Energy Level and Line Tables for One-Electron Atomic Spectra*

Garcia, J. D.; Mack, J. E.

doi:10.1364/josa.55.000654

Cited by 319 publications

(139 citation statements)

References 5 publications

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“…3). The O vii f narrow emission line (rest wavelength 22.101 Å, Kelly 1987), as well as the broad O vii recombination line at 21.602 Å (Engstrom & Litzen 1995) and a broad N vii emission line at 24.78 Å (Garcia & Mack 1965). The oxygen lines have already been detected by S07 (although they detect a broad intercombination line instead of a recombination line), but the N vii emission line is a newly detected feature.…”

Section: Emission Linesmentioning

confidence: 84%

The outflow in Mrk 509

Detmers¹,

Kaastra

Costantini³

et al. 2010

A&A

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We analyzed three XMM-Newton observations of the Seyfert 1 galaxy Mrk 509, with the goal of detecting small variations in the ionized outflow properties. Measurements such as these are limited by the quality of the cross-calibration between RGS, the best instrument for characterizing the spectrum, and EPIC-pn, the best instrument for characterizing the variability. For all three observations we are able to improve the relative calibration of RGS and pn consistently to 4%. In all observations we detect three different outflow components and, thanks to our accurate cross-calibration, we are able to detect small differences in the ionization parameter and column density in the highest ionized component of the outflow. This constrains the location of this component of the outflow to within 0.5 pc of the central source. Our method for modeling the relative effective area is not restricted to just this source and can in principle be extended to other types of sources as well.

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Section: Emission Linesmentioning

confidence: 84%

The outflow in Mrk 509

Detmers¹,

Kaastra

Costantini³

et al. 2010

A&A

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“…3 and 4). They were calibrated with the very well known 1s -np transitions in H-like C 6+ ions, and 1s 2 1 S 0 -1s2p 1,3 P 1 and 1s 2 1 S 0 -1s3p 1 P 1 transitions in He-like ions of N [16,17,18,19]. Each of these is known to better than 1 mÅ.…”

Section: Methodsmentioning

confidence: 99%

Soft-X-ray spectra of highly charged Os, Bi, Th, and U ions in an electron beam ion trap

Beiersdörfer¹,

Fournier²,

Chen³

2005

Can. J. Phys.

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Systematic variation of the electron-beam energy in an electron-beam ion trap has been employed to produce soft-X-ray spectra of Os, Bi, Th, and U with highest charge states ranging up to Ni-like ions. Guided by relativistic atomic structure calculations, the strongest lines have been identified with ∆n=0 (n=4 to n =4) transitions in Rb-to Cu-like ions. The rather weak 4p-4d transitions are much less affected by QED contributions than the dominant 4s-4p transitions. Our wavelength measurements consequently provide benchmarks with and (almost) without QED. Because the radiative corrections are not very sensitive to the number of electrons in the valence shell, our data, moreover, provide benchmarks for the evaluation of electron-electron interactions.Résumé francais: (traduit par le journal)

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“…The wavelengths for  1s 3p 1s 2 Kβ and  1s 4p 1s 2 Kγ Rydberg states were taken from Vainshtein & Safronova (1985) and corrected for the ground state of Drake (1988) according to Beiersdorfer et al (1989). Values for the Lyman series in the H-like systems are from Garcia & Mack (1965). The wavelengths were converted to energy using l = -E hc 1 where Å = hc 12398.42 eV (with values for h, c and e from CODATA 2014, Mohr et al 2015).…”

Section: Calibrationmentioning

confidence: 99%

Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

Hell

Brown

Wilms

et al. 2016

ApJ

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We have measured the energies of the strongest 1s-2 ( ) = ℓ ℓ s, p transitions in He-through Ne-like silicon and sulfur ions to an accuracy of <1 eV using the Lawrence Livermore National Laboratory's electron beam ion traps, EBIT-I and SuperEBIT, and the NASA/GSFC EBIT Calorimeter Spectrometer (ECS). We identify and measure the energies of 18 and 21 X-ray features from silicon and sulfur, respectively. The results are compared to new Flexible Atomic Code calculations and to semi-relativistic Hartree-Fock calculations by Palmeri et al. (2008). These results will be especially useful for wind diagnostics in high-mass X-ray binaries, such as Vela X-1 and Cygnus X-1, where high-resolution spectral measurements using Chandraʼs high-energy transmission grating has made it possible to measure Doppler shifts of -100 km s 1 . The accuracy of our measurements is consistent with that needed to analyze Chandra observations, exceeding Chandraʼs -100 km s 1 limit. Hence, the results presented here not only provide benchmarks for theory, but also accurate rest energies that can be used to determine the bulk motion of material in astrophysical sources. We show the usefulness of our results by applying them to redetermine Doppler shifts from Chandra observations of Vela X-1.

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Energy Level and Line Tables for One-Electron Atomic Spectra*

Cited by 319 publications

References 5 publications

The outflow in Mrk 509

The outflow in Mrk 509

Soft-X-ray spectra of highly charged Os, Bi, Th, and U ions in an electron beam ion trap

Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

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