M. Fatih Hasoglu Thomas W. Gorczyca X-ray absorption by interstellar atomic gases near the K-edges of C, O, Ne, Mg, and Si, and the L-edge of Fe M. Fatih Hasoglu Thomas W. Gorczyca AtomDB UGA 11/4/17

Outline Previous X-ray Photoabsorption Calculations Current Work Simplest Neutral Neon and Ions Carbon Isonuclear Sequence Oxygen Isonuclear Sequence Mg Isonuclear Sequence Current Work Si K-shell Fe L-shell Perturbed Hydrogen Photoabsorption (Multiple Scattering)

Theoretical Methodology Belfast R-matrix Codes: Cross Sections and Auger Rates Pseudoresonance Elimination Inclusion of Radiative and Spectator Auger Broadening Wigner Time-Delay Method for Spectator Auger Rates Autostructure: DW Wavefunctions, Auger and Radiative Rates An extension of SUPERSTRUCTURE. Eissner et al. CPC 8, 220 (1972). Charlotte F. Fischer’s MCHF: Improved Atomic Structure and Energies. Charlotte Froese Fischer et al. CPC 176, 559 (2007).

Photobsorption: Atomic Physics Perspective I0=Source Intensity I =Observed Intensity σ = Absorption Cross Section N = Column Density n = Number / Volume Cross Section = Golden Rule Rate / (Poynting Vector/Photon Energy)

6/2/2016

Simplest K-Shell Photoabsorption: Neon Experiment : Coreno et al. (1999) Theory: Gorczyca (2000) Optical Potential R-matrix with Auger Broadening Participator Auger Decays Spectator Auger Decays Standard R-matrix vs R-matrix with Auger Broadening Experiment vs. Theory Excellent agreement with Experiment!

Ne : QDT Parameterization of Rydberg Series 9/21/2018

Ne Isonuclear Sequence and High Resolutions X-Ray… Photoabsorption Cross Sections X-Ray Spectra Ne Abundance in the ISM Intensity: I = I0 e-σN Column Density: N = ∫ n dx

X-Ray Spectra O Abundance in the ISM Best broadband fits with the TBnew model of the spectra toward eight Galactic low-mass X-ray binaries. For each source the observation with highestsignal-to-noise ratio is shown. E. Gatuzz et al. ApJ 790, 131 (2014) X-Ray Spectra O Abundance in the ISM

Carbon Cross Sections: ISM Modelling First detection of interstellar C II.

Mg I – X Isonuclear Sequence Cross Sections Mg VIII Mg II Hasoglu et al., ApJS 214, 8 (2014). Witthoeft et al. , ApJS, 182, 127 (2009). No Mg I, Mg II K-edge over estimated. Verner et al. (1993) _____ ____

Fe L-Edge and Si K-Edge Spectra Ne and O K-Edge Spectra vs. Fe L-Edge and Si K-Edge Spectra Atomic Si K Region: Solid-State Solid-State Molecular or Solid-State Oxygen Abundance? Atomic Silicon or Iron Abundance? Atomic

Chandra X-ray Observation for the Si K-edge Observed Si K edge region from Galactic Bulge source GX 3+1, with NH= 3.5 x 10 22 cm -2 Preliminary measurements of this source indicate a two-part edge, with solid silicate at 1.845 keV plus a contribution presumably from atomic Si at 1.839 keV from Norbert S. Schulz et al. ApJ 827:49 (2016).

Available Si K-edge Photoabsoprtion Cross Sections L. R. Corrales et al., MNRAS 458, 1345 (2016) : Si Dust cross section Astrophysics Modelling of Chandra Observations. S. T. Zeegers et al., A&A 599, A117 (2017) : Si (olivine) cross section per Si atom - Astrophysics Modelling of Chandra Observations and Experiment.

Theoretical R-Matrix Cross Sections for Si Atom

Atomic Si vs. Silicate Dust – Silicon Mineral

Fe L-Edge – Experiment for Solid State Fe Poor Man's shift, semi relativistic BP calculations are required and we are working on it. Solid Iron. Experiment near L-Edge for Solid Fe: Kortright, J. B. & Kim, S.-K. 2000, Phys. Rev. B, 62, 12216.

Fe L-Edge – Minimal R-Matrix in LS vs Exp. Poor Man's shift, semi relativistic BP calculations are required and we are working on it. Solid Iron.

Fe L-Edge – Minimal R-Matrix in LS vs Exp. Poor Man's shift, semi relativistic BP calculations are required and we are working on it. Solid Iron. Experiment near L-Edge for Solid Fe: Kortright, J. B. & Kim, S.-K. 2000, Phys. Rev. B, 62, 12216.

Multiphase Oxygen Photoabsorption Cross Sections O and O2 Gas H2O Gas 9/21/2018

Photoionization in Atoms: Photoionization in Solids: (XAFS)

H + Perturber: Modified K-Matrix Modified Amplitude

Analytic Behavior, H + Delta Function Perturber The cross section above threshold is modified by a factor that oscillates about unity, with an oscillation magnitude that depends on the ratio V0 /R2 and also the Coulomb amplitudes sl(R) and cl(R). The cross section below threshold is now split into two Rydberg series, one at the unperturbed positions ν = n and a second series at ν = n-μ0 ; for weak perturbations V 0 /R2 << 1, most of the oscillator strength remains in the original positions ν = n series, and the remainder is transferred into the second, quantum-defect-shifted series. More general case requires analytic transformation of K-matrices, from each scattering site, via Green’s function techniques – future work!

Acknowledgments Astrophysics Atomic Physics Funded by NASA APRA K. T. Korista, Western Michigan University T. R. Kallman, NASA Goddard Space Flight Center C. Mendoza, Western Michigan University M. A. Bautista, Western Michigan University J. Garcia, Cahill Center for Astronomy and Astrophysics (Caltech) E. Gatuzz, Centro de Fisica, Instituto Venezolano de Investigaciones Cientificas J. J. Drake, Harvard-Smithsonian Center for Astrophysics Norbert Schulz, MIT/Kavli Atomic Physics S. T. Manson, Georgia State University B. M. McLaughlin, Queen’s University Belfast Funded by NASA APRA Consulting with Manson and Brendan

WMU Graduate Students in Theoretical Atomic Physics