![Page 1: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/1.jpg)
Astronomy 1143 – Spring 2014
Lecture 21:
The Evidence for Dark Matter
![Page 2: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/2.jpg)
Key Ideas:Dark Matter - detected by its gravitational pullGravity appears stronger than can be accounted for by “normal” matter
• Expected: speeds lower if the star is very distant from the galaxy center
Mass-to-Light Ratios Evidence for Dark Matter
• Rotation curves of spiral galaxies• Hot gas halos around elliptical galaxie• Velocities of Galaxies in Cluster• Gravitational Lensing
Candidates for Dark Matter – stay tuned for evidence
![Page 3: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/3.jpg)
Is that all there is?
We have measured many forms of normal matter from light
• Stars – absorption-line spectra• Low-density gas – emission-line spectra• Dust – blocks optical/emits in the far infraredIs that amount of matter enough to explain the
gravitational force pulling on stars in a galaxy or on galaxies in a cluster?
![Page 4: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/4.jpg)
Matter produces gravity
Gravity depends on mass and distance
d M2M1
![Page 5: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/5.jpg)
Planets in the Solar System
![Page 6: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/6.jpg)
More distant planets move more slowly
![Page 7: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/7.jpg)
From Solar System to GalaxyPlanets have smaller speeds the further they are
from the Sun• Sun has about 99.8% of the mass in the Solar
System• No substantial contribution from dark matter
When we look at the same idea in a galaxy it is a little more complicated because the mass isn’t essentially concentrated in the center.
• Clearest signal looking relatively far out from center
![Page 8: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/8.jpg)
Inside the Galaxy
Gravity depends on mass and distance
rM2
M(r)
M(r) is the mass inside of radius (r)
![Page 9: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/9.jpg)
Rotation of the DiskMeasure using the Doppler EffectStars:
• Doppler shifts of stellar absorption linesIonized Gas:
• Doppler shifts of emission lines from HII regionsAtomic Hydrogen (HI) Gas:
• Cold H clouds emit a radio emission line at a wavelength of 21-cm
• Can trace nearly the entire disk beyond where the stars have begun to thin out.
![Page 10: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/10.jpg)
Measuring Masses of Galaxies
Star or Gas cloud is held in its orbit by the gravity of the mass interior to its orbit.
Newton’s Gravity:
M(R) = mass interior to radius R
Vrot = rotation speedSimilar to how we calculated the mass of the Sun in Lecture 8
![Page 11: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/11.jpg)
Rotating Disk
Rotation Axis
Approaching SideBLUESHIFT
Receding SideREDSHIFT
![Page 12: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/12.jpg)
Which galaxy is good for measuring rotation curves?
![Page 13: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/13.jpg)
Example: Milky WaySun:
r=8 kpc, vcirc=220 km/secGives: M = 91010 Msun inside r=8 kpc
Gas Cloud in Outer Disk:r=16 kpc, Vcirc=275 km/secGives: M=2.81011 Msun inside r=16 kpc
Measuring the rotation curves gives us a good way to measure the masses of Spiral Galaxies.
![Page 14: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/14.jpg)
How much mass can we find?
Gravity holding stars in their orbits tells us how much matter there needs to be
How much of that gravity is caused by the stars/gas/dust that we see?
Difference between mass needed and mass observed evidence for dark matter
Turns out that counting up the mass that we see is a little tricky, because what we see is light and what we want is mass
![Page 15: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/15.jpg)
Mass-to-light Ratio
Some of the mass in a galaxy comes from “normal” matter – stars, gas, & dust
How do we find the amount of material?• Use the light we see from stars, gas and dust• Stars – optical/near infrared light• Gas – emission lines in radio• Dust – emission in far infrared
![Page 16: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/16.jpg)
ExampleA spiral galaxy has a luminosity of 2.5x1010
LSun
If each star is like the Sun, the mass is 2.5x1010 Msun
But not every star has the same mass as the Sun – a 10 Msun main-sequence star radiates about 104 Lsun.
If each star is 10 MSun, the total mass of the Galaxy is
![Page 17: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/17.jpg)
Example
A lot smaller!
The kind of stars in a galaxy makes a big difference in the amount of matter you infer
![Page 18: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/18.jpg)
Mass in stars, gas, & dust
Measuring the amount of matter in stars, gas and dust is not easy
• Mass-to-light ratio of stars depends on age and composition
• Luminosity of starlight may be difficult to measure because of dust
• Radio and far-infrared maps need to measure gas and dust
![Page 19: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/19.jpg)
Rotation Curve if no dark matter
![Page 20: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/20.jpg)
Typical Spiral Galaxy Rotation Curve
0
0
25
200
100
5 10 15 20Radius from the Center (kpc)
Rot
atio
n S
peed
(k
m/s
ec)
![Page 21: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/21.jpg)
Picture of rotation curve on galaxy
![Page 22: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/22.jpg)
Dark matterDark matter = stuff that doesn’t emit, absorb, or otherwise interact with photons.
Other galaxies are found to have dark matterdark matter, too.
Andromeda Galaxy
![Page 23: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/23.jpg)
Galaxies are surrounded by dark matter halos
![Page 24: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/24.jpg)
Escape VelocityOne measure of the strength of the gravitational force is the escape velocityHow fast you need to be traveling to leave a gravitating mass and never come backEarth: 11 km/sJupiter: 59.5 km/s
![Page 25: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/25.jpg)
Velocities < Escape VelocitiesFor long-lived systems:
• Planets in a solar system• Stars in a galaxy• Galaxies in a galaxy cluster
velocities should be less than the escape velocity, otherwise structures would disperse
• Measure a velocity• Calculate how much mass is needed for the
escape velocity to be larger than observed velocities
![Page 26: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/26.jpg)
Velocity Dispersions in Ellipticals
Elliptical Galaxies have little to no organized rotation
But stars still bound to galaxy – cannot exceed escape velocity
Measure the velocity dispersion for ellipticalsShows that dark matter is neededBut it’s not just stars that have velocities –
gas particles do too!
![Page 27: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/27.jpg)
Hot Gas in Ellipticals
We see hot X-ray emitting gas around ellipticals. The gas is gravitationally bound to the galaxy.
Velocities of gas particles must be smaller than escape velocity
Velocity from Temperature of Gas
![Page 28: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/28.jpg)
ExampleThe T of X-ray gas in NGC 4636 is 11.6 million K. How
much mass is needed to hold onto that gas?T=11.6 million K velocity of proton = 437,740 m/s60 kpc from the center = 1.85 x 1021 m
Only about 1x1011MSun in stars, gas & dust. Need dark matter!
![Page 29: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/29.jpg)
![Page 30: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/30.jpg)
Velocities of Galaxies in Clusters
Additional evidence for the presence of dark matter comes from the high velocities of galaxies in clusters
Galaxies are moving at 800-1000 km/s compared to the cluster center
Amount of matter we measure from the light is not enough to prevent their escape!
90-99% of the matter in clusters is dark matter
![Page 31: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/31.jpg)
Zwicky in actionWhere’s the matter?
![Page 32: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/32.jpg)
Insight from Einstein: Gravitational Lensing
![Page 33: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/33.jpg)
Gravitational LensingThe amount of
gravitational lensing depends on the curvature of spacetime
We see lots of bending – lots of matter
Conclusion: cluster masses are dominated by dark matter
![Page 34: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/34.jpg)
Possible candidatesStellar remnants • Black holes• Neutron stars• White dwarfsBrown Dwarfs & PlanetsParticle• Neutrino• New Particle – Weakly Interacting Massive
Particles (WIMPs)
MACHOs --MAssive COmpact Halo Objects
![Page 35: Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter](https://reader035.vdocument.in/reader035/viewer/2022081514/5a4d1b4f7f8b9ab0599a7023/html5/thumbnails/35.jpg)
Is “Dark Matter” the only possible explanation?It is not easy to believe that we are unaware of
the nature of something that has 5-6 times more mass than “normal” matter
However, many lines of evidence are pointing to the same conclusion!
Possible counter explanation: • Neither Newton nor Einstein got the law of gravity
quite right. • On galaxy-sized scales, gravity stronger than what
Law of Universal Gravity states