X-ray spectra of the Fe-L complex
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F19%3A00110204" target="_blank" >RIV/00216224:14310/19:00110204 - isvavai.cz</a>
Result on the web
<a href="https://www.aanda.org/articles/aa/abs/2019/07/aa33860-18/aa33860-18.html" target="_blank" >https://www.aanda.org/articles/aa/abs/2019/07/aa33860-18/aa33860-18.html</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/201833860" target="_blank" >10.1051/0004-6361/201833860</a>
Alternative languages
Result language
angličtina
Original language name
X-ray spectra of the Fe-L complex
Original language description
The Hitomi results on the Perseus cluster have led to improvements in our knowledge of atomic physics that are crucial for the precise diagnostic of hot astrophysical plasma observed with high-resolution X-ray spectrometers. However, modeling uncertainties remains, both within but especially beyond Hitomi's spectral window. A major challenge in spectral modeling is the Fe-L spectrum, which is basically a complex assembly of n >= 3 to n = 2 transitions of Fe ions in different ionization states, affected by a range of atomic processes such as collisional excitation, resonant excitation, radiative recombination, dielectronic recombination, and innershell ionization. In this paper we perform a large-scale theoretical calculation on each of the processes with the flexible atomic code (FAC), focusing on ions of Fe XVII to Fe XXIV that form the main body of the Fe-L complex. The calculation includes a large set of energy levels with a broad range of quantum number n and l, taking into account the full-order configuration interaction and all possible resonant channels between two neighboring ions. The new data are found to be consistent within 20% with the recent individual R-matrix calculations for the main Fe-L lines, although the discrepancies become significantly larger for the weaker transitions, in particular for Fe XVIII, Fe XIX, and Fe XX. By further testing the new FAC calculations with the high-quality RGS data from 15 elliptical galaxies and galaxy clusters, we note that the new model gives systematically better fits than the current SPEX v3.04 code, and the mean Fe abundance decreases by 12%, while the O/Fe ratio increases by 16% compared with the results from the current code. Comparing the FAC fit results to those with the R-matrix calculations, we find a temperature-dependent discrepancy of up to similar to 10% on the Fe abundance between the two theoretical models. Further dedicated tests with both observed spectra and targeted laboratory measurements are needed to resolve the discrepancies, and ultimately to get the atomic data ready for the next high-resolution X-ray spectroscopy mission.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
—
Continuities
S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2019
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
ASTRONOMY & ASTROPHYSICS
ISSN
1432-0746
e-ISSN
—
Volume of the periodical
627
Issue of the periodical within the volume
JUL 2019
Country of publishing house
FR - FRANCE
Number of pages
24
Pages from-to
51-74
UT code for WoS article
000473255900004
EID of the result in the Scopus database
2-s2.0-85103686607