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Horizon-Free Measurement of $H_0$ in DESI 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zaborowski%2C+E+A">E. A. Zaborowski</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+P">P. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Huterer%2C+D">D. Huterer</a>, <a href="/search/astro-ph?searchtype=author&query=Krolewski%2C+A">A. Krolewski</a>, <a href="/search/astro-ph?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+C">C. To</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+A">A. Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a> , et al. (31 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="2411.16677v1-abstract-short" style="display: inline;"> The physical size of the sound horizon at recombination is a powerful source of information for early-time measurements of the Hubble constant $H_0$, and many proposed solutions to the Hubble tension therefore involve modifications to this scale. In light of this, there has been growing interest in measuring $H_0$ independently of the sound horizon. We present the first such measurement to use dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16677v1-abstract-full').style.display = 'inline'; document.getElementById('2411.16677v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16677v1-abstract-full" style="display: none;"> The physical size of the sound horizon at recombination is a powerful source of information for early-time measurements of the Hubble constant $H_0$, and many proposed solutions to the Hubble tension therefore involve modifications to this scale. In light of this, there has been growing interest in measuring $H_0$ independently of the sound horizon. We present the first such measurement to use data from the Dark Energy Spectroscopic Instrument (DESI), jointly analyzing the full-shape galaxy power spectra of DESI luminous red galaxies, emission line galaxies, quasars, and the bright galaxy sample, in a total of six redshift bins. Information from the sound horizon scale is removed from our constraints via a rescaling procedure at the power spectrum level, with our sound horizon-marginalized measurement being driven instead primarily by the matter-radiation equality scale. This measurement is then combined with additional sound horizon-free information from Planck+ACT CMB lensing, uncalibrated type Ia supernovae, and the DESI Lyman-$伪$ forest. We agnostically combine with the DESY5, Pantheon+, and Union3 supernova datasets, with our tightest respective constraints being $H_0=66.7^{+1.7}_{-1.9},~67.9^{+1.9}_{-2.1},$ and $67.8^{+2.0}_{-2.2}$ km s-1 Mpc-1. This corresponds to a sub-3% sound horizon-free constraint of the Hubble constant, and is the most precise measurement of its kind to date. Even without including information from the sound horizon, our measurement is still in 2.2-3.0$蟽$ tension with SH0ES. Additionally, the consistency between our result and other measurements that do rely on the sound horizon scale provides no evidence for new early-Universe physics (e.g. early dark energy). Future DESI data releases will allow unprecedented measurements of $H_0$ and place strong constraints on models that use beyond-$螞$CDM physics to ameliorate the Hubble tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16677v1-abstract-full').style.display = 'none'; document.getElementById('2411.16677v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 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">17+7 pages; 5 figures. Submitted to 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/2411.12027">arXiv:2411.12027</a> <span> [<a href="https://arxiv.org/pdf/2411.12027">pdf</a>, <a href="https://arxiv.org/format/2411.12027">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"> Analytical and EZmock covariance validation for the DESI 2024 results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Forero-S%C3%A1nchez%2C+D">Daniel Forero-S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">Michael Rashkovetskyi</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">Ot谩vio Alves</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">Arnaud de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">Seshadri Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">Pauline Zarrouk</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H茅ctor Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Zhejie Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+J">Jiaxi Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">Uendert Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xinyi Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">Cristhian Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">Juan Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">Davide Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">Etienne Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">Edmond Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+M+E">Miguel Enriquez Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a> , et al. (21 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="2411.12027v2-abstract-short" style="display: inline;"> The estimation of uncertainties in cosmological parameters is an important challenge in Large-Scale-Structure (LSS) analyses. For standard analyses such as Baryon Acoustic Oscillations (BAO) and Full Shape, two approaches are usually considered. First: analytical estimates of the covariance matrix use Gaussian approximations and (nonlinear) clustering measurements to estimate the matrix, which all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12027v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12027v2-abstract-full" style="display: none;"> The estimation of uncertainties in cosmological parameters is an important challenge in Large-Scale-Structure (LSS) analyses. For standard analyses such as Baryon Acoustic Oscillations (BAO) and Full Shape, two approaches are usually considered. First: analytical estimates of the covariance matrix use Gaussian approximations and (nonlinear) clustering measurements to estimate the matrix, which allows a relatively fast and computationally cheap way to generate matrices that adapt to an arbitrary clustering measurement. On the other hand, sample covariances are an empirical estimate of the matrix based on en ensemble of clustering measurements from fast and approximate simulations. While more computationally expensive due to the large amount of simulations and volume required, these allow us to take into account systematics that are impossible to model analytically. In this work we compare these two approaches in order to enable DESI's key analyses. We find that the configuration space analytical estimate performs satisfactorily in BAO analyses and its flexibility in terms of input clustering makes it the fiducial choice for DESI's 2024 BAO analysis. On the contrary, the analytical computation of the covariance matrix in Fourier space does not reproduce the expected measurements in terms of Full Shape analyses, which motivates the use of a corrected mock covariance for DESI's Full Shape analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12027v2-abstract-full').style.display = 'none'; document.getElementById('2411.12027v2-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">23 pages, 5 figures 7 tables, submitted to 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/2411.12026">arXiv:2411.12026</a> <span> [<a href="https://arxiv.org/pdf/2411.12026">pdf</a>, <a href="https://arxiv.org/format/2411.12026">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"> Modified Gravity Constraints from the Full Shape Modeling of Clustering Measurements from DESI 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+J">J. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Calderon%2C+R">R. Calderon</a>, <a href="/search/astro-ph?searchtype=author&query=Lodha%2C+K">K. Lodha</a>, <a href="/search/astro-ph?searchtype=author&query=Valogiannis%2C+G">G. Valogiannis</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Niz%2C+G">G. Niz</a>, <a href="/search/astro-ph?searchtype=author&query=Yi%2C+L">L. Yi</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+C">C. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Medina-Varela%2C+L">L. Medina-Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Cervantes-Cota%2C+J+L">J. L. Cervantes-Cota</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Huterer%2C+D">D. Huterer</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega%2C+H+E">H. E. Noriega</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+G">G. Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Shafieloo%2C+A">A. Shafieloo</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+W">W. Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.12026v1-abstract-short" style="display: inline;"> We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other datasets. We first consider the $渭(a,k)$-$危(a,k)$ modified gravity (MG) parametrization (as well as $畏(a,k)$) in flat $螞$CDM and $w_0 w_a$CDM backgrounds. Using a functional form for time-only ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12026v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12026v1-abstract-full" style="display: none;"> We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other datasets. We first consider the $渭(a,k)$-$危(a,k)$ modified gravity (MG) parametrization (as well as $畏(a,k)$) in flat $螞$CDM and $w_0 w_a$CDM backgrounds. Using a functional form for time-only evolution gives $渭_0= 0.11^{+0.44}_{-0.54}$ from DESI(FS+BAO)+BBN and a wide prior on $n_{s}$. Using DESI(FS+BAO)+CMB+DESY3+DESY5-SN, we obtain $渭_0 = 0.05\pm 0.22$ and $危_0 = 0.009\pm 0.045$ in the $螞$CDM background. In $w_0 w_a$CDM, we obtain $渭_0 =-0.24^{+0.32}_{-0.28}$ and $危_0 = 0.006\pm 0.043$, consistent with GR, and we still find a preference of the data for dynamical dark energy with $w_0>-1$ and $w_a<0$. We then use binned forms in the two backgrounds starting with two bins in redshift and then combining them with two bins in scale for a total of 4 and 8 MG parameters, respectively. All MG parameters are found consistent with GR. We also find that the tension reported for $危_0$ with GR when using Planck PR3 goes away when we use the recent LoLLiPoP+HiLLiPoP likelihoods. As noted previously, this seems to indicate that the tension is related to the CMB lensing anomaly in PR3 which is also alleviated when using these likelihoods. We then constrain the class of Horndeski theory in the effective field theory of dark energy. We consider both EFT-basis and $伪$-basis. Assuming a power law parametrization for the function $惟$, which controls non-minimal coupling, we obtain $惟_0 = 0.0120^{+0.0021}_{-0.013}$ and $s_0 = 0.99^{+0.54}_{-0.20}$ from DESI(FS+BAO)+DESY5SN+CMB in a $螞$CDM background. Similar results are obtained when using the $伪$-basis, where we constrain $c_M<1.24$, and are all consistent with GR. [Abridged.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12026v1-abstract-full').style.display = 'none'; document.getElementById('2411.12026v1-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">52 pages, 10 figures. This DESI Collaboration 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/2411.12025">arXiv:2411.12025</a> <span> [<a href="https://arxiv.org/pdf/2411.12025">pdf</a>, <a href="https://arxiv.org/format/2411.12025">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 DESI fiber assignment incompleteness effect on 2-point clustering and mitigation methods for DR1 analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Hanif%2C+M+M+S">M. M. S Hanif</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">J. Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Pinon%2C+M">M. Pinon</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">M. White</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">C. Hahn</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a> , et al. (30 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="2411.12025v1-abstract-short" style="display: inline;"> We present an in-depth analysis of the fiber assignment incompleteness in the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1). This incompleteness is caused by the restricted mobility of the robotic fiber positioner in the DESI focal plane, which limits the number of galaxies that can be observed at the same time, especially at small angular separations. As a result, the observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12025v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12025v1-abstract-full" style="display: none;"> We present an in-depth analysis of the fiber assignment incompleteness in the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1). This incompleteness is caused by the restricted mobility of the robotic fiber positioner in the DESI focal plane, which limits the number of galaxies that can be observed at the same time, especially at small angular separations. As a result, the observed clustering amplitude is suppressed in a scale-dependent manner, which, if not addressed, can severely impact the inference of cosmological parameters. We discuss the methods adopted for simulating fiber assignment on mocks and data. In particular, we introduce the fast fiber assignment (FFA) emulator, which was employed to obtain the power spectrum covariance adopted for the DR1 full-shape analysis. We present the mitigation techniques, organised in two classes: measurement stage and model stage. We then use high fidelity mocks as a reference to quantify both the accuracy of the FFA emulator and the effectiveness of the different measurement-stage mitigation techniques. This complements the studies conducted in a parallel paper for the model-stage techniques, namely the $胃$-cut approach. We find that pairwise inverse probability (PIP) weights with angular upweighting recover the "true" clustering in all the cases considered, in both Fourier and configuration space. Notably, we present the first ever power spectrum measurement with PIP weights from real data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12025v1-abstract-full').style.display = 'none'; document.getElementById('2411.12025v1-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">42 pages, 19 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/2411.12023">arXiv:2411.12023</a> <span> [<a href="https://arxiv.org/pdf/2411.12023">pdf</a>, <a href="https://arxiv.org/format/2411.12023">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"> Exploring HOD-dependent systematics for the DESI 2024 Full-Shape galaxy clustering analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Findlay%2C+N">N. Findlay</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">S. Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+W+J">W. J. Percival</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">P. Zarrouk</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Rocher%2C+A">A. Rocher</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">C. Hahn</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.12023v2-abstract-short" style="display: inline;"> We analyse the robustness of the DESI 2024 cosmological inference from fits to the full shape of the galaxy power spectrum to uncertainties in the Halo Occupation Distribution (HOD) model of the galaxy-halo connection and the choice of priors on nuisance parameters. We assess variations in the recovered cosmological parameters across a range of mocks populated with different HOD models and find th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12023v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12023v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12023v2-abstract-full" style="display: none;"> We analyse the robustness of the DESI 2024 cosmological inference from fits to the full shape of the galaxy power spectrum to uncertainties in the Halo Occupation Distribution (HOD) model of the galaxy-halo connection and the choice of priors on nuisance parameters. We assess variations in the recovered cosmological parameters across a range of mocks populated with different HOD models and find that shifts are often greater than 20% of the expected statistical uncertainties from the DESI data. We encapsulate the effect of such shifts in terms of a systematic covariance term, $\mathsf{C}_{\rm HOD}$, and an additional diagonal contribution quantifying the impact of our choice of nuisance parameter priors on the ability of the effective field theory (EFT) model to correctly recover the cosmological parameters of the simulations. These two covariance contributions are designed to be added to the usual covariance term, $\mathsf{C}_{\rm stat}$, describing the statistical uncertainty in the power spectrum measurement, in order to fairly represent these sources of systematic uncertainty. This approach is more general and robust to choices of model free parameters or additional external datasets used in cosmological fits than the alternative approach of adding systematic uncertainties at the level of the recovered marginalised parameter posteriors. We compare the approaches within the context of a fixed $螞$CDM model and demonstrate that our method gives conservative estimates of the systematic uncertainty that nevertheless have little impact on the final posteriors obtained from DESI data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12023v2-abstract-full').style.display = 'none'; document.getElementById('2411.12023v2-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 Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 26 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/2411.12022">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="2411.12021v1-abstract-short" style="display: inline;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we exte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12021v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12021v1-abstract-full" style="display: none;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we extend previous DESI DR1 baryon acoustic oscillation (BAO) measurements to include redshift-space distortions and signals from the matter-radiation equality scale. For the first time, this Full-Shape analysis is blinded at the catalogue-level to avoid confirmation bias and the systematic errors are accounted for at the two-point clustering level, which automatically propagates them into any cosmological parameter. When analysing the data in terms of compressed model-agnostic variables, we obtain a combined precision of 4.7\% on the amplitude of the redshift space distortion signal reaching similar precision with just one year of DESI data than with 20 years of observation from previous generation surveys. We analyse the data to directly constrain the cosmological parameters within the $螞$CDM model using perturbation theory and combine this information with the reconstructed DESI DR1 galaxy BAO. Using a Big Bang Nucleosynthesis Gaussian prior on the baryon density parameter, and a Gaussian prior on the spectral index, we constrain the matter density is $惟_m=0.296\pm 0.010 $ and the Hubble constant $H_0=(68.63 \pm 0.79)[{\rm km\, s^{-1}Mpc^{-1}}]$. Additionally, we measure the amplitude of clustering $蟽_8=0.841 \pm 0.034$. The DESI DR1 results are in agreement with the $螞$CDM model based on general relativity with parameters consistent with those from Planck. The cosmological interpretation of these results in combination with external datasets are presented in a companion paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v1-abstract-full').style.display = 'none'; document.getElementById('2411.12021v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 76 pages, 20 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12020">arXiv:2411.12020</a> <span> [<a href="https://arxiv.org/pdf/2411.12020">pdf</a>, <a href="https://arxiv.org/format/2411.12020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 II: Sample Definitions, Characteristics, and Two-point Clustering Statistics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/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/2411.00148">arXiv:2411.00148</a> <span> [<a href="https://arxiv.org/pdf/2411.00148">pdf</a>, <a href="https://arxiv.org/format/2411.00148">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"> DESIVAST: A Catalog of Low-Redshift Voids using Data from the DESI DR1 Bright Galaxy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rincon%2C+H">Hernan Rincon</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">Segev BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Douglass%2C+K">Kelly Douglass</a>, <a href="/search/astro-ph?searchtype=author&query=Veyrat%2C+D">Dahlia Veyrat</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">Davide Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S">Sergey Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">Andrew Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">Laurent Le Guillou</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.00148v1-abstract-short" style="display: inline;"> We present three separate void catalogs created using a volume-limited sample of the DESI Year 1 Bright Galaxy Survey. We use the algorithms VoidFinder and V2 to construct void catalogs out to a redshift of z=0.24. We obtain 1,461 interior voids with VoidFinder, 420 with V2 using REVOLVER pruning, and 295 with V2 using VIDE pruning. Comparing our catalog with an overlapping SDSS void catalog, we f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00148v1-abstract-full').style.display = 'inline'; document.getElementById('2411.00148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.00148v1-abstract-full" style="display: none;"> We present three separate void catalogs created using a volume-limited sample of the DESI Year 1 Bright Galaxy Survey. We use the algorithms VoidFinder and V2 to construct void catalogs out to a redshift of z=0.24. We obtain 1,461 interior voids with VoidFinder, 420 with V2 using REVOLVER pruning, and 295 with V2 using VIDE pruning. Comparing our catalog with an overlapping SDSS void catalog, we find generally consistent void properties but significant differences in the void volume overlap, which we attribute to differences in the galaxy selection and survey masks. These catalogs are suitable for studying the variation in galaxy properties with cosmic environment and for cosmological studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00148v1-abstract-full').style.display = 'none'; document.getElementById('2411.00148v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 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">17 pages, 6 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/2410.19475">arXiv:2410.19475</a> <span> [<a href="https://arxiv.org/pdf/2410.19475">pdf</a>, <a href="https://arxiv.org/format/2410.19475">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The unabridged satellite luminosity function of Milky Way-like galaxies in $螞$CDM: the contribution of "orphan" satellites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Santos-Santos%2C+I">Isabel Santos-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C">Carlos Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J">Julio Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Helly%2C+J">John Helly</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="2410.19475v1-abstract-short" style="display: inline;"> We study the abundance, radial distribution, and orbits of luminous satellites in simulations of Milky Way-mass dark halos in the $螞$CDM cosmology. We follow the evolution of a halo from the Aquarius project and the formation of satellites with the GALFORM semi-analytic model of galaxy formation, in which gas cools radiatively into halos before reionization and in halos that exceed a redshift-depe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19475v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19475v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19475v1-abstract-full" style="display: none;"> We study the abundance, radial distribution, and orbits of luminous satellites in simulations of Milky Way-mass dark halos in the $螞$CDM cosmology. We follow the evolution of a halo from the Aquarius project and the formation of satellites with the GALFORM semi-analytic model of galaxy formation, in which gas cools radiatively into halos before reionization and in halos that exceed a redshift-dependent ``critical'' virial mass after that. Subhalos are prone to disruption in the tidal field of the main halo, with the number of surviving self-bound subhalos increasing with resolution. Even in the highest resolution simulation (Aq-L1, with particle mass $m_{\rm p}\sim10^3\, M_\odot$), a substantial number of subhalos are disrupted but their galaxies may survive as ``orphans''. Whether or not a satellite becomes an orphan depends primarily on its time of infall. When orphans are included, the simulations yield a converged satellite stellar mass function across different resolution levels. The total number of luminous satellites is sensitive to the assumed redshift of reionization, but the shape of the satellite stellar mass function is robust, peaking at the stellar mass ($\sim 10^3\, M_\odot$) of a halo just above the critical threshold. Most orphans are found in the central regions of the main halo and make up roughly half of all satellites in Aq-L1. When orphans are taken into account there is no need to populate subhalos below the critical mass with satellites to fit the radial distribution of Milky Way satellites, as had been argued in recent work. Our model predicts that orphans dominate the ultra-faint population and that many more satellites with small apocentric radii should be detected in upcoming deep wide-field surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19475v1-abstract-full').style.display = 'none'; document.getElementById('2410.19475v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages, 10 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.12987">arXiv:2410.12987</a> <span> [<a href="https://arxiv.org/pdf/2410.12987">pdf</a>, <a href="https://arxiv.org/format/2410.12987">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"> Galaxy Mass Modelling from Multi-Wavelength JWST Strong Lens Analysis: Dark Matter Substructure, Angular Mass Complexity, or Both? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lange%2C+S+C">Samuel C. Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Amvrosiadis%2C+A">Aristeidis Amvrosiadis</a>, <a href="/search/astro-ph?searchtype=author&query=Nightingale%2C+J+W">James W. Nightingale</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+Q">Qiuhan He</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+A">Andrew Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Massey%2C+R">Richard Massey</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+X">Xiaoyue Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">Ran Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kaihao Wang</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="2410.12987v1-abstract-short" style="display: inline;"> We analyze two galaxy-scale strong gravitational lenses, SPT0418-47 and SPT2147-50, using JWST NIRCam imaging across multiple filters. To account for angular complexity in the lens mass distribution, we introduce multipole perturbations with orders $m=1, 3, 4$. Our results show strong evidence for angular mass complexity in SPT2147, with multipole strengths of 0.3-1.7 $\%$ for $m=3, 4$ and 2.4-9.5… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12987v1-abstract-full').style.display = 'inline'; document.getElementById('2410.12987v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12987v1-abstract-full" style="display: none;"> We analyze two galaxy-scale strong gravitational lenses, SPT0418-47 and SPT2147-50, using JWST NIRCam imaging across multiple filters. To account for angular complexity in the lens mass distribution, we introduce multipole perturbations with orders $m=1, 3, 4$. Our results show strong evidence for angular mass complexity in SPT2147, with multipole strengths of 0.3-1.7 $\%$ for $m=3, 4$ and 2.4-9.5 $\%$ for $m=1$, while SPT0418 shows no such preference. We also test lens models that include a dark matter substructure, finding a strong preference for a substructure in SPT2147-50 with a Bayes factor (log-evidence change) of $\sim 60$ when multipoles are not included. Including multipoles reduces the Bayes factor to $\sim 11$, still corresponding to a $5蟽$ detection of a subhalo with an NFW mass of $\log_{10}(M_{200}/M_{\odot}) = 10.87\substack{+0.53\\ -0.71}$. While SPT2147-50 may represent the fourth detection of a dark matter substructure in a strong lens, further analysis is needed to confirm that the signal is not due to systematics associated with the lens mass model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12987v1-abstract-full').style.display = 'none'; document.getElementById('2410.12987v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages, 11 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09149">arXiv:2410.09149</a> <span> [<a href="https://arxiv.org/pdf/2410.09149">pdf</a>, <a href="https://arxiv.org/format/2410.09149">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Exploring the interaction between the MW and LMC with a large sample of blue horizontal branch stars from the DESI survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bystr%C3%B6m%2C+A">Amanda Bystr枚m</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Lilleengen%2C+S">Sophia Lilleengen</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T+S">Ting S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E">Eric Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L+B+e">Leandro Beraldo e Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Carrillo%2C+A">Andreia Carrillo</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+V">Vedant Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O+Y">Oleg Y. Gnedin</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J+J">Jiwon Jesse Han</a>, <a href="/search/astro-ph?searchtype=author&query=Medina%2C+G+E">Gustavo E. Medina</a>, <a href="/search/astro-ph?searchtype=author&query=Najita%2C+J">Joan Najita</a>, <a href="/search/astro-ph?searchtype=author&query=Riley%2C+A+H">Alexander H. Riley</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G">Guillaume Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Valluri%2C+M">Monica Valluri</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica N. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</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=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a> , et al. (20 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="2410.09149v1-abstract-short" style="display: inline;"> The Large Magellanic Cloud (LMC) is a Milky Way (MW) satellite that is massive enough to gravitationally attract the MW disc and inner halo, causing significant motion of the inner MW with respect to the outer halo. In this work, we probe this interaction by constructing a sample of 9,866 blue horizontal branch (BHB) stars with radial velocities from the DESI spectroscopic survey out to 120 kpc fr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09149v1-abstract-full').style.display = 'inline'; document.getElementById('2410.09149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09149v1-abstract-full" style="display: none;"> The Large Magellanic Cloud (LMC) is a Milky Way (MW) satellite that is massive enough to gravitationally attract the MW disc and inner halo, causing significant motion of the inner MW with respect to the outer halo. In this work, we probe this interaction by constructing a sample of 9,866 blue horizontal branch (BHB) stars with radial velocities from the DESI spectroscopic survey out to 120 kpc from the Galactic centre. This is the largest spectroscopic set of BHB stars in the literature to date, and it contains four times more stars with Galactocentric distances beyond 50 kpc than previous BHB catalogues. Using the DESI BHB sample combined with SDSS BHBs, we measure the bulk radial velocity of stars in the outer halo and observe that the velocity in the Southern Galactic hemisphere is different by 3.7$蟽$ from the North. Modelling the projected velocity field shows that its dipole component is directed at a point 22 degrees away from the LMC along its orbit, which we interpret as the travel direction of the inner MW. The velocity field includes a monopole term that is -24 km/s, which we refer to as compression velocity. This velocity is significantly larger than predicted by the current models of the MW and LMC interaction. This work uses DESI data from its first two years of observations, but we expect that with upcoming DESI data releases, the sample of BHB stars will increase and our ability to measure the MW-LMC interaction will improve significantly. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09149v1-abstract-full').style.display = 'none'; document.getElementById('2410.09149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">22 pages, 19 figures. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.08062">arXiv:2410.08062</a> <span> [<a href="https://arxiv.org/pdf/2410.08062">pdf</a>, <a href="https://arxiv.org/format/2410.08062">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"> High-redshift LBG selection from broadband and wide photometric surveys using a Random Forest algorithm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Payerne%2C+C">C. Payerne</a>, <a href="/search/astro-ph?searchtype=author&query=Doumerg%2C+W+d">W. d'Assignies Doumerg</a>, <a href="/search/astro-ph?searchtype=author&query=Y%C3%A8che%2C+C">C. Y猫che</a>, <a href="/search/astro-ph?searchtype=author&query=Ruhlmann-Kleider%2C+V">V. Ruhlmann-Kleider</a>, <a href="/search/astro-ph?searchtype=author&query=Raichoor%2C+A">A. Raichoor</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">D. Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">J. N. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M+E">M. E. Levi</a> , et al. (18 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="2410.08062v1-abstract-short" style="display: inline;"> In this paper, we investigate the possibility of selecting high-redshift Lyman-Break Galaxies (LBG) using current and future broadband wide photometric surveys, such as UNIONS or the Vera C. Rubin LSST, using a Random Forest algorithm. This work is conducted in the context of future large-scale structure spectroscopic surveys like DESI-II, the next phase of the Dark Energy Spectroscopic Instrument… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08062v1-abstract-full').style.display = 'inline'; document.getElementById('2410.08062v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.08062v1-abstract-full" style="display: none;"> In this paper, we investigate the possibility of selecting high-redshift Lyman-Break Galaxies (LBG) using current and future broadband wide photometric surveys, such as UNIONS or the Vera C. Rubin LSST, using a Random Forest algorithm. This work is conducted in the context of future large-scale structure spectroscopic surveys like DESI-II, the next phase of the Dark Energy Spectroscopic Instrument (DESI), which will start around 2029. We use deep imaging data from HSC and CLAUDS on the COSMOS and XMM-LSS fields. To predict the selection performance of LBGs with image quality similar to UNIONS, we degrade the $u, g, r, i$ and $z$ bands to UNIONS depth. The Random Forest algorithm is trained with the $u,g,r,i$ and $z$ bands to classify LBGs in the $2.5 < z < 3.5$ range. We find that fixing a target density budget of $1,100$ deg$^{-2}$, the Random Forest approach gives a density of $z>2$ targets of $873$ deg$^{-2}$, and a density of $493$ deg$^{-2}$ of confirmed LBGs after spectroscopic confirmation with DESI. This UNIONS-like selection was tested in a dedicated spectroscopic observation campaign of 1,000 targets with DESI on the COSMOS field, providing a safe spectroscopic sample with a mean redshift of 3. This sample is used to derive forecasts for DESI-II, assuming a sky coverage of 5,000 deg$^2$. We predict uncertainties on Alcock-Paczynski parameters $伪_\perp$ and $伪_{\parallel}$ to be 0.7$\%$ and 1$\%$ for $2.6<z<3.2$, resulting in a 2$\%$ measurement of the dark energy fraction. Additionally, we estimate the uncertainty in local non-Gaussianity and predict $蟽_{f_{\rm NL}}\approx 7$, which is comparable to the current best precision achieved by Planck. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08062v1-abstract-full').style.display = 'none'; document.getElementById('2410.08062v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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, 28 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07601">arXiv:2410.07601</a> <span> [<a href="https://arxiv.org/pdf/2410.07601">pdf</a>, <a href="https://arxiv.org/format/2410.07601">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> DESI Emission Line Galaxies: Unveiling the Diversity of [OII] Profiles and its Links to Star Formation and Morphology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lan%2C+T">Ting-Wen Lan</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">J. Xavier Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Siudek%2C+M">Ma艂gorzata Siudek</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=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">A. Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">R. Miquel</a> , et al. (12 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="2410.07601v1-abstract-short" style="display: inline;"> We study the [OII] profiles of emission line galaxies (ELGs) from the Early Data Release of the Dark Energy Spectroscopic Instrument (DESI). To this end, we decompose and classify the shape of [OII] profiles with the first two eigenspectra derived from Principal Component Analysis. Our results show that DESI ELGs have diverse line profiles which can be categorized into three main types: (1) narrow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07601v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07601v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07601v1-abstract-full" style="display: none;"> We study the [OII] profiles of emission line galaxies (ELGs) from the Early Data Release of the Dark Energy Spectroscopic Instrument (DESI). To this end, we decompose and classify the shape of [OII] profiles with the first two eigenspectra derived from Principal Component Analysis. Our results show that DESI ELGs have diverse line profiles which can be categorized into three main types: (1) narrow lines with a median width of ~50 km/s, (2) broad lines with a median width of ~80 km/s, and (3) two-redshift systems with a median velocity separation of ~150 km/s, i.e., double-peak galaxies. To investigate the connections between the line profiles and galaxy properties, we utilize the information from the COSMOS dataset and compare the properties of ELGs, including star-formation rate (SFR) and galaxy morphology, with the average properties of reference star-forming galaxies with similar stellar mass, sizes, and redshifts. Our findings show that on average, DESI ELGs have higher SFR and more asymmetrical/disturbed morphology than the reference galaxies. Moreover, we uncover a relationship between the line profiles, the excess SFR and the excess asymmetry parameter, showing that DESI ELGs with broader [OII] line profiles have more disturbed morphology and higher SFR than the reference star-forming galaxies. Finally, we discuss possible physical mechanisms giving rise to the observed relationship and the implications of our findings on the galaxy clustering measurements, including the halo occupation distribution modeling of DESI ELGs and the observed excess velocity dispersion of the satellite ELGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07601v1-abstract-full').style.display = 'none'; document.getElementById('2410.07601v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">24 pages, 13 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.19066">arXiv:2409.19066</a> <span> [<a href="https://arxiv.org/pdf/2409.19066">pdf</a>, <a href="https://arxiv.org/format/2409.19066">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Value Added Catalog of physical properties of more than 1.3 million galaxies from the DESI Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Siudek%2C+M">M. Siudek</a>, <a href="/search/astro-ph?searchtype=author&query=Pucha%2C+R">R. Pucha</a>, <a href="/search/astro-ph?searchtype=author&query=Mezcua%2C+M">M. Mezcua</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</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=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.19066v1-abstract-short" style="display: inline;"> Aims. We present an extensive catalog of the physical properties of more than a million galaxies within the Dark Energy Spectroscopic Instrument (DESI), one of the largest spectroscopic surveys to date. Spanning over a full variety of target types, including emission line galaxies and luminous red galaxies as well as quasars, our survey encompasses an unprecedented range of spectroscopic redshifts… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19066v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19066v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19066v1-abstract-full" style="display: none;"> Aims. We present an extensive catalog of the physical properties of more than a million galaxies within the Dark Energy Spectroscopic Instrument (DESI), one of the largest spectroscopic surveys to date. Spanning over a full variety of target types, including emission line galaxies and luminous red galaxies as well as quasars, our survey encompasses an unprecedented range of spectroscopic redshifts, stretching from 0 to 6. Methods. The physical properties, such as stellar masses and star formation rates, are derived via the CIGALE spectral energy distribution (SED) fitting code accounting for the contribution coming from active galactic nuclei (AGN). Based on the modeling of the optical-mid-infrared (grz complemented by WISE photometry) SEDs, we study galaxy properties with respect to their location on the main sequence. Results. We revise the dependence of stellar mass estimates on model choices and availability of the WISE photometry. The WISE information is mandatory to minimize the misclassification of star-forming galaxies as AGN. The lack of WISE bands in SED fits leads to elevated AGN fractions for 68% of star-forming galaxies identified using emission line diagnostic diagram but does not significantly affect their stellar mass nor star formation estimates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19066v1-abstract-full').style.display = 'none'; document.getElementById('2409.19066v1-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">originally announced</span> September 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">resubmitted after addressing minor referee comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.05682">arXiv:2409.05682</a> <span> [<a href="https://arxiv.org/pdf/2409.05682">pdf</a>, <a href="https://arxiv.org/format/2409.05682">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"> ForestFlow: cosmological emulation of Lyman-$伪$ forest clustering from linear to nonlinear scales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/astro-ph?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Lokken%2C+M">M. Lokken</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</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=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">R. Miquel</a> , et al. (9 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="2409.05682v1-abstract-short" style="display: inline;"> On large scales, measurements of the Lyman-$伪$ forest offer insights into the expansion history of the Universe, while on small scales, these impose strict constraints on the growth history, the nature of dark matter, and the sum of neutrino masses. This work introduces ForestFlow, a cosmological emulator designed to bridge the gap between large- and small-scale Lyman-$伪$ forest analyses. Using co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05682v1-abstract-full').style.display = 'inline'; document.getElementById('2409.05682v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.05682v1-abstract-full" style="display: none;"> On large scales, measurements of the Lyman-$伪$ forest offer insights into the expansion history of the Universe, while on small scales, these impose strict constraints on the growth history, the nature of dark matter, and the sum of neutrino masses. This work introduces ForestFlow, a cosmological emulator designed to bridge the gap between large- and small-scale Lyman-$伪$ forest analyses. Using conditional normalizing flows, ForestFlow emulates the 2 Lyman-$伪$ linear biases ($b_未$ and $b_畏$) and 6 parameters describing small-scale deviations of the 3D flux power spectrum ($P_\mathrm{3D}$) from linear theory. These 8 parameters are modeled as a function of cosmology $\unicode{x2013}$ the small-scale amplitude and slope of the linear power spectrum $\unicode{x2013}$ and the physics of the intergalactic medium. Thus, in combination with a Boltzmann solver, ForestFlow can predict $P_\mathrm{3D}$ on arbitrarily large (linear) scales and the 1D flux power spectrum ($P_\mathrm{1D}$) $\unicode{x2013}$ the primary observable for small-scale analyses $\unicode{x2013}$ without the need for interpolation or extrapolation. Consequently, ForestFlow enables for the first time multiscale analyses. Trained on a suite of 30 fixed-and-paired cosmological hydrodynamical simulations spanning redshifts from $z=2$ to $4.5$, ForestFlow achieves $3$ and $1.5\%$ precision in describing $P_\mathrm{3D}$ and $P_\mathrm{1D}$ from linear scales to $k=5\,\mathrm{Mpc}^{-1}$ and $k_\parallel=4\,\mathrm{Mpc}^{-1}$, respectively. Thanks to its parameterization, the precision of the emulator is also similar for both ionization histories and two extensions to the $螞$CDM model $\unicode{x2013}$ massive neutrinos and curvature $\unicode{x2013}$ not included in the training set. ForestFlow will be crucial for the cosmological analysis of Lyman-$伪$ forest measurements from the DESI survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05682v1-abstract-full').style.display = 'none'; document.getElementById('2409.05682v1-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> 9 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 11 figures. Submitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.16042">arXiv:2408.16042</a> <span> [<a href="https://arxiv.org/pdf/2408.16042">pdf</a>, <a href="https://arxiv.org/format/2408.16042">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Constraints on the properties of $谓$MSM dark matter using the satellite galaxies of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Newton%2C+O">Oliver Newton</a>, <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+M+R">Mark R. Lovell</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+A">Adrian Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Helly%2C+J+C">John C. Helly</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+A+J">Andrew J. Benson</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="2408.16042v1-abstract-short" style="display: inline;"> Low-mass galaxies provide a powerful tool with which to investigate departures from the standard cosmological paradigm in models that suppress the abundance of small dark matter structures. One of the simplest metrics that can be used to compare different models is the abundance of satellite galaxies in the Milky Way. Viable dark matter models must produce enough substructure to host the observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16042v1-abstract-full').style.display = 'inline'; document.getElementById('2408.16042v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.16042v1-abstract-full" style="display: none;"> Low-mass galaxies provide a powerful tool with which to investigate departures from the standard cosmological paradigm in models that suppress the abundance of small dark matter structures. One of the simplest metrics that can be used to compare different models is the abundance of satellite galaxies in the Milky Way. Viable dark matter models must produce enough substructure to host the observed number of Galactic satellites. Here, we scrutinize the predictions of the neutrino Minimal Standard Model ($谓{\rm MSM}$), a well-motivated extension of the Standard Model of particle physics in which the production of sterile neutrino dark matter is resonantly enhanced by a lepton asymmetry in the primordial plasma. This process enables the model to evade current constraints associated with non-resonantly produced dark matter. Independently of assumptions about galaxy formation physics we rule out, with at least 95 per cent confidence, all parameterizations of the $谓{\rm MSM}$ with sterile neutrino rest mass, $M_{\rm s} \leq 1.4\, {\rm keV}$. Incorporating physically motivated prescriptions of baryonic processes and modelling the effects of reionization strengthen our constraints, and we exclude all $谓{\rm MSM}$ parameterizations with $M_{\rm s} \leq 4\, {\rm keV}$. Unlike other literature, our fiducial constraints do not rule out the putative 3.55 keV X-ray line, if it is indeed produced by the decay of a sterile neutrino; however, some of the most favoured parameter space is excluded. If the Milky Way satellite count is higher than we assume, or if the Milky Way halo is less massive than $M^{\rm MW}_{200} = 8 \times 10^{11}\, {\rm M_\odot}$, we rule out the $谓{\rm MSM}$ as the origin of the 3.55 keV excess. In contrast with other work, we find that the constraints from satellite counts are substantially weaker than those reported from X-ray non-detections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16042v1-abstract-full').style.display = 'none'; document.getElementById('2408.16042v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">14 pages, six figures, two appendices. A repository of reduced scripts and data will be made available at https://github.com/Musical-Neutron/nuMSM_constraints. Submitted, comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.12983">arXiv:2407.12983</a> <span> [<a href="https://arxiv.org/pdf/2407.12983">pdf</a>, <a href="https://arxiv.org/format/2407.12983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Lopsidedness in Early-Type Galaxies: the role of the $m=1$ multipole in Isophote Fitting and Strong Lens Modelling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amvrosiadis%2C+A">Aristeidis Amvrosiadis</a>, <a href="/search/astro-ph?searchtype=author&query=Nightingale%2C+J+W">James W. Nightingale</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+Q">Qiuhan He</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+A">Andrew Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+S+C">Samuel C. Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Massey%2C+R">Richard Massey</a>, <a href="/search/astro-ph?searchtype=author&query=Poci%2C+A">Adriano Poci</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.12983v1-abstract-short" style="display: inline;"> The surface brightness distribution of massive early-type galaxies (ETGs) often deviates from a perfectly elliptical shape. To capture these deviations in their isophotes during an ellipse fitting analysis, Fourier modes of order $m = 3, 4$ are often used. In such analyses the centre of each ellipse is treated as a free parameter, which may result in offsets from the centre of light, particularly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12983v1-abstract-full').style.display = 'inline'; document.getElementById('2407.12983v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.12983v1-abstract-full" style="display: none;"> The surface brightness distribution of massive early-type galaxies (ETGs) often deviates from a perfectly elliptical shape. To capture these deviations in their isophotes during an ellipse fitting analysis, Fourier modes of order $m = 3, 4$ are often used. In such analyses the centre of each ellipse is treated as a free parameter, which may result in offsets from the centre of light, particularly for ellipses in the outer regions. This complexity is not currently accounted for in the mass models used in either strong gravitational lensing or galactic dynamical studies. In this work, we adopt a different approach, using the $m=1$ Fourier mode to account for this complexity while keeping the centres of all perturbed ellipses fixed, showing that it fits the data equally well. We applied our method to the distribution of light emission to a sample of ETGs from the MASSIVE survey and found that the majority have low $m_1$ amplitudes, below 2 percent. Five out of the 30 galaxies we analysed have high $m_1$ amplitudes, ranging from 2 to 10 percent in the outer parts ($R \gtrsim 3$ kpc), all of which have a physically associated companion. Based on our findings, we advocate the use of the $m=1$ multipole in the mass models used in strong lensing and dynamical studies, particularly for galaxies with recent or ongoing interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12983v1-abstract-full').style.display = 'none'; document.getElementById('2407.12983v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 6 figures. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.11721">arXiv:2407.11721</a> <span> [<a href="https://arxiv.org/pdf/2407.11721">pdf</a>, <a href="https://arxiv.org/format/2407.11721">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Inferring the mass content of galaxy clusters with satellite kinematics and Jeans Anisotropic modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Wenting Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhaozhou Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Ling Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A">Alexander Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">Hongyu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xiaokai Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qingyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">Jiaxin Han</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.11721v1-abstract-short" style="display: inline;"> Satellite galaxies can be used to indicate the dynamical mass of galaxy groups and clusters. In this study, we apply the axis-symmetric Jeans Anisotropic Multi-Gaussian Expansion JAM modeling to satellite galaxies in 28 galaxy clusters selected from the TNG300-1 simulation with halo mass of $\log_{10}M_{200}/M_\odot>14.3$. If using true bound satellites as tracers, the best constrained total mass… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11721v1-abstract-full').style.display = 'inline'; document.getElementById('2407.11721v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.11721v1-abstract-full" style="display: none;"> Satellite galaxies can be used to indicate the dynamical mass of galaxy groups and clusters. In this study, we apply the axis-symmetric Jeans Anisotropic Multi-Gaussian Expansion JAM modeling to satellite galaxies in 28 galaxy clusters selected from the TNG300-1 simulation with halo mass of $\log_{10}M_{200}/M_\odot>14.3$. If using true bound satellites as tracers, the best constrained total mass within the half-mass radius of satellites, $M(<r_\mathrm{half})$, and the virial mass, $M_{200}$, have average biases of -0.01 and $0.03$~dex, with average scatters of 0.11~dex and 0.15~dex. If selecting companions in redshift space with line-of-sight depth of 2,000~km/s, the biases are -0.06 and $0.01$~dex, while the scatters are 0.12 and 0.18~dex for $M(<r_\mathrm{half})$ and $M_{200}$. By comparing the best-fitting and actual density profiles, we find $\sim$29% of best-fitting density profiles show very good agreement with the truth, $\sim$32% display over or under estimates at most of the radial range with biased $M(<r_\mathrm{half})$, and 39% show under/over estimates in central regions and over/under estimates in the outskirts, with good constraints on $M(<r_\mathrm{half})$, yet most of the best constraints are still consistent with the true profiles within 1-$蟽$ statistical uncertainties for the three circumstances. Using a mock DESI Bright Galaxy Survey catalog with the effect of fiber incompleteness, we find DESI fiber assignments and the choice of flux limits barely modify the velocity dispersion profiles and are thus unlikely to affect the dynamical modeling outcomes. Our results show that with current and future deep spectroscopic surveys, JAM can be a powerful tool to constrain the underlying density profiles of individual massive galaxy clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11721v1-abstract-full').style.display = 'none'; document.getElementById('2407.11721v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.06280">arXiv:2407.06280</a> <span> [<a href="https://arxiv.org/pdf/2407.06280">pdf</a>, <a href="https://arxiv.org/format/2407.06280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> DESI Early Data Release Milky Way Survey Value-Added Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Allende-Prieto%2C+C">C. Allende-Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+A+P">A. P. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T+S">T. S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L+B+e">L. Beraldo e Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+B">B. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Carrillo%2C+A">A. Carrillo</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Manser%2C+C+J">C. J. Manser</a>, <a href="/search/astro-ph?searchtype=author&query=Nikakhtar%2C+F">F. Nikakhtar</a>, <a href="/search/astro-ph?searchtype=author&query=Riley%2C+A+H">A. H. Riley</a>, <a href="/search/astro-ph?searchtype=author&query=Rockosi%2C+C">C. Rockosi</a>, <a href="/search/astro-ph?searchtype=author&query=Valluri%2C+M">M. Valluri</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=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">J. Guy</a> , et al. (18 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="2407.06280v2-abstract-short" style="display: inline;"> We present the stellar value-added catalogue based on the Dark Energy Spectroscopic Instrument (DESI) Early Data Release. The catalogue contains radial velocity and stellar parameter measurements for $\simeq$ 400,000 unique stars observed during commissioning and survey validation by DESI. These observations were made under conditions similar to the Milky Way Survey (MWS) currently carried out by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06280v2-abstract-full').style.display = 'inline'; document.getElementById('2407.06280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06280v2-abstract-full" style="display: none;"> We present the stellar value-added catalogue based on the Dark Energy Spectroscopic Instrument (DESI) Early Data Release. The catalogue contains radial velocity and stellar parameter measurements for $\simeq$ 400,000 unique stars observed during commissioning and survey validation by DESI. These observations were made under conditions similar to the Milky Way Survey (MWS) currently carried out by DESI but also include multiple specially targeted fields, such as those containing well-studied dwarf galaxies and stellar streams. The majority of observed stars have $16<r<20$ with a median signal-to-noise ratio in the spectra of $\sim$ 20. In the paper, we describe the structure of the catalogue, give an overview of different target classes observed, as well as provide recipes for selecting clean stellar samples. We validate the catalogue using external high-resolution measurements and show that radial velocities, surface gravities, and iron abundances determined by DESI are accurate to 1 km/s, $0.3$ dex and $\sim$ 0.15 dex respectively. We also demonstrate possible uses of the catalogue for chemo-dynamical studies of the Milky Way stellar halo and Draco dwarf spheroidal. The value-added catalogue described in this paper is the very first DESI MWS catalogue. The next DESI data release, expected in less than a year, will add the data from the first year of DESI survey operations and will contain approximately 4 million stars, along with significant processing improvements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06280v2-abstract-full').style.display = 'none'; document.getElementById('2407.06280v2-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 8 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to MNRAS; Value added catalogue is available at https://data.desi.lbl.gov/public/edr/vac/edr/mws/fuji/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.06085">arXiv:2406.06085</a> <span> [<a href="https://arxiv.org/pdf/2406.06085">pdf</a>, <a href="https://arxiv.org/format/2406.06085">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"> Fiducial-Cosmology-dependent systematics for the DESI 2024 BAO Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Fern%C3%A1ndez%2C+A">A. P茅rez-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Medina-Varela%2C+L">L. Medina-Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+R">R. Ruggeri</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Maga%C3%B1a%2C+M">M. Vargas-Maga帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.06085v1-abstract-short" style="display: inline;"> When measuring the Baryon Acoustic Oscillations (BAO) scale from galaxy surveys, one typically assumes a fiducial cosmology when converting redshift measurements into comoving distances and also when defining input parameters for the reconstruction algorithm. A parameterised template for the model to be fitted is also created based on a (possibly different) fiducial cosmology. This model reliance… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06085v1-abstract-full').style.display = 'inline'; document.getElementById('2406.06085v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06085v1-abstract-full" style="display: none;"> When measuring the Baryon Acoustic Oscillations (BAO) scale from galaxy surveys, one typically assumes a fiducial cosmology when converting redshift measurements into comoving distances and also when defining input parameters for the reconstruction algorithm. A parameterised template for the model to be fitted is also created based on a (possibly different) fiducial cosmology. This model reliance can be considered a form of data compression, and the data is then analysed allowing that the true answer is different from the fiducial cosmology assumed. In this study, we evaluate the impact of the fiducial cosmology assumed in the BAO analysis of the Dark Energy Spectroscopic Instrument (DESI) survey Data Release 1 (DR1) on the final measurements in DESI 2024 III. We utilise a suite of mock galaxy catalogues with survey realism that mirrors the DESI DR1 tracers: the bright galaxy sample (BGS), the luminous red galaxies (LRG), the emission line galaxies (ELG) and the quasars (QSO), spanning a redshift range from 0.1 to 2.1. We compare the four secondary AbacusSummit cosmologies against DESI's fiducial cosmology (Planck 2018). The secondary cosmologies explored include a lower cold dark matter density, a thawing dark energy universe, a higher number of effective species, and a lower amplitude of matter clustering. The mocks are processed through the BAO pipeline by consistently iterating the grid, template, and reconstruction reference cosmologies. We determine a conservative systematic contribution to the error of $0.1\%$ for both the isotropic and anisotropic dilation parameters $伪_{\rm iso}$ and $伪_{\rm AP}$. We then directly test the impact of the fiducial cosmology on DESI DR1 data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06085v1-abstract-full').style.display = 'none'; document.getElementById('2406.06085v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 III: Baryon Acoustic Oscillations from Galaxies and Quasars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.04804">arXiv:2406.04804</a> <span> [<a href="https://arxiv.org/pdf/2406.04804">pdf</a>, <a href="https://arxiv.org/format/2406.04804">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"> Mitigation of DESI fiber assignment incompleteness effect on two-point clustering with small angular scale truncated estimators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pinon%2C+M">M. Pinon</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+P">P. McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Ruhlmann-Kleider%2C+V">V. Ruhlmann-Kleider</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">M. White</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</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=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cahn%2C+R+N">R. N. Cahn</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">T. Kisner</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.04804v2-abstract-short" style="display: inline;"> We present a method to mitigate the effects of fiber assignment incompleteness in two-point power spectrum and correlation function measurements from galaxy spectroscopic surveys, by truncating small angular scales from estimators. We derive the corresponding modified correlation function and power spectrum windows to account for the small angular scale truncation in the theory prediction. We vali… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04804v2-abstract-full').style.display = 'inline'; document.getElementById('2406.04804v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.04804v2-abstract-full" style="display: none;"> We present a method to mitigate the effects of fiber assignment incompleteness in two-point power spectrum and correlation function measurements from galaxy spectroscopic surveys, by truncating small angular scales from estimators. We derive the corresponding modified correlation function and power spectrum windows to account for the small angular scale truncation in the theory prediction. We validate this approach on simulations reproducing the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1) with and without fiber assignment. We show that we recover unbiased cosmological constraints using small angular scale truncated estimators from simulations with fiber assignment incompleteness, with respect to standard estimators from complete simulations. Additionally, we present an approach to remove the sensitivity of the fits to high $k$ modes in the theoretical power spectrum, by applying a transformation to the data vector and window matrix. We find that our method efficiently mitigates the effect of fiber assignment incompleteness in two-point correlation function and power spectrum measurements, at low computational cost and with little statistical loss. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04804v2-abstract-full').style.display = 'none'; document.getElementById('2406.04804v2-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 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">36 pages, 23 figures, typos corrected, clarifications added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.02672">arXiv:2406.02672</a> <span> [<a href="https://arxiv.org/pdf/2406.02672">pdf</a>, <a href="https://arxiv.org/format/2406.02672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> A comparison of pre-existing $螞$CDM predictions with the abundance of {\it JWST} galaxies at high redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shengdong Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+S">Sownak Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Lacey%2C+C+G">Cedric G. Lacey</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Baugh%2C+C+M">Carlton M. Baugh</a>, <a href="/search/astro-ph?searchtype=author&query=Helly%2C+J+C">John C. Helly</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="2406.02672v2-abstract-short" style="display: inline;"> Observations with the {\it James Webb Space Telescope} have revealed a high abundance of bright galaxies at redshift, $z\gtrsim 12$, which has been widely interpreted as conflicting with the $螞$CDM model. In Cowley et al. (2018) predictions were made -- prior to the {\it JWST} observations -- for the expected abundance of these galaxies using the Durham semi-analytic galaxy formation model, {\sc g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02672v2-abstract-full').style.display = 'inline'; document.getElementById('2406.02672v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.02672v2-abstract-full" style="display: none;"> Observations with the {\it James Webb Space Telescope} have revealed a high abundance of bright galaxies at redshift, $z\gtrsim 12$, which has been widely interpreted as conflicting with the $螞$CDM model. In Cowley et al. (2018) predictions were made -- prior to the {\it JWST} observations -- for the expected abundance of these galaxies using the Durham semi-analytic galaxy formation model, {\sc galform}, which is known to produce a realistic population of galaxies at lower redshifts including the present day. Key to this model is the assumption of a ``top-heavy" initial mass function of stars formed in bursts (required to explain the number counts and redshift distribution of sub-millimetre galaxies). Here, we compare the rest-frame ultraviolet luminosity functions derived from {\it JWST} observations with those predicted by the Cowley et al. model up to $z=14$ and make further predictions for $z=16$. We find that below $z\sim 10$, the Cowley et al. predictions agree very well with observations, while agreement at $z\gtrsim12$ requires extending the model to take into account the timescale for the growth of obscuring dust grains at these very early times and its dependence on gas metallicity. We trace the evolution of these galaxies from $z=14$ to $z=0$ and find that their descendants typically reside in halos with a median mass $2.5\times 10^{13}\,h^{-1}\,\mathrm{M_{\odot}}$. The stellar masses of the descendants range from $3.2\times 10^{6}\,h^{-1}\,\mathrm{M_{\odot}}$ to $3.2\times 10^{11}\,h^{-1}\,\mathrm{M_{\odot}}$. Although these galaxies were all central galaxies at $z=14$, over half of their descendants end up as satellites in massive halos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02672v2-abstract-full').style.display = 'none'; document.getElementById('2406.02672v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">16 pages, 11 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.00191">arXiv:2406.00191</a> <span> [<a href="https://arxiv.org/pdf/2406.00191">pdf</a>, <a href="https://arxiv.org/format/2406.00191">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"> Blinding scheme for the scale-dependence bias signature of local primordial non-Gaussianity for DESI 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Y%C3%A8che%2C+C">C. Y猫che</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=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">A. Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">R. Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Niz%2C+G">G. Niz</a>, <a href="/search/astro-ph?searchtype=author&query=Palanque-Delabrouille%2C+N">N. Palanque-Delabrouille</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+W+J">W. J. Percival</a>, <a href="/search/astro-ph?searchtype=author&query=Prada%2C+F">F. Prada</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.00191v1-abstract-short" style="display: inline;"> The next generation of spectroscopic surveys is expected to achieve an unprecedented level of accuracy in the measurement of cosmological parameters. To avoid confirmation bias and thereby improve the reliability of these results, blinding procedures become a standard practice in the cosmological analyses of such surveys. Blinding is especially crucial when the impact of observational systematics… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00191v1-abstract-full').style.display = 'inline'; document.getElementById('2406.00191v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.00191v1-abstract-full" style="display: none;"> The next generation of spectroscopic surveys is expected to achieve an unprecedented level of accuracy in the measurement of cosmological parameters. To avoid confirmation bias and thereby improve the reliability of these results, blinding procedures become a standard practice in the cosmological analyses of such surveys. Blinding is especially crucial when the impact of observational systematics is important relative to the cosmological signal, and a detection of that signal would have significant implications. This is the case for local primordial non-gaussianity, as probed by the scale-dependent bias of the galaxy power spectrum at large scales that are heavily sensitive to the dependence of the target selection on the imaging quality, known as imaging systematics. We propose a blinding method for the scale-dependent bias signature of local primordial non-gaussianity at the density field level which consists in generating a set of weights for the data that replicate the scale-dependent bias. The applied blinding is predictable, and can be straightforwardly combined with other catalog-level blinding procedures that have been designed for the baryon acoustic oscillation and redshift space distortion signals. The procedure is validated through simulations that replicate data from the first year of observation of the Dark Energy Spectroscopic Instrument, but may find applications to other upcoming spectroscopic surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00191v1-abstract-full').style.display = 'none'; document.getElementById('2406.00191v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.20125">arXiv:2405.20125</a> <span> [<a href="https://arxiv.org/pdf/2405.20125">pdf</a>, <a href="https://arxiv.org/format/2405.20125">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"> Haloes, other dark matter candidates and astrophysical implications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cole%2C+P+S">Philippa S. Cole</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="2405.20125v1-abstract-short" style="display: inline;"> It is possible that a multi-component dark matter model is required if primordial black holes only contribute to a fraction of the energy density in dark matter. This is increasingly more likely with respect to the case of $f_{\rm PBH} = 1$, since there is only one remaining window, on asteroid-mass scales, where primordial black holes can make up all of the dark matter. A mixed dark matter model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20125v1-abstract-full').style.display = 'inline'; document.getElementById('2405.20125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.20125v1-abstract-full" style="display: none;"> It is possible that a multi-component dark matter model is required if primordial black holes only contribute to a fraction of the energy density in dark matter. This is increasingly more likely with respect to the case of $f_{\rm PBH} = 1$, since there is only one remaining window, on asteroid-mass scales, where primordial black holes can make up all of the dark matter. A mixed dark matter model can lead to interesting observables that come about due to the interactions between primordial black holes and the second dark matter component. This can provide unique signatures of the presence of primordial black holes and increase the prospects of detection or improvement of constraints in the mass ranges where $f_{\rm PBH} < 1$, whilst simultaneously exploring the remaining open parameter space for other dark matter candidates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20125v1-abstract-full').style.display = 'none'; document.getElementById('2405.20125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 4 figures. To appear (with updates) in the book "Primordial Black Holes", ed. Chris Byrnes, Gabriele Franciolini, Tomohiro Harada, Paolo Pani, Misao Sasaki; Springer (2024). Comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.19288">arXiv:2405.19288</a> <span> [<a href="https://arxiv.org/pdf/2405.19288">pdf</a>, <a href="https://arxiv.org/format/2405.19288">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 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/ad60c2">10.3847/1538-3881/ad60c2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Archetype-Based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">Abhijeet Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</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=Bolton%2C+A">A. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J">J. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.19288v2-abstract-short" style="display: inline;"> We present a computationally efficient galaxy archetype-based redshift estimation and spectral classification method for the Dark Energy Survey Instrument (DESI) survey. The DESI survey currently relies on a redshift fitter and spectral classifier using a linear combination of PCA-derived templates, which is very efficient in processing large volumes of DESI spectra within a short time frame. Howe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19288v2-abstract-full').style.display = 'inline'; document.getElementById('2405.19288v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19288v2-abstract-full" style="display: none;"> We present a computationally efficient galaxy archetype-based redshift estimation and spectral classification method for the Dark Energy Survey Instrument (DESI) survey. The DESI survey currently relies on a redshift fitter and spectral classifier using a linear combination of PCA-derived templates, which is very efficient in processing large volumes of DESI spectra within a short time frame. However, this method occasionally yields unphysical model fits for galaxies and fails to adequately absorb calibration errors that may still be occasionally visible in the reduced spectra. Our proposed approach improves upon this existing method by refitting the spectra with carefully generated physical galaxy archetypes combined with additional terms designed to absorb data reduction defects and provide more physical models to the DESI spectra. We test our method on an extensive dataset derived from the survey validation (SV) and Year 1 (Y1) data of DESI. Our findings indicate that the new method delivers marginally better redshift success for SV tiles while reducing catastrophic redshift failure by $10-30\%$. At the same time, results from millions of targets from the main survey show that our model has relatively higher redshift success and purity rates ($0.5-0.8\%$ higher) for galaxy targets while having similar success for QSOs. These improvements also demonstrate that the main DESI redshift pipeline is generally robust. Additionally, it reduces the false positive redshift estimation by $5-40\%$ for sky fibers. We also discuss the generic nature of our method and how it can be extended to other large spectroscopic surveys, along with possible future improvements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19288v2-abstract-full').style.display = 'none'; document.getElementById('2405.19288v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in AJ, 33 pages, 15 figures, 7 Tables, 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/2405.16593">arXiv:2405.16593</a> <span> [<a href="https://arxiv.org/pdf/2405.16593">pdf</a>, <a href="https://arxiv.org/format/2405.16593">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Construction of Large-scale Structure Catalogs for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</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=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Ereza%2C+J">J. Ereza</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.16593v2-abstract-short" style="display: inline;"> We present the technical details on how large-scale structure (LSS) catalogs are constructed from redshifts measured from spectra observed by the Dark Energy Spectroscopic Instrument (DESI). The LSS catalogs provide the information needed to determine the relative number density of DESI tracers as a function of redshift and celestial coordinates and, e.g., determine clustering statistics. We produ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16593v2-abstract-full').style.display = 'inline'; document.getElementById('2405.16593v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.16593v2-abstract-full" style="display: none;"> We present the technical details on how large-scale structure (LSS) catalogs are constructed from redshifts measured from spectra observed by the Dark Energy Spectroscopic Instrument (DESI). The LSS catalogs provide the information needed to determine the relative number density of DESI tracers as a function of redshift and celestial coordinates and, e.g., determine clustering statistics. We produce catalogs that are weighted subsamples of the observed data, each matched to a weighted `random' catalog that forms an unclustered sampling of the probability density that DESI could have observed those data at each location. Precise knowledge of the DESI observing history and associated hardware performance allows for a determination of the DESI footprint and the number of times DESI has covered it at sub-arcsecond level precision. This enables the completeness of any DESI sample to be modeled at this same resolution. The pipeline developed to create LSS catalogs has been designed to easily allow robustness tests and enable future improvements. We describe how it allows ongoing work improving the match between galaxy and random catalogs, such as including further information when assigning redshifts to randoms, accounting for fluctuations in target density, accounting for variation in the redshift success rate, and accommodating blinding schemes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16593v2-abstract-full').style.display = 'none'; document.getElementById('2405.16593v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted (by JCAP) version of supporting publication of DESI 2024II: Sample definitions, characteristics, and two-point clustering statistics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.16299">arXiv:2405.16299</a> <span> [<a href="https://arxiv.org/pdf/2405.16299">pdf</a>, <a href="https://arxiv.org/format/2405.16299">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"> Forward modeling fluctuations in the DESI LRGs target sample using image simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kong%2C+H">Hui Kong</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">Ashley J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">Dustin Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">Anna Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">Arnaud de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Rezaie%2C+M">Mehdi Rezaie</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Schlafly%2C+E">Edward Schlafly</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Rosado-Marin%2C+A">Alberto Rosado-Marin</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">Edmond Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gaztanaga%2C+E">Enrique Gaztanaga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.16299v2-abstract-short" style="display: inline;"> We use the forward modeling pipeline, Obiwan, to study the imaging systematics of the Luminous Red Galaxies (LRGs) targeted by the Dark Energy Spectroscopic Instrument (DESI). We update the Obiwan pipeline, which had previously been developed to simulate the optical images used to target DESI data, to further simulate WISE images in the infrared. This addition makes it possible to simulate the DES… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16299v2-abstract-full').style.display = 'inline'; document.getElementById('2405.16299v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.16299v2-abstract-full" style="display: none;"> We use the forward modeling pipeline, Obiwan, to study the imaging systematics of the Luminous Red Galaxies (LRGs) targeted by the Dark Energy Spectroscopic Instrument (DESI). We update the Obiwan pipeline, which had previously been developed to simulate the optical images used to target DESI data, to further simulate WISE images in the infrared. This addition makes it possible to simulate the DESI LRGs sample, which utilizes WISE data in the target selection. Deep DESI imaging data combined with a method to account for biases in their shapes is used to define a truth sample of potential LRG targets. We simulate a total of 15 million galaxies to obtain a simulated LRG sample (Obiwan LRGs) that predicts the variations in target density due to imaging properties. We find that the simulations predict the trends with depth observed in the data, including how they depend on the intrinsic brightness of the galaxies. We observe that faint LRGs are the main contributing power of the imaging systematics trend induced by depth. We also find significant trends in the data against Galactic extinction that are not predicted by Obiwan. These trends depend strongly on the particular map of Galactic extinction chosen to test against, implying Large-Scale Structure systematic contamination (e.g. Cosmic-Infrared Background) in the Galactic extinction maps is a likely root cause. We additionally observe that the DESI LRGs sample exhibits a complex dependency on a combination of seeing, depth, and intrinsic galaxy brightness, which is not replicated by Obiwan, suggesting discrepancies between the current simulation settings and the actual observations. The detailed findings we present should be used to guide any observational systematics mitigation treatment for the clustering of the DESI LRG sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16299v2-abstract-full').style.display = 'none'; document.getElementById('2405.16299v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">46 pages, 26 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/2404.07312">arXiv:2404.07312</a> <span> [<a href="https://arxiv.org/pdf/2404.07312">pdf</a>, <a href="https://arxiv.org/format/2404.07312">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"> An analysis of parameter compression and full-modeling techniques with Velocileptors for DESI 2024 and beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maus%2C+M">M. Maus</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">M. White</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=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Findlay%2C+N">N. Findlay</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">C. Hahn</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a> , et al. (30 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="2404.07312v4-abstract-short" style="display: inline;"> In anticipation of forthcoming data releases of current and future spectroscopic surveys, we present the validation tests and analysis of systematic effects within \texttt{velocileptors} modeling pipeline when fitting mock data from the \texttt{AbacusSummit} N-body simulations. We compare the constraints obtained from parameter compression methods to the direct fitting (Full-Modeling) approaches o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07312v4-abstract-full').style.display = 'inline'; document.getElementById('2404.07312v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07312v4-abstract-full" style="display: none;"> In anticipation of forthcoming data releases of current and future spectroscopic surveys, we present the validation tests and analysis of systematic effects within \texttt{velocileptors} modeling pipeline when fitting mock data from the \texttt{AbacusSummit} N-body simulations. We compare the constraints obtained from parameter compression methods to the direct fitting (Full-Modeling) approaches of modeling the galaxy power spectra, and show that the ShapeFit extension to the traditional template method is consistent with the Full-Modeling method within the standard $螞$CDM parameter space. We show the dependence on scale cuts when fitting the different redshift bins using the ShapeFit and Full-Modeling methods. We test the ability to jointly fit data from multiple redshift bins as well as joint analysis of the pre-reconstruction power spectrum with the post-reconstruction BAO correlation function signal. We further demonstrate the behavior of the model when opening up the parameter space beyond $螞$CDM and also when combining likelihoods with external datasets, namely the Planck CMB priors. Finally, we describe different parametrization options for the galaxy bias, counterterm, and stochastic parameters, and employ the halo model in order to physically motivate suitable priors that are necessary to ensure the stability of the perturbation theory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07312v4-abstract-full').style.display = 'none'; document.getElementById('2404.07312v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">56 pages, 23 figures. Supporting publication of DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.07282">arXiv:2404.07282</a> <span> [<a href="https://arxiv.org/pdf/2404.07282">pdf</a>, <a href="https://arxiv.org/format/2404.07282">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"> Validating the Galaxy and Quasar Catalog-Level Blinding Scheme for the DESI 2024 analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+J">J. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">C. Hahn</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.07282v2-abstract-short" style="display: inline;"> In the era of precision cosmology, ensuring the integrity of data analysis through blinding techniques is paramount -- a challenge particularly relevant for the Dark Energy Spectroscopic Instrument (DESI). DESI represents a monumental effort to map the cosmic web, with the goal to measure the redshifts of tens of millions of galaxies and quasars. Given the data volume and the impact of the finding… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07282v2-abstract-full').style.display = 'inline'; document.getElementById('2404.07282v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07282v2-abstract-full" style="display: none;"> In the era of precision cosmology, ensuring the integrity of data analysis through blinding techniques is paramount -- a challenge particularly relevant for the Dark Energy Spectroscopic Instrument (DESI). DESI represents a monumental effort to map the cosmic web, with the goal to measure the redshifts of tens of millions of galaxies and quasars. Given the data volume and the impact of the findings, the potential for confirmation bias poses a significant challenge. To address this, we implement and validate a comprehensive blind analysis strategy for DESI Data Release 1 (DR1), tailored to the specific observables DESI is most sensitive to: Baryonic Acoustic Oscillations (BAO), Redshift-Space Distortion (RSD) and primordial non-Gaussianities (PNG). We carry out the blinding at the catalog level, implementing shifts in the redshifts of the observed galaxies to blind for BAO and RSD signals and weights to blind for PNG through a scale-dependent bias. We validate the blinding technique on mocks, as well as on data by applying a second blinding layer to perform a battery of sanity checks. We find that the blinding strategy alters the data vector in a controlled way such that the BAO and RSD analysis choices do not need any modification before and after unblinding. The successful validation of the blinding strategy paves the way for the unblinded DESI DR1 analysis, alongside future blind analyses with DESI and other surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07282v2-abstract-full').style.display = 'none'; document.getElementById('2404.07282v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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 II: Sample definitions, characteristics, and two-point clustering statistics", "DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars", and "DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars". (v2 - update DESI references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.07272">arXiv:2404.07272</a> <span> [<a href="https://arxiv.org/pdf/2404.07272">pdf</a>, <a href="https://arxiv.org/format/2404.07272">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"> A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maus%2C+M">M. Maus</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+Y">Y. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega%2C+H+E">H. E. Noriega</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez-Solano%2C+S">S. Ramirez-Solano</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Fromenteau%2C+S">S. Fromenteau</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Maga%C3%B1a%2C+M">M. Vargas-Maga帽a</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">M. White</a>, <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">P. Zarrouk</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=Icaza-Lizaola%2C+M">M. Icaza-Lizaola</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a> , et al. (32 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="2404.07272v4-abstract-short" style="display: inline;"> In preparation for the next generation of galaxy redshift surveys, and in particular the year-one data release from the Dark Energy Spectroscopic Instrument (DESI), we investigate the consistency of a variety of effective field theory models that describe the galaxy-galaxy power spectra in redshift space into the quasi-linear regime using 1-loop perturbation theory. These models are employed in th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07272v4-abstract-full').style.display = 'inline'; document.getElementById('2404.07272v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07272v4-abstract-full" style="display: none;"> In preparation for the next generation of galaxy redshift surveys, and in particular the year-one data release from the Dark Energy Spectroscopic Instrument (DESI), we investigate the consistency of a variety of effective field theory models that describe the galaxy-galaxy power spectra in redshift space into the quasi-linear regime using 1-loop perturbation theory. These models are employed in the pipelines \texttt{velocileptors}, \texttt{PyBird}, and \texttt{Folps$谓$}. While these models have been validated independently, a detailed comparison with consistent choices has not been attempted. After briefly discussing the theoretical differences between the models we describe how to provide a more apples-to-apples comparison between them. We present the results of fitting mock spectra from the \texttt{AbacusSummit} suite of N-body simulations provided in three redshift bins to mimic the types of dark time tracers targeted by the DESI survey. We show that the theories behave similarly and give consistent constraints in both the forward-modeling and ShapeFit compressed fitting approaches. We additionally generate (noiseless) synthetic data from each pipeline to be fit by the others, varying the scale cuts in order to show that the models agree within the range of scales for which we expect 1-loop perturbation theory to be applicable. This work lays the foundation of Full-Shape analysis with DESI Y1 galaxy samples where in the tests we performed, we found no systematic error associated with the modeling of the galaxy redshift space power spectrum for this volume. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07272v4-abstract-full').style.display = 'none'; document.getElementById('2404.07272v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">33 pages, 12 figures. Supporting publication of DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.07269">arXiv:2404.07269</a> <span> [<a href="https://arxiv.org/pdf/2404.07269">pdf</a>, <a href="https://arxiv.org/format/2404.07269">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"> Comparing Compressed and Full-modeling Analyses with FOLPS: Implications for DESI 2024 and beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Noriega%2C+H+E">H. E. Noriega</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez-Solano%2C+S">S. Ramirez-Solano</a>, <a href="/search/astro-ph?searchtype=author&query=Fromenteau%2C+S">S. Fromenteau</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Maga%C3%B1a%2C+M">M. Vargas-Maga帽a</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cervantes-Cota%2C+J+L">J. L. Cervantes-Cota</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Findlay%2C+N">N. Findlay</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Hou%2C+J">J. Hou</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="2404.07269v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) will provide unprecedented information about the large-scale structure of our Universe. In this work, we study the robustness of the theoretical modelling of the power spectrum of FOLPS, a novel effective field theory-based package for evaluating the redshift space power spectrum in the presence of massive neutrinos. We perform this validation by fit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07269v3-abstract-full').style.display = 'inline'; document.getElementById('2404.07269v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07269v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) will provide unprecedented information about the large-scale structure of our Universe. In this work, we study the robustness of the theoretical modelling of the power spectrum of FOLPS, a novel effective field theory-based package for evaluating the redshift space power spectrum in the presence of massive neutrinos. We perform this validation by fitting the AbacusSummit high-accuracy $N$-body simulations for Luminous Red Galaxies, Emission Line Galaxies and Quasar tracers, calibrated to describe DESI observations. We quantify the potential systematic error budget of FOLPS, finding that the modelling errors are fully sub-dominant for the DESI statistical precision within the studied range of scales. Additionally, we study two complementary approaches to fit and analyse the power spectrum data, one based on direct Full-Modelling fits and the other on the ShapeFit compression variables, both resulting in very good agreement in precision and accuracy. In each of these approaches, we study a set of potential systematic errors induced by several assumptions, such as the choice of template cosmology, the effect of prior choice in the nuisance parameters of the model, or the range of scales used in the analysis. Furthermore, we show how opening up the parameter space beyond the vanilla $螞$CDM model affects the DESI observables. These studies include the addition of massive neutrinos, spatial curvature, and dark energy equation of state. We also examine how relaxing the usual Cosmic Microwave Background and Big Bang Nucleosynthesis priors on the primordial spectral index and the baryonic matter abundance, respectively, impacts the inference on the rest of the parameters of interest. This paper pathways towards performing a robust and reliable analysis of the shape of the power spectrum of DESI galaxy and quasar clustering using FOLPS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07269v3-abstract-full').style.display = 'none'; document.getElementById('2404.07269v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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 VII: Cosmological constraints from full-shape analyses of the two-point clustering statistics measurements, in preparation (2024)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.07268">arXiv:2404.07268</a> <span> [<a href="https://arxiv.org/pdf/2404.07268">pdf</a>, <a href="https://arxiv.org/format/2404.07268">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"> Full Modeling and Parameter Compression Methods in configuration space for DESI 2024 and beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ramirez-Solano%2C+S">S. Ramirez-Solano</a>, <a href="/search/astro-ph?searchtype=author&query=Icaza-Lizaola%2C+M">M. Icaza-Lizaola</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega%2C+H+E">H. E. Noriega</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Maga%C3%B1a%2C+M">M. Vargas-Maga帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Fromenteau%2C+S">S. Fromenteau</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez-Martinez%2C+F">F. Rodriguez-Martinez</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a> , et al. (27 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="2404.07268v2-abstract-short" style="display: inline;"> In the contemporary era of high-precision spectroscopic surveys, led by projects like DESI, there is an increasing demand for optimizing the extraction of cosmological information from clustering data. This work conducts a thorough comparison of various methodologies for modeling the full shape of the two-point statistics in configuration space. We investigate the performance of both direct fits (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07268v2-abstract-full').style.display = 'inline'; document.getElementById('2404.07268v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07268v2-abstract-full" style="display: none;"> In the contemporary era of high-precision spectroscopic surveys, led by projects like DESI, there is an increasing demand for optimizing the extraction of cosmological information from clustering data. This work conducts a thorough comparison of various methodologies for modeling the full shape of the two-point statistics in configuration space. We investigate the performance of both direct fits (Full-Modeling) and the parameter compression approaches (ShapeFit and Standard). We utilize the ABACUS-SUMMIT simulations, tailored to exceed DESI's precision requirements. Particularly, we fit the two-point statistics of three distinct tracers (LRG, ELG, and QSO), by employing a Gaussian Streaming Model in tandem with Convolution Lagrangian Perturbation Theory and Effective Field Theory. We explore methodological setup variations, including the range of scales, the set of galaxy bias parameters, the inclusion of the hexadecapole, as well as model extensions encompassing varying $n_s$ and allowing for $w_0w_a$CDM dark energy model. Throughout these varied explorations, while precision levels fluctuate and certain configurations exhibit tighter parameter constraints, our pipeline consistently recovers the parameter values of the mocks within $1蟽$ in all cases for a 1-year DESI volume. Additionally, we compare the performance of configuration space analysis with its Fourier space counterpart using three models: PyBird, FOLPS and velocileptors, presented in companion papers. We find good agreement with the results from all these models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07268v2-abstract-full').style.display = 'none'; document.getElementById('2404.07268v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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 KP5</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03621">arXiv:2404.03621</a> <span> [<a href="https://arxiv.org/pdf/2404.03621">pdf</a>, <a href="https://arxiv.org/format/2404.03621">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Identifying Quasars from the DESI Bright Galaxy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Canning%2C+R">R. Canning</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=Pucha%2C+R">R. Pucha</a>, <a href="/search/astro-ph?searchtype=author&query=Fawcett%2C+V+A">V. A. Fawcett</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+A+D">A. D. Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">J. Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiz-Macias%2C+O">O. Ruiz-Macias</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Z. Pan</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=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</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="2404.03621v1-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) cosmology survey includes a Bright Galaxy Survey (BGS) which will yield spectra for over ten million bright galaxies (r<20.2 AB mag). The resulting sample will be valuable for both cosmological and astrophysical studies. However, the star/galaxy separation criterion implemented in the nominal BGS target selection algorithm excludes quasar host galaxi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03621v1-abstract-full').style.display = 'inline'; document.getElementById('2404.03621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03621v1-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) cosmology survey includes a Bright Galaxy Survey (BGS) which will yield spectra for over ten million bright galaxies (r<20.2 AB mag). The resulting sample will be valuable for both cosmological and astrophysical studies. However, the star/galaxy separation criterion implemented in the nominal BGS target selection algorithm excludes quasar host galaxies in addition to bona fide stars. While this excluded population is comparatively rare (~3-4 per square degrees), it may hold interesting clues regarding galaxy and quasar physics. Therefore, we present a target selection strategy that was implemented to recover these missing active galactic nuclei (AGN) from the BGS sample. The design of the selection criteria was both motivated and confirmed using spectroscopy. The resulting BGS-AGN sample is uniformly distributed over the entire DESI footprint. According to DESI survey validation data, the sample comprises 93% quasi-stellar objects (QSOs), 3% narrow-line AGN or blazars with a galaxy contamination rate of 2% and a stellar contamination rate of 2%. Peaking around redshift z=0.5, the BGS-AGN sample is intermediary between quasars from the rest of the BGS and those from the DESI QSO sample in terms of redshifts and AGN luminosities. The stacked spectrum is nearly identical to that of the DESI QSO targets, confirming that the sample is dominated by quasars. We highlight interesting small populations reaching z>2 which are either faint quasars with nearby projected companions or very bright quasars with strong absorption features including the Lyman-apha forest, metal absorbers and/or broad absorption lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03621v1-abstract-full').style.display = 'none'; document.getElementById('2404.03621v1-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 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">41 pages, 31 figures, submitted to the AAS journals. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03009">arXiv:2404.03009</a> <span> [<a href="https://arxiv.org/pdf/2404.03009">pdf</a>, <a href="https://arxiv.org/format/2404.03009">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"> HOD-Dependent Systematics in Emission Line Galaxies for the DESI 2024 BAO analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Rocher%2C+A">A. Rocher</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">S. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">B. Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">M. Rashkovetskyi</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">S. Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/astro-ph?searchtype=author&query=Medina-Varela%2C+L">L. Medina-Varela</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+P">P. McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+Y">Y. Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Bera%2C+A">A. Bera</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=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a> , et al. (51 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="2404.03009v2-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) will provide precise measurements of Baryon Acoustic Oscillations (BAO) to constrain the expansion history of the Universe and set stringent constraints on dark energy. Therefore, precise control of the global error budget due to various systematic effects is required for the DESI 2024 BAO analysis. In this work, we focus on the robustness of the BAO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03009v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03009v2-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) will provide precise measurements of Baryon Acoustic Oscillations (BAO) to constrain the expansion history of the Universe and set stringent constraints on dark energy. Therefore, precise control of the global error budget due to various systematic effects is required for the DESI 2024 BAO analysis. In this work, we focus on the robustness of the BAO analysis against the Halo Occupation Distribution (HOD) modeling for the Emission Line Galaxy (ELG) tracer. Based on a common dark matter simulation, our analysis relies on HOD mocks tuned to early DESI data, namely the One-Percent survey data. To build the mocks, we use several HOD models for the ELG tracer as well as extensions to the baseline HOD models. Among these extensions, we consider distinct recipes for galactic conformity and assembly bias. We perform two independent analyses in the Fourier space and in the configuration space. We recover the BAO signal from two-point measurements after performing reconstruction on our mocks. Additionally, we also apply the control variates technique to reduce sample variance noise. Our BAO analysis can recover the isotropic BAO parameter $伪_\text{iso}$ within 0.1\% and the Alcock Paczynski parameter $伪_\text{AP}$ within 0.3\%. Overall, we find that our systematic error due to the HOD dependence is below 0.17\%, with the Fourier space analysis being more robust against the HOD systematics. We conclude that our analysis pipeline is robust enough against the HOD systematics for the ELG tracer in the DESI 2024 BAO analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03009v2-abstract-full').style.display = 'none'; document.getElementById('2404.03009v2-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 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 III: Baryon Acoustic Oscillations from Galaxies and Quasars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03008">arXiv:2404.03008</a> <span> [<a href="https://arxiv.org/pdf/2404.03008">pdf</a>, <a href="https://arxiv.org/format/2404.03008">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"> HOD-Dependent Systematics for Luminous Red Galaxies in the DESI 2024 BAO Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">S. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">B. Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">M. Rashkovetskyi</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">S. Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Rocher%2C+A">A. Rocher</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+E">E. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Ishak%2C+M">M. Ishak</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=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a> , et al. (50 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="2404.03008v2-abstract-short" style="display: inline;"> In this paper, we present the estimation of systematics related to the halo occupation distribution (HOD) modeling in the baryon acoustic oscillations (BAO) distance measurement of the Dark Energy Spectroscopic Instrument (DESI) 2024 analysis. This paper focuses on the study of HOD systematics for luminous red galaxies (LRG). We consider three different HOD models for LRGs, including the base 5-pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03008v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03008v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03008v2-abstract-full" style="display: none;"> In this paper, we present the estimation of systematics related to the halo occupation distribution (HOD) modeling in the baryon acoustic oscillations (BAO) distance measurement of the Dark Energy Spectroscopic Instrument (DESI) 2024 analysis. This paper focuses on the study of HOD systematics for luminous red galaxies (LRG). We consider three different HOD models for LRGs, including the base 5-parameter vanilla model and two extensions to it, that we refer to as baseline and extended models. The baseline model is described by the 5 vanilla HOD parameters, an incompleteness factor and a velocity bias parameter, whereas the extended one also includes a galaxy assembly bias and a satellite profile parameter. We utilize the 25 dark matter simulations available in the AbacusSummit simulation suite at $z=$ 0.8 and generate mock catalogs for our different HOD models. To test the impact of the HOD modeling in the position of the BAO peak, we run BAO fits for all these sets of simulations and compare the best-fit BAO-scaling parameters $伪_{\rm iso}$ and $伪_{\rm AP}$ between every pair of HOD models. We do this for both Fourier and configuration spaces independently, using post-reconstruction measurements. We find a 3.3$蟽$ detection of HOD systematic for $伪_{\rm AP}$ in configuration space with an amplitude of 0.19%. For the other cases, we did not find a 3$蟽$ detection, and we decided to compute a conservative estimation of the systematic using the ensemble of shifts between all pairs of HOD models. By doing this, we quote a systematic with an amplitude of 0.07% in $伪_{\rm iso}$ for both Fourier and configuration spaces; and of 0.09% in $伪_{\rm AP}$ for Fourier space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03008v2-abstract-full').style.display = 'none'; document.getElementById('2404.03008v2-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 April, 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">36 pages, 9 figures. Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03007">arXiv:2404.03007</a> <span> [<a href="https://arxiv.org/pdf/2404.03007">pdf</a>, <a href="https://arxiv.org/format/2404.03007">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="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Semi-analytical covariance matrices for two-point correlation function for DESI 2024 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">M. Rashkovetskyi</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-S%C3%A1nchez%2C+D">D. Forero-S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D+J">D. J. Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">C. Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Gil-Mar%C3%ADn%2C+H">H. Gil-Mar铆n</a> , et al. (35 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="2404.03007v4-abstract-short" style="display: inline;"> We present an optimized way of producing the fast semi-analytical covariance matrices for the Legendre moments of the two-point correlation function, taking into account survey geometry and mimicking the non-Gaussian effects. We validate the approach on simulated (mock) catalogs for different galaxy types, representative of the Dark Energy Spectroscopic Instrument (DESI) Data Release 1, used in 20… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03007v4-abstract-full').style.display = 'inline'; document.getElementById('2404.03007v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03007v4-abstract-full" style="display: none;"> We present an optimized way of producing the fast semi-analytical covariance matrices for the Legendre moments of the two-point correlation function, taking into account survey geometry and mimicking the non-Gaussian effects. We validate the approach on simulated (mock) catalogs for different galaxy types, representative of the Dark Energy Spectroscopic Instrument (DESI) Data Release 1, used in 2024 analyses. We find only a few percent differences between the mock sample covariance matrix and our results, which can be expected given the approximate nature of the mocks, although we do identify discrepancies between the shot-noise properties of the DESI fiber assignment algorithm and the faster approximation (emulator) used in the mocks. Importantly, we find a close agreement (<=8% relative differences) in the projected errorbars for distance scale parameters for the baryon acoustic oscillation measurements. This confirms our method as an attractive alternative to simulation-based covariance matrices, especially for non-standard models or galaxy sample selections, making it particularly relevant to the broad current and future analyses of DESI data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03007v4-abstract-full').style.display = 'none'; document.getElementById('2404.03007v4-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 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 Publication is part of the 2024 series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 41 pages, 4 figures. Major rewrite after v2. Accepted to JCAP. Code available at https://github.com/oliverphilcox/RascalC and https://github.com/cosmodesi/RascalC-scripts/tree/DESI2024. Figure and table data available at https://zenodo.org/doi/10.5281/zenodo.10895161</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03006">arXiv:2404.03006</a> <span> [<a href="https://arxiv.org/pdf/2404.03006">pdf</a>, <a href="https://arxiv.org/format/2404.03006">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"> Production of Alternate Realizations of DESI Fiber Assignment for Unbiased Clustering Measurement in Data and Simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">J. Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+A+D">A. D. Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Hanif%2C+M+M+S">M. M. S Hanif</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+W+J">W. J. Percival</a>, <a href="/search/astro-ph?searchtype=author&query=Staten%2C+R">R. Staten</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=Bigwood%2C+L">L. Bigwood</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a> , et al. (30 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="2404.03006v3-abstract-short" style="display: inline;"> A critical requirement of spectroscopic large scale structure analyses is correcting for selection of which galaxies to observe from an isotropic target list. This selection is often limited by the hardware used to perform the survey which will impose angular constraints of simultaneously observable targets, requiring multiple passes to observe all of them. In SDSS this manifested solely as the co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03006v3-abstract-full').style.display = 'inline'; document.getElementById('2404.03006v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03006v3-abstract-full" style="display: none;"> A critical requirement of spectroscopic large scale structure analyses is correcting for selection of which galaxies to observe from an isotropic target list. This selection is often limited by the hardware used to perform the survey which will impose angular constraints of simultaneously observable targets, requiring multiple passes to observe all of them. In SDSS this manifested solely as the collision of physical fibers and plugs placed in plates. In DESI, there is the additional constraint of the robotic positioner which controls each fiber being limited to a finite patrol radius. A number of approximate methods have previously been proposed to correct the galaxy clustering statistics for these effects, but these generally fail on small scales. To accurately correct the clustering we need to upweight pairs of galaxies based on the inverse probability that those pairs would be observed (Bianchi \& Percival 2017). This paper details an implementation of that method to correct the Dark Energy Spectroscopic Instrument (DESI) survey for incompleteness. To calculate the required probabilities, we need a set of alternate realizations of DESI where we vary the relative priority of otherwise identical targets. These realizations take the form of alternate Merged Target Ledgers (AMTL), the files that link DESI observations and targets. We present the method used to generate these alternate realizations and how they are tracked forward in time using the real observational record and hardware status, propagating the survey as though the alternate orderings had been adopted. We detail the first applications of this method to the DESI One-Percent Survey (SV3) and the DESI year 1 data. We include evaluations of the pipeline outputs, estimation of survey completeness from this and other methods, and validation of the method using mock galaxy catalogs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03006v3-abstract-full').style.display = 'none'; document.getElementById('2404.03006v3-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 April, 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">30 pages, 21 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/2404.03005">arXiv:2404.03005</a> <span> [<a href="https://arxiv.org/pdf/2404.03005">pdf</a>, <a href="https://arxiv.org/format/2404.03005">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Optimal Reconstruction of Baryon Acoustic Oscillations for DESI 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Paillas%2C+E">E. Paillas</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">A. de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">S. Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">E. Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a> , et al. (51 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="2404.03005v3-abstract-short" style="display: inline;"> Baryon acoustic oscillations (BAO) provide a robust standard ruler to measure the expansion history of the Universe through galaxy clustering. Density-field reconstruction is now a widely adopted procedure for increasing the precision and accuracy of the BAO detection. With the goal of finding the optimal reconstruction settings to be used in the DESI 2024 galaxy BAO analysis, we assess the sensit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03005v3-abstract-full').style.display = 'inline'; document.getElementById('2404.03005v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03005v3-abstract-full" style="display: none;"> Baryon acoustic oscillations (BAO) provide a robust standard ruler to measure the expansion history of the Universe through galaxy clustering. Density-field reconstruction is now a widely adopted procedure for increasing the precision and accuracy of the BAO detection. With the goal of finding the optimal reconstruction settings to be used in the DESI 2024 galaxy BAO analysis, we assess the sensitivity of the post-reconstruction BAO constraints to different choices in our analysis configuration, performing tests on blinded data from the first year of DESI observations (DR1), as well as on mocks that mimic the expected clustering and selection properties of the DESI DR1 target samples. Overall, we find that BAO constraints remain robust against multiple aspects in the reconstruction process, including the choice of smoothing scale, treatment of redshift-space distortions, fiber assignment incompleteness, and parameterizations of the BAO model. We also present a series of tests that DESI followed in order to assess the maturity of the end-to-end galaxy BAO pipeline before the unblinding of the large-scale structure catalogs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03005v3-abstract-full').style.display = 'none'; document.getElementById('2404.03005v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 April, 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 III: Baryon Acoustic Oscillations from Galaxies and Quasars</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> <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/2404.01918">arXiv:2404.01918</a> <span> [<a href="https://arxiv.org/pdf/2404.01918">pdf</a>, <a href="https://arxiv.org/format/2404.01918">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The onset of bar formation in a massive galaxy at $z \sim 3.8$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amvrosiadis%2C+A">Aristeidis Amvrosiadis</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+S">Samuel Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Nightingale%2C+J">James Nightingale</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+Q">Qiuhan He</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Oman%2C+K+A">Kyle A. Oman</a>, <a href="/search/astro-ph?searchtype=author&query=Smail%2C+I">Ian Smail</a>, <a href="/search/astro-ph?searchtype=author&query=Swinbank%2C+M+A">Mark A. Swinbank</a>, <a href="/search/astro-ph?searchtype=author&query=Fragkoudi%2C+F">Francesca Fragkoudi</a>, <a href="/search/astro-ph?searchtype=author&query=Gadotti%2C+D+A">Dimitri A. Gadotti</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Borsato%2C+E">Edoardo Borsato</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+A">Andrew Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Massey%2C+R">Richard Massey</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+X">Xiaoyue Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">Ran Li</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="2404.01918v1-abstract-short" style="display: inline;"> We examine the morphological and kinematical properties of SPT-2147, a strongly lensed, massive, dusty, star-forming galaxy at $z = 3.762$. Combining data from JWST, HST, and ALMA, we study the galaxy's stellar emission, dust continuum and gas properties. The imaging reveals a central bar structure in the stars and gas embedded within an extended disc with a spiral arm-like feature. The kinematics… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01918v1-abstract-full').style.display = 'inline'; document.getElementById('2404.01918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.01918v1-abstract-full" style="display: none;"> We examine the morphological and kinematical properties of SPT-2147, a strongly lensed, massive, dusty, star-forming galaxy at $z = 3.762$. Combining data from JWST, HST, and ALMA, we study the galaxy's stellar emission, dust continuum and gas properties. The imaging reveals a central bar structure in the stars and gas embedded within an extended disc with a spiral arm-like feature. The kinematics confirm the presence of the bar and of the regularly rotating disc. Dynamical modeling yields a dynamical mass, ${M}_{\rm dyn} = (9.7 \pm 2.0) \times 10^{10}$ ${\rm M}_{\odot}$, and a maximum rotational velocity to velocity dispersion ratio, $V / 蟽= 9.8 \pm 1.2$. From multi-band imaging we infer, via SED fitting, a stellar mass, ${M}_{\star} = (6.3 \pm 0.9) \times 10^{10}$ $\rm{M}_{\odot}$, and a star formation rate, ${\rm SFR} = 781 \pm 99$ ${\rm M_{\odot} yr^{-1}}$, after correcting for magnification. Combining these measurements with the molecular gas mass, we derive a baryonic-to-total mass ratio of ${M}_{\rm bar} / {M}_{\rm dyn} = 0.9 \pm 0.2$ within 4.0 kpc. This finding suggests that the formation of bars in galaxies begins earlier in the history of the Universe than previously thought and can also occur in galaxies with elevated gas fractions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01918v1-abstract-full').style.display = 'none'; document.getElementById('2404.01918v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 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">19 pages, 11 figures. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.20093">arXiv:2403.20093</a> <span> [<a href="https://arxiv.org/pdf/2403.20093">pdf</a>, <a href="https://arxiv.org/format/2403.20093">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"> Neural Network-based model of galaxy power spectrum: Fast full-shape galaxy power spectrum analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trusov%2C+S">Svyatoslav Trusov</a>, <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">Pauline Zarrouk</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</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="2403.20093v1-abstract-short" style="display: inline;"> We present a Neural Network based emulator for the galaxy redshift-space power spectrum that enables several orders of magnitude acceleration in the galaxy clustering parameter inference, while preserving 3$蟽$ accuracy better than 0.5\% up to $k_{\mathrm{max}}$=0.25$h^{-1}Mpc$ within $螞$CDM and around 0.5\% $w_0$-$w_a$CDM. Our surrogate model only emulates the galaxy bias-invariant terms of 1-loop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.20093v1-abstract-full').style.display = 'inline'; document.getElementById('2403.20093v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.20093v1-abstract-full" style="display: none;"> We present a Neural Network based emulator for the galaxy redshift-space power spectrum that enables several orders of magnitude acceleration in the galaxy clustering parameter inference, while preserving 3$蟽$ accuracy better than 0.5\% up to $k_{\mathrm{max}}$=0.25$h^{-1}Mpc$ within $螞$CDM and around 0.5\% $w_0$-$w_a$CDM. Our surrogate model only emulates the galaxy bias-invariant terms of 1-loop perturbation theory predictions, these terms are then combined analytically with galaxy bias terms, counter-terms and stochastic terms in order to obtain the non-linear redshift space galaxy power spectrum. This allows us to avoid any galaxy bias prescription in the training of the emulator, which makes it more flexible. Moreover, we include the redshift $z \in [0,1.4]$ in the training which further avoids the need for re-training the emulator. We showcase the performance of the emulator in recovering the cosmological parameters of $螞$CDM by analysing the suite of 25 AbacusSummit simulations that mimic the DESI Luminous Red Galaxies at $z=0.5$ and $z=0.8$, together as the Emission Line Galaxies at $z=0.8$. We obtain similar performance in all cases, demonstrating the reliability of the emulator for any galaxy sample at any redshift in $0 < z < 1.4$ <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.20093v1-abstract-full').style.display = 'none'; document.getElementById('2403.20093v1-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> 29 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.18789">arXiv:2403.18789</a> <span> [<a href="https://arxiv.org/pdf/2403.18789">pdf</a>, <a href="https://arxiv.org/format/2403.18789">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"> Constraining primordial non-Gaussianity from the large scale structure two-point and three-point correlation functions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brown%2C+Z">Z. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Demina%2C+R">R. Demina</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=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">S. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Perez%2C+V">V. Gonzalez-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</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=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</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="2403.18789v1-abstract-short" style="display: inline;"> Surveys of cosmological large-scale structure (LSS) are sensitive to the presence of local primordial non-Gaussianity (PNG), and may be used to constrain models of inflation. Local PNG, characterized by fNL, the amplitude of the quadratic correction to the potential of a Gaussian random field, is traditionally measured from LSS two-point and three-point clustering via the power spectrum and bi-spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18789v1-abstract-full').style.display = 'inline'; document.getElementById('2403.18789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18789v1-abstract-full" style="display: none;"> Surveys of cosmological large-scale structure (LSS) are sensitive to the presence of local primordial non-Gaussianity (PNG), and may be used to constrain models of inflation. Local PNG, characterized by fNL, the amplitude of the quadratic correction to the potential of a Gaussian random field, is traditionally measured from LSS two-point and three-point clustering via the power spectrum and bi-spectrum. We propose a framework to measure fNL using the configuration space two-point correlation function (2pcf) monopole and three-point correlation function (3pcf) monopole of survey tracers. Our model estimates the effect of the scale-dependent bias induced by the presence of PNG on the 2pcf and 3pcf from the clustering of simulated dark matter halos. We describe how this effect may be scaled to an arbitrary tracer of the cosmological matter density. The 2pcf and 3pcf of this tracer are measured to constrain the value of fNL. Using simulations of luminous red galaxies observed by the Dark Energy Spectroscopic Instrument (DESI), we demonstrate the accuracy and constraining power of our model, and forecast the ability to constrainfNL to a precision of sigma(fNL) = 22 with one year of DESI survey data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18789v1-abstract-full').style.display = 'none'; document.getElementById('2403.18789v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16253">arXiv:2403.16253</a> <span> [<a href="https://arxiv.org/pdf/2403.16253">pdf</a>, <a href="https://arxiv.org/format/2403.16253">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Unveiling Lens Light Complexity with A Novel Multi-Gaussian Expansion Approach for Strong Gravitational Lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=He%2C+Q">Qiuhan He</a>, <a href="/search/astro-ph?searchtype=author&query=Nightingale%2C+J+W">James W. Nightingale</a>, <a href="/search/astro-ph?searchtype=author&query=Amvrosiadis%2C+A">Aris Amvrosiadis</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+A">Andrew Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Frenk%2C+C+S">Carlos S. Frenk</a>, <a href="/search/astro-ph?searchtype=author&query=Massey%2C+R">Richard Massey</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">Ran Li</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+X">Xiaoyue Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+S+C">Samuel C. Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7a%2C+J+P+C">Jo茫o Paulo C. Fran莽a</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="2403.16253v1-abstract-short" style="display: inline;"> In a strong gravitational lensing system, the distorted light from a source is analysed to infer the properties of the lens. However, light emitted by the lens itself can contaminate the image of the source, introducing systematic errors in the analysis. We present a simple and efficient lens light model based on the well-tested multi-Gaussian expansion (MGE) method for representing galaxy surface… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16253v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16253v1-abstract-full" style="display: none;"> In a strong gravitational lensing system, the distorted light from a source is analysed to infer the properties of the lens. However, light emitted by the lens itself can contaminate the image of the source, introducing systematic errors in the analysis. We present a simple and efficient lens light model based on the well-tested multi-Gaussian expansion (MGE) method for representing galaxy surface brightness profiles, which we combine with a semi-linear inversion scheme for pixelized source modelling. Testing it against realistic mock lensing images, we show that our scheme can fit the lensed images to the noise level, with relative differences between the true input and best-fit lens light model remaining below 5%. We apply the MGE lens light model to 38 lenses from the HST SLACS sample. We find that the new scheme provides a good fit for the majority of the sample with only 3 exceptions -- these show clear asymmetric residuals in the lens light. We examine the radial dependence of the ellipticity and position angles and confirm that it is common for a typical lens galaxy to exhibit twisting, non-elliptical isophotes and boxy / disky isophotes. Our MGE lens light model will be a valuable tool for understanding the hidden complexity of the lens mass distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16253v1-abstract-full').style.display = 'none'; document.getElementById('2403.16253v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 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">22 pages, 15 figures. Submitted to MNRAS. Comments Welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.14070">arXiv:2402.14070</a> <span> [<a href="https://arxiv.org/pdf/2402.14070">pdf</a>, <a href="https://arxiv.org/format/2402.14070">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"> Baryon Acoustic Oscillation Theory and Modelling Systematics for the DESI 2024 results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">Shi-Fan Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">Martin White</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+P">Patrick McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">Ashley J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">Hee-Jong Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">Nikhil Padmanabhan</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-S%C3%A1nchez%2C+D">D. Forero-S谩nchez</a> , et al. (36 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="2402.14070v2-abstract-short" style="display: inline;"> This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential bias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14070v2-abstract-full').style.display = 'inline'; document.getElementById('2402.14070v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.14070v2-abstract-full" style="display: none;"> This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic ($伪_{\mathrm{iso}}$) and anisotropic ($伪_{\mathrm{ap}}$) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than $0.1\%$ ($0.2\%$) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14070v2-abstract-full').style.display = 'none'; document.getElementById('2402.14070v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">30 pages, 18 figures, 1 table, updated to match version accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.17459">arXiv:2312.17459</a> <span> [<a href="https://arxiv.org/pdf/2312.17459">pdf</a>, <a href="https://arxiv.org/format/2312.17459">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Measuring the conditional luminosity and stellar mass functions of galaxies by combining the DESI LS DR9, SV3 and Y1 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yirong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Y">Yizhou Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+X">Xiaoju Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+H">Haojie Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yuyu Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Katsianis%2C+A">Antonios Katsianis</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">Jiaxin Han</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+M">Min He</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y">Yunliang Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qingyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yaru Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+W">Wensheng Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jiaqi Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+Z">Zhenlin Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+H">Hu Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+J+U">Johannes Ulf Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">ChangHoon Hahn</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">Peter Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a> , et al. (20 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="2312.17459v2-abstract-short" style="display: inline;"> In this investigation, we leverage the combination of Dark Energy Spectroscopic Instrument Legacy imaging Surveys Data Release 9 (DESI LS DR9), Survey Validation 3 (SV3), and Year 1 (Y1) data sets to estimate the conditional luminosity and stellar mass functions (CLFs & CSMFs) of galaxies across various halo mass bins and redshift ranges. To support our analysis, we utilize a realistic DESI Mock G… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.17459v2-abstract-full').style.display = 'inline'; document.getElementById('2312.17459v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.17459v2-abstract-full" style="display: none;"> In this investigation, we leverage the combination of Dark Energy Spectroscopic Instrument Legacy imaging Surveys Data Release 9 (DESI LS DR9), Survey Validation 3 (SV3), and Year 1 (Y1) data sets to estimate the conditional luminosity and stellar mass functions (CLFs & CSMFs) of galaxies across various halo mass bins and redshift ranges. To support our analysis, we utilize a realistic DESI Mock Galaxy Redshift Survey (MGRS) generated from a high-resolution Jiutian simulation. An extended halo-based group finder is applied to both MGRS catalogs and DESI observation. By comparing the r and z-band luminosity functions (LFs) and stellar mass functions (SMFs) derived using both photometric and spectroscopic data, we quantified the impact of photometric redshift (photo-z) errors on the galaxy LFs and SMFs, especially in the low redshift bin at low luminosity/mass end. By conducting prior evaluations of the group finder using MGRS, we successfully obtain a set of CLF and CSMF measurements from observational data. We find that at low redshift the faint end slopes of CLFs and CSMFs below $10^{9}h^{-2}L_{\odot}$ (or $h^{-2}M_{\odot}$) evince a compelling concordance with the subhalo mass functions. After correcting the cosmic variance effect of our local Universe following arXiv:1809.00523, the faint end slopes of the LFs/SMFs turn out to be also in good agreement with the slope of the halo mass function. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.17459v2-abstract-full').style.display = 'none'; document.getElementById('2312.17459v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 13 figures, Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08792">arXiv:2312.08792</a> <span> [<a href="https://arxiv.org/pdf/2312.08792">pdf</a>, <a href="https://arxiv.org/format/2312.08792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae1503">10.1093/mnras/stae1503 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Generating mock galaxy catalogues for flux-limited samples like the DESI Bright Galaxy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A">A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Grove%2C+C">C. Grove</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Norberg%2C+P">P. Norberg</a>, <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">P. Zarrouk</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">S. Yuan</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=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Hahn%2C+C">C. Hahn</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M+E">M. E. Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">A. Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">R. Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">J. Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Nie%2C+J">J. Nie</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+W+J">W. J. Percival</a> , et al. (6 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="2312.08792v2-abstract-short" style="display: inline;"> Accurate mock galaxy catalogues are crucial to validate analysis pipelines used to constrain dark energy models. We present a fast HOD-fitting method which we apply to the AbacusSummit simulations to create a set of mock catalogues for the DESI Bright Galaxy Survey, which contain r-band magnitudes and g-r colours. The halo tabulation method fits HODs for different absolute magnitude threshold samp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08792v2-abstract-full').style.display = 'inline'; document.getElementById('2312.08792v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08792v2-abstract-full" style="display: none;"> Accurate mock galaxy catalogues are crucial to validate analysis pipelines used to constrain dark energy models. We present a fast HOD-fitting method which we apply to the AbacusSummit simulations to create a set of mock catalogues for the DESI Bright Galaxy Survey, which contain r-band magnitudes and g-r colours. The halo tabulation method fits HODs for different absolute magnitude threshold samples simultaneously, preventing unphysical HOD crossing between samples. We validate the HOD fitting procedure by fitting to real-space clustering measurements and galaxy number densities from the MXXL BGS mock, which was tuned to the SDSS and GAMA surveys. The best-fitting clustering measurements and number densities are mostly within the assumed errors, but the clustering for the faint samples is low on large scales. The best-fitting HOD parameters are robust when fitting to simulations with different realisations of the initial conditions. When varying the cosmology, trends are seen as a function of each cosmological parameter. We use the best-fitting HOD parameters to create cubic box and cut sky mocks from the AbacusSummit simulations, in a range of cosmologies. As an illustration, we compare the Mr<-20 sample of galaxies in the mock with BGS measurements from the DESI one-percent survey. We find good agreement in the number densities, and the projected correlation function is reasonable, with differences that can be improved in the future by fitting directly to BGS clustering measurements. The cubic box and cut-sky mocks in different cosmologies are made publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08792v2-abstract-full').style.display = 'none'; document.getElementById('2312.08792v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">17 pages, 9 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09329">arXiv:2310.09329</a> <span> [<a href="https://arxiv.org/pdf/2310.09329">pdf</a>, <a href="https://arxiv.org/format/2310.09329">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Unraveling emission line galaxy conformity at z~1 with DESI early data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">Sihan Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Wechsler%2C+R+H">Risa H. Wechsler</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yunchong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Reyes%2C+M+A+C+d+l">Mithi A. C. de los Reyes</a>, <a href="/search/astro-ph?searchtype=author&query=Myles%2C+J">Justin Myles</a>, <a href="/search/astro-ph?searchtype=author&query=Rocher%2C+A">Antoine Rocher</a>, <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">Boryana Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">Theodore Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M">Michael Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">Marc Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">Aaron Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">Ramon Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Nie%2C+J">Jundan Nie</a>, <a href="/search/astro-ph?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.09329v1-abstract-short" style="display: inline;"> Emission line galaxies (ELGs) are now the preeminent tracers of large-scale structure at z>0.8 due to their high density and strong emission lines, which enable accurate redshift measurements. However, relatively little is known about ELG evolution and the ELG-halo connection, exposing us to potential modeling systematics in cosmology inference using these sources. In this paper, we propose a phys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09329v1-abstract-full').style.display = 'inline'; document.getElementById('2310.09329v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09329v1-abstract-full" style="display: none;"> Emission line galaxies (ELGs) are now the preeminent tracers of large-scale structure at z>0.8 due to their high density and strong emission lines, which enable accurate redshift measurements. However, relatively little is known about ELG evolution and the ELG-halo connection, exposing us to potential modeling systematics in cosmology inference using these sources. In this paper, we propose a physical picture of ELGs and improve ELG-halo connection modeling using a variety of observations and simulated galaxy models. We investigate DESI-selected ELGs in COSMOS data, and infer that ELGs are rapidly star-forming galaxies with a large fraction exhibiting disturbed morphology, implying that many of them are likely to be merger-driven starbursts. We further postulate that the tidal interactions from mergers lead to correlated star formation in central-satellite ELG pairs, a phenomenon dubbed "conformity." We argue for the need to include conformity in the ELG-halo connection using galaxy models such as IllustrisTNG, and by combining observations such as the DESI ELG auto-correlation, ELG cross-correlation with Luminous Red Galaxies (LRGs), and ELG-cluster cross-correlation. We also explore the origin of conformity using the UniverseMachine model and elucidate the difference between conformity and the well-known galaxy assembly bias effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09329v1-abstract-full').style.display = 'none'; document.getElementById('2310.09329v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 20 figures, submitted to MNRAS, comments welcome</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" 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