Galactic population synthesis of radioactive nucleosynthesis ejecta

¹ Julius-Maximilians-Universität Würzburg, Fakultät für Physik und Astronomie, Institut für Theoretische Physik und Astrophysik, Lehrstuhl für Astronomie, Emil-Fischer-Str. 31, 97074 Würzburg, Germany
e-mail: thomas.siegert@uni-wuerzburg.de
² Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching b. München, Germany
³ Horn & Company Financial Services GmbH, Kaistraße 20, 40221 Düsseldorf, Germany
⁴ Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
⁵ Industrieanlagen-Betriebsgesellschaft mbH, Einsteinstr. 20, 85521 Ottobrunn, Germany

Received: 8 July 2022
Accepted: 23 January 2023

Abstract

Diffuse γ-ray line emission traces freshly produced radioisotopes in the interstellar gas, providing a unique perspective on the entire Galactic cycle of matter from nucleosynthesis in massive stars to their ejection and mixing in the interstellar medium (ISM). We aim to construct a model of nucleosynthesis ejecta on a galactic scale that is specifically tailored to complement the physically most important and empirically accessible features of γ-ray measurements in the MeV range, in particular for decay γ rays such as ²⁶Al, ⁶⁰Fe, or ⁴⁴Ti. Based on properties of massive star groups, we developed a Population SYnthesis COde (PSYCO), which can instantiate galaxy models quickly and based on many different parameter configurations, such as the star formation rate (SFR), density profiles, or stellar evolution models. As a result, we obtain model maps of nucleosynthesis ejecta in the Galaxy which incorporate the population synthesis calculations of individual massive star groups. Based on a variety of stellar evolution models, supernova (SN) explodabilities, and density distributions, we find that the measured ²⁶Al distribution from INTEGRAL/SPI can be explained by a Galaxy-wide population synthesis model with a SFR of 4–8 M_⊙ yr⁻¹ and a spiral-arm-dominated density profile with a scale height of at least 700 pc. Our model requires that most massive stars indeed undergo a SN explosion. This corresponds to a SN rate in the Milky Way of 1.8–2.8 per century, with quasi-persistent ²⁶Al and ⁶⁰Fe masses of 1.2–2.4 M_⊙ and 1–6 M_⊙, respectively. Comparing the simulated morphologies to SPI data suggests that a frequent merging of superbubbles may take place in the Galaxy, and that an unknown yet strong foreground emission at 1.8 MeV could be present.