On German Nationalism: Reply to Geulen
In: Telos: critical theory of the contemporary, Band 1995, Heft 105, S. 21-42
ISSN: 1940-459X
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In: Telos: critical theory of the contemporary, Band 1995, Heft 105, S. 21-42
ISSN: 1940-459X
World Affairs Online
In: Journal of marine engineering & technology, Band 5, Heft 1, S. 35-40
ISSN: 2056-8487
In: Social science quarterly, Band 69, Heft Jun 88
ISSN: 0038-4941
Social and geographic mobility have been shown to be associated for past immigrant groups in the United States. Moving up socially meant moving away from the community of origin. Examines the extent to which this thesis is true. Shows that there has been significant growth in suburban Hispanic populations and these populations in general are shown to be better educated and have higher incomes. (Abstract amended)
In: Peace research abstracts journal, Band 44, Heft 5, S. 237-243
ISSN: 0031-3599
In: Journal of marine engineering & technology, Band 6, Heft 2, S. 3-15
ISSN: 2056-8487
This is the author accepted manuscript ; To be competitive against other renewable energy sources, energy converted 1 from the ocean waves needs to reduce its associated levelised cost of energy. It has been proven that advanced control algorithms can increase power production and device reliability. They act throughout the power conversion chain, from the hydrodynamics of wave absorption to the power take-off to improve the energy yield. The present work highlights the development and test of several algorithms to control the biradial turbine which is to be installed in the Mutriku oscillating water column plant. A collection of adaptive and predictive controllers is explored and both turbine speed controllers and latching strategies are examined. AWave-to-Wire model of one chamber of the plant is detailed and simulation results of six control laws are obtained. The controllers are then validated using an electrical test infrastructure to prepare the future deployment in the plant. Finally, the control strategies are assessed against criteria like energy production, power quality or reliability. ; European Union's Horizon 2020
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This is the final version. Available from MDPI via the DOI in this record. ; The majority of Smartline data are available by registering interest at www.smartline.org.uk/main-content-area/data-access (accessed on 8 January 2021). ; In response to the COVID-19 outbreak, the UK Government provided public health advice to stay at home from 16 March 2020, followed by instruction to stay at home (full lockdown) from 24 March 2020. We use data with high temporal resolution from utility sensors installed in 280 homes across social housing in Cornwall, UK, to test for changes in domestic electricity, gas and water usage in response to government guidance. Gas usage increased by 20% following advice to stay at home, the week before full lockdown, although no difference was seen during full lockdown itself. During full lockdown, morning electricity usage shifted to later in the day, decreasing at 6 a.m. and increasing at midday. These changes in energy were echoed in water usage, with a 17% increase and a one-hour delay in peak morning usage. Changes were consistent with people getting up later, spending more time at home and washing more during full lockdown. Evidence for these changes was also observed in later lockdowns, but not between lockdowns. Our findings suggest more compliance with an enforced stay-at-home message than with advice. We discuss implications for socioeconomically disadvantaged households given the indication of inability to achieve increased energy needs during the pandemic. ; European Regional Development Fund (ERDF) ; European Regional Development Fund (ERDF)
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In: Journal of the International AIDS Society, Band 11, Heft Suppl 1, S. P25
ISSN: 1758-2652
In: Journal of the International AIDS Society, Band 15, Heft S4, S. 1-2
ISSN: 1758-2652
Purpose of the studyIn Germany, older age is described as a risk factor for late presentation of HIV disease (defined as<200 CD4/μL or AIDS at diagnosis). We describe treatment outcomes with respect to age distribution at the time of antiretroviral therapy (ART) initiation in the multicentre, observational, ongoing STAR and STELLA cohorts, which included patients (pts) initiated on LPV/r‐based ART.MethodsThis analysis included ART‐naïve HIV+ pts with a minimum of 48 weeks follow‐up. Time to virologic response (defined as HIV1‐RNA <50 c/mL) and time to CD4 cell increase of at least 100/μL were calculated using Kaplan‐Meier analyses. Virologic response rates at week 48 were evaluated using 2 approaches: i) defining discontinuations for virologic or immunologic failure, side effects, noncompliance, or death as failures (ITT) and ii) as‐treated (AT) analysis excluding discontinuations for reasons other than virologic failure.Summary of results1011 ART‐naïve pts were included (85% men; median age 43 years [y]). Baseline (BL) characteristics and treatment response rates are shown in Table 1. The overall prevalence of advanced immunodeficiency with<200 CD4/μL at ART initiation was 48%:*Comparison across groups64% in pts aged >60 y and 31%–49% in the younger age groups (see Table 1). Across age groups, 43%–60% of pts had pretreatment HIV1‐RNA levels>100,000 c/mL. Median times to virologic response (Figure 1) and response rates at week 48 did not differ across age groups in either analysis, nor did immunologic outcomes. Median times to+100/μL CD4 increase were between 11.1 and 15.3 weeks. CD4 increase at week 48 was lower in pts >60 y compared to patients of younger age categories (165/μL vs 211/μL; P=ns). However, these differences between age groups did not reach statistical significance, even when stratified by baseline CD4 count<vs=200/μL. Over the first 48 weeks of therapy, clinical and laboratory adverse events (AEs) of grade 3 or 4 were spontaneously reported in 9.6% of pts in the=60 y group and 4.5% of pts in the >60 y group (P=0.194). In addition, 11.3 % of pts =60 and 14.9% of pts >60 y discontinued therapy prior to week 48 due to treatment related AEs (P=0.427).
Age, y
≤30
>30–40
>40–50
>50–60
>60
P value
Statistical tests*
N
68
321
411
144
67
Male, %
69
80
89
89
88
P<0.001
χ2
Median time since diagnosis, y (IQR)
0.79 (0.21–2.98)
0.67 (0.09–3.23)
0.32 (0.06–3.24)
0.35 (0.06–2.27)
0.10 (0.05–0.69)
P=0.015
Kruskal‐Wallis
BL HIV1‐RNA>100,000 c/mL, %
43
49
56
60
48
P=0.038
χ2
BL median CD4 count, cells/μL
256
208
203
212
121
P=0.001*
Kruskal‐Wallis
BL CD4 count<200/μL, %
31
47
49
48
64
BL CD4 count200–350/μL, %
47
36
33
31
31
BL CD4 count>350/μL, %
22
17
18
21
5
Median CD4 count at wk 48, 1/μL
446
416
412
392
361
P=0.033*
Kruskal‐Wallis
Median time to+100/μL CD4 increase, wk
11.1
12.1
12.1
12.9
15.3
P=0.754
log‐rank
Median change in CD4 at wk 48, 1/μL
234
214
214
180
165
P=0.113*
Kruskal‐Wallis
Median time to HIV1‐RNA<50 c/mL, wk
25.1
25.6
25.9
25.1
35.0
P=0.496
log‐rank
Wk 48 HIV1‐RNA<50 c/mL, % ITT
63.2
69.8
69.6
68.1
61.2
P=0.556
χ2
Wk 48 HIV1‐RNA<50 c/mL, % AT
75.4
82.1
80.1
77.8
78.9
P=0.755
χ2
ConclusionsIn the STAR/STELLA cohorts, pts aged >60 y had high rates of late presentation, with two‐thirds of patients with CD4 cell counts<200/μL. Nevertheless, older pts did not differ significantly from younger pts regarding immunologic and virologic response after initiation of LPV/r‐based therapy. image
Context. A group of trans-Neptunian objects (TNOs) are dynamically related to the dwarf planet 136108 Haumea. Ten of them show strong indications of water ice on their surfaces, are assumed to have resulted from a collision, and are accepted as the only known TNO collisional family. Nineteen other dynamically similar objects lack water ice absorptions and are hypothesized to be dynamical interlopers. Aims. We have made observations to determine sizes and geometric albedos of six of the accepted Haumea family members and one dynamical interloper. Ten other dynamical interlopers have been measured by previous works. We compare the individual and statistical properties of the family members and interlopers, examining the size and albedo distributions of both groups. We also examine implications for the total mass of the family and their ejection velocities. Methods. We use far-infrared space-based telescopes to observe the target TNOs near their thermal peak and combine these data with optical magnitudes to derive sizes and albedos using radiometric techniques. Using measured and inferred sizes together with ejection velocities, we determine the power-law slope of ejection velocity as a function of effective diameter. Results. The detected Haumea family members have a diversity of geometric albedos 0.3-0.8, which are higher than geometric albedos of dynamically similar objects without water ice. The median geometric albedo for accepted family members is pV = 0.48-0.18 +0.28, compared to 0.08-0.05 +0.07 for the dynamical interlopers. In the size range D = 175-300 km, the slope of the cumulative size distribution is q = 3.2-0.4 +0.7 for accepted family members, steeper than the q = 2.0 ± 0.6 slope for the dynamical interlopers with D < 500 km. The total mass of Haumea's moons and family members is 2.4% of Haumea's mass. The ejection velocities required to emplace them on their current orbits show a dependence on diameter, with a power-law slope of 0.21-0.50. © ESO 2018. ; Part of this work was supported by the German DLR project number 50 OR 1108. T.M., C.K., P.S., and R.D. acknowledge that the research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378. A.P. acknowledges the grant LP2012-31 of the Hungarian Academy of Sciences. N.P. acknowledges funding by the Portuguese FCT - Foundation for Science and Technology (ref: SFRH/BGCT/113686/2015). CITEUC is funded by Portuguese National Funds through FCT - Foundation for Science and Technology (project: UID/Multi/00611/2013) and FEDER - European Regional Development Fund through COMPETE 2020 - Operational Programme Competitiveness and Internationalisation (project: POCI-01-0145-FEDER-006922). C.K. has been supported by the K-125015 and GINOP-2.3.2-15-2016-00003 grants of the National Research, Development and Innovation Office (NKFIH, Hungary).
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In: Third world quarterly, Band 3, Heft 4, S. 715-759
ISSN: 1360-2241
The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project. ; Google; NumFOCUS; Python Software Foundation; Space Telescope Science Institute; Harvard-Smithsonian Center for Astrophysics; South African Astronomical Observatory; National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory [SV3-73016]; National Aeronautics Space Administration [NAS8-03060]; UW eScience Institute via Moore Foundation; Sloan Foundation; Washington Research Foundation; NASA's Planetary Astronomy Program; NASA [NAS8-03060, NAS 5-26555]; NASA through Hubble Fellowship - Space Telescope Science Institute [51316.01]; Giacconi Fellowship; FONDECYT [1170618]; MINEDUC-UA [ANT 1655, ANT 1656]; German Research Foundation (DFG) [SFB 881]; German Research Foundation (DFG); NSF [AST-1313484]; Spanish government [AYA2016-75808-R]; Gemini Observatory; Korea Astronomy and Space Science Institute, under the RD program ; The Astropy community is supported by and makes use of a number of organizations and services outside the traditional academic community. We thank Google for financing and organizing the Google Summer of Code (GSoC) program, that has funded several students per year to work on Astropy related projects over the summer. These students often turn into longterm contributors. We also thank NumFOCUS and the Python Software Foundation for financial support. Within the academic community, we thank institutions that make it possible for astronomers and other developers on their staff to contribute their time to the development of Astropy projects. We acknowledge the support of the Space Telescope Science Institute, Harvard-Smithsonian Center for Astrophysics, and the South African Astronomical Observatory.r The following individuals would like to recognize support for their personal contributions. H.M.G. was supported by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.T.V. was supported by the UW eScience Institute via grants from the Moore Foundation, the Sloan Foundation, and the Washington Research Foundation. S.M.C. acknowledges the National Research Foundation of South Africa. M.V.B. was supported by NASA's Planetary Astronomy Program. T.L.A. was supported by NASA contract NAS8-03060. Support for E.J.T. was provided by NASA through Hubble Fellowship grant No. 51316.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, as well as a Giacconi Fellowship. M.B. was supported by the FONDECYT regular project 1170618 and the MINEDUC-UA projects codes ANT 1655 and ANT 1656. D.H. was supported through the SFB 881 "The Milky Way System" by the German Research Foundation (DFG). W.E.K was supported by an ESO Fellowship. C.M. is supported by NSF grant AST-1313484. S.P. was supported by grant AYA2016-75808-R (FEDER) issued by the Spanish government. J.E.H.T. was supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Brazil, Canada, Chile, and the United States of America. Y.P.B was supported by the Korea Astronomy and Space Science Institute, under the R&D program supervised by the Ministry of Science, ICT, and Future Planning.
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The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.© 2018. The American Astronomical Society. ; The Astropy community is supported by and makes use of a number of organizations and services outside the traditional academic community. We thank Google for financing and organizing the Google Summer of Code (GSoC) program, that has funded several students per year to work on Astropy related projects over the summer. These students often turn into longterm contributors. We also thank NumFOCUS and the Python Software Foundation for financial support. Within the academic community, we thank institutions that make it possible for astronomers and other developers on their staff to contribute their time to the development of Astropy projects. We acknowledge the support of the Space Telescope Science Institute, Harvard-Smithsonian Center for Astrophysics, and the South African Astronomical Observatory.r The following individuals would like to recognize support for their personal contributions. H.M.G. was supported by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.T.V. was supported by the UW eScience Institute via grants from the Moore Foundation, the Sloan Foundation, and the Washington Research Foundation. S.M.C. acknowledges the National Research Foundation of South Africa. M.V.B. was supported by NASA's Planetary Astronomy Program. T.L.A. was supported by NASA contract NAS8-03060. Support for E.J.T. was provided by NASA through Hubble Fellowship grant No. 51316.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, as well as a Giacconi Fellowship. M.B. was supported by the FONDECYT regular project 1170618 and the MINEDUC-UA projects codes ANT 1655 and ANT 1656. D.H. was supported through the SFB 881 >The Milky Way System> by the German Research Foundation (DFG). W.E.K was supported by an ESO Fellowship. C.M. is supported by NSF grant AST-1313484. S.P. was supported by grant AYA2016-75808-R (FEDER) issued by the Spanish government. J.E.H.T. was supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Brazil, Canada, Chile, and the United States of America. Y.P.B was supported by the Korea Astronomy and Space Science Institute, under the R&D program supervised by the Ministry of Science, ICT, and Future Planning.
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BMWFW (Austria) ; FWF (Austria) ; FNRS (Belgium) ; FWO (Belgium) ; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) ; Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) ; Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) ; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) ; MES (Bulgaria) ; CERN ; CAS (China) ; MoST (China) ; NSFC (China) ; COLCIENCIAS (Colombia) ; MSES (Croatia) ; CSF (Croatia) ; RPF (Cyprus) ; SENESCYT (Ecuador) ; MoER (Estonia) ; ERC IUT (Estonia) ; ERDF (Estonia) ; Academy of Finland (Finland) ; MEC (Finland) ; HIP (Finland) ; CEA (France) ; CNRS/IN2P3 (France) ; BMBF (Germany) ; DFG (Germany) ; HGF (Germany) ; GSRT (Greece) ; OTKA (Hungary) ; NIH (Hungary) ; DAE (India) ; DST (India) ; IPM (Iran) ; SFI (Ireland) ; INFN (Italy) ; MSIP (Republic of Korea) ; NRF (Republic of Korea) ; LAS (Lithuania) ; MOE (Malaysia) ; UM (Malaysia) ; BUAP (Mexico) ; CINVESTAV (Mexico) ; CONACYT (Mexico) ; LNS (Mexico) ; SEP (Mexico) ; UASLP-FAI (Mexico) ; MBIE (New Zealand) ; PAEC (Pakistan) ; MSHE (Poland) ; NSC (Poland) ; FCT (Portugal) ; JINR (Dubna) ; MON (Russia) ; RosAtom (Russia) ; RAS (Russia) ; RFBR (Russia) ; MESTD (Serbia) ; SEIDI (Spain) ; CPAN (Spain) ; Swiss Funding Agencies (Switzerland) ; MST (Taipei) ; ThEPCenter (Thailand) ; IPST (Thailand) ; STAR (Thailand) ; NSTDA (Thailand) ; TUBITAK (Turkey) ; TAEK (Turkey) ; NASU (Ukraine) ; SFFR (Ukraine) ; STFC (United Kingdom) ; DOE (USA) ; NSF (USA) ; Marie-Curie programme (European Union) ; European Research Council (European Union) ; EPLANET (European Union) ; Leventis Foundation ; A. P. Sloan Foundation ; Alexander von Humboldt Foundation ; Belgian Federal Science Policy Office ; Fonds pour la Formation a la Recherche dans l'Industrie et dans l'Agriculture (FRIA-Belgium) ; Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium) ; Ministry of Education, Youth and Sports (MEYS) of the Czech Republic ; Council of Science and Industrial Research, India ; HOMING PLUS programme of the Foundation for Polish Science - European Union, Regional Development Fund ; Ministry of Science and Higher Education ; National Science Center (Poland) ; Thalis programme - EU-ESF ; Aristeia programme - EU-ESF ; Greek NSRF ; National Priorities Research Program by Qatar National Research Fund ; Programa Clarin-COFUND del Principado de Asturias ; Rachadapisek Sompot Fund for Postdoctoral Fellowship, Chulalongkorn University ; Chulalongkorn Academic into Its second Century Project Advancement Project (Thailand) ; Welch Foundation ; National Science Center (Poland): Harmonia 2014/14/M/ST2/00428 ; National Science Center (Poland): Opus 2013/11/B/ST2/04202 ; National Science Center (Poland): 2014/13/B/ST2/02543 ; National Science Center (Poland): 2014/15/B/ST2/03998 ; National Science Center (Poland): Sonata-bis 2012/07/E/ST2/01406 ; Welch Foundation: C-1845 ; The WZ production cross section is measured by the CMS experiment at the CERN LHC in proton proton collision data samples corresponding to integrated luminosities of 4.9 fb(-1) collected at root s = 7 TeV, and 19.6fb(-1) at root s = 8 TeV. The measurements are performed using the fully-leptonic WZ decay modes with electrons and muons in the final state. The measured cross sections for 71 WZ; root s = 7 TeV) = 20.14 +/- 1.32 (stat)+/- 0.38 (theo)+/- 1.06 (exp)+/- 0.44 (lumi) pb and sigma (pp -> WZ; root s = 8 TeV) = 24.09 +/- 0.87 (stat) 0.80 (theo) +/- 1.40 (exp) +/- 0.63 (lumi) pb. Differential cross sections with respect to the Z boson p(T), the leading jet p(T), and the number of jets are obtained using the root s = 8 TeV data. The results are consistent with standard model predictions and constraints on anomalous triple gauge couplings are obtained.
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