Luminosity functions consistent with a pulsar-dominated Galactic Center Excess

TL;DR

This study evaluates luminosity functions of millisecond pulsars as an explanation for the Galactic Center gamma-ray excess, comparing predictions with observational data and exploring the potential of future detection methods.

Contribution

It provides a systematic analysis of luminosity functions for pulsars, linking them to observational constraints and forecasting the impact of improved detection techniques.

Findings

Existing models are consistent with current data within certain parameter regions.

Approximately 10,000 to 100,000 pulsars could explain the gamma-ray excess.

Enhanced analysis methods could resolve over 30% of the excess flux.

Abstract

A new population of millisecond pulsars is a long-standing proposed explanation for the excess of GeV-scale gamma rays emanating from the region surrounding the center of the Milky Way (the "Galactic Center excess"). We examine several simple parameterizations of possible luminosity functions for this population, as well as several benchmark luminosity functions proposed in the literature, and compare the predicted populations of resolved point sources to the Fermi 4FGL-DR2 point source catalog and a sub-population recently identified using wavelet-based methods. We provide general results that can be used to translate upper limits on the number of resolved point sources associated with the excess, and the fraction of the flux in the excess that can be attributed to resolved sources, into limits on the luminosity function parameter space. We discuss a number of important systematic uncertainties, including in the detection threshold model and the total flux attributed to the excess. We delineate regions of parameter space (containing existing benchmark models) where there is no apparent tension with current data, and the number of total pulsars needed to explain the excess is in the range of O(10,000-100,000). Forecasting the effects of lowered point source detection thresholds, we show that novel analysis methods that probe sub-threshold point source populations can hope to resolve more than 30% of the flux of the excess.