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  • Inorganic Chemistry  (5)
  • ASTROPHYSICS  (4)
  • Condensed Matter: Electronic Properties, etc.
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  • 1990-1994  (4)
  • 1985-1989  (5)
  • 1
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Berichte der deutschen chemischen Gesellschaft 122 (1989), S. 2209-2209 
    ISSN: 0009-2940
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
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  • 2
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 608 (1992), S. 33-42 
    ISSN: 0044-2313
    Keywords: Diacylphosphines ; Di-cyclohexoylposphine ; Diadamant-1-oylphosphine ; keto-enol tautomerism ; NMR-parameters, thermodynamic data ; X-ray structure determination ; very short O‥H‥O bridge ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Acyl- and Alkylidenephosphines. XXXII. Di-cyclohexoyl- and Diadamant-1-oylphosphine - Keto-Enol Tautomerism and StructureLithium dihydrogenphosphide · DME (1) [12] and cyclo-hexoyl or adamant-1-oyl chloride react in a molar ratio of 3:2 to give lithium di-cyclo-hexoylphosphide · DME and the corresponding diadamant-1-oylphosphide.2THF (1) resp. Treatment of these two compounds with 85% tetrafluoroboric acid. diethylether adduct yields di-cyclo-hexoyl- (1b) and diadamant-1-oylphosphine (1c). In nmr spectroscopic studies 1b over a range of 203 to 343 K, a strong temperature dependence of the keto-enol equilibrium is found; thermodynamic data characteristic for the formation of the enol tautomer (ΔH0 = -4.3 kJ. mol-1; ΔS0 = -9.2 J. mol-1. K (-1) are compared of 1,3-diketones.The enol tautomer of diadamant-1-oylphosphine (E-1c) as obtained from a benzene solution in thin colourless plates, crystallizes in the monoclinic space group P21/c {a = 722.2(2); b = 1085.5(4); c = 2434.8(5) pm; ß = 96.43(2)° at -100 ± 3°C; Z = 4}. An X- ray structure analysis (Rw = 0.033) shows bond lengths and angles to be almost identical within the enolic system (P—C 179/180; C—O 130/129; C—C(adamant-1-yl) 152/153 pm; C—P—C 99°; P—C—O 124°/124°; P—C—C 120°/120°; C—C—O 116°/116°. The geometry of the very strong, but probably asymmetric O‥H‥O bridge is discussed (O—H 120/130, O‥O 245 pm).
    Notes: Aus Lithium-dihydrogenphosphid · DME (1) [12] und cyclo-Hexoyl- bzw. Adamant-1-oyl-chlorid im Molverhältnis 3:2 zugängliches Lithium-di-cyclo-hexoylphosphid · DME und -diadamant-1-oylphosphid · 2THF 1) reagieren mit 85proz. Tetrafluoroborsäure · Diethylether-Addukt zu Di-cyclo-hexoyl- 1b) und Diadamant-1-oylphosphan (1 c). Die Lage des Keto-Enol-Gleichgewichts zwischen 203 und 343 K sowie thermodynamische Daten zur Bildung des Enol-Isomers ΔH0= -4,3kJ.Mol-1; ΔS0;=-9,2 J · mol-1 · K-1 () wurden NMR-spektroskopisch an einer 2 M Lösung des bei +20°C flüssigen Di-cyclo-Hexoyl-Derivates 1b in d8-Toluol ermittelt und mit Werten von 1,3-Diketonen verglichen.Das farblose, sich aus Benzol in dünnen Plättchen abscheidende Enol-Tautomer des Diadamant-1-oylphosphans (E-1 c) kristallisiert monoklin in der Raumgruppe P21/c {a = 722,2(2) b = 1085,5(4); c = 2434,8(5) pm; ß = 96,43(2)° bei - 100 ± 3°C; Z = 4}. Nach den Ergebnissen der Röntgenstrukturanalyse (Rw=0,033) weist das Molekül in beiden des Hälften des Enolrings nahezu identische Bindungslängen und -winkel auf P—C 179/180; C—O 130/129; C—C(Adamant-1-yl) 152/153 pm; C—P—C 99°; P—C—O 124°/124°; P—C—C 120°/120°; C—C—O 116°/116°. Die Geometrie der sehr starken, aber vermutlich asymmetrischen O‥H‥O-Brücke wird diskutiert (O—H 120/130; O‥O 245 pm).
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  • 3
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 553 (1987), S. 239-247 
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Reactions of elemental Sulfur with Halogenated MethanesAt 250°C a reaction between CCl4 and sulfur forms S2Cl2 and CS2 (besides small amounts of S3Cl2 and S4Cl2). CHCl3 and sulfur above 200°C under catalytic influence of AlCl3 are forming HCl, S2Cl2, and CS2; CH2Cl2 and sulfur also are reacting (with AlCl3 or AI as catalyst) to CS2 and HCl. Only at 345°C one gets,CS2, HCl, and H2S from CH3Cl and sulfur. At 160°C forms HBR,BR2, and CS2. Aluminium is necessary for the reaction of CH2Br2 at 250°C with sulfur, forming CS2 and HBr. A mixture of products (CS2,H2S, HBr, CH3SCH3, and (CH3)3SBr) results from CH3 Br and sulfur at 250°C. CH3I and sulfur produce CS2,I2, and H2S at 145°C. The same products are formed from CH2I2 and sulfur with aluminium as catalyst at 175°C.
    Notes: CCl4 reagiert bei 250°C mit Schwefel zu S2Cl2 und CS2 (neben wenig S3Cl2 und S4Cl2). Aus CHCl3 und Schwefel bilden sich oberhalb 200°C unter AlCl3-Katalyse HCl, S2Cl2 und Cs2. CH2Cl2 und Schwefel liefern (wieder mit AlCl3 bzw. auch Al) CS2 und HCl. CH3Cl reagiert mit Schwefel erst oberhalb 345°C zu CS2, HCl und H2S. CBr4erst ab 245°C mit Schwefel zu HBR, Br2un 1 CS2 umsetzt. CH2BR2 benötigt bei 250°C wieder Aluminium als Katalysator, um mit Schwefel CS2 und HBr zu bilden. CH3Br reagiert mit Schwefel bei 250° zu einem nicht genau definierten Produktgemisch aus CS2, H2S, HBr, Ch3SCH3 und (CH3)3 SBr. Aus CHI3 und Schwefel erhält man bei 145°C CS2,i2 undH2S, ebenso wie aus CH2I2 und Schwefel, allerdings nur unter Aluminiumkatalyse bei 175°C.
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  • 4
    ISSN: 0044-2313
    Keywords: Lithium bis(2,2-dimethylpropionl)arsenide · DME ; tetrakis(2,2-dimethylpropionyl)diarsine ; X-ray structure determination ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Acyl- and Alkylidenearsines VII Synthesis and Structure of Tetrakis(2,2-dimethylpropionyl)diarsineLithium dihydrogenarsenide and 2,2-dimethylpropionyl chloride in a molar ratio of 3:2 react at -40 to -50°C in tetrahydrofuran or 1,2-dimethoxyethane to give the corresponding etherate of lithium bis(2,2-dimethylpropionyl)arsenide (2a). Treatment of these solutions with stoichiometric amounts of 85% tetrafluoroboric acid · diethylether adduct yields yelloworange tetrakis(2,2-dimethylpropionyl)diarsine (5) in 64 or 62% yield resp., but not the expected bis (2,2-dimethylpropionyl)arsine (4a). The very air-sensitive compound crystallizes in the monoclinic space group P21/n {-100 ± 3° C; a = 1224.6(3); b = 1419.7(3); c = 1333.1(3) pm; β = 96.22(2)°; Z = 4}. According to the X-ray structure analysis (Rw = 0.036) the molecule shows synclinal conformation; the two diacylarsyl-subunits are twisted against one another by an angle of 86°. As in another acylarsine [1] the As—C distances (203 to 205 pm) were found to be significantly longer then the standard value of 196 pm. Further characteristic bond lengths and angles are: As- 242; C—O 120 to 121 pm; As—As—C 88 to 107°; As—C—O 118 to 122°
    Notes: Wird das jeweilige, aus Lithiumdihydrogenarsenid und 2,2-Dimethylpropionylchlorid im Molverhältnis 3:2 bei -40 bis -50°C in TetrahydrofuranTetrahydrofuran (THF); 1,2-Dimethoxyethan (DME); Bis( 1,2-dimethylamino)ethan (TMEDA); Tetramethylsilan (TMS). oder 1,2-Dimethoxyethan gebildete, aber nicht isolierte Etherat des Lithium-bis(2,2-dimethypropionyl)arsenids (2a) mit 85proz. Tetrafluorborsäure · Diethylether-Addukt weiter umgesetzt, so erhält man nach der üblichen Aufarbeitung des Ansatzes nicht Bis(2,2-dimethylpropionyl)arsan (4a), sondern mit 64- bzw. 62proz.Ausbeute Tetrakis(2,2-dimethylpropionyl)diarsan (5). Die äußerst oxydationsempfindliche gelborange Verbindung kristallisiert monoklin in der Raumgruppe P21/n {-100 ± 3° C; a = 1224,6(3); b = 1419,7(3); c = 1333,1(3)pm; β = 96,22(2)°; Z = 4}. Nach den Ergebnissen der Röntgenstrukturanalyse (Rw = 0,036) weist das Molekül mit zwei um 86° gegeneinander verdrehten Hälften die synclinale Konformation auf; die As—C-Abstände liegen mit 203 bis 205 pm wie in einem anderen Acylarsan [1] deutlich über dem Standard von 196 pm. Weitere Charakteristische Bindungslängen und -winkel sind: As—As242; C—O 120 bis 121 pm; As—As—C 88 bis 107°; As—C—O 118 bis 122°.
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  • 5
    ISSN: 0044-2313
    Keywords: Dicopper trihydroxide nitrite ; crystal structure ; i.r., Raman spectra ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Lattice Vibration Spectra. LXXVI. On Basic Copper Salts  -  Crystal Structure, IR and Raman Spectra of Cu2(OH)3NO2Single-crystal X-ray as well as IR and Raman data of Cu2(OH)3NO2 are presented and discussed with respect to an order-disorder (OD) phase transition and the strength of hydrogen bonds. Cu2(OH)3NO2 crystallizes pseudosymmetrically in the monoclinic space group P21/m (Z = 2, a = 562.22(4), b = 605.94(5), c = 663.55(4) pm and β = 95.415(5)°) forming a layered structure of edge-connected, elongated CuO6 octahedra (final R value 2.5% for 1047 symmetry averaged reflections with I ≥ 2.5 μ1). The NO2- ions are on a split position with dynamic disordering at ambient temperature. On temperature lowering the disorder is frozen out with a symmetry decrease to space group P21. The disorder of the NO2- ions causes four different arrangements of OH(2)- with different strengths of the H…O hydrogen bonds present OD stretching modes in the spectra of isotopically dilute samples 2628, 2535, 2435, and 2343 cm-1 at 90 K. The OH(1)- ions form weak H…N H-bonds to the lone-pair of the nitrogen atoms of the NO2- ions (vOD 2563 cm-1).
    Notes: Die Kristallstruktur sowie die IR- und Raman-Spektren von Cu2(OH)3NO2 werden mitgeteilt und im Hinblick auf eine Ordnungs-Unordnungs(OD)-Phasenumwandlung sowie die Stärke der vorhandenen Wasserstoffbrücken diskutiert. Das basische Nitrit kristallisiert pseudosymmetrisch in der monoklinen Raumgruppe P21/m (Z = 2, R = 2,5%, 1047 symmetriegemittelte Reflexe mit 1 〉 2,5 μ1). Cu2(OH)3NO2 bildet eine Schichtenstruktur kantenverknüpfter, gestreckter CuO6-Oktaeder. Die Nitritionen befinden sich auf einer Splitlage mit dynamischer Fehlordnung bei Raumtemperatur. Bei niedrigeren Temperaturen friert die Fehlordnung unter Bildung von NO2--Zick-Zack-Ketten und Symmetrieerniedrigung zu P21 aus. Aufgrund der Fehlordnung der NO2--Ionen ergeben sich für die OH(2)--Ionen vier verschiedene Anordnungen mit entsprechend unterschiedlich starken H-Brücken (H…O). Die OH(1)--Ionen bilden H…N-Wasserstoffbrücken zum freien Elektronenpaar des N-Atoms der NO2--Ionen.
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  • 6
    Publication Date: 2019-08-27
    Description: We report preliminary results from a program to identify optical counterparts of ROSAT sources in the North Ecliptic Pole (NEP) region. The most striking X-ray feature reported by Hasinger et al. (1991) is an extended low surface brightness region of X-ray emission. Within the two X-ray contours of highest count rate we find a cluster of galaxies at a redshift of 0.09 and an early-type galaxy at a redshift of 0.03. X-ray emission from these objects may provide an explanation for the observed X-ray morphology. We also find evidence that other X-ray sources in this region are coincident with clusters or groups of galaxies at redshifts between 0.08 and 0.09. The presence of at least five X-ray detected clusters or groups in this narrow redshift band within a 1.5 deg radius field seems to indicate the existence of a moderate redshift supercluster. The existence of these clusters will have major implications for the study of large-scale structure through X-ray surveys such as ROSAT.
    Keywords: ASTROPHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 259; 1; p. L9-L11.
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  • 7
    Publication Date: 2019-07-12
    Description: Images of the gravitational lens 2237+0305 acquired in good seeing have resolved the system into at least five components within the central few arsec of the object: the galaxy nucleus and four point sources in a ringlike formation approximately centered on the galaxy. It is found that the four point sources are distinctly bluer than the galaxy, but that they do not have identical colors. The observed configuration is well reproduced by a simple model that assumes that the four objects are images of the quasar and that the lens is a constant mass-to-light ratio, elliptical, de Vaucouleurs bulge.
    Keywords: ASTROPHYSICS
    Type: Astronomical Journal (ISSN 0004-6256); 95; 1619-162
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  • 8
    Publication Date: 2019-07-12
    Description: Moderate-resolution slit spectroscopy of the extended emission-line objects A1 and B1 located within 5 arcsec of the triple radio source 2016 + 112 shows that at least one is physically associated with the z = 3.273 quasar thought to be multiply imaged by a foreground galaxy. The data and theoretical models unanimously favor the identification of A1 and B1 with two separate clouds of ionized gas that lie within a few kiloparsecs of the primary A/B QSO and radio source. The available evidence does not support the view that they are multiple images of a single object or their classification as separate (companion) galaxies.
    Keywords: ASTROPHYSICS
    Type: Astronomical Journal (ISSN 0004-6256); 94; 12-15
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  • 9
    Publication Date: 2019-07-12
    Description: A survey for faint quasars has been conducted using slitless spectroscopy with the PFUEI at the 200 inch (5 m) telescope. The survey covers a total of 0.91 sq deg in 113 fields at galactic latitudes above 30 deg. Calibrated spectra in the range 4500-7200 A were obtained for more than 9000 objects. Emission-line candidates were selected on the basis of two criteria: the equivalent width must exceed 50 A, and the signal-to-noise ratio of the detection of the line versus the sky background should be larger than 7. Among 45 candidates so selected, subsequent slit spectroscopy confirmed 27 emission-line objects. Among these, 17 are emission-line galaxies with redshifts in the range 0.04-0.31, and 10 are quasars with redshifts between 0.91 and 2.66. The well-defined selection criteria for these objects, together with the distribution of rest frame equivalent widths of the emission lines, allow derivation of the area of sky covered as a function of the continuum limiting magnitude. The observed number of quasars in the redshift range 0.7-2.7 agrees well with that predicted by the luminosity function models published by Schmidt and Green in 1983. It is concluded that quasars with an absolute magnitude of M(B) = -25 suffer a redshift cutoff near or below a redshift of 3.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 306; 411-427
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