A hard spectrum diffuse γ-ray component associated with H II gas in the Galactic plane

¹ Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, PR China
e-mail: yangrz@ustc.edu.cn
² CAS Key Laboratory for Research in Galaxies and Cosmology, University of Science and Technology of China, Hefei, Anhui 230026, PR China
³ School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, PR China

Received: 26 October 2020
Accepted: 16 January 2022

Abstract

We analyzed 12-year Fermi Large Area Telescope γ-ray data in the inner Galaxy centered at (l = 30°, b = 0°) and (l = 330°, b = 0°). We found significant hardening of the spectrum of the diffuse γ-ray emission in these regions as previously reported. We further deduced that the diffuse γ rays can be divided into two components from the likelihood analysis. One component is associated with the total gas column density and reveals a soft spectrum, while the other is associated with the H II gas and presents a hard spectrum. Assuming the diffuse γ-ray emissions are mainly produced through the interaction between cosmic rays (CRs) and the ambient gas, these two components are produced by the CR populations with spectral indices of 2.8 (“soft”) and 2.3 (“hard”), respectively. We argue that the hard CR population may come from the vicinity of the CR accelerators. The soft CR population has a similar spectral shape and density as measured in the solar neighborhood, which implies a uniform CR “sea” with a similar density and spectral shape in the Galaxy.