Physicists and astronomers have studied gamma rays caused by the Sagittarius Dwarf, a small neighboring galaxy of our Milky Way. They showed that all the observed gamma radiation can be explained by millisecond pulsars, and can therefore not be interpreted as a smoking gun signature for the presence of dark matter.
A team of researchers, including UvA physicists and astronomers, has studied gamma rays caused by the Sagittarius Dwarf, a small neighbouring galaxy of our Milky Way. They showed that all the observed gamma radiation can be explained by millisecond pulsars, and can therefore not be interpreted as a smoking gun signature for the presence of dark matter. The results were published in Nature Astronomy this week.
The center of our galaxy is blowing a pair of colossal bubbles of gamma radiation (the magenta structures in the image above) that span a whopping 50,000 light-years across. Discovered with the Fermi Gamma-ray Space Telescope about a decade ago, the source of this hourglass-shaped phenomenon remains unclear.
Millisecond pulsars are the remnants of certain types of stars, significantly more massive than the Sun, that are in close binary systems, and now blast out cosmic particles as a result of their extreme rotational energies.
These Fermi bubbles are patched with a few enigmatic substructures of very bright gamma-ray emission. One of the brightest spots, the so-called Fermi cocoon, is found in the southern lobe and was originally thought to be due to past outbursts from the Galaxy’s supermassive black hole.
A team including Oscar Macias at the University of Amsterdam & Kavli IPMU and Roland Crocker at the Australian National University analyzed data from the GAIA and Fermi space telescopes to reveal that the Fermi cocoon is actually due to emission from the Sagittarius dwarf galaxy.
This satellite galaxy of the Milky Way is seen through the Fermi bubbles from our position on Earth. Due to its tight orbit around our galaxy and previous passages through the galactic disk, it has lost most of its interstellar gas and many of its stars have been ripped from its core into elongated streams.
Given that the Sagittarius dwarf is completely quiescent – it has no gas, and no stellar nurseries – there are only a few possibilities for its gamma-ray emission, including
(1) a population of unknown millisecond pulsars or
(2) dark matter annihilations.
Millisecond pulsars are the remnants of certain types of stars, significantly more massive than the Sun, that are in close binary systems, and now blast out cosmic particles as a result of their extreme rotational energies. The electrons fired by millisecond pulsars collide with low-energy photons of the Cosmic Microwave Background, propelling them to become high-energy gamma radiation.
Crocker, Macias, and collaborators have convincingly demonstrated that the gamma-ray cocoon is explained by millisecond pulsars in the Sagittarius dwarf, and that the dark matter hypothesis is strongly disfavoured. This discovery sheds light on millisecond pulsars as efficient accelerators of highly energetic electrons and positrons. It also suggests that similar physical processes could be ongoing in other dwarf satellite galaxies of the Milky Way. This is highly significant because dark matter researchers have long believed that an observation of gamma rays from a dwarf satellite would be a smoking gun signature for dark matter annihilation.
This study compels a reassessment of the high energy emission capabilities of quiescent stellar objects, such as dwarf spheroidal galaxies, and their role as prime targets for dark matter annihilation searches.
