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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/1502.00612">arXiv:1502.00612</a> <span> [<a href="https://arxiv.org/pdf/1502.00612">pdf</a>, <a href="https://arxiv.org/format/1502.00612">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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="High Energy Physics - Theory">hep-th</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/10.1103/PhysRevLett.114.101301">10.1103/PhysRevLett.114.101301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Joint Analysis of BICEP2/Keck Array and Planck Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BICEP2%2FKeck"> BICEP2/Keck</a>, <a href="/search/hep-ph?searchtype=author&query=Collaborations%2C+P">Planck Collaborations</a>, <a href="/search/hep-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/hep-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Aikin%2C+R+W">R. W. Aikin</a>, <a href="/search/hep-ph?searchtype=author&query=Alexander%2C+K+D">K. D. Alexander</a>, <a href="/search/hep-ph?searchtype=author&query=Arnaud%2C+M">M. Arnaud</a>, <a href="/search/hep-ph?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/hep-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/hep-ph?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/hep-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/hep-ph?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/hep-ph?searchtype=author&query=Bartlett%2C+J+G">J. G. Bartlett</a>, <a href="/search/hep-ph?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/hep-ph?searchtype=author&query=Battaner%2C+E">E. Battaner</a>, <a href="/search/hep-ph?searchtype=author&query=Benabed%2C+K">K. Benabed</a>, <a href="/search/hep-ph?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/hep-ph?searchtype=author&query=Benoit-L%C3%A9vy%2C+A">A. Benoit-L茅vy</a>, <a href="/search/hep-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+J+-">J. -P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/hep-ph?searchtype=author&query=Bielewicz%2C+P">P. Bielewicz</a>, <a href="/search/hep-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a> , et al. (254 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="1502.00612v2-abstract-short" style="display: inline;"> We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg$^2$ patch of sky centered on RA 0h, Dec. $-57.5掳$. The combined maps reach a depth of 57 nK deg in Stokes $Q$ and $U$ in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.00612v2-abstract-full').style.display = 'inline'; document.getElementById('1502.00612v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.00612v2-abstract-full" style="display: none;"> We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg$^2$ patch of sky centered on RA 0h, Dec. $-57.5掳$. The combined maps reach a depth of 57 nK deg in Stokes $Q$ and $U$ in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2 $渭$K deg in $Q$ and $U$ at 143 GHz). We detect 150$\times$353 cross-correlation in $B$-modes at high significance. We fit the single- and cross-frequency power spectra at frequencies $\geq 150$ GHz to a lensed-$螞$CDM model that includes dust and a possible contribution from inflationary gravitational waves (as parameterized by the tensor-to-scalar ratio $r$), using a prior on the frequency spectral behavior of polarized dust emission from previous \planck\ analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the $r$ constraint. Finally we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for $r$, and yields an upper limit $r_{0.05}<0.12$ at 95% confidence. Marginalizing over dust and $r$, lensing $B$-modes are detected at $7.0\,蟽$ significance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.00612v2-abstract-full').style.display = 'none'; document.getElementById('1502.00612v2-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> 14 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Version updated to match published. Data and figures available for download at http://bicepkeck.org and http://pla.esac.esa.int/pla</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 114, 101301 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.1488">arXiv:1307.1488</a> <span> [<a href="https://arxiv.org/pdf/1307.1488">pdf</a>, <a href="https://arxiv.org/ps/1307.1488">ps</a>, <a href="https://arxiv.org/format/1307.1488">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1088/1475-7516/2013/11/067">10.1088/1475-7516/2013/11/067 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Axion searches with the EDELWEISS-II experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/hep-ph?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/hep-ph?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/hep-ph?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/hep-ph?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/hep-ph?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/hep-ph?searchtype=author&query=Bergmann%2C+T">T. Bergmann</a>, <a href="/search/hep-ph?searchtype=author&query=Bl%C3%BCmer%2C+J">J. Bl眉mer</a>, <a href="/search/hep-ph?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/hep-ph?searchtype=author&query=Brudanin%2C+V">V. Brudanin</a>, <a href="/search/hep-ph?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/hep-ph?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/hep-ph?searchtype=author&query=Censier%2C+B">B. Censier</a>, <a href="/search/hep-ph?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/hep-ph?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/hep-ph?searchtype=author&query=Cou%C3%ABdo%2C+F">F. Cou毛do</a>, <a href="/search/hep-ph?searchtype=author&query=Coulter%2C+P">P. Coulter</a>, <a href="/search/hep-ph?searchtype=author&query=Cox%2C+G+A">G. A. Cox</a>, <a href="/search/hep-ph?searchtype=author&query=de+Boissi%C3%A8re%2C+T">T. de Boissi猫re</a>, <a href="/search/hep-ph?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/hep-ph?searchtype=author&query=Dolgorouky%2C+Y">Y. Dolgorouky</a>, <a href="/search/hep-ph?searchtype=author&query=Drillien%2C+A+A">A. A. Drillien</a>, <a href="/search/hep-ph?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/hep-ph?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/hep-ph?searchtype=author&query=Filosofov%2C+D">D. Filosofov</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="1307.1488v1-abstract-short" style="display: inline;"> We present new constraints on the couplings of axions and more generic axion-like particles using data from the EDELWEISS-II experiment. The EDELWEISS experiment, located at the Underground Laboratory of Modane, primarily aims at the direct detection of WIMPs using germanium bolometers. It is also sensitive to the low-energy electron recoils that would be induced by solar or dark matter axions. Us… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1488v1-abstract-full').style.display = 'inline'; document.getElementById('1307.1488v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.1488v1-abstract-full" style="display: none;"> We present new constraints on the couplings of axions and more generic axion-like particles using data from the EDELWEISS-II experiment. The EDELWEISS experiment, located at the Underground Laboratory of Modane, primarily aims at the direct detection of WIMPs using germanium bolometers. It is also sensitive to the low-energy electron recoils that would be induced by solar or dark matter axions. Using a total exposure of up to 448 kg.d, we searched for axion-induced electron recoils down to 2.5 keV within four scenarios involving different hypotheses on the origin and couplings of axions. We set a 95% CL limit on the coupling to photons $g_{A纬}<2.13\times 10^{-9}$ GeV$^{-1}$ in a mass range not fully covered by axion helioscopes. We also constrain the coupling to electrons, $g_{Ae} < 2.56\times 10^{-11}$, similar to the more indirect solar neutrino bound. Finally we place a limit on $g_{Ae}\times g_{AN}^{\rm eff}<4.70 \times 10^{-17}$, where $g_{AN}^{\rm eff}$ is the effective axion-nucleon coupling for $^{57}$Fe. Combining these results we fully exclude the mass range $0.91\,{\rm eV}<m_A<80$ keV for DFSZ axions and $5.73\,{\rm eV}<m_A<40$ keV for KSVZ axions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1488v1-abstract-full').style.display = 'none'; document.getElementById('1307.1488v1-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 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 1311 (2013) 067 </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" 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