variable stars.
24 Mt. Wilson Observatory, San Gabriel Mountains, California Edwin Hubble Milton Humason In the 1920s, these guys were busy trying to measure the distance to nearish galaxies using variable stars.
25 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift
26 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
27 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
28 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
29 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
30 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
31 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift Vesto Slipher
32 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift energy output energy output energy output wavelength
33 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift energy output energy output energy output Vesto Slipher wavelength
34 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift energy output energy output energy output Vesto Slipher wavelength
35 Meanwhile, in Flagstaff, AZ measurements of galaxies spectra were being made. He kept finding a shift energy output energy output energy output Vesto Slipher wavelength
36 What does this shift tell us? energy output wavelength (a) (b) (c) (d) the galaxy composition is different than initially thought the galaxy is moving away from us the galaxy is moving towards us the galaxy is made up of billions of stars
37 What does this shift tell us? energy output wavelength (a) (b) (c) (d) the galaxy composition is different than initially thought the galaxy is moving away from us the galaxy is moving towards us the galaxy is made up of billions of stars
38 What does this shift tell us? energy output 1+z = obs emit wavelength redshift (a) (b) (c) (d) the galaxy composition is different than initially thought the galaxy is moving away from us the galaxy is moving towards us the galaxy is made up of billions of stars
39 What does this shift tell us? energy output 1+z = obs emit wavelength redshift (a) (b) (c) (d) the galaxy composition is different than initially thought the galaxy is moving away from us the galaxy is moving towards us the galaxy is made up of billions of stars
40 Holds when v is small Holds ALWAYS z v c 1+z = obs emit redshift
41 And slowly the measurements were compiled (Redshift) Doppler Velocity Distance
42 And slowly the measurements were compiled (Redshift) Doppler Velocity Distance
43 And slowly the measurements were compiled
44 Where are these galaxies located in the sky? EVERYWHERE
45 Where are these galaxies located in the sky? EVERYWHERE (WOAH)
46 Where are these galaxies located in the sky? Galaxies further away from us are speeding away from us faster than those closer to us: the Universe is Expanding EVERYWHERE (WOAH)
47 Let s think about this whole expanding Universe thing. Why isn t this just something going on with our point of view?
48 Hubble s Law (a) (b) galaxies are mostly receding away from us, the velocity of their recession is proportional to their distance from us. (Redshift) Doppler Velocity Distance
49 (Redshift) Doppler Velocity Work through the following with your groups A Hubble Plot Distance 1. Imagine the Hubble plot at right represents a universe that doubles in size over a certain amount of time. Which of the Hubble plots below might represent a Universe that triples in size over the same amount of time? (Redshift) Doppler Velocity (Redshift) Doppler Velocity Distance Distance 2. The expansion rate of the Universe determines how fast the universe increases in size with time. For example, a universe that is tripling in size has a faster expansion rate than a universe that is doubling in size over the same amount of time. In a Hubble plot, what quantity represents the expansion rate of the Universe? 3. From the plot in the upper left, would you say the Universe has a constant expansion rate, an increase or a decreasing expansion rate with time? 4. Rank the three plots above from fastest (1) to slowest (3) expansion rates. 5. If the expansion rate had been faster than measured, would the Universe have reached its current size earlier in its history or later? 6. Using your answers from #4 and #5, rank the three plots above from youngest (1) to oldest (3) Universe. Learning Catalytics Question: On the blank graph at right, draw a Hubble plot for which the expansion rate of the Universe is zero (i.e. no expansion). (Redshift) Doppler Velocity Distance
50 (Redshift) Doppler Velocity Work through the following with your groups A Hubble Plot Distance 1. Imagine the Hubble plot at right represents a universe that doubles in size over a certain amount of time. Which of the Hubble plots below might represent a Universe that triples in size over the same amount of time? (Redshift) Doppler Velocity (Redshift) Doppler Velocity Distance Distance 2. The expansion rate of the Universe determines how fast the universe increases in size with time. For example, a universe that is tripling in size has a faster expansion rate than a universe that is doubling in size over the same amount of time. In a Hubble plot, what quantity represents the expansion rate of the Universe? 3. From the plot in the upper left, would you say the Universe has a constant expansion rate, an increase or a decreasing expansion rate with time? 4. Rank the three plots above from fastest (1) to slowest (3) expansion rates. 5. If the expansion rate had been faster than measured, would the Universe have reached its current size earlier in its history or later? 6. Using your answers from #4 and #5, rank the three plots above from youngest (1) to oldest (3) Universe. Learning Catalytics Question: On the blank graph at right, draw a Hubble plot for which the expansion rate of the Universe is zero (i.e. no expansion). (Redshift) Doppler Velocity Distance
51 The expanding Universe! By Phil
52 The expanding Universe! By Phil
53 An expanding Universe implies a Big Bang.
54 An expanding Universe implies a Big Bang.
55 Answer to learning catalytics question. velocity distance Expanding Contracting
56 Answer to learning catalytics question. Expanding quickly velocity distance Expanding Contracting Expanding slowly
57 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H 0 D H 0 70km s 1 Mpc 1
58 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H 0 D H 0 70km s 1 Mpc 1
59 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H 0 D H 0 70km s 1 Mpc 1
60 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H 0 D H 0 70km s 1 Mpc 1
61 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H0 D H0 70km s 1 Mpc 1
62 Expanding slowly Expanding Expanding quickly The slope of this line is called the HUBBLE CONSTANT, describes the expansion rate of the Universe. v = H0 D H0 70km s 1 Mpc 1
63 velocity Question 13 Now sketch what you think you might see for a Universe where the expansion rate increases throughout the lifetime of the Universe. distance Expanding Contracting?
64 velocity Question 13 Now sketch what you think you might see for a Universe where the expansion rate increases throughout the lifetime of the Universe. distance Expanding Contracting?
65 Recall from Lecture #1?? ~1 hour ~8 min billions of years! ~25,000 years ~4.4 years? ~2.5 million years ~13.8 billion years? LIGHT is what we measure in the Universe, 8 and its speed is finite and fixed: 3 x10 m/s THE FURTHER AWAY THINGS ARE THE LONGER IT TOOK THAT LIGHT TO REACH US.
66 2010s 1960s 1940s 1950s 1990s 1970s Let s use events from history to context this
67 2010s 1960s 1940s 1950s 1990s 1970s Let s use events from history to context this fa
68 (Redshift) Doppler Velocity Distance
69 (Redshift) Doppler Velocity Distance
70 faster growth (Redshift) Doppler Velocity Distance
71 faster growth (Redshift) Doppler Velocity Distance slower growth
72 faster growth? (Redshift) Doppler Velocity Distance slower growth
73 How would you describe this type of curve on the Hubble plot? faster growth t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
74 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
75 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
76 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
77 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
78 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
79 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
80 How would you describe this type of curve on the Hubble plot? faster growth these measurements are from galaxies in the distant past! t0 (Redshift) Doppler Velocity t3 t2 t1 slower growth Distance
81 One comment on distances. The vast majority of galaxies do NOT have distance measurements. They only have redshift measurements, because Supernovae are rare, and cepheid variables only take us so far (not bright enough to see across the Universe). Most galaxies only have redshifts. But this is actually used as a distance proxy, in the context of the Hubble plot where we do have distances.
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