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Gamma-ray spectroscopy of Positron Annihilation in the Milky Way

The annihilation of positrons in the Galaxy's interstellar medium produces characteristic gamma-rays with a line at 511 keV. This emission has been observed with the spectrometer SPI on INTEGRAL, confirming a puzzling morphology with bright emission from an extended bulge-like region, and faint disk emission. Most plausible sources of positrons are believed to be distributed throughout the disk of the Galaxy. We aim to constrain characteristic spectral shapes for different spatial components in the disk and bulge with the high-resolution gamma-ray spectrometer SPI, based on a new instrumental background method and detailed multi-component sky model fitting. We confirm the detection of the main extended components of characteristic annihilation gamma-ray signatures at 58$σ$ significance in the line. The total Galactic line intensity amounts to $(2.7\pm0.3)\times10^{-3}~\mathrm{ph~cm^{-2}~s^{-1}}$ for our assumed spatial model. We derive spectra for the bulge and disk, and a central point-like and at the position of Sgr A*, and discuss spectral differences. The bulge shows a 511 keV line intensity of $(0.96\pm0.07)\times10^{-3}~\mathrm{ph~cm^{-2}~s^{-1}}$ and an ortho-positronium continuum equivalent to a positronium fraction of ($1.08\pm0.03$). The 2D-Gaussian representing the disk has an extent of $60^{+10}_{-5}$ deg in longitude and a latitudinal extent of $10.5^{+2.5}_{-1.5}$ deg; the line intensity is $(1.7\pm0.4)\times10^{-3}~\mathrm{ph~cm^{-2}~s^{-1}}$ with a marginal detection of ortho-positronium and an overall diffuse Galactic continuum of $(5.85\pm1.05)\times10^{-5}~\mathrm{ph~cm^{-2}~s^{-1}~keV^{-1}}$ at 511 keV. The disk shows no flux asymmetry between positive and negative longitudes, although spectral details differ. The flux ratio between bulge and disk is ($0.6\pm0.1$). The central source has an intensity of $(0.8\pm0.2)\times10^{-4}~\mathrm{ph~cm^{-2}~s^{-1}}$.