J. Goodman – May 2003 Quarknet Symposium May 2003 Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.

Slides:



Advertisements
Similar presentations
EXTREME ENERGY COSMIC RAYS AND THE UNIVERSE General scope: a new universe Cosmic rays: facts and puzzles.
Advertisements

Ch1 0 The Big Bang Where do we come from, where are we going?
Chapter 26: Cosmology Why is the sky dark? The expanding universe Beginning of the universe: The Big Bang Cosmic microwave background The early universe.
Dark Matter, Dark Energy, and the Fate of the Universe.
Dark Energy. Conclusions from Hubble’s Law The universe is expanding Space itself is expanding Galaxies are held together by gravity on “small” distance.
Chapter 20 Dark Matter, Dark Energy, and the Fate of the Universe.
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.
Cosmology Past, present and future of the universe Is space flat or curved? Where is the center? What lies beyond our limit of vision? What is the universe.
15 The Big Bang Where do we come from, where are we going?
What is the Ultimate Fate of the Universe? Nick Kaiser.
© 2010 Pearson Education, Inc. Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe.
The New Cosmology flat, critical density, accelerating universe early period of rapid expansion (inflation) density inhomogeneities produced from quantum.
18 The Big Bang Where do we come from, where are we going?
Galaxy Evolution 1) Density fluctuations in the primordial matter 2) galaxies grew by repeated merging of smaller objects - evidence: galaxies at large.
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.
1 Announcements Cosmos Assignment 5, due Monday 4/26, Angel Quiz Monday, April 26 Quiz 3 & Review, chapters Wednesday, April 28, Midterm 3: chapters.
ASTR100 (Spring 2008) Introduction to Astronomy The Case for Dark Matter Prof. D.C. Richardson Sections
Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 26 Cosmology Cosmology.
Universe: Space-time, Matter, Energy Very little matter-energy is observable Critical matter-energy density balances expansion and gravitational collapse.
Cosmology: The Study of the Universe as a Whole Physics 360 Geol 360 Astronomy John Swez.
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.
Announcements The final exam will be at Noon on Monday, December 13 in Van Allen Hall LR1. The final exam will be cumulative. The final will be 40 questions,
Standard Cosmology.
Astronomy Topic 4 Revision Booster. Milky way facts 200 billion stars 250 million years to orbit One of a group of about 30 galaxies (The local group)
COSMOLOGY SL - summary. STRUCTURES Structure  Solar system  Galaxy  Local group  Cluster  Super-cluster Cosmological principle  Homogeneity – no.
Our Evolving Universe1 Vital Statistics of the Universe Today… l l Observational evidence for the Big Bang l l Vital statistics of the Universe   Hubble’s.
Chapter 16 Dark Matter, Dark Energy, and the Fate of the Universe.
Cosmology, Cosmology I & II Fall Cosmology, Cosmology I & II  Cosmology I:  Cosmology II: 
The Fate of the Universe
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.
Dark Energy Expanding Universe Accelerating Universe Dark Energy Scott Dodelson March 7, 2004.
Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe.
Universe Scale We can’t measure size of universe (especially if infinite), so compare distances at different times in history: Distances between non-moving.
J. Goodman – May 2003 Ghosts in the Universe Jordan A. Goodman University of Maryland Fall 2003 The world we don’t see around us.
What is the Universe Made of? The Case for Dark Energy and Dark Matter Cliff Burgess.
Ghosts in the Universe Jordan A. Goodman Department of Physics University of Maryland The world we don’t see around us.
J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.
The Universe Characteristics –Expanding (Hubble’s Law) –Finite age –Cool now, hotter long ago –Composition 70% H, 28% He, 2% the rest – Why? –Most matter.
Astro-2: History of the Universe Lecture 10; May
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.
J. Goodman – May 2003 Quarknet Symposium May 2003 Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.
J. Goodman – May 2010 Physics Olympics Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe.
J. Goodman Richtmyer Lecture – Jan Richtmyer Lecture Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman.
To do: Run through the ppt on Big Bang and Cosmology (resources.faulkes-telescope.com > GCSE Astronomy > Class Exercises > Cosmology Complete the following.
DCMST May 22 nd, 2007 Dark matter and dark energy Gavin Lawes Wayne State University.
Announcements Final exam is Monday, May 9, at 7:30 am. –Students with last names A-K go to 225 CB. –Students with last names L-Z go to 300 CB. –All students.
The cosmic connection There is a very close connection between particle physics and astrophysics. I’m going to show two examples: Type II supernovas Dark.
Universe Tenth Edition Chapter 25 Cosmology: The Origin and Evolution of the Universe Roger Freedman Robert Geller William Kaufmann III.
Lecture 27: The Shape of Space Astronomy Spring 2014.
The Beginning of Time Review: evidence for dark matter evidence for dark matter comes from  motions of stars and gas in galaxies  motions of galaxies.
WMAP The Wilkinson Microwave Anisotropy Probe Universe.
The Fate of the Universe. The fate depends on the rate of expansion and the density Density greater than critical value – gravity will halt expansion.
Milky Way Galaxy. Galaxy A group of stars, dust and gases held together by gravity. 170 billion galaxies in the universe 200 billion stars in a galaxy.
Cosmology That part of astronomy which deals with the nature of the universe as a whole.
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.
Cosmology Scale factor Cosmology à la Newton Cosmology à la Einstein
J. Goodman – Jan 2005 Smithsonian Institution Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.
Dark Matter, Dark Energy
© 2010 Pearson Education, Inc. Chapter 14 Dark Matter and Dark Energy.
J. Goodman – Spring 2002 Colloquium – UCR Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.
The Dark Universe Susan Cartwright.
The Big Bang The Big Bang
WHAT KIND OF UNIVERSE DO YOU LIVE IN?
Cosmology What is Cosmology? Stellar Systems
Dark matter and dark energy
Dark Matter, Dark Energy, and the Fate of the Universe
Cosmology: The Origin and Evolution of the Universe
The Big Bang The Big Bang
Cosmology What is Cosmology? Study of the universe as a whole
Presentation transcript:

J. Goodman – May 2003 Quarknet Symposium May 2003 Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University of Maryland

J. Goodman – May 2003 Outline Why do we care about neutrinos? Why do we think there is dark matter? Could some of it be neutrinos? The search for neutrino mass – Solar Neutrinos –Super-K –SNO –Kamland The accelerating Universe - Dark Energy –SCP –WMAP

J. Goodman – May 2003 Seeing Big Picture

J. Goodman – May 2003 Why do we think there is dark matter? Isn’t obvious that most of the matter in the Universe is in Stars? Spiral Galaxy

J. Goodman – May 2003 Why do we think there is dark matter? In a gravitationally bound system out past most of the mass V ~ 1/r 1/2 We can look at the rotation curves of other galaxies –They should drop off But they don’t!

J. Goodman – May 2003 Why do we think there is dark matter? There must be a large amount of unseen matter in the halo of galaxies –Maybe 20 times more than in the stars! –Our galaxy looks 30 kpc across but recent data shows that it looks like it’s 200 kpc across

J. Goodman – May 2003 Measuring the energy in the Universe We can measure the mass of clusters of galaxies with gravitational lensing These measurements give  mass ~0.3 We also know (from the primordial deuterium abundance) that only a small fraction is nucleons  nucleons < ~0.04 Gravitational lensing

J. Goodman – May 2003 What is this ghostly matter? Could it be neutrinos? How much neutrino mass would it take? –Proton mass is 938 MeV –Electron mass is 511 KeV –Neutrino mass of 2eV would solve the galaxy rotation problem – 20eV would close the Universe Theories say it can’t be all neutrinos –They have difficulty forming the kinds of structure observed. The structures they create are too large and form too late in the history of the universe

J. Goodman – May 2003 Super-Kamiokande

J. Goodman – May 2003 Super-Kamiokande

J. Goodman – May 2003 Cherenkov Radiation Boat moves through water faster than wave speed. Bow wave (wake)

J. Goodman – May 2003 Cherenkov Radiation Faster than wave speed Slower than wave speed

J. Goodman – May 2003 Cherenkov Radiation Aircraft moves through air faster than speed of sound. Sonic boom

J. Goodman – May 2003 Cherenkov Radiation When a charged particle moves through transparent media faster than speed of light in that media. Cherenkov radiation Cone of light

J. Goodman – May 2003 Cherenkov Radiation

J. Goodman – May 2003 Hubble Law

J. Goodman – May 2003 The expanding Universe The Universe is expanding Everything is moving away from everything Hubble’s law says the faster things are moving away the further they are away

J. Goodman – May 2003 The expanding Universe

J. Goodman – May 2003 Supernova Cosmology Project Set out to directly measure the deceleration of the Universe Measure distance vs brightness of a standard candle (type Ia Supernova) The Universe seems to be accelerating! Doesn’t fit Hubble Law (at 99% c.l.)

J. Goodman – May 2003 The expanding Universe

J. Goodman – May 2003 Energy Density in the Universe    may be made up of 2 parts a mass term and a “dark energy”  term (Cosmological Constant)    mass  energy Einstein invented  to keep the Universe static He later rejected it when he found out about Hubble expansion He called it his “biggest blunder”  m   

J. Goodman – May 2003 The Cosmological Constant

J. Goodman – May 2003 What is the “Shape” of Space? Closed Universe   >1 – C < 2  R Open Universe   <1 –Circumference (C) of a circle of radius R is C > 2  R Flat Universe   =1 – C = 2  R – Euclidean space

J. Goodman – May 2003 Results of SN Cosmology Project The Universe is accelerating The data require a positive value of  “Cosmological Constant” If    =1 then they find    ~ 0.7 ± 0.1

J. Goodman – May 2003 Accelerating Universe

J. Goodman – May 2003 Accelerating Universe

J. Goodman – May 2003 Measuring the energy in the Universe Studying the Cosmic Microwave radiation looks back at the radiation from 400,000 years after the “Big Bang”. This gives a measure of  0

J. Goodman – May 2003 Recent Results  0 =1  nucleon

J. Goodman – May 2003 WMAP -2003

J. Goodman – May 2003 WMAP

J. Goodman – May 2003 WMAP Results Universe is 13.7 billion years old with a margin of error of close to 1% Content of the Universe: 4% Atoms, 23% Cold Dark Matter, 73% Dark energy. Fast moving neutrinos do not play any major role in the evolution of structure in the universe. Expansion rate (Hubble constant) value: H o = 71 km/sec/Mpc (with a margin of error of about 5%) New evidence for Inflation (in polarized signal)

J. Goodman – May 2003 What does all the data say? Three pieces of data come together in one region    ~ 0.73  m ~ 0.27 (uncertainty  ~0.04) Universe is expanding & won’t collapse Only ~1/6 of the dark matter is ordinary matter (atoms) A previously unknown and unseen “dark energy” pervades all of space and is causing it to expand and accelerate

J. Goodman – May 2003 What do we know about “Dark Energy” It emits no light It acts like a large negative pressure P x ~ -  x It is approximately homogenous –At least it doesn’t cluster like matter Calculations of this pressure from first principles fail miserably – assuming it’s vacuum energy you predict a value of   ~ Bottom line – we know very little!

J. Goodman – May 2003 Conclusion  tota l = 1.02 ± 0.02 –The Universe is flat! The Universe is : ~1/2% Stars ~1/2% Neutrinos ~27% Dark Matter (only 4% is ordinary matter) ~73% Dark Energy We can see ~1/2% We can measure ~1/2% We can see the effect of ~27% (but don’t know what most of it is) And we are pretty much clueless about the other 3/4 of the Universe There is still a lot of Physics to learn!