Search for Electron-Positron Annihilation Radiation from the Jet in 3C 120

Details Search for Electron-Positron Annihilation Radiation from the Jet in 3C 120 Search for Electron-Positron Annihilation Radiation from the Jet in 3C 120

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...665..232m&link_type=abstract

The Astrophysical Journal, Volume 665, Issue 1, pp. 232-236.

Astronomy and Astrophysics

Astronomy

14

Galaxies: Active, Galaxies: Individual: Alphanumeric: 3C 120, Galaxies: Jets, Gamma Rays: Observations, Radio Continuum: Galaxies

Scientific paper

We report an attempt to detect the electron-positron annihilation line from the radio galaxy 3C 120, in which the jet interacts strongly with interstellar clouds. Such interactions should cause most of the jet plasma to mix with the gas in the clouds. This will thermalize the majority of any positrons in the jet, leading to continuous annihilation with ambient electrons. We derive the number density of the combined electron-positron population in the core and compact knots in the jet of 3C 120 using ultrahigh-resolution observations with the Global millimeter-VLBI Array at 86 GHz and the Very Long Baseline Array at 43 GHz, along with the millimeter-wave continuum spectrum and a computational code that maps the synchrotron intensity of a model jet. If the jet contains a pure pair plasma, the production rate of positrons required to produce this density plus the efficiency of eventual annihilation predict the emission of a narrow spectral line at a rest energy of 511 keV, or 495 keV in the observer's frame. Our spectral observations with the SPI instrument on INTEGRAL failed to detect the line. The upper limit, which is 30% lower than our rather uncertain prediction, does not significantly constrain the positron-to-proton ratio in the jet of 3C 120. However, our procedure provides a robust method for determining the flux of electrons and positrons in a jet that will be useful when more sensitive soft γ-ray spectrometers and millimeter-wave VLBI arrays become available.

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