For almost 10 years, astronomers have been studying a mysterious diffuse radiation coming from the centre of our galaxy. Originally, it was thought that this radiation could originate from the elusive dark matter particles that many researchers are hoping to find. However, physicists from the University of Amsterdam and the Laboratoire d”Annecy-le-Vieux de Physique Théorique have now found further evidence that rapidly spinning neutron stars are a much more likely source for this radiation. Their findings are published today in Nature Astronomy.
Observations of gamma-ray radiation from the galactic centre region with the Fermi Large Area Telescope have revealed a mysterious diffuse and extended emission. Discovered almost 10 years ago, this emission generated a lot of excitement in the particle physics community, since it had all the characteristics of a long-sought signal from the self-annihilation of dark matter particles in the inner galaxy. Finding such a signal would confirm that dark matter, which has so far has only been observed through its gravitational effects on other objects, is made out of new fundamental particles. Moreover, it would help to determine the mass and other properties of these elusive dark matter particles. However, a recent study shows that arguably the best astrophysical interpretation of the excess emission is a new population in the galactic bulge of thousands of rapidly spinning neutron stars called millisecond pulsars, which have escaped observation at other frequencies up to now.
Where there are stars, there is radiation
“Understanding in detail the morphology [the location and shape] and spectrum [the combined frequencies] of the excess emission is of vital importance for discriminating between the dark matter and astrophysical interpretations of the galactic centre excess radiation,” says Christoph Weniger, one of the researchers that conducted the study. A new study by researchers at the University of Amsterdam and the Laboratoire d”Annecy-le-Vieux de Physique Théorique, a research unit of the French Centre National de la Recherche Scientifique, found strong evidence that the emission actually seems to come from regions where there is also a large amount of stellar mass in the galactic bulge (the ‘boxy bulge’) and centre (the ‘nuclear bulge’). Furthermore, the researchers found that the light-to-mass ratio in the galactic bulge and centre are mutually consistent, so that the gamma ray GeV emission is a surprisingly accurate tracer of stellar mass in the inner galaxy (figure 2). This study was based on a new analysis tool, Sky Factorization with Adaptive Constrained Templates (SkyFACT), developed by the researchers themselves, which combines physical modeling with image analysis.
The findings support the millisecond pulsar interpretation of the excess emission, since neither a dark matter signal nor other astrophysical interpretations are expected to show such a correlation. “The results will help guide upcoming radio searches for this hidden population of millisecond pulsars in the galactic bulge with MeerKAT and the future Square Kilometre Array,” said Francesca Calore, another of the paper’s authors. “This makes these upcoming searches even more promising.”
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Delta Institute for Theoretical Physics
R. Bartels, E. Storm, C. Weniger and F. Calore. The Fermi-LAT GeV excess traces stellar mass in the Galactic bulge. Nature Astronomy (2018). DOI: doi.org/10.1038/s41550-018-0531-z
Figure 1: Observed gamma ray emission from the Galactic disk, with the bulge region indicated. The insets show the expected profiles of excess radiation coming from dark matter and stars respectively. The researchers were able to show that the stars profile matches the measurements much better than the dark matter profile
Credit: Christoph Weniger, University of Amsterdam/FermiLAT