# Observations of M31 and M33 with the Fermi Large Area Telescope: a galactic center excess in Andromeda?

## TL;DR

This study analyzes gamma-ray emissions from M31 and M33 using over 7 years of Fermi LAT data, revealing a potential galactic center excess in M31 that may be linked to dark matter or millisecond pulsars.

## Contribution

It provides detailed morphological and spectral analyses of M31 and M33, with the first detection of an extended gamma-ray source in M31 and constraints on M33's emission.

## Key findings

- M31 is detected with nearly 10 sigma significance and is extended with 4 sigma.
- M33 remains undetected, with an updated upper limit consistent with star-formation correlations.
- Gamma-ray emission in M31 is confined to the inner regions and not correlated with star-forming areas.

## Abstract

The Fermi LAT has opened the way for comparative studies of cosmic rays (CRs) and high-energy objects in the Milky Way (MW) and in other, external, star-forming galaxies. Using 2 yr of observations with the Fermi LAT, local Group galaxy M31 was detected as a marginally extended gamma-ray source, while only an upper limit (UL) has been derived for the other nearby galaxy M33. We revisited the gamma-ray emission in the direction of M31 and M33 using more than 7 yr of LAT Pass 8 data in the energy range 0.1-100 GeV, presenting detailed morphological and spectral analyses. M33 remains undetected and we computed an UL for it. This revised UL remains consistent with the observed correlation between gamma-ray luminosity and star-formation rate tracers and implies an average CR density in M33 that is at most half of that of the MW. M31 is detected with a significance of nearly 10 sigma and to be extended with 4 sigma. Its spectrum is consistent with a power law. The spatial distribution of the emission is consistent with a uniform disk with a radius of 0.4 deg and no offset from the center of M31, but nonuniform intensity distributions cannot be excluded. The flux from M31 appears confined to the inner regions of the galaxy and does not fill the disk or extend far from it. The gamma-ray signal is not correlated with regions rich in gas or star-formation activity suggesting that the emission is not interstellar in origin, unless the energetic particles radiating in gamma rays do not originate in recent star formation. Alternative and nonexclusive interpretations are that the emission results from a population of millisecond pulsars dispersed in the bulge and disk of M31 by disrupted globular clusters or from the decay or annihilation of dark matter particles, similar to what has been proposed to account for the so-called Galactic Center excess found in Fermi-LAT observations of the MW.