Conveners
Morning 32
- Pierre Sikivie (University of Florida)
Mr
A Colijn
(Nikhef)
05/06/2019, 11:05
Oral
The Universe became transparent to neutrino’s approximately 1 second after the Big Bang. These neutrino’s are omnipresent with a density of around 300 cm$^{-3}$. However, they have never been observed since they have cooled down to a temperature of 1.9K, corresponding to an energy of just several 100 µeV. Within the PTOLEMY collaboration we are investigating techniques to observe these...
Ken'ichi Saikawa
(Max Planck Institute for Physics)
05/06/2019, 11:25
Oral
In light of recent developments of experimental approaches on the search for axion dark matter, it is important to clarify what is the typical theoretical prediction for its mass. The prediction for the axion dark matter mass can be obtained by estimating the relic axion abundance, which is given as a function of the Peccei-Quinn scale. However, the estimation of the axion abundance suffers...
Prof.
Matthias Schott
(Uni Mainz)
05/06/2019, 11:45
Oral
FASER, the ForwArd Search ExpeRiment, is a newly approved experiment at the LHC, dedicated to searching for light, extremely weakly-interacting particles during the LHC Run 3. Such particles may be produced in the LHC's high-energy collisions in large numbers in the far-forward region and then travel long distances through concrete and rock without interacting. They may then decay to visible...
Dr
Roberta Volpe
(UCLouvain (Belgium))
05/06/2019, 12:05
Oral
The features of the NA62 experiment at the CERN SPS – high-intensity setup, trigger-system flexibility, high-frequency tracking of beam particles, redundant particle identification, and
ultra-high-efficiency photon vetoes – make NA62 particularly suitable to search for long-lived, weakly-coupled particles within Beyond the Standard Model physics, using kaon and pion decays as well as...
Dr
Michael A. Fedderke
(Stanford University, University of California Berkeley, and LBNL)
05/06/2019, 12:25
Oral
In this talk, I will detail two ways to search for low-mass axion dark matter using cosmic microwave background (CMB) polarization measurements. These appear, in particular, to be some of the most promising ways to directly detect fuzzy dark matter. Axion dark matter causes rotation of the polarization of light passing through it. This gives rise to two novel phenomena in the CMB. First, the...
Dr
IPPEI OBATA
(ICRR, University of Tokyo)
05/06/2019, 12:45
Oral
Axion dark matter differentiates the phase velocities of the circular-polarized photons. In this work, we present a scheme to measure its phase difference by using a linear optical cavity. We applied this scheme to the Fabry-Perot arm of gravitational wave detectors such as aLIGO, CE, and DECIGO. We found that their potential sensitivities to the axion-photon coupling constant, g_{aγ}, can...
