<subfield code="a">ALEPH experiment: Candidate of Higgs boson production</subfield>
</datafield>
<datafield tag="246" ind1=" " ind2="1">
<subfield code="a">Expérience ALEPH: Candidat de la production d'un boson Higgs</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">14 06 2000</subfield>
</datafield>
<datafield tag="340" ind1=" " ind2=" ">
<subfield code="a">FILM</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">Candidate for the associated production of the Higgs boson and Z boson. Both, the Higgs and Z boson decay into 2 jets each. The green and the yellow jets belong to the Higgs boson. They represent the fragmentation of a bottom andanti-bottom quark. The red and the blue jets stem from the decay of the Z boson into a quark anti-quark pair. Left: View of the event along the beam axis. Bottom right: Zoom around the interaction point at the centre showing detailsof the fragmentation of the bottom and anti-bottom quarks. As expected for b quarks, in each jet the decay of a long-lived B meson is visible. Top right: "World map" showing the spatial distribution of the jets in the event.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">Press</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Experiments and Tracks</subfield>
<subfield code="a">The first CERN-built module of the barrel section of ATLAS's electromagnetic calorimeter</subfield>
</datafield>
<datafield tag="246" ind1=" " ind2="1">
<subfield code="a">Premier module du tonneau du calorimètre electromagnétique d'ATLAS</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">10 Apr 2001</subfield>
</datafield>
<datafield tag="340" ind1=" " ind2=" ">
<subfield code="a">DIGITAL</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">Behind the module, left to right Ralf Huber, Andreas Bies and Jorgen Beck Hansen. In front of the module, left to right: Philippe Lançon and Edward Wood.</subfield>
</datafield>
<datafield tag="590" ind1=" " ind2=" ">
<subfield code="a">Derrière le module, de gauche à droite: Ralf Huber, Andreas Bies, Jorgen Beck Hansen. Devant le module, de gauche à droite : Philippe Lançon et Edward Wood.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">CERN EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Experiments and Tracks</subfield>
<subfield code="a">In February, the Agreement establishing the European Molecular Biology Conference was signed at CERN. Willy Spuhler is signing for Switzerland.</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Personalities and History of CERN</subfield>
<subfield code="a">High energy cosmic rays striking atoms at the top of the atmosphere give the rise to showers of particles striking the Earth's surface</subfield>
</datafield>
<datafield tag="246" ind1=" " ind2="1">
<subfield code="a">Des rayons cosmiques de haute energie heurtent des atomes dans la haute atmosphere et donnent ainsi naissance a des gerbes de particules projetees sur la surface terrestre</subfield>
<subfield code="s">eight Nobel prizewinners</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">1962</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">In 1962, CERN hosted the 11th International Conference on High Energy Physics. Among the distinguished visitors were eight Nobel prizewinners.Left to right: Cecil F. Powell, Isidor I. Rabi, Werner Heisenberg, Edwin M. McMillan, Emile Segre, Tsung Dao Lee, Chen Ning Yang and Robert Hofstadter.</subfield>
</datafield>
<datafield tag="590" ind1=" " ind2=" ">
<subfield code="a">En 1962, le CERN est l'hote de la onzieme Conference Internationale de Physique des Hautes Energies. Parmi les visiteurs eminents se trouvaient huit laureats du prix Nobel.De gauche a droite: Cecil F. Powell, Isidor I. Rabi, Werner Heisenberg, Edwin M. McMillan, Emile Segre, Tsung Dao Lee, Chen Ning Yang et Robert Hofstadter.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">Press</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Personalities and History of CERN</subfield>
<subfield code="p">The Nobel Prize in Physics 1961 : Robert Hofstadter</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="P">
<subfield code="s">6206002 (1962)</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">n</subfield>
<subfield code="w">199830</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">PICTURE</subfield>
</datafield>
</record>
<record>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">CERN-GE-9806033</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Tim Berners-Lee</subfield>
<subfield code="s">World-Wide Web inventor</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">28 Jun 1998</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">Conference "Internet, Web, What's next?" on 26 June 1998 at CERN : Tim Berners-Lee, inventor of the World-Wide Web and Director of the W3C, explains how the Web came to be and give his views on the future.</subfield>
</datafield>
<datafield tag="590" ind1=" " ind2=" ">
<subfield code="a">Conference "Internet, Web, What's next?" le 26 juin 1998 au CERN: Tim Berners-Lee, inventeur du World-Wide Web et directeur du W3C, explique comment le Web est ne, et donne ses opinions sur l'avenir.</subfield>
<subfield code="a">Constraints on $\Omega_{\Lambda}$ and $\Omega_{m}$from Distant Type 1a Supernovae and Cosmic Microwave Background Anisotropies</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">14 Dec 1998</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">6 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We perform a combined likelihood analysis of the latest cosmic microwave background anisotropy data and distant Type 1a Supernova data of Perlmutter etal (1998a). Our analysis is restricted tocosmological models where structure forms from adiabatic initial fluctuations characterised by a power-law spectrum with negligible tensor component. Marginalizing over other parameters, our bestfit solution gives Omega_m = 0.25 (+0.18, -0.12) and Omega_Lambda = 0.63 (+0.17, -0.23) (95 % confidence errors) for the cosmic densities contributed by matter and a cosmological constantrespectively. The results therefore strongly favour a nearly spatially flat Universe with a non-zero cosmological constant.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">LANL EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Astrophysics and Astronomy</subfield>
<subfield code="p">Mon. Not. R. Astron. Soc.</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="O">
<subfield code="i">SLAC</subfield>
<subfield code="s">4162242</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="5">
<subfield code="b">CER</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">n</subfield>
<subfield code="w">200231</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">PREPRINT</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Bond, J.R. 1996, Theory and Observations of the Cosmic Background Radiation, in "Cosmology and Large Scale Structure", Les Houches Session LX, August 1993, eds. R. Schaeffer, J. Silk, M. Spiro and J. Zinn-Justin, Elsevier SciencePress, Amsterdam, p469</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Bond J.R., Efstathiou G., Tegmark M., 1997</subfield>
<subfield code="p">L33</subfield>
<subfield code="t">Mon. Not. R. Astron. Soc.</subfield>
<subfield code="v">291</subfield>
<subfield code="y">1997</subfield>
<subfield code="s">Mon. Not. R. Astron. Soc. 291 (1997) L33</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Bond, J.R., Jaffe, A. 1997, in Proc. XXXI Rencontre de Moriond, ed. F. Bouchet, Edition Fronti eres, in press</subfield>
<subfield code="r">astro-ph/9610091</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Bond J.R., Jaffe A.H. and Knox L.E., 1998</subfield>
<subfield code="m">Burles S., Tytler D., 1998a, to appear in the Proceedings of the Second Oak Ridge Symposium on Atomic & Nuclear Astrophysics, ed. A. Mezzacappa, Institute of Physics, Bristol</subfield>
<subfield code="r">astro-ph/9803071</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Burles S., Tytler D., 1998b, Astrophys. J.in press</subfield>
<subfield code="m">Devlin M.J., De Oliveira-Costa A., Herbig T., Miller A.D., Netterfield C.B., Page L., Tegmark M., 1998, submitted to Astrophys. J</subfield>
<subfield code="r">astro-ph/9808043</subfield>
<subfield code="s">Astrophys. J. 509 (1998) L69-72</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Efstathiou G. 1996, Observations of Large-Scale Structure in the Universe, in "Cosmology and Large Scale Structure", Les Houches Session LX, August 1993, eds. R. Schaeffer, J. Silk, M. Spiro and J. Zinn-Justin, Elsevier SciencePress, Amsterdam, p135. Efstathiou G., Bond J.R., Mon. Not. R. Astron. Soc.in press</subfield>
<subfield code="r">astro-ph/9807130</subfield>
<subfield code="s">Astrophys. J. 518 (1999) 2-23</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Evrard G., 1998, submitted to Mon. Not. R. Astron. Soc</subfield>
<subfield code="m">Peebles P.J.E., 1993, Principles of Physical Cosmology, Princeton University Press, Princeton, New Jersey. Perlmutter S, et al., 1995, In Presentations at the NATO ASI in Aiguablava, Spain, LBL-38400; also published in Thermonuclear Supernova, P. Ruiz-Lapuente, R. Cana and J. Isern (eds), Dordrecht, Kluwer, 1997, p749. Perlmutter S, et al., 1997</subfield>
<subfield code="p">565</subfield>
<subfield code="t">Astrophys. J.</subfield>
<subfield code="v">483</subfield>
<subfield code="y">1997</subfield>
<subfield code="s">Astrophys. J. 483 (1997) 565</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Perlmutter S. et al., 1998a, Astrophys. J.in press. (P98)</subfield>
<subfield code="r">astro-ph/9812133</subfield>
<subfield code="s">Astrophys. J. 517 (1999) 565-586</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Perlmutter S. et al., 1998b, In Presentation at the January 1988 Meeting of the American Astronomical Society, Washington D.C., LBL-42230, available at www-supernova.lbl.gov; B.A.A.S., volume : 29 (1997) 1351Perlmutter S, et al., 1998c</subfield>
<subfield code="a">Search for R-Parity Violating Production of Single Sneutrinos in $e^{+}e^{-}$ Collisions at $\sqrt{s}$ = 189-209 GeV</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Geneva</subfield>
<subfield code="b">CERN</subfield>
<subfield code="c">17 Dec 2001</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">22 p</subfield>
</datafield>
<datafield tag="490" ind1=" " ind2=" ">
<subfield code="a">ALEPH Papers</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">A search for single sneutrino production under the assumption that $R$-parity is violated via a single dominant $LL\bar{E}$ coupling is presented. This search considers the process ${\rm e} \gamma\;{\smash{\mathop{\rightarrow}}}\;\tilde{\nu}\ell$ and is performed using the data collected by the ALEPH detector at centre-of-mass energies from 189\,GeV up to 209\,GeV corresponding to an integrated luminosity of637.1\,$\mathrm{pb}^{-1}$. The numbers of observed candidate events are in agreement with Standard Model expectations and 95\% confidence level upper limits on five of the $LL\bar{E}$ couplings are given as a function of the assumedsneutrino mass.</subfield>
<subfield code="m">G. Farrar and P. Fayet</subfield>
<subfield code="p">575</subfield>
<subfield code="t">Phys. Lett., B</subfield>
<subfield code="v">76</subfield>
<subfield code="y">1978</subfield>
<subfield code="s">Phys. Lett. B 76 (1978) 575</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[3]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. Weinberg</subfield>
<subfield code="p">287</subfield>
<subfield code="t">Phys. Rev., B</subfield>
<subfield code="v">26</subfield>
<subfield code="y">1982</subfield>
<subfield code="s">Phys. Rev. B 26 (1982) 287</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">N. Sakai and T. Yanagida</subfield>
<subfield code="p">83</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">197</subfield>
<subfield code="y">1982</subfield>
<subfield code="s">Nucl. Phys. B 197 (1982) 83</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. Dimopoulos, S. Raby and F. Wilczek</subfield>
<subfield code="p">133</subfield>
<subfield code="t">Phys. Lett., B</subfield>
<subfield code="v">212</subfield>
<subfield code="y">1982</subfield>
<subfield code="s">Phys. Lett. B 212 (1982) 133</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[4]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">B.C. Allanach, H. Dreiner, P. Morawitz and M.D. Williams, "Single Sneutrino/Slepton Production at LEP2 and the NLC"</subfield>
<subfield code="p">307</subfield>
<subfield code="t">Phys. Lett., B</subfield>
<subfield code="v">420</subfield>
<subfield code="y">1998</subfield>
<subfield code="s">Phys. Lett. B 420 (1998) 307</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[5]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">ALEPH Collaboration, "Search for R-Parity Violating Decays of Supersymmetric Particles in e+e- Collisions at Centre-of-Mass Energies between s = 189202 GeV"</subfield>
<subfield code="p">415</subfield>
<subfield code="t">Eur. Phys. J., C</subfield>
<subfield code="v">19</subfield>
<subfield code="y">2001</subfield>
<subfield code="s">Eur. Phys. J. C 19 (2001) 415</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[6]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">ALEPH Collaboration, "ALEPH: a detector for electron-positron annihilations at LEP", Nucl. Instrum. and Methods. A : 294 (1990) 121</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[7]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. Cantini, Yu. L. Dokshitzer, M. Olsson, G. Turnock and B.R. Webber, `New clustering algorithm for multijet cross sections in e+e- annihilation"</subfield>
<subfield code="p">432</subfield>
<subfield code="t">Phys. Lett., B</subfield>
<subfield code="v">269</subfield>
<subfield code="y">1991</subfield>
<subfield code="s">Phys. Lett. B 269 (1991) 432</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[8]</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">ALEPH Collaboration, "Performance of the ALEPH detector at LEP", Nucl. Instrum. and Methods. A : 360 (1995) 481</subfield>
<subfield code="s">Nucl. Instrum. and Methods. 360 (1995) 481</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[9]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. Katsanevas and P. Morawitz, "SUSYGEN 2.2 - A Monte Carlo Event Generator for MSSM Sparticle Production at e+e- Colliders"</subfield>
<subfield code="s">Phys. Lett. B 390 (1997) 298</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[16]</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">J.A.M. Vermaseren, in Proceedings of the IVth International Workshop on Gamma Gamma Interactions, Eds. G. Cochard and P. Kessler, Springer Verlag, 1980</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[17]</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">J. -F. Grivaz and F. Le Diberder, "Complementary analyses and acceptance optimization in new particle searches", LAL preprint # 92-37 (1992)</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[18]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">ALEPH Collaboration, "Search for Supersymmetry with a dominant R-Parity Violating LL ¯ E Coupling in e+e- Collisions at Centre-of-Mass Energies of 130 GeV to 172 GeV"</subfield>
<subfield code="p">433</subfield>
<subfield code="t">Eur. Phys. J., C</subfield>
<subfield code="v">4</subfield>
<subfield code="y">1998</subfield>
<subfield code="s">Eur. Phys. J. C 4 (1998) 433</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[19]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">For reviews see for example: H. Dreiner, "An Introduction to Explicit R-parity Violation"</subfield>
<subfield code="r">hep-ph/9707435</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">published in Perspectives on Supersymmetry, ed. G.L. Kane, World Scientific, Singapore (1998); G. Bhattacharyya</subfield>
<subfield code="p">83</subfield>
<subfield code="t">Nucl. Phys. B, Proc. Suppl.</subfield>
<subfield code="v">52</subfield>
<subfield code="y">1997</subfield>
<subfield code="s">Nucl. Phys. B Proc. Suppl. 52 (1997) 83</subfield>
<subfield code="a">Infrared constraints on the dark mass concentration observed in the cluster Abell 1942</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">24 Jan 2001</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">8 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We present a deep H-band image of the region in the vicinity of the cluster Abell 1942 containing the puzzling dark matter concentration detected in an optical weak lensing study by Erben et al. (2000). We demonstrate that ourlimiting magnitude, H=22, would be sufficient to detect clusters of appropriate mass out to redshifts comparable with the mean redshift of the background sources. Despite this, our infrared image reveals no obvious overdensity ofsources at the location of the lensing mass peak, nor an excess of sources in the I-H vs. H colour-magnitude diagram. We use this to further constrain the luminosity and mass-to-light ratio of the putative dark clump as a function ofits redshift. We find that for spatially-flat cosmologies, background lensing clusters with reasonable mass-to-light ratios lying in the redshift range 0<z<1 are strongly excluded, leaving open the possibility that the massconcentration is a new type of truly dark object.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">LANL EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Astrophysics and Astronomy</subfield>
<subfield code="y">Mahon, Richard G. Mc</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="1">
<subfield code="y">Firth, Andrew E.</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="4">
<subfield code="p">Mon. Not. R. Astron. Soc.</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">n</subfield>
<subfield code="w">200104</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">PREPRINT</subfield>
</datafield>
</record>
<record>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">hep-ph/0105155</subfield>
</datafield>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">CERN-TH-2001-131</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Mangano, M L</subfield>
<subfield code="u">CERN</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Physics at the front-end of a neutrino factory : a quantitative appraisal</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Geneva</subfield>
<subfield code="b">CERN</subfield>
<subfield code="c">16 May 2001</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">1 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We present a quantitative appraisal of the physics potential for neutrino experiments at the front-end of a muon storage ring. We estimate the forseeable accuracy in the determination of several interesting observables, and explorethe consequences of these measurements. We discuss the extraction of individual quark and antiquark densities from polarized and unpolarized deep-inelastic scattering. In particular we study the implications for the undertanding ofthe nucleon spin structure. We assess the determination of alpha_s from scaling violation of structure functions, and from sum rules, and the determination of sin^2(theta_W) from elastic nu-e and deep-inelastic nu-p scattering. Wethen consider the production of charmed hadrons, and the measurement of their absolute branching ratios. We study the polarization of Lambda baryons produced in the current and target fragmentation regions. Finally, we discuss thesensitivity to physics beyond the Standard Model.</subfield>
<subfield code="u">nuDIS Working group of the ECFA-CERN Neutrino-Factory Study Group</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="1">
<subfield code="c">2001-05-17</subfield>
<subfield code="l">50</subfield>
<subfield code="m">2001-05-25</subfield>
<subfield code="o">MH</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="O">
<subfield code="i">SLAC</subfield>
<subfield code="s">4628020</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="5">
<subfield code="b">CER</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">n</subfield>
<subfield code="w">200231</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">PREPRINT</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
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<subfield code="m">in Proceedings of Rencontre de Moriond - Hadronic session of `QCD and high energy hadronic interactions', M´eribel-les-Allues, 1994, ed. J. Tr an Thanh V an (Editions Fronti eres, Gif-sur-Yvette, 1995), p. 189</subfield>
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<subfield code="m">A.L. Kataev and A.V. Sidorov</subfield>
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<subfield code="m">J. Blümlein and W. L. van Neerven</subfield>
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<subfield code="m">A.L. Kataev and V.V. Starshenko</subfield>
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<subfield code="m">M.A. Samuel, J. Ellis and M. Karliner</subfield>
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<subfield code="m">W. Bernreuther and W. Wetzel</subfield>
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<subfield code="m">]; S.A. Larin, T. van Ritbergen and J.A. Vermaseren</subfield>
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<subfield code="m">K.G. Chetyrkin, B.A. Kniehl and M. Steinhauser</subfield>
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<subfield code="m">E.V. Shuryak and A.I. Vainshtein</subfield>
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<subfield code="m">M.A. Shifman, A.I. Vainshtein and V.I. Zakharov</subfield>
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<subfield code="m">V.M. Braun and A.V. Kolesnichenko</subfield>
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<subfield code="m">G.G. Ross and R.G. Roberts</subfield>
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<subfield code="m">J. Balla, M.V. Polyakov and C. Weiss</subfield>
<subfield code="p">327</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">510</subfield>
<subfield code="y">1998</subfield>
<subfield code="s">Nucl. Phys. B 510 (1998) 327</subfield>
<subfield code="a">Cosmic equation of state, Gravitational Lensing Statistics and Merging of Galaxies</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">4 Apr 2001</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">28 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">In this paper we investigate observational constraints on the cosmic equation of state of dark energy ($p = w \rho$) using gravitational lensing statistics. We carry out likelihood analysis of the lens surveys to constrain thecosmological parameters $\Omega_{m}$ and $w$. We start by constraining $\Omega_{m}$ and $w$ in the no-evolution model of galaxies where the comoving number density of galaxies is constant. We extend our study to evolutionary modelsof galaxies - Volmerange $&$ Guiderdoni Model and Fast-Merging Model (of Broadhurst, Ellis $&$ Glazebrook). For the no-evolution model we get $w \leq -0.24$ and $\Omega_{m}\leq 0.48$ at $1\sigma$ (68% confidence level). For theVolmerange $&$ Guiderdoni Model we have $w \leq -0.2$ and $\Omega_{m} \leq 0.58$ at $1 \sigma$, and for the Fast Merging Model we get $w \leq -0.02$ and $\Omega_{m} \leq 0.93$ at $1\sigma$. For the case of constant $\Lambda$ ($w=-1$), all the models permit $\Omega_{m} = 0.3$ with 68% CL. We observe that the constraints on $w$ and $\Omega_{m}$ (and on $\Omega_{m}$ in the case of $w = -1$) obtained in the case of evolutionary models are weaker than thoseobtained in the case of the no-evolution model.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">LANL EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Astrophysics and Astronomy</subfield>
<subfield code="m">B. Rocca-Volmerange & B. Guiderdoni, Mon. Not. R. As-tron. Soc.: 247 (1990) 166</subfield>
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<subfield code="m">A. Toomre, in The Evolution of Galaxies and Stellar Pop-ulations eds: B. M. Tinsley & R. B. Larson ( Yale Univ. Observatory), p-401 (1977)</subfield>
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<subfield code="m">F. Schwezier</subfield>
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<subfield code="y">1996</subfield>
<subfield code="s">Astron. J. 111 (1996) 109</subfield>
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<subfield code="m">O. J. Eggen, D. Lynden-Bell & A. R. Sandage</subfield>
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<subfield code="m">R. B. Partridge & P. J. E. Peebles</subfield>
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<subfield code="m">S. P. Driver et al</subfield>
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<subfield code="t">Astrophys. J.</subfield>
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<subfield code="s">Astrophys. J. 449 (1995) L23</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">J. M. Burkey et al</subfield>
<subfield code="p">L13</subfield>
<subfield code="t">Astrophys. J.</subfield>
<subfield code="v">429</subfield>
<subfield code="y">1994</subfield>
<subfield code="s">Astrophys. J. 429 (1994) L13</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. M. Faber et al</subfield>
<subfield code="p">668</subfield>
<subfield code="t">Astrophys. J.</subfield>
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<subfield code="s">Astrophys. J. 204 (1976) 668</subfield>
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<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">R. G. Carlberg et al</subfield>
<subfield code="p">540</subfield>
<subfield code="t">Astrophys. J.</subfield>
<subfield code="v">435</subfield>
<subfield code="y">1994</subfield>
<subfield code="s">Astrophys. J. 435 (1994) 540</subfield>
<subfield code="g">AACHEN - BIRMINGHAM - CERN - HELSINKI - KIEL - IMP. COLL. LONDON - QUEEN MARY COLL. LONDON - MADRID CIEMAT - MIT - RUTHERFORD APPLETON LAB. - VIENNA Collaboration</subfield>
<subfield code="a">Not held by the library</subfield>
</datafield>
<datafield tag="502" ind1=" " ind2=" ">
<subfield code="a">Ph.D. : Univ. Central Florida : 1999</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">Recent advances in multimedia processing technologies, internetworking technologies, and the World Wide Web phenomenon have resulted in a vast creation and use of digital videos in all kinds of applications ranging fromentertainment, business solutions, to education. Designing efficient techniques for searching and retrieving videos over the networks becomes increasingly more important as future applications will include a huge volume of multimediacontent. One practical approach to search for a video segment is as follows. Step 1: Apply an initial search to determine the set of candidate videos. Step 2: Browse the candidates to identify the relevant videos. Step 3: Searchwithin the relevant videos for interesting video segments. In practice, a user might have to iterate through these steps multiple times in order to locate the desired video segments. Independently, database researchers have beeninvestigating techniques for the initial search in Step 1. Multimedia researchers have proposed several techniques for video browsing in Step 2. Computer communications researchers have been investigating video delivery techniques. Iidentify that searching for video data is an interactive process which involves the transmission of video data. Developing techniques for each step independently could result in a system with less performance. In this dissertation, Ipresent a unified approach taking into accounts all fundamental characteristics of multimedia data. I evaluated the proposed techniques through both simulation and system implementation. The resulting system is less expensive andoffers better performance. The simulation results demonstrate that the proposed technique can offer video browsing and search operations with little delays and with minimum storage overhead at the server. Client machines can handletheir search operations without involving the server making the design more scalable, which is vital for large systems deployed over the Internet. The implemented system shows that the visual quality of the browsing and the searchoperations are excellent.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">PROQUEST200009</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Computing and Computers</subfield>
<subfield code="u">California State Univ</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Neural Networks For Speech Recognition Of A Phonetic Language</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Long Beach, CA</subfield>
<subfield code="b">Calif. State Univ.</subfield>
<subfield code="c">1999</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">55 p</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">No fulltext</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">Not held by the library</subfield>
</datafield>
<datafield tag="502" ind1=" " ind2=" ">
<subfield code="a">Ms : California State Univ. : 1999</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">The goal of this thesis is to explore a possibility for a viable alternative/replacement to the Amharic typewriter. Amharic is the national language of Ethiopia. It is one of the oldest languages in the world. Actually, the root-language of Amharic, called Geez, is a descendent of Sabean, which is the direct ancestor of all Semitic languages including English. A phonetic language with 276 phonemes/characters, Amharic has posed quite a challenge to those who,like the author of this thesis, have attempted to design an easy-to-use word processor that interfaces with the conventional keyboard. With current Amharic word processing software, each character requires an average of threekeystrokes thus making typing Amharic literature quite a task. This thesis researches the feasibility of developing a PC-based speech recognition system to recognize the spoken phonemes of the Amharic language. Artificial NeuralNetworks are used for the recognition of spoken alphabets that form Amharic words. A neural network with feed-forward architecture is trained with a series of alphabets and is evaluated on its ability to recognize subsequent testdata. The neural network used in this project is a static classification network; that is, it focuses on the frequency domain of speech while making no attempt to process temporal information. The network training procedure uses thegeneralized Delta Rule. The recognition system developed in this project is an Isolated Speech Recognition System. The approach taken is to recognize the spoken word character by character. This approach is expected to work well dueto the phonetic nature of Amharic.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">PROQUEST200009</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Computing and Computers</subfield>
</datafield>
<datafield tag="690" ind1="C" ind2=" ">
<subfield code="a">THESIS</subfield>
</datafield>
<datafield tag="690" ind1="C" ind2=" ">
<subfield code="a">notheld</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="0">
<subfield code="y">1999</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="0">
<subfield code="b">14</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="1">
<subfield code="c">2000-09-22</subfield>
<subfield code="l">00</subfield>
<subfield code="m">2002-02-22</subfield>
<subfield code="o">BATCH</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="O">
<subfield code="i">PROQUEST</subfield>
<subfield code="s">1397120</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="O">
<subfield code="i">PROQUEST</subfield>
<subfield code="s">MAI38/02p448Apr2000</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">n</subfield>
<subfield code="w">200034</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">THESIS</subfield>
</datafield>
</record>
<record>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Topcuoglu, H R</subfield>
<subfield code="u">Syracuse Univ.</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Scheduling Task Graphs In Heterogeneous Computing Environments</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Syracuse, NY</subfield>
<subfield code="b">Syracuse Univ.</subfield>
<subfield code="c">1999</subfield>
</datafield>
<datafield tag="270" ind1=" " ind2=" ">
<subfield code="g">dir.</subfield>
<subfield code="p">Hariri, S</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">126 p</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">No fulltext</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">Not held by the library</subfield>
<subfield code="a">Efficient application scheduling is critical for achieving high performance in heterogeneous computing environments. An application is represented by a directed acyclic graph (DAG) whose nodes represent tasks and whose edgesrepresent communication messages and precedence constraints among the tasks. The general task-scheduling problem maps the tasks of an application on processors and orders their execution so that task precedence requirements aresatisfied and a minimum schedule length is obtained. The task-scheduling problem has been shown to be NP- complete in general cases as well as in several restricted cases. Although a large number of scheduling heuristics arepresented in the literature, most of them target homogeneous processors. Existing algorithms for heterogeneous processors are not generally efficient because of their high complexity and the quality of their results. This thesisstudies the scheduling of DAG-structured application tasks on heterogeneous domains. We develop two novel low-complexity and efficient scheduling algorithms for bounded number of heterogeneous processors, the HeterogeneousEarliest-Finish-Time (HEFT) algorithm and the Critical-Path-on-a-Processor (CPOP) algorithm. The experimental work presented in this thesis shows that these algorithms significantly surpass previous approaches in terms of performance(schedule length ratio, speed-up, and frequency of best results) and cost (running time and time complexity). Our experimental work includes randomly generated graphs and graphs deducted from real applications. As part of thecomparison study, a parametric graph generator is introduced to generate graphs with various characteristics. We also present a further optimization of the HEFT Algorithm by introducing alternative methods for task prioritizing andprocessor selection phases. A novel processor selection policy based on the earliest finish time of the critical child task improves the performance of the HEFT algorithm. Several strategies for selecting the critical child task of agiven task are presented. This thesis addresses embedding the task scheduling algorithms into an application-development environment for distributed resources. An analytical model is introduced for setting the computation costs oftasks and communication costs of edges of a graph. As part of the design framework of our application development environment, a novel, two-phase, distributed scheduling algorithm is presented for scheduling an application overwide-area distributed resources.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">PROQUEST200009</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Computing and Computers</subfield>
<subfield code="a">Software De Apoyo Educativo Al Concepto De Funcion En Precalculo I (spanish Text)</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Rio Piedras</subfield>
<subfield code="b">Puerto Rico Univ.</subfield>
<subfield code="c">1999</subfield>
</datafield>
<datafield tag="270" ind1=" " ind2=" ">
<subfield code="g">dir.</subfield>
<subfield code="p">Monroy, H</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">64 p</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">No fulltext</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">Not held by the library</subfield>
</datafield>
<datafield tag="502" ind1=" " ind2=" ">
<subfield code="a">Ms : Univ. Puerto Rico : 1999</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">This thesis reports on the evaluation of the use of an educational software, designed to improve student's learning of the concept of mathematical function. The students in the study were registered in Precalculus I at theUniversity of Puerto Rico, Mayaguez Campus. The educational software allows the practice of changing the representation of a function among tabular, analytic, and graphical representations. To carry the evaluation, 59 students wereselected and were divided in two groups: control and experimental. Both groups received the 'traditional' classroom lectures on the topic. The experimental group, in addition, was allowed to practice with the educational software. Tomeasure their performance and the effect of the educational software, two tests were given: a pre-test and a post-test. The results of this study shows that the experimental group improved significantly more than the control group,thus demonstrating the validity of the educational software in the learning of the concept of mathematical function.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">PROQUEST200009</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Computing and Computers</subfield>
<subfield code="a">Systeme Multiagent Pour Les Environnements Riches En Informations (french Text)</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Laval</subfield>
<subfield code="b">Laval Univ.</subfield>
<subfield code="c">1999</subfield>
</datafield>
<datafield tag="270" ind1=" " ind2=" ">
<subfield code="g">dir.</subfield>
<subfield code="p">Chaib-Draa, B</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">101 p</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">No fulltext</subfield>
</datafield>
<datafield tag="500" ind1=" " ind2=" ">
<subfield code="a">Not held by the library</subfield>
</datafield>
<datafield tag="502" ind1=" " ind2=" ">
<subfield code="a">Msc : Universite Laval : 1999</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">La croissance du Web est spectaculaire, puisqu'on estime aujourd'hui a plus de 50 millions, le nombre de pages sur le Web qui ne demandent qu'a etre consultees. Un simple calcul montre qu'en consacrant ne serait-ce qu'une minute parpage, il faudrait environ 95 ans pour consulter toutes ces pages. L'utilisation d'une strategie de recherche est donc vitale. Dans ce cadre, de nombreux outils de recherche ont ete proposes. Ces outils appeles souvent moteurs derecherche se sont averes aujourd'hui incapables de fournir de l'aide aux utilisateurs. Les raisons principales a cela sont les suivantes: (1) La nature ouverte de l'Internet: aucune supervision centrale ne s'applique quant audeveloppement d'Internet, puisque toute personne qui desire l'utiliser et/ou offrir des informations est libre de le faire; (2) La nature dynamique des informations: les informations qui ne sont pas disponibles aujourd'hui peuventl'etre demain et inversement; (3) La nature heterogene de l'information: l'information est offerte sous plusieurs formats et de plusieurs facons, compliquant ainsi la recherche automatique de l'information. Devant ce constat, ilsemble important de chercher de nouvelles solutions pour aider l'utilisateur dans sa recherche d'informations. (Abstract shortened by UMI.)</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">PROQUEST200009</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Computing and Computers</subfield>
<subfield code="a">Accelerators and Storage Rings</subfield>
</datafield>
<datafield tag="653" ind1="1" ind2=" ">
<subfield code="a">bibliography</subfield>
</datafield>
<datafield tag="690" ind1="C" ind2=" ">
<subfield code="a">REPORT</subfield>
</datafield>
<datafield tag="690" ind1="C" ind2=" ">
<subfield code="a">THESIS</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="0">
<subfield code="b">14</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="0">
<subfield code="y">1989</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="1">
<subfield code="c">1990-02-28</subfield>
<subfield code="l">50</subfield>
<subfield code="m">2002-03-22</subfield>
<subfield code="o">BATCH</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="S">
<subfield code="s">h</subfield>
<subfield code="w">199010n</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">THESIS</subfield>
</datafield>
</record>
<record>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">gr-qc/0204045</subfield>
</datafield>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Khalatnikov, I M</subfield>
<subfield code="u">L D Landau Institute for Theoretical Physics of Russian Academy of Sciences</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Comment about quasiisotropic solution of Einstein equations near cosmological singularity</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">12 Apr 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">7 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We generalize for the case of arbitrary hydrodynamical matter the quasiisotropic solution of Einstein equations near cosmological singularity, found by Lifshitz and Khalatnikov in 1960 for the case of radiation-dominated universe. Itis shown that this solution always exists, but dependence of terms in the quasiisotropic expansion acquires a more complicated form.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">LANL EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">General Relativity and Cosmology</subfield>
<subfield code="m">Lifshitz E M and Khalatnikov I M 1964 Sov. Phys. Uspekhi 6 495</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[3]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Landau L D and Lifshitz E M 1979 The Classical Theory of Fields (Perg-amon Press)</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[4]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Starobinsky A A 1986 Stochastic De Sitter (inflationary stage) in the early universe in Field Theory, Quantum Gravity and Strings, (Eds. H.J. De Vega and N. Sanchez, Springer-Verlag, Berlin) 107; Linde A D 1990 Particle Physics and Inflationary Cosmology (Harward Academic Publishers, New York)</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[5]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Banks T and Fischler W 2001 M theory observables for cosmolog-ical space-times</subfield>
<subfield code="m">Perlmutter S J et al 1999</subfield>
<subfield code="p">565</subfield>
<subfield code="t">Astrophys. J.</subfield>
<subfield code="v">517</subfield>
<subfield code="y">1999</subfield>
<subfield code="s">Astrophys. J. 517 (1999) 565</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Riess A et al 1998</subfield>
<subfield code="p">1009</subfield>
<subfield code="t">Astron. J.</subfield>
<subfield code="v">116</subfield>
<subfield code="y">1998</subfield>
<subfield code="s">Astron. J. 116 (1998) 1009</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[7]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Sahni V and Starobinsky A A 2000</subfield>
<subfield code="p">373</subfield>
<subfield code="t">Int. J. Mod. Phys., D</subfield>
<subfield code="v">9</subfield>
<subfield code="y">2000</subfield>
<subfield code="s">Int. J. Mod. Phys. D 9 (2000) 373</subfield>
</datafield>
</record>
<record>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">gr-qc/0204046</subfield>
</datafield>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Bento, M C</subfield>
<subfield code="u">CERN</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Supergravity Inflation on the Brane</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">12 Apr 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">5 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We study N=1 Supergravity inflation in the context of the braneworld scenario. Particular attention is paid to the problem of the onset of inflation at sub-Planckian field values and the ensued inflationary observables. We find thatthe so-called $\eta$-problem encountered in supergravity inspired inflationary models can be solved in the context of the braneworld scenario, for some range of the parameters involved. Furthermore, we obtain an upper bound on thescale of the fifth dimension, $M_5 \lsim 10^{-3} M_P$, in case the inflationary potential is quadratic in the inflaton field, $\phi$. If the inflationary potential is cubic in $\phi$, consistency with observational data requires that$M_5 \simeq 9.2 \times 10^{-4} M_P$.</subfield>
</datafield>
<datafield tag="595" ind1=" " ind2=" ">
<subfield code="a">LANL EDS</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">General Relativity and Cosmology</subfield>
</datafield>
<datafield tag="700" ind1=" " ind2=" ">
<subfield code="a">Bertolami, O</subfield>
</datafield>
<datafield tag="700" ind1=" " ind2=" ">
<subfield code="a">Sen, A A</subfield>
</datafield>
<datafield tag="856" ind1="0" ind2=" ">
<subfield code="f">Maria da Conceicao Bento <bento@sirius.ist.utl.pt></subfield>
<subfield code="a">Reply to 'Comment on "Solution of the Relativistic Dirac-Morse Problem"'</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">11 Apr 2002</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">This combines a reply to the Comment [hep-th/0203067 v1] by A. N. Vaidya and R. de L. Rodrigues with an erratum to our Letter [Phys. Rev. Lett. 87, 210405 (2001)]</subfield>
<subfield code="a">It has long been known that strings wound around incontractible cycles can play a vital role in cosmology. In particular, in a spacetime with toroidal spatial hypersurfaces, the dynamics of the winding modes may help yield threelarge spatial dimensions. However, toroidal compactifications are phenomenologically unrealistic. In this paper we therefore take a first step toward extending these cosmological considerations to $D$-dimensional toroidal orbifolds.We use numerical simulation to study the timescales over which "pseudo-wound" strings unwind on these orbifolds with trivial fundamental group. We show that pseudo-wound strings can persist for many ``Hubble times'' in some of thesespaces, suggesting that they may affect the dynamics in the same way as genuinely wound strings. We also outline some possible extensions that include higher-dimensional wrapped branes.</subfield>
<subfield code="m">R. Brandenberger and C. Vafa</subfield>
<subfield code="p">391</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">316</subfield>
<subfield code="y">1989</subfield>
<subfield code="s">Nucl. Phys. B 316 (1989) 391</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[2]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">A. A. Tseytlin and C. Vafa</subfield>
<subfield code="p">443</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">372</subfield>
<subfield code="y">1992</subfield>
<subfield code="s">Nucl. Phys. B 372 (1992) 443</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="r">hep-th/9109048</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[3]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">M. Sakellariadou</subfield>
<subfield code="p">319</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">468</subfield>
<subfield code="y">1996</subfield>
<subfield code="s">Nucl. Phys. B 468 (1996) 319</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="r">hep-th/9511075</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[4]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">A. G. Smith and A. Vilenkin</subfield>
<subfield code="p">990</subfield>
<subfield code="t">Phys. Rev., D</subfield>
<subfield code="v">36</subfield>
<subfield code="y">1987</subfield>
<subfield code="s">Phys. Rev. D 36 (1987) 990</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[5]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">R. Brandenberger, D. A. Easson and D. Kimberly</subfield>
<subfield code="p">421</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">623</subfield>
<subfield code="y">2002</subfield>
<subfield code="s">Nucl. Phys. B 623 (2002) 421</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="r">hep-th/0109165</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[6]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">B. R. Greene, A. D. Shapere, C. Vafa, and S. T. Yau</subfield>
<subfield code="p">1</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">337</subfield>
<subfield code="y">1990</subfield>
<subfield code="s">Nucl. Phys. B 337 (1990) 1</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[7]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">L. Dixon, J. Harvey, C. Vafa and E. Witten</subfield>
<subfield code="p">678</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">261</subfield>
<subfield code="y">1985</subfield>
<subfield code="s">Nucl. Phys. B 261 (1985) 678</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">L. Dixon, J. Harvey, C. Vafa and E. Witten</subfield>
<subfield code="p">285</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">274</subfield>
<subfield code="y">1986</subfield>
<subfield code="s">Nucl. Phys. B 274 (1986) 285</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[8]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">M. Sakellariadou and A. Vilenkin</subfield>
<subfield code="p">885</subfield>
<subfield code="t">Phys. Rev., D</subfield>
<subfield code="v">37</subfield>
<subfield code="y">1988</subfield>
<subfield code="s">Phys. Rev. D 37 (1988) 885</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[9]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">J. J. Atick and E. Witten</subfield>
<subfield code="p">291</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">310</subfield>
<subfield code="y">1988</subfield>
<subfield code="s">Nucl. Phys. B 310 (1988) 291</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[10]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">D. Mitchell and N. Turok</subfield>
<subfield code="p">1577</subfield>
<subfield code="t">Phys. Rev. Lett.</subfield>
<subfield code="v">58</subfield>
<subfield code="y">1987</subfield>
<subfield code="s">Phys. Rev. Lett. 58 (1987) 1577</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">Imperial College report, 1987 (unpublished)</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[11]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. Alexander, R. Brandenberger, and D. Easson</subfield>
<subfield code="p">103509</subfield>
<subfield code="t">Phys. Rev., D</subfield>
<subfield code="v">62</subfield>
<subfield code="y">2000</subfield>
<subfield code="s">Phys. Rev. D 62 (2000) 103509</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="r">hep-th/0005212</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[12]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">D. Easson</subfield>
<subfield code="r">hep-th/0110225</subfield>
</datafield>
</record>
<record>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">hep-ph/0204132</subfield>
</datafield>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">NUC-MINN-02-3-T</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Shovkovy, I A</subfield>
<subfield code="u">Minnesota Univ.</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Thermal conductivity of dense quark matter and cooling of stars</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="a">Minneapolis, MN</subfield>
<subfield code="b">Minnesota Univ.</subfield>
<subfield code="c">11 Apr 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">9 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">The thermal conductivity of the color-flavor locked phase of dense quark matter is calculated. The dominant contribution to the conductivity comes from photons and Nambu-Goldstone bosons associated with breaking of baryon numberwhich are trapped in the quark core. Because of their very large mean free path the conductivity is also very large. The cooling of the quark core arises mostly from the heat flux across the surface of direct contact with the nuclearmatter. As the thermal conductivity of the neighboring layer is also high, the whole interior of the star should be nearly isothermal. Our results imply that the cooling time of compact stars with color-flavor locked quark cores issimilar to that of ordinary neutron stars.</subfield>
<subfield code="m">J.C. Collins and M.J. Perry</subfield>
<subfield code="p">1353</subfield>
<subfield code="t">Phys. Rev. Lett.</subfield>
<subfield code="v">34</subfield>
<subfield code="y">1975</subfield>
<subfield code="s">Phys. Rev. Lett. 34 (1975) 1353</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[2]</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">B. C. Barrois</subfield>
<subfield code="p">390</subfield>
<subfield code="t">Nucl. Phys., B</subfield>
<subfield code="v">129</subfield>
<subfield code="y">1977</subfield>
<subfield code="s">Nucl. Phys. B 129 (1977) 390</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="m">S. C. Frautschi, in "Hadronic matter at extreme energy density", edited by N. Cabibbo and L. Sertorio (Plenum Press, 1980); D. Bailin and A. Love</subfield>
<subfield code="m">S. L. Shapiro and S. A. Teukolsky, Black holes, white dwarfs, and neutron stars: the physics of compact ob-jects, (John Wiley & Sons, 1983)</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[31]</subfield>
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<subfield code="a">We have calculated the 6s-7s parity nonconserving (PNC) E1 transition amplitude, E_{PNC}, in cesium. We have used an improved all-order technique in the calculation of the correlations and have included all significant contributionsto E_{PNC}. Our final value E_{PNC} = 0.904 (1 +/- 0.5 %) \times 10^{-11}iea_{B}(-Q_{W}/N) has half the uncertainty claimed in old calculations used for the interpretation of Cs PNC experiments. The resulting nuclear weak chargeQ_{W} for Cs deviates by about 2 standard deviations from the value predicted by the standard model.</subfield>
<subfield code="a">Neutrino Indirect Detection of Neutralino Dark Matter in the CMSSM</subfield>
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<subfield code="c">12 Apr 2002</subfield>
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<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">16 p</subfield>
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<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We study potential signals of neutralino dark matter indirect detection by neutrino telescopes in a wide range of CMSSM parameters. We also compare with direct detection potential signals taking into account in both cases present andfuture experiment sensitivities. Only models with neutralino annihilation into gauge bosons can satisfy cosmological constraints and current neutrino indirect detection sensitivities. For both direct and indirect detection, only nextgeneration experiments will be able to really test this kind of models.</subfield>
<subfield code="a">Supersymmetry and a rationale for small CP violating phases</subfield>
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<subfield code="c">12 Apr 2002</subfield>
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<subfield code="a">28 p</subfield>
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<subfield code="a">We analyse the CP problem in the context of a supersymmetric extension of the standard model with universal strength of Yukawa couplings. A salient feature of these models is that the CP phases are constrained to be very small by thehierarchy of the quark masses, and the pattern of CKM mixing angles. This leads to a small amount of CP violation from the usual KM mechanism and a significant contribution from supersymmetry is required. Due to the large generationmixing in some of the supersymmetric interactions, the electric dipole moments impose severe constraints on the parameter space, forcing the trilinear couplings to be factorizable in matrix form. We find that the LL mass insertionsgive the dominant gluino contribution to saturate epsilon_K. The chargino contributions to epsilon'/epsilon are significant and can accommodate the experimental results. In this framework, the standard model gives a negligiblecontribution to the CP asymmetry in B-meson decay, a_{J/\psi K_s}. However, due to supersymmetric contributions to B_d-\bar{B}_d mixing, the recent large value of a_{J/\psi K_s} can be accommodated.</subfield>
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<subfield code="m">P. Q. Hung and M. Seco</subfield>
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<subfield code="o">[8]</subfield>
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<subfield code="m">G. C. Branco and J. I. Silva-Marcos</subfield>
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<subfield code="m">S. Khalil and O. Lebedev</subfield>
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<subfield code="m">See, for example, G. C. Branco, L. Lavoura and J. P. Silva, CP Violation, Interna-tional Series of Monographs on Physics (103), Oxford University Press, Clarendon (1999)</subfield>
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<subfield code="m">V. Fanti et al</subfield>
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<subfield code="m">CLEO Collaboration, S. Ahmed et al, CLEO-CONF-99-10</subfield>
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<subfield code="a">hep-ph/0204137</subfield>
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<subfield code="a">eng</subfield>
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<subfield code="a">DO-TH-02-05</subfield>
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<subfield code="a">Paschos, E A</subfield>
<subfield code="u">Univ. Dortmund</subfield>
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<subfield code="a">Leptogenesis with Majorana neutrinos</subfield>
<subfield code="a">I review the origin of the lepton asymmetry which is converted to a baryon excess at the electroweak scale. This scenario becomes more attractive if we can relate it to other physical phenomena. For this reason I elaborate on theconditions of the early universe which lead to a sizable lepton asymmetry. Then I describe methods and models which relate the low energy parameters of neutrinos to the high energy (cosmological) CP-violation and to neutrinolessdouble beta-decay.</subfield>
<subfield code="b">CONTRIBUTED TO 1ST WORKSHOP ON NEUTRINO - NUCLEUS INTERACTIONS IN THE FEW GEV REGION (NUINT01) TSUKUBA JAPAN 13-16 DEC 2001 6 PAGES 6 FIGURES</subfield>
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<subfield code="a">PREPRINT</subfield>
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<subfield code="o">1.</subfield>
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<subfield code="m">Fukugida and Yanagida</subfield>
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<subfield code="m">M. Flanz, E.A. Paschos and U. Sarkar</subfield>
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<subfield code="m">M. Luty</subfield>
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<subfield code="m">M. Flanz, E.A. Paschos, U. Sarkar and J. Weiss</subfield>
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<subfield code="m">M. Flanz and E.A. Paschos</subfield>
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<subfield code="m">W. Buchmüller and M. Plümacher</subfield>
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<subfield code="m">L. Covi, E. Roulet and F. Vissani</subfield>
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<subfield code="b">CONTRIBUTED TO 1ST WORKSHOP ON NEUTRINO - NUCLEUS INTERACTIONS IN THE FEW GEV REGION (NUINT01) TSUKUBA JAPAN 13-16 DEC 2001 9 PAGES 15 FIGURES</subfield>
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<subfield code="a">PREPRINT</subfield>
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<subfield code="o">1.</subfield>
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<subfield code="m">C. Albright and C. Jarlskog</subfield>
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<subfield code="a">The quark-level linear sigma model is revisited, in particular concerning the identification of the f_0(400-1200) (or \sigma(600)) scalar meson as the chiral partner of the pion. We demonstrate the predictive power of the linearsigma model through the pi-pi and pi-N s-wave scattering lengths, as well as several electromagnetic, weak, and strong decays of pseudoscalar and vector mesons. The ease with which the data for these observables are reproduced in thelinear sigma model lends credit to the necessity to include the sigma as a fundamental q\bar{q} degree of freedom, to be contrasted with approaches like chiral perturbation theory or the confining NJL model of Shakin and Wang.</subfield>
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<subfield code="a">By studying singularities in stationary axisymmetric Kerr and Tomimatsu-Sato solutions with distortion parameter \d = 2, 3, ... in general relativity, we conclude that these singularities can be regarded as nothing other than closedstring-like circular mass distributions. We use two different regularizations to identify \d-function type singularities in the energy-momentum tensor for these solutions, realizing a regulator independent result. This result givessupporting evidence that these axisymmetric exact solutions may well be the classical solutions around closed string-like mass distributions, just like Schwarzschild solution corresponding to a point mass distribution. In otherwords, these axisymmetric exact solutions may well provide the classical backgrounds around closed strings.</subfield>
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<subfield code="a">Following the construction of the projection operators on $ T^2 $ presented by Gopakumar, Headrick and Spradin, we construct the projection operators on the integral noncommutative orbifold $ T^2/G (G=Z_k,k=2, 3, 4, 6)$. Suchoperators are expressed by a function on this orbifold. So it provides a complete set of projection operators upon the moduli space $T^2 \times K/Z_k$. All these operators has the same trace 1/A ($A$ is an integer). Since theprojection operators correspond to solitons in noncommutative string field theory, we obtained the explicit expression of all the soliton solutions on $ T^2/Z_k $.</subfield>
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<subfield code="a">We examine relations among the parameters characterizing the phenomenological equation of state (EOS) of nearly symmetric, uniform nuclear matter near the saturation density by comparing macroscopic calculations of radii and massesof stable nuclei with the experimental data. The EOS parameters of interest here are the symmetry energy S_0, the symmetry energy density-derivative coefficient L and the incompressibility K_0 at the normal nuclear density. We find aconstraint on the relation between K_0 and L from the empirically allowed values of the slope of the saturation line (the line joining the saturation points of nuclear matter at finite neutron excess), together with a strongcorrelation between S_0 and L. In the light of the uncertainties in the values of K_0 and L, we macroscopically calculate radii of unstable nuclei as expected to be produced in future facilities. We find that the matter radii dependstrongly on L while being almost independent of K_0, a feature that will help to determine the L value via systematic measurements of nuclear size.</subfield>
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<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Медный всадник</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">
<!--HTML-->На берегу пустынных волн, <br />
Стоял он, дум великих полн, <br />
И вдаль глядел. Пред ним широко<br />
Река неслася; бедный чёлн<br />
По ней стремился одиноко. <br />
По мшистым, топким берегам<br />
Чернели избы здесь и там, <br />
Приют убогого чухонца; <br />
И лес, неведомый лучам<br />
В тумане спрятанного солнца, <br />
Кругом шумел.
</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="0">
<subfield code="y">1833</subfield>
</datafield>
<datafield tag="909" ind1="C" ind2="1">
<subfield code="c">1990-01-27</subfield>
<subfield code="l">00</subfield>
<subfield code="m">2002-04-12</subfield>
<subfield code="o">BATCH</subfield>
</datafield>
<datafield tag="980" ind1=" " ind2=" ">
<subfield code="a">POETRY</subfield>
</datafield>
</record>
<record>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">gre</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Καβάφης, Κ Π</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Ιθάκη</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">
<!--HTML-->Σα βγεις στον πηγαιμό για την Ιθάκη, <br />
να εύχεσαι νάναι μακρύς ο δρόμος, <br />
γεμάτος περιπέτειες, γεμάτος γνώσεις. <br/>
Τους Λαιστρυγόνας και τους Κύκλωπας, <br />
τον θυμωμένο Ποσειδώνα μη φοβάσαι, <br />
τέτοια στον δρόμο σου ποτέ σου δεν θα βρείς, <br />
αν μέν' η σκέψις σου υψηλή, αν εκλεκτή<br />
συγκίνησις το πνεύμα και το σώμα σου αγγίζει. <br />
Τους Λαιστρυγόνας και τους Κύκλωπας, <br />
τον άγριο Ποσειδώνα δεν θα συναντήσεις, <br />
αν δεν τους κουβανείς μες στην ψυχή σου, <br />
αν η ψυχή σου δεν τους στήνει εμπρός σου. <br />
<br>
Να εύχεσαι νάναι μακρύς ο δρόμος. <br />
Πολλά τα καλοκαιρινά πρωϊά να είναι<br />
που με τι ευχαρίστησι, με τι χαρά<br />
θα μπαίνεις σε λιμένας πρωτοειδωμένους· <br />
να σταματήσεις σ' εμπορεία Φοινικικά, <br />
και τες καλές πραγμάτειες ν' αποκτήσεις, <br />
σεντέφια και κοράλλια, κεχριμπάρια κ' έβενους, <br />
και ηδονικά μυρωδικά κάθε λογής, <br />
όσο μπορείς πιο άφθονα ηδονικά μυρωδικά· <br />
σε πόλεις Αιγυπτιακές πολλές να πας, <br />
να μάθεις και να μάθεις απ' τους σπουδασμένους. <br />
<br />
Πάντα στον νου σου νάχεις την Ιθάκη. <br/>
Το φθάσιμον εκεί είν' ο προορισμός σου. <br />
Αλλά μη βιάζεις το ταξίδι διόλου. <br />
Καλλίτερα χρόνια πολλά να διαρκέσει· <br />
και γέρος πια ν' αράξεις στο νησί, <br />
πλούσιος με όσα κέρδισες στον δρόμο, <br />
μη προσδοκώντας πλούτη να σε δώσει η Ιθάκη. <br />
<br />
Η Ιθάκη σ' έδωσε το ωραίο ταξίδι. <br />
Χωρίς αυτήν δεν θάβγαινες στον δρόμο. <br />
Αλλο δεν έχει να σε δώσει πια. <br />
<br />
Κι αν πτωχική την βρεις, η Ιθάκη δεν σε γέλασε. <br />
Ετσι σοφός που έγινες, με τόση πείρα, <br />
<subfield code="a">AdS Dual of the Critical O(N) Vector Model</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2002</subfield>
</datafield>
<datafield tag="269" ind1=" " ind2=" ">
<subfield code="c">11 Oct 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">11 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We suggest a general relation between theories of infinite number of higher-spin massless gauge fields in $AdS_{d+1}$ and large $N$ conformal theories in $d$ dimensions containing $N$-component vector fields. In particular, we propose that the singlet sector of the well-known critical 3-d O(N) model with the $(\phi^a \phi^a)^2$ interaction is dual, in the large $N$ limit, to the minimal bosonic theory in $AdS_4$ containing massless gauge fields of even spin.</subfield>
<subfield code="m">E. D’Hoker, D. Z. Freedman, S. Mathur, A. Matusis and L. Rastelli, "Graviton exchange and complete 4-point functions in the AdS/CFT correspondence, "</subfield>
<subfield code="r">hep-th/9903196</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
<subfield code="o">[26]</subfield>
<subfield code="m">For a review with a comprehensive set of references, see E. d‘Hoker and D.Z. Freedman, "Supersymmetric Gauge Theories and the AdS/CFT Correspondence,"</subfield>
<subfield code="u">Universita di Napoli</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">An improved correspondence formula for AdS/CFT with multi-trace operators</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2002</subfield>
</datafield>
<datafield tag="269" ind1=" " ind2=" ">
<subfield code="a">Napoli</subfield>
<subfield code="b">Napoli Univ.</subfield>
<subfield code="c">15 Jan 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">6 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">An improved correspondence formula is proposed for the calculation of correlation functions of a conformal field theory perturbed by multi-trace operators from the analysis of the dynamics of the dual field theory in Anti-de Sitter space. The formula reduces to the usual AdS/CFT correspondence formula in the case of single-trace perturbations.</subfield>
<subfield code="u">University of London</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Holographic Renormalization and Ward Identities with the Hamilton-Jacobi Method</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2003</subfield>
</datafield>
<datafield tag="269" ind1=" " ind2=" ">
<subfield code="a">Napoli</subfield>
<subfield code="b">Napoli Univ.</subfield>
<subfield code="c">7 May 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">31 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">A systematic procedure for performing holographic renormalization, which makes use of the Hamilton-Jacobi method, is proposed and applied to a bulk theory of gravity interacting with a scalar field and a U(1) gauge field in the Stueckelberg formalism. We describe how the power divergences are obtained as solutions of a set of "descent equations" stemming from the radial Hamiltonian constraint of the theory. In addition, we isolate the logarithmic divergences, which are closely related to anomalies. The method allows to determine also the exact one-point functions of the dual field theory. Using the other Hamiltonian constraints of the bulk theory, we derive the Ward identities for diffeomorphisms and gauge invariance. In particular, we demonstrate the breaking of U(1)_R current conservation, recovering the holographic chiral anomaly recently discussed in hep-th/0112119 and hep-th/0202056.</subfield>
<subfield code="a">Higher dimensional geometries related to fuzzy odd-dimensional spheres</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2002</subfield>
</datafield>
<datafield tag="269" ind1=" " ind2=" ">
<subfield code="a">Providence, RI</subfield>
<subfield code="b">Brown Univ.</subfield>
<subfield code="c">11 Jul 2002</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">32 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We study $SO(m)$ covariant Matrix realizations of $ \sum_{i=1}^{m} X_i^2 = 1 $ for even $m$ as candidate fuzzy odd spheres following hep-th/0101001. As for the fuzzy four sphere, these Matrix algebras contain more degrees of freedom than the sphere itself and the full set of variables has a geometrical description in terms of a higher dimensional coset. The fuzzy $S^{2k-1} $ is related to a higher dimensional coset $ {SO(2k) \over U(1) \times U(k-1)}$. These cosets are bundles where base and fibre are hermitian symmetric spaces. The detailed form of the generators and relations for the Matrix algebras related to the fuzzy three-spheres suggests Matrix actions which admit the fuzzy spheres as solutions. These Matrix actions are compared with the BFSS, IKKT and BMN Matrix models as well as some others. The geometry and combinatorics of fuzzy odd spheres lead to some remarks on the transverse five-brane problem of Matrix theories and the exotic scaling of the entropy of 5-branes with the brane number.</subfield>
<subfield code="m">M. Fabinger, "Higher-Dimensional Quantum Hall Effect in String Theory,"</subfield>
<subfield code="s">J. High Energy Phys. 0205 (2002) 037</subfield>
<subfield code="r">hep-th/0201016</subfield>
</datafield>
<datafield tag="999" ind1="C" ind2="5">
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<subfield code="m">A.P. Balachandran "Quantum Spacetimes in the Year 1,"</subfield>
<subfield code="r">hep-th/0203259</subfield>
</datafield>
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<subfield code="m">M. Kramer, " Some remarks suggesting an interesting theory of harmonic functions on SU(2n + 1)/Sp(n) and SO(2n + 1)/U(n)," Arch. Math. 33 ( 1979/80), 76-79.</subfield>
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<subfield code="m">P.M. Ho, "Fuzzy sphere from Matrix model,"</subfield>
<subfield code="s">J. High Energy Phys. 0012 (2000) 015</subfield>
<subfield code="r">hep-th/0110165</subfield>
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<subfield code="m">T. Banks, W. Fischler, S. Shenker, L. Susskind, "M-Theory Ann. Sci. a Matrix model A conjecture,"</subfield>
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<subfield code="r">hep-th/9610043</subfield>
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<subfield code="m">N. Ishibashi, H. Kawai, Y. Kitazawa, A. Tsuchiya, " A large-N reduced model Ann. Sci. Superstring, "</subfield>
<subfield code="s">Nucl. Phys. B 498 (1997) 467</subfield>
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<subfield code="m">V. Periwal, "Matrices on a point Ann. Sci. the theory of everything,"</subfield>
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<subfield code="m">S. Chaudhuri, "Bosonic Matrix Theory and D-branes,"</subfield>
<subfield code="r">hep-th/0205306</subfield>
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<subfield code="m">M. Bagnoud, L. Carlevaro, A. Bilal, "Supermatrix models for M-theory based on osp(1—32,R),"</subfield>
<subfield code="r">hep-th/0201183</subfield>
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<subfield code="m">L. Smolin, "M theory Ann. Sci. a matrix extension of Chern Simons theory,"</subfield>
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<subfield code="r">hep-th/0002009</subfield>
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<subfield code="m">I. Bandos, J. Lukierski, "New superparticle models outside the HLS suersymmetry scheme,"</subfield>
<subfield code="r">hep-th/9812074</subfield>
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<subfield code="m">S.Iso, Y.Kimura, K.Tanaka, K. Wakatsuki, "Noncommutative Gauge Theory on Fuzzy Sphere from Matrix Model,"</subfield>
<subfield code="r">hep-th/0101102</subfield>
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<subfield code="m">W. Fulton and G. Harris, "Representation theory," Springer Verlag 1991.</subfield>
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<subfield code="m">M. Atiyah and E. Witten, "M-Theory Dynamics On A Manifold Of G2 Holonomy,"</subfield>
<subfield code="r">hep-th/0107177</subfield>
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<subfield code="m">S. Ramgoolam, D. Waldram, "Zero branes on a compact orbifold,"</subfield>
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<subfield code="r">hep-th/9805191</subfield>
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<subfield code="m">Brian R. Greene, C.I. Lazaroiu, Piljin Yi " D Particles on T4 /Z(N) Orbifolds and their resolutions,"</subfield>
<subfield code="s">Nucl. Phys. B 539 (1999) 135</subfield>
<subfield code="r">hep-th/9807040</subfield>
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<subfield code="m">I. Klebanov, A. Tseytlin, "Entropy of Near-Extremal Black p-branes,"</subfield>
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<subfield code="a">We argue that perturbative quantum field theory and string theory can be consistently modified in the infrared to eliminate, in a radiatively stable manner, tadpole instabilities that arise after supersymmetry breaking. This is achieved by deforming the propagators of classically massless scalar fields and the graviton so as to cancel the contribution of their zero modes. In string theory, this modification of propagators is accomplished by perturbatively deforming the world-sheet action with bi-local operators similar to those that arise in double-trace deformations of AdS/CFT. This results in a perturbatively finite and unitary S-matrix (in the case of string theory, this claim depends on standard assumptions about unitarity in covariant string diagrammatics). The S-matrix is parameterized by arbitrary scalar VEVs, which exacerbates the vacuum degeneracy problem. However, for generic values of these parameters, quantum effects produce masses for the nonzero modes of the scalars, lifting the fluctuating components of the moduli.</subfield>
<subfield code="m">W. Fischler and L. Susskind, "Dilaton Tadpoles, String Condensates And Scale In-variance,"</subfield>
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<subfield code="m">W. Fischler and L. Susskind, "Dilaton Tadpoles, String Condensates And Scale In-variance. 2,"</subfield>
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<subfield code="m">C. G. Callan, C. Lovelace, C. R. Nappi and S. A. Yost, "Loop Corrections To Super-string Equations Of Motion,"</subfield>
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<subfield code="m">J. Polchinski, "Factorization Of Bosonic String Amplitudes,"</subfield>
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<subfield code="m">H. La and P. Nelson, "Effective Field Equations For Fermionic Strings,"</subfield>
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<subfield code="m">E. Witten, "Strong Coupling Expansion Of Calabi-Yau Compactification,"</subfield>
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<subfield code="m">T. Banks, "On isolated vacua and background independence," arXiv</subfield>
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<subfield code="m">A. Maloney, E. Silverstein and A. Strominger, "De Sitter space in noncritical string theory," arXiv</subfield>
<subfield code="r">hep-th/0205316</subfield>
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<subfield code="m">S. Kachru and E. Silverstein, "4d conformal theories and strings on orbifolds,"</subfield>
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<subfield code="r">hep-th/9802183</subfield>
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<subfield code="m">A. E. Lawrence, N. Nekrasov and C. Vafa, "On conformal field theories in four di-mensions,"</subfield>
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<subfield code="r">hep-th/9803015</subfield>
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<subfield code="r">hep-th/9803076</subfield>
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<subfield code="m">I. R. Klebanov and Astron. Astrophys. Tseytlin, "A non-supersymmetric large N CFT from type 0 string theory,"</subfield>
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<subfield code="u">The Weizmann Inst. of Science</subfield>
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<subfield code="c">2003</subfield>
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<subfield code="a">Trieste</subfield>
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<subfield code="a">26 p</subfield>
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<subfield code="a">We study the quantum stability of Type IIB orbifold and orientifold string models in various dimensions, including Melvin backgrounds, where supersymmetry (SUSY) is broken {\it \`a la} Scherk-Schwarz (SS) by twisting periodicity conditions along a circle of radius R. In particular, we compute the R-dependence of the one-loop induced vacuum energy density $\rho(R)$, or cosmological constant. For SS twists different from Z2 we always find, for both orbifolds and orientifolds, a monotonic $\rho(R)<0$, eventually driving the system to a tachyonic instability. For Z2 twists, orientifold models can have a different behavior, leading either to a runaway decompactification limit or to a negative minimum at a finite value R_0. The last possibility is obtained for a 4D chiral orientifold model where a more accurate but yet preliminary analysis seems to indicate that $R_0\to \infty$ or towards the tachyonic instability, as the dependence on the other geometric moduli is included.</subfield>
<subfield code="a">We study large N conformal field theories perturbed by relevant double-trace deformations. Using the auxiliary field trick, or Hubbard-Stratonovich transformation, we show that in the infrared the theory flows to another CFT. The generating functionals of planar correlators in the ultraviolet and infrared CFT's are shown to be related by a Legendre transform. Our main result is a universal expression for the difference of the scale anomalies between the ultraviolet and infrared fixed points, which is of order 1 in the large N expansion. Our computations are entirely field theoretic, and the results are shown to agree with predictions from AdS/CFT. We also remark that a certain two-point function can be computed for all energy scales on both sides of the duality, with full agreement between the two and no scheme dependence.</subfield>
<subfield code="u">Universita di Milano-Bicocca</subfield>
</datafield>
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<subfield code="a">3-D Interacting CFTs and Generalized Higgs Phenomenon in Higher Spin Theories on AdS</subfield>
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<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2003</subfield>
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<subfield code="c">16 Dec 2002</subfield>
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<subfield code="a">8 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We study a duality, recently conjectured by Klebanov and Polyakov, between higher-spin theories on AdS_4 and O(N) vector models in 3-d. These theories are free in the UV and interacting in the IR. At the UV fixed point, the O(N) model has an infinite number of higher-spin conserved currents. In the IR, these currents are no longer conserved for spin s>2. In this paper, we show that the dual interpretation of this fact is that all fields of spin s>2 in AdS_4 become massive by a Higgs mechanism, that leaves the spin-2 field massless. We identify the Higgs field and show how it relates to the RG flow connecting the two CFTs, which is induced by a double trace deformation.</subfield>
<subfield code="a">The holographic renormalization group (RG) is reviewed in a self-contained manner. The holographic RG is based on the idea that the radial coordinate of a space-time with asymptotically AdS geometry can be identified with the RG flow parameter of the boundary field theory. After briefly discussing basic aspects of the AdS/CFT correspondence, we explain how the notion of the holographic RG comes out in the AdS/CFT correspondence. We formulate the holographic RG based on the Hamilton-Jacobi equations for bulk systems of gravity and scalar fields, as was introduced by de Boer, Verlinde and Verlinde. We then show that the equations can be solved with a derivative expansion by carefully extracting local counterterms from the generating functional of the boundary field theory. The calculational methods to obtain the Weyl anomaly and scaling dimensions are presented and applied to the RG flow from the N=4 SYM to an N=1 superconformal fixed point discovered by Leigh and Strassler. We further discuss a relation between the holographic RG and the noncritical string theory, and show that the structure of the holographic RG should persist beyond the supergravity approximation as a consequence of the renormalizability of the nonlinear sigma model action of noncritical strings. As a check, we investigate the holographic RG structure of higher-derivative gravity systems, and show that such systems can also be analyzed based on the Hamilton-Jacobi equations, and that the behaviour of bulk fields are determined solely by their boundary values. We also point out that higher-derivative gravity systems give rise to new multicritical points in the parameter space of the boundary field theories.</subfield>
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<subfield code="a">In this lecture I address the issue of possible large distance modification of gravity and its observational consequences. Although, for the illustrative purposes we focus on a particular simple generally-covariant example, our conclusions are rather general and apply to large class of theories in which, already at the Newtonian level, gravity changes the regime at a certain very large crossover distance $r_c$. In such theories the cosmological evolution gets dramatically modified at the crossover scale, usually exhibiting a "self-accelerated" expansion, which can be differentiated from more conventional "dark energy" scenarios by precision cosmology. However, unlike the latter scenarios, theories of modified-gravity are extremely constrained (and potentially testable) by the precision gravitational measurements at much shorter scales. Despite the presence of extra polarizations of graviton, the theory is compatible with observations, since the naive perturbative expansion in Newton's constant breaks down at a certain intermediate scale. This happens because the extra polarizations have couplings singular in $1/r_c$. However, the correctly resummed non-linear solutions are regular and exhibit continuous Einsteinian limit. Contrary to the naive expectation, explicit examples indicate that the resummed solutions remain valid after the ultraviolet completion of the theory, with the loop corrections taken into account.</subfield>
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<subfield code="a">Quasi-normal Modes of Electromagnetic Perturbations of Four-Dimensional Topological Black Holes with Scalar Hair</subfield>
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<subfield code="a">17 p</subfield>
</datafield>
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<subfield code="a">We study the perturbative behaviour of topological black holes with scalar hair. We calculate both analytically and numerically the quasi-normal modes of the electromagnetic perturbations. In the case of small black holes we find clear evidence of a second-order phase transition of a topological black hole to a hairy configuration. We also find evidence of a second-order phase transition of the AdS vacuum solution to a topological black hole.</subfield>
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<subfield code="u">The Pennsylvania State University</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">A new PPN parameter to test Chern-Simons gravity</subfield>
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<subfield code="c">2007</subfield>
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<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">4 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">We study Chern-Simons (CS) gravity in the parameterized post-Newtonian (PPN) framework through weak-field solutions of the modified field equations for a perfect fluid source. We discover that CS gravity possesses the same PPN parameters as general relativity, except for the inclusion of a new term, proportional both to the CS coupling parameter and the curl of the PPN vector potentials. This new term encodes the key physical effect of CS gravity in the weak-field limit, leading to a modification of frame dragging and, thus, the Lense-Thirring contribution to gyroscopic precession. We provide a physical interpretation for the new term, as well as an estimate of the size of this effect relative to the general relativistic Lense-Thirring prediction. This correction to frame dragging might be used in experiments, such as Gravity Probe B and lunar ranging, to place bounds on the CS coupling parameter, as well as other intrinsic parameters of string theory.</subfield>
<subfield code="a">It is shown that the world-line can be eliminated in the matrix quantum mechanics conjectured by Banks, Fischler, Shenker and Susskind to describe the light-cone physics of M theory. The resulting matrix model has a form that suggests origins in the reduction to a point of a Yang-Mills theory. The reduction of the Nishino-Sezgin $10+2$ dimensional supersymmetric Yang-Mills theory to a point gives a matrix model with the appropriate features: Lorentz invariance in $9+1$ dimensions, supersymmetry, and the correct number of physical degrees of freedom.</subfield>
<subfield code="a">The wall of the cave</subfield>
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<subfield code="a">In this article old and new relations between gauge fields and strings are discussed. We add new arguments that the Yang Mills theories must be described by the non-critical strings in the five dimensional curved space. The physical meaning of the fifth dimension is that of the renormalization scale represented by the Liouville field. We analyze the meaning of the zigzag symmetry and show that it is likely to be present if there is a minimal supersymmetry on the world sheet. We also present the new string backgrounds which may be relevant for the description of the ordinary bosonic Yang-Mills theories. The article is written on the occasion of the 40-th anniversary of the IHES.</subfield>
<!--added the following record to get an example of finding a reference-->
<!--by 999C5s to 909C4-->
<!--It's probably a good article, anyway-->
<record>
<controlfield tag="003">SzGeCERN</controlfield>
<datafield tag="035" ind1=" " ind2=" ">
<subfield code="a">2174811CERCER</subfield>
</datafield>
<datafield tag="035" ind1=" " ind2=" ">
<subfield code="9">SLAC</subfield>
<subfield code="a">4308492</subfield>
</datafield>
<datafield tag="037" ind1=" " ind2=" ">
<subfield code="a">hep-ph/0002060</subfield>
</datafield>
<datafield tag="041" ind1=" " ind2=" ">
<subfield code="a">eng</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">ACT-2000-1</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">CTP-TAMU-2000-2</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">OUTP-2000-03-P</subfield>
</datafield>
<datafield tag="088" ind1=" " ind2=" ">
<subfield code="a">TPI-MINN-2000-6</subfield>
</datafield>
<datafield tag="100" ind1=" " ind2=" ">
<subfield code="a">Cleaver, G B</subfield>
</datafield>
<datafield tag="245" ind1=" " ind2=" ">
<subfield code="a">Non-Abelian Flat Directions in a Minimal Superstring Standard Model</subfield>
</datafield>
<datafield tag="260" ind1=" " ind2=" ">
<subfield code="c">2000</subfield>
</datafield>
<datafield tag="269" ind1=" " ind2=" ">
<subfield code="a">Houston, TX</subfield>
<subfield code="b">Houston Univ. Adv. Res. Cent. The Woodlands</subfield>
<subfield code="c">4 Feb 2000</subfield>
</datafield>
<datafield tag="300" ind1=" " ind2=" ">
<subfield code="a">14 p</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="a">Recently, by studying exact flat directions of non-Abelian singlet fields, wedemonstrated the existence of free fermionic heterotic-string models in whichthe SU(3)_C x SU(2)_L x U(1)_Y-charged matter spectrum, just below the stringscale, consists solely of the MSSM spectrum. In this paper we generalize theanalysis to include VEVs of non-Abelian fields. We find several,MSSM-producing, exact non-Abelian flat directions, which are the first suchexamples in the literature. We examine the possibility that hidden sectorcondensates lift the flat directions.</subfield>
<subfield code="a">Development of photon beam diagnostics for VUV radiation from a SASE FEL</subfield>
</datafield>
<datafield tag="260" ind1="" ind2="">
<subfield code="c">2000</subfield>
</datafield>
<datafield tag="269" ind1="" ind2="">
<subfield code="a">Hamburg</subfield>
<subfield code="b">DESY</subfield>
<subfield code="c">Dec 1999</subfield>
</datafield>
<datafield tag="520" ind1="" ind2="">
<subfield code="a">For the proof-of-principle experiment of self-amplified spontaneous emission (SASE) at short wavelengths on the VUV FEL at DESY a multi-facetted photon beam diagnostics experiment has been developed employing new detection concepts to measure all SASE specific properties on a single pulse basis. The present setup includes instrumentation for the measurement of the energy and the angular and spectral distribution of individual photon pulses. Different types of photon detectors such as PtSi-photodiodes and fast thermoelectric detectors based on YBaCuO-films are used to cover some five orders of magnitude of intensity from the level of spontaneous emission to FEL radiation at saturation. A 1 m normal incidence monochromator in combination with a fast intensified CCD camera allows to select single photon pulses and to record the full spectrum at high resolution to resolve the fine structure due to the start-up from noise.</subfield>
</datafield>
<datafield tag="595" ind1="" ind2="">
<subfield code="a">SIS INIS2004</subfield>
</datafield>
<datafield tag="595" ind1="" ind2="">
<subfield code="a">SIS UNC2002</subfield>
</datafield>
<datafield tag="595" ind1="" ind2="">
<subfield code="d">Development of photon beam diagnostics for VUV radiation from a SASE FEL</subfield>
</datafield>
<datafield tag="650" ind1="1" ind2="7">
<subfield code="2">SzGeCERN</subfield>
<subfield code="a">Accelerators and Storage Rings</subfield>
<subfield code="a">A naturalist's voyage around the world</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="b"><!--HTML--><p class="articleHeader">After having been twice driven back by heavy south-western gales, Her Majesty's ship Beagle" a ten-gun brig, under the command of Captain Fitz Roy, R.N., sailed from Devonport on the 27th of December, 1831. The object of the expedition was to complete the survey of Patagonia and Tierra del Fuego, commenced under Captain King in 1826 to 1830--to survey the shores of Chile, Peru, and of some islands in the Pacific--and to carry a chain of chronometrical measurements round the World.</p> <div class="phwithcaption"> <div class="imageScale"><img alt="" src="http://cdsware.cern.ch/download/invenio-demo-site-files/icon-journal_hms_beagle_image.gif" /></div> <p>H.M.S. Beagle</p> </div> <p>On the 6th of January we reached Teneriffe, but were prevented landing, by fears of our bringing the cholera: the next morning we saw the sun rise behind the rugged outline of the Grand Canary Island, and suddenly illumine the Peak of Teneriffe, whilst the lower parts were veiled in fleecy clouds. This was the first of many delightful days never to be forgotten. On the 16th of January 1832 we anchored at Porto Praya, in St. Jago, the chief island of the Cape de Verd archipelago.</p> <p>The neighbourhood of Porto Praya, viewed from the sea, wears a desolate aspect. The volcanic fires of a past age, and the scorching heat of a tropical sun, have in most places rendered the soil unfit for vegetation. The country rises in successive steps of table-land, interspersed with some truncate conical hills, and the horizon is bounded by an irregular chain of more lofty mountains. The scene, as beheld through the hazy atmosphere of this climate, is one of great interest; if, indeed, a person, fresh from sea, and who has just walked, for the first time, in a grove of cocoa-nut trees, can be a judge of anything but his own happiness. The island would generally be considered as very uninteresting, but to any one accustomed only to an English landscape, the novel aspect of an utterly sterile land possesses a grandeur which more vegetation might spoil. A single green leaf can scarcely be discovered over wide tracts of the lava plains; yet flocks of goats, together with a few cows, contrive to exist. It rains very seldom, but during a short portion of the year heavy torrents fall, and immediately afterwards a light vegetation springs out of every crevice. This soon withers; and upon such naturally formed hay the animals live. It had not now rained for an entire year. When the island was discovered, the immediate neighbourhood of Porto Praya was clothed with trees,1 the reckless destruction of which has caused here, as at St. Helena, and at some of the Canary islands, almost entire sterility. The broad, flat-bottomed valleys, many of which serve during a few days only in the season as watercourses, are clothed with thickets of leafless bushes. Few living creatures inhabit these valleys. The commonest bird is a kingfisher (Dacelo Iagoensis), which tamely sits on the branches of the castor-oil plant, and thence darts on grasshoppers and lizards. It is brightly coloured, but not so beautiful as the European species: in its flight, manners, and place of habitation, which is generally in the driest valley, there is also a wide difference. One day, two of the officers and myself rode to Ribeira Grande, a village a few miles eastward of Porto Praya. Until we reached the valley of St. Martin, the country presented its usual dull brown appearance; but here, a very small rill of water produces a most refreshing margin of luxuriant vegetation. In the course of an hour we arrived at Ribeira Grande, and were surprised at the sight of a large ruined fort and cathedral. This little town, before its harbour was filled up, was the principal place in the island: it now presents a melancholy, but very picturesque appearance. Having procured a black Padre for a guide, and a Spaniard who had served in the Peninsular war as an interpreter, we visited a collection of buildings, of which an ancient church formed the principal part. It is here the governors and captain-generals of the islands have been buried. Some of the tombstones recorded dates of the sixteenth century.1 The heraldic ornaments were the only things in this retired place that reminded us of Europe. The church or chapel formed one side of a quadrangle, in the middle of which a large clump of bananas were growing. On another side was a hospital, containing about a ozen miserable-looking inmates.</p> <p>We returned to the Vênda to eat our dinners. A considerable number of men, women, and children, all as black as jet, collected to watch us. Our companions were extremely merry; and everything we said or did was followed by their hearty laughter. Before leaving the town we visited the cathedral. It does not appear so rich as the smaller church, but boasts of a little organ, which sent forth singularly inharmonious cries. We presented the black priest with a few shillings, and the Spaniard, patting him on the head, said, with much candour, he thought his colour made no great difference. We then returned, as fast as the ponies would go, to Porto Praya.</p> (Excerpt from A NATURALIST'S VOYAGE ROUND THE WORLD Chapter 1, By Charles Darwin)</subfield>
<subfield code="b"><!--HTML--><p class="articleHeader">I have before remarked in speaking of the allotments of the gods, that they distributed the whole earth into portions differing in extent, and made for themselves temples and instituted sacrifices. And Poseidon, receiving for his lot the island of Atlantis, begat children by a mortal woman, and settled them in a part of the island, which I will describe.</p> <p>Looking towards the sea, but in the centre of the whole island, there was a plain which is said to have been the fairest of all plains and very fertile. Near the plain again, and also in the centre of the island at a distance of about fifty stadia, there was a mountain not very high on any side. In this mountain there dwelt one of the earth-born primeval men of that country, whose name was Evenor, and he had a wife named Leucippe, and they had an only daughter who was called Cleito. The maiden had already reached womanhood, when her father and mother died; Poseidon fell in love with her and had intercourse with her, and breaking the ground, inclosed the hill in which she dwelt all round, making alternate zones of sea and land larger and smaller, encircling one another; there were two of land and three of water, which he turned as with a lathe, each having its circumference equidistant every way from the centre, so that no man could get to the island, for ships and voyages were not as yet. He himself, being a god, found no difficulty in making special arrangements for the centre island, bringing up two springs of water from beneath the earth, one of warm water and the other of cold, and making every variety of food to spring up abundantly from the soil. He also begat and brought up five pairs of twin male children; and dividing the island of Atlantis into ten portions, he gave to the first-born of the eldest pair his mother's dwelling and the surrounding allotment, which was the largest and best, and made him king over the rest; the others he made princes, and gave them rule over many men, and a large territory. And he named them all; the eldest, who was the first king, he named Atlas, and after him the whole island and the ocean were called Atlantic. To his twin brother, who was born after him, and obtained as his lot the extremity of the island towards the pillars of Heracles, facing the country which is now called the region of Gades in that part of the world, he gave the name which in the Hellenic language is Eumelus, in the language of the country which is named after him, Gadeirus. Of the second pair of twins he called one Ampheres, and the other Evaemon. To the elder of the third pair of twins he gave the name Mneseus, and Autochthon to the one who followed him. Of the fourth pair of twins he called the elder Elasippus, and the younger Mestor. And of the fifth pair he gave to the elder the name of Azaes, and to the younger that of Diaprepes. All these and their descendants for many generations were the inhabitants and rulers of divers islands in the open sea; and also, as has been already said, they held sway in our direction over the country within the pillars as far as Egypt and Tyrrhenia. Now Atlas had a numerous and honourable family, and they retained the kingdom, the eldest son handing it on to his eldest for many generations; and they had such an amount of wealth as was never before possessed by kings and potentates, and is not likely ever to be again, and they were furnished with everything which they needed, both in the city and country. For because of the greatness of their empire many things were brought to them from foreign countries, and the island itself provided most of what was required by them for the uses of life. In the first place, they dug out of the earth whatever was to be found there, solid as well as fusile, and that which is now only a name and was then something more than a name, orichalcum, was dug out of the earth in many parts of the island, being more precious in those days than anything except gold. There was an abundance of wood for carpenter's work, and sufficient maintenance for tame and wild animals. Moreover, there were a great number of elephants in the island; for as there was provision for all other sorts of animals, both for those which live in lakes and marshes and rivers, and also for those which live in mountains and on plains, so there was for the animal which is the largest and most voracious of all. Also whatever fragrant things there now are in the earth, whether roots, or herbage, or woods, or essences which distil from fruit and flower, grew and thrived in that land; also the fruit which admits of cultivation, both the dry sort, which is given us for nourishment and any other which we use for food&mdash;we call them all by the common name of pulse, and the fruits having a hard rind, affording drinks and meats and ointments, and good store of chestnuts and the like, which furnish pleasure and amusement, and are fruits which spoil with keeping, and the pleasant kinds of dessert, with which we console ourselves after dinner, when we are tired of eating&mdash;all these that sacred island which then beheld the light of the sun, brought forth fair and wondrous and in infinite abundance. With such blessings the earth freely furnished them; meanwhile they went on constructing their temples and palaces and harbours and docks.</p> (Excerpt from CRITIAS, By Plato, translated By Jowett, Benjamin)</subfield>
<subfield code="b"><!--HTML--><p class="articleHeader">This great island lay over against the Pillars of Heracles, in extent greater than Libya and Asia put together, and was the passage to other islands and to a great ocean of which the Mediterranean sea was only the harbour; and within the Pillars the empire of Atlantis reached in Europe to Tyrrhenia and in Libya to Egypt.</p> <p>This mighty power was arrayed against Egypt and Hellas and all the countries</p> <div class="phrwithcaption"> <div class="imageScale"><img src="http://cdsware.cern.ch/download/invenio-demo-site-files/icon-journal_Athanasius_Kircher_Atlantis_image.gif" alt="" /></div> <p>Representation of Atlantis by Athanasius Kircher (1669)</p> </div> bordering on the Mediterranean. Then your city did bravely, and won renown over the whole earth. For at the peril of her own existence, and when the other Hellenes had deserted her, she repelled the invader, and of her own accord gave liberty to all the nations within the Pillars. A little while afterwards there were great earthquakes and floods, and your warrior race all sank into the earth; and the great island of Atlantis also disappeared in the sea. This is the explanation of the shallows which are found in that part of the Atlantic ocean. <p> </p> (Excerpt from TIMAEUS, By Plato, translated By Jowett, Benjamin)<br /></subfield>
<subfield code="a">The order Rodentia in South America</subfield>
</datafield>
<datafield tag="520" ind1=" " ind2=" ">
<subfield code="b"><!--HTML--><p>The order Rodentia is here very numerous in species: of mice alone I obtained no less than eight kinds. <sup><a name="note1" href="#footnote1">1</a></sup>The largest gnawing animal in the world, the Hydrochærus capybara (the water-hog), is here also common. One which I shot at Monte Video weighed ninety-eight pounds: its length, from the end of the snout to the stump-like tail, was three feet two inches; and its girth three feet eight. These great Rodents occasionally frequent the islands in the mouth of the Plata, where the water is quite salt, but are far more abundant on the borders of fresh-water lakes and rivers. Near Maldonado three or four generally live together. In the daytime they either lie among the aquatic plants, or openly feed on the turf plain.<sup><a name="note2" href="#footnote2">2</a></sup></p> <p> <div class="phlwithcaption"> <div class="imageScale"><img src="http://cdsware.cern.ch/download/invenio-demo-site-files/icon-journal_water_dog_image.gif" alt="" /></div> <p>Hydrochærus capybara or Water-hog</p> </div> When viewed at a distance, from their manner of walking and colour they resemble pigs: but when seated on their haunches, and attentively watching any object with one eye, they reassume the appearance of their congeners, cavies and rabbits. Both the front and side view of their head has quite a ludicrous aspect, from the great depth of their jaw. These animals, at Maldonado, were very tame; by cautiously walking, I approached within three yards of four old ones. This tameness may probably be accounted for, by the Jaguar having been banished for some years, and by the Gaucho not thinking it worth his while to hunt them. As I approached nearer and nearer they frequently made their peculiar noise, which is a low abrupt grunt, not having much actual sound, but rather arising from the sudden expulsion of air: the only noise I know at all like it, is the first hoarse bark of a large dog. Having watched the four from almost within arm's length (and they me) for several minutes, they rushed into the water at full gallop with the greatest impetuosity, and emitted at the same time their bark. After diving a short distance they came again to the surface, but only just showed the upper part of their heads. When the female is swimming in the water, and has young ones, they are said to sit on her back. These animals are easily killed in numbers; but their skins are of trifling value, and the meat is very indifferent. On the islands in the Rio Parana they are exceedingly abundant, and afford the ordinary prey to the Jaguar.</p> <p><small><sup><a name="footnote1" href="#note1">1</a></sup>. In South America I collected altogether twenty-seven species of mice, and thirteen more are known from the works of Azara and other authors. Those collected by myself have been named and described by Mr. Waterhouse at the meetings of the Zoological Society. I must be allowed to take this opportunity of returning my cordial thanks to Mr. Waterhouse, and to the other gentleman attached to that Society, for their kind and most liberal assistance on all occasions.</small></p> <p><small><sup><a name="footnote2" href="#note2">2</a></sup>. In the stomach and duodenum of a capybara which I opened, I found a very large quantity of a thin yellowish fluid, in which scarcely a fibre could be distinguished. Mr. Owen informs me that a part of the oesophagus is so constructed that nothing much larger than a crowquill can be passed down. Certainly the broad teeth and strong jaws of this animal are well fitted to grind into pulp the aquatic plants on which it feeds.</small></p> (Excerpt from A NATURALIST'S VOYAGE ROUND THE WORLD Chapter 3, By Charles Darwin)</subfield>
<subfield code="b"><!--HTML--><p class="articleHeader">April 14th, 1832.—Leaving Socêgo, we rode to another estate on the Rio Macâe, which was the last patch of cultivated ground in that direction. The estate was two and a half miles long, and the owner had forgotten how many broad.</p> <p> <div class="phlwithcaption"> <div class="imageScale"><img src="http://cdsware.cern.ch/download/invenio-demo-site-files/icon-journal_virgin_forest_image.gif" alt="" /></div> <p>Virgin Forest</p> </div> Only a very small piece had been cleared, yet almost every acre was capable of yielding all the various rich productions of a tropical land. Considering the enormous area of Brazil, the proportion of cultivated ground can scarcely be considered as anything compared to that which is left in the state of nature: at some future age, how vast a population it will support! During the second day's journey we found the road so shut up that it was necessary that a man should go ahead with a sword to cut away the creepers. The forest abounded with beautiful objects; among which the tree ferns, though not large, were, from their bright green foliage, and the elegant curvature of their fronds, most worthy of admiration. In the evening it rained very heavily, and although the thermometer stood at 65°, I felt very cold. As soon as the rain ceased, it was curious to observe the extraordinary evaporation which commenced over the whole extent of the forest. At the height of a hundred feet the hills were buried in a dense white vapour, which rose like columns of smoke from the most thickly-wooded parts, and especially from the valleys. I observed this phenomenon on several occasions: I suppose it is owing to the large surface of foliage, previously heated by the sun's rays.</p> <p>While staying at this estate, I was very nearly being an eye-witness to one of those atrocious acts which can only take place in a slave country. Owing to a quarrel and a lawsuit, the owner was on the point of taking all the women and children from the male slaves, and selling them separately at the public auction at Rio. Interest, and not any feeling of compassion, prevented this act. Indeed, I do not believe the inhumanity of separating thirty families, who had lived together for many years, even occurred to the owner. Yet I will pledge myself, that in humanity and good feeling he was superior to the common run of men. It may be said there exists no limit to the blindness of interest and selfish habit. I may mention one very trifling anecdote, which at the time struck me more forcibly than any story of cruelty. I was crossing a ferry with a negro who was uncommonly stupid. In endeavouring to make him understand, I talked loud, and made signs, in doing which I passed my hand near his face. He, I suppose, thought I was in a passion, and was going to strike him; for instantly, with a frightened look and half-shut eyes, he dropped his hands. I shall never forget my feelings of surprise, disgust, and shame, at seeing a great powerful man afraid even to ward off a blow, directed, as he thought, at his face. This man had been trained to a degradation lower than the slavery of the most helpless animal.</p> (Excerpt from A NATURALIST'S VOYAGE ROUND THE WORLD Chapter 2, By Charles Darwin)</subfield>