Suchergebnisse

Chau, Tsz Kin. ; "December 2011." ; Thesis (M.Phil.)--Chinese University of Hong Kong, 2012. ; Includes bibliographical references. ; Abstracts in English and Chinese. ; Introduction --- p.1 ; Chapter Chapter 1 --- Who's Pan Yuliang? Whose Pan Yuliang? --- p.7 ; Who's Pan Yuliang? --- p.7 ; Life and Art of Pan Yuliang: Existing Account --- p.12 ; Whose Pan Yuliang? --- p.22 ; "Summary of Existing Accounts: Biography, Oedipus complex and Narcissism" --- p.30 ; Chapter Chapter 2 --- Reconsidering Pan Yuliang --- p.33 ; Academic works in Mainland China and Taiwan since 2000 --- p.33 ; Theorizing the Woman Painter --- p.42 ; Background I: Modern Art in Republican China --- p.54 ; Background II: Paris Modernism --- p.60 ; Chapter Chapter 3 --- Expanding Biography into History --- p.63 ; Chapter Chapter 4 --- The Political Xiesheng and its Gender Politics --- p.82 ; "Pan Yuliang: from Shanghai (1928-32, 36-37) to Nanjing (1933-35)" --- p.83 ; The Mission ofNanjang: National Administering of Modernism --- p.86 ; Pan Yuliang and the Chinese Arts Association --- p.97 ; Xiesheng and a New Woman/painter Subject --- p.113 ; Conclusion: a Different Modern for a Woman Painter --- p.123 ; Chapter Chapter 5 --- Differencing the Modern and Women's Culture --- p.127 ; Theorizing Women's Culture --- p.130 ; Pan Yuliang and Women's Community --- p.134 ; Contextualizing Women's Community: Republican Modernity and Post-war ; Pacifism --- p.137 ; Conclusion: Women's Art and Modernism --- p.145 ; Conclusion Rethinking Republican and Women's Art --- p.146 ; Appendix --- p.150 ; Glossary --- p.158 ; Graphical Materials --- p.165 ; Bibliography --- p.251

Anti-imperialistic articles, mostly reprinted from the European edition of the New York herald, 1898 to 1905. ; Mode of access: Internet.

Anti-imperialistic articles, mostly reprinted from the European edition of the New York Herald, 1898 to 1902. ; Mode of access: Internet.

Bright and eclipsing, the high-mass X-ray binary Vela X-1 offers a unique opportunity to study accretion onto a neutron star from clumpy winds of O/B stars and to disentangle the complex accretion geometry of these systems. In Chandra-HETGS spectroscopy at orbital phase 0.25, when our line of sight towards the source does not pass through the large-scale accretion structure such as the accretion wake, we observe changes in overall spectral shape on timescales of a few kiloseconds. This spectral variability is, at least in part, caused by changes in overall absorption and we show that such strongly variable absorption cannot be caused by unperturbed clumpy winds of O/B stars. We detect line features from high and low ionization species of silicon, magnesium, and neon whose strengths and presence depend on the overall level of absorption. These features imply a co-existence of cool and hot gas phases in the system, which we interpret as a highly variable, structured accretion flow close to the compact object such as has been recently seen in simulations of wind accretion in high-mass X-ray binaries. ; V.G. is thankful for support of her work through the ESA internal research fellowship. Part of this work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Support for this work was provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. I.E.M. acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie SkłlCodowska-Curie grant agreement No. 665501 with the Research Foundation Flanders (FWO). A.A.C.S. is supported by the Deutsche Forschungsgemeinschaft (DFG) under grant HA 1455/26. J.N. acknowledges support from NASA through the Hubble Postdoctoral Fellowship Program, grant HST-HF2-51343.001-A. S.M.N. acknowledges support by research project ESP2016-76683-C3-1-R. ; Peer Reviewed

Contiene: In The United States / Pearce Bailey. [et al.] -- In The American expeditionary forces / Thomas W. Salmon, Norman Fenton ; En: The Medical Department of The United States Army in the World War

Mixed crystals Cs1−x(NH4)xH2PO4 of the ferroelectric CsH2PO4 (CDP) and the antiferroelectric (NH4)H2PO4 were grown with x=0.2 (CADP0.2) in solution. The structural properties of the crystal were analyzed by means of x-ray diffraction. Dielectric measurements at several temperatures and frequencies have been performed along the three crystallographic axes in this sample and also in the fully deuterated CADP0.2 sample (DCADP0.2). NMR experiments were also performed. ; NSFgrantDMR-9520215; Basque Government under grant BFI96.041

arXiv:1302.6719v1 ; Luminosity functions are one of the most important observational clues when studying galaxy evolution over cosmic time. In this paper we present the X-ray luminosity functions for X-ray detected AGN in the SXDS and GWS fields. The limiting fluxes of our samples are 9.0 ×10-15 and 4.8 ×10-16 erg cm-2 s-1 in the 0.5-7.0 keV band in the two fields, respectively. We carried out analysis in three X-ray bands and in two redshift intervals up to z ≤ 1.4. Moreover, we derive the luminosity functions for different optical morphologies and X-ray types. We confirm strong luminosity evolution in all three bands, finding the most luminous objects at higher redshift. However, no signs of density evolution are found in any tested X-ray band. We obtain similar results for compact and early-type objects. Finally, we observe the >Steffen effect>, where X-ray type-1 sources are more numerous at higher luminosities in comparison with type-2 sources. ; This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant AYA2011-29517-C03-01. MP, IM, and JM acknowledge Junta de Andalucía and MINECO through projects PO8-TIC-03531 and AYA2010-15169. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). JIGS acknowledge financial support from the MINECO under project AYA2008-06311-C02-02 and AYA2011-29517-C03-02. JG acknowledges support from the MINECO through AYA2009-10368 project. The CEFCA is funded by the Fondo de Inversiones de Teruel, supported by both the Government of Spain (50%) and the regional Government of Aragón (50%). This work has been partially funded by the Spanish Ministerio de Ciencia e Innovación through the PNAYA, under grants AYA2006-14056 and th-rough the ICTS 2009-14. ; Peer Reviewed

Cen X−3 is a compact high-mass X-ray binary likely powered by Roche lobe overflow. We present a phase-resolved X-ray spectral and timing analysis of two pointed XMM–Newton observations. The first one took place during a normal state of the source, when it has a luminosity LX ∼ 1036 erg s−1. This observation covered orbital phases ϕ = 0.00–0.37, i.e. the egress from the eclipse. The egress light curve is highly structured, showing distinctive intervals. We argue that different intervals correspond to the emergence of different emitting structures. The light-curve analysis enables us to estimate the size of such structures around the compact star, the most conspicuous of which has a size ∼0.3R*, of the order of the Roche lobe radius. During the egress, the equivalent width of Fe emission lines, from highly ionized species, decreases as the X-ray continuum grows. On the other hand, the equivalent width of the Fe K α line, from near-neutral Fe, strengthens. This line is likely formed due to the X-ray illumination of the accretion stream. The second observation was taken when the source was 10 times X-ray brighter and covered the orbital phases ϕ = 0.36–0.80. The X-ray light curve in the high state shows dips. These dips are not caused by absorption but can be due to instabilities in the accretion stream. The typical dip duration, of about 1000 s, is much longer than the time-scale attributed to the accretion of the clumpy stellar wind of the massive donor star, but is similar to the viscous time-scale at the inner radius of the accretion disc. ; This research has been supported by the project ESP2017-85691-P. LMO acknowledges Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50 OR 1508 and partial support by the Russian Government Program of Competitive Growth of Kazan Federal University. JJRR acknowledges financial support from the Spanish Ministry of Education, Culture and Sport fellowship PRX17/00114, and also thanks all the staff from SRON for their collaboration and hospitality there. KP acknowledges support from Russian Foundation for Basic Research (RFBR) grant 18-502-12025.

Aql X-1 is one of the best-studied neutron star low-mass X-ray binaries. It was previously targeted using quasi-simultaneous radio and X-ray observations during at least seven different accretion outbursts. Such observations allow us to probe the interplay between accretion inflow (X-ray) and jet outflow (radio). Thus far, these combined observations have only covered one order of magnitude in radio and X-ray luminosity range; this means that any potential radio-X-ray luminosity correlation, L ∝ L, is not well constrained (β ≈ 0.4-0.9, based on various studies) or understood. Here we present quasi-simultaneous Very Large Array and Swift-XRT observations of Aql X-1's 2016 outburst, with which we probe one order of magnitude fainter in radio and X-ray luminosity compared to previous studies (6 × 10 erg s < L <3 × 10 erg s, i.e. the intermediate to low-luminosity regime between outburst peak and quiescence). The resulting radio non-detections indicate that Aql X-1's radio emission decays more rapidly at low X-ray luminosities than previously assumed - at least during the 2016 outburst. Assuming similar behaviour between outbursts, and combining all available data in the hard X-ray state, this can be modelled as a steep β =1.17 power-law index or as a sharp radio cut-off at L ≲ 5 × 10 erg s (given our deep radio upper limits at X-ray luminosities below this value). We discuss these results in the context of other similar studies. ; NVG acknowledges funding from Netherlands Research School for Astronomy (NOVA). JWTH acknowledges funding from an Netherlands Organisation for Scientific Research (NWO) Vidi fellowship and from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) / ERC Starting Grant agreement nr. 337062 ('DRAGNET'). The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by Commonwealth Scientific and Industrial Research (CSIRO). JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT140101082), funded by the Australian government. ND is supported by a Vidi grant from NWO.

The melting temperature, Tm, of YBa2Cu3O7−x and GdBa2Cu3O7−x superconductor ceramic compounds has been measured by differential thermal analysis (DTA) over a large oxygen partial pressure range of five orders of magnitude (2·10−5 < PO2 < 1 bar). It is shown that the DTA peak and endset temperatures are closer to Tm than the onset temperature. Correct measurement of Tm requires low heating rates and subatmospheric pressure conditions to avoid temperature shifts due to local oxygen overpressure and kinetic effects ; This work was funded by the Spanish Programa Nacional de Materiales through projects MAT2014-51778-C2-1-R and MAT2014-51778-C2-2-R. We also acknowledge: the Center of Excellence award Severo OchoaSEV-2015-0496, SGR753 and SGR948 from the Generalitat of Catalunya, the European Union through projects Eurotapes (EU-FP7 NMP-LA-2012-280432) and Ultrasupertape (ERC ADG-2014-669504), and the Universitat de Girona (MPCUdG2016/059)

The melting temperature, Tm, of YBa2Cu3O7−x and GdBa2Cu3O7−x superconductor ceramic compounds has been measured by differential thermal analysis (DTA) over a large oxygen partial pressure range of five orders of magnitude (2·10−5 < PO2 < 1 bar). It is shown that the DTA peak and endset temperatures are closer to Tm than the onset temperature. Correct measurement of Tm requires low heating rates and subatmospheric pressure conditions to avoid temperature shifts due to local oxygen overpressure and kinetic effects ; This work was funded by the Spanish Programa Nacional de Materiales through projects MAT2014-51778-C2-1-R and MAT2014-51778-C2-2-R. We also acknowledge: the Center of Excellence award Severo OchoaSEV-2015-0496, SGR753 and SGR948 from the Generalitat of Catalunya, the European Union through projects Eurotapes (EU-FP7 NMP-LA-2012-280432) and Ultrasupertape (ERC ADG-2014-669504), and the Universitat de Girona (MPCUdG2016/059)

The melting temperature, Tm, of YBa2Cu3O7−x and GdBa2Cu3O7−x superconductor ceramic compounds has been measured by differential thermal analysis (DTA) over a large oxygen partial pressure range of five orders of magnitude (2·10−5 < PO2 < 1 bar). It is shown that the DTA peak and endset temperatures are closer to Tm than the onset temperature. Correct measurement of Tm requires low heating rates and subatmospheric pressure conditions to avoid temperature shifts due to local oxygen overpressure and kinetic effects ; This work was funded by the Spanish Programa Nacional de Materiales through projects MAT2014-51778-C2-1-R and MAT2014-51778-C2-2-R. We also acknowledge: the Center of Excellence award Severo OchoaSEV-2015-0496, SGR753 and SGR948 from the Generalitat of Catalunya, the European Union through projects Eurotapes (EU-FP7 NMP-LA-2012-280432) and Ultrasupertape (ERC ADG-2014-669504), and the Universitat de Girona (MPCUdG2016/059)

The melting temperature, Tm, of YBa2Cu3O7 x and GdBa2Cu3O7 x superconductor ceramic compounds has been measured by differential thermal analysis (DTA) over a large oxygen partial pressure range of five orders of magnitude (2$10 5 < PO2 < 1 bar). It is shown that the DTA peak and endset temperatures are closer to Tm than the onset temperature. Correct measurement of Tm requires low heating rates and subatmospheric pressure conditions to avoid temperature shifts due to local oxygen overpressure and kinetic effects. ; This work was funded by the Spanish Programa Nacional de Materiales through projects MAT2014-51778-C2-1-R and MAT2014-51778-C2-2-R. We also acknowledge: the Center of Excellence award Severo Ochoa SEV-2015-0496, SGR753 and SGR948 from the Generalitat of Catalunya and European Union through projects Eurotapes (EU-FP7 NMP-LA-2012-280432) and Ultrasupertape (ERC ADG-2014-669504). FT acknowledges financial support from USTO. The authors are indebted to Dr. Joan Pere López Olmedo and Dr. Xavier Fontrodona of STR, University of Girona, for their technical assistance. ; Peer reviewed

1 sheet ([1] p.) ; Signed at end: H El., i.e. Henry Elsynge?. ; A satire on Pariament in the form of parodies of the Ten commandments, the Lord's prayer, and the Apostles' Creed. ; Imprint from Wing. ; Annotation on Thomason copy: "Jan: 25. 1647". ; Reproduction of the original in the British Library.

We present photometric redshifts for 1031 X-ray sources in the X-ATLAS field using the machine-learning technique TPZ. X-ATLAS covers 7.1 deg observed with XMM-Newton within the Science Demonstration Phase of the H-ATLAS field, making it one of the largest contiguous areas of the sky with both XMM-Newton and Herschel coverage. All of the sources have available SDSS photometry, while 810 additionally have mid-IR and/or near-IR photometry. A spectroscopic sample of 5157 sources primarily in the XMM/XXL field, but also from several X-ray surveys and the SDSS DR13 redshift catalogue, was used to train the algorithm. Our analysis reveals that the algorithm performs best when the sources are split, based on their optical morphology, into point-like and extended sources. Optical photometry alone is not enough to estimate accurate photometric redshifts, but the results greatly improve when at least mid-IR photometry is added in the training process. In particular, our measurements show that the estimated photometric redshifts for the X-ray sources of the training sample have a normalized absolute median deviation, nmad - 0.06, and a percentage of outliers, - = 10-14%, depending upon whether the sources are extended or point like. Our final catalogue contains photometric redshifts for 933 out of the 1031 X-ray sources with a median redshift of 0.9. ; The research leading to these results has received funding from the European Union's Horizon 2020 Programme under the AHEAD project (grant agreement No. 654215). G.M. acknowledges financial support from the AHEAD project, which is funded by the European Union as Research and Innovation Action under Grant No: 654215. F.J.C. and A.C.R. acknowledge financial support through grant AYA2015-64346-C2-1-P (MINECO/FEDER). A.C.R. also acknowledges financial support by the European Space Agency (ESA) under the PRODEX program. ; Peer Reviewed