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value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?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/2404.03002">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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Bera%2C+A">A. Bera</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?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/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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?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/2101.11564">arXiv:2101.11564</a> <span> [<a href="https://arxiv.org/pdf/2101.11564">pdf</a>, <a href="https://arxiv.org/format/2101.11564">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 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/10.1117/12.2562565">10.1117/12.2562565 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the Dark Energy Spectroscopic Instrument(DESI) Fiber System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Poppett%2C+C">Claire Poppett</a>, <a href="/search/astro-ph?searchtype=author&query=Jelinsky%2C+P">Patrick Jelinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Edelstein%2C+J">Jerry Edelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Jelinsky%2C+S">Sharon Jelinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Sharples%2C+R">Ray Sharples</a>, <a href="/search/astro-ph?searchtype=author&query=Schmoll%2C+J">Jurgen Schmoll</a>, <a href="/search/astro-ph?searchtype=author&query=Bramall%2C+D">David Bramall</a>, <a href="/search/astro-ph?searchtype=author&query=Tyas%2C+L">Luke Tyas</a>, <a href="/search/astro-ph?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M">Michael Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Yutong%2C+D">Duan Yutong</a>, <a href="/search/astro-ph?searchtype=author&query=Tarle%2C+G">Gregory Tarle</a>, <a href="/search/astro-ph?searchtype=author&query=Gaztanaga%2C+E">Erique Gaztanaga</a>, <a href="/search/astro-ph?searchtype=author&query=Prada%2C+F">Francisco Prada</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+t+D">the DESI 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="2101.11564v2-abstract-short" style="display: inline;"> The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion historyof the universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasarsover 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for theKPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11564v2-abstract-full').style.display = 'inline'; document.getElementById('2101.11564v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.11564v2-abstract-full" style="display: none;"> The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion historyof the universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasarsover 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for theKPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers in turn feed ten broad-bandspectrographs. We describe key aspects and lessons learned from the development, delivery and installation ofthe fiber system at the Mayall telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11564v2-abstract-full').style.display = 'none'; document.getElementById('2101.11564v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">9 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SPIE 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.00037">arXiv:1611.00037</a> <span> [<a href="https://arxiv.org/pdf/1611.00037">pdf</a>, <a href="https://arxiv.org/format/1611.00037">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> <p class="title is-5 mathjax"> The DESI Experiment Part II: Instrument Design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aghamousa%2C+A">Amir Aghamousa</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steve Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L+E">Lori E. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">James Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balland%2C+C">Christophe Balland</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">Otger Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">Charles Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Beaufore%2C+L">Lucas Beaufore</a>, <a href="/search/astro-ph?searchtype=author&query=Bebek%2C+C">Chris Bebek</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bernal%2C+J+L">Jos茅 Luis Bernal</a>, <a href="/search/astro-ph?searchtype=author&query=Besuner%2C+R">Robert Besuner</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">Chris Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Bleuler%2C+H">Hannes Bleuler</a>, <a href="/search/astro-ph?searchtype=author&query=Blomqvist%2C+M">Michael Blomqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+A+S">Adam S. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Briceno%2C+C">Cesar Briceno</a> , et al. (268 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="1611.00037v2-abstract-short" style="display: inline;"> DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00037v2-abstract-full').style.display = 'inline'; document.getElementById('1611.00037v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00037v2-abstract-full" style="display: none;"> DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= 位/螖位$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00037v2-abstract-full').style.display = 'none'; document.getElementById('1611.00037v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.00036">arXiv:1611.00036</a> <span> [<a href="https://arxiv.org/pdf/1611.00036">pdf</a>, <a href="https://arxiv.org/format/1611.00036">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> <p class="title is-5 mathjax"> The DESI Experiment Part I: Science,Targeting, and Survey Design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aghamousa%2C+A">Amir Aghamousa</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steve Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L+E">Lori E. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">James Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balland%2C+C">Christophe Balland</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">Otger Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">Charles Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Beaufore%2C+L">Lucas Beaufore</a>, <a href="/search/astro-ph?searchtype=author&query=Bebek%2C+C">Chris Bebek</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bernal%2C+J+L">Jos茅 Luis Bernal</a>, <a href="/search/astro-ph?searchtype=author&query=Besuner%2C+R">Robert Besuner</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">Chris Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Bleuler%2C+H">Hannes Bleuler</a>, <a href="/search/astro-ph?searchtype=author&query=Blomqvist%2C+M">Michael Blomqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+A+S">Adam S. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Briceno%2C+C">Cesar Briceno</a> , et al. (268 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="1611.00036v2-abstract-short" style="display: inline;"> DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00036v2-abstract-full').style.display = 'inline'; document.getElementById('1611.00036v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00036v2-abstract-full" style="display: none;"> DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$伪$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00036v2-abstract-full').style.display = 'none'; document.getElementById('1611.00036v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.0847">arXiv:1308.0847</a> <span> [<a href="https://arxiv.org/pdf/1308.0847">pdf</a>, <a href="https://arxiv.org/format/1308.0847">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The DESI Experiment, a whitepaper for Snowmass 2013 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M">Michael Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Bebek%2C+C">Chris Bebek</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T">Timothy Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Cahn%2C+R">Robert Cahn</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D">Daniel Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">Brenna Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kron%2C+R">Richard Kron</a>, <a href="/search/astro-ph?searchtype=author&query=Lahav%2C+O">Ofer Lahav</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+P">Patrick McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Roe%2C+N">Natalie Roe</a>, <a href="/search/astro-ph?searchtype=author&query=Schlegel%2C+D">David Schlegel</a>, <a href="/search/astro-ph?searchtype=author&query=collaboration%2C+r+t+D">representing the DESI 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="1308.0847v1-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) is a massively multiplexed fiber-fed spectrograph that will make the next major advance in dark energy in the timeframe 2018-2022. On the Mayall telescope, DESI will obtain spectra and redshifts for at least 18 million emission-line galaxies, 4 million luminous red galaxies and 3 million quasi-stellar objects, in order to: probe the effects of dark e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0847v1-abstract-full').style.display = 'inline'; document.getElementById('1308.0847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.0847v1-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) is a massively multiplexed fiber-fed spectrograph that will make the next major advance in dark energy in the timeframe 2018-2022. On the Mayall telescope, DESI will obtain spectra and redshifts for at least 18 million emission-line galaxies, 4 million luminous red galaxies and 3 million quasi-stellar objects, in order to: probe the effects of dark energy on the expansion history using baryon acoustic oscillations (BAO), measure the gravitational growth history through redshift-space distortions, measure the sum of neutrino masses, and investigate the signatures of primordial inflation. The resulting 3-D galaxy maps at z<2 and Lyman-alpha forest at z>2 will make 1%-level measurements of the distance scale in 35 redshift bins, thus providing unprecedented constraints on cosmological models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0847v1-abstract-full').style.display = 'none'; document.getElementById('1308.0847v1-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 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </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">14 pages, 4 figures, a White Paper for Snowmass 2013</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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