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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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/2411.12022">arXiv:2411.12022</a> <span> [<a href="https://arxiv.org/pdf/2411.12022">pdf</a>, <a href="https://arxiv.org/format/2411.12022">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a> , et al. (188 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="2411.12022v2-abstract-short" style="display: inline;"> We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been validated in a series of supporting p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12022v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12022v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12022v2-abstract-full" style="display: none;"> We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been validated in a series of supporting papers. In the flat $螞$CDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to $惟_\mathrm{m}=0.2962\pm 0.0095$, and the amplitude of mass fluctuations to $蟽_8=0.842\pm 0.034$. The addition of the cosmic microwave background (CMB) data tightens these constraints to $惟_\mathrm{m}=0.3056\pm 0.0049$ and $蟽_8=0.8121\pm 0.0053$, while further addition of the the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data leads to a 0.4% determination of the Hubble constant, $H_0 = (68.40\pm 0.27)\,{\rm km\,s^{-1}\,Mpc^{-1}}$. In models with a time-varying dark energy equation of state, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for $w_0>-1$ and $w_a<0$ with similar levels of significance. DESI data, in combination with the CMB, impose the upper limits on the sum of the neutrino masses of $\sum m_谓< 0.071\,{\rm eV}$ at 95% confidence. DESI data alone measure the modified-gravity parameter that controls the clustering of massive particles, $渭_0=0.11^{+0.45}_{-0.54}$, while the combination of DESI with the CMB and the clustering and lensing analysis from DESY3 constrains both modified-gravity parameters, giving $渭_0 = 0.04\pm 0.22$ and $危_0 = 0.044\pm 0.047$, in agreement with general relativity. [Abridged.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12022v2-abstract-full').style.display = 'none'; document.getElementById('2411.12022v2-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> 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 55 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12021">arXiv:2411.12021</a> <span> [<a href="https://arxiv.org/pdf/2411.12021">pdf</a>, <a href="https://arxiv.org/format/2411.12021">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (174 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="2411.12021v1-abstract-short" style="display: inline;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we exte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12021v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12021v1-abstract-full" style="display: none;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we extend previous DESI DR1 baryon acoustic oscillation (BAO) measurements to include redshift-space distortions and signals from the matter-radiation equality scale. For the first time, this Full-Shape analysis is blinded at the catalogue-level to avoid confirmation bias and the systematic errors are accounted for at the two-point clustering level, which automatically propagates them into any cosmological parameter. When analysing the data in terms of compressed model-agnostic variables, we obtain a combined precision of 4.7\% on the amplitude of the redshift space distortion signal reaching similar precision with just one year of DESI data than with 20 years of observation from previous generation surveys. We analyse the data to directly constrain the cosmological parameters within the $螞$CDM model using perturbation theory and combine this information with the reconstructed DESI DR1 galaxy BAO. Using a Big Bang Nucleosynthesis Gaussian prior on the baryon density parameter, and a Gaussian prior on the spectral index, we constrain the matter density is $惟_m=0.296\pm 0.010 $ and the Hubble constant $H_0=(68.63 \pm 0.79)[{\rm km\, s^{-1}Mpc^{-1}}]$. Additionally, we measure the amplitude of clustering $蟽_8=0.841 \pm 0.034$. The DESI DR1 results are in agreement with the $螞$CDM model based on general relativity with parameters consistent with those from Planck. The cosmological interpretation of these results in combination with external datasets are presented in a companion paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v1-abstract-full').style.display = 'none'; document.getElementById('2411.12021v1-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> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 76 pages, 20 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12020">arXiv:2411.12020</a> <span> [<a href="https://arxiv.org/pdf/2411.12020">pdf</a>, <a href="https://arxiv.org/format/2411.12020">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 II: Sample Definitions, Characteristics, and Two-point Clustering Statistics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (178 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="2411.12020v1-abstract-short" style="display: inline;"> We present the samples of galaxies and quasars used for DESI 2024 cosmological analyses, drawn from the DESI Data Release 1 (DR1). We describe the construction of large-scale structure (LSS) catalogs from these samples, which include matched sets of synthetic reference `randoms' and weights that account for variations in the observed density of the samples due to experimental design and varying in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12020v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12020v1-abstract-full" style="display: none;"> We present the samples of galaxies and quasars used for DESI 2024 cosmological analyses, drawn from the DESI Data Release 1 (DR1). We describe the construction of large-scale structure (LSS) catalogs from these samples, which include matched sets of synthetic reference `randoms' and weights that account for variations in the observed density of the samples due to experimental design and varying instrument performance. We detail how we correct for variations in observational completeness, the input `target' densities due to imaging systematics, and the ability to confidently measure redshifts from DESI spectra. We then summarize how remaining uncertainties in the corrections can be translated to systematic uncertainties for particular analyses. We describe the weights added to maximize the signal-to-noise of DESI DR1 2-point clustering measurements. We detail measurement pipelines applied to the LSS catalogs that obtain 2-point clustering measurements in configuration and Fourier space. The resulting 2-point measurements depend on window functions and normalization constraints particular to each sample, and we present the corrections required to match models to the data. We compare the configuration- and Fourier-space 2-point clustering of the data samples to that recovered from simulations of DESI DR1 and find they are, generally, in statistical agreement to within 2\% in the inferred real-space over-density field. The LSS catalogs, 2-point measurements, and their covariance matrices will be released publicly with DESI DR1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12020v1-abstract-full').style.display = 'none'; document.getElementById('2411.12020v1-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> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04473">arXiv:2407.04473</a> <span> [<a href="https://arxiv.org/pdf/2407.04473">pdf</a>, <a href="https://arxiv.org/format/2407.04473">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="Computational Physics">physics.comp-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/10.1093/mnras/stae2255">10.1093/mnras/stae2255 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ACCEL$^2$ project: simulating Lyman-$伪$ forest in large-volume hydrodynamical simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Chabanier%2C+S">Sol猫ne Chabanier</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Latrille%2C+L">Lucas Latrille</a>, <a href="/search/?searchtype=author&query=Sexton%2C+J">Jean Sexton</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+%C3%89">脡ric Armengaud</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">Julian Bautista</a>, <a href="/search/?searchtype=author&query=Dumerchat%2C+T">Tyann Dumerchat</a>, <a href="/search/?searchtype=author&query=Luki%C4%87%2C+Z">Zarija Luki膰</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="2407.04473v2-abstract-short" style="display: inline;"> Cosmological information is usually extracted from the Lyman-$伪$ forest correlations using only either large-scale information interpreted through linear theory or using small-scale information interpreted by means of expensive hydrodynamical simulations. A complete cosmological interpretation of the 3D correlations at all measurable scales is challenged by the need of more realistic models includ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04473v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04473v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04473v2-abstract-full" style="display: none;"> Cosmological information is usually extracted from the Lyman-$伪$ forest correlations using only either large-scale information interpreted through linear theory or using small-scale information interpreted by means of expensive hydrodynamical simulations. A complete cosmological interpretation of the 3D correlations at all measurable scales is challenged by the need of more realistic models including the complex growth of non-linear small scales that can only be studied within large hydrodynamical simulations. Past work were often limited by the trade off between the simulated cosmological volume and the resolution of the low-density intergalactic medium from which the Lyman-$伪$ signal originates. We conduct a suite of hydrodynamical simulations of the intergalactic medium, including one of the largest Lyman-$伪$ simulations ever performed in terms of volume (640 $h^{-1}\mathrm{Mpc}$), alongside simulations in smaller volumes with resolutions up to 25 $h^{-1}\mathrm{kpc}$, which will be further improved to show resolution convergence in future studies. We compare the 3D Lyman-$伪$ power spectra predicted by those simulations to different non-linear models. The inferred Lyman-$伪$ bias and redshift space distortion (RSD) parameters, $b_伪$ and $尾_伪$ are in remarkable agreement with those measured in SDSS and DESI data. We find that, contrary to intuition, the convergence of large-scale modes of the 3D Lyman-$伪$ power spectra, which determines $尾_伪$, is primarily influenced by the resolution of the simulation box through mode coupling, rather than the box size itself. Finally, we study the BAO signal encoded in the 3D Lyman-$伪$ power spectra. For the first time with a hydrodynamical simulation, we clearly detect the BAO signal, however we only marginally detect its damping, associated with the non-linear growth of the structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04473v2-abstract-full').style.display = 'none'; document.getElementById('2407.04473v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </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">17 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 534, Issue 3, November 2024, Pages 2674-2693 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14988">arXiv:2405.14988</a> <span> [<a href="https://arxiv.org/pdf/2405.14988">pdf</a>, <a href="https://arxiv.org/format/2405.14988">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> </div> </div> <p class="title is-5 mathjax"> CMB lensing and Ly伪 forest cross bispectrum from DESI's first-year quasar sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/?searchtype=author&query=Weinberg%2C+D+H">D. H. Weinberg</a>, <a href="/search/?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/?searchtype=author&query=de+Belsunce%2C+R">R. de Belsunce</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">A. X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/?searchtype=author&query=Landriau%2C+M">M. Landriau</a> , et al. (28 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="2405.14988v1-abstract-short" style="display: inline;"> The squeezed cross-bispectrum \bispeconed\ between the gravitational lensing in the Cosmic Microwave Background and the 1D \lya\ forest power spectrum can constrain bias parameters and break degeneracies between $蟽_8$ and other cosmological parameters. We detect \bispeconed\ with $4.8蟽$ significance at an effective redshift $z_\mathrm{eff}=2.4$ using Planck PR3 lensing map and over 280,000 quasar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14988v1-abstract-full').style.display = 'inline'; document.getElementById('2405.14988v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14988v1-abstract-full" style="display: none;"> The squeezed cross-bispectrum \bispeconed\ between the gravitational lensing in the Cosmic Microwave Background and the 1D \lya\ forest power spectrum can constrain bias parameters and break degeneracies between $蟽_8$ and other cosmological parameters. We detect \bispeconed\ with $4.8蟽$ significance at an effective redshift $z_\mathrm{eff}=2.4$ using Planck PR3 lensing map and over 280,000 quasar spectra from the Dark Energy Spectroscopic Instrument's first-year data. We test our measurement against metal contamination and foregrounds such as Galactic extinction and clusters of galaxies by deprojecting the thermal Sunyaev-Zeldovich effect. We compare our results to a tree-level perturbation theory calculation and find reasonable agreement between the model and measurement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14988v1-abstract-full').style.display = 'none'; document.getElementById('2405.14988v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </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">13 pages excluding references, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03569">arXiv:2404.03569</a> <span> [<a href="https://arxiv.org/pdf/2404.03569">pdf</a>, <a href="https://arxiv.org/format/2404.03569">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> </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/10.1088/1475-7516/2024/08/059">10.1088/1475-7516/2024/08/059 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High redshift LBGs from deep broadband imaging for future spectroscopic surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ruhlmann-Kleider%2C+V">Vanina Ruhlmann-Kleider</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</a>, <a href="/search/?searchtype=author&query=Magneville%2C+C">Christophe Magneville</a>, <a href="/search/?searchtype=author&query=Coquinot%2C+H">Henri Coquinot</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Raichoor%2C+A">Anand Raichoor</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/?searchtype=author&query=Arnouts%2C+S">St茅phane Arnouts</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">Edmond Chaussidon</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a> , et al. (38 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="2404.03569v5-abstract-short" style="display: inline;"> Lyman break galaxies (LBGs) are promising probes for clustering measurements at high redshift, $z>2$, a region only covered so far by Lyman-$伪$ forest measurements. In this paper, we investigate the feasibility of selecting LBGs by exploiting the existence of a strong deficit of flux shortward of the Lyman limit, due to various absorption processes along the line of sight. The target selection rel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03569v5-abstract-full').style.display = 'inline'; document.getElementById('2404.03569v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03569v5-abstract-full" style="display: none;"> Lyman break galaxies (LBGs) are promising probes for clustering measurements at high redshift, $z>2$, a region only covered so far by Lyman-$伪$ forest measurements. In this paper, we investigate the feasibility of selecting LBGs by exploiting the existence of a strong deficit of flux shortward of the Lyman limit, due to various absorption processes along the line of sight. The target selection relies on deep imaging data from the HSC and CLAUDS surveys in the $g,r,z$ and $u$ bands, respectively, with median depths reaching 27 AB in all bands. The selections were validated by several dedicated spectroscopic observation campaigns with DESI. Visual inspection of spectra has enabled us to develop an automated spectroscopic typing and redshift estimation algorithm specific to LBGs. Based on these data and tools, we assess the efficiency and purity of target selections optimised for different purposes. Selections providing a wide redshift coverage retain $57\%$ of the observed targets after spectroscopic confirmation with DESI, and provide an efficiency for LBGs of $83\pm3\%$, for a purity of the selected LBG sample of $90\pm2\%$. This would deliver a confirmed LBG density of $\sim 620$ deg$^{-2}$ in the range $2.3<z<3.5$ for a $r$-band limiting magnitude $r<24.2$. Selections optimised for high redshift efficiency retain $73\%$ of the observed targets after spectroscopic confirmation, with $89\pm4\%$ efficiency for $97\pm2\%$ purity. This would provide a confirmed LBG density of $\sim 470$ deg$^{-2}$ in the range $2.8<z<3.5$ for a $r$-band limiting magnitude $r<24.5$. A preliminary study of the LBG sample 3d-clustering properties is also presented and used to estimate the LBG linear bias. A value of $b_{LBG} = 3.3 \pm 0.2 (stat.)$ is obtained for a mean redshift of 2.9 and a limiting magnitude in $r$ of 24.2, in agreement with results reported in the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03569v5-abstract-full').style.display = 'none'; document.getElementById('2404.03569v5-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> 2 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">45 pages, 29 figures, published in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 08 (2024) 059 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03004">arXiv:2404.03004</a> <span> [<a href="https://arxiv.org/pdf/2404.03004">pdf</a>, <a href="https://arxiv.org/format/2404.03004">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> </div> </div> <p class="title is-5 mathjax"> Validation of the DESI 2024 Ly$伪$ forest BAO analysis using synthetic datasets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cuceu%2C+A">Andrei Cuceu</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">Hiram K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">Calum Gordon</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">Alma X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a> , et al. (34 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="2404.03004v2-abstract-short" style="display: inline;"> The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$伪$ (Ly$伪$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 202… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03004v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03004v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03004v2-abstract-full" style="display: none;"> The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$伪$ (Ly$伪$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 2024 Ly$伪$ forest BAO measurement. The synthetic data sets are based on Gaussian random fields using the log-normal approximation. We produce realistic synthetic DESI spectra that include all major contaminants affecting the Ly$伪$ forest. The synthetic data sets span a redshift range $1.8<z<3.8$, and are analysed using the same framework and pipeline used for the DESI 2024 Ly$伪$ forest BAO measurement. To measure BAO, we use both the Ly$伪$ auto-correlation and its cross-correlation with quasar positions. We use the mean of correlation functions from the set of DESI DR1 realizations to show that our model is able to recover unbiased measurements of the BAO position. We also fit each mock individually and study the population of BAO fits in order to validate BAO uncertainties and test our method for estimating the covariance matrix of the Ly$伪$ forest correlation functions. Finally, we discuss the implications of our results and identify the needs for the next generation of Ly$伪$ forest synthetic data sets, with the top priority being to simulate the effect of BAO broadening due to non-linear evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03004v2-abstract-full').style.display = 'none'; document.getElementById('2404.03004v2-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> 5 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">Supporting publication of DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03003">arXiv:2404.03003</a> <span> [<a href="https://arxiv.org/pdf/2404.03003">pdf</a>, <a href="https://arxiv.org/format/2404.03003">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> </div> </div> <p class="title is-5 mathjax"> Characterization of contaminants in the Lyman-alpha forest auto-correlation with DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Guti%C3%A9rrez%2C+A">A. Mu帽oz-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Pieri%2C+M">M. Pieri</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C. Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">M. Walther</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a> , et al. (39 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="2404.03003v4-abstract-short" style="display: inline;"> Baryon Acoustic Oscillations can be measured with sub-percent precision above redshift two with the Lyman-alpha forest auto-correlation and its cross-correlation with quasar positions. This is one of the key goals of the Dark Energy Spectroscopic Instrument (DESI) which started its main survey in May 2021. We present in this paper a study of the contaminants to the lyman-alpha forest which are mai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03003v4-abstract-full').style.display = 'inline'; document.getElementById('2404.03003v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03003v4-abstract-full" style="display: none;"> Baryon Acoustic Oscillations can be measured with sub-percent precision above redshift two with the Lyman-alpha forest auto-correlation and its cross-correlation with quasar positions. This is one of the key goals of the Dark Energy Spectroscopic Instrument (DESI) which started its main survey in May 2021. We present in this paper a study of the contaminants to the lyman-alpha forest which are mainly caused by correlated signals introduced by the spectroscopic data processing pipeline as well as astrophysical contaminants due to foreground absorption in the intergalactic medium. Notably, an excess signal caused by the sky background subtraction noise is present in the lyman-alpha auto-correlation in the first line-of-sight separation bin. We use synthetic data to isolate this contribution, we also characterize the effect of spectro-photometric calibration noise, and propose a simple model to account for both effects in the analysis of the lyman-alpha forest. We then measure the auto-correlation of the quasar flux transmission fraction of low redshift quasars, where there is no lyman-alpha forest absorption but only its contaminants. We demonstrate that we can interpret the data with a two-component model: data processing noise and triply ionized Silicon and Carbon auto-correlations. This result can be used to improve the modeling of the lyman-alpha auto-correlation function measured with DESI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03003v4-abstract-full').style.display = 'none'; document.getElementById('2404.03003v4-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> 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">32 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03002">arXiv:2404.03002</a> <span> [<a href="https://arxiv.org/pdf/2404.03002">pdf</a>, <a href="https://arxiv.org/format/2404.03002">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Bera%2C+A">A. Bera</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a> , et al. (178 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="2404.03002v3-abstract-short" style="display: inline;"> We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03002v3-abstract-full').style.display = 'inline'; document.getElementById('2404.03002v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03002v3-abstract-full" style="display: none;"> We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the sound horizon, in seven redshift bins from over 6 million extragalactic objects in the redshift range $0.1<z<4.2$. DESI BAO data alone are consistent with the standard flat $螞$CDM cosmological model with a matter density $惟_\mathrm{m}=0.295\pm 0.015$. Paired with a BBN prior and the robustly measured acoustic angular scale from the CMB, DESI requires $H_0=(68.52\pm0.62)$ km/s/Mpc. In conjunction with CMB anisotropies from Planck and CMB lensing data from Planck and ACT, we find $惟_\mathrm{m}=0.307\pm 0.005$ and $H_0=(67.97\pm0.38)$ km/s/Mpc. Extending the baseline model with a constant dark energy equation of state parameter $w$, DESI BAO alone require $w=-0.99^{+0.15}_{-0.13}$. In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with CMB or with SN~Ia individually prefer $w_0>-1$ and $w_a<0$. This preference is 2.6$蟽$ for the DESI+CMB combination, and persists or grows when SN~Ia are added in, giving results discrepant with the $螞$CDM model at the $2.5蟽$, $3.5蟽$ or $3.9蟽$ levels for the addition of Pantheon+, Union3, or DES-SN5YR datasets respectively. For the flat $螞$CDM model with the sum of neutrino mass $\sum m_谓$ free, combining the DESI and CMB data yields an upper limit $\sum m_谓< 0.072$ $(0.113)$ eV at 95% confidence for a $\sum m_谓>0$ $(\sum m_谓>0.059)$ eV prior. These neutrino-mass constraints are substantially relaxed in models beyond $螞$CDM. [Abridged.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03002v3-abstract-full').style.display = 'none'; document.getElementById('2404.03002v3-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). 68 pages, 15 figures. Version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03001">arXiv:2404.03001</a> <span> [<a href="https://arxiv.org/pdf/2404.03001">pdf</a>, <a href="https://arxiv.org/format/2404.03001">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/?searchtype=author&query=Brieden%2C+S">S. Brieden</a> , et al. (174 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="2404.03001v4-abstract-short" style="display: inline;"> We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$伪$ (Ly$伪$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$伪$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03001v4-abstract-full').style.display = 'inline'; document.getElementById('2404.03001v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03001v4-abstract-full" style="display: none;"> We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$伪$ (Ly$伪$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$伪$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a new analysis methodology on a blinded dataset. We conducted rigorous tests using synthetic data to ensure the reliability of our methodology and findings before unblinding. Additionally, we conducted multiple data splits to assess the consistency of the results and scrutinized various analysis approaches to confirm their robustness. For a given value of the sound horizon ($r_d$), we measure the expansion at $z_{\rm eff}=2.33$ with 2\% precision, $H(z_{\rm eff}) = (239.2 \pm 4.8) (147.09~{\rm Mpc} /r_d)$ km/s/Mpc. Similarly, we present a 2.4\% measurement of the transverse comoving distance to the same redshift, $D_M(z_{\rm eff}) = (5.84 \pm 0.14) (r_d/147.09~{\rm Mpc})$ Gpc. Together with other DESI BAO measurements at lower redshifts, these results are used in a companion paper to constrain cosmological parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03001v4-abstract-full').style.display = 'none'; document.getElementById('2404.03001v4-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> 27 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). Minor changes in v4, version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03000">arXiv:2404.03000</a> <span> [<a href="https://arxiv.org/pdf/2404.03000">pdf</a>, <a href="https://arxiv.org/format/2404.03000">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> </div> </div> <p class="title is-5 mathjax"> DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (171 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="2404.03000v1-abstract-short" style="display: inline;"> We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1<z<2.1. Divided by tracer type, we utilize 300,017 galaxies from the magnitude-limited Bright Galaxy Survey with 0.1<z<0.4, 2,138,600 Luminous Red Galaxies with 0.4<z<1.1, 2,432,022 Emission Line Galaxies with 0.8<z<1.6, and 856,652 qu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03000v1-abstract-full').style.display = 'inline'; document.getElementById('2404.03000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03000v1-abstract-full" style="display: none;"> We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1<z<2.1. Divided by tracer type, we utilize 300,017 galaxies from the magnitude-limited Bright Galaxy Survey with 0.1<z<0.4, 2,138,600 Luminous Red Galaxies with 0.4<z<1.1, 2,432,022 Emission Line Galaxies with 0.8<z<1.6, and 856,652 quasars with 0.8<z<2.1, over a ~7,500 square degree footprint. The analysis was blinded at the catalog-level to avoid confirmation bias. All fiducial choices of the BAO fitting and reconstruction methodology, as well as the size of the systematic errors, were determined on the basis of the tests with mock catalogs and the blinded data catalogs. We present several improvements to the BAO analysis pipeline, including enhancing the BAO fitting and reconstruction methods in a more physically-motivated direction, and also present results using combinations of tracers. We present a re-analysis of SDSS BOSS and eBOSS results applying the improved DESI methodology and find scatter consistent with the level of the quoted SDSS theoretical systematic uncertainties. With the total effective survey volume of ~ 18 Gpc$^3$, the combined precision of the BAO measurements across the six different redshift bins is ~0.52%, marking a 1.2-fold improvement over the previous state-of-the-art results using only first-year data. We detect the BAO in all of these six redshift bins. The highest significance of BAO detection is $9.1蟽$ at the effective redshift of 0.93, with a constraint of 0.86% placed on the BAO scale. We find our measurements are systematically larger than the prediction of Planck-2018 LCDM model at z<0.8. We translate the results into transverse comoving distance and radial Hubble distance measurements, which are used to constrain cosmological models in our companion paper [abridged]. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03000v1-abstract-full').style.display = 'none'; document.getElementById('2404.03000v1-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> 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.00303">arXiv:2401.00303</a> <span> [<a href="https://arxiv.org/pdf/2401.00303">pdf</a>, <a href="https://arxiv.org/format/2401.00303">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> </div> </div> <p class="title is-5 mathjax"> Synthetic spectra for Lyman-$伪$ forest analysis in the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">Hiram K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Guti%C3%A9rrez%2C+A">Andrea Mu帽oz-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">Ting Tan</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Morales%2C+A+X">Alma X. Gonz谩lez-Morales</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+L+%C3%81">L. 脕. Garc铆a</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">C. Gordon</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Goff%2C+J+M+L">J. M. Le Goff</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Niz%2C+G">G. Niz</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C. Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">M. Walther</a> , et al. (29 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="2401.00303v2-abstract-short" style="display: inline;"> Synthetic data sets are used in cosmology to test analysis procedures, to verify that systematic errors are well understood and to demonstrate that measurements are unbiased. In this work we describe the methods used to generate synthetic datasets of Lyman-$伪$ quasar spectra aimed for studies with the Dark Energy Spectroscopic Instrument (DESI). In particular, we focus on demonstrating that our si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00303v2-abstract-full').style.display = 'inline'; document.getElementById('2401.00303v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.00303v2-abstract-full" style="display: none;"> Synthetic data sets are used in cosmology to test analysis procedures, to verify that systematic errors are well understood and to demonstrate that measurements are unbiased. In this work we describe the methods used to generate synthetic datasets of Lyman-$伪$ quasar spectra aimed for studies with the Dark Energy Spectroscopic Instrument (DESI). In particular, we focus on demonstrating that our simulations reproduces important features of real samples, making them suitable to test the analysis methods to be used in DESI and to place limits on systematic effects on measurements of Baryon Acoustic Oscillations (BAO). We present a set of mocks that reproduce the statistical properties of the DESI early data set with good agreement. Additionally, we use full survey synthetic data to forecast the BAO scale constraining power with DESI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00303v2-abstract-full').style.display = 'none'; document.getElementById('2401.00303v2-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> 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </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">42 pages, 17 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.18996">arXiv:2310.18996</a> <span> [<a href="https://arxiv.org/pdf/2310.18996">pdf</a>, <a href="https://arxiv.org/format/2310.18996">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> </div> </div> <p class="title is-5 mathjax"> Mock data sets for the Eboss and DESI Lyman-$伪$ forest surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Etourneau%2C+T">Thomas Etourneau</a>, <a href="/search/?searchtype=author&query=Goff%2C+J+L">Jean-Marc Le Goff</a>, <a href="/search/?searchtype=author&query=Rich%2C+J">James Rich</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">Ting Tan</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">Andrei Cuceu</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">A. X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/?searchtype=author&query=Miquel%2C+R">R. Miquel</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Guti%C3%A9rrez%2C+A">A. Mu帽oz-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Nie%2C+J">J. Nie</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a> , et al. (10 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="2310.18996v2-abstract-short" style="display: inline;"> We present a publicly-available code to generate sets of mock Lyman-$伪$ (\lya) forest data that have realistic large-scale correlations including those due to the Baryonic Acoustic Oscillations (BAO). The primary purpose of these mocks is to test the analysis procedures of the Extended Baryon Oscillation Survey (eBOSS) and the Dark Energy Spectroscopy Instrument (DESI) surveys. The transmitted flu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18996v2-abstract-full').style.display = 'inline'; document.getElementById('2310.18996v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.18996v2-abstract-full" style="display: none;"> We present a publicly-available code to generate sets of mock Lyman-$伪$ (\lya) forest data that have realistic large-scale correlations including those due to the Baryonic Acoustic Oscillations (BAO). The primary purpose of these mocks is to test the analysis procedures of the Extended Baryon Oscillation Survey (eBOSS) and the Dark Energy Spectroscopy Instrument (DESI) surveys. The transmitted flux fraction, $F(位)$, of background quasars due to \lya\ absorption in the intergalactic medium (IGM) is simulated using the Fluctuating Gunn-Petterson Approximation (FGPA) applied to Gaussian random fields produced through the use of fast Fourier transforms (FFT). The output includes the IGM-\lya\ transmitted flux fraction along quasar lines of sight and a catalog of high-column-density systems appropriately placed at high-density regions of the IGM. This output serves as input to additional code that superimposes the IGM tranmission on realistic quasar spectra, adds absorption by high-column-density systems and metals, and simulates instrumental transmission and noise. Redshift space distortions (RSD) of the flux correlations are implemented by including the large-scale velocity-gradient field in the FGPA resulting in a correlation function of $F(位)$ that can be accurately predicted. One hundred realizations have been produced over the 14,000 deg$^2$ DESI survey footprint with 100 quasars per deg$^{2}$. The analysis of these realizations shows that the correlations of $F(位)$ follows the prediction within the accuracy of eBOSS survey. The most time-consuming part of the mock production occurs before application of the FGPA, and the existing pre-FGPA forests can be used to easily produce new mock sets with modified redshift-dependent bias parameters or observational conditions <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18996v2-abstract-full').style.display = 'none'; document.getElementById('2310.18996v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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">accepted by JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09116">arXiv:2310.09116</a> <span> [<a href="https://arxiv.org/pdf/2310.09116">pdf</a>, <a href="https://arxiv.org/format/2310.09116">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> </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/10.1088/1475-7516/2024/05/088">10.1088/1475-7516/2024/05/088 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the small-scale 3D Lyman-$伪$ forest power spectrum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abdul-Karim%2C+M+L">Marie Lynn Abdul-Karim</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Mention%2C+G">Guillaume Mention</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">Sol猫ne Chabanier</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Luki%C4%87%2C+Z">Zarija Luki膰</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="2310.09116v2-abstract-short" style="display: inline;"> Small-scale correlations measured in the Lyman-$伪$ (Ly$伪$) forest encode information about the intergalactic medium and the primordial matter power spectrum. In this article, we present and implement a simple method to measure the 3-dimensional power spectrum, $P_{\rm 3D}$, of the Ly$伪$ forest at wavenumbers $k$ corresponding to small, $\sim$ Mpc scales. In order to estimate $P_{\rm 3D}$ from spar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09116v2-abstract-full').style.display = 'inline'; document.getElementById('2310.09116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09116v2-abstract-full" style="display: none;"> Small-scale correlations measured in the Lyman-$伪$ (Ly$伪$) forest encode information about the intergalactic medium and the primordial matter power spectrum. In this article, we present and implement a simple method to measure the 3-dimensional power spectrum, $P_{\rm 3D}$, of the Ly$伪$ forest at wavenumbers $k$ corresponding to small, $\sim$ Mpc scales. In order to estimate $P_{\rm 3D}$ from sparsely and unevenly distributed data samples, we rely on averaging 1-dimensional Fourier Transforms, as previously carried out to estimate the 1-dimensional power spectrum of the Ly$伪$ forest, $P_{\rm 1D}$. This methodology exhibits a very low computational cost. We confirm the validity of this approach through its application to Nyx cosmological hydrodynamical simulations. Subsequently, we apply our method to the eBOSS DR16 Ly$伪$ forest sample, providing as a proof of principle, a first $P_{\rm 3D}$ measurement averaged over two redshift bins $z=2.2$ and $z=2.4$. This work highlights the potential for forthcoming $P_{\rm 3D}$ measurements, from upcoming large spectroscopic surveys, to untangle degeneracies in the cosmological interpretation of $P_{\rm 1D}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09116v2-abstract-full').style.display = 'none'; document.getElementById('2310.09116v2-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> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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">28 pages, 9 figures; matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2024)088 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.10950">arXiv:2308.10950</a> <span> [<a href="https://arxiv.org/pdf/2308.10950">pdf</a>, <a href="https://arxiv.org/format/2308.10950">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> </div> </div> <p class="title is-5 mathjax"> 3D Correlations in the Lyman-$伪$ Forest from Early DESI Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gordon%2C+C">Calum Gordon</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">Andrei Cuceu</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">Jon谩s Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Morales%2C+A+X">Alma Xochitl Gonz谩lez-Morales</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a> , et al. (34 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="2308.10950v1-abstract-short" style="display: inline;"> We present the first measurements of Lyman-$伪$ (Ly$伪$) forest correlations using early data from the Dark Energy Spectroscopic Instrument (DESI). We measure the auto-correlation of Ly$伪$ absorption using 88,509 quasars at $z>2$, and its cross-correlation with quasars using a further 147,899 tracer quasars at $z\gtrsim1.77$. Then, we fit these correlations using a 13-parameter model based on linear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10950v1-abstract-full').style.display = 'inline'; document.getElementById('2308.10950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.10950v1-abstract-full" style="display: none;"> We present the first measurements of Lyman-$伪$ (Ly$伪$) forest correlations using early data from the Dark Energy Spectroscopic Instrument (DESI). We measure the auto-correlation of Ly$伪$ absorption using 88,509 quasars at $z>2$, and its cross-correlation with quasars using a further 147,899 tracer quasars at $z\gtrsim1.77$. Then, we fit these correlations using a 13-parameter model based on linear perturbation theory and find that it provides a good description of the data across a broad range of scales. We detect the BAO peak with a signal-to-noise ratio of $3.8蟽$, and show that our measurements of the auto- and cross-correlations are fully-consistent with previous measurements by the Extended Baryon Oscillation Spectroscopic Survey (eBOSS). Even though we only use here a small fraction of the final DESI dataset, our uncertainties are only a factor of 1.7 larger than those from the final eBOSS measurement. We validate the existing analysis methods of Ly$伪$ correlations in preparation for making a robust measurement of the BAO scale with the first year of DESI data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10950v1-abstract-full').style.display = 'none'; document.getElementById('2308.10950v1-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> 21 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06316">arXiv:2306.06316</a> <span> [<a href="https://arxiv.org/pdf/2306.06316">pdf</a>, <a href="https://arxiv.org/format/2306.06316">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> </div> </div> <p class="title is-5 mathjax"> Optimal 1D Ly$伪$ Forest Power Spectrum Estimation -- III. DESI early data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">Naim G枚ksel Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+L+A">Marie Lynn Abdul Karim</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">S. Chabanier</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">A. X. Gonzalez-Morales</a> , et al. (37 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="2306.06316v3-abstract-short" style="display: inline;"> The one-dimensional power spectrum $P_{\mathrm{1D}}$ of the Ly$伪$ forest provides important information about cosmological and astrophysical parameters, including constraints on warm dark matter models, the sum of the masses of the three neutrino species, and the thermal state of the intergalactic medium. We present the first measurement of $P_{\mathrm{1D}}$ with the quadratic maximum likelihood e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06316v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06316v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06316v3-abstract-full" style="display: none;"> The one-dimensional power spectrum $P_{\mathrm{1D}}$ of the Ly$伪$ forest provides important information about cosmological and astrophysical parameters, including constraints on warm dark matter models, the sum of the masses of the three neutrino species, and the thermal state of the intergalactic medium. We present the first measurement of $P_{\mathrm{1D}}$ with the quadratic maximum likelihood estimator (QMLE) from the Dark Energy Spectroscopic Instrument (DESI) survey early data sample. This early sample of $54~600$ quasars is already comparable in size to the largest previous studies, and we conduct a thorough investigation of numerous instrumental and analysis systematic errors to evaluate their impact on DESI data with QMLE. We demonstrate the excellent performance of the spectroscopic pipeline noise estimation and the impressive accuracy of the spectrograph resolution matrix with two-dimensional image simulations of raw DESI images that we processed with the DESI spectroscopic pipeline. We also study metal line contamination and noise calibration systematics with quasar spectra on the red side of the Ly$伪$ emission line. In a companion paper, we present a similar analysis based on the Fast Fourier Transform estimate of the power spectrum. We conclude with a comparison of these two approaches and implications for the upcoming DESI Year 1 analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06316v3-abstract-full').style.display = 'none'; document.getElementById('2306.06316v3-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> 12 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </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">23 pages, 20 figures. To be published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06312">arXiv:2306.06312</a> <span> [<a href="https://arxiv.org/pdf/2306.06312">pdf</a>, <a href="https://arxiv.org/format/2306.06312">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> </div> </div> <p class="title is-5 mathjax"> The Lyman-$伪$ forest catalog from the Dark Energy Spectroscopic Instrument Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C茅sar Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">Ignasi P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Cai%2C+Z">Z. Cai</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">S. Chabanier</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">A. X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">C. Gordon</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Luki%C4%87%2C+Z">Zarija Luki膰</a>, <a href="/search/?searchtype=author&query=Manser%2C+C+J">C. J. Manser</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a> , et al. (45 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="2306.06312v6-abstract-short" style="display: inline;"> We present and validate the catalog of Lyman-$伪$ forest fluctuations for 3D analyses using the Early Data Release (EDR) from the Dark Energy Spectroscopic Instrument (DESI) survey. We used 88,511 quasars collected from DESI Survey Validation (SV) data and the first two months of the main survey (M2). We present several improvements to the method used to extract the Lyman-$伪$ absorption fluctuation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06312v6-abstract-full').style.display = 'inline'; document.getElementById('2306.06312v6-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06312v6-abstract-full" style="display: none;"> We present and validate the catalog of Lyman-$伪$ forest fluctuations for 3D analyses using the Early Data Release (EDR) from the Dark Energy Spectroscopic Instrument (DESI) survey. We used 88,511 quasars collected from DESI Survey Validation (SV) data and the first two months of the main survey (M2). We present several improvements to the method used to extract the Lyman-$伪$ absorption fluctuations performed in previous analyses from the Sloan Digital Sky Survey (SDSS). In particular, we modify the weighting scheme and show that it can improve the precision of the correlation function measurement by more than 20%. This catalog can be downloaded from https://data.desi.lbl.gov/public/edr/vac/edr/lya/fuji/v0.3 and it will be used in the near future for the first DESI measurements of the 3D correlations in the Lyman-$伪$ forest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06312v6-abstract-full').style.display = 'none'; document.getElementById('2306.06312v6-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> 25 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06311">arXiv:2306.06311</a> <span> [<a href="https://arxiv.org/pdf/2306.06311">pdf</a>, <a href="https://arxiv.org/format/2306.06311">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> </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/10.1093/mnras/stad3008">10.1093/mnras/stad3008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Spectroscopic Instrument: One-dimensional power spectrum from first Lyman-$伪$ forest samples with Fast Fourier Transform </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+L+A">Marie Lynn Abdul Karim</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">Naim G枚ksel Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">Julian Bautista</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">Sergio Felipe Beltran</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">Laura Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">Sol猫ne Chabanier</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">Edmond Chaussidon</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">Jon谩s Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">Rodrigo de la Cruz</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J">Jaime Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</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="2306.06311v3-abstract-short" style="display: inline;"> We present the one-dimensional Lyman-$伪$ forest power spectrum measurement using the first data provided by the Dark Energy Spectroscopic Instrument (DESI). The data sample comprises $26,330$ quasar spectra, at redshift $z > 2.1$, contained in the DESI Early Data Release and the first two months of the main survey. We employ a Fast Fourier Transform (FFT) estimator and compare the resulting power… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06311v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06311v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06311v3-abstract-full" style="display: none;"> We present the one-dimensional Lyman-$伪$ forest power spectrum measurement using the first data provided by the Dark Energy Spectroscopic Instrument (DESI). The data sample comprises $26,330$ quasar spectra, at redshift $z > 2.1$, contained in the DESI Early Data Release and the first two months of the main survey. We employ a Fast Fourier Transform (FFT) estimator and compare the resulting power spectrum to an alternative likelihood-based method in a companion paper. We investigate methodological and instrumental contaminants associated to the new DESI instrument, applying techniques similar to previous Sloan Digital Sky Survey (SDSS) measurements. We use synthetic data based on log-normal approximation to validate and correct our measurement. We compare our resulting power spectrum with previous SDSS and high-resolution measurements. With relatively small number statistics, we successfully perform the FFT measurement, which is already competitive in terms of the scale range. At the end of the DESI survey, we expect a five times larger Lyman-$伪$ forest sample than SDSS, providing an unprecedented precise one-dimensional power spectrum measurement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06311v3-abstract-full').style.display = 'none'; document.getElementById('2306.06311v3-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> 24 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </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">23 pages, 23 figures, Journal version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, Volume 526, Issue 4, December 2023, Pages 5118-5140 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06308">arXiv:2306.06308</a> <span> [<a href="https://arxiv.org/pdf/2306.06308">pdf</a>, <a href="https://arxiv.org/format/2306.06308">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> </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/10.3847/1538-3881/ad3217">10.3847/1538-3881/ad3217 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Data Release of the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (244 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="2306.06308v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06308v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06308v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'none'; document.getElementById('2306.06308v3-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> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </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">43 pages, 7 figures, 17 tables, accepted for publication in the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ 168 58 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06307">arXiv:2306.06307</a> <span> [<a href="https://arxiv.org/pdf/2306.06307">pdf</a>, <a href="https://arxiv.org/format/2306.06307">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> </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/10.5281/zenodo.7858207">10.5281/zenodo.7858207 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (239 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="2306.06307v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06307v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06307v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg$^2$ using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg$^2$ program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval $z<1.1$, 0.39% over the redshift interval $1.1<z<1.9$, and 0.46% over the redshift interval $1.9<z<3.5$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'none'; document.getElementById('2306.06307v3-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> 12 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </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">42 pages, 18 figures, accepted by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.10426">arXiv:2305.10426</a> <span> [<a href="https://arxiv.org/pdf/2305.10426">pdf</a>, <a href="https://arxiv.org/format/2305.10426">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.3847/1538-3881/ace35d">10.3847/1538-3881/ace35d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the Quasar Spectral Templates for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Brodzeller%2C+A">Allyson Brodzeller</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/?searchtype=author&query=Yu%2C+J">Jiaxi Yu</a>, <a href="/search/?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Filbert%2C+S">S. Filbert</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/?searchtype=author&query=Fawcett%2C+V+A">V. A. Fawcett</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/?searchtype=author&query=Kisner%2C+T">T. Kisner</a> , et al. (22 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="2305.10426v2-abstract-short" style="display: inline;"> Millions of quasar spectra will be collected by the Dark Energy Spectroscopic Instrument (DESI), leading to a four-fold increase in the number of known quasars. High accuracy quasar classification is essential to tighten constraints on cosmological parameters measured at the highest redshifts DESI observes ($z>2.0$). We present the spectral templates for identification and redshift estimation of q… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10426v2-abstract-full').style.display = 'inline'; document.getElementById('2305.10426v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.10426v2-abstract-full" style="display: none;"> Millions of quasar spectra will be collected by the Dark Energy Spectroscopic Instrument (DESI), leading to a four-fold increase in the number of known quasars. High accuracy quasar classification is essential to tighten constraints on cosmological parameters measured at the highest redshifts DESI observes ($z>2.0$). We present the spectral templates for identification and redshift estimation of quasars in the DESI Year 1 data release. The quasar templates are comprised of two quasar eigenspectra sets, trained on spectra from the Sloan Digital Sky Survey. The sets are specialized to reconstruct quasar spectral variation observed over separate yet overlapping redshift ranges and, together, are capable of identifying DESI quasars from $0.05 < z <7.0$. The new quasar templates show significant improvement over the previous DESI quasar templates regarding catastrophic failure rates, redshift precision and accuracy, quasar completeness, and the contamination fraction in the final quasar sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10426v2-abstract-full').style.display = 'none'; document.getElementById('2305.10426v2-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> 3 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </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">to be published in Astronomical Journal; 21 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08517">arXiv:2208.08517</a> <span> [<a href="https://arxiv.org/pdf/2208.08517">pdf</a>, <a href="https://arxiv.org/format/2208.08517">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.3847/1538-3881/acacfc">10.3847/1538-3881/acacfc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Davis%2C+T+M">Tamara M. Davis</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/?searchtype=author&query=Fawcett%2C+V+A">V. A. Fawcett</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">Alma X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Lan%2C+T">Ting-Wen Lan</a>, <a href="/search/?searchtype=author&query=Yeche%2C+C">Christophe Yeche</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J+N">J. N. Aguilar</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Cai%2C+Z">Z. Cai</a>, <a href="/search/?searchtype=author&query=Canning%2C+R">R. Canning</a>, <a href="/search/?searchtype=author&query=Carr%2C+A">A. Carr</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">S. Chabanier</a>, <a href="/search/?searchtype=author&query=Cousinou%2C+M">Marie-Claude Cousinou</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/?searchtype=author&query=Dhungana%2C+G">G. Dhungana</a>, <a href="/search/?searchtype=author&query=Edge%2C+A+C">A. C. Edge</a>, <a href="/search/?searchtype=author&query=Eftekharzadeh%2C+S">S. Eftekharzadeh</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a> , et al. (47 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="2208.08517v3-abstract-short" style="display: inline;"> A key component of the Dark Energy Spectroscopic Instrument (DESI) survey validation (SV) is a detailed visual inspection (VI) of the optical spectroscopic data to quantify key survey metrics. In this paper we present results from VI of the quasar survey using deep coadded SV spectra. We show that the majority (~70%) of the main-survey targets are spectroscopically confirmed as quasars, with ~16%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08517v3-abstract-full').style.display = 'inline'; document.getElementById('2208.08517v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08517v3-abstract-full" style="display: none;"> A key component of the Dark Energy Spectroscopic Instrument (DESI) survey validation (SV) is a detailed visual inspection (VI) of the optical spectroscopic data to quantify key survey metrics. In this paper we present results from VI of the quasar survey using deep coadded SV spectra. We show that the majority (~70%) of the main-survey targets are spectroscopically confirmed as quasars, with ~16% galaxies, ~6% stars, and ~8% low-quality spectra lacking reliable features. A non-negligible fraction of the quasars are misidentified by the standard spectroscopic pipeline but we show that the majority can be recovered using post-pipeline "afterburner" quasar-identification approaches. We combine these "afterburners" with our standard pipeline to create a modified pipeline to improve the overall quasar yield. At the depth of the main DESI survey both pipelines achieve a good-redshift purity (reliable redshifts measured within 3000 km/s) of ~99%; however, the modified pipeline recovers ~94% of the visually inspected quasars, as compared to ~86% from the standard pipeline. We demonstrate that both pipelines achieve an median redshift precision and accuracy of ~100 km/s and ~70 km/s, respectively. We constructed composite spectra to investigate why some quasars are missed by the standard spectroscopic pipeline and find that they are more host-galaxy dominated (i.e., distant analogs of "Seyfert galaxies") and/or dust reddened than the standard-pipeline quasars. We also show example spectra to demonstrate the overall diversity of the DESI quasar sample and provide strong-lensing candidates where two targets contribute to a single spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08517v3-abstract-full').style.display = 'none'; document.getElementById('2208.08517v3-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> 28 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </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">Astronomical journal (in press). 26 pages, 15 figures, 9 tables, one of a suite of 8 papers detailing targeting for DESI. Figure data available from Zenodo (see paper for details)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08516">arXiv:2208.08516</a> <span> [<a href="https://arxiv.org/pdf/2208.08516">pdf</a>, <a href="https://arxiv.org/format/2208.08516">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="Astrophysics of Galaxies">astro-ph.GA</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/10.3847/1538-4357/aca5fa">10.3847/1538-4357/aca5fa <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The DESI Survey Validation: Results from Visual Inspection of Bright Galaxies, Luminous Red Galaxies, and Emission Line Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lan%2C+T">Ting-Wen Lan</a>, <a href="/search/?searchtype=author&query=Tojeiro%2C+R">R. Tojeiro</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Prochaska%2C+J+X">J. Xavier Prochaska</a>, <a href="/search/?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Raichoor%2C+A">A. Raichoor</a>, <a href="/search/?searchtype=author&query=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/?searchtype=author&query=Yeche%2C+C">Christophe Yeche</a>, <a href="/search/?searchtype=author&query=Balland%2C+C">C. Balland</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Canning%2C+R">R. Canning</a>, <a href="/search/?searchtype=author&query=Carr%2C+A">A. Carr</a>, <a href="/search/?searchtype=author&query=Chittenden%2C+H">H. Chittenden</a>, <a href="/search/?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/?searchtype=author&query=Cousinou%2C+M+-">M. -C. Cousinou</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/?searchtype=author&query=Douglass%2C+K">K. Douglass</a>, <a href="/search/?searchtype=author&query=Edge%2C+A">A. Edge</a>, <a href="/search/?searchtype=author&query=Escoffier%2C+S">S. Escoffier</a>, <a href="/search/?searchtype=author&query=Glanville%2C+A">A. Glanville</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a> , et al. (57 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="2208.08516v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) Survey has obtained a set of spectroscopic measurements of galaxies to validate the final survey design and target selections. To assist in these tasks, we visually inspect (VI) DESI spectra of approximately 2,500 bright galaxies, 3,500 luminous red galaxies (LRGs), and 10,000 emission line galaxies (ELGs), to obtain robust redshift identifications.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08516v3-abstract-full').style.display = 'inline'; document.getElementById('2208.08516v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08516v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) Survey has obtained a set of spectroscopic measurements of galaxies to validate the final survey design and target selections. To assist in these tasks, we visually inspect (VI) DESI spectra of approximately 2,500 bright galaxies, 3,500 luminous red galaxies (LRGs), and 10,000 emission line galaxies (ELGs), to obtain robust redshift identifications. We then utilize the VI redshift information to characterize the performance of the DESI operation. Based on the VI catalogs, our results show that the final survey design yields samples of bright galaxies, LRGs, and ELGs with purity greater than $99\%$. Moreover, we demonstrate that the precision of the redshift measurements is approximately 10 km/s for bright galaxies and ELGs and approximately 40 km/s for LRGs. The average redshift accuracy is within 10 km/s for the three types of galaxies. The VI process also helps improve the quality of the DESI data by identifying spurious spectral features introduced by the pipeline. Finally, we show examples of unexpected real astronomical objects, such as Ly$伪$ emitters and strong lensing candidates, identified by VI. These results demonstrate the importance and utility of visually inspecting data from incoming and upcoming surveys, especially during their early operation phases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08516v3-abstract-full').style.display = 'none'; document.getElementById('2208.08516v3-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> 15 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </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">22 pages, 14 figures, 3 tables, one of a suite of 8 papers detailing targeting for DESI. ApJ accepted version with minor textual updates</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023 ApJ 943 68 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.10939">arXiv:2205.10939</a> <span> [<a href="https://arxiv.org/pdf/2205.10939">pdf</a>, <a href="https://arxiv.org/format/2205.10939">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.3847/1538-3881/ac882b">10.3847/1538-3881/ac882b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abareshi%2C+B">B. Abareshi</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Ameel%2C+J">J. Ameel</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">Alejandro Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/?searchtype=author&query=Benavides%2C+B">B. Benavides</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besuner%2C+R">R. Besuner</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a> , et al. (242 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="2205.10939v1-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'inline'; document.getElementById('2205.10939v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.10939v1-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt脜 > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'none'; document.getElementById('2205.10939v1-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> 22 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </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">78 pages, 32 figures, submitted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.11045">arXiv:2203.11045</a> <span> [<a href="https://arxiv.org/pdf/2203.11045">pdf</a>, <a href="https://arxiv.org/format/2203.11045">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> </div> </div> <p class="title is-5 mathjax"> First measurement of the correlation between cosmic voids and the Lyman-$伪$ forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">Julian Bautista</a>, <a href="/search/?searchtype=author&query=Goff%2C+J+L">Jean-Marc Le Goff</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Rich%2C+J">James Rich</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</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="2203.11045v1-abstract-short" style="display: inline;"> We report the first detection of large-scale matter flows around cosmic voids at a median redshift z = 2.49. Voids are identified within a tomographic map of the large-scale matter density built from eBOSS Lyman-$伪$ (Lya) forests in SDSS Stripe 82. We measure the imprint of flows around voids, known as redshift-space distortions (RSD), with a statistical significance of 10 $蟽$. The observed quadru… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11045v1-abstract-full').style.display = 'inline'; document.getElementById('2203.11045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.11045v1-abstract-full" style="display: none;"> We report the first detection of large-scale matter flows around cosmic voids at a median redshift z = 2.49. Voids are identified within a tomographic map of the large-scale matter density built from eBOSS Lyman-$伪$ (Lya) forests in SDSS Stripe 82. We measure the imprint of flows around voids, known as redshift-space distortions (RSD), with a statistical significance of 10 $蟽$. The observed quadrupole of the void-forest cross-correlation is described by a linear RSD model. The derived RSD parameter is $尾= 0.52 \pm 0.05$. Our model accounts for the tomographic effect induced by the Lya data being located along parallel quasar lines of sight. This work paves the way towards growth-rate measurements at redshifts currently inaccessible to galaxy surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11045v1-abstract-full').style.display = 'none'; document.getElementById('2203.11045v1-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> 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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">5 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07491">arXiv:2203.07491</a> <span> [<a href="https://arxiv.org/pdf/2203.07491">pdf</a>, <a href="https://arxiv.org/ps/2203.07491">ps</a>, <a href="https://arxiv.org/format/2203.07491">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Snowmass2021 Cosmic Frontier White Paper: Prospects for obtaining Dark Matter Constraints with DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Valluri%2C+M">Monica Valluri</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">Solene Chabanier</a>, <a href="/search/?searchtype=author&query=Irsic%2C+V">Vid Irsic</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Rockosi%2C+C">Connie Rockosi</a>, <a href="/search/?searchtype=author&query=Sanchez-Conde%2C+M+A">Miguel A. Sanchez-Conde</a>, <a href="/search/?searchtype=author&query=Silva%2C+L+B+e">Leandro Beraldo e Silva</a>, <a href="/search/?searchtype=author&query=Cooper%2C+A+P">Andrew P. Cooper</a>, <a href="/search/?searchtype=author&query=Darragh-Ford%2C+E">Elise Darragh-Ford</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/?searchtype=author&query=Deason%2C+A+J">Alis J. Deason</a>, <a href="/search/?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Garzilli%2C+A">Antonella Garzilli</a>, <a href="/search/?searchtype=author&query=Li%2C+T">Ting Li</a>, <a href="/search/?searchtype=author&query=Lukic%2C+Z">Zarija Lukic</a>, <a href="/search/?searchtype=author&query=Manser%2C+C+J">Christopher J. Manser</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">Ting Tan</a>, <a href="/search/?searchtype=author&query=Wang%2C+W">Wenting Wang</a>, <a href="/search/?searchtype=author&query=Wechsler%2C+R">Risa Wechsler</a>, <a href="/search/?searchtype=author&query=Carrillo%2C+A">Andreia Carrillo</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">Arjun Dey</a> , et al. (7 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="2203.07491v2-abstract-short" style="display: inline;"> Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on thei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07491v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07491v2-abstract-full" style="display: none;"> Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on their properties can ONLY be arrived at using astrophysical observations. The Dark Energy Spectroscopic Instrument (DESI) is currently one of the most powerful instruments for wide-field surveys. The synergy of DESI with ESA's Gaia satellite and future observing facilities will yield datasets of unprecedented size and coverage that will enable constraints on DM over a wide range of physical and mass scales and across redshifts. DESI will obtain spectra of the Lyman-alpha forest out to z~5 by detecting about 1 million QSO spectra that will put constraints on clustering of the low-density intergalactic gas and DM halos at high redshift. DESI will obtain radial velocities of 10 million stars in the Milky Way (MW) and Local Group satellites enabling us to constrain their global DM distributions, as well as the DM distribution on smaller scales. The paradigm of cosmological structure formation has been extensively tested with simulations. However, the majority of simulations to date have focused on collisionless CDM. Simulations with alternatives to CDM have recently been gaining ground but are still in their infancy. While there are numerous publicly available large-box and zoom-in simulations in the LCDM framework, there are no comparable publicly available WDM, SIDM, FDM simulations. DOE support for a public simulation suite will enable a more cohesive community effort to compare observations from DESI (and other surveys) with numerical predictions and will greatly impact DM science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07491v2-abstract-full').style.display = 'none'; document.getElementById('2203.07491v2-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> 1 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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">Contributed white paper to Snowmass 2021, CF03; minor revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.03993">arXiv:2203.03993</a> <span> [<a href="https://arxiv.org/pdf/2203.03993">pdf</a>, <a href="https://arxiv.org/format/2203.03993">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</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/PhysRevD.106.062004">10.1103/PhysRevD.106.062004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for sub-GeV Dark Matter via Migdal effect with an EDELWEISS germanium detector with NbSi TES sensors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Caze%2C+A">A. Caze</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=De+J%C3%A9sus%2C+M">M. De J茅sus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/?searchtype=author&query=Filippini%2C+J+B">J. B. Filippini</a>, <a href="/search/?searchtype=author&query=Filosofov%2C+D">D. Filosofov</a>, <a href="/search/?searchtype=author&query=Gascon%2C+J">J. Gascon</a>, <a href="/search/?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/?searchtype=author&query=Gros%2C+M">M. Gros</a>, <a href="/search/?searchtype=author&query=Guy%2C+E">E. Guy</a>, <a href="/search/?searchtype=author&query=Jin%2C+Y">Y. Jin</a>, <a href="/search/?searchtype=author&query=Juillard%2C+A">A. Juillard</a>, <a href="/search/?searchtype=author&query=Kleifges%2C+M">M. Kleifges</a>, <a href="/search/?searchtype=author&query=Lattaud%2C+H">H. Lattaud</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a> , et al. (15 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="2203.03993v4-abstract-short" style="display: inline;"> The EDELWEISS collaboration reports on the search for Dark Matter (DM) particle interactions via Migdal effect with masses between $32$ MeV$\cdot$c$^{-2}$ to $2$ GeV$\cdot$c$^{-2}$ using a $200$ g cryogenic Ge detector sensitive to simultaneously heat and ionization signals and operated underground at the Laboratoire Souterrain de Modane in France. The phonon signal was read out using a Transition… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.03993v4-abstract-full').style.display = 'inline'; document.getElementById('2203.03993v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.03993v4-abstract-full" style="display: none;"> The EDELWEISS collaboration reports on the search for Dark Matter (DM) particle interactions via Migdal effect with masses between $32$ MeV$\cdot$c$^{-2}$ to $2$ GeV$\cdot$c$^{-2}$ using a $200$ g cryogenic Ge detector sensitive to simultaneously heat and ionization signals and operated underground at the Laboratoire Souterrain de Modane in France. The phonon signal was read out using a Transition Edge Sensor made of a NbSi thin film. The detector was biased at $66$ V in order to benefit from the Neganov-Trofimov-Luke amplification and resulting in a resolution on the energy of electron recoils of $4.46$ eV$_{ee}$ (RMS) and an analysis threshold of $30$ eV$_{ee}$. The sensitivity is limited by a dominant background not associated to charge creation in the detector. The search constrains a new region of parameter space for cross-sections down to $10^{-29}$ cm$^2$ and masses between $32$ and $100$ MeV$\cdot$c$^{-2}$. The achieved low threshold with the NbSi sensor shows the relevance of its use for athermal-phonon sensitive devices for low-mass DM searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.03993v4-abstract-full').style.display = 'none'; document.getElementById('2203.03993v4-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> 3 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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">10 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 106, 062004 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.05097">arXiv:2202.05097</a> <span> [<a href="https://arxiv.org/pdf/2202.05097">pdf</a>, <a href="https://arxiv.org/format/2202.05097">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 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/10.21468/SciPostPhysProc.9.001">10.21468/SciPostPhysProc.9.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EXCESS workshop: Descriptions of rising low-energy spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Adari%2C+P">P. Adari</a>, <a href="/search/?searchtype=author&query=Aguilar-Arevalo%2C+A">A. Aguilar-Arevalo</a>, <a href="/search/?searchtype=author&query=Amidei%2C+D">D. Amidei</a>, <a href="/search/?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Balogh%2C+L">L. Balogh</a>, <a href="/search/?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/?searchtype=author&query=Baxter%2C+D">D. Baxter</a>, <a href="/search/?searchtype=author&query=Beaufort%2C+C">C. Beaufort</a>, <a href="/search/?searchtype=author&query=Beaulieu%2C+G">G. Beaulieu</a>, <a href="/search/?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/?searchtype=author&query=Gal%2C+Y+B">Y. Ben Gal</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/?searchtype=author&query=Bhattacharyya%2C+R">R. Bhattacharyya</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Bloch%2C+I+M">I. M. Bloch</a>, <a href="/search/?searchtype=author&query=Botti%2C+A">A. Botti</a>, <a href="/search/?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/?searchtype=author&query=Bres%2C+G">G. Bres</a>, <a href="/search/?searchtype=author&query=Bret%2C+J+L">J-. L. Bret</a> , et al. (281 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="2202.05097v2-abstract-short" style="display: inline;"> Many low-threshold experiments observe sharply rising event rates of yet unknown origins below a few hundred eV, and larger than expected from known backgrounds. Due to the significant impact of this excess on the dark matter or neutrino sensitivity of these experiments, a collective effort has been started to share the knowledge about the individual observations. For this, the EXCESS Workshop was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05097v2-abstract-full').style.display = 'inline'; document.getElementById('2202.05097v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.05097v2-abstract-full" style="display: none;"> Many low-threshold experiments observe sharply rising event rates of yet unknown origins below a few hundred eV, and larger than expected from known backgrounds. Due to the significant impact of this excess on the dark matter or neutrino sensitivity of these experiments, a collective effort has been started to share the knowledge about the individual observations. For this, the EXCESS Workshop was initiated. In its first iteration in June 2021, ten rare event search collaborations contributed to this initiative via talks and discussions. The contributing collaborations were CONNIE, CRESST, DAMIC, EDELWEISS, MINER, NEWS-G, NUCLEUS, RICOCHET, SENSEI and SuperCDMS. They presented data about their observed energy spectra and known backgrounds together with details about the respective measurements. In this paper, we summarize the presented information and give a comprehensive overview of the similarities and differences between the distinct measurements. The provided data is furthermore publicly available on the workshop's data repository together with a plotting tool for visualization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05097v2-abstract-full').style.display = 'none'; document.getElementById('2202.05097v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </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">44 pages, 20 figures; Editors: A. Fuss, M. Kaznacheeva, F. Reindl, F. Wagner; updated copyright statements and funding information</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SciPost Phys. Proc. 9, 001 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.01639">arXiv:2201.01639</a> <span> [<a href="https://arxiv.org/pdf/2201.01639">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 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/10.1007/s10909-022-02899-2">10.1007/s10909-022-02899-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High impedance TES bolometers for EDELWEISS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=De+J%C3%A9sus%2C+M">M. De J茅sus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/?searchtype=author&query=Fillipini%2C+J+-">J. -B. Fillipini</a>, <a href="/search/?searchtype=author&query=Filosofov%2C+D">D. Filosofov</a>, <a href="/search/?searchtype=author&query=Gascon%2C+J">J. Gascon</a>, <a href="/search/?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/?searchtype=author&query=Gros%2C+M">M. Gros</a>, <a href="/search/?searchtype=author&query=Jin%2C+Y">Y. Jin</a>, <a href="/search/?searchtype=author&query=Juillard%2C+A">A. Juillard</a>, <a href="/search/?searchtype=author&query=Kleifges%2C+M">M. Kleifges</a>, <a href="/search/?searchtype=author&query=Lattaud%2C+H">H. Lattaud</a>, <a href="/search/?searchtype=author&query=Misiak%2C+D">D. Misiak</a> , et al. (13 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="2201.01639v1-abstract-short" style="display: inline;"> The EDELWEISS collaboration aims for direct detection of light dark matter using germanium cryogenic detectors with low threshold phonon sensor technologies and efficient charge readout designs. We describe here the development of Ge bolometers equipped with high impedance thermistors based on a NbxSi1-x TES alloy. High aspect ratio spiral designs allow the TES impedance to match with JFET or HEMT… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01639v1-abstract-full').style.display = 'inline'; document.getElementById('2201.01639v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01639v1-abstract-full" style="display: none;"> The EDELWEISS collaboration aims for direct detection of light dark matter using germanium cryogenic detectors with low threshold phonon sensor technologies and efficient charge readout designs. We describe here the development of Ge bolometers equipped with high impedance thermistors based on a NbxSi1-x TES alloy. High aspect ratio spiral designs allow the TES impedance to match with JFET or HEMT front-end amplifiers. We detail the behavior of the superconducting transition properties of these sensors and the detector optimization in terms of sensitivity to out-of-equilibrium phonons. We report preliminary results of a 200 g Ge detector that was calibrated using 71Ge activation by neutrons at the LSM underground laboratory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01639v1-abstract-full').style.display = 'none'; document.getElementById('2201.01639v1-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> 5 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </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">Submitted to Journal of Low Temperature Physics, Special Issue for the 19th International Workshop on Low Temperature Detectors 19-29 July 2021 (Virtual event hold by NIST)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.05467">arXiv:2112.05467</a> <span> [<a href="https://arxiv.org/pdf/2112.05467">pdf</a>, <a href="https://arxiv.org/format/2112.05467">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> </div> </div> <p class="title is-5 mathjax"> Low-mass Dark Matter searches with EDELWEISS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gascon%2C+J">J. Gascon</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=De+J%C3%A9sus%2C+M">M. De J茅sus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/?searchtype=author&query=Filippini%2C+J+-">J. -B. Filippini</a>, <a href="/search/?searchtype=author&query=Filosofov%2C+D">D. Filosofov</a>, <a href="/search/?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/?searchtype=author&query=Gros%2C+M">M. Gros</a>, <a href="/search/?searchtype=author&query=Jin%2C+Y">Y. Jin</a>, <a href="/search/?searchtype=author&query=Juillard%2C+A">A. Juillard</a>, <a href="/search/?searchtype=author&query=Kleifges%2C+M">M. Kleifges</a>, <a href="/search/?searchtype=author&query=Lattaud%2C+H">H. Lattaud</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Misiak%2C+D">D. Misiak</a> , et al. (13 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="2112.05467v2-abstract-short" style="display: inline;"> The EDELWEISS collaboration searches for light Dark Matter (DM) particles using germanium detectors equipped with a charge and phonon signal readout. Using the Neganov-Trofimov-Luke effect, an rms resolution of 0.53 electron-hole pair was obtained on a massive (33.4 g) Ge detector operated underground at the Laboratoire Souterrain de Modane. This record sensitivity made possible a search for Dark… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.05467v2-abstract-full').style.display = 'inline'; document.getElementById('2112.05467v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.05467v2-abstract-full" style="display: none;"> The EDELWEISS collaboration searches for light Dark Matter (DM) particles using germanium detectors equipped with a charge and phonon signal readout. Using the Neganov-Trofimov-Luke effect, an rms resolution of 0.53 electron-hole pair was obtained on a massive (33.4 g) Ge detector operated underground at the Laboratoire Souterrain de Modane. This record sensitivity made possible a search for Dark Photon DM down to 1 eV/c2 and to DM-electron interactions below 1 MeV/c2. This demonstrates for the first time the high relevance of cryogenic Ge detectors in searches at low thresholds and is an important step of the development of Ge detectors with improved performance in the context of the EDELWEISS-SubGeV program. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.05467v2-abstract-full').style.display = 'none'; document.getElementById('2112.05467v2-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> 10 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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">Submitted to Journal of Low Temperature Physics, Special Issue for the 19th International Workshop on Low Temperature Detectors 19-29 July 2021 (Virtual event hold by NIST)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.06543">arXiv:2107.06543</a> <span> [<a href="https://arxiv.org/pdf/2107.06543">pdf</a>, <a href="https://arxiv.org/format/2107.06543">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> </div> <p class="title is-5 mathjax"> TEACHING -- Trustworthy autonomous cyber-physical applications through human-centred intelligence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bacciu%2C+D">Davide Bacciu</a>, <a href="/search/?searchtype=author&query=Akarmazyan%2C+S">Siranush Akarmazyan</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Bacco%2C+M">Manlio Bacco</a>, <a href="/search/?searchtype=author&query=Bravos%2C+G">George Bravos</a>, <a href="/search/?searchtype=author&query=Calandra%2C+C">Calogero Calandra</a>, <a href="/search/?searchtype=author&query=Carlini%2C+E">Emanuele Carlini</a>, <a href="/search/?searchtype=author&query=Carta%2C+A">Antonio Carta</a>, <a href="/search/?searchtype=author&query=Cassara%2C+P">Pietro Cassara</a>, <a href="/search/?searchtype=author&query=Coppola%2C+M">Massimo Coppola</a>, <a href="/search/?searchtype=author&query=Davalas%2C+C">Charalampos Davalas</a>, <a href="/search/?searchtype=author&query=Dazzi%2C+P">Patrizio Dazzi</a>, <a href="/search/?searchtype=author&query=Degennaro%2C+M+C">Maria Carmela Degennaro</a>, <a href="/search/?searchtype=author&query=Di+Sarli%2C+D">Daniele Di Sarli</a>, <a href="/search/?searchtype=author&query=Dobaj%2C+J">J眉rgen Dobaj</a>, <a href="/search/?searchtype=author&query=Gallicchio%2C+C">Claudio Gallicchio</a>, <a href="/search/?searchtype=author&query=Girbal%2C+S">Sylvain Girbal</a>, <a href="/search/?searchtype=author&query=Gotta%2C+A">Alberto Gotta</a>, <a href="/search/?searchtype=author&query=Groppo%2C+R">Riccardo Groppo</a>, <a href="/search/?searchtype=author&query=Lomonaco%2C+V">Vincenzo Lomonaco</a>, <a href="/search/?searchtype=author&query=Macher%2C+G">Georg Macher</a>, <a href="/search/?searchtype=author&query=Mazzei%2C+D">Daniele Mazzei</a>, <a href="/search/?searchtype=author&query=Mencagli%2C+G">Gabriele Mencagli</a>, <a href="/search/?searchtype=author&query=Michail%2C+D">Dimitrios Michail</a>, <a href="/search/?searchtype=author&query=Micheli%2C+A">Alessio Micheli</a> , et al. (10 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="2107.06543v1-abstract-short" style="display: inline;"> This paper discusses the perspective of the H2020 TEACHING project on the next generation of autonomous applications running in a distributed and highly heterogeneous environment comprising both virtual and physical resources spanning the edge-cloud continuum. TEACHING puts forward a human-centred vision leveraging the physiological, emotional, and cognitive state of the users as a driver for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.06543v1-abstract-full').style.display = 'inline'; document.getElementById('2107.06543v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.06543v1-abstract-full" style="display: none;"> This paper discusses the perspective of the H2020 TEACHING project on the next generation of autonomous applications running in a distributed and highly heterogeneous environment comprising both virtual and physical resources spanning the edge-cloud continuum. TEACHING puts forward a human-centred vision leveraging the physiological, emotional, and cognitive state of the users as a driver for the adaptation and optimization of the autonomous applications. It does so by building a distributed, embedded and federated learning system complemented by methods and tools to enforce its dependability, security and privacy preservation. The paper discusses the main concepts of the TEACHING approach and singles out the main AI-related research challenges associated with it. Further, we provide a discussion of the design choices for the TEACHING system to tackle the aforementioned challenges <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.06543v1-abstract-full').style.display = 'none'; document.getElementById('2107.06543v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.01729">arXiv:2106.01729</a> <span> [<a href="https://arxiv.org/pdf/2106.01729">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Software Engineering">cs.SE</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/10.1007/978-3-319-66972-4_13">10.1007/978-3-319-66972-4_13 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> DEIS: Dependability Engineering Innovation for Industrial CPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">Erik Armengaud</a>, <a href="/search/?searchtype=author&query=Macher%2C+G">Georg Macher</a>, <a href="/search/?searchtype=author&query=Massoner%2C+A">Alexander Massoner</a>, <a href="/search/?searchtype=author&query=Frager%2C+S">Sebastian Frager</a>, <a href="/search/?searchtype=author&query=Adler%2C+R">Rasmus Adler</a>, <a href="/search/?searchtype=author&query=Schneider%2C+D">Daniel Schneider</a>, <a href="/search/?searchtype=author&query=Longo%2C+S">Simone Longo</a>, <a href="/search/?searchtype=author&query=Melis%2C+M">Massimiliano Melis</a>, <a href="/search/?searchtype=author&query=Groppo%2C+R">Riccardo Groppo</a>, <a href="/search/?searchtype=author&query=Villa%2C+F">Federica Villa</a>, <a href="/search/?searchtype=author&query=OLeary%2C+P">Padraig OLeary</a>, <a href="/search/?searchtype=author&query=Bambury%2C+K">Kevin Bambury</a>, <a href="/search/?searchtype=author&query=Anita%2C+F">Finnegan Anita</a>, <a href="/search/?searchtype=author&query=Zeller%2C+M">Marc Zeller</a>, <a href="/search/?searchtype=author&query=Hoefig%2C+K">Kai Hoefig</a>, <a href="/search/?searchtype=author&query=Papadopoulos%2C+Y">Yiannis Papadopoulos</a>, <a href="/search/?searchtype=author&query=Hawkins%2C+R">Richard Hawkins</a>, <a href="/search/?searchtype=author&query=Kelly%2C+T">Tim Kelly</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="2106.01729v1-abstract-short" style="display: inline;"> The open and cooperative nature of Cyber-Physical Systems (CPS) poses new challenges in assuring dependability. The DEIS project (Dependability Engineering Innovation for automotive CPS. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 732242, see http://www.deis-project.eu) addresses these challenges by developing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01729v1-abstract-full').style.display = 'inline'; document.getElementById('2106.01729v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.01729v1-abstract-full" style="display: none;"> The open and cooperative nature of Cyber-Physical Systems (CPS) poses new challenges in assuring dependability. The DEIS project (Dependability Engineering Innovation for automotive CPS. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 732242, see http://www.deis-project.eu) addresses these challenges by developing technologies that form a science of dependable system integration. In the core of these technologies lies the concept of a Digital Dependability Identity (DDI) of a component or system. DDIs are modular, composable, and executable in the field facilitating (a) efficient synthesis of component and system dependability information over the supply chain and (b) effective evaluation of this information in-the-field for safe and secure composition of highly distributed and autonomous CPS. The paper outlines the DDI concept and opportunities for application in four industrial use cases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01729v1-abstract-full').style.display = 'none'; document.getElementById('2106.01729v1-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> 3 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.14984">arXiv:2105.14984</a> <span> [<a href="https://arxiv.org/pdf/2105.14984">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Other Computer Science">cs.OH</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/10.1109/ISSRE.2015.7381825">10.1109/ISSRE.2015.7381825 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WAP: Digital Dependability Identities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schneider%2C+D">Daniel Schneider</a>, <a href="/search/?searchtype=author&query=Trapp%2C+M">Mario Trapp</a>, <a href="/search/?searchtype=author&query=Papadopoulos%2C+Y">Yiannis Papadopoulos</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Zeller%2C+M">Marc Zeller</a>, <a href="/search/?searchtype=author&query=Hoefig%2C+K">Kai Hoefig</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="2105.14984v1-abstract-short" style="display: inline;"> Cyber-Physical Systems (CPS) provide enormous potential for innovation but a precondition for this is that the issue of dependability has been addressed. This paper presents the concept of a Digital Dependability Identity (DDI) of a component or system as foundation for assuring the dependability of CPS. A DDI is an analyzable and potentially executable model of information about the dependability… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.14984v1-abstract-full').style.display = 'inline'; document.getElementById('2105.14984v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.14984v1-abstract-full" style="display: none;"> Cyber-Physical Systems (CPS) provide enormous potential for innovation but a precondition for this is that the issue of dependability has been addressed. This paper presents the concept of a Digital Dependability Identity (DDI) of a component or system as foundation for assuring the dependability of CPS. A DDI is an analyzable and potentially executable model of information about the dependability of a component or system. We argue that DDIs must fulfill a number of properties including being universally useful across supply chains, enabling off-line certification of systems where possible, and providing capabilities for in-field certification of safety of CPS. In this paper, we focus on system safety as one integral part of dependability and as a practical demonstration of the concept, we present an initial implementation of DDIs in the form of Conditional Safety Certificates (also known as ConSerts). We explain ConSerts and their practical operationalization based on an illustrative example. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.14984v1-abstract-full').style.display = 'none'; document.getElementById('2105.14984v1-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> 31 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2015 IEEE 26th International Symposium on Software Reliability Engineering (ISSRE) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.04008">arXiv:2012.04008</a> <span> [<a href="https://arxiv.org/pdf/2012.04008">pdf</a>, <a href="https://arxiv.org/format/2012.04008">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> </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/10.1088/1475-7516/2021/04/059">10.1088/1475-7516/2021/04/059 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulating intergalactic gas for DESI-like small scale Lyman伪 forest observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</a>, <a href="/search/?searchtype=author&query=Luki%C4%87%2C+Z">Zarija Luki膰</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="2012.04008v2-abstract-short" style="display: inline;"> Measurements of the Ly$伪$ forest based on large numbers of quasar spectra from sky surveys such as SDSS/eBOSS accurately probe the distribution of matter on small scales and thus provide important constraints on several ingredients of the cosmological model. A main summary statistic derived from those measurements is the one-dimensional power spectrum, P1D, of the Ly$伪$ absorption. However, model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04008v2-abstract-full').style.display = 'inline'; document.getElementById('2012.04008v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.04008v2-abstract-full" style="display: none;"> Measurements of the Ly$伪$ forest based on large numbers of quasar spectra from sky surveys such as SDSS/eBOSS accurately probe the distribution of matter on small scales and thus provide important constraints on several ingredients of the cosmological model. A main summary statistic derived from those measurements is the one-dimensional power spectrum, P1D, of the Ly$伪$ absorption. However, model predictions for P1D rely on expensive hydrodynamical simulations of the intergalactic medium, which was the limiting factor in previous analyses. Datasets from upcoming surveys such as DESI will push observational accuracy near the 1%-level and probe even smaller scales. This observational push mandate seven more accurate simulations as well as more careful exploration of parameter space. In this work we evaluate the robustness and accuracy of simulations and the statistical framework used to constrain cosmological parameters. We present a comparison between the grid-based simulation code Nyx and SPH-based code Gadget in the context ofP1D. In addition, we perform resolution and box-size convergence tests using Nyx code. We use a Gaussian process emulation scheme to reduce the number of simulations required for exploration of parameter space without sacrificing the model accuracy. We demonstrate the ability to produce unbiased parameter constraints in an end-to-end inference test using mock eBOSS- and DESI-like data, and we advocate for the usage of adaptive sampling schemes as opposed to using a fixed Latin hypercube design. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04008v2-abstract-full').style.display = 'none'; document.getElementById('2012.04008v2-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> 22 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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">36 pages, 17 figures, accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP04(2021)059 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13806">arXiv:2011.13806</a> <span> [<a href="https://arxiv.org/pdf/2011.13806">pdf</a>, <a href="https://arxiv.org/format/2011.13806">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> </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/10.1088/1748-0221/16/02/P02037">10.1088/1748-0221/16/02/P02037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A CUPID Li$_{2}$$^{100}$MoO$_4$ scintillating bolometer tested in the CROSS underground facility </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+CUPID+Interest+Group"> The CUPID Interest Group</a>, <a href="/search/?searchtype=author&query=Armatol%2C+A">A. Armatol</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+W">W. Armstrong</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone III</a>, <a href="/search/?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/?searchtype=author&query=Bandac%2C+I+C">I. C. Bandac</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/?searchtype=author&query=Baudin%2C+D">D. Baudin</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+M">M. Biassoni</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Boldrini%2C+V">V. Boldrini</a>, <a href="/search/?searchtype=author&query=Branca%2C+A">A. Branca</a>, <a href="/search/?searchtype=author&query=Brofferio%2C+C">C. Brofferio</a>, <a href="/search/?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/?searchtype=author&query=Calvo-Mozota%2C+J+M">J. M. Calvo-Mozota</a>, <a href="/search/?searchtype=author&query=Camilleri%2C+J">J. Camilleri</a> , et al. (156 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="2011.13806v1-abstract-short" style="display: inline;"> A scintillating bolometer based on a large cubic Li$_{2}$$^{100}$MoO$_4$ crystal (45 mm side) and a Ge wafer (scintillation detector) has been operated in the CROSS cryogenic facility at the Canfranc underground laboratory in Spain. The dual-readout detector is a prototype of the technology that will be used in the next-generation $0\nu2尾$ experiment CUPID. The measurements were performed at 18 an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13806v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13806v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13806v1-abstract-full" style="display: none;"> A scintillating bolometer based on a large cubic Li$_{2}$$^{100}$MoO$_4$ crystal (45 mm side) and a Ge wafer (scintillation detector) has been operated in the CROSS cryogenic facility at the Canfranc underground laboratory in Spain. The dual-readout detector is a prototype of the technology that will be used in the next-generation $0\nu2尾$ experiment CUPID. The measurements were performed at 18 and 12 mK temperature in a pulse tube dilution refrigerator. This setup utilizes the same technology as the CUORE cryostat that will host CUPID and so represents an accurate estimation of the expected performance. The Li$_{2}$$^{100}$MoO$_4$ bolometer shows a high energy resolution of 6 keV FWHM at the 2615 keV $纬$ line. The detection of scintillation light for each event triggered by the Li$_{2}$$^{100}$MoO$_4$ bolometer allowed for a full separation ($\sim$8$蟽$) between $纬$($尾$) and $伪$ events above 2 MeV. The Li$_{2}$$^{100}$MoO$_4$ crystal also shows a high internal radiopurity with $^{228}$Th and $^{226}$Ra activities of less than 3 and 8 $渭$Bq/kg, respectively. Taking also into account the advantage of a more compact and massive detector array, which can be made of cubic-shaped crystals (compared to the cylindrical ones), this test demonstrates the great potential of cubic Li$_{2}$$^{100}$MoO$_4$ scintillating bolometers for high-sensitivity searches for the $^{100}$Mo $0\nu2尾$ decay in CROSS and CUPID projects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13806v1-abstract-full').style.display = 'none'; document.getElementById('2011.13806v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13656">arXiv:2011.13656</a> <span> [<a href="https://arxiv.org/pdf/2011.13656">pdf</a>, <a href="https://arxiv.org/format/2011.13656">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Characterization of cubic Li$_{2}$$^{100}$MoO$_4$ crystals for the CUPID experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armatol%2C+A">A. Armatol</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+W">W. Armstrong</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone III</a>, <a href="/search/?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A">A. Barabash</a>, <a href="/search/?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/?searchtype=author&query=Baudin%2C+D">D. Baudin</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A8%2C+L">L. Berg猫</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+M">M. Biassoni</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Boldrini%2C+V">V. Boldrini</a>, <a href="/search/?searchtype=author&query=Branca%2C+A">A. Branca</a>, <a href="/search/?searchtype=author&query=Brofferio%2C+C">C. Brofferio</a>, <a href="/search/?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/?searchtype=author&query=Camilleri%2C+J">J. Camilleri</a>, <a href="/search/?searchtype=author&query=Capelli%2C+S">S. Capelli</a>, <a href="/search/?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Carniti%2C+P">P. Carniti</a> , et al. (147 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="2011.13656v1-abstract-short" style="display: inline;"> The CUPID Collaboration is designing a tonne-scale, background-free detector to search for double beta decay with sufficient sensitivity to fully explore the parameter space corresponding to the inverted neutrino mass hierarchy scenario. One of the CUPID demonstrators, CUPID-Mo, has proved the potential of enriched Li$_{2}$$^{100}$MoO$_4$ crystals as suitable detectors for neutrinoless double beta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13656v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13656v1-abstract-full" style="display: none;"> The CUPID Collaboration is designing a tonne-scale, background-free detector to search for double beta decay with sufficient sensitivity to fully explore the parameter space corresponding to the inverted neutrino mass hierarchy scenario. One of the CUPID demonstrators, CUPID-Mo, has proved the potential of enriched Li$_{2}$$^{100}$MoO$_4$ crystals as suitable detectors for neutrinoless double beta decay search. In this work, we characterised cubic crystals that, compared to the cylindrical crystals used by CUPID-Mo, are more appealing for the construction of tightly packed arrays. We measured an average energy resolution of (6.7$\pm$0.6) keV FWHM in the region of interest, approaching the CUPID target of 5 keV FWHM. We assessed the identification of $伪$ particles with and without a reflecting foil that enhances the scintillation light collection efficiency, proving that the baseline design of CUPID already ensures a complete suppression of this $伪$-induced background contribution. We also used the collected data to validate a Monte Carlo simulation modelling the light collection efficiency, which will enable further optimisations of the detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13656v1-abstract-full').style.display = 'none'; document.getElementById('2011.13656v1-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> 27 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13243">arXiv:2011.13243</a> <span> [<a href="https://arxiv.org/pdf/2011.13243">pdf</a>, <a href="https://arxiv.org/format/2011.13243">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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.126.181802">10.1103/PhysRevLett.126.181802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New Limit for Neutrinoless Double-Beta Decay of $^{100}$Mo from the CUPID-Mo Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Borovlev%2C+Y+A">Yu. A. Borovlev</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Brudanin%2C+V+B">V. B. Brudanin</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=Chiesa%2C+D">D. Chiesa</a>, <a href="/search/?searchtype=author&query=de+Combarieu%2C+M">M. de Combarieu</a>, <a href="/search/?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/?searchtype=author&query=Dixon%2C+T">T. Dixon</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a> , et al. (69 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="2011.13243v2-abstract-short" style="display: inline;"> The CUPID-Mo experiment at the Laboratoire Souterrain de Modane (France) is a demonstrator for CUPID, the next-generation ton-scale cryogenic $0谓尾尾$ experiment. It consists of a 4.2 kg array of 20 enriched Li$_{2}$$^{100}$MoO$_4$ scintillating bolometers to search for the lepton number violating process of $0谓尾尾$ decay in $^{100}$Mo. With more than one year of operation (2.16 kg$\times$yr of physi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13243v2-abstract-full').style.display = 'inline'; document.getElementById('2011.13243v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13243v2-abstract-full" style="display: none;"> The CUPID-Mo experiment at the Laboratoire Souterrain de Modane (France) is a demonstrator for CUPID, the next-generation ton-scale cryogenic $0谓尾尾$ experiment. It consists of a 4.2 kg array of 20 enriched Li$_{2}$$^{100}$MoO$_4$ scintillating bolometers to search for the lepton number violating process of $0谓尾尾$ decay in $^{100}$Mo. With more than one year of operation (2.16 kg$\times$yr of physics data), no event in the region of interest and hence no evidence for $0谓尾尾$ is observed. We report a new limit on the half-life of $0谓尾尾$ decay in $^{100}$Mo of $T_{1/2} > 1.5 \times 10^{24}\,$yr at 90 % C.I. The limit corresponds to an effective Majorana neutrino mass $\langle m_{尾尾} \rangle$ $<$ (0.31--0.54)$\,$eV, dependent on the nuclear matrix element in the light Majorana neutrino exchange interpretation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13243v2-abstract-full').style.display = 'none'; document.getElementById('2011.13243v2-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> 5 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 126, 181802 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.11726">arXiv:2011.11726</a> <span> [<a href="https://arxiv.org/pdf/2011.11726">pdf</a>, <a href="https://arxiv.org/format/2011.11726">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> </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/PhysRevC.104.015501">10.1103/PhysRevC.104.015501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel technique for the study of pile-up events in cryogenic bolometers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armatol%2C+A">A. Armatol</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+W">W. Armstrong</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone III</a>, <a href="/search/?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A">A. Barabash</a>, <a href="/search/?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/?searchtype=author&query=Baudin%2C+D">D. Baudin</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+M">M. Biassoni</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Boldrini%2C+V">V. Boldrini</a>, <a href="/search/?searchtype=author&query=Branca%2C+A">A. Branca</a>, <a href="/search/?searchtype=author&query=Brofferio%2C+C">C. Brofferio</a>, <a href="/search/?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/?searchtype=author&query=Camilleri%2C+J">J. Camilleri</a>, <a href="/search/?searchtype=author&query=Capelli%2C+S">S. Capelli</a>, <a href="/search/?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Carniti%2C+P">P. Carniti</a> , et al. (144 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="2011.11726v2-abstract-short" style="display: inline;"> Precise characterization of detector time resolution is of crucial importance for next-generation cryogenic-bolometer experiments searching for neutrinoless double-beta decay, such as CUPID, in order to reject background due to pile-up of two-neutrino double-beta decay events. In this paper, we describe a technique developed to study the pile-up rejection capability of cryogenic bolometers. Our ap… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11726v2-abstract-full').style.display = 'inline'; document.getElementById('2011.11726v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.11726v2-abstract-full" style="display: none;"> Precise characterization of detector time resolution is of crucial importance for next-generation cryogenic-bolometer experiments searching for neutrinoless double-beta decay, such as CUPID, in order to reject background due to pile-up of two-neutrino double-beta decay events. In this paper, we describe a technique developed to study the pile-up rejection capability of cryogenic bolometers. Our approach, which consists of producing controlled pile-up events with a programmable waveform generator, has the benefit that we can reliably and reproducibly control the time separation and relative energy of the individual components of the generated pile-up events. The resulting data allow us to optimize and benchmark analysis strategies to discriminate between individual and pile-up pulses. We describe a test of this technique performed with a small array of detectors at the Laboratori Nazionali del Gran Sasso, in Italy; we obtain a 90% rejection efficiency against pulser-generated pile-up events with rise time of ~15ms down to time separation between the individual events of about 2ms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11726v2-abstract-full').style.display = 'none'; document.getElementById('2011.11726v2-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> 12 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 104, 015501 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.12076">arXiv:2010.12076</a> <span> [<a href="https://arxiv.org/pdf/2010.12076">pdf</a>, <a href="https://arxiv.org/format/2010.12076">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Conceptual Design of BabyIAXO, the intermediate stage towards the International Axion Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abeln%2C+A">A. Abeln</a>, <a href="/search/?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/?searchtype=author&query=De+Sousa%2C+P+T+C+B">P. T. C. Borges De Sousa</a>, <a href="/search/?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/?searchtype=author&query=Bykovskiy%2C+N">N. Bykovskiy</a>, <a href="/search/?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/?searchtype=author&query=Dafn%C3%AD%2C+T">T. Dafn铆</a>, <a href="/search/?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/?searchtype=author&query=D%C3%ADez%2C+D">D. D铆ez</a>, <a href="/search/?searchtype=author&query=Dinter%2C+M">M. Dinter</a> , et al. (101 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="2010.12076v3-abstract-short" style="display: inline;"> This article describes BabyIAXO, an intermediate experimental stage of the International Axion Observatory (IAXO), proposed to be sited at DESY. IAXO is a large-scale axion helioscope that will look for axions and axion-like particles (ALPs), produced in the Sun, with unprecedented sensitivity. BabyIAXO is conceived to test all IAXO subsystems (magnet, optics and detectors) at a relevant scale for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.12076v3-abstract-full').style.display = 'inline'; document.getElementById('2010.12076v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.12076v3-abstract-full" style="display: none;"> This article describes BabyIAXO, an intermediate experimental stage of the International Axion Observatory (IAXO), proposed to be sited at DESY. IAXO is a large-scale axion helioscope that will look for axions and axion-like particles (ALPs), produced in the Sun, with unprecedented sensitivity. BabyIAXO is conceived to test all IAXO subsystems (magnet, optics and detectors) at a relevant scale for the final system and thus serve as prototype for IAXO, but at the same time as a fully-fledged helioscope with relevant physics reach itself, and with potential for discovery. The BabyIAXO magnet will feature two 10 m long, 70 cm diameter bores, and will host two detection lines (optics and detector) of dimensions similar to the final ones foreseen for IAXO. BabyIAXO will detect or reject solar axions or ALPs with axion-photon couplings down to $g_{a纬} \sim 1.5 \times 10^{-11}$ GeV$^{-1}$, and masses up to $m_a\sim 0.25$ eV. BabyIAXO will offer additional opportunities for axion research in view of IAXO, like the development of precision x-ray detectors to identify particular spectral features in the solar axion spectrum, and the implementation of radiofrequency-cavity-based axion dark matter setups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.12076v3-abstract-full').style.display = 'none'; document.getElementById('2010.12076v3-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">77 pages, 49 figures. Prepared for submission to JHEP. Third version after referees comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.04033">arXiv:2010.04033</a> <span> [<a href="https://arxiv.org/pdf/2010.04033">pdf</a>, <a href="https://arxiv.org/format/2010.04033">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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/10.1088/1748-0221/16/03/P03032">10.1088/1748-0221/16/03/P03032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pulse Shape Discrimination in CUPID-Mo using Principal Component Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Huang%2C+R">R. Huang</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Borovlev%2C+Y+A">Yu. A. Borovlev</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Brudanin%2C+V+B">V. B. Brudanin</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=de+Combarieu%2C+M">M. de Combarieu</a>, <a href="/search/?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/?searchtype=author&query=Dixon%2C+T">T. Dixon</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a> , et al. (64 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="2010.04033v2-abstract-short" style="display: inline;"> CUPID-Mo is a cryogenic detector array designed to search for neutrinoless double-beta decay ($0谓尾尾$) of $^{100}$Mo. It uses 20 scintillating $^{100}$Mo-enriched Li$_2$MoO$_4$ bolometers instrumented with Ge light detectors to perform active suppression of $伪$ backgrounds, drastically reducing the expected background in the $0谓尾尾$ signal region. As a result, pileup events and small detector instab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04033v2-abstract-full').style.display = 'inline'; document.getElementById('2010.04033v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.04033v2-abstract-full" style="display: none;"> CUPID-Mo is a cryogenic detector array designed to search for neutrinoless double-beta decay ($0谓尾尾$) of $^{100}$Mo. It uses 20 scintillating $^{100}$Mo-enriched Li$_2$MoO$_4$ bolometers instrumented with Ge light detectors to perform active suppression of $伪$ backgrounds, drastically reducing the expected background in the $0谓尾尾$ signal region. As a result, pileup events and small detector instabilities that mimic normal signals become non-negligible potential backgrounds. These types of events can in principle be eliminated based on their signal shapes, which are different from those of regular bolometric pulses. We show that a purely data-driven principal component analysis based approach is able to filter out these anomalous events, without the aid of detector response simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04033v2-abstract-full').style.display = 'none'; document.getElementById('2010.04033v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 16 (2021) P03032 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.01448">arXiv:2004.01448</a> <span> [<a href="https://arxiv.org/pdf/2004.01448">pdf</a>, <a href="https://arxiv.org/format/2004.01448">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> </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/10.1088/1475-7516/2020/07/010">10.1088/1475-7516/2020/07/010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A tomographic map of the large-scale matter distribution using the eBOSS Stripe 82 Ly-$伪$ forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">M. Walther</a>, <a href="/search/?searchtype=author&query=Etourneau%2C+T">T. Etourneau</a>, <a href="/search/?searchtype=author&query=Pomar%C3%A8de%2C+D">D. Pomar猫de</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">N. Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">C. Y猫che</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Bourboux%2C+H+d+M+d">H. du Mas des Bourboux</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">S. Chabanier</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=Goff%2C+J+-+L">J. -M. Le Goff</a>, <a href="/search/?searchtype=author&query=Lyke%2C+B">B. Lyke</a>, <a href="/search/?searchtype=author&query=Myers%2C+A+D">A. D. Myers</a>, <a href="/search/?searchtype=author&query=Petitjean%2C+P">P. Petitjean</a>, <a href="/search/?searchtype=author&query=Pieri%2C+M+M">M. M. Pieri</a>, <a href="/search/?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/?searchtype=author&query=Rossi%2C+G">G. Rossi</a>, <a href="/search/?searchtype=author&query=Schneider%2C+D+P">D. P. Schneider</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="2004.01448v2-abstract-short" style="display: inline;"> The Lyman-$伪$ (hereafter Ly-$伪$) forest is a probe of large-scale matter density fluctuations at high redshift, $z > 2.1$. It consists of HI absorption spectra along individual lines-of-sight. If the line-of-sight density is large enough, 3D maps of HI absorption can be inferred by tomographic reconstruction. In this article, we investigate the Ly-$伪$ forest available in the Stripe 82 field (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.01448v2-abstract-full').style.display = 'inline'; document.getElementById('2004.01448v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.01448v2-abstract-full" style="display: none;"> The Lyman-$伪$ (hereafter Ly-$伪$) forest is a probe of large-scale matter density fluctuations at high redshift, $z > 2.1$. It consists of HI absorption spectra along individual lines-of-sight. If the line-of-sight density is large enough, 3D maps of HI absorption can be inferred by tomographic reconstruction. In this article, we investigate the Ly-$伪$ forest available in the Stripe 82 field ($220\,\mathrm{deg^{2}}$), based on the quasar spectra from SDSS Data Release DR16. The density of observed quasar spectra is $37\,\mathrm{deg^{-2}}$ with a mean pixel signal-to-noise ratio of two per angstrom. This study provides an intermediate case between the average SDSS density and that of the much denser but smaller CLAMATO survey. We derive a 3D map of large-scale matter fluctuations from these data, using a Wiener filter technique. The total volume of the map is $0.94\,\mathrm{h^{-3} Gpc^{3}}$. Its resolution is $13\,\mathrm{h^{-1} Mpc}$, which is related to the mean transverse distance between nearest lines-of-sight. From this map, we provide a catalog of voids and protocluster candidates in the cosmic web. The map-making and void catalog are compared to simulated eBOSS Stripe 82 observations. A stack over quasar positions provides a visualization of the Ly-$伪$ quasar cross-correlation. This tomographic reconstruction constitutes the largest-volume high-redshift 3D map of matter fluctuations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.01448v2-abstract-full').style.display = 'none'; document.getElementById('2004.01448v2-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> 8 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP07(2020)010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.01046">arXiv:2003.01046</a> <span> [<a href="https://arxiv.org/pdf/2003.01046">pdf</a>, <a href="https://arxiv.org/format/2003.01046">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey 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/10.1103/PhysRevLett.125.141301">10.1103/PhysRevLett.125.141301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First germanium-based constraints on sub-MeV Dark Matter with the EDELWEISS experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=EDELWEISS+Collaboration"> EDELWEISS Collaboration</a>, <a href="/search/?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=De+J%C3%A9sus%2C+M">M. De J茅sus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/?searchtype=author&query=Elkhoury%2C+E">E. Elkhoury</a>, <a href="/search/?searchtype=author&query=Fillipini%2C+J+-">J. -B. Fillipini</a>, <a href="/search/?searchtype=author&query=Filosofov%2C+D">D. Filosofov</a>, <a href="/search/?searchtype=author&query=Gascon%2C+J">J. Gascon</a>, <a href="/search/?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/?searchtype=author&query=Gros%2C+M">M. Gros</a>, <a href="/search/?searchtype=author&query=Jin%2C+Y">Y. Jin</a>, <a href="/search/?searchtype=author&query=Juillard%2C+A">A. Juillard</a>, <a href="/search/?searchtype=author&query=Kleifges%2C+M">M. Kleifges</a>, <a href="/search/?searchtype=author&query=Lattaud%2C+H">H. Lattaud</a> , et al. (17 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="2003.01046v2-abstract-short" style="display: inline;"> The EDELWEISS collaboration has performed a search for Dark Matter (DM) particles interacting with electrons using a 33.4 g Ge cryogenic detector operated underground at the LSM. A charge resolution of 0.53 electron-hole pairs (RMS) has been achieved using the Neganov-Trofimov-Luke amplification with a bias of 78 V. We set the first Ge-based constraints on sub-MeV/c$^{2}$ DM particles interacting… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.01046v2-abstract-full').style.display = 'inline'; document.getElementById('2003.01046v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.01046v2-abstract-full" style="display: none;"> The EDELWEISS collaboration has performed a search for Dark Matter (DM) particles interacting with electrons using a 33.4 g Ge cryogenic detector operated underground at the LSM. A charge resolution of 0.53 electron-hole pairs (RMS) has been achieved using the Neganov-Trofimov-Luke amplification with a bias of 78 V. We set the first Ge-based constraints on sub-MeV/c$^{2}$ DM particles interacting with electrons, as well as on dark photons down to 1 eV/c$^2$. These are competitive with other searches. In particular, new limits are set on the kinetic mixing of dark photon DM in a so far unconstrained parameter space region in the 6 to 9 eV/c$^2$ mass range. These results demonstrate the high relevance of cryogenic Ge detectors for the search of DM interactions producing eV-scale electron signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.01046v2-abstract-full').style.display = 'none'; document.getElementById('2003.01046v2-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> 10 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </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">6 pages, 4 figures, corrected typos</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 125, 141301 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.02822">arXiv:2002.02822</a> <span> [<a href="https://arxiv.org/pdf/2002.02822">pdf</a>, <a href="https://arxiv.org/format/2002.02822">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1093/mnras/staa1242">10.1093/mnras/staa1242 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The impact of AGN feedback on the 1D power spectra from the Ly$伪$ forest using the Horizon-AGN suite of simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Chabanier%2C+S">Sol猫ne Chabanier</a>, <a href="/search/?searchtype=author&query=Bournaud%2C+F">Fr茅d茅ric Bournaud</a>, <a href="/search/?searchtype=author&query=Dubois%2C+Y">Yohan Dubois</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Peirani%2C+S">S茅bastien Peirani</a>, <a href="/search/?searchtype=author&query=Beckmann%2C+R+S">Ricarda S. Beckmann</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="2002.02822v3-abstract-short" style="display: inline;"> The Lyman-$伪$ forest is a powerful probe for cosmology, but it is also strongly impacted by galaxy evolution and baryonic processes such as Active Galactic Nuclei (AGN) feedback, which can redistribute mass and energy on large scales. We constrain the signatures of AGN feedback on the 1D power spectrum of the Lyman-$伪$ forest using a series of eight hydro-cosmological simulations performed with th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.02822v3-abstract-full').style.display = 'inline'; document.getElementById('2002.02822v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.02822v3-abstract-full" style="display: none;"> The Lyman-$伪$ forest is a powerful probe for cosmology, but it is also strongly impacted by galaxy evolution and baryonic processes such as Active Galactic Nuclei (AGN) feedback, which can redistribute mass and energy on large scales. We constrain the signatures of AGN feedback on the 1D power spectrum of the Lyman-$伪$ forest using a series of eight hydro-cosmological simulations performed with the Adaptative Mesh Refinement code RAMSES. This series starts from the Horizon-AGN simulation and varies the sub-grid parameters for AGN feeding, feedback and stochasticity. These simulations cover the whole plausible range of feedback and feeding parameters according to the resulting galaxy properties. AGNs globally suppress the Lyman-$伪$ power at all scales. On large scales, the energy injection and ionization dominate over the supply of gas mass from AGN-driven galactic winds, thus suppressing power. On small scales, faster cooling of denser gas mitigates the suppression. This effect increases with decreasing redshift. We provide lower and upper limits of this signature at nine redshifts between $z=4.25$ and $z=2.0$, making it possible to account for it at post-processing stage in future work given that running simulations without AGN feedback can save considerable amounts of computing resources. Ignoring AGN feedback in cosmological inference analyses leads to strong biases with 2\% shift on $蟽_8$ and 1\% shift on $n_s$, which represents twice the standards deviation of the current constraints on $n_s$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.02822v3-abstract-full').style.display = 'none'; document.getElementById('2002.02822v3-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> 1 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </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">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.07272">arXiv:1912.07272</a> <span> [<a href="https://arxiv.org/pdf/1912.07272">pdf</a>, <a href="https://arxiv.org/ps/1912.07272">ps</a>, <a href="https://arxiv.org/format/1912.07272">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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/10.1140/epjc/s10052-020-8203-4">10.1140/epjc/s10052-020-8203-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precise measurement of $2谓尾尾$ decay of $^{100}$Mo with the CUPID-Mo detection technology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Borovlev%2C+Y+A">Yu. A. Borovlev</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Briere%2C+M">M. Briere</a>, <a href="/search/?searchtype=author&query=Brudanin%2C+V">V. Brudanin</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=de+Combarieu%2C+M">M. de Combarieu</a>, <a href="/search/?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a> , et al. (65 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="1912.07272v1-abstract-short" style="display: inline;"> We report the measurement of the two-neutrino double-beta ($2谓尾尾$) decay of $^{100}$Mo to the ground state of $^{100}$Ru using lithium molybdate (\crystal) scintillating bolometers. The detectors were developed for the CUPID-Mo program and operated at the EDELWEISS-III low background facility in the Modane underground laboratory. From a total exposure of $42.235$ kg$\times$d, the half-life of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.07272v1-abstract-full').style.display = 'inline'; document.getElementById('1912.07272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.07272v1-abstract-full" style="display: none;"> We report the measurement of the two-neutrino double-beta ($2谓尾尾$) decay of $^{100}$Mo to the ground state of $^{100}$Ru using lithium molybdate (\crystal) scintillating bolometers. The detectors were developed for the CUPID-Mo program and operated at the EDELWEISS-III low background facility in the Modane underground laboratory. From a total exposure of $42.235$ kg$\times$d, the half-life of $^{100}$Mo is determined to be $T_{1/2}^{2谓}=[7.12^{+0.18}_{-0.14}\,\mathrm{(stat.)}\pm0.10\,\mathrm{(syst.)}]\times10^{18}$ years. This is the most accurate determination of the $2谓尾尾$ half-life of $^{100}$Mo to date. We also confirm, with the statistical significance of $>3蟽$, that the single-state dominance model of the $2谓尾尾$ decay of $^{100}$Mo is favored over the high-state dominance model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.07272v1-abstract-full').style.display = 'none'; document.getElementById('1912.07272v1-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> 16 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </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">11 pages, 6 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.02905">arXiv:1912.02905</a> <span> [<a href="https://arxiv.org/pdf/1912.02905">pdf</a>, <a href="https://arxiv.org/format/1912.02905">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey 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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.3847/1538-4365/ab929e">10.3847/1538-4365/ab929e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Sixteenth Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ahumada%2C+R">Romina Ahumada</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/?searchtype=author&query=Anders%2C+F">Friedrich Anders</a>, <a href="/search/?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/?searchtype=author&query=Andrews%2C+B+H">Brett H. Andrews</a>, <a href="/search/?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Aubert%2C+M">Marie Aubert</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">Santiago Avila</a>, <a href="/search/?searchtype=author&query=Avila-Reese%2C+V">Vladimir Avila-Reese</a>, <a href="/search/?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/?searchtype=author&query=Balland%2C+C">Christophe Balland</a>, <a href="/search/?searchtype=author&query=Barger%2C+K">Kat Barger</a>, <a href="/search/?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/?searchtype=author&query=Basu%2C+S">Sarbani Basu</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">Julian Bautista</a>, <a href="/search/?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/?searchtype=author&query=Benavides%2C+B+I+T">B. Izamar T. Benavides</a>, <a href="/search/?searchtype=author&query=Bender%2C+C+F">Chad F. Bender</a>, <a href="/search/?searchtype=author&query=Bernardi%2C+M">Mariangela Bernardi</a>, <a href="/search/?searchtype=author&query=Bershady%2C+M">Matthew Bershady</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">Florian Beutler</a> , et al. (289 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="1912.02905v2-abstract-short" style="display: inline;"> This paper documents the sixteenth data release (DR16) from the Sloan Digital Sky Surveys; the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the southern hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.02905v2-abstract-full').style.display = 'inline'; document.getElementById('1912.02905v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.02905v2-abstract-full" style="display: none;"> This paper documents the sixteenth data release (DR16) from the Sloan Digital Sky Surveys; the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the southern hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey (TDSS) and new data from the SPectroscopic IDentification of ERosita Survey (SPIDERS) programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.02905v2-abstract-full').style.display = 'none'; document.getElementById('1912.02905v2-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> 11 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </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">DR16 release: Monday Dec 9th 2019. This is the alphabetical order SDSS-IV collaboration data release paper. 25 pages, 6 figures, accepted by ApJS on 11th May 2020. Minor changes clarify or improve text and figures relative to v1</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.10426">arXiv:1911.10426</a> <span> [<a href="https://arxiv.org/pdf/1911.10426">pdf</a>, <a href="https://arxiv.org/format/1911.10426">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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/10.1088/1742-6596/1468/1/012129">10.1088/1742-6596/1468/1/012129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First data from the CUPID-Mo neutrinoless double beta decay experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schmidt%2C+B">B. Schmidt</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Borovlev%2C+Y+A">Yu. A. Borovlev</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Briere%2C+M">M. Briere</a>, <a href="/search/?searchtype=author&query=Brudanin%2C+V+B">V. B. Brudanin</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=de+Combarieu%2C+M">M. de Combarieu</a>, <a href="/search/?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a> , et al. (65 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="1911.10426v1-abstract-short" style="display: inline;"> The CUPID-Mo experiment is searching for neutrinoless double beta decay in $^{100}$Mo, evaluating the technology of cryogenic scintillating Li$_{2}^{100}$MoO$_4$ detectors for CUPID (CUORE Upgrade with Particle ID). CUPID-Mo detectors feature background suppression using a dual-readout scheme with Li$_{2}$MoO$_4$ crystals complemented by Ge bolometers for light detection. The detection of both hea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.10426v1-abstract-full').style.display = 'inline'; document.getElementById('1911.10426v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.10426v1-abstract-full" style="display: none;"> The CUPID-Mo experiment is searching for neutrinoless double beta decay in $^{100}$Mo, evaluating the technology of cryogenic scintillating Li$_{2}^{100}$MoO$_4$ detectors for CUPID (CUORE Upgrade with Particle ID). CUPID-Mo detectors feature background suppression using a dual-readout scheme with Li$_{2}$MoO$_4$ crystals complemented by Ge bolometers for light detection. The detection of both heat and scintillation light signals allows the efficient discrimination of $伪$ from $纬$&$尾$ events. In this proceedings, we discuss results from the first 2 months of data taking in spring 2019. In addition to an excellent bolometric performance of 6.7$\,$keV (FWHM) at 2615$\,$keV and an $伪$ separation of better than 99.9\% for all detectors, we report on bulk radiopurity for Th and U. Finally, we interpret the accumulated physics data in terms of a limit of $T_{1/2}^{0谓}\,> 3\times10^{23}\,$yr for $^{100}$Mo and discuss the sensitivity of CUPID-Mo until the expected end of physics data taking in early 2020. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.10426v1-abstract-full').style.display = 'none'; document.getElementById('1911.10426v1-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </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">Proceedings for TAUP 2019, submitted to IOP Journal of Physics: Conference Series</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics: Conference Series 1468 (2020) 012129 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.09073">arXiv:1911.09073</a> <span> [<a href="https://arxiv.org/pdf/1911.09073">pdf</a>, <a href="https://arxiv.org/format/1911.09073">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> </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/10.1088/1475-7516/2020/04/038">10.1088/1475-7516/2020/04/038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hints, neutrino bounds and WDM constraints from SDSS DR14 Lyman-$伪$ and Planck full-survey data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</a>, <a href="/search/?searchtype=author&query=Sch%C3%B6neberg%2C+N">Nils Sch枚neberg</a>, <a href="/search/?searchtype=author&query=Lesgourgues%2C+J">Julien Lesgourgues</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">Sol猫ne Chabanier</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</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="1911.09073v3-abstract-short" style="display: inline;"> The Ly-$伪$ forest 1D flux power spectrum is a powerful probe of several cosmological parameters. Assuming a $螞$CDM cosmology including massive neutrinos, we find that the latest SDSS DR14 BOSS and eBOSS Ly-$伪$ forest data is in very good agreement with current weak lensing constraints on $(惟_m, 蟽_8)$ and has the same small level of tension with Planck. We did not identify a systematic effect in th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09073v3-abstract-full').style.display = 'inline'; document.getElementById('1911.09073v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.09073v3-abstract-full" style="display: none;"> The Ly-$伪$ forest 1D flux power spectrum is a powerful probe of several cosmological parameters. Assuming a $螞$CDM cosmology including massive neutrinos, we find that the latest SDSS DR14 BOSS and eBOSS Ly-$伪$ forest data is in very good agreement with current weak lensing constraints on $(惟_m, 蟽_8)$ and has the same small level of tension with Planck. We did not identify a systematic effect in the data analysis that could explain this small tension, but we show that it can be reduced in extended cosmological models where the spectral index is not the same on the very different times and scales probed by CMB and Ly-$伪$ data. A particular case is that of a $螞$CDM model including a running of the spectral index on top of massive neutrinos. With combined Ly-$伪$ and Planck data, we find a slight (3$蟽$) preference for negative running, $伪_s= -0.010 \pm 0.004$ (68% CL). Neutrino mass bounds are found to be robust against different assumptions. In the $螞$CDM model with running, we find $\sum m_谓<0.11$ eV at the 95% confidence level for combined Ly-$伪$ and Planck (temperature and polarisation) data, or $\sum m_谓< 0.09$ eV when adding CMB lensing and BAO data. We further provide strong and nearly model-independent bounds on the mass of thermal warm dark matter. For a conservative configuration consisting of SDSS data restricted to $z<4.5$ combined with XQ-100 \lya data, we find $m_X > 5.3\;\mathrm{keV}$ (95\%CL). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09073v3-abstract-full').style.display = 'none'; document.getElementById('1911.09073v3-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> 6 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </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">accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 04 (2020) 038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02994">arXiv:1909.02994</a> <span> [<a href="https://arxiv.org/pdf/1909.02994">pdf</a>, <a href="https://arxiv.org/format/1909.02994">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 Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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/10.1140/epjc/s10052-019-7578-6">10.1140/epjc/s10052-019-7578-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CUPID-Mo experiment for neutrinoless double-beta decay: performance and prospects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/?searchtype=author&query=Barabash%2C+A+S">A. S. Barabash</a>, <a href="/search/?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/?searchtype=author&query=Borovlev%2C+Y+A">Yu. A. Borovlev</a>, <a href="/search/?searchtype=author&query=Bourgeois%2C+C">Ch. Bourgeois</a>, <a href="/search/?searchtype=author&query=Briere%2C+M">M. Briere</a>, <a href="/search/?searchtype=author&query=Brudanin%2C+V+B">V. B. Brudanin</a>, <a href="/search/?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/?searchtype=author&query=de+Combarieu%2C+M">M. de Combarieu</a>, <a href="/search/?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/?searchtype=author&query=Eitel%2C+K">K. Eitel</a> , et al. (64 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="1909.02994v1-abstract-short" style="display: inline;"> CUPID-Mo is a bolometric experiment to search for neutrinoless double-beta decay ($0谓尾尾$) of $^{100}$Mo. In this article, we detail the CUPID-Mo detector concept, assembly, installation in the underground laboratory in Modane in 2018, and provide results from the first datasets. The demonstrator consists of an array of 20 scintillating bolometers comprised of $^{100}$Mo-enriched 0.2 kg Li$_2$MoO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02994v1-abstract-full').style.display = 'inline'; document.getElementById('1909.02994v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02994v1-abstract-full" style="display: none;"> CUPID-Mo is a bolometric experiment to search for neutrinoless double-beta decay ($0谓尾尾$) of $^{100}$Mo. In this article, we detail the CUPID-Mo detector concept, assembly, installation in the underground laboratory in Modane in 2018, and provide results from the first datasets. The demonstrator consists of an array of 20 scintillating bolometers comprised of $^{100}$Mo-enriched 0.2 kg Li$_2$MoO$_4$ crystals. The detectors are complemented by 20 thin cryogenic Ge bolometers acting as light detectors to distinguish $伪$ from $纬$/$尾$ events by the detection of both heat and scintillation light signals. We observe good detector uniformity, facilitating the operation of a large detector array as well as excellent energy resolution of 5.3 keV (6.5 keV) FWHM at 2615 keV, in calibration (physics) data. Based on the observed energy resolutions and light yields a separation of $伪$ particles at much better than 99.9\% with equally high acceptance for $纬$/$尾$ events is expected for events in the region of interest for $^{100}$Mo $0谓尾尾$. We present limits on the crystals' radiopurity ($\leq$3 $渭$Bq/kg of $^{226}$Ra and $\leq$2 $渭$Bq/kg of $^{232}$Th). Based on these initial results we also discuss a sensitivity study for the science reach of the CUPID-Mo experiment, in particular, the ability to set the most stringent half-life limit on the $^{100}$Mo $0谓尾尾$ decay after half a year of livetime. The achieved results show that CUPID-Mo is a successful demonstrator of the technology - developed in the framework of the LUMINEU project - selected for the CUPID experiment, a proposed follow-up of CUORE, the currently running first tonne-scale cryogenic $0谓尾尾$ experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02994v1-abstract-full').style.display = 'none'; document.getElementById('1909.02994v1-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> 6 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </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">15 pages, 18 figures, 3 tables; to be submitted to EPJC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.10009">arXiv:1906.10009</a> <span> [<a href="https://arxiv.org/pdf/1906.10009">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Signal Processing">eess.SP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Robotics">cs.RO</span> </div> </div> <p class="title is-5 mathjax"> Development Framework for Longitudinal Automated Driving Functions with Off-board Information Integration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Frager%2C+S">Sebastian Frager</a>, <a href="/search/?searchtype=author&query=Jones%2C+S">Stephen Jones</a>, <a href="/search/?searchtype=author&query=Massoner%2C+A">Alexander Massoner</a>, <a href="/search/?searchtype=author&query=Parrilla%2C+A+F">Alejandro Ferreira Parrilla</a>, <a href="/search/?searchtype=author&query=Wikstr%C3%B6m%2C+N">Niklas Wikstr枚m</a>, <a href="/search/?searchtype=author&query=Macher%2C+G">Georg Macher</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="1906.10009v1-abstract-short" style="display: inline;"> Increasingly sophisticated function development is taking place with the aim of developing efficient, safe and increasingly Automated Driving Functions. This development is possible with the use of diverse data from sources such as Navigation Systems, eHorizon, on-board sensor data, Vehicle-to-Infrastructure (V2I) and Vehicle-to-Vehicle (V2V) communication. Increasing challenges arise with the dep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.10009v1-abstract-full').style.display = 'inline'; document.getElementById('1906.10009v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.10009v1-abstract-full" style="display: none;"> Increasingly sophisticated function development is taking place with the aim of developing efficient, safe and increasingly Automated Driving Functions. This development is possible with the use of diverse data from sources such as Navigation Systems, eHorizon, on-board sensor data, Vehicle-to-Infrastructure (V2I) and Vehicle-to-Vehicle (V2V) communication. Increasing challenges arise with the dependency on large amounts of real-time data coming from off-board sources. At the core of addressing these challenges lies the concept of a Digital Dependability Identity (DDI) of a component or system. DDIs are modular, composable, and executable components in the field, facilitating: $\bullet$ efficient synthesis of component and system dependability information, $\bullet$ effective evaluation of information for safe and secure composition of highly distributed and autonomous Cyber Physical Systems. In AVL's Connected Powertrain (TM), Automated Driving Functions are tailored to Powertrain Control Strategies that predictively increase energy efficiency according to the powertrain type and its component efficiencies. Simultaneously, the burden on the driver is reduced by optimizing the vehicle velocity, whilst minimizing any journey time penalty.In this work, the development of dependable Automated Driving Functions is exemplified by the Traffic Light Assistant, an adaptive strategy that utilizes predictions of preceding traffic, upcoming road curvature, inclination, speed limits, and especially traffic light signal phase and timing information to increase the energy efficiency in an urban traffic environment. A key aspect of this development is the possibility for seamless and simultaneous development; from office simulation to human-in-the-loop and to real-time tests that include vehicle and powertrain hardware. Driver's acceptance and comfort is rated in an advanced diver simulator mounted on a hexapod, capable of emulating longitudinal and lateral acceleration of a real vehicle. Test results from real-time function validation on a Powertrain Testbed are shown, including real traffic light signal phasing information and traffic flow representation on Graz city roads. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.10009v1-abstract-full').style.display = 'none'; document.getElementById('1906.10009v1-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> 18 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </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">ERTS 2018, Jan 2018, Toulouse, France</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.09155">arXiv:1904.09155</a> <span> [<a href="https://arxiv.org/pdf/1904.09155">pdf</a>, <a href="https://arxiv.org/format/1904.09155">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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 - Experiment">hep-ex</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/10.1088/1475-7516/2019/06/047">10.1088/1475-7516/2019/06/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Physics potential of the International Axion Observatory (IAXO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Attie%2C+D">D. Attie</a>, <a href="/search/?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/?searchtype=author&query=Bykovskiy%2C+N">N. Bykovskiy</a>, <a href="/search/?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/?searchtype=author&query=Cicoli%2C+M">M. Cicoli</a>, <a href="/search/?searchtype=author&query=Civitani%2C+M">M. Civitani</a>, <a href="/search/?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/?searchtype=author&query=Conlon%2C+J+P">J. P. Conlon</a>, <a href="/search/?searchtype=author&query=Costa%2C+D">D. Costa</a>, <a href="/search/?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/?searchtype=author&query=Daido%2C+R">R. Daido</a>, <a href="/search/?searchtype=author&query=Derbin%2C+A+V">A. V. Derbin</a>, <a href="/search/?searchtype=author&query=Descalle%2C+M+A">M. A. Descalle</a>, <a href="/search/?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/?searchtype=author&query=Dratchnev%2C+I+S">I. S. Dratchnev</a>, <a href="/search/?searchtype=author&query=D%7F%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/?searchtype=author&query=Dudarev%2C+A">A. Dudarev</a>, <a href="/search/?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/?searchtype=author&query=Fleck%2C+I">I. Fleck</a>, <a href="/search/?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/?searchtype=author&query=Galanti%2C+G">G. Galanti</a> , et al. (66 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="1904.09155v3-abstract-short" style="display: inline;"> We review the physics potential of a next generation search for solar axions: the International Axion Observatory (IAXO). Endowed with a sensitivity to discover axion-like particles (ALPs) with a coupling to photons as small as $g_{a纬}\sim 10^{-12}$ GeV$^{-1}$, or to electrons $g_{ae}\sim$10$^{-13}$, IAXO has the potential to find the QCD axion in the 1 meV$\sim$1 eV mass range where it solves the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09155v3-abstract-full').style.display = 'inline'; document.getElementById('1904.09155v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.09155v3-abstract-full" style="display: none;"> We review the physics potential of a next generation search for solar axions: the International Axion Observatory (IAXO). Endowed with a sensitivity to discover axion-like particles (ALPs) with a coupling to photons as small as $g_{a纬}\sim 10^{-12}$ GeV$^{-1}$, or to electrons $g_{ae}\sim$10$^{-13}$, IAXO has the potential to find the QCD axion in the 1 meV$\sim$1 eV mass range where it solves the strong CP problem, can account for the cold dark matter of the Universe and be responsible for the anomalous cooling observed in a number of stellar systems. At the same time, IAXO will have enough sensitivity to detect lower mass axions invoked to explain: 1) the origin of the anomalous "transparency" of the Universe to gamma-rays, 2) the observed soft X-ray excess from galaxy clusters or 3) some inflationary models. In addition, we review string theory axions with parameters accessible by IAXO and discuss their potential role in cosmology as Dark Matter and Dark Radiation as well as their connections to the above mentioned conundrums. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09155v3-abstract-full').style.display = 'none'; document.getElementById('1904.09155v3-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> 6 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </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">Prepared for submission to JCAP; new version with very minor corrections after referee review</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Armengaud%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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 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