title: Testing the Axion-Conversion Hypothesis of 3.5 keV Emission with Polarization.
abstract: The recently measured 3.5 keV line in a number of galaxy clusters, the Andromeda galaxy (M31), and the Milky Way (MW) center can be well accounted for by a scenario in which dark matter decays to axionlike particles (ALPs) and subsequently convert to 3.5 keV photons in magnetic fields of galaxy clusters or galaxies. We propose to test this hypothesis by performing x-ray polarization measurements. Since ALPs can only couple to photons with a polarization orientation parallel to the magnetic field, we can confirm or reject this model by measuring the polarization of the 3.5 keV line and compare it to the orientation of the magnetic field. We discuss luminosity and polarization measurements for both a galaxy cluster and spiral galaxy, and provide a general relation between the polarization and galaxy inclination angle. This effect is marginally detectable with x-ray polarimetry detectors currently under development, such as the enhanced X-ray Timing and Polarization satellite, the Imaging X-ray Polarimetry Explorer and the X-ray Imaging Polarimetry Explorer. The sensitivity can be further improved in the future with detectors of a larger effective area or better energy resolutions.
authors.affiliation: Key Laboratory of Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Beijing 100012, China.
authors.forename: Yan
authors.initials: Y
authors.lastname: Gong
authors.affiliation: Key Laboratory of Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Beijing 100012, China.|University of Chinese Academy of Sciences, Beijing 100049, China.|Center of High Energy Physics, Peking University, Beijing 100871, China.
authors.forename: Xuelei
authors.initials: X
authors.lastname: Chen
authors.affiliation: Department of Engineering Physics and Center for Astrophysics, Tsinghua University, Beijing 100084, China.
authors.forename: Hua
authors.initials: H
authors.lastname: Feng