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Sequential covalent transformation and metalation were performed on (Zn(4)O)(3)(BDC-NH(2))(3)(BTB)(4) with maintenance of crystallinity and porosity. Reaction of (Zn(4)O)(3)(BDC-NH(2))(3)(BTB)(4) with 2-pyridinecarboxaldehyde in toluene at room temperature for 5 days resulted in the formation of the extended crystalline structure (Zn(4)O)(3)(BDC-C(6)H(5)N(2))(3)(BTB)(4), which possesses iminopyridine moieties covalently bound to the organic links of the framework. Subsequent reaction with PdCl(2)(CH(3)CN)(2) in CH(2)Cl(2) at room temperature for 12 h yielded the metalated metal-organic framework (Zn(4)O)(3)(BDC-C(6)H(5)N(2)PdCl(2))(3)(BTB)(4). Both functionalized materials retained high crystallinity and were permanently porous with high surface areas [3200 and 1700 m(2) g(-1) for (Zn(4)O)(3)(BDC-C(6)H(5)N(2))(3)(BTB)(4) and (Zn(4)O)(3)(BDC-C(6)H(5)N(2)PdCl(2))(3)(BTB)(4), respectively.].
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Novel ruthenium and osmium silylene species containing Si-H bonds have been synthesized and characterized by NMR spectroscopy. The ruthenium complex [Cp*(iPr3P)(H)2Ru=Si(H)Ph.Et2O][B(C6F5)4] catalyzes the hydrosilyation of alkenes with excellent substrate selectivity for primary silanes and exclusive anti-Markovnikov regiochemistry. Evidence for a novel mechanism involving direct addition of an alkene to the silylene Si-H bond is presented.
view Abstract Citations (186) References (18) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Discovery of an Extremely Low Luminosity Seyfert 1 Nucleus in the Dwarf Galaxy NGC 4395 Filippenko, Alexei V. ; Sargent, Wallace L. W. Abstract We have discovered a Seyfert 1 nucleus in the center of the nearby (d ~ 2.6 Mpc), late-type (Sd III-IV), dwarf galaxy NGC 4395. Such nuclei have never been seen in galaxies of this kind. The optical spectrum reveals very strong, narrow emission lines covering a wide range of ionization from [O I] to [Fe X]. Weak wings having FWZI ~ 4000-8000 km s^-1^ are visible in the permitted-line profiles, including He II λ4686. H II regions in the rest of the galaxy have normal spectra. The luminosity of the broad Hα emission is ~ 1.2 x 10^38^ ergs s^-1^, a factor of 10 fainter than in the nucleus of M81; thus, NGC 4395 contains the least luminous known Seyfert 1 nucleus. The equivalent width of broad Hα (270 A) is similar to that in normal, luminous Seyfert 1 galaxies. The optical continuum is featureless, and has M_B_ ~ 9.8 mag--less luminous than the brightest known supergiant stars. It is possible that the nuclear properties of NGC 4395 can be explained in terms of stellar phenomena, rather than by accretion onto a black hole. Publication: The Astrophysical Journal Pub Date: July 1989 DOI: 10.1086/185472 Bibcode: 1989ApJ...342L..11F Keywords: Dwarf Galaxies; Galactic Nuclei; Light (Visible Radiation); Seyfert Galaxies; Stellar Luminosity; Emission Spectra; H Alpha Line; H Ii Regions; Line Spectra; Astrophysics; GALAXIES: INDIVIDUAL NGC NUMBER: NGC 4395; GALAXIES: NUCLEI; GALAXIES: SEYFERT; LINE PROFILES; SPECTROPHOTOMETRY full text sources ADS | data products SIMBAD (2) NED (2)
This paper provides a review on the optimal design of photonic bandgap structures by inverse problem techniques. An overview of inverse problems techniques is given, with a special focus on topology design methods. A review of first applications of inverse problems techniques to photonic bandgap structures and waveguides is given, as well as some model problems, which provide a deeper insight into the structure of the optimal design problems.
The location and bonding of atoms and molecules on surfaces is of great interest to surface chemists and to those interested in the application of surfaces through exploitation of their unique properties. These properties include chemical properties that give rise to selective adsorption and heterogeneous catalysis; mechanical properties that control adhesion, fric tion, slide, or fracture; electrical properties utilized in microelectronic circuitry and xerography; magnetic properties used in information storage on tape or disk drives; and optical properties that give rise to nonlinear effects such as second harmonic and sum frequency generation. During the past 25 years, over 50 new techniques have been developed that permit the investigation of surfaces on the molecular level (l). The ability to study surfaces with increased time and spatial resolution (and energy resolution, when applicable) controls the development of many surface technologies. The contributions of science push and surface technology pull have resulted in an exponential growth in the field of surface science and pro pelled it among the frontier fields of physical chemistry. Several new surface science techniques permit quantitative deter-