Dark matter: summary Gravity and detecting Dark Matter Massive objects, even if they emit no light, exert gravitational forces on other massive objects. m 1 r 12 m 2 We study the motions (dynamics) of visible objects like stars in galaxies, and look for effects that are not explicable by the mass of the other light emitting or absorbing objects around them. http://www.hep.shef.ac.uk/cartwright/phy111/ppt/dark_matter_intro.ppt 1
Doppler effect: measure velocities from shift of spectral lines Dark matter Fritz Zwicky California Institute of Technology Coma Cluster: 1000 galaxies 321 million light years away He measured the speed with which the galaxies in Coma move. To his surprise, he found enormous speeds thousands of kilometers per second fast enough to rip the cluster apart. Why was the cluster not tearing itself up? Zwicky concluded that the cluster must be filled with additional unseen matter that holds the galaxies together with its gravitational force. 2
Fritz Zwicky measurements Were redone with much better instruments. Measure the velocities of galaxies in a cluster from their Doppler shifts. The mass we find from galaxy motions in a cluster is about 50 times larger than the mass in stars! Further evidence for dark matter Rotation curves Measure velocities of stars and gas clouds orbiting the galaxy center. One would expect that outer stars should behave much like the planets of our solar system. Inner planets rotate faster and outer planets rotate slower (Keplerian motion). In galaxies, however, both inner and outer stars rotate at about the same speed. http://www.haystack.mit.edu/edu/pcr/astrochemistry/3 - MATTER/Dark Matter.ppt 3
1973: Further evidence for dark matter Problem with galactic simulations James Peebles Jeremiah Ostriker Princeton University Jeremiah Ostriker and James Peebles used numerical simulation to study how galaxies evolve: they programmed 300 mass points into their computer to represent groups of stars in a galaxy rotating about a central point. Ostriker and Peebles found that in a time less than an orbital period, most of the mass points would collapse to a bar-shaped, dense concentration close to the center of the galaxy with only a few mass points at larger radii. However, if they added a static, uniform distribution of mass three to 10 times the size of the total mass of the mass points, they found a more recognizable structure would emerge. https://www.learner.org/courses/physics/unit/text.html?unit=10&secnum=2 Gravitational Lensing of Light Bending of light in gravitational fields can make lenses out of massive objects NO LENS LENS SOURCE LENSING OBJECT US Strong or close lens, expect a ring of light, or a ring of images in the presence of the lens. When not resolved, expect increased intensity. http://www.hep.shef.ac.uk/cartwright/phy111/ppt/dark_matter_intro.ppt 4
Gravitational lensing by dark matter Sometimes galaxies are lensed by other galaxies. Other times they were lensed by invisible objects dark matter. By measuring the distortion of the galaxies, scientists were able to weigh the dark matter. They found that it accounts for 90% of the mass of the universe. Cosmic shear: the light from distant galaxies is distorted by dark matter. https://www.nsf.gov/od/lpa/news/press/00/pr0029.htm 2006: Bullet cluster The hot gas in each cluster was slowed by a drag force, similar to air resistance, during the collision. In contrast, the dark matter was not slowed by the impact because it does not interact directly with itself or the gas except through gravity. Therefore, during the collision the dark matter clumps from the two clusters moved ahead of the hot gas, producing the separation of the dark and normal matter seen in the image. If hot gas was the most massive component in the clusters, as proposed by alternative theories of gravity, such an effect would not be seen. Instead, this result shows that dark matter is required. Credit: X-ray: NASA/CXC/CfA/M.Markevitch et al.; Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe et al.; Lensing Map: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al. http://chandra.harvard.edu/press/06_releases/press_082106.html 5
The visible portion of a galaxy lies deep in the heart of a large halo of dark matter. http://www.sjsu.edu/people/monika.kress/courses/sci255/ 6
85% of matter in the universe is of unknown nature Normal matter: ~15% of total matter? Dark matter ~85% of total matter Dark Matter: An undetected form of mass that emits little or no photons, but we know it must exist because we observe the effects of its gravity. We know it is out there but we do not know what it is. What dark matter is not: MACHOS hypothesis have been ruled out MACHOS: MAssive Compact Halo Objects: dim stars (white dwarfs, drown dwarfs, neutron stars), black holes, and Jupiter-sized planets, http://www.jcschroder.com/phy111/machos.htm 7
What do we know about dark matter? Mostly have negative information from astrophysics and searches for new particles: No electric charge No colour charge (property of quarks and gluons that is related to the particles' strong interactions) No strong self-interaction Does not seem to decay: stable, or very long-lived Not a particle in the Standard Model of particle physics Dark matter candidate particle zoo proton mass WIMP: Weakly Interacting Massive Particle SuperWIMPS: superweakly-interacting massive particles produced in the late decays of other particles Axion, Peccei Quinn symmetry Kaluza-Klein (KK) photon and graviton are from universal extra dimension models Neutralino and gravitino are particles of supersymmetric models WIMPZILLA (nonthermal dark matter) https://indico.in2p3.fr/event/10162/session/5/contribution/10/material/slides/0.pdf 8
How to search for dark matter particles Search for things dark matter can decay to Build a trap for dark matter Make dark matter particles http://www.ippp.dur.ac.uk/~ross/invisibles13/talks/78-marrod_xe1n_undagoita/slides/78-0-marrodan_invis_durham2013.pdf Supersymmetry and WIMPs: The lightest (stable) supersymmetries particle is your dark matter WIMP: neutralino (combination of inos) 9
The Large Hadron Collider (LHC) CERN (Conseil Européen pour la Recherche Nucléaire) LHC: 27-kilometre ring of superconducting magnets with a number of accelerating structures to boost the energy of the particles along the way. The world's largest and most powerful particle collider: 13 TeV (10 12 ev). The largest, most complex experimental facility ever built. The largest single machine in the world. Cost: 3 billion euro. Credit: CERN Slide from: T. Kono (ATLAS), BW2011 workshop 10
How to search for dark matter particles Search for things dark matter can decay to Build a trap for dark matter Make dark matter particles http://www.ippp.dur.ac.uk/~ross/invisibles13/talks/78-marrod_xe1n_undagoita/slides/78-0-marrodan_invis_durham2013.pdf Direct detection: How to detects WIMPs? http://cdms.berkeley.edu/education/dmpages/essays/essays/essays/science/images/nucrecoilatoms.jpg 11
Earth is moving through dark matter halo ( dark matter not moving) MAX signal ~ June 2 Dark matter signal should vary during the year Earth s orbital speed around the Sun is 30 km/s Smallest signal http://www.hep.ucl.ac.uk/darkmatter/ Detection principle: Measure the recoil energy imparted to detector nuclei through WIMP-nucleon collisions. Scientific American 288, 50-59 (March 2003) 12
2/25/2016 https://indico.in2p3.fr/event/10162/session/5/contribution/10/material/slides/0.pdf 13