Modeling of iron K lines: Radiative and Auger decay data for $\ion{Fe}{ii}$–$\ion{Fe}{ix}$

Palmeri, P.; Mendoza, C.; Kallman, T. R.; Bautista, M. A.; Meléndez, M.

doi:10.1051/0004-6361:20031262

Cited by 139 publications

(152 citation statements)

References 38 publications

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“…The Ni Kβ/Ni Kα ratio is marginally consistent with all these values within its uncertainties, but the measured iron ratio is clearly higher. Other measurements and calculations for neutral iron give figures of the same order with Fe Kβ/Fe Kα ≈ 0.13 (see, e.g., Palmeri et al 2003, and references therein).…”

Section: Time Resolved Spectramentioning

confidence: 52%

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

Fürst¹,

Suchy

Kreykenbohm³

et al. 2011

A&A

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We present an in-depth study of the high mass X-ray binary (HMXB) GX 301−2 during its pre-periastron flare using data from the XMM-Newton satellite. The energy spectrum shows a power law continuum absorbed by a large equivalent hydrogen column on the order of 10 24 cm −2 and a prominent Fe Kα fluorescent emission line. Besides the Fe Kα line, evidence for Fe Kβ, Ni Kα, Ni Kβ, S Kα, Ar Kα, Ca Kα, and Cr Kα fluorescent lines is found. The observed line strengths are consistent with fluorescence in a cold absorber. This is the first time that Cr Kα is seen in emission in the X-ray spectrum of a HMXB. In addition to the modulation by the strong pulse period of ∼685 s the source is highly variable and shows different states of activity. We perform time-resolved as well as pulse-to-pulse resolved spectroscopy to investigate differences between these states of activity. We find that fluorescent line fluxes are strongly variable and generally follow the overall flux. The N H value is variable by a factor of 2, but not correlated to continuum normalization. We find an interval of low flux in the light curve in which the pulsations cease almost completely, without any indication of an increasing absorption column. We investigate this dip in detail and argue that it is most likely that during the dip the accretion ceased and the afterglow of the fluorescent iron accounted for the main portion of the X-ray flux. A similar dip was found earlier in RXTE data, and we compare our findings to these results.

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Section: Time Resolved Spectramentioning

confidence: 52%

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

Fürst¹,

Suchy

Kreykenbohm³

et al. 2011

A&A

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“…Some of the characteristics of the unresolved transition arrays (UTAs) are studied in the singly-ionized (Z c = Z − N + 1 = 2) ions with 11 ≤ Z ≤ 30, namely the λ Kα 1 , λ Kα 2 and λ Kβ UTA centroid wavelengths, the Kα 2 /Kα 1 and Kβ/Kα intensity ratios, the KLM/KLL and KMM/KLL Auger channel ratios and the K-shell fluorescence yield ω K . As a matter of fact, xstar simulations of iron K lines showed that K lines of second and third-row ions will appear in astrophysical spectra as UTAs (Palmeri et al 2003b). …”

Section: Resultsmentioning

confidence: 99%

Atomic decay data for modeling K lines of iron peak and light odd-Zelements

Palmeri

Quinet

Mendoza

et al. 2012

A&A

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Complete data sets of level energies, transition wavelengths, A-values, radiative and Auger widths and fluorescence yields for K-vacancy levels of the F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu and Zn isonuclear sequences have been computed by a Hartree-Fock method that includes relativistic corrections as implemented in Cowan's atomic structure computer suite. The atomic parameters for more than 3 million fine-structure K lines have been determined. Ions with electron number N > 9 are treated for the first time, and detailed comparisons with available measurements and theoretical data for ions with N ≤ 9 are carried out in order to estimate reliable accuracy ratings.

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“…The presence of Fe K β, insures that the ionization state of iron is less than Fe xvii (Yaqoob et al 2007). A further constraint on the ionization state of iron would be based on the Fe Kα/Fe K β branching ratio, which ranges from 0.12 for Fe i up to 0.17 for Fe ix (Palmeri et al 2003). Unfortunately, considering the associated errors on the observed line fluxes, we only obtain a lower limit of 0.1 to that ratio.…”

Section: The Origin Of the Fe Kα Linementioning

confidence: 94%

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

Costantini¹,

Kaastra

Korista

et al. 2010

A&A

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We present the results of a ∼160 ks-long XMM-Newton observation of the Seyfert 1 galaxy Mrk 279. The spectrum shows evidence of both broad and narrow emission features. The Fe Kα line may be equally well explained by a single broad Gaussian (FWHM ∼ 10 000 km s −1 ) or by two components: an unresolved core plus a very broad profile (FWHM ∼ 14 000 km s −1 ). For the first time we quantified, via the "locally optimally emitting cloud" model, the contribution of the broad line region (BLR) to the absolute luminosity of the broad component of the Fe Kα at 6.4 keV. We find that the contribution of the BLR is only ∼3%. In the two-line component scenario, we also evaluated the contribution of the highly ionized gas component, which produces the Fe xxvi line in the iron K region. This contribution to the narrow core of the Fe Kα line is marginal <0.1%. Most of the luminosity of the unresolved, component of Fe Kα may come from the obscuring torus, while the very-broad associated component may come from the accretion disk. However, models of reflection by cold gas are difficult to test because of the limited energy band. The Fe xxvi line at 6.9 keV is consistent to be produced in a high column density (N H ∼ 10 23 cm −2 ), extremely ionized (log ξ ∼ 5.5−7) gas. This gas may be a highly ionized outer layer of the torus.

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Modeling of iron K lines: Radiative and Auger decay data for $\ion{Fe}{ii}$–$\ion{Fe}{ix}$

Cited by 139 publications

References 38 publications

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

Atomic decay data for modeling K lines of iron peak and light odd-Zelements

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

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