From the Big Bang to Dark Energy
From the Big Bang to Dark Energy Hitoshi Murayama Kavli IPMU, University of Tokyo UC Berkeley, Lawrence Berkeley Laboratory
1 Credit:(NASA(
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from? Now in the realm of science!
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Outline 1. From daily life to the Big Bang 2. Birth of elements and Higgs boson 3. Dark matter and anti-matter 4. Inflation and Dark energy
3
1. From daily life to the Big Bang
4
familiar phenomena
Credit:(NASA(
5
familiar phenomena
cause
Credit:(NASA(
5
Universe familiar phenomena
cause parBcles
Credit:(NASA(
5
Night and Day
6
Credit: NASA
7
Many phenomena we take for granted require thinking about outer space 8
9
Four Seasons
10
Credit: NASA
11
Tokyo%(northern%hemi)%
Sydney%(southern%hemi)%
Tokyo%(northern%hemi)
Sydney%(southern%hemi)
35%
30% 31% 28%
25%
23%
20%
18%
15% 10%
12% 9% 9%
5% 2%
22% 18%
14% 10%
24%
20% 20%
21%
14%
15%
16%
25%
25%
24%
10%
9% 4%
Average%Low%
19% 19%
20% 18%
23%
20% 17% 17%
18%
18% 16%
15%
14%
13% 12%
4%
Average%High%
26% 26%
22%
Jan% Feb% Mar% Apr% May% Jun% Jul% Aug% Sep% Oct% Nov% Dec%
0%
1%
25%
25% 27%
11% 9%
8%
9%
5% 0%
Jan% Feb% Mar% Apr% May% Jun% Jul% Aug% Sep% Oct% Nov% Dec%
30%
Average%High%
Average%Low%
12
Sun Sun
cos 0∘=1 at an angle, the same area received less sun light
cos 60∘=1/2
13
Credit: NASA
If#true,#there#must#be#two#summers#at#the#equator#
14
Nairobi# 30# 27# 27# 25# 25#
25#
25# 23#
26# 24# 24#
22# 22# 22#
20#
15#
10# 10#
11#
12#
13#
12# 10#
11#
12# 12#
9# 9# 9#
Credit: Mandingoesque, CC BY-SA 3.0 https://commons.wikimedia.org/wiki/File:Kenya_(orthographic_projection).svg
Average#High#
Oct#
Dec#
Sep#
Nov#
Jul#
Aug#
Jun#
Apr#
May#
Jan#
Feb#
0#
Mar#
5#
Average#Low#
15
RevoluBon of the Earth
16
We are here
Aristotle
17
this is why the word “planet” means “wandering star”
18 Epicycles Ptolemy
19 Epicycles Ptolemy
Complex explanaBon!
19
You are here
8 light minutes
Copernicus
20 You are here
8 light minutes
Copernicus
Simple, but doesn’t agree with observaBons
20 Kepler
Credit:(NASA(
ellipBcal orbits single concept explains them all!
21
criteria for a good physical theory
22
criteria for a good physical theory •agree with observations/experiments
22
criteria for a good physical theory •agree with observations/experiments •unified description
22
criteria for a good physical theory •agree with observations/experiments •unified description •simple 22
why ellipBc?
23
universal gravitaBon
F =G
Mm r2 24
descendant of Newton’s apple tree
Univ. of Tokyo, Koishikawa botanical garden
25
F=ma mass ＝how difficult it is to change the motion
26
Which one is easier to move with the same force?
F＝ma 27
Credit: Gonfer, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Kepler-‐second-‐law.gif
F＝ma
F =
G
Mm R2
28
solar system
Credit: NASA/JPL
29
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
solar system
1 v/ p r
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
rotaBon speed • approximately circular F = 2 • centrifugal force F = mvr mv 2 Mm =G 2 r r r GM • orbital speed v = r
G
Mm r2
1 v/ p r
• outer planets are moving more slowly
• inner planets are faster 30
why does everything fall the same way?
31
32
32
why fall the same way? • heavier objects are hard to move ⇒ slow F＝ma • gravity is stronger on heavier objects ⇒fast Mm F = G 2 • they exactly cancel R • the answer doesn’t depend on ma = G M R2 • doesn’t sound very convincing
33
space warps • gravity is a property of space • space warps • everything is going “straight”, but ends up curving because space is warped
• then it is easy to understand why everything moves the same way!
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
general relaBvity
34
35
Black Hole • so heavy that even light can’t escape its gravity
• there are many in the Universe • heavy stars collapse to black holes at the end of their lives
• supermassive blackholes at the center of galaxies
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
36
escape velocity 1 mv 2 2 2GM v2 = R
E=
G
Mm =0 R
can’t escape if v=c c2 =
2GMBH R
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
radius of the blackhole (Schwarzschild radius) R=
2GMBH c2
R=2.95km for solar mass
strictly speaking, this Newtonian derivaBon is not correct needs to rely on general relaBvity, but the answer is right
37
beginning of the Universe look far into the past
38
Credit: NASA
39
alBtude: 375 km Credit: NASA
39
Credit: NASA
alBtude: 375 km skin of a peach
39 Kaguya Sep 30, 2008
Credit: JAXA/NHK
40 Kaguya Sep 30, 2008
380,000km =1.3 light seconds
Credit: JAXA/NHK
40
380,000km =1.3 light seconds
Credit: JAXA/NHK
41
Credit: NASA
42
1.5 108 km =8.3 light min
Credit: NASA
42
solar system
Credit: NASA/JPL
43
solar system
Credit: NASA/JPL
43
solar system Hayabusa=20 light min
Credit: NASA/JPL
43 Neptune 4 light hours
solar system
Hayabusa=20 light min
Credit: NASA/JPL
43 Neptune 4 light hours
solar system
Credit: NASA
Voyager 16 light hours
Hayabusa=20 light min
Credit: NASA/JPL
43
closest star
44
closest star
44
closest star
Proxima Centauri 4.2 lyr
44
Credit: ESO/A. Fitzsimmons, CC BY-‐SA 3.0
45
Credit: NASA
46 a hundred billion stars
Credit: NASA
47 a hundred billion stars
28,000 lyrs
Credit: NASA
47
a hundred billion stars yrs 00 l 0 , 8 2
150
rs 0 ly
Credit: Jschulman555 hZp://commons.wikimedia.org/wiki/File:NGC_4565_and_4562.jpg
48
28,000 lyrs
Credit: NASA
49
solar system revolves at 220 km/s what is pulling us inside?
28,000 lyrs
Credit: NASA
49
center of Milky Way
Credit: ESO/S. Gillessen and B. Gilli, CC BY-‐SA 3.0
50
Credit: ESO, CC BY-‐SA 3.0
51
Black Hole
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million
times solar mass at the center of Milky Way
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million •
times solar mass at the center of Milky Way other galaxies have even heavier ones
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light but no comparison to the mass of all stars combined Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light but no comparison to the mass of all stars combined can’t help keep the solar system in Credit: ESO, CC BY-‐SA 3.0
52
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
53
will collide with us in 4.5Byrs
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
53
will collide with us in 4.5Byrs
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
53
Local Group >40 galaxies
Credit: Selbst erstelltes Diagramm aus Rohdaten von CWiZe und daher gemeinfrei., CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Local_Group_Diagram_750px.png
54
Local Group >40 galaxies
4.5B years?
Credit: Selbst erstelltes Diagramm aus Rohdaten von CWiZe und daher gemeinfrei., CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Local_Group_Diagram_750px.png
54
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)-‐ESA/Hubble CollaboraBon
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)-‐ESA/Hubble CollaboraBon
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
mergers rejuvenate galaxies
55
Credit: ESA/Hubble and NASA
56
Credit: Vicent Peris, CC BY-‐SA 2.0 hZp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
57
Credit: Vicent Peris, CC BY-‐SA 2.0 hZp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
57
true nature of galaxies 100k lyrs stars
dark maZer
>M lyrs
58
cluster of galaxies
Credit: Andrew Fruchter (STScI) et al., WFPC2, HST, NASA
Abell 2218 2.1B lyrs
59
Credit: Sloan Digital Sky Survey
flying through the 3d map of galaxies based on data
60
rs ly 2B 2B lyrs
nearly uniform small wrinkles
rs ly 2B Credit: Sloan Digital Sky Survey
61
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
62
a galaxy >13B lyrs away?
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
62
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
63
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
63
Credit: NASA/ESA/STScI/JHU
64
Credit: NASA/ESA/STScI/JHU
64
Credit: NASA/ESA/STScI/JHU
64
a galaxy 13.3B lyrs away Credit: NASA/ESA/STScI/JHU
64
dark ages 13.6B lyrs
65
Universe is expanding • distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding • distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
&c q Q q Q
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red
&c q Q q Q
color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red
&c q Q q Q
color
66
Doppler effect • you may know two formulae for sounds
f0 =
V f V +v
f0 =
V
v V
f
67
Doppler effect • you may know two formulae for sounds
• Einstein’s relativity gives their geometric mean
f0 =
V f V +v
f0 =
V
f0 =
r
v V
f
V v f V +v
67
Doppler effect f0 =
V f V +v
f0 =
V
• you may know two formulae for sounds
•
Einstein’s relativity gives their geometric mean
• for slow speed
f0 =
r
v V
V
f
v
f
(v/c
1 Credit:(NASA(
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from?
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from? Now in the realm of science!
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Outline 1. From daily life to the Big Bang 2. Birth of elements and Higgs boson 3. Dark matter and anti-matter 4. Inflation and Dark energy
3
1. From daily life to the Big Bang
4
familiar phenomena
Credit:(NASA(
5
familiar phenomena
cause
Credit:(NASA(
5
Universe familiar phenomena
cause parBcles
Credit:(NASA(
5
Night and Day
6
Credit: NASA
7
Many phenomena we take for granted require thinking about outer space 8
9
Four Seasons
10
Credit: NASA
11
Tokyo%(northern%hemi)%
Sydney%(southern%hemi)%
Tokyo%(northern%hemi)
Sydney%(southern%hemi)
35%
30% 31% 28%
25%
23%
20%
18%
15% 10%
12% 9% 9%
5% 2%
22% 18%
14% 10%
24%
20% 20%
21%
14%
15%
16%
25%
25%
24%
10%
9% 4%
Average%Low%
19% 19%
20% 18%
23%
20% 17% 17%
18%
18% 16%
15%
14%
13% 12%
4%
Average%High%
26% 26%
22%
Jan% Feb% Mar% Apr% May% Jun% Jul% Aug% Sep% Oct% Nov% Dec%
0%
1%
25%
25% 27%
11% 9%
8%
9%
5% 0%
Jan% Feb% Mar% Apr% May% Jun% Jul% Aug% Sep% Oct% Nov% Dec%
30%
Average%High%
Average%Low%
12
Sun Sun
cos 0∘=1 at an angle, the same area received less sun light
cos 60∘=1/2
13
Credit: NASA
If#true,#there#must#be#two#summers#at#the#equator#
14
Nairobi# 30# 27# 27# 25# 25#
25#
25# 23#
26# 24# 24#
22# 22# 22#
20#
15#
10# 10#
11#
12#
13#
12# 10#
11#
12# 12#
9# 9# 9#
Credit: Mandingoesque, CC BY-SA 3.0 https://commons.wikimedia.org/wiki/File:Kenya_(orthographic_projection).svg
Average#High#
Oct#
Dec#
Sep#
Nov#
Jul#
Aug#
Jun#
Apr#
May#
Jan#
Feb#
0#
Mar#
5#
Average#Low#
15
RevoluBon of the Earth
16
We are here
Aristotle
17
this is why the word “planet” means “wandering star”
18 Epicycles Ptolemy
19 Epicycles Ptolemy
Complex explanaBon!
19
You are here
8 light minutes
Copernicus
20 You are here
8 light minutes
Copernicus
Simple, but doesn’t agree with observaBons
20 Kepler
Credit:(NASA(
ellipBcal orbits single concept explains them all!
21
criteria for a good physical theory
22
criteria for a good physical theory •agree with observations/experiments
22
criteria for a good physical theory •agree with observations/experiments •unified description
22
criteria for a good physical theory •agree with observations/experiments •unified description •simple 22
why ellipBc?
23
universal gravitaBon
F =G
Mm r2 24
descendant of Newton’s apple tree
Univ. of Tokyo, Koishikawa botanical garden
25
F=ma mass ＝how difficult it is to change the motion
26
Which one is easier to move with the same force?
F＝ma 27
Credit: Gonfer, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Kepler-‐second-‐law.gif
F＝ma
F =
G
Mm R2
28
solar system
Credit: NASA/JPL
29
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
solar system
1 v/ p r
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
29
rotaBon speed • approximately circular F = 2 • centrifugal force F = mvr mv 2 Mm =G 2 r r r GM • orbital speed v = r
G
Mm r2
1 v/ p r
• outer planets are moving more slowly
• inner planets are faster 30
why does everything fall the same way?
31
32
32
why fall the same way? • heavier objects are hard to move ⇒ slow F＝ma • gravity is stronger on heavier objects ⇒fast Mm F = G 2 • they exactly cancel R • the answer doesn’t depend on ma = G M R2 • doesn’t sound very convincing
33
space warps • gravity is a property of space • space warps • everything is going “straight”, but ends up curving because space is warped
• then it is easy to understand why everything moves the same way!
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
general relaBvity
34
35
Black Hole • so heavy that even light can’t escape its gravity
• there are many in the Universe • heavy stars collapse to black holes at the end of their lives
• supermassive blackholes at the center of galaxies
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
36
escape velocity 1 mv 2 2 2GM v2 = R
E=
G
Mm =0 R
can’t escape if v=c c2 =
2GMBH R
Credit: AllenMcC, CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Flamm.jpg
radius of the blackhole (Schwarzschild radius) R=
2GMBH c2
R=2.95km for solar mass
strictly speaking, this Newtonian derivaBon is not correct needs to rely on general relaBvity, but the answer is right
37
beginning of the Universe look far into the past
38
Credit: NASA
39
alBtude: 375 km Credit: NASA
39
Credit: NASA
alBtude: 375 km skin of a peach
39 Kaguya Sep 30, 2008
Credit: JAXA/NHK
40 Kaguya Sep 30, 2008
380,000km =1.3 light seconds
Credit: JAXA/NHK
40
380,000km =1.3 light seconds
Credit: JAXA/NHK
41
Credit: NASA
42
1.5 108 km =8.3 light min
Credit: NASA
42
solar system
Credit: NASA/JPL
43
solar system
Credit: NASA/JPL
43
solar system Hayabusa=20 light min
Credit: NASA/JPL
43 Neptune 4 light hours
solar system
Hayabusa=20 light min
Credit: NASA/JPL
43 Neptune 4 light hours
solar system
Credit: NASA
Voyager 16 light hours
Hayabusa=20 light min
Credit: NASA/JPL
43
closest star
44
closest star
44
closest star
Proxima Centauri 4.2 lyr
44
Credit: ESO/A. Fitzsimmons, CC BY-‐SA 3.0
45
Credit: NASA
46 a hundred billion stars
Credit: NASA
47 a hundred billion stars
28,000 lyrs
Credit: NASA
47
a hundred billion stars yrs 00 l 0 , 8 2
150
rs 0 ly
Credit: Jschulman555 hZp://commons.wikimedia.org/wiki/File:NGC_4565_and_4562.jpg
48
28,000 lyrs
Credit: NASA
49
solar system revolves at 220 km/s what is pulling us inside?
28,000 lyrs
Credit: NASA
49
center of Milky Way
Credit: ESO/S. Gillessen and B. Gilli, CC BY-‐SA 3.0
50
Credit: ESO, CC BY-‐SA 3.0
51
Black Hole
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million
times solar mass at the center of Milky Way
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million •
times solar mass at the center of Milky Way other galaxies have even heavier ones
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light
Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light but no comparison to the mass of all stars combined Credit: ESO, CC BY-‐SA 3.0
52
Black Hole • a supermassive blackhole of 4 million • • • • •
times solar mass at the center of Milky Way other galaxies have even heavier ones literally swallow gas around it their “last word” is the light but no comparison to the mass of all stars combined can’t help keep the solar system in Credit: ESO, CC BY-‐SA 3.0
52
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
53
will collide with us in 4.5Byrs
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
53
will collide with us in 4.5Byrs
Andromeda=2.5M lyr away also dark maZer important Credit: NASA
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Local Group >40 galaxies
Credit: Selbst erstelltes Diagramm aus Rohdaten von CWiZe und daher gemeinfrei., CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Local_Group_Diagram_750px.png
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Local Group >40 galaxies
4.5B years?
Credit: Selbst erstelltes Diagramm aus Rohdaten von CWiZe und daher gemeinfrei., CC BY-‐SA 3.0 hZp://commons.wikimedia.org/wiki/File:Local_Group_Diagram_750px.png
54
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)-‐ESA/Hubble CollaboraBon
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
55 Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)-‐ESA/Hubble CollaboraBon
Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. HarBg (STScI), the ACS Science Team, and ESA
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)
mergers rejuvenate galaxies
55
Credit: ESA/Hubble and NASA
56
Credit: Vicent Peris, CC BY-‐SA 2.0 hZp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
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Credit: Vicent Peris, CC BY-‐SA 2.0 hZp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
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true nature of galaxies 100k lyrs stars
dark maZer
>M lyrs
58
cluster of galaxies
Credit: Andrew Fruchter (STScI) et al., WFPC2, HST, NASA
Abell 2218 2.1B lyrs
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Credit: Sloan Digital Sky Survey
flying through the 3d map of galaxies based on data
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rs ly 2B 2B lyrs
nearly uniform small wrinkles
rs ly 2B Credit: Sloan Digital Sky Survey
61
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
62
a galaxy >13B lyrs away?
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
62
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
63
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
63
Credit: NASA/ESA/STScI/JHU
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Credit: NASA/ESA/STScI/JHU
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Credit: NASA/ESA/STScI/JHU
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a galaxy 13.3B lyrs away Credit: NASA/ESA/STScI/JHU
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dark ages 13.6B lyrs
65
Universe is expanding • distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding • distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red color
&c q Q q Q
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red
&c q Q q Q
color
66
Universe is expanding Q Q Q &c Q
• distant stars and
galaxies appear red
• approaching: high pitch
• receding: low pitch • receding stars: red
&c q Q q Q
color
66
Doppler effect • you may know two formulae for sounds
f0 =
V f V +v
f0 =
V
v V
f
67
Doppler effect • you may know two formulae for sounds
• Einstein’s relativity gives their geometric mean
f0 =
V f V +v
f0 =
V
f0 =
r
v V
f
V v f V +v
67
Doppler effect f0 =
V f V +v
f0 =
V
• you may know two formulae for sounds
•
Einstein’s relativity gives their geometric mean
• for slow speed
f0 =
r
v V
V
f
v
f
(v/c
