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  • Astrophysics  (4)
  • crystal structure  (3)
  • 1
    ISSN: 0044-2313
    Keywords: Phosphorus sulfides ; 31P NMR spectroscopy ; phosphorus sulfur melts ; tetra phosphorus hexasulfide ; crystal structure ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: The Molecular Composition of Solidified Phosphorus-Sulfur Melts and the Crystal Structure of β-P4S6Phosphorus sulfur melts were annealed for one week at 673 K and then quenched in ice water. The solids were dissolved in CS2 and the concentrations of phosphorus sulfides were determined by 31P NMR spectroscopy. Samples containing between 44 and 70 mol% sulfur dissolved completely in CS2. Between 0 and 42 mol% remains an insoluble residue of red phosphorus. Above 72 mol% it consisted of sulfur chains linked by phosphorus atoms. The solutions contained mainly the congruently melting compounds P4S3, P4S7, and P4S10 having maximum concentrations at their stoichiometric compositions. Other compounds P4Sn (n = 4-9) which decompose on heating, according to the phase diagram, were also found in surprisingly high concentrations. One of these was β-P4S6 which crystallizes in the monoclinic space group P21/c with the lattice parameters a = 702.4(2), b = 1 205.6(2), c = 1 148.9(6) pm and β = 103.4(2)°.Reaction of white phosphorus with sulfur was also investigated. In contrast to the results of previous authors, who described the system P4-S8 below 373 K as eutectic, we found that the elements reacted below this temperature.
    Notes: Phosphor-Schwefel-Schmelzen wurden eine Woche bei 673 K getempert und anschließend in Eiswasser abgeschreckt, dann in CS2 gelöst und die Konzentration der Phosphorsulfide mit Hilfe der 31P-NMR-Spektroskopie bestimmt. Proben mit Zusammensetzungen zwischen 44 und 70 Mol-% Schwefel lösten sich vollständig auf. Zwischen 0 und 42 Mol-% Schwefel traten als unlöslicher Rückstand roter Phosphor, oberhalb von 72 Mol-% Schwefel über Phosphoratome vernetzte Schwefelketten auf. Die löslichen Bestandteile waren hauptsächlich die kongruent schmelzenden Verbindungen P4S3, P4S7 und P4S10. Die maximalen Konzentrationen lagen bei den jeweiligen stöchiometrischen Zusammensetzungen. Andere P4Sn (n = 4-9) Verbindungen, deren Molekülkristalle sich beim Erwärmen peritektisch oder peritektoid zersetzen, wurden ebenfalls mit höheren Konzentrationen gefunden, dazu gehörte β-P4S6, das in der monoklinen Raumgruppe P21/c mit den Gitterkonstanten a = 702,4(2), b = 1 205,6(2), c = 1 148,9(6) pm und β = 103,4(2)° kristallisiert.Die Reaktion von weißem Phosphor mit Schwefel wurde ebenfalls untersucht. Im Gegensatz zu Angaben anderer Autoren, die das P4-S8-System unterhalb von 373 K als einfach eutektisch beschreiben, wurden in diesem Temperaturbereich Reaktionen zwischen den Komponenten beobachtet.
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  • 2
    ISSN: 0044-2313
    Keywords: Selenites ; hydrates ; X-ray ; IR ; crystal structure ; pseudosymmetry ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Polymorphic and Pseudosymmetrical Hydrates MSeO3 · H2O (M = Mn, Co, Ni, Zn, Cd)By crystallization from aqueous solutions of MSeO3 and M(HSeO3)2, the selenites MSeO3 · H2O (M = Mn, Co, Ni, Zn, Cd) were obtained and characterized by means of X-ray diffraction and IR-spectroscopy. The crystal structure of ZnSeO3 · H2O was determined. The IR spectra indicate that the hydrates are isotypic and contain H2O molecules of symmetry mm2. However, the X-ray data show different structure types with H2O molecules of site symmetry m or 1. CdSeO3 · H2O and MnSeO3 · H2O are isotypic (o.rh., MnSeO3 · D2O type). CoSeO3 · H2O (mon.) as well as the isotypic NiSeO3 · H2O and ZnSeO3 · H2O (mon.) form new structure types. These findings are discussed on the basis of the crystal structure of ZnSeO3 · H2O (P21/n, a = 477.9(1), b = 1319.4(5), c = 570.1(1) pm, β = 90.84(2)°, Z = 4, Dx = 3.886 g · cm-3, R = 0.035 for 722 reflections with I 〉 2σ1) and the local pseudosymmetry of its components, i.e., layers ∞2[ZnSeO3 · H2O] of ZnO6 octahedra sharing four equatorial vertices, SeO32- anions and H2O molecules.
    Notes: Durch Kristallisation aus MSeO3- und M(HSeO3)2-Lösungen wurden die Selenite MSeO3 · H2O (M = Mn, Co, Ni, Zn, Cd) erhalten und röntgenographisch sowie IR-spektroskopisch charakterisiert. Von ZnSeO3 · H2O wurde die Kristallstruktur bestimmt. Die IR-Spektren deuten auf Isotypie der Hydrate und H2O-Moleküle der Symmetrie mm2. Die Röntgenbeugungsdaten zeigen dagegen das Vorliegen verschiedener Strukturtypen mit H2O-Molekülen der Lagesymmetrie m oder 1. CdSeO3 · H2O und MnSeO3 · H2O sind isotyp (o.rh., MnSeO3 · D2O-Typ). CoSeO3 · H2O (mon.) sowie die isotypen NiSeO3 · H2O und ZnSeO3 · H2O (mon.) kristallisieren in neuen Strukturtypen. Diese Befunde werden auf der Basis der Kristallstruktur von ZnSeO3 · H2O (P21/n, a = 477,9(1), b = 1319,4(5), c = 570,1(1) pm, β = 90,84(2)°, Z = 4, Dx = 3,886 g · cm-3, R = 0,035 für 722 Reflexe mit I 〉 2σ1) und der lokalen Pseudosymmetrie ihrer Bausteine (Schichten ∞2[ZnSeO3 · H2O] aus vierfach eckenverknüpften ZnO6-Oktaedern, SeO32--Anionen und H2O-Moleküle) diskutiert.
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  • 3
    ISSN: 0044-2313
    Keywords: Hydrogen selenites ; crystal structure ; IR ; Raman heating ; thermal analysis ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: On the Hydrates M(HSeO3)2 · 4H2O (M = Mg, Co, Ni, Zn) - Crystal Structures, IR, Raman, and Thermoanalytical InvestigationsFrom aqueous solutions of M(HSeO3)2 single crystals of Mg(HSeO3)2 · 4H2O and of the hitherto unknown compounds Co(HSeO3)2 · 4H2O, Ni(HSeO3)2 · 4H2O and Zn(HSeO3)2 · 4H2O could be obtained. The crystal structures, X-ray powder, IR, Raman and thermoanalytical (DTA, TG, Raman heating) data are presented and discussed. The crystal data of the isotypic compounds are: monoclinic, space group C2/c, Z = 4, Mg: a = 1 464.6(2), b = 755.3(1), c = 1 099.9(1) pm, β = 126.59(1)°, V = 0.9769(1) nm3, Co: a = 1 462.5(2), b = 756.5(2), c = 1 102.2(2) pm, β = 126.53(1)°, V = 0.9798(2) nm3, Ni: a = 1 452.2(2), b = 751.0(1), c = 1 091.5(1) pm, β = 126.28(1)°, V = 0.9595(1) nm3, Zn: a = 1 468.3(2), b = 755.8(1), c = 1 103.1(1) pm, β = 126.79(1)°, V = 0.9804(2) nm3. The crystal structures consist of hexagonal packed [M(HSeO3)2 · 2H2O]n chains of [MO4(H2O)2] octahedra linked by Se atoms. They contain trigonal pyramidal SeO2OH-ions with “free” hydroxyl groups and also “free” molecules of water of crystallization. The hydroxyl groups build strong H-bonds (O—H … O distances: 265-268 pm). The IR spectra show AB doublett bands in the OH stretching mode region of the hydroxyl groups. The water molecules of crystallization are linked to planar (H2O)4 tetramers by H-bonds with unusually short O—H … O bond distances of 271-273 pm. DTA and TG measurements indicate that thermal decomposition results in the direct formation of the respective diselenite MSe2O5. Raman heating measurements show under quasi static conditions the intermediate formation of the anhydrous hydrogen selenites.
    Notes: Aus M(HSeO3)2-Lösungen konnten erstmals Einkristalle von Mg(HSeO3)2 · 4H2O sowie die bisher nicht bekannten Verbindungen Co(HSeO3)2 · 4H2O, Ni(HSeO3)2 · 4H2O und Zn(HSeO3)2 · 4H2O erhalten werden. Die Kristallstrukturen, Röntgenpulverdaten, IR- und Raman-Spektren sowie die Ergebnisse thermoanalytischer (DTA, TG, Raman-Heizaufnahmen) Untersuchungen werden mitgeteilt und diskutiert. Die Kristalldaten der isotypen Verbindungen sind: monoklin, Raumgruppe C2/c, Z = 4, Mg: a = 1 464,6(2), b = 755,3(1), c = 1 099,9(1) pm, β = 126,59(1)°, V = 0,9769(1) nm3, Co: a = 1 462,5(2), b = 756,5(2), c = 1 102,2(2) pm, β = 126,53(1)°, V = 0,9798(2) nm3, Ni: a = 1 452,2(2), b = 751,0(1), c = 1 091,5(1) pm, β = 126,28(1)°, V = 0,9595(1) nm3, Zn: a = 1 468,3(2), b = 755,8(1), c = 1 103,1(1) pm, β = 126,79(1)°, V = 0,9804(2) nm3. Die Kristallstrukturen bestehen aus hexagonal gepackten [M(HSeO3)2 · 2H2O]n-Ketten Se-verbrückter [MO4(H2O)2]-Oktaeder. Sie enthalten trigonal pyramidale SeO2OH--Ionen mit „freien“ Hydroxylgruppen und „freie“ Kristallwassermoleküle. Die Hydroxylgruppen bilden starke H-Brücken (O—H … O-Abstände: 265-268 pm). Die IR-Spektren zeigen im Bereich der OH-Streckschwingungen der Hydroxylgruppen AB-Doublett-Banden. Die Kristallwassermoleküle sind zu planaren (H2O)4-Tetrameren mit ungewöhnlich kurzen O—H … Ow-Abständen (271 - 273 pm) H-verbrückt. Die thermische Zersetzung führt nach DTA- und TG-Messungen direkt zum jeweiligen Diselenit MSe2O5. Mittels Raman-Heizaufnahmen unter Quasi-Gleichgewichtsbedingungen konnte erstmals die intermediäre Bildung wasserfreier Hydrogenselenite beobachtet werden.
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  • 4
    Publication Date: 2019-07-31
    Description: A millimeter-wave survey over half the sky, that spans frequencies in the range of 30 to 350 gigahertz, and that is both an order of magnitude deeper and of higher-resolution than currently funded surveys would yield an enormous gain in understanding of both fundamental physics and astrophysics. By providing such a deep, high-resolution millimeter-wave survey (about 0.5 microK-arcminutes noise and 15 arcseconds resolution at 150 gigahertz), CMB-HD (Cosmic Microwave Background - Henry Draper catalog entry) will enable major advances. It will allow 1) the use of gravitational lensing of the primordial microwave background to map the distribution of matter on small scales (k approximately equal to 10 h per megaparsec), which probes dark matter particle properties. It will also allow 2) measurements of the thermal and kinetic Sunyaev-Zeldovich effects on small scales to map the gas density and gas pressure profiles of halos over a wide field, which probes galaxy evolution and cluster astrophysics. In addition, CMB-HD would allow us to cross critical thresholds in fundamental physics: 3) ruling out or detecting any new, light (less than 0.1 electronvolts), thermal particles, which could potentially be the dark matter, and 4) testing a wide class of multi-field models that could explain an epoch of inflation in the early Universe. Such a survey would also 5) monitor the transient sky by mapping the full observing region every few days, which opens a new window on gamma-ray bursts, novae, fast radio bursts, and variable active galactic nuclei. Moreover, CMB-HD would 6) provide a census of planets, dwarf planets, and asteroids in the outer Solar System, and 7) enable the detection of exo-Oort clouds around other solar systems, shedding light on planet formation. The combination of CMB-HD with contemporary ground and space-based experiments will also provide powerful synergies. CMB-HD will deliver this survey in 5 years of observing 20,000 square degrees, using two new 30-meter-class off-axis cross-Dragone telescopes to be located at Cerro Toco in the Atacama Desert. The telescopes will field about 2.4 million detectors (600,000 pixels) in total. The CMB-HD survey will be made publicly available, with usability and accessibility a priority.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN70476
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  • 5
    Publication Date: 2019-10-23
    Description: The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form (SO-Nominal) consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating (Stage 3) experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4. Construction of SO-Nominal is fully funded, and operations and data analysis are funded for part of the planned five-year observations. We will seek federal funding to complete the observations and analysis of SO-Nominal, at the $25M level. The SO has a low risk and cost efficient upgrade path the 6 m LAT can accommodate almost twice the baseline number of detectors and the SATs can be duplicated at low cost. We will seek funding at the $75M level for an expansion of the SO (SO-Enhanced) that fills the remaining focal plane in the LAT, adds three SATs, and extends operations by five years, substantially improving our science return. By this time SO may be operating as part of the larger CMB-S4 project. This white paper summarizes and extends material presented in, which describes the science goals of SO-Nominal, and which describe the instrument design.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN74208
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  • 6
    Publication Date: 2019-07-13
    Description: We report a measurement of the power spectrum of cosmic microwave background (CMB) lensing from two seasons of Atacama Cosmology Telescope polarimeter (ACTPol) CMB data. The CMB lensing power spectrum is extracted from both temperature and polarization data using quadratic estimators. We obtain results that are consistent with the expectation from the best-fit Planck CDM model over a range of multipoles L 80-2100, with an amplitude of lensing A(sub lens) = 1.06 +/- 0.15 stat +/- 0.06 sys relative to Planck. Our measurement of the CMB lensing power spectrum gives sigma 8 omega m(sup 0.25) = 0.643 +/- 0.054; including baryon acoustic oscillation scale data, we constrain the amplitude of density fluctuations to be sigma 8 = 0.831 +/- 0.053. We also update constraints on the neutrino mass sum. We verify our lensing measurement with a number of null tests and systematic checks, finding no evidence of significant systematic errors. This measurement relies on a small fraction of the ACTPol data already taken; more precise lensing results can therefore be expected from the full ACTPol data set.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN44620 , Physical Review D (ISSN 1550-7998) (e-ISSN 1089-4918); 95; 12; 123529
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  • 7
    Publication Date: 2019-10-23
    Description: A millimeter-wave survey over half the sky, that spans frequencies in the range of 30 to 350 GHz, and that is both an order of magnitude deeper and of higher-resolution than currently funded surveys would yield an enormous gain in understanding of both fundamental physics and astrophysics. By providing such a deep, high-resolution millimeter-wave survey (about 0.5 Karcmin noise and 15 arcsecond resolution at 150 GHz), CMB-HD will enable major advances.It will allow 1.) the use of gravitational lensing of the primordial microwave background to map the distribution of matter on small scales (k 10 hMpc1), which probes dark matter particle properties. It will also allow 2.) measurements of the thermal and kinetic Sunyaev-Zel'dovich effects on small scales to map the gas density and gas pressure profiles of halos over a wide field,which probes galaxy evolution and cluster astrophysics. In addition, CMB-HD would allow us to cross critical thresholds in fundamental physics: 3.) ruling out or detecting any new, light (〈 0:1 eV), thermal particles, which could potentially be the dark matter, and 4.) testing a wide class of multi-field models that could explain an epoch of inflation in the early Universe. Such a survey would also 5.) monitor the transient sky by mapping the full observing region every few days,which opens a new window on gamma-ray bursts, novae, fast radio bursts, and variable active galactic nuclei. Moreover, CMB-HD would 6.) provide a census of planets, dwarf planets, andasteroids in the outer Solar System, and 7.) enable the detection of exo-Oort clouds around othersolar systems, shedding light on planet formation. The combination of CMB-HD with contemporaryground and space-based experiments will also provide powerful synergies. CMB-HD willdeliver this survey in 5 years of observing 20,000 square degrees, using two new 30-meter-classoff-axis cross-Dragone telescopes to be located at Cerro Toco in the Atacama Desert. The telescopeswill field about 2.4 million detectors (600,000 pixels) in total. The CMB-HD survey willbe made publicly available, with usability and accessibility a priority.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN74211
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