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  • Mail Code: 4060

All Publications

  • Observing the dark sector with supernovae DeRocco, W., IOP IOP PUBLISHING LTD. 2020

    View details for DOI 10.1088/1742-6596/1468/1/012048

    View details for Web of Science ID 000539995300047

  • Constraining Primordial Black Hole Abundance with the Galactic 511 keV Line PHYSICAL REVIEW LETTERS DeRocco, W., Graham, P. W. 2019; 123 (25)

    View details for DOI 10.1103/PhysRevLett.123.251102

    View details for Web of Science ID 000502796900002

  • Supernova signals of light dark matter PHYSICAL REVIEW D DeRocco, W., Graham, P. W., Kasen, D., Marques-Tavares, G., Rajendran, S. 2019; 100 (7)

    View details for DOI 10.1103/PhysRevD.100.075018

    View details for Web of Science ID 000490474400001

  • Observable signatures of dark photons from supernovae JOURNAL OF HIGH ENERGY PHYSICS DeRocco, W., Graham, P. W., Kasen, D., Marques-Tavares, G., Rajendran, S. 2019

    View details for DOI 10.1007/JHEP02(2019)171

    View details for Web of Science ID 000460261800002

  • Constraining Primordial Black Hole Abundance with the Galactic 511 keV Line. Physical review letters DeRocco, W., Graham, P. W. 2019; 123 (25): 251102

    Abstract

    Models in which dark matter consists entirely of primordial black holes (PBHs) with masses around 10^{17}  g are currently unconstrained. However, if PBHs are a component of the Galactic dark matter density, they will inject a large flux of energetic particles into the Galaxy as they radiate. Positrons produced by these black holes will subsequently propagate throughout the Galaxy and annihilate, contributing to the Galactic 511 keV line. Using measurements of this line by the INTEGRAL satellite as a constraint on PBH positron injection, we place new limits on PBH abundance in the mass range 10^{16}-10^{17}  g, ruling out models in which these PBHs constitute the entirety of dark matter.

    View details for DOI 10.1103/PhysRevLett.123.251102

    View details for PubMedID 31922803

  • Axion interferometry PHYSICAL REVIEW D DeRocco, W., Hook, A. 2018; 98 (3)

    View details for DOI 10.1103/PhysRevD.98.035021

    View details for Web of Science ID 000441718100006