J/ApJS/239/30 S-like ions from Cr IX to Cu XIV transitions (Wang+, 2018)
Benchmarking atomic data from large-scale multiconfiguration Dirac-Hartree-Fock
calculations for astrophysics: S-like ions from Cr IX to Cu XIV.
Wang K., Song C.X., Jonsson P., Del Zanna G., Schiffmann S., Godefroid M.,
Gaigalas G., Zhao X.H., Si R., Chen C.Y., Yan J.
<Astrophys. J. Suppl. Ser., 239, 30 (2018)>
=2018ApJS..239...30W 2018ApJS..239...30W
ADC_Keywords: Atomic physics
Keywords: atomic data ; atomic processes
Abstract:
We present a consistent set of calculated energies and E1, M1, E2, M2
radiative transition data for the main n=3 levels from the 3s23p4,
3p6, 3s3p43d, 3s23p23d2, 3s3p5, 3s23p33d, and
3s3p33d2 configurations for S-like ions from CrIX to CuXIV. The
fully relativistic multiconfiguration Dirac-Hartree-Fock method
implemented in the GRASP2K code (Jonsson+ 2007CoPhC.177..597J 2007CoPhC.177..597J ;
2013CoPhC.184.2197J 2013CoPhC.184.2197J) is used to perform the present calculations. The
excitation energies of the lowest 47 levels from the 3s23p4,
3s3p5, and 3s23p33d configurations, producing the strongest
lines, are found to be in good agreement, reaching spectroscopic
accuracy, with the latest experimental values for FeXI evaluated by
Del Zanna. Our energies can reliably be used to identify in
astrophysical and laboratory spectra the 3s23p33d levels in other
S-like ions, which are mostly unknown. On the contrary, significant
discrepancies with the 3s3p43d levels were found, emphasizing the
need for more detailed experimental studies. A few new tentative
identifications are suggested. The benchmarks we present indicate that
our consistent set of radiative data is accurate and can be used for
spectral line modeling.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 251 1737 Energy levels relative to the ground state along
with radiative lifetime for the lowest 159
(227, 236, 304, 376, 436) states of Cr IX
(Mn X, Fe XI, Co XII, Ni XIII, Cu XIV).
table4.dat 104 54343 Transition wavelengths, transition rates A,
weighted oscillator strengths gf and line strengths
between the states of Cr IX, Mn X, Fe XI, Co XII,
Ni XIII, and Cu XIV listed in Table 3.
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See also:
J/A+AS/125/149 : CHIANTI- An Atomic Database For Emission Lines I. (Dere+ 1997)
J/ApJ/543/1016 : SERTS-97 EUV spectrum of solar active region (Brosius+ 2000)
J/A+A/514/A40 : IRON project. LXVIII (Del Zanna+, 2010)
J/A+A/549/A42 : FeXI soft X-ray lines (Del Zanna+, 2013)
J/A+A/559/A100 : Boron isoelectronic sequence data (Jonsson+, 2013)
J/ApJS/215/26 : Energy levels & transition rates of C-like ions (Wang+, 2014)
J/ApJS/218/16 : Energy levels & transition rates of Be-like ions (Wang+, 2015)
J/ApJS/227/16 : Energy levels & transition rates for F-like ions (Si+, 2016)
J/ApJS/226/14 : MBPT calculations for Ne-like ions (Wang+, 2016)
J/ApJS/223/3 : Energies & radiative transition ArXII to ZnXXIV (Wang+, 2016)
J/ApJS/229/37 : Energy levels & transition rates of O-like ions (Wang+, 2017)
J/ApJS/234/40 : Be-like ions from BII to NeVII transition data (Wang+, 2018)
J/ApJS/235/27 : Energy levels & transition rates for P-like ions (Wang+, 2018)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Z [24/29] Atomic number
5- 7 I3 --- Key [1/435] Key number
9- 68 A60 --- Level Configuration and LSJ level
70- 76 I7 cm-1 EMCDHF1 [0/1631257] Energy levels, the present
ab initio calculations
78- 84 I7 cm-1 EMCDHF2 [0/1631005] Energy levels, shifted energies
of excited states (1)
86- 91 I6 cm-1 ENIST [0/763830]? Observed NIST energies (2)
93- 98 I6 cm-1 EMRMP [0/763720]? MR-MP calculations (3)
100-108 E9.3 s Lifetime-l [0/21.1] Lifetimes, present calculations in
length gauge
110-118 E9.3 s Lifetime-v [0/21.5] Lifetimes, present calculations in
velocity gauge
120-251 A132 --- LS-comp LS eigenvector (4)
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Note (1): The present calculations where energies of excited states have
been shifted by a constant ES given in Table 2 (see text for more
details).
Note (2): Observed energies listed in the NIST Atomic Spectra Database (ver.
5.5.6), Kramida+ (2018 - https://physics.nist.gov/asd/);
Note (3): MR-MP calculations by Ishikawa & Vilkas (2008PhRvA..78d2501I 2008PhRvA..78d2501I)
Note (4): The first number is the expansion coefficient for the leading
LS-composition.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Z [24/29] Atomic number
4- 6 I3 --- j [1/245] Upper level
8- 10 I3 --- i [2/434] Lower level
12- 21 E10.4 0.1nm Wave [61.3/200240] Wavelength; Angstroms
23- 24 A2 --- Type Transition type
26- 34 E9.3 s-1 A-l [0.0001/3e+11] Transition rates, length form
36- 44 E9.3 --- gf-l [5.9e-13/7.5] Weighted oscillator strengths,
length form
46- 54 E9.3 --- Str-l [5.7e-10/84] Line strength; Atomic units,
length form
56- 64 E9.3 s-1 A-v [6.7e-05/3e+11]? Transition rates, velocity form
66- 74 E9.3 --- gf-v [1.8e-12/7.5]? Weighted oscillator strengths,
velocity form
76- 84 E9.3 --- Str-v [6.8e-10/4.6]? Line strength; Atomic units,
velocity form
86- 94 E9.3 --- BF [1e-05/1]? Branching fraction from the
upper level
96-104 E9.3 --- dT [0/1]? Relative difference of the transition
rates (1)
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Note (1): dT is the relative difference of the transition rates in length
and velocity form as given by Eq. (3).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Feb-2019