Parts-per-million-accurate determination of the K alpha photoionization resonance of Be-like oxygen with resolution of its 16 O- 18 O isotopic shift
Jonas Danisch, Marc Botz, Chintan Shah, Moto Togawa, Joschka Goes, Dominic Hache, Filipe Grilo, Pedro Amaro, Vladimir A. Yerokhin, Steffen Kühn, Awad Mohamed, Roberta Totani, Monica de Simone, Stefano Orlando, Thomas Pfeifer, Fabrizio Nicastro, Marcello Coreno, José R. Crespo López-Urrutia
physics.atom-ph, astro-ph.HE, astro-ph.IM, physics.plasm-ph
Submitted: 2026-07-01
Comments: 9 pages, 6 figures, 4 tables, published in Physical Review A
Journal ref: Physical Review A 113, 022811 (2026)
DOI: 10.1103/d4h7-ykwn
License: http://creativecommons.org/licenses/by/4.0/
The gist: We determine with high accuracy the energy of the inner-shell transition 1s squared 2s 2 1 S 0 to 1s 2s 2 2p 3/2 1 P 1 16 O K alpha 4+ at 554.372(3) eV (lambda = 22.36480(12)) as well as its small
Terminology
Abstract
We determine with high accuracy the energy of the inner-shell transition 1s squared 2s 2 1 S 0 to 1s 2s 2 2p 3/2 1 P 1 16 O K alpha 4+ at 554.372(3) eV (lambda = 22.36480(12)) as well as its small shift of 2.2 plus or minus 1.3 meV (lambda = 0.089(52) m) for the 18 O isotope. This transition blends with a K alpha line of O 5+ used in astrophysical diagnostics, potentially affecting its reliability. In contrast to our experimental uncertainty of plus or minus 3 meV, advanced electronic structure predictions for this four-electron system, including quantum electrodynamic (QED) corrections on the order of 100 meV, still scatter by more than plus or minus 250 meV. Ions generated and stored in an electron beam ion trap were excited at the ELETTRA synchrotron facility with monochromatic soft x rays, with photon energies corrected by an additional spectrometer. Upon resonant excitation of O 4+ and subsequent autoionization, we separate the photoions of each isotope by a time-of-flight measurement. This way, we resolve soft x-ray isotopic shifts of a few meV, obtain very accurate data on an essential astrophysical ion, and test calculations down to the level of QED contributions.
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