PPT-Gravitational Wave Detection and Dark Matter Searches with Atom Interferometry

Tim Kovachy Department of Physics and Astronomy and Center for Fundamental Physics Northwestern University NPS Colloquium February 1 2019 Conceptual overview of atom interferometry Motivation for gravitational wave detection in the midband frequency range of 01 Hz to 10 Hz. Roberta Sparvoli. Rome . “. Tor Vergata. ”. . University. and . INFN, ITALY. PCC 2011 - CERN. SIGNALS . from. RELIC . WIMPs. Direct . searches. :. . elastic. . scattering. of a WIMP off detector . This . powerpoint. will show you the basics of dark matter and dark energy . Their place in the universe . By Jordan . Ilori. . DARK MATTER. Dark matter is a type of matter hypothesized in astronomy and cosmology to account for a large part of the mass that appears to be missing from the universe. Dark matter cannot be seen directly with telescopes; evidently it neither emits nor absorbs light or other electromagnetic radiation at any significant level. Instead, the existence and properties of dark matter are inferred from its gravitational effects on visible matter, radiation, and the large-scale structure of the universe. According to the Planck mission team, and based on the standard model of cosmology, the total mass–energy of the known universe contains 4.9% ordinary matter, 26.8% dark matter and 68.3% dark energy. Thus, dark matter is estimated to constitute 84.5% of the total matter in the universe and 26.8% of the total content of the universe.. limits on . dark . energy. Jun. 17. 2011. Geena Kim. P. Hamilton, D. Schlippe, and H. Mueller. University of California, Berkeley. Paul Hamilton. Müller group. University of California at Berkeley. . D.S. . Hajdukovic. GBAR Collaboration Meeting. 18. th. April 2012. Our best physics . The Standard Model of Particles and Fields. +. . General Relativity . is . considered. as insufficient to explain the observed phenomena in Astrophysics and Cosmology.. Clare Burrage. University of Nottingham. Clare.Burrage@nottingham.ac.uk. Outline:. Chameleon dark energy. A . review of atom interferometry. Dark energy in the laboratory. Solutions to the Cosmological Constant Problem. Paul McMillan. Surveys For All, 1st February 2016 . Why do we care?. On the biggest scales, the ΛCDM model works. Why do we care?. On the scale of individual galaxies, agreement is less obvious.. Things are more complicated, we have to consider the baryons. Overview of Why and How. Dan Burbank and Tony Young. AST5022. Introduction. Background. Physics. Sources. Detectors and Detector Implications. Questions. Gravitational Waves . Speed-of-light wave propagation solution of Einstein’s Field Equations. Lisa Randall. Harvard University. @. lirarandall. . What do we know about dark matter?. It has gravitational interactions—of matter!. Gravitational . lensing. Rotation curves in galaxies. Detailed measurements of energy abundances—total and normal matter. Dr. Simona . Murgia. (UC, Irvine). Dr. Will Dawson (Lawrence Livermore National Laboratory). Carolyn Slivinski (STScI). Facilitator: Dr. Emma Marcucci (STScI). Science Briefing. October . 5. , 2017. Dainis Dravins, . Hannes. Jensen . Lund Observatory, Sweden. Stephan LeBohec, Paul D.. . Nuñez. . The University of Utah, Salt Lake City. STELLAR INTENSITY INTERFEROMETRY. . Astrophysical targets for sub-. Very Long Baseline Interferometry. Very Long Baseline Interferometry. time.  . θ.  . t. Very Long Baseline Interferometry. Moving Sources.  .  .  .  .  .  . 0 .  .  .  .  .  .  . What is the signal made of?. Achuta . Kadambi. , Jamie . Schiel. and Ramesh . Raskar. , IEEE CVPR16 . An interferometric 3D camera for multipath imaging for meter scale scenes. Swept Frequency Electronic Interferometry. Take-home message:. Tim Kovachy. Department of Physics and Astronomy and Center for Fundamental Physics (CFP), Northwestern University. CPAD 2021. Brief overview of atom interferometry. Enabling technology advances for large-area/long-baseline atom interferometry demonstrated with 10-meter baselines. Jeffrey Kissel. LIGO Hanford Controls Engineer. LIGO Calibration Group Co-Chair. G1800393-v2. 1. Inspiration. G1800393-v2. 2. PRL. . 116.23 (2016): . 231102. 2G , 3G, Space, and PTAs. will have events with SNRs of O(~100).