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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="2411.12021v2-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('2411.12021v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12021v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12021v2-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('2411.12021v2-abstract-full').style.display = 'none'; document.getElementById('2411.12021v2-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 December, 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/). 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/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 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/10.1088/1475-7516/2025/01/124">10.1088/1475-7516/2025/01/124 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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/2403.05688">arXiv:2403.05688</a> <span> [<a href="https://arxiv.org/pdf/2403.05688">pdf</a>, <a href="https://arxiv.org/format/2403.05688">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> </div> </div> <p class="title is-5 mathjax"> Measuring Fiber Positioning Accuracy and Throughput with Fiber Dithering for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schlafly%2C+E+F">E. F. Schlafly</a>, <a href="/search/?searchtype=author&query=Schlegel%2C+D">D. Schlegel</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Raichoor%2C+A">A. Raichoor</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</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=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=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">Arjun Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</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=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Hahn%2C+C">C. Hahn</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Jimenez%2C+J">J. Jimenez</a>, <a href="/search/?searchtype=author&query=Kent%2C+S">S. Kent</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> , et al. (25 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="2403.05688v1-abstract-short" style="display: inline;"> Highly multiplexed, fiber-fed spectroscopy is enabling surveys of millions of stars and galaxies. The performance of these surveys depends on accurately positioning fibers in the focal plane to capture target light. We describe a technique to measure the positioning accuracy of fibers by dithering fibers slightly around their ideal locations. This approach also enables measurement of the total sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05688v1-abstract-full').style.display = 'inline'; document.getElementById('2403.05688v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05688v1-abstract-full" style="display: none;"> Highly multiplexed, fiber-fed spectroscopy is enabling surveys of millions of stars and galaxies. The performance of these surveys depends on accurately positioning fibers in the focal plane to capture target light. We describe a technique to measure the positioning accuracy of fibers by dithering fibers slightly around their ideal locations. This approach also enables measurement of the total system throughput and point spread function delivered to the focal plane. We then apply this technique to observations from the Dark Energy Survey Instrument (DESI), and demonstrate that DESI positions fibers to within 0.08" of their targets (5% of a fiber diameter) and achieves a system throughput within about 5% of expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05688v1-abstract-full').style.display = 'none'; document.getElementById('2403.05688v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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, 9 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/2402.18009">arXiv:2402.18009</a> <span> [<a href="https://arxiv.org/pdf/2402.18009">pdf</a>, <a href="https://arxiv.org/format/2402.18009">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/10.1088/1475-7516/2025/01/130">10.1088/1475-7516/2025/01/130 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of Systematic Redshift Errors on the Cross-correlation of the Lyman-$伪$ Forest with Quasars at Small Scales Using DESI Early Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bault%2C+A">Abby Bault</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">Allyson Brodzeller</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=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=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</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=Dey%2C+A">A. Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Filbert%2C+S">S. Filbert</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=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=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=Honscheid%2C+K">K. Honscheid</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="2402.18009v2-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) will measure millions of quasar spectra by the end of its 5 year survey. Quasar redshift errors impact the shape of the Lyman-$伪$ forest correlation functions, which can affect cosmological analyses and therefore cosmological interpretations. Using data from the DESI Early Data Release and the first two months of the main survey, we measure the syste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18009v2-abstract-full').style.display = 'inline'; document.getElementById('2402.18009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18009v2-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) will measure millions of quasar spectra by the end of its 5 year survey. Quasar redshift errors impact the shape of the Lyman-$伪$ forest correlation functions, which can affect cosmological analyses and therefore cosmological interpretations. Using data from the DESI Early Data Release and the first two months of the main survey, we measure the systematic redshift error from an offset in the cross-correlation of the Lyman-$伪$ forest with quasars. We find evidence for a redshift dependent bias causing redshifts to be underestimated with increasing redshift, stemming from improper modeling of the Lyman-$伪$ optical depth in the templates used for redshift estimation. New templates were derived for the DESI Year 1 quasar sample at $z > 1.6$ and we found the redshift dependent bias, $螖r_\parallel$, increased from $-1.94 \pm 0.15$ $h^{-1}$ Mpc to $-0.08 \pm 0.04$ $h^{-1}$ Mpc ($-205 \pm 15~\text{km s}^{-1}$ to $-9.0 \pm 4.0~\text{km s}^{-1}$). These new templates will be used to provide redshifts for the DESI Year 1 quasar sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18009v2-abstract-full').style.display = 'none'; document.getElementById('2402.18009v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">29 pages, 9 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP01(2025)130 </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 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/10.1088/1475-7516/2025/01/141">10.1088/1475-7516/2025/01/141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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="2401.00303v3-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('2401.00303v3-abstract-full').style.display = 'inline'; document.getElementById('2401.00303v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.00303v3-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('2401.00303v3-abstract-full').style.display = 'none'; document.getElementById('2401.00303v3-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 January, 2025; <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, JCAP accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03434">arXiv:2309.03434</a> <span> [<a href="https://arxiv.org/pdf/2309.03434">pdf</a>, <a href="https://arxiv.org/format/2309.03434">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"> Broad Absorption Line Quasars in the Dark Energy Spectroscopic Instrument Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Filbert%2C+S">S. Filbert</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/?searchtype=author&query=Seebaluck%2C+K">K. Seebaluck</a>, <a href="/search/?searchtype=author&query=Ennesser%2C+L">L. Ennesser</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</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=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</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=Tan%2C+T">T. Tan</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=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</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=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</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> , et al. (19 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="2309.03434v2-abstract-short" style="display: inline;"> Broad absorption line (BAL) quasars are characterized by gas clouds that absorb flux at the wavelength of common quasar spectral features, although blueshifted by velocities that can exceed 0.1c. BAL features are interesting as signatures of significant feedback, yet they can also compromise cosmological studies with quasars by distorting the shape of the most prominent quasar emission lines, impa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03434v2-abstract-full').style.display = 'inline'; document.getElementById('2309.03434v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03434v2-abstract-full" style="display: none;"> Broad absorption line (BAL) quasars are characterized by gas clouds that absorb flux at the wavelength of common quasar spectral features, although blueshifted by velocities that can exceed 0.1c. BAL features are interesting as signatures of significant feedback, yet they can also compromise cosmological studies with quasars by distorting the shape of the most prominent quasar emission lines, impacting redshift accuracy and measurements of the matter density distribution traced by the Lyman-alpha forest. We present a catalog of BAL quasars discovered in the Dark Energy Spectroscopic Instrument (DESI) survey Early Data Release, which were observed as part of DESI Survey Validation, as well as the first two months of the main survey. We describe our method to automatically identify BAL quasars in DESI data, the quantities we measure for each BAL, and investigate the completeness and purity of this method with mock DESI observations. We mask the wavelengths of the BAL features and re-evaluate each BAL quasar redshift, finding new redshifts which are 243 km/s smaller on average for the BAL quasar sample. These new, more accurate redshifts are important to obtain the best measurements of quasar clustering, especially at small scales. Finally, we present some spectra of rarer classes of BALs that illustrate the potential of DESI data to identify such populations for further study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03434v2-abstract-full').style.display = 'none'; document.getElementById('2309.03434v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </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/2306.06308">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/2212.06754">arXiv:2212.06754</a> <span> [<a href="https://arxiv.org/pdf/2212.06754">pdf</a>, <a href="https://arxiv.org/format/2212.06754">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/10.3847/1538-4357/accc88">10.3847/1538-4357/accc88 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved Tomographic Binning of 3x2pt Lens Samples: Neural Network Classifiers and Optimal Bin Assignments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Moskowitz%2C+I">Irene Moskowitz</a>, <a href="/search/?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">Abby Bault</a>, <a href="/search/?searchtype=author&query=Broussard%2C+A">Adam Broussard</a>, <a href="/search/?searchtype=author&query=Newman%2C+J+A">Jeffrey A. Newman</a>, <a href="/search/?searchtype=author&query=Zuntz%2C+J">Joe Zuntz</a>, <a href="/search/?searchtype=author&query=Collaboration%2C+t+L+D+E+S">the LSST Dark Energy Science Collaboration</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="2212.06754v2-abstract-short" style="display: inline;"> Large imaging surveys, such as the Legacy Survey of Space and Time, rely on photometric redshifts and tomographic binning for 3x2pt analyses that combine galaxy clustering and weak lensing. In this paper, we propose a method for optimizing the tomographic binning choice for the lens sample of galaxies. We divide the CosmoDC2 and Buzzard simulated galaxy catalogs into a training set and an applicat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06754v2-abstract-full').style.display = 'inline'; document.getElementById('2212.06754v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.06754v2-abstract-full" style="display: none;"> Large imaging surveys, such as the Legacy Survey of Space and Time, rely on photometric redshifts and tomographic binning for 3x2pt analyses that combine galaxy clustering and weak lensing. In this paper, we propose a method for optimizing the tomographic binning choice for the lens sample of galaxies. We divide the CosmoDC2 and Buzzard simulated galaxy catalogs into a training set and an application set, where the training set is nonrepresentative in a realistic way, and then estimate photometric redshifts for the application sets. The galaxies are sorted into redshift bins covering equal intervals of redshift or comoving distance, or with an equal number of galaxies in each bin, and we consider a generalized extension of these approaches. We find that bins of equal comoving distance produce the highest dark energy figure of merit of the initial binning choices, but that the choice of bin edges can be further optimized. We then train a neural network classifier to identify galaxies that are either highly likely to have accurate photometric redshift estimates or highly likely to be sorted into the correct redshift bin. The neural network classifier is used to remove poor redshift estimates from the sample, and the results are compared to the case when none of the sample is removed. We find that the neural network classifiers are able to improve the figure of merit by ~13% and are able to recover ~25% of the loss in the figure of merit that occurs when a nonrepresentative training sample is used. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06754v2-abstract-full').style.display = 'none'; document.getElementById('2212.06754v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">18 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 950 49 (2023) </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/2108.13418">arXiv:2108.13418</a> <span> [<a href="https://arxiv.org/pdf/2108.13418">pdf</a>, <a href="https://arxiv.org/format/2108.13418">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/10.21105/astro.2108.13418">10.21105/astro.2108.13418 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LSST-DESC 3x2pt Tomography Optimization Challenge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zuntz%2C+J">Joe Zuntz</a>, <a href="/search/?searchtype=author&query=Lanusse%2C+F">Fran莽ois Lanusse</a>, <a href="/search/?searchtype=author&query=Malz%2C+A+I">Alex I. Malz</a>, <a href="/search/?searchtype=author&query=Wright%2C+A+H">Angus H. Wright</a>, <a href="/search/?searchtype=author&query=Slosar%2C+A">An啪e Slosar</a>, <a href="/search/?searchtype=author&query=Abolfathi%2C+B">Bela Abolfathi</a>, <a href="/search/?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">Abby Bault</a>, <a href="/search/?searchtype=author&query=Bom%2C+C+R">Cl茅cio R. Bom</a>, <a href="/search/?searchtype=author&query=Brescia%2C+M">Massimo Brescia</a>, <a href="/search/?searchtype=author&query=Broussard%2C+A">Adam Broussard</a>, <a href="/search/?searchtype=author&query=Campagne%2C+J">Jean-Eric Campagne</a>, <a href="/search/?searchtype=author&query=Cavuoti%2C+S">Stefano Cavuoti</a>, <a href="/search/?searchtype=author&query=Cypriano%2C+E+S">Eduardo S. Cypriano</a>, <a href="/search/?searchtype=author&query=Fraga%2C+B+M+O">Bernardo M. O. Fraga</a>, <a href="/search/?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/?searchtype=author&query=Gonzalez%2C+E+J">Elizabeth J. Gonzalez</a>, <a href="/search/?searchtype=author&query=Green%2C+D">Dylan Green</a>, <a href="/search/?searchtype=author&query=Hatfield%2C+P">Peter Hatfield</a>, <a href="/search/?searchtype=author&query=Iyer%2C+K">Kartheik Iyer</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/?searchtype=author&query=Nicola%2C+A">Andrina Nicola</a>, <a href="/search/?searchtype=author&query=Nourbakhsh%2C+E">Erfan Nourbakhsh</a>, <a href="/search/?searchtype=author&query=Park%2C+A">Andy Park</a>, <a href="/search/?searchtype=author&query=Teixeira%2C+G">Gabriel Teixeira</a> , et al. (3 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="2108.13418v2-abstract-short" style="display: inline;"> This paper presents the results of the Rubin Observatory Dark Energy Science Collaboration (DESC) 3x2pt tomography challenge, which served as a first step toward optimizing the tomographic binning strategy for the main DESC analysis. The task of choosing an optimal tomographic binning scheme for a photometric survey is made particularly delicate in the context of a metacalibrated lensing catalogue… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.13418v2-abstract-full').style.display = 'inline'; document.getElementById('2108.13418v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.13418v2-abstract-full" style="display: none;"> This paper presents the results of the Rubin Observatory Dark Energy Science Collaboration (DESC) 3x2pt tomography challenge, which served as a first step toward optimizing the tomographic binning strategy for the main DESC analysis. The task of choosing an optimal tomographic binning scheme for a photometric survey is made particularly delicate in the context of a metacalibrated lensing catalogue, as only the photometry from the bands included in the metacalibration process (usually riz and potentially g) can be used in sample definition. The goal of the challenge was to collect and compare bin assignment strategies under various metrics of a standard 3x2pt cosmology analysis in a highly idealized setting to establish a baseline for realistically complex follow-up studies; in this preliminary study, we used two sets of cosmological simulations of galaxy redshifts and photometry under a simple noise model neglecting photometric outliers and variation in observing conditions, and contributed algorithms were provided with a representative and complete training set. We review and evaluate the entries to the challenge, finding that even from this limited photometry information, multiple algorithms can separate tomographic bins reasonably well, reaching figures-of-merit scores close to the attainable maximum. We further find that adding the g band to riz photometry improves metric performance by ~15% and that the optimal bin assignment strategy depends strongly on the science case: which figure-of-merit is to be optimized, and which observables (clustering, lensing, or both) are included. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.13418v2-abstract-full').style.display = 'none'; document.getElementById('2108.13418v2-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">30 pages (incl. 12 in appendix), 12 figures. Version accepted for publication in the Open Journal of Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESC-PUB-00054 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 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