Dark Matter Mike Brotherton Professor of Astronomy, University of Wyoming Author of Star Dragon and Spider Star.

Slides:



Advertisements
Similar presentations
Dark Matter, Dark Energy, and the Current State of Cosmology
Advertisements

Olber’s paradox Why isn't the night sky as uniformly bright as the surface of the Sun? If the Universe has infinitely many stars, then it should be uniformly.
Week 10 Dark Matter Reading: Dark Matter: 16.1, 16.5d (4 pages)
Dark Matter. Either dark matter exists or we do not understand how gravity operates across galaxy-sized distances. We have many reasons to have confidence.
Dark Matter Da yang Jacob Daeffler. What do we mean by dark matter? Material whose presence can be inferred from its effects on the motions of stars and.
Dark Matter, Dark Energy, and the Fate of the Universe.
Chapter 16 Dark Matter And The Fate Of The Universe.
Newton’s Hypothesis The universe is infinite, static and uniform. Proven to be incorrect by Olber’s Paradox. Olber theorised that if this was correct then.
Chapter 20 Dark Matter, Dark Energy, and the Fate of the Universe.
Components of the Milky Way. Examples of Rotation Curves.
Stellar Kinematics Astronomy 315 Professor Lee Carkner Lecture 17.
PRESENTATION TOPIC  DARK MATTER &DARK ENERGY.  We know about only normal matter which is only 5% of the composition of universe and the rest is  DARK.
© 2010 Pearson Education, Inc. Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe.
Chapter 23: Our Galaxy Our location in the galaxy Structure of the galaxy Dark matter Spiral arm formation Our own supermassive black hole.
Physics 133: Extragalactic Astronomy and Cosmology Lecture 12; February
The latest experimental evidence suggests that the universe is made up of just 4% ordinary matter, 23% cold dark matter and 73% dark energy. These values.
ASTR100 (Spring 2008) Introduction to Astronomy The Case for Dark Matter Prof. D.C. Richardson Sections
DARK MATTER Matthew Bruemmer. Observation There are no purely observational facts about the heavenly bodies. Astronomical measurements are, without exception,
Stellar Kinematics Astronomy 315 Professor Lee Carkner Lecture 18.
What is the Dark Matter? What about “ordinary” non-luminous matter (basically, made from proton, neutrons and electrons)? “Dead stars” (White Dwarfs,
Dark Matter Masses of Galaxies Gravity and Light Black Holes What is Dark Matter?
Astro-2: History of the Universe Lecture 5; April
Dark Matter begin. Definition Dark Matter is matter that we cannot see. It neither emits nor reflects any light. If we can’t see it, how do we know it.
Dark Matter and Dark Energy Just because something is unknown does not make it unknowable 1.
Components of the Milky Way The light from galaxies is centrally concentrated. But is the mass also centrally concentrated? Does Mass follow Light in Galaxies?
Galaxy Mass Star Number/Density Counting stars in a given volume
Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe
Dark Matter, Dark Energy, How Come Some People Think We Need It and Others Don’t and the Fate of the Universe.
Dark Matter in Galaxies and Clusters AST 112. Matter Galaxies appear to be made up of stars, gas and dust Reasonable to think that’s the end of the story…
YSS - Intro. to Observational Astrophysics (ASTR 205) Class #13 Dark Matter, Dark Energy, and the Fate of the Universe (Chapter 16) Professor: José Maza.
North America at night from space. Light can be: broken up into component colors broken up into component colors absorbed absorbed reflected reflected.
The Universe  What do we know about it  age: 14.6 billion years  Evolved from Big Bang  chemical composition  Structures.
Lecture 18 : Weighing the Universe, and the need for dark matter Recap – Constraints on the baryon density parameter  B The importance of measuring the.
Dark Matter. Zwicky’s Coma In 1933 Fred Zwicky measured the speed of Coma cluster galaxies. –Too fast for the visible stars –Cluster would fly apart Either.
Cosmology Olber’s Paradox Big Bang Development of the Universe.
Chapter 16 Dark Matter, Dark Energy, and the Fate of the Universe.
Lecture Outline Chapter 18: Dark Matter, Dark Energy, and the Fate of the Universe © 2015 Pearson Education, Inc.
So, how’s it gonna end? The Big Bang started the universe expanding fast, but gravity should have put on the brakes. Expansion should slow down after.
Origins: Dark Matter & Dark Energy WWK: Students will understand the theories of Dark Matter & Dark Energy and how they’re thought to affect the Universe.
Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe.
Dark Matter: Some Observational Evidence Mike Gladders.
Gravitational Lensing: How to See the Dark J. E. Bjorkman University of Toledo Department of Physics & Astronomy.
Dark Matter and Dark Energy. Most of the universe is dark matter and dark energy. Most of the mass-energy, about 95%, in the universe is ‘dark’. By dark.
What forms the “texture” of the universe? Figure from book.
Astronomy 1143 – Spring 2014 Lecture 30: Dark Matter Revisted…..
Goal: To understand clusters of galaxies including the one we are located in called the Local Group Objectives: 1)To learn about the Sizes of Clusters.
A Quick Look At The History of Dark Matter Dan Hooper Fermilab/University of Chicago Cosmology Short Course For Museum and Planetarium Staff September.
Lecture 39: Dark Matter review from last time: quasars first discovered in radio, but not all quasars are detected in the radio first discovered in radio,
More to the universe than meets the eye
Composition Until 30 years ago, we thought all matter was “baryonic” matter (protons, neutrons, electrons). Now: 4.6% is baryonic matter 95% is non-baryonic.
Physics 55 Monday, December 5, Course evaluations. 2.General relativity with applications to black holes, dark matter, and cosmology. 3.Hubble’s.
Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter.
Dark Matter By Joel Tome Period 3. What is Dark Matter? ►T►T►T►The mass in galaxies and galactic clusters inferred to exist: bbbby rotational properties.
LUMINOUS MATTER  luminous = »The matter that astronomers see in the Universe (stars, dust clouds, etc.) makes up less than 1/2 of one percent of.
Yale Summer Class: Observational Astronomy. Class #13 Dark Matter, Dark Energy, and the Fate of the Universe Professor: José Maza July 6, 2009 Professor:
Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.
Public Star Party Organized by Institute for Astronomy, University of Hawaii. Contact person: Prof. Jim Heasley. When? Tonight between 8:30 and 10 pm.
Dark Matter, Dark Energy
2. April 2007J.Wicht : Dark Matter2 Outline ● Three lecturers spoke about Dark Matter : – John Ellis, CMB and the Early Universe – Felix Mirabel, High-Energy.
Wormholes. The simplest example The r = 2m singularity is more complicated than previously mentioned… Has solution (the Schwarzschild metric):
Homework: To prepare for TMT discussions next week, you should read the following article critically…
The Dark Universe Susan Cartwright.
Lecture 18 : Weighing the Universe, and the need for dark matter
Dark Matter, Dark Energy And The Fate Of The Universe
dark matter and the Fate of the Universe
FORMATION OF THE UNIVERSE
Dark Matter Background Possible causes Dark Matter Candidates
The “Dark Matter” Problem…!
Dark Matter, Dark Energy, and the Fate of the Universe
Homework #10 is due Wednesday, April 25, 9:00 pm. Review session Wednesday, April 25, 7:15 pm.
Presentation transcript:

Dark Matter Mike Brotherton Professor of Astronomy, University of Wyoming Author of Star Dragon and Spider Star

The Father of Dark Matter In 1933, Fritz Zwicky checked out the Coma Cluster. The galaxies were flying around too fast (as measured by the Doppler effect) for their visible mass to keep them together, so he proposed dark matter was present.

The Mother of Dark Matter A few decades later, Vera Rubin started to notice FLAT rotation curves in spiral galaxies.

Flat Rotation Curves – so what? Following Rieke, images from Bennett and Pryke

The Nature of Dark Matter Can dark matter be composed of normal matter? If so, then its mass would mostly come from protons and neutrons = baryons The density of baryons right after the big bang leaves a unique imprint in the abundances of deuterium and lithium. Density of baryonic matter is only ~ 4 % of critical density, total is 30%. Most dark matter must be non-baryonic!

WIMPs??? “WIMP” = Weakly interactive massive particle –Neutrinos? Seem to have mass, but too small. –Axions? From Wikipedia, “The axion is a hypothetical elementary particle postulated by Peccei-Quinn theory in 1977 to resolve the strong-CP problem in quantum chromodynamics (QCD).” elementary particlePeccei-Quinn theorystrong-CP problem quantum chromodynamics As yet, not detected (axions are predicted to change to and from photons in the presence of strong magnetic fields, and this property is used for creating experiments to detect axions)photons

MaCHOs “MaCHO” = Massive Compact Halo Object –Just trying to explain flat rotation curves with things like black holes, brown dwarfs, etc. –These are “Baryonic,” made from conventional stuff on the periodic table (like people, planets, etc.) –Can be probed via gravitational microlensing

Baryonic Dark Matter Nature of baryonic dark matter still very uncertain and speculative. One component: Massive Compact Halo Objects = “MACHOs”: Small compact objects (e.g., brown dwarfs, small black holes) acting as gravitational lenses. Earth Brightness of background star Time Distant background star MACHO

Are we sure Dark Matter is real? Astronomers have argued that dark matter can explain the strange motions of galaxies in clusters and stars in galaxies, but that it can’t be normal stuff Could we just have gotten gravity wrong on large scales? –“MoND” = Modified Newtonian Dynamics Viable alternative, until 2006… –Need to look more into the phenomenon of gravitational lensing on larger scales

Probing Dark Matter with Distant Quasars: Gravitational Lensing Light from a quasar behind a galaxy cluster is bent by the mass in the cluster. Use to probe the distribution of matter in the cluster. Light from a distant quasar is bent around a foreground galaxy  two images of the same quasar!

Gravitational Lensing of Quasars

Gravitational Lensing The huge mass of gas in a cluster of galaxies can bend the light from a more distant galaxy. Image of the galaxy is strongly distorted into arcs.

Hot Gas in Clusters of Galaxies Coma Cluster of Galaxies (From Horizons by Seeds) Visible light X rays Space between galaxies is not empty, but filled with hot gas (observable in X rays) That this gas remains gravitationally bound, provides further evidence for dark matter.

The Bullet Cluster Given what we know about gravitational lensing (tracing the total mass in blue), hot X-ray gas in (the dominant baryonic mass, red), we can show that dark matter exists in at least one system: Images from Clowe et al and the Chandra press release

The Bullet Cluster Lensing of background galaxies seen in the optical images lets the mass distribution be mapped. The X-rays trace the hot gas, the dominant source of baryons in this cluster merger. They don’t line up! Why? Dark Matter seems to not interact with itself the way diffuse gas does during a cluster collision.

The Bullet Cluster

Summary That Zwicky Bastard was right! Dark Matter does indeed seem to be real, thank you Bullet Cluster. The majority of matter, dark or otherwise, is “non-baryonic” exotic stuff, and we don’t know for sure what it is. It’s likely flying through this room right this instant in huge amounts. WIMPs, not MaCHOs.