2024/02/26 by Alessa Ibrahim Wiggins, Wiggins, Alessa Ibrahim, Mia Sauda Bovill +7
Social Sciences · #Astrophysics of Galaxies (astro-ph.GA) #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Insurance, Mortality, Demography, Risk Management
paper · pdf · doi:10.48550/arxiv.2402.17076
openalex publication_date 2024/02/26 · openalex created_date 2024/03/05 · openalex updated_date 2026/07/28
Population III (Pop III) stars formed out of metal free gas in minihalos at z>20. While their ignition ended the Dark Ages and begin enrichment of the IGM, their mass distribution remains unconstrained. To date, no confirmed Pop III star has been observed and their direct detection is beyond the reach of the James Webb Space Telescope (JWST) without gravitational lensing. However, a subset of massive Pop III stars end their lives in pair instability supernova (PISN). With typical energies of ∼1053~erg, PISN light curve peaks are bright enough to be detectable by JWST and the Roman Space Telescope. The fundamental question of this work is whether or not observed PISN can be used as a diagnostic of the Pop III IMF. In this work, we use a model of the formation of the first stars to determine the dependence of PISN rates at z~>~5 for a range of Pop III power law IMFs (α~=~0.2~-~2.35) and, critically, the method by which the IMF is populated. At z~>~15, we predict typical rates of 10-2~-~102 per deg2 per year which will produce 10-3~-~0.1/year in a single NIRCam pointing and 0.003~-~30/year in a single Roman pointing with 0.1~-~1000 per year detected in the HLTDS. Our work highlights that theoretical modeling of PISN rates is required if upcoming PISN studies with JWST and Roman are going to constrain the Pop III IMF.