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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06657">arXiv:1503.06657</a> <span> [<a href="https://arxiv.org/pdf/1503.06657">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2015.06.040">10.1016/j.asr.2015.06.040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A separation of electrons and protons in the GAMMA-400 gamma-ray telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Leonov%2C+A+A">A. A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.06657v1-abstract-short" style="display: inline;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emissi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'inline'; document.getElementById('1503.06657v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06657v1-abstract-full" style="display: none;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emission, studies of gamma-ray bursts and gamma-ray emission from the active Sun, as well as high-precision measurements of spectra of high-energy electrons and positrons, protons, and nuclei up to the knee. The main components of cosmic rays are protons and helium nuclei, whereas the part of lepton component in the total flux is ~10E-3 for high energies. In present paper, the capability of the GAMMA-400 gamma-ray telescope to distinguish electrons and positrons from protons in cosmic rays is investigated. The individual contribution to the proton rejection is studied for each detector system of the GAMMA-400 gamma-ray telescope. Using combined information from all detector systems allow us to provide the proton rejection from electrons with a factor of ~4x10E5 for vertical incident particles and ~3x10E5 for particles with initial inclination of 30 degrees. The calculations were performed for the electron energy range from 50 GeV to 1 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'none'; document.getElementById('1503.06657v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 figures, submitted to Advances and Space Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.4239">arXiv:1412.4239</a> <span> [<a href="https://arxiv.org/pdf/1412.4239">pdf</a>, <a href="https://arxiv.org/format/1412.4239">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The GAMMA-400 space observatory: status and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Boyarchuk%2C+K+A">K. A. Boyarchuk</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1412.4239v1-abstract-short" style="display: inline;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'inline'; document.getElementById('1412.4239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.4239v1-abstract-full" style="display: none;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as well as protons and nuclei spectra up to the knee region. The GAMMA-400 observatory will allow to address a broad range of science topics, like search for signatures of dark matter, studies of Galactic and extragalactic gamma-ray sources, Galactic and extragalactic diffuse emission, gamma-ray bursts and charged cosmic rays acceleration and diffusion mechanism up to the knee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'none'; document.getElementById('1412.4239v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.2194">arXiv:1409.2194</a> <span> [<a href="https://arxiv.org/pdf/1409.2194">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1063/1.4895099">10.1063/1.4895099 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-resonant silver nano-disk patterned thin film hydrogenated amorphous silicon solar cells for Staebler-Wronski effect compensation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Vora%2C+A">Ankit Vora</a>, <a href="/search/physics?searchtype=author&query=Gwamuri%2C+J">Jephias Gwamuri</a>, <a href="/search/physics?searchtype=author&query=Pearce%2C+J+M">Joshua M. Pearce</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+P+L">Paul L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=G%C3%BCney%2C+D+%C3%96">Durdu 脰. G眉ney</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1409.2194v1-abstract-short" style="display: inline;"> We study polarization independent improved light trapping in commercial thin film hydrogenated amorphous silicon (a-Si:H) solar photovoltaic cells using a three-dimensional silver array of multi-resonant nano-disk structures embedded in a silicon nitride anti-reflection coating (ARC) to enhance optical absorption in the intrinsic layer (i-a-Si:H) for the visible spectrum for any polarization angle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.2194v1-abstract-full').style.display = 'inline'; document.getElementById('1409.2194v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.2194v1-abstract-full" style="display: none;"> We study polarization independent improved light trapping in commercial thin film hydrogenated amorphous silicon (a-Si:H) solar photovoltaic cells using a three-dimensional silver array of multi-resonant nano-disk structures embedded in a silicon nitride anti-reflection coating (ARC) to enhance optical absorption in the intrinsic layer (i-a-Si:H) for the visible spectrum for any polarization angle. Predicted total optical enhancement (OE) in absorption in the i-a-Si:H for AM-1.5 solar spectrum is 18.51% as compared to the reference, and producing a 19.65% improvement in short-circuit current density (JSC) over 11.7 mA/cm2 for a reference cell. The JSC in the nano-disk patterned solar cell (NDPSC) was found to be higher than the commercial reference structure for any incident angle. The NDPSC has a multi-resonant optical response for the visible spectrum and the associated mechanism for OE in i-a-Si:H layer is excitation of Fabry-Perot resonance facilitated by surface plasmon resonances. The detrimental Staebler-Wronski effect (SWE) in a-Si:H solar cell can be minimized by the additional OE in the NDPSC and self-annealing of defect states by additional heat generation, thus likely improving the overall stabilized characteristics of a-Si:H solar cells. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.2194v1-abstract-full').style.display = 'none'; document.getElementById('1409.2194v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 journal pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Appl. Phys., 116, 093103 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0712.1548">arXiv:0712.1548</a> <span> [<a href="https://arxiv.org/pdf/0712.1548">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Science with the new generation high energy gamma- ray experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/physics?searchtype=author&query=D%27Armiento%2C+D">D. D'Armiento</a>, <a href="/search/physics?searchtype=author&query=Agnetta%2C+G">G. Agnetta</a>, <a href="/search/physics?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+A">A. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/physics?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/physics?searchtype=author&query=Baltz%2C+E+A">E. A. Baltz</a>, <a href="/search/physics?searchtype=author&query=Bambi%2C+C">C. Bambi</a>, <a href="/search/physics?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/physics?searchtype=author&query=Bartko%2C+H">H. Bartko</a>, <a href="/search/physics?searchtype=author&query=Basset%2C+M">M. Basset</a>, <a href="/search/physics?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/physics?searchtype=author&query=Belli%2C+P">P. Belli</a>, <a href="/search/physics?searchtype=author&query=Benford%2C+G">G. Benford</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Bernabei%2C+R">R. Bernabei</a>, <a href="/search/physics?searchtype=author&query=Bertone%2C+G">G. Bertone</a>, <a href="/search/physics?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/physics?searchtype=author&query=Biondo%2C+B">B. Biondo</a>, <a href="/search/physics?searchtype=author&query=Bocchino%2C+F">F. Bocchino</a>, <a href="/search/physics?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/physics?searchtype=author&query=Brigida%2C+M">M. Brigida</a>, <a href="/search/physics?searchtype=author&query=Bringmann%2C+T">T. Bringmann</a>, <a href="/search/physics?searchtype=author&query=Brogueira%2C+P">P. Brogueira</a> , et al. (175 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0712.1548v1-abstract-short" style="display: inline;"> This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invaria… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0712.1548v1-abstract-full').style.display = 'inline'; document.getElementById('0712.1548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0712.1548v1-abstract-full" style="display: none;"> This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invariance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0712.1548v1-abstract-full').style.display = 'none'; document.getElementById('0712.1548v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">328 pages, 7.8Mb, Proceedings of the 5th SCINEGHE Workshop, June 18-20, 2007 http://www.roma2.infn.it/SciNeGHE07/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Frascati Physics Series vol.45 (2007) A.Lionetto, A.Morselli editors ISBN 978-88-86409-54-0 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/physics/9701025">arXiv:physics/9701025</a> <span> [<a href="https://arxiv.org/pdf/physics/9701025">pdf</a>, <a href="https://arxiv.org/ps/physics/9701025">ps</a>, <a href="https://arxiv.org/format/physics/9701025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1364/AO.36.004168">10.1364/AO.36.004168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical Properties of Deep Ice at the South Pole - Absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="physics/9701025v1-abstract-short" style="display: inline;"> We discuss recent measurements of the wavelength-dependent absorption coefficients in deep South Pole ice. The method uses transit time distributions of pulses from a variable-frequency laser sent between emitters and receivers embedded in the ice. At depths of 800 to 1000 m scattering is dominated by residual air bubbles, whereas absorption occurs both in ice itself and in insoluble impurities.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/9701025v1-abstract-full').style.display = 'inline'; document.getElementById('physics/9701025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="physics/9701025v1-abstract-full" style="display: none;"> We discuss recent measurements of the wavelength-dependent absorption coefficients in deep South Pole ice. The method uses transit time distributions of pulses from a variable-frequency laser sent between emitters and receivers embedded in the ice. At depths of 800 to 1000 m scattering is dominated by residual air bubbles, whereas absorption occurs both in ice itself and in insoluble impurities. The absorption coefficient increases approximately exponentially with wavelength in the measured interval 410 to 610 nm. At the shortest wavelength our value is about a factor 20 below previous values obtained for laboratory ice and lake ice; with increasing wavelength the discrepancy with previous measurements decreases. At around 415 to 500 nm the experimental uncertainties are small enough for us to resolve an extrinsic contribution to absorption in ice: submicron dust particles contribute by an amount that increases with depth and corresponds well with the expected increase seen near the Last Glacial Maximum in Vostok and Dome C ice cores. The laser pulse method allows remote mapping of gross structure in dust concentration as a function of depth in glacial ice. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/9701025v1-abstract-full').style.display = 'none'; document.getElementById('physics/9701025v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 1997. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, LaTex, Accepted for publication in Applied Optics. 9 figures, not included, available on request from lbe@physto.se</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Appl.Opt.36:4168-4180,1997 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 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