Kshell photoabsorption and photoionization of trace elements. II. Isoelectronic sequences with electron number $12\leq N \leq 18$
Key Words.:
atomic data – Xrays: generalAbstract
Context:We are concerned with improving the diagnostic potential of the K lines and edges of elements with low cosmic abundances, namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn, that are observed in the Xray spectra of supernova remnants, galaxy clusters and accreting black holes and neutron stars.
Aims:Since accurate photoabsorption and photoionization cross sections are needed in their spectral models, they have been computed for isoelectronic sequences with electron number using a multichannel method.
Methods:Target representations are obtained with the atomic structure code autostructure, and groundstate cross sections are computed with the Breit–Pauli matrix method (bprm) in intermediate coupling, including damping (radiative and Auger) effects.
Results:Following the findings in our earlier work on sequences with , the contributions from channels associated with the 2shole target configurations and those containing 3d orbitals are studied in the Mg () and Ar () isoelectronic sequences. Cross sections for the latter ions are also calculated in the isolatedresonance approximation as implemented in autostructure and compared with bprm to test their accuracy.
Conclusions:It is confirmed that the collisional channels associated with the target configurations must be taken into account owing to significant increases in the monotonic background cross section between the L and K edges. Target configurations with 3d orbitals give rise to fairly conspicuous unresolved transition arrays in the Ledge region, but to a much lesser extent in the Kedge which is our main concern; therefore, they have been neglected throughout owing to their computationally intractable channel inventory, thus allowing the computation of cross sections for all the ions with in intermediate coupling with bprm. We find that the isolatedresonance approximations performs satisfactorily and will be our best choice to tackle the systems with ground configuration () in isoelectronic sequences with .
1 Introduction
K lines and edges from elements with low cosmic abundance (trace elements) have been observed with the Chandra, XMMNewton and Suzaku space telescopes in the Xray spectra of supernova remnants, galaxy clusters, and accreting black holes and neutron stars. They have been used to constrain the ionization, metallicity, abundances, blackhole progenitor mass, and, in the case of warm absorbers, the flow properties (see, for instance, Hwang et al. 2000; Miller et al. 2006; Badenes et al. 2008; Kallman et al. 2009; Tamura et al. 2009; Ueda et al. 2009; Nobukawa et al. 2010; Park et al. 2013). Their diagnostic potential was set to become exploited with the launching last February 2016 of the Hitomi spatial telescope (previously referred to as AstroH), an instrument of remarkable spectroscopic capabilities. In spite of its becoming inoperative soon after, there is currently a definite intention to replace it by 2020; therefore, the continuity of support projects, such as the present one to compute the atomic data required in specialised spectral modeling, is still arguable.
We have been involved for some time in the computation of atomic data to enable the reliable modeling of the traceelement K lines. Palmeri et al. (2012), to be referred to hereafter as PQM12, computed with hfr (a Hartree–Fock code with relativistic corrections by Cowan 1981) level energies, radiative and Auger widths, and fluorescence yields for Kvacancy levels of the complete isonuclear sequences of F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn. Using the atomic target models developed therein, Palmeri et al. (2016) (Paper 1 hereafter) calculated photoabsorption and photoionization cross sections of the ground state of ionic systems with electron number . In this report, we extend this work to the thirdrow isoelectronic sequences () which, owing to the atomic complexity brought about by the open 3p subshell, implies a different computational strategy.
Cross sections for the finestructure ground levels of the secondrow ions () were computed in Paper 1 in the closecoupling framework with the Breit–Pauli matrix method (bprm, Berrington et al. 1995), which enabled the rendering of the resonance structures of the open L shell and K ionization edge. Radiation and spectatorAuger damping that causes Kedge smearing was taken into account (Palmeri et al. 2002). The Nalike ions (), in particular P v and Zn xx, were then used as test cases to extend this approach to the more complex members of the third row with . For instance, since the inclusion of target configurations with 3d orbitals dramatically increases the collisional channel inventory, particularly when the 3p subshell is half filled, matrix calculations would then have to be performed in coupling rather than in intermediate coupling or, alternatively, be replaced by the uncoupled isolatedresonance approximation (AbdelNaby et al. 2012) of the atomic structure code autostructure (Eissner et al. 1974; Badnell 2011). We found in Paper 1 that 3d resonances were mainly conspicuous in the L edge rather than the K edge, the latter being our main concern and, therefore, they could be practically neglected in spite of the everpresent configurationinteraction (CI) effects.
These computational tradeoffs are examined in greater depth in this work, specifically for the simpler isoelectronic sequences with and , in an attempt to maintain the intermediate coupling scheme for all the ionic systems of interest. A brief description of the numerical methods is given in Sect. 2 and the results of the targetrepresentation investigations and final calculations are discussed in Sect. 3. Conclusions are drawn in Sect. 4, together with some guidelines for the future consideration of the fourthrow ions.
2 Numerical methods
This project intends to compute photoabsorption and total and partial photoionization cross sections for ionic species of the isonuclear series P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn with electron numbers , where is the atomic number identifying the sequence. Cross sections for isoelectronic sequences with were reported in Paper 1, and here we discuss the details of those with . As previously mentioned in Paper 1, species with will be treated elsewhere.
The closecoupling framework of scattering theory is the main quantummechanical backbone, where the wave function of the total electron system is expanded in terms of the eigenfunctions of an ()electron target. Calculations are performed in intermediate coupling with the relativistic (Breit–Pauli) bprm method, where configuration space is partitioned by a sphere of radius into two regions: an inner region () treated with the rmatrx1 package that takes into account exchange and correlation effects between the target and the active electron; and an asymptotic region () where these effects may be neglected and the active electron is subject to longrange multipole potentials. This external region is solved with the stgbf0damp7 code that also includes radiation and spectatorAuger damping by means of a model potential (Robicheaux et al. 1995; Gorczyca & Badnell 1996, 2000). For comparison purposes, particularly for the large target representations, the matrix package is also run in the more concise coupling scheme.
Adopting the target representations listed in Table 9 of PQM12 – namely configuration expansions, level energies, and Auger widths – orbitals are generated in a Thomas–Fermi–Dirac statistical potential with the autostructure atomic structure code (Eissner et al. 1974; Badnell 2011). Cross sections in the isolatedresonance approximation are also obtained with this code. We note that, due to the complexity of thirdrow ions, the target representations of PQM12 do not list the levels that arise from a large number of correlation configurations that were taken into account to obtain reasonably accurate level energies and a level order similar to the spectroscopic.
3 Results
Cross sections are calculated right from threshold up to the monotonic decreasing tail beyond the K edge. Although our main interest is the Kedge structure, an effort is also made to resolve the resonances associated with the valence shell and the L edge. In the resonance regions, a fine mesh step of Ryd is used where .
Following the findings of Paper 1, we analyse some of the problems discussed therein, in particular the contributions from target configurations and those from missing configurations (mainly those with 3d orbitals) in both the K and Ledge regions using ions of the Mg () and Ar () isoelectronic sequences.
3.1 target configurations
In Paper 1 we find that, in the case of the Nalike sequence (), the corresponding Nelike target models in PQM12 comprised the following configurations: , , , , and , but neglected and . If the latter two are not taken into account in the closecoupling expansion, some resonances (mostly narrow) in the Ledge region would be missing, but more importantly, the background cross section between the L and K edges is significantly underestimated. This effect is further examined here in Mglike P iv and Arlike Sc iv by using the following target representations:
 Target A –

As listed in Table 9 of PQM12, the Nalike P v target is represented with the configurations , , , , and ;
 Target B –

The P v target includes the configurations of Target A plus and ;
 Target C –

As listed in Table 9 of PQM12, the Cllike Sc v target is represented with the configurations , , and ;
 Target D –

Sc v target includes the configurations of Target C plus .
In Fig. 1 the photoabsorption cross sections of P iv and Sc iv ions are plotted in both the L and Kedge regions, where the underestimated background cross sections caused by the exclusion of channels associated to the target configurations can be seen. Although the K edge is hardly altered, when these configurations are taken into account, additional unresolved transition arrays (UTAs) appear ( Ryd for P iv and Ryd in Sc iv) in the Ledge region.
In the case of P iv, the L edge is amplified in Fig. 2a where, to estimate the variations of the UTA morphology, the cross sections have been convolved with a Gaussian of width . We see that, apart from the extra features emerging when using Target B in the 14–17 Ryd energy interval, the resonance structure is also somewhat perturbed around the edge head ( Ryd).
3.2 Missing configurations
An inherent problem in the computation of radiative properties for thirdrow ions () with an incomplete 3p subshell is the large number of closely coupled states to be considered from configurations of the type . If electron promotions from the K and L shells are additionally involved, such as in this work, then the channel inventory in the closecoupling expansion rapidly becomes computationally intractable; therefore, compromises are unavoidable in spite of the ensuing CI shortcomings. For instance, in the Nalike targets () of PQM12, configurations of the type and were neither listed, nor those containing 3d orbitals for all the systems with .
To study the impact of these exclusions on the edgeregion cross sections, three targets are considered:
 Target E –

Nalike P v target is represented with configurations of Target B plus , and ;
 Target F –

P v target includes the configurations of Target E plus , , , , , , , , and ;
 Target G –

Cllike Sc v target is represented with the configurations of Target D plus , , , , , , and .
Target B comprises 39 finestructure levels, an inventory that is almost doubled in Target E to 76 levels while Target F gives rise to 305. This sharp level increase, when only singleelectron promotions are considered, supports our previous comments on computationally unmanageable atomic models, even for the relatively simple Na and Cllike targets. A similar situation is found for the latter, where Target D encompasses 72 levels in comparison with 208 in Target G.
Photoabsorption cross sections for Mglike P iv in the Kedge region computed with Target B and Target E are very similar but, as shown in Fig. 2b, the UTAs in the edge head at 13–14 Ryd show different morphologies. These behavioral patterns are maintained in comparisons between the cross sections computed with Target E and Target F (Fig. 3) and, in the case of Arlike Sc iv, between Target D and Target G (Fig. 4). Owing to the large number of collisional channels, cross sections in Figs. 3–4 have been computed in coupling; thus, a comparison between the black curves in Fig. 2b and Fig. 3a gives a measure of the small but distinguishable resonancestructure differences resulting from the  and intermediatecoupling frameworks.
3.3 Isolatedresonance approximation
A comparison is depicted in Fig. 5 between the photoabsorption cross sections of Sc iv in the K and Ledge regions computed in intermediate coupling with bprm and, in the isolated resonance approximation, with autostructure, where it may be seen that the latter performs surprisingly well in spite of the neglect of channel coupling and the adoption of symmetric Lorentzian resonance profiles. In this plot, a small energy shift was performed to match the resonance series, which is due to differences in the bprm and autostructure ionization potentials. Moreover, a comparison of the K resonance position in Fig. 4b and Fig. 5b reveals a 1.5 Ryd discrepancy that is caused by the relativistic contribution since the former was obtained in coupling. This discrepancy can be reduced by running bprm in coupling but including the relativistic corrections that do not lead to fine structure; i.e. the masscorrection and Darwin onebody terms.
3.4 Sequences with
Taking into account the findings that emerged from the different target representations considered for the Mg and Arlike isoelectronic sequences in Sects. 3.1–3.2, we proceeded to compute with bprm cross sections for the other more computationally involved sequences, namely those with electron number . We adopted the target models of PQM12, but additionally included the configurations that, as shown in Fig. 1, affect the background photoabsorption cross sections between the L and K edges. Configurations including 3d orbitals were thus excluded leading to underrepresented L edges (see Figs. 3–4).
As an example, photoabsorption cross sections in the K and Ledge regions for Zn ions with electron number are plotted in Fig. 6, showing contrasting edge resonance structures. The K edge is dominated by welldefined resonance series (K lines) whose broad and practically constant widths are regulated by damping (radiative and spectatorelectron Auger); they thus lead to smeared edges in the photon energy band 745–765 Ryd. The sharp L edges in the energy band 110–130 Ryd are populated by a very large number of narrow resonances where the and UTAs at Ryd and Ryd, respectively, can be distinguished. Less pronounced UTAs between 38 and 55 Ryd due to valence resonances may also be appreciated.
From the astronomical diagnostic point of view, Fig. 6 appears to indicate that the K, K, and K edge will give rise to resolvable spectral signatures with information about the plasma ionization state, while L edge dominated by several UTAs will be messy and thus less astrophysically useful; in fact, in such spectral ranges K lines from the lower species are the features to single out.
4 Conclusions

Photoabsorption and photoionization (total and partial) cross sections for the ions of P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn with electron numbers have been computed with the Breit–Pauli matrix method (bprm) in intermediate coupling. Both the L and K resonance structures are well resolved with fine energy meshes. Damping effects have been shown to be relevant in the Kedge resonance structures.

Regarding the importance of 2s promotion discussed in Paper 1, it is reaffirmed that, for thirdrow ions, this must be taken into account with configurations of the type otherwise the background cross sections between the K and L edges are underestimated.

We have excluded target configurations with 3d orbitals, thus enabling the computations of cross sections in intermediate coupling with bprm that adopt the ion models of PQM12 for isoelectronic sequences with . As shown in Sect. 3.2, the L edge will be somewhat affected, but a more realistic representation of its intricate resonance series would require more sophisticated target models and a computational effort beyond the scope of this project that is mainly focused on the Kedge structures. For tractable targetmodel management, we have only considered single excitations within the complex that certainly lead to unconverged CI expansions, in particular in the valence electron shell. In Paper 1, the possibility of rendering the K and L edges in separate calculations was mentioned, but this scheme was dropped since it would have made the determination of partial photoionization cross section, which are required in the atomic database of the xstar spectral modeling code (Bautista & Kallman 2001; Kallman & Bautista 2001), very cumbersome.

For ions with , namely Sc iv, we have made comparisons of the present bprm photoabsorption cross sections with those computed in the isolatedresonance approximation with the autostructure code. This is an important step since cross sections for most of the lowly ionized species with electron number and ground configurations with will not be calculated with bprm owing to target size. In this respect, it has been shown that, in spite of the shortcomings of the isolatedresonance approximation, i.e. neglected channelcoupling and symmetric resonance profiles, its performance and general accuracy is satisfactory.

When cross sections are computed with bprm in coupling, it is emphasized that the relativistic onebody, nonfinestructure corrections must be taken into account otherwise poor energy resonance positions, in particular those associated with the K edge, will be obtained.

Data access will be managed through the Centre de Données astronomiques de Strasbourg (CDS
^{1} ) taking into consideration previous longterm arrangements with this data center, which have led to sustainable and efficient data services, e.g. TOPbase^{2} (Cunto et al. 1993). The complete data sets will be uploaded with the upcoming Paper 3 of the present series, and the corresponding links will be provided through the ADS.
Acknowledgements.
This project is sponsored by the NASA grant 12APRA120070 through the Astrophysics Research and Analysis Program. Pascal Quinet and Patrick Palmeri are Research Director and Research Associate, respectively, of the Belgian Fund for Scientific Research F.R.S.FNRS.Footnotes
 http://cdsweb.ustrasbg.fr/
 http://cdsweb.ustrasbg.fr/topbase/topbase.html
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