1. NEI Modeling What do we have? What do we need? 2012.08.09 AtomDB workshop Hiroya Yamaguchi (CfA) Fe ion population in CIE (AtomDB v.2.0.2) Temperature (keV) Fe 24+ Fe 25+ Fe 26+ Fe 16+ APED/APEC state-of-the-art dataset for He- & H-like ions of Z<=30 (+ DR lines of Fe) X-ray-emitting plasma: T = 10 6-8 K (0.1-10 keV) most of atoms are ionized to be He- or H-like states in CIE

2. Supernova Remnants = NEI !! E0102-72 H-dominant (solar abundance) matter heavy elements are neutral metal-rich, almost neutral Shock-heated electrons ionize heavy elements.  = n e t = 10 12 (cm -3 s) t = 30000 (n e /1cm -3 ) -1 yr

3. Supernova Remnants = NEI !! n e t (cm -3 s) Fe ion population in NEI (AtomDB v.2.0.2) Fe 24+ Fe 25+ Fe 26+ Fe 16+ kTe = 20 keV typical SNRs - Inner-shell process is essentially important for SNRs! - APEC can calculate ion population, but doesn’t output emission.

4. SNRs’ spectra of Fe K-shell band 9 3C397 (Type II) Kepler (Type Ia) Cr Mn Fe Ni Fe K  6.44 keV -> Fe XVII-XVIII (Palmeri+03) Ne-like neutral He-like RCW86 G272 SN1006 Tycho Kepler G344 0509 0519 N103B W49B CasA 3C397 G349 G292 G350 N132D

5. Innershell ionization of Be-like ions Li-like : 1s2s 2 ( 2 S) ->  K = 0 (for single-configuration wave function) in fact, K&M(1993) gave zero values for every Li-like ions. Configuration interaction (CI) effect cannot be ignored  CI = c 1 1s2s 2 ( 2 S) + c 2 1s2p 2 ( 2 S) ; c 2 ~ 0.3 (Gorczyca+2006)  K ≠ 0 ! Li-like (Gorczyca+06) Innershell process - Innershell ionization/excitation - Fluorescence or Auger (Kaastra & Mewe 93) … SPEX, XSPEC NEI v.1 # of electrons Fe K  a energy (Mendoza+04) K&M93 this work

6. Atomic data for emission above 5 keV Fe I-XVIXVII-XIVNi I-XVIIIXIX-XVICr, Mn A r, A a Palmeri+03a Mendoza+04 Gorczyca+03;06 Hasogle 08 (thesis) Palmeri+08aPalmeri+12 (K  ) Palmeri +03b (K  ) (not detected) x-sec (EII) phenomenological formula (Haque+06) x-sec (EIE) (IRON Project) Kris DR data for Fe e.g., Bautista & Badnell 07

7. Atomic data for emission below 5 keV A r, A a, (K  ) for all ionization states Palmeri+08b, Kucas+12: Ne, Mg, Si, S, Ar, Ca Palmeri+11: Al Palmeri+12: Na, Cl, Ti, Zn, etc.(Z <= 30) No longer need Kaastra & Mewe’s data Si XII Fe L S XIV Ar XVI Ca XVIII Fe Kepler Lighter elements are usually ionized to be He-like state. but a few exception… 0509-67.5: K  from low-ionized Si (Warren & Hughes 04) Tycho: low-ionized Ca (Hwang+98) Also needed: Si thru Ca (Ne-like – Li-like) and L-shell data for Fe, Ca, Ni, …

8. Recombining plasma RRC (Fe 25+ -> Fe 24+ ) Fe 24+ K  W49B (Ozawa+09) What’s the origin? - collision with dense stellar wind matter and following adiabatic cooling? (HY+09) - thermal conduction into cloudy matter? (Zhou+11) Abundance & density are important information.

9. Recombining plasma RRC (Fe 25+ -> Fe 24+ ) Fe 24+ K  W49B (Ozawa+09)  (recomb rate) : Badnell+06  = n Fe25+ / (n Fe26+ + n Fe25+ + n Fe24+ + …) We only know n Fe25+ /n Fe24+ from the RRC/line ratio…  0.06 in W49B) Fe ion population in CIE (Mazzotta+98) Temperature (keV) Fe 24+ Fe 25+ Fe 26+ Fe 16+ then, used  = 0.04 to estimate Fe abundance and density. We (wrongly) assumed that ion pop in arbitrary recomb plasma is consistent to that in CIE plasma with a certain electron temperature.

10. Recombining plasma n e t (cm -3 s) Fe 24+ Fe 25+ Fe 26+ Fe 16+ kT e = 0.5 keV temperature (keV) n e t (cm -3 s) CIE Ionizing Recombining plasma model in XSPEC must be useful. We do already have atomic data! Some difficulty… Ionizing: kT e, n e t, abundances, normalization Recombining: + initial ion population -> 3-dimensional

11. Summary Ionizing NEI plasma - APEC is ready. - Fluorescence data are completed for all elements (Z <=30)! except for K  lines from lowly-ionized atoms (Kaastra & Mewe’s is no longer needed.) - EII/EIE rates for Fe & Ni are calculated by Kris & collaborators! - EII/EIE rates for Cr & Mn would be mostly important now. - and other abundant elements, Si, S, Ca… Recombining plasma - APEC & APED are both (almost) ready. - one more parameter (init ion pop.) is needed.