High energy gamma-ray emission powered by a young protostar: the case of S255 NIRS 3
| Autor: | Emma de Oña Wilhelmi, Rubén López-Coto, Yang Su |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2023 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
individual: S255 NIRS 3 [stars] FOS: Physical sciences Astronomy and Astrophysics interaction [p p] energy [gamma ray] GeV bremsstrahlung GLAST stars [gamma-rays] massive [stars] Space and Planetary Science emission [gamma ray] gas secondary [electron] synchrotron flare [stars] ddc:520 high [energy] acceleration [cosmic radiation] structure Astrophysics - High Energy Astrophysical Phenomena protostars [stars] |
| DOI: | 10.3204/PUBDB-2023-04006 |
| Popis: | Evidence of efficient acceleration of cosmic rays in massive young stellar objects has been recently reported. Among these massive protostars, S255 NIRS 3 for which extreme flaring events associated with radio jets have been detected, is one of the best objects to test this hypothesis. We search for gamma-ray emission associated with this object in Fermi-LAT data and inspect the gas content in different molecular lines using the MWISP survey. A GeV source dubbed 4FGL J0613.1+1749c lies on top of the MYSO region, where two filamentary ~10 pc CO structures extend along the same direction of the sub-parsec radio jets. We investigate the spectrum, morphology, and light curve of the gamma-ray source and compare it with the theoretical emission expected from hadronic and leptonic populations accelerated in the radio jets. We argue that the gamma-ray source could be powered by particles accelerated in the S255 NIRS 3 jets, radiating via Bremsstrahlung or proton-proton interaction, and with a synchrotron component shinning in radio from primary or secondary electrons in the case of a leptonic or hadronic population. accepted for publication in Monthly Notices of the Royal Astronomical Society |
| Databáze: | OpenAIRE |
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