J/A+A/664/A62 Fe-L list of lines of interest (Gu+, 2022)
X-ray spectra of the Fe-L complex. III: systematic uncertainties in atomic data.
Gu L., Shah C., Mao J., Raassen A.J.J., de Plaa J., Pinto C., Akamatsu H.,
Werner N., Simionescu A., Mernier F., Sawada M., Mohanty P., Amaro P.,
Gu M.F., Porter F.S., Lopez-Urrutia J.R.C., Kaastra J.S.
<Astron. Astrophys. 664, A62 (2022)>
=2022A&A...664A..62G 2022A&A...664A..62G (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics
Keywords: atomic data - techniques: spectroscopic - stars: coronae -
galaxies: clusters: intracluster medium
Abstract:
There has been a growing request from the X-ray astronomy community
for a quantitative estimate of systematic uncertainties originating
from the atomic data used in plasma codes. Though there have been
several studies looking into atomic data uncertainties using
theoretical calculations, in general, there is no commonly accepted
solution for this task. We present a new approach for estimating
uncertainties in the line emissivities for the current models of
collisional plasma, mainly based upon a dedicated analysis of observed
high resolution spectra of stellar coronae and galaxy clusters. We
find that the systematic uncertainties of the observed lines
consistently show an anticorrelation with the model line fluxes, after
properly accounting for the additional uncertainties from the ion
concentration calculation. The strong lines in the spectra are in
general better reproduced, indicating that the atomic data and
modeling of the main transitions are more accurate than those for the
minor ones. This underlying anticorrelation is found to be roughly
independent of source properties, line positions, ion species, and the
line formation processes. We further applied our method to the
simulated XRISM and Athena observations of collisional plasma sources
and discuss the impact of uncertainties on the interpretation of these
spectra. The typical uncertainties are 1-2% on temperature and 3-20%
on abundances of O, Ne, Fe, Mg, and Ni.
Description:
List of the lines of interest from the Chandra HETG spectra of Capella
and HR 1099. For each line, the line ID given in the Figure A1 and A2,
ion, wavelength, line formation processes, line emissivities measured
from the Capella and HR 1099 data, and their uncertainties are
provided. The wavelength, line formation and emissivities are
calculated with the SPEX code.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 99 750 Line information
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See also:
J/A+A/627/A51 : Levels and rate coefficients of the Fe-L (Gu+, 2019)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Index Line ID as given in Figures A1 and A2
6- 15 F10.4 0.1nm lambda Line wavelength
17- 18 I2 --- Z Element
20- 21 I2 --- Ion Isoelectronic sequence number
24- 28 F5.3 --- EX Contribution of upper level population
from direct excitation
31- 35 F5.3 --- CEX contribution of upper level population
from excitation followed by cascade
38- 42 F5.3 --- RR contribution of upper level population
from radiative recombination
45- 49 F5.3 --- CRR contribution of upper level population
from radiative recombination followed by
cascade
52- 56 F5.3 --- DR contribution of upper level population
from dielectronic recombination
59- 63 F5.3 --- CDR contribution of upper level population
from dielectronic recombination followed by
cascade
66- 72 F7.4 ph/m2/s Icap Capella line emissivity from the best-fit
models (model 1)
74- 81 F8.4 --- Ucap Capella fractional Gaussian contribution
(model 2)
84- 90 F7.4 ph/m2/s IHR HR 1099 line emissivity from the best-fit
models (model 1)
93- 99 F7.4 --- UHR ? HR 1099 fractional Gaussian contribution
(model 2)
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Acknowledgements:
Liyi Gu, l.gu(at)sron.nl
References:
Gu et al., Paper I 2019A&A...627A..51G 2019A&A...627A..51G, Cat. J/A+A/627/A51
Gu et al., Paper II 2020A&A...641A..93G 2020A&A...641A..93G
(End) Liyi Gu [SRON], Patricia Vannier [CDS] 21-Jun-2022