Bulletin of the American Physical Society
47th Annual Meeting of the APS Division of Atomic, Molecular and Optical Physics
Volume 61, Number 8
Monday–Friday, May 23–27, 2016; Providence, Rhode Island
Session T3: Invited Session: Astrophysical DetectorsInvited
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Sponsoring Units: GPMFC Chair: David DeMille, Yale University Room: Ballroom D |
Friday, May 27, 2016 8:00AM - 8:30AM |
T3.00001: Searching for dark energy with matter wave interferometry Invited Speaker: Paul Hamilton The nature of dark energy, which makes up 70{\%} of the mass-energy of the universe, remains completely unknown. Chameleons are a simple scalar model for dark energy that mediate a force which is screened by bulk matter. However we can now probe these scalar fields using atoms as nearly ideal test masses in the vacuum of our cavity-based matter wave interferometer [1, 2]. Our first measurements ruled out a range of chameleons that would reproduce the observed cosmic acceleration [3]. Since then we have improved sensitivity by a factor of 100. With a similar future improvement, we will be sensitive to any possible chameleon field and other exotic models for dark energy and dark matter, such as symmetrons or f(R) gravity.\\[4 pt] \\[4 pt] [1] C. Burrage, E. Copeland, E Hinds, JCAP 03 (2015) 042 \\[4 pt] [2] P. Hamilton, M. Jaffe, J.M. Brown, L. Maisenbacher, B. Estey, H. M\"{u}ller, Phys. Rev. Lett. \textbf{114}, 100405 (2015) \\[4 pt] [3] P. Hamilton, M. Jaffe, P. Haslinger, Q. Simmons, H. M\"{u}ller, J. Khoury, Science \textbf{349}, 6250 (2015) [Preview Abstract] |
Friday, May 27, 2016 8:30AM - 9:00AM |
T3.00002: Gravitational wave detection using atom interferometry Invited Speaker: Jason Hogan The advent of gravitational wave astronomy promises to provide a new window into the universe. Low frequency gravitational waves below 10 Hz are expected to offer rich science opportunities both in astrophysics and cosmology, complementary to signals in LIGO's band. Detector designs based on atom interferometry have a number of advantages over traditional approaches in this band, including the possibility of substantially reduced antenna baseline length in space and high isolation from seismic noise for a terrestrial detector. In particular, atom interferometry based on the clock transition in group II atoms offers tantalizing new possibilities. Such a design is expected to be highly immune to laser frequency noise because the signal arises strictly from the light propagation time between two ensembles of atoms. This would allow for a gravitational wave detector with a single linear baseline, potentially offering advantages in cost and design flexibility. In support of these proposals, recent progress in long baseline atom interferometry in a 10-meter drop tower has enabled observation of matter wave interference with atomic wavepacket separations exceeding 50 cm and interferometer durations of more than 2 seconds. This approach can provide ground-based proof-of-concept demonstrations of many of the technical requirements of both terrestrial and satellite gravitational wave detectors. [Preview Abstract] |
Friday, May 27, 2016 9:00AM - 9:30AM |
T3.00003: Unraveling the mystery of Dark Matter Invited Speaker: Asimina Arvanitaki Dark Matter constitutes a significant component of the energy budget of our Universe and we have diagnosed its existence through its gravitational interaction with us. Our theories of Dark Matter though predict that this glue that is responsible for the existence of our Galaxy should also interact with us in non-trivial ways. After I review these ideas, I will discuss how we can learn more about the properties of Dark Matter in a variety of new experiments, ranging from atomic clocks to black holes and gravitational waves. [Preview Abstract] |
Friday, May 27, 2016 9:30AM - 10:00AM |
T3.00004: Manifestations of Dark matter and variation of the fundamental constants in atomic and astrophysical phenomena Invited Speaker: Victor Flambaum Low-mass boson dark matter particles produced after Big Bang form classical field and/or topological defects. In contrast to traditional dark matter searches, effects produced by interaction of an ordinary matter with this field and defects may be first power in the underlying interaction strength rather than the second or fourth power (which appears in a traditional search for the dark matter). This may give a huge advantage since the dark matter interaction constant is extremely small. Interaction between the density of the dark matter particles and ordinary matter produces both ‘slow’ cosmological evolution and oscillating variations of the fundamental constants including the fine structure constant alpha and particle masses [1]. Recent atomic dysprosium spectroscopy measurements and the primordial helium abundance data allowed us to improve on existing constraints on the quadratic interactions of the scalar dark matter with the photon, electron and light quarks by up to 15 orders of magnitude. Limits on the linear and quadratic interactions of the dark matter with W and Z bosons have been obtained for the first time. In addition to traditional methods to search for the variation of the fundamental constants (atomic clocks, quasar spectra, Big Bang Nucleosynthesis, etc) we discuss variations in phase shifts produced in laser/maser interferometers (such as giant LIGO, Virgo, GEO600 and TAMA300, and the table-top silicon cavity and sapphire interferometers) [2], changes in pulsar rotational frequencies (which may have been observed already in pulsar glitches), non-gravitational lensing of cosmic radiation and the time-delay of pulsar signals [3]. Other effects of dark matter and dark energy include apparent violation of the fundamental symmetries: oscillating or transient atomic electric dipole moments, precession of electron and nuclear spins about the direction of Earth’s motion through an axion condensate, and axion-mediated spin-gravity couplings [4-6], violation of Lorentz symmetry and Einstein equivalence principle [7,8]. Finally, we explore a possibility to explain the DAMA collaboration claim of dark matter detection by the dark matter scattering on electrons. We have shown that the electron relativistic effects increase the ionization differential cross section up to 3 orders of magnitude [9]. References: [1] Y. V. Stadnik and V. V. Flambaum. Phys. Rev. Lett. 115, 201301 (2015). [2] Y. V. Stadnik, V. V. Flambaum. Phys. Rev. Lett. 114, 161301 (2015). 1511.00447 [3] Y. V. Stadnik, V. V. Flambaum. Phys. Rev. Lett. 113, 151301 (2014). [4] Y. V. Stadnik, V. V. Flambaum. Phys. Rev. D 89, 043522 (2014). [5] B. M. Roberts, Y. V. Stadnik, V. A. Dzuba, V. V. Flambaum, N. Leefer, D. Budker. Phys. Rev. Lett. 113, 081601 (2014). [6] B. M. Roberts, Y. V. Stadnik, V. A. Dzuba, V. V. Flambaum, N. Leefer, D. Budker. Phys. Rev. D 90, 096005 (2014). [7] V.A. Dzuba, V.V. Flambaum, M. Safronova, S.G. Porsev, T. Pruttivarasin, M.A. Hohensee, H. Haffner. NaturePhysics(2016). V.V. Flambaum.1511.04848 [9] B. M. Roberts, V. V. Flambaum, G. F. Gribakin, Phys. Rev. Lett. 116, 023201 (2016). [Preview Abstract] |
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