Jonathan Roberts

New York, New York, United States Contact Info
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I oversee research, data science, and open market revenue for Dotdash Meredith…

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  • Dotdash Meredith

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Publications

  • Limit on the mass of a long-lived or stable gluino.

    Journal of High Energy Physics

    We reinterpret the generic CDF charged massive particle limit to obtain a limit
    on the mass of a stable or long-lived gluino. Various sources of uncertainty are examined.
    The R-hadron spectrum and scattering cross sections are modeled based on known lowenergy hadron physics and the resultant uncertainties are quantified and found to be small
    compared to uncertainties from the scale dependence of the NLO pQCD production cross
    sections. The largest uncertainty in the limit comes from…

    We reinterpret the generic CDF charged massive particle limit to obtain a limit
    on the mass of a stable or long-lived gluino. Various sources of uncertainty are examined.
    The R-hadron spectrum and scattering cross sections are modeled based on known lowenergy hadron physics and the resultant uncertainties are quantified and found to be small
    compared to uncertainties from the scale dependence of the NLO pQCD production cross
    sections. The largest uncertainty in the limit comes from the unknown squark mass: when
    the squark - gluino mass splitting is small, we obtain a gluino mass limit of 407 GeV, while
    in the limit of heavy squarks the gluino mass limit is 397 GeV. For arbitrary (degenerate)
    squark masses, we obtain a lower limit of 322 GeV on the gluino mass. These limits apply
    for any gluino lifetime longer than ~30 ns, and are the most stringent limits for such a
    long-lived or stable gluino.

    Other authors
    • G.R.Farrar
    • R. Mackeprang
    • D. Milstead
    See publication
  • Pamela Through a Magnetic Lens

    Journal of Cosmology and Astroparticle Physics

    The PAMELA satellite has observed an excess in the positron to electron ratio above theoretical predictions in the range 10-100 GeV that increases with energy. We propose that the excess is not due to a change in the local interstellar spectrum, but is due to heliospheric modulation. We motivate this from the known form of the heliospheric magnetic field and predict that the excess will disappear when we enter a period of solar maximum activity.

    See publication

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