1. Pedro F. Guillén. "Why do people have to make things so complicated? Science is trying to make it simple" - Paco Beretta

3.  I AM NOT THE EXEPERT: I aim (at least try) to describe this EXAFS method. And the main result of the paper I’ve chosen for this Journal Club.  However, at the end of the talk I suggest the audience to establish a discussion about this new discovery.

4. Sco X-1, X-ray source. Interstellar medium, dust XMM-Newton Spectrum

5.  X-ray diffraction  Long-range crystalline order. X-ray diffuse scattering Short range order, info on alloys, vibrations, etc. Sees all possible atom pairs X-ray reflectivity (or reflectometry) Measure specular-reflected beam intensity as function of incidence angle. Reveals electron density as function of depth near surface or interface. X-ray absorption spectroscopy (XAS) …

6.  X-ray interacts with all electrons in matter when its energy exceeds the binding energy of the electron.  X-ray excites or ionizes the electron to a previously unoccupied electronic state (bound, quasi bound or continuum). The study of this process is XAS  Since the binding energy of core electrons is element specific, XAS is element and core level specific (e.g. Si K-edge at 1840 eV is the 1s electronic excitation threshold of silicon)  Extended X-ray Absorption Fine Structure (EXAFS)  X-ray Absorption Near Edge Structure (XANES) Photoelectric effect.

7. The measured spectrum is an average of the “snapshot” spectra (~10-15 sec) of all the atoms of the selected type that are probed by the x-ray beam In general XAFS determines the statistical moments of the distribution of atoms relative to the central absorbers. –This information is encoded in the (chi) function: ( = absorption for isolated or embedded atom)

8. Modulations in encode information about the local structure. function represents the fractional change in the absorption coefficient that is due to the presence of neighboring atoms. Variations in x-ray absorption coefficient as function of energy related to structural or electronic properties of sample

9. Absorbed x-ray photon induces transition of electron to unfilled final state of appropriate symmetry. * Bound states for low energies near absorption edge Wave characterized by electron wavenumber

10. tt XANES (NEXAFS) 1s to LUMO EXAFS Near edge Si(CH3)4 Tetramethylsilane Si K-edge C Si

11. Mass absorption cross section is often expressed in barn/atom or cm 2 /g; (1 barn = 10 -24 cm 2 ) absorption coefficient (cm -1 ) mass absorption cross section (cm 2 /g) density (g/cm 3 ) Note: µ or  is a function of photon energy incident photon flux transmitted flux t = thickness IoIo ItIt “He couldn't hit the broad side of a barn”

12. Transmission: % of incident photons transmitted for a given thickness of a uniform sample: E.g. the transmission of 1000 eV photon through a 1 micron (10 –4 cm) graphite film(normal incidence) is density of graphite mass abs. coeff.

13. 13 One-absorption length (hv): the thickness of the sample t1, such that  t =1 or t1 =1/µ E.g. the one absorption length of graphite at 1000 eV is One absorption length corresponds to 37% transmission, 63% absorption

14. 14 This is also known as the 1/e attenuation length or simply attenuation length by which the incident photon flux has been attenuated to 1/e = 0.368 or 36.8 % of its intensity. One absorption length is often used as an optimum length for the thickness of the sample in XAFS measurement for best signal to noise ratio

15. 15 This provides info. about sample depth Element Density Energy Mass abs. Coeff. One-abs. length (g/cm 3 ) (eV) (cm 2 /g) ( μ m) Si 2.33 1840 (K) 3.32 x 10 3 1.3 100 (L 3,2 ) 8.6 x 10 4 0.05 30 (VB) 1.4 x 10 4 0.28 C(graphite) 1.58 300 (K) 4.01 x 10 4 0.16 30 (VB) 1.87 x 10 5 0.034 Au 12000 (L3) 1.796X10 2 2.88

16. 16  Each element has its set of absorption edges (energy) and decay channels characteristic of the element.  Excitation channel specific (multi dimensional info) dipole selection rules, symmetry  Sensitive to chemical environment (molecular potential)  Tunability, high brightness, microbeam, polarization, time structure etc. provide many unprecedented capabilities for materials analysis

17. 17 Low z elements: all levels are accessible with VUV (vacuum UV, 30 – 1000 eV) and soft X-rays (1000 – 5000 eV). In this region, absorption is the dominant process (measurement in high vacuum environment) High z elements: deeper core levels are only accessible with hard X-rays (5 KeV to 40 keV). (measurements can be made in the ambient atmosphere) The absorption characteristics and the periodic table of the elements

19.  Sco X-1 is one of the brightest X-ray sources in the sky, and its emission is subject to interstellar absorption. It is located at a distance of about 2.8 kpc (Bradshaw et al. 1999) at a galactic latitude of 23.8 ◦, which means the source is situated about 1.1 kpc above the galactic plane.

20.  The XMM-Newton satellite was employed.  Instrument: Reflection Grating Spectrometer.  It provides high-resolution X-ray spectra in the soft energy band (6−38 Å). In this energy band the predominant interstellar absorption features are caused by the elements oxygen, nitrogen, neon, and iron.

28.  In the X-ray spectrum of Sco X-1, the Oxygen-K edge was searched for the existence of EXAFS, which indicate the presence of solids in the absorbing medium. A clear signal was found. When comparing with spectra of Mrk 421, it is found that instrumental effects may account for 40% of the signal. Assuming that EXAFS signals scale with that of water ice, we find roughly 30−50% of the absorbing oxygen is bound in solid material. Although amorphous water ice, does fit the EXAFS peaks found, this material is an unlikely candidate given the diffuse character of the absorbing medium. The data presented here can help solve the character of interstellar dust grains when appropriate laboratory data on various plausible materials become available.