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class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16150">arXiv:2411.16150</a> <span> [<a href="https://arxiv.org/pdf/2411.16150">pdf</a>, <a href="https://arxiv.org/ps/2411.16150">ps</a>, <a href="https://arxiv.org/format/2411.16150">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"> Characterizing Stellar and Gas Properties in NGC 628: Spatial Distributions, Radial Gradients, and Resolved Scaling Relations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wei%2C+P">Peng Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+H">Hu Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jing Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Kong%2C+X">Xu Kong</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+S">Shuguo Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Ruilei Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Esamdin%2C+A">Ali Esamdin</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiantao Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Zhong%2C+T">Tuhong Zhong</a>, <a href="/search/astro-ph?searchtype=author&query=Dang%2C+F">Fei Dang</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="2411.16150v1-abstract-short" style="display: inline;"> Building on our previous research of multi-wavelength data from UV to IR, we employ spectroscopic observations of ionized gas, as well as neutral hydrogen gas obtained from the Five-hundred Meter Aperture Spherical Telescope (FAST), to explore the intrinsic processes of star formation and chemical enrichment within NGC 628. Our analysis focuses on several key properties, including gas-phase extinc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16150v1-abstract-full').style.display = 'inline'; document.getElementById('2411.16150v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16150v1-abstract-full" style="display: none;"> Building on our previous research of multi-wavelength data from UV to IR, we employ spectroscopic observations of ionized gas, as well as neutral hydrogen gas obtained from the Five-hundred Meter Aperture Spherical Telescope (FAST), to explore the intrinsic processes of star formation and chemical enrichment within NGC 628. Our analysis focuses on several key properties, including gas-phase extinction, star formation rate (SFR) surface density, oxygen abundance, and H I mass surface density. The azimuthal distributions of these parameters in relation to the morphological and kinematic features of FAST H I reveal that NGC 628 is an isolated galaxy that has not undergone recent interactions. We observe a mild radial extinction gradient accompanied by a notable dispersion. The SFR surface density also shows a gentle radial gradient, characteristic of typical spiral galaxies. Additionally, we find a negative radial metallicity gradient of $-0.44$ dex $R_{25}^{-1}$, supporting the "inside-out" scenario of galaxy formation. We investigate the resolved Mass-Metallicity Relation (MZR) and the resolved Star Formation Main Sequence (SFMS) alongside their dependencies on the physical properties of both ionized and neutral hydrogen gas. Our findings indicate no secondary dependency of the resolved MZR on SFR surface density or H I mass surface density. Furthermore, we observe that gas-phase extinction and the equivalent width of H伪 both increase with SFR surface density in the resolved SFMS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16150v1-abstract-full').style.display = 'none'; document.getElementById('2411.16150v1-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">20 pages, 15 figures. Accepted for publication in the Astrophysical Journal</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/2411.12024">arXiv:2411.12024</a> <span> [<a href="https://arxiv.org/pdf/2411.12024">pdf</a>, <a href="https://arxiv.org/format/2411.12024">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"> Mitigating Imaging Systematics for DESI 2024 Emission Line Galaxies and Beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rosado-Mar%C3%ADn%2C+A+J">A. J. Rosado-Mar铆n</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=Seo%2C+H">H. Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Rezaie%2C+M">M. Rezaie</a>, <a href="/search/astro-ph?searchtype=author&query=Kong%2C+H">H. Kong</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=Zhou%2C+R">R. Zhou</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=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=Ferraro%2C+S">S. Ferraro</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=Hahn%2C+C">C. Hahn</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>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</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=Newman%2C+J+A">J. A. Newman</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="2411.12024v1-abstract-short" style="display: inline;"> Emission Line Galaxies (ELGs) are one of the main tracers that the Dark Energy Spectroscopic Instrument (DESI) uses to probe the universe. However, they are afflicted by strong spurious correlations between target density and observing conditions known as imaging systematics. We present the imaging systematics mitigation applied to the DESI Data Release 1 (DR1) large-scale structure catalogs used… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12024v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12024v1-abstract-full" style="display: none;"> Emission Line Galaxies (ELGs) are one of the main tracers that the Dark Energy Spectroscopic Instrument (DESI) uses to probe the universe. However, they are afflicted by strong spurious correlations between target density and observing conditions known as imaging systematics. We present the imaging systematics mitigation applied to the DESI Data Release 1 (DR1) large-scale structure catalogs used in the DESI 2024 cosmological analyses. We also explore extensions of the fiducial treatment. This includes a combined approach, through forward image simulations in conjunction with neural network-based regression, to obtain an angular selection function that mitigates the imaging systematics observed in the DESI DR1 ELGs target density. We further derive a line-of-sight selection function from the forward model that removes the strong redshift dependence between imaging systematics and low redshift ELGs. Combining both angular and redshift-dependent systematics, we construct a 3D selection function and assess the impact of all selection functions on clustering statistics. We quantify differences between these extended treatments and the fiducial treatment in terms of the measured 2-point statistics. We find that the results are generally consistent with the fiducial treatment and conclude that the differences are far less than the imaging systematics uncertainty included in DESI 2024 full-shape measurements. We extend our investigation to the ELGs at $0.6<z<0.8$, i.e., beyond the redshift range ($0.8<z<1.6$) adopted for the DESI clustering catalog, and demonstrate that determining the full 3D selection function is necessary in this redshift range. Our tests showed that all changes are consistent with statistical noise for BAO analyses indicating they are robust to even severe imaging systematics. Specific tests for the full-shape analysis will be presented in a companion paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12024v1-abstract-full').style.display = 'none'; document.getElementById('2411.12024v1-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 Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 44 pages, 21 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2411.08313">arXiv:2411.08313</a> <span> [<a href="https://arxiv.org/pdf/2411.08313">pdf</a>, <a href="https://arxiv.org/format/2411.08313">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The Oscillation in Evolution of Changing-look Blazar OQ 334 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ren%2C+S+S">S. S. Ren</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R+X">R. X. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y+G">Y. G. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kang%2C+S+J">S. J. Kang</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="2411.08313v1-abstract-short" style="display: inline;"> We investigate the evolution of a changing-look blazar (CLB) on long timescales and expect to trace the state change of a CLB. Three morphological types, including a flat spectrum radio quasar (FSRQ) state, transition state, and BL Lacertae (BL Lac) state are classified according to the criteria proposed by analyzing the relationship between the equivalent width of the emission line and the $纬$-ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08313v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08313v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08313v1-abstract-full" style="display: none;"> We investigate the evolution of a changing-look blazar (CLB) on long timescales and expect to trace the state change of a CLB. Three morphological types, including a flat spectrum radio quasar (FSRQ) state, transition state, and BL Lacertae (BL Lac) state are classified according to the criteria proposed by analyzing the relationship between the equivalent width of the emission line and the $纬$-ray photon spectral index $螕_纬$. The multiwavelength light curves and spectral energy distributions corresponding to different epochs are obtained. The efforts found that $螕_纬$ satisfy the relationships with $螕_纬 $ $\gtrsim$ 2.2 for the FSRQ state, $2.0 < 螕_纬 < 2.2$ for the transition state, and $螕_纬$ $\lesssim$ 2.0 for the BL Lac state. We apply the criteria to the photon spectrum evolution of CLB OQ 334 during MJD 58678 - 60387. The evolution is subdivided into five FSRQ states, nine transition states, and four BL Lac states. Moreover, we use the model spectra parameters of each state epoch to test the reliability of subdivided morphological types. The result shows that: (1) the accretion rate parameter is consistent with our earlier research; and (2) there is an increasing trend in the epochs of the BL Lac states, even if there is not an obvious decreasing trend in epochs of the FSRQ states. We issue that strong evidence that a CLB is an especial epoch in the evolution of blazars that could be obtained from the oscillation phenomenon in the CLB evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08313v1-abstract-full').style.display = 'none'; document.getElementById('2411.08313v1-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 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">16 pages, 7 figures, accepted by the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.01215">arXiv:2411.01215</a> <span> [<a href="https://arxiv.org/pdf/2411.01215">pdf</a>, <a href="https://arxiv.org/format/2411.01215">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Detection of two TeV gamma-ray outbursts from NGC 1275 by LHAASO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T+L">T. L. Chen</a> , et al. (254 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.01215v2-abstract-short" style="display: inline;"> The Water Cherenkov Detector Array (WCDA) is one of the components of Large High Altitude Air Shower Observatory (LHAASO) and can monitor any sources over two-thirds of the sky for up to 7 hours per day with >98\% duty cycle. In this work, we report the detection of two outbursts of the Fanaroff-Riley I radio galaxy NGC 1275 that were detected by LHAASO-WCDA between November 2022 and January 2023… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01215v2-abstract-full').style.display = 'inline'; document.getElementById('2411.01215v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.01215v2-abstract-full" style="display: none;"> The Water Cherenkov Detector Array (WCDA) is one of the components of Large High Altitude Air Shower Observatory (LHAASO) and can monitor any sources over two-thirds of the sky for up to 7 hours per day with >98\% duty cycle. In this work, we report the detection of two outbursts of the Fanaroff-Riley I radio galaxy NGC 1275 that were detected by LHAASO-WCDA between November 2022 and January 2023 with statistical significance of 5.2~$蟽$ and 8.3~$蟽$. The observed spectral energy distribution in the range from 500 GeV to 3 TeV is fitted by a power-law with a best-fit spectral index of $伪=-3.37\pm0.52$ and $-3.35\pm0.29$, respectively. The outburst flux above 0.5~TeV was ($4.55\pm 4.21)\times~10^{-11}~\rm cm^{-2}~s^{-1}$ and ($3.45\pm 1.78)\times~10^{-11}~\rm cm^{-2}~s^{-1}$, corresponding to 60\%, 45\% of Crab Nebula flux. Variation analysis reveals the variability time-scale of days at the TeV energy band. A simple test by one-zone synchrotron self-Compton model reproduces the data in the gamma-ray band well. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01215v2-abstract-full').style.display = 'none'; document.getElementById('2411.01215v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">11 pages, 8 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/2410.16565">arXiv:2410.16565</a> <span> [<a href="https://arxiv.org/pdf/2410.16565">pdf</a>, <a href="https://arxiv.org/format/2410.16565">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for gravitational waves emitted from SN 2023ixf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1758 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="2410.16565v1-abstract-short" style="display: inline;"> We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19th, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16565v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16565v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16565v1-abstract-full" style="display: none;"> We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19th, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been identified in data when at least two gravitational-wave observatories were operating, which covered $\sim 14\%$ of this five-day window. We report the search detection efficiency for various possible gravitational-wave emission models. Considering the distance to M101 (6.7 Mpc), we derive constraints on the gravitational-wave emission mechanism of core-collapse supernovae across a broad frequency spectrum, ranging from 50 Hz to 2 kHz where we assume the GW emission occurred when coincident data are available in the on-source window. Considering an ellipsoid model for a rotating proto-neutron star, our search is sensitive to gravitational-wave energy $1 \times 10^{-5} M_{\odot} c^2$ and luminosity $4 \times 10^{-5} M_{\odot} c^2/\text{s}$ for a source emitting at 50 Hz. These constraints are around an order of magnitude more stringent than those obtained so far with gravitational-wave data. The constraint on the ellipticity of the proto-neutron star that is formed is as low as $1.04$, at frequencies above $1200$ Hz, surpassing results from SN 2019ejj. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16565v1-abstract-full').style.display = 'none'; document.getElementById('2410.16565v1-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 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">Main paper: 6 pages, 4 figures and 1 table. Total with appendices: 20 pages, 4 figures, and 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2400125 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.13402">arXiv:2410.13402</a> <span> [<a href="https://arxiv.org/pdf/2410.13402">pdf</a>, <a href="https://arxiv.org/format/2410.13402">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Monte Carlo Simulation of Angular Response of GRID Detectors for GRID Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Q">Qize Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+X">Xiaofan Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+X">Xutao Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">Huaizhong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+L">Longhao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Q">Qidong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Z">Zirui Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+C">Chenchong Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+W">Wenxuan Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+J">Jianping Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zeng%2C+Z">Zhi Zeng</a>, <a href="/search/astro-ph?searchtype=author&query=Zeng%2C+M">Ming Zeng</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Hua Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Binbin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Zhonghai Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rong Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuanyuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+L">Lin Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Zhong%2C+J">Jiayong Zhong</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Jianyong Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+W">Wentao Han</a>, <a href="/search/astro-ph?searchtype=author&query=Tian%2C+Y">Yang Tian</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+B">Benda Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+G">GRID Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.13402v1-abstract-short" style="display: inline;"> The Gamma-Ray Integrated Detectors (GRID) are a space science mission that employs compact gamma-ray detectors mounted on NanoSats in low Earth orbit (LEO) to monitor the transient gamma-ray sky. Owing to the unpredictability of the time and location of gamma-ray bursts (GRBs), obtaining the photon responses of gamma-ray detectors at various incident angles is important for the scientific analysis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13402v1-abstract-full').style.display = 'inline'; document.getElementById('2410.13402v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.13402v1-abstract-full" style="display: none;"> The Gamma-Ray Integrated Detectors (GRID) are a space science mission that employs compact gamma-ray detectors mounted on NanoSats in low Earth orbit (LEO) to monitor the transient gamma-ray sky. Owing to the unpredictability of the time and location of gamma-ray bursts (GRBs), obtaining the photon responses of gamma-ray detectors at various incident angles is important for the scientific analysis of GRB data captured by GRID detectors. For this purpose, a dedicated Monte Carlo simulation framework has been developed for GRID detectors. By simulating each GRID detector and the NanoSat carrying it, the spectral energy response, detection efficiency, and other angular responses of each detector for photons with different incident angles and energies can be obtained within this framework. The accuracy of these simulations has been corroborated through on-ground calibration, and the derived angular responses have been successfully applied to the data analysis of recorded GRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13402v1-abstract-full').style.display = 'none'; document.getElementById('2410.13402v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">15 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09151">arXiv:2410.09151</a> <span> [<a href="https://arxiv.org/pdf/2410.09151">pdf</a>, <a href="https://arxiv.org/format/2410.09151">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A search using GEO600 for gravitational waves coincident with fast radio bursts from SGR 1935+2154 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a> , et al. (1758 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="2410.09151v1-abstract-short" style="display: inline;"> The magnetar SGR 1935+2154 is the only known Galactic source of fast radio bursts (FRBs). FRBs from SGR 1935+2154 were first detected by CHIME/FRB and STARE2 in 2020 April, after the conclusion of the LIGO, Virgo, and KAGRA Collaborations' O3 observing run. Here we analyze four periods of gravitational wave (GW) data from the GEO600 detector coincident with four periods of FRB activity detected by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09151v1-abstract-full').style.display = 'inline'; document.getElementById('2410.09151v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09151v1-abstract-full" style="display: none;"> The magnetar SGR 1935+2154 is the only known Galactic source of fast radio bursts (FRBs). FRBs from SGR 1935+2154 were first detected by CHIME/FRB and STARE2 in 2020 April, after the conclusion of the LIGO, Virgo, and KAGRA Collaborations' O3 observing run. Here we analyze four periods of gravitational wave (GW) data from the GEO600 detector coincident with four periods of FRB activity detected by CHIME/FRB, as well as X-ray glitches and X-ray bursts detected by NICER and NuSTAR close to the time of one of the FRBs. We do not detect any significant GW emission from any of the events. Instead, using a short-duration GW search (for bursts $\leq$ 1 s) we derive 50\% (90\%) upper limits of $10^{48}$ ($10^{49}$) erg for GWs at 300 Hz and $10^{49}$ ($10^{50}$) erg at 2 kHz, and constrain the GW-to-radio energy ratio to $\leq 10^{14} - 10^{16}$. We also derive upper limits from a long-duration search for bursts with durations between 1 and 10 s. These represent the strictest upper limits on concurrent GW emission from FRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09151v1-abstract-full').style.display = 'none'; document.getElementById('2410.09151v1-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">15 pages of text including references, 4 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2400192 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07038">arXiv:2410.07038</a> <span> [<a href="https://arxiv.org/pdf/2410.07038">pdf</a>, <a href="https://arxiv.org/format/2410.07038">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"> Deep HI Mapping of M 106 Group with FAST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+M">Ming Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+H">Hai-Yang Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rui-Lei Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+J">Jin-Long Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Ai%2C+M">Mei Ai</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+P">Peng Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+L">Li-Xia Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hai-Yan Zhang</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="2410.07038v1-abstract-short" style="display: inline;"> We used FAST to conduct deep HI imaging of the entire M 106 group region, and have discovered a few new HI filaments and clouds. Three HI clouds/filaments are found in a region connecting DDO 120 and NGC 4288, indicating an interaction between these two galaxies. The HI features in this region suggest that DDO 120 is probably the origin of the HI stream extending from the northern end of NGC 4288… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07038v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07038v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07038v1-abstract-full" style="display: none;"> We used FAST to conduct deep HI imaging of the entire M 106 group region, and have discovered a few new HI filaments and clouds. Three HI clouds/filaments are found in a region connecting DDO 120 and NGC 4288, indicating an interaction between these two galaxies. The HI features in this region suggest that DDO 120 is probably the origin of the HI stream extending from the northern end of NGC 4288 to M 106. This structure is similar to the SMC-LMC stream, but much longer, about 190 kpc. Furthermore, based on the distance measurements, we have determined the satellite galaxy members of M 106. With an absolute magnitude cutoff of M_B=-10, we obtained a sample of 11 member satellite galaxies for M 106. Using the observed HI mass with FAST, we studied the properties of satellite galaxies in M 106 and found that satellite galaxies with lower stellar masses exhibit more significant deviations from the star-forming main sequence (SFMS) in their specific star formation rates. Furthermore, the relationship between the HI mass of satellite galaxies and optical diameter generally follows the field galaxies relation. We discuss the possible mechanisms leading to the quenching in the M 106 group based on the new data from FAST <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07038v1-abstract-full').style.display = 'none'; document.getElementById('2410.07038v1-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 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">18 pages,11 figures and 3 tables.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/2410.04425">arXiv:2410.04425</a> <span> [<a href="https://arxiv.org/pdf/2410.04425">pdf</a>, <a href="https://arxiv.org/format/2410.04425">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> LHAASO detection of very-high-energy gamma-ray emission surrounding PSR J0248+6021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 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="2410.04425v1-abstract-short" style="display: inline;"> We report the detection of an extended very-high-energy (VHE) gamma-ray source coincident with the locations of middle-aged (62.4~\rm kyr) pulsar PSR J0248+6021, by using the LHAASO-WCDA data of live 796 days and LHAASO-KM2A data of live 1216 days. A significant excess of \gray induced showers is observed both by WCDA in energy bands of 1-25~\rm TeV and KM2A in energy bands of $>$ 25~\rm TeV with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.04425v1-abstract-full').style.display = 'inline'; document.getElementById('2410.04425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.04425v1-abstract-full" style="display: none;"> We report the detection of an extended very-high-energy (VHE) gamma-ray source coincident with the locations of middle-aged (62.4~\rm kyr) pulsar PSR J0248+6021, by using the LHAASO-WCDA data of live 796 days and LHAASO-KM2A data of live 1216 days. A significant excess of \gray induced showers is observed both by WCDA in energy bands of 1-25~\rm TeV and KM2A in energy bands of $>$ 25~\rm TeV with 7.3 $蟽$ and 13.5 $蟽$, respectively. The best-fit position derived through WCDA data is R.A. = 42.06$^\circ \pm$ 0.12$^\circ$ and Dec. = 60.24$^\circ \pm $ 0.13$^\circ$ with an extension of 0.69$^\circ\pm$0.15$^\circ$ and that of the KM2A data is R.A.= 42.29$^\circ \pm $ 0.13$^\circ$ and Dec. = 60.38$^\circ \pm$ 0.07$^\circ$ with an extension of 0.37$^\circ\pm$0.07$^\circ$. No clear extended multiwavelength counterpart of this LHAASO source has been found from the radio band to the GeV band. The most plausible explanation of the VHE \gray emission is the inverse Compton process of highly relativistic electrons and positrons injected by the pulsar. These electrons/positrons are hypothesized to be either confined within the pulsar wind nebula or to have already escaped into the interstellar medium, forming a pulsar halo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.04425v1-abstract-full').style.display = 'none'; document.getElementById('2410.04425v1-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 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">12 pages, 10 figures, Accepted by Sci. China-Phys. Mech. Astron</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.05140">arXiv:2409.05140</a> <span> [<a href="https://arxiv.org/pdf/2409.05140">pdf</a>, <a href="https://arxiv.org/format/2409.05140">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"> Stellar reddening map from DESI imaging and spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</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=Schlafly%2C+E+F">Edward F. Schlafly</a>, <a href="/search/astro-ph?searchtype=author&query=Schlegel%2C+D">David Schlegel</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">David Bianchi</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=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=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D+J">Daniel J. Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</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=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</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="2409.05140v2-abstract-short" style="display: inline;"> We present new Galactic reddening maps of the high Galactic latitude sky using DESI imaging and spectroscopy. We directly measure the reddening of 2.6 million stars by comparing the observed stellar colors in $g-r$ and $r-z$ from DESI imaging with the synthetic colors derived from DESI spectra from the first two years of the survey. The reddening in the two colors is on average consistent with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05140v2-abstract-full').style.display = 'inline'; document.getElementById('2409.05140v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.05140v2-abstract-full" style="display: none;"> We present new Galactic reddening maps of the high Galactic latitude sky using DESI imaging and spectroscopy. We directly measure the reddening of 2.6 million stars by comparing the observed stellar colors in $g-r$ and $r-z$ from DESI imaging with the synthetic colors derived from DESI spectra from the first two years of the survey. The reddening in the two colors is on average consistent with the \cite{fitzpatrick_correcting_1999} extinction curve with $R_\mathrm{V}=3.1$. We find that our reddening maps differ significantly from the commonly used \cite{schlegel_maps_1998} (SFD) reddening map (by up to 80 mmag in $E(B-V)$), and we attribute most of this difference to systematic errors in the SFD map. To validate the reddening map, we select a galaxy sample with extinction correction based on our reddening map, and this yields significantly better uniformity than the SFD extinction correction. Finally, we discuss the potential systematic errors in the DESI reddening measurements, including the photometric calibration errors that are the limiting factor on our accuracy. The $E(g-r)$ and $E(g-r)$ maps presented in this work, and for convenience their corresponding $E(B-V)$ maps with SFD calibration, are publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05140v2-abstract-full').style.display = 'none'; document.getElementById('2409.05140v2-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">v1</span> submitted 8 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">Submitted to the Open Journal of Astrophysics. Associated data files: https://data.desi.lbl.gov/public/papers/mws/desi_dust/y2/v1/maps/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.12867">arXiv:2407.12867</a> <span> [<a href="https://arxiv.org/pdf/2407.12867">pdf</a>, <a href="https://arxiv.org/format/2407.12867">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Swift-BAT GUANO follow-up of gravitational-wave triggers in the third LIGO-Virgo-KAGRA observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raman%2C+G">Gayathri Raman</a>, <a href="/search/astro-ph?searchtype=author&query=Ronchini%2C+S">Samuele Ronchini</a>, <a href="/search/astro-ph?searchtype=author&query=Delaunay%2C+J">James Delaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Parsotan%2C+T">Tyler Parsotan</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+E">Elena Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+M+G">Maria Grazia Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Cusumano%2C+G">Giancarlo Cusumano</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ai%2C+A">Antonino D'Ai</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">Paolo D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Elia%2C+V">Valerio D'Elia</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pasquale%2C+M">Massimiliano De Pasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Dichiara%2C+S">Simone Dichiara</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P">Phil Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">Dieter Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kuin%2C+P">Paul Kuin</a>, <a href="/search/astro-ph?searchtype=author&query=Melandri%2C+A">Andrea Melandri</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+J+P">Julian P. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K">Kim Page</a>, <a href="/search/astro-ph?searchtype=author&query=Palmer%2C+D+M">David M. Palmer</a>, <a href="/search/astro-ph?searchtype=author&query=Sbarufatti%2C+B">Boris Sbarufatti</a>, <a href="/search/astro-ph?searchtype=author&query=Tagliaferri%2C+G">Gianpiero Tagliaferri</a> , et al. (1797 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="2407.12867v1-abstract-short" style="display: inline;"> We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO-Virgo-KAGRA (LVK) network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received in low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wav… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12867v1-abstract-full').style.display = 'inline'; document.getElementById('2407.12867v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.12867v1-abstract-full" style="display: none;"> We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO-Virgo-KAGRA (LVK) network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received in low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum--likelihood NITRATES pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15-350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10$^{-3}$ Hz, we compute the GW--BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12867v1-abstract-full').style.display = 'none'; document.getElementById('2407.12867v1-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 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">50 pages, 10 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.10788">arXiv:2407.10788</a> <span> [<a href="https://arxiv.org/pdf/2407.10788">pdf</a>, <a href="https://arxiv.org/format/2407.10788">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450886">10.1051/0004-6361/202450886 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CircleZ: Reliable Photometric redshifts for AGN computed using only photometry from Legacy Survey Imaging for DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Roster%2C+W">W. Roster</a>, <a href="/search/astro-ph?searchtype=author&query=Shirley%2C+R">R. Shirley</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Kohl%2C+C">C. Kohl</a>, <a href="/search/astro-ph?searchtype=author&query=Starck%2C+H">H. Starck</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/astro-ph?searchtype=author&query=Krippendorf%2C+S">S. Krippendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Zenteno%2C+A">A. Zenteno</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">D. Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Schlegel%2C+D">D. Schlegel</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">R. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+F">F. Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+A">A. Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">S. F. Anderson</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.10788v2-abstract-short" style="display: inline;"> (abridged)Photometric redshifts for AGN (galaxies hosting an accreting supermassive black hole in their center) are notoriously challenging and currently better computed via SED fitting, assuming that deep photometry for many wavelengths is available. However, for AGN detected all-sky, the photometry is limited and provided by different projects. This makes the task of homogenising the data challe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10788v2-abstract-full').style.display = 'inline'; document.getElementById('2407.10788v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10788v2-abstract-full" style="display: none;"> (abridged)Photometric redshifts for AGN (galaxies hosting an accreting supermassive black hole in their center) are notoriously challenging and currently better computed via SED fitting, assuming that deep photometry for many wavelengths is available. However, for AGN detected all-sky, the photometry is limited and provided by different projects. This makes the task of homogenising the data challenging and is a dramatic drawback for the millions of AGN that wide surveys like SRG/eROSITA will detect. This work aims to compute reliable photometric redshifts for X-ray-detected AGN using only one dataset that covers a large area: the 10th Data Release of the Imaging Legacy Survey (LS10) for DESI. LS10 provides deep grizW1-W4 forced photometry within various apertures, thus avoids issues related to the cross-calibration of surveys. We present the results from CircleZ, a machine-learning algorithm based on a Fully Connected Neural Network. CircleZ uses training sample of 14,000 X-ray-detected AGN and utilizes multi-aperture photometry. The accuracy and the fraction of outliers reached in a test sample of 2913 AGN are 0.067 and 11.6%, respectively. The results are comparable to or better than those obtained previously for the same field but with much less effort. We further tested the stability of the results by computing the photometric redshifts for the sources detected in CSC2 and Chandra-COSMOS Legacy, reaching comparable accuracy as in eFEDS when limiting the magnitude of the counterparts with respect to the depth of LS10. The method applies to fainter samples of AGN using deeper optical data from future surveys (e.g., LSST, Euclid), granted LS10-like information on the light distribution beyond a morphological type is provided. With the paper, we release an updated version of the photometric redshifts (including errors and probability distribution function) for eROSITA/eFEDS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10788v2-abstract-full').style.display = 'none'; document.getElementById('2407.10788v2-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> 20 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">A&A, paper accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A365 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.07152">arXiv:2407.07152</a> <span> [<a href="https://arxiv.org/pdf/2407.07152">pdf</a>, <a href="https://arxiv.org/format/2407.07152">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"> Evidence for large baryonic feedback at low and intermediate redshifts from kinematic Sunyaev-Zel'dovich observations with ACT and DESI photometric galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">B. Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Guachalla%2C+B+R">B. Ried Guachalla</a>, <a href="/search/astro-ph?searchtype=author&query=Schaan%2C+E">E. Schaan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">N. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">S. K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">W. R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">M. Devlin</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=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">J. Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">G. S. Farren</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=Gallardo%2C+P+A">P. A. Gallardo</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">S. Gontcho Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gralla%2C+M">M. Gralla</a> , et al. (48 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="2407.07152v1-abstract-short" style="display: inline;"> Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$蟽$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07152v1-abstract-full').style.display = 'inline'; document.getElementById('2407.07152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07152v1-abstract-full" style="display: none;"> Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$蟽$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamical simulation IllustrisTNG compared with high-feedback models such as that of the original Illustris simulation. This has important implications for bridging the gap between theory and observations and understanding galaxy formation and evolution. Furthermore, a better grasp of the baryon-dark matter link is critical to future cosmological analyses, which are currently impeded by our limited knowledge of baryonic feedback. Here, we measure the kinematic Sunyaev-Zel'dovich (kSZ) effect from the Atacama Cosmology Telescope (ACT), stacked on the luminous red galaxy (LRG) sample of the Dark Energy Spectroscopic Instrument (DESI) imaging survey. This is the first analysis to use photometric redshifts for reconstructing galaxy velocities. Due to the large number of galaxies comprising the DESI imaging survey, this is the highest signal-to-noise stacked kSZ measurement to date: we detect the signal at 13$蟽$ and find that the gas is more spread out than the dark matter at $\sim$40$蟽$. Our work opens up the possibility to recalibrate large hydrodynamical simulations using the kSZ effect. In addition, our findings point towards a way of alleviating inconsistencies between weak lensing surveys and cosmic microwave background (CMB) experiments such as the `low $S_8$' tension, and shed light on long-standing enigmas in astrophysics such as the `missing baryon' problem. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07152v1-abstract-full').style.display = 'none'; document.getElementById('2407.07152v1-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 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">20 pages, 8 figures, submitting to PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.06336">arXiv:2407.06336</a> <span> [<a href="https://arxiv.org/pdf/2407.06336">pdf</a>, <a href="https://arxiv.org/format/2407.06336">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"> GD-1 Stellar Stream and Cocoon in the DESI Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Valluri%2C+M">Monica Valluri</a>, <a href="/search/astro-ph?searchtype=author&query=Fagrelius%2C+P">Parker Fagrelius</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=Li%2C+T+S">Ting S. Li</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=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+R+G">Raymond G. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+A+P">Andrew P. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessia N. Aguilar</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=Belokurov%2C+V">Vasily Belokurov</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=Brooks%2C+D">David Brooks</a>, <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=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">Kyle Dawson</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">Peter Doel</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=Honscheid%2C+K">Klaus Honscheid</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">Anthony Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+A">A. Lambert</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="2407.06336v1-abstract-short" style="display: inline;"> We present ~ 126 new spectroscopically identified members of the GD-1 tidal stream obtained with the 5000-fiber Dark Energy Spectroscopic Instrument (DESI). We confirm the existence of a ``cocoon'' which is broad (FWHM~2.932deg~460pc) and kinematically hot (velocity dispersion, sigma~5-8km/s) component that surrounds a narrower (FWHM~0.353deg~55pc) and colder (sigma~ 2.2-2.6km/s) thin stream compo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06336v1-abstract-full').style.display = 'inline'; document.getElementById('2407.06336v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06336v1-abstract-full" style="display: none;"> We present ~ 126 new spectroscopically identified members of the GD-1 tidal stream obtained with the 5000-fiber Dark Energy Spectroscopic Instrument (DESI). We confirm the existence of a ``cocoon'' which is broad (FWHM~2.932deg~460pc) and kinematically hot (velocity dispersion, sigma~5-8km/s) component that surrounds a narrower (FWHM~0.353deg~55pc) and colder (sigma~ 2.2-2.6km/s) thin stream component (based on a median per star velocity precision of 2.7km/s). The cocoon extends over at least a ~ 20deg segment of the stream observed by DESI. The thin and cocoon components have similar mean values of [Fe/H]: -2.54+/- 0.04dex and -2.45+/-0.06dex suggestive of a common origin. The data are consistent with the following scenarios for the origin of the cocoon. The progenitor of the GD-1 stream was an accreted globular cluster (GC) and: (a) the cocoon was produced by pre-accretion tidal stripping of the GC while it was still inside its parent dwarf galaxy; (b) the cocoon is debris from the parent dwarf galaxy; (c) an initially thin GC tidal stream was heated by impacts from dark subhalos in the Milky Way; (d) an initially thin GC stream was heated by a massive Sagittarius dwarf galaxy; or a combination of some these. In the first two cases the velocity dispersion and mean metallicity are consistent with the parent dwarf galaxy having a halo mass of ~0^9\msun. Future DESI spectroscopy and detailed modeling may enable us to distinguish between these possible origins. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06336v1-abstract-full').style.display = 'none'; document.getElementById('2407.06336v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 July, 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">Submitted to ApJ, 23 pages, 13 figures 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04795">arXiv:2407.04795</a> <span> [<a href="https://arxiv.org/pdf/2407.04795">pdf</a>, <a href="https://arxiv.org/format/2407.04795">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"> Not all lensing is low: An analysis of DESI$\times$DES using the Lagrangian Effective Theory of LSS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=DeRose%2C+J">J. DeRose</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">R. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">M. White</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+J+U">J. U. Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Wechsler%2C+R+H">R. H. Wechsler</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=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=Font-Ribera%2C+A">A. Font-Ribera</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=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=Kisner%2C+T">T. Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</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="2407.04795v2-abstract-short" style="display: inline;"> In this work we use Lagrangian perturbation theory to analyze the harmonic space galaxy clustering signal of Bright Galaxy Survey (BGS) and Luminous Red Galaxies (LRGs) targeted by the Dark Energy Spectroscopic Instrument (DESI), combined with the galaxy--galaxy lensing signal measured around these galaxies using Dark Energy Survey Year 3 source galaxies. The BGS and LRG galaxies are extremely wel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04795v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04795v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04795v2-abstract-full" style="display: none;"> In this work we use Lagrangian perturbation theory to analyze the harmonic space galaxy clustering signal of Bright Galaxy Survey (BGS) and Luminous Red Galaxies (LRGs) targeted by the Dark Energy Spectroscopic Instrument (DESI), combined with the galaxy--galaxy lensing signal measured around these galaxies using Dark Energy Survey Year 3 source galaxies. The BGS and LRG galaxies are extremely well characterized by DESI spectroscopy and, as a result, lens galaxy redshift uncertainty and photometric systematics contribute negligibly to the error budget of our ``$2\times2$-point'' analysis. On the modeling side, this work represents the first application of the \texttt{spinosaurus} code, implementing an effective field theory model for galaxy intrinsic alignments, and we additionally introduce a new scheme (\texttt{MAIAR}) for marginalizing over the large uncertainties in the redshift evolution of the intrinsic alignment signal. Furthermore, this is the first application of a hybrid effective field theory (HEFT) model for galaxy bias based on the $\texttt{Aemulus}\, 谓$ simulations. Our main result is a measurement of the amplitude of the lensing signal, $S_8=蟽_8 \left(惟_m/0.3\right)^{0.5} = 0.850^{+0.042}_{-0.050}$, consistent with values of this parameter derived from the primary CMB. This constraint is artificially improved by a factor of $51\%$ if we assume a more standard, but restrictive parameterization for the redshift evolution and sample dependence of the intrinsic alignment signal, and $63\%$ if we additionally assume the nonlinear alignment model. We show that when fixing the cosmological model to the best-fit values from Planck PR4 there is $> 5 蟽$ evidence for a deviation of the evolution of the intrinsic alignment signal from the functional form that is usually assumed in cosmic shear and galaxy--galaxy lensing studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04795v2-abstract-full').style.display = 'none'; document.getElementById('2407.04795v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">53 pages, 25 figures, updated to match version accepted by PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04607">arXiv:2407.04607</a> <span> [<a href="https://arxiv.org/pdf/2407.04607">pdf</a>, <a href="https://arxiv.org/format/2407.04607">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"> Cosmological constraints from the cross-correlation of DESI Luminous Red Galaxies with CMB lensing from Planck PR4 and ACT DR6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sailer%2C+N">Noah Sailer</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">Martin White</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</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=Bond%2C+J+R">J. Richard Bond</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=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">Shi-Fan Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</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=DeRose%2C+J">Joseph DeRose</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=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Embil-Villagra%2C+C">Carmen Embil-Villagra</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">Gerrit S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04607v1-abstract-short" style="display: inline;"> We infer the growth of large scale structure over the redshift range $0.4\lesssim z \lesssim 1$ from the cross-correlation of spectroscopically calibrated Luminous Red Galaxies (LRGs) selected from the Dark Energy Spectroscopic Instrument (DESI) legacy imaging survey with CMB lensing maps reconstructed from the latest Planck and ACT data. We adopt a hybrid effective field theory (HEFT) model that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04607v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04607v1-abstract-full" style="display: none;"> We infer the growth of large scale structure over the redshift range $0.4\lesssim z \lesssim 1$ from the cross-correlation of spectroscopically calibrated Luminous Red Galaxies (LRGs) selected from the Dark Energy Spectroscopic Instrument (DESI) legacy imaging survey with CMB lensing maps reconstructed from the latest Planck and ACT data. We adopt a hybrid effective field theory (HEFT) model that robustly regulates the cosmological information obtainable from smaller scales, such that our cosmological constraints are reliably derived from the (predominantly) linear regime. We perform an extensive set of bandpower- and parameter-level systematics checks to ensure the robustness of our results and to characterize the uniformity of the LRG sample. We demonstrate that our results are stable to a wide range of modeling assumptions, finding excellent agreement with a linear theory analysis performed on a restricted range of scales. From a tomographic analysis of the four LRG photometric redshift bins we find that the rate of structure growth is consistent with $螞$CDM with an overall amplitude that is $\simeq5-7\%$ lower than predicted by primary CMB measurements with modest $(\sim2蟽)$ statistical significance. From the combined analysis of all four bins and their cross-correlations with Planck we obtain $S_8 = 0.765\pm0.023$, which is less discrepant with primary CMB measurements than previous DESI LRG cross Planck CMB lensing results. From the cross-correlation with ACT we obtain $S_8 = 0.790^{+0.024}_{-0.027}$, while when jointly analyzing Planck and ACT we find $S_8 = 0.775^{+0.019}_{-0.022}$ from our data alone and $蟽_8 = 0.772^{+0.020}_{-0.023}$ with the addition of BAO data. These constraints are consistent with the latest Planck primary CMB analyses at the $\simeq 1.6-2.2蟽$ level, and are in excellent agreement with galaxy lensing surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04607v1-abstract-full').style.display = 'none'; document.getElementById('2407.04607v1-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 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">60 pages, 26 figures, 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/2406.08698">arXiv:2406.08698</a> <span> [<a href="https://arxiv.org/pdf/2406.08698">pdf</a>, <a href="https://arxiv.org/format/2406.08698">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Constraints on Ultra Heavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 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="2406.08698v1-abstract-short" style="display: inline;"> In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08698v1-abstract-full').style.display = 'inline'; document.getElementById('2406.08698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.08698v1-abstract-full" style="display: none;"> In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes of astrophysical $纬$-ray background while large amount of dark matter. By analyzing more than 700 days observational data at LHAASO, no significant dark matter signal from 1 TeV to 1 EeV is detected. Accordingly we derive the most stringent constraints on the ultra-heavy dark matter annihilation cross-section up to EeV. The constraints on the lifetime of dark matter in decay mode are also derived. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08698v1-abstract-full').style.display = 'none'; document.getElementById('2406.08698v1-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 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">17 pages, 12 figures, accepted by PRL</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/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/2405.17208">arXiv:2405.17208</a> <span> [<a href="https://arxiv.org/pdf/2405.17208">pdf</a>, <a href="https://arxiv.org/format/2405.17208">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"> Impact and mitigation of spectroscopic systematics on DESI DR1 clustering measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Krolewski%2C+A">A. Krolewski</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+J">J. Yu</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=Penmetsa%2C+S">S. Penmetsa</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=Zhou%2C+R">R. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Hou%2C+J">J. Hou</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=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=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep 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=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=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=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>, <a href="/search/astro-ph?searchtype=author&query=Le-Guillou%2C+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="2405.17208v1-abstract-short" style="display: inline;"> The large scale structure catalogs within DESI Data Release 1 (DR1) use nearly 6 million galaxies and quasars as tracers of the large-scale structure of the universe to measure the expansion history with baryon acoustic oscillations and the growth of structure with redshift-space distortions. In order to take advantage of DESI's unprecedented statistical power, we must ensure that the galaxy clust… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17208v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17208v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17208v1-abstract-full" style="display: none;"> The large scale structure catalogs within DESI Data Release 1 (DR1) use nearly 6 million galaxies and quasars as tracers of the large-scale structure of the universe to measure the expansion history with baryon acoustic oscillations and the growth of structure with redshift-space distortions. In order to take advantage of DESI's unprecedented statistical power, we must ensure that the galaxy clustering measurements are unaffected by non-cosmological density fluctuations. One source of spurious fluctuations comes from variation in galaxy density with spectroscopic observing conditions, lowering the redshift efficiency (and thus galaxy density) in certain areas of the sky. We measure the uniformity of the redshift success rate for DESI luminous red galaxies (LRG), bright galaxies (BGS) and quasars (QSO), complementing the detailed discussion of emission line galaxy (ELG) systematics in a companion paper (Yu et al., 2024). We find small but significant fluctuations of up to 3% in redshift success rate with the effective spectroscopic signal-to-noise, and create and describe weights that remove these fluctuations. We also describe the process to identify and remove data from certain poorly performing fibers from DESI DR1, and measure the stability of the redshift success rate with time. Finally, we find small but significant correlations of redshift success rate with position on the focal plane, survey speed, and number of exposures required, and show the impact of weights correcting these trends on the power spectrum multipoles and on cosmological parameters from BAO and RSD fits. These corrections change the best-fit parameters by $<15\%$ of their statistical errors, and thus contribute negligibly to the overall DESI error budget. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17208v1-abstract-full').style.display = 'none'; document.getElementById('2405.17208v1-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 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">53 pages, 41 figures. Supporting paper for DESI DR1 cosmological measurements</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.16657">arXiv:2405.16657</a> <span> [<a href="https://arxiv.org/pdf/2405.16657">pdf</a>, <a href="https://arxiv.org/format/2405.16657">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"> ELG Spectroscopic Systematics Analysis of the DESI Data Release 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yu%2C+J">Jiaxi Yu</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=Rocher%2C+A">Antoine Rocher</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=Forero-S%C3%A1nchez%2C+D">Daniel Forero-S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/astro-ph?searchtype=author&query=Krolewski%2C+A">Alex Krolewski</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%2C+T">TingWen Lan</a>, <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">Michael Rashkovetskyi</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=Bailey%2C+S">Stephen Bailey</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=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=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=Honscheid%2C+K">Klaus Honscheid</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="2405.16657v6-abstract-short" style="display: inline;"> Dark Energy Spectroscopic Instrument (DESI) uses more than 2.4 million Emission Line Galaxies (ELGs) for 3D large-scale structure (LSS) analyses in its Data Release 1 (DR1). Such large statistics enable thorough research on systematic uncertainties. In this study, we focus on spectroscopic systematics of ELGs. The redshift success rate ($f_{\rm goodz}$) is the relative fraction of secure redshifts… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16657v6-abstract-full').style.display = 'inline'; document.getElementById('2405.16657v6-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.16657v6-abstract-full" style="display: none;"> Dark Energy Spectroscopic Instrument (DESI) uses more than 2.4 million Emission Line Galaxies (ELGs) for 3D large-scale structure (LSS) analyses in its Data Release 1 (DR1). Such large statistics enable thorough research on systematic uncertainties. In this study, we focus on spectroscopic systematics of ELGs. The redshift success rate ($f_{\rm goodz}$) is the relative fraction of secure redshifts among all measurements. It depends on observing conditions, thus introduces non-cosmological variations to the LSS. We, therefore, develop the redshift failure weight ($w_{\rm zfail}$) and a per-fibre correction ($畏_{\rm zfail}$) to mitigate these dependences. They have minor influences on the galaxy clustering. For ELGs with a secure redshift, there are two subtypes of systematics: 1) catastrophics (large) that only occur in a few samples; 2) redshift uncertainty (small) that exists for all samples. The catastrophics represent 0.26\% of the total DR1 ELGs, composed of the confusion between O\,\textsc{ii} and sky residuals, double objects, total catastrophics and others. We simulate the realistic 0.26\% catastrophics of DR1 ELGs, the hypothetical 1\% catastrophics, and the truncation of the contaminated $1.31<z<1.33$ in the \textsc{AbacusSummit} ELG mocks. Their $P_\ell$ show non-negligible bias from the uncontaminated mocks. But their influences on the redshift space distortions (RSD) parameters are smaller than $0.2蟽$. The redshift uncertainty of \Yone ELGs is 8.5 km/s with a Lorentzian profile. The code for implementing the catastrophics and redshift uncertainty on mocks can be found in https://github.com/Jiaxi-Yu/modelling_spectro_sys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16657v6-abstract-full').style.display = 'none'; document.getElementById('2405.16657v6-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 November, 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> </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/2405.11826">arXiv:2405.11826</a> <span> [<a href="https://arxiv.org/pdf/2405.11826">pdf</a>, <a href="https://arxiv.org/format/2405.11826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Data quality control system and long-term performance monitor of the LHAASO-KM2A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bian%2C+W">W. Bian</a>, <a href="/search/astro-ph?searchtype=author&query=Bukevich%2C+A+V">A. V. Bukevich</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H+X">H. X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a> , et al. (263 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="2405.11826v3-abstract-short" style="display: inline;"> The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic ray and gamma-ray showers. This information is used for physical analysis in gamma-ray astronomy and cosmic ray physics. To… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11826v3-abstract-full').style.display = 'inline'; document.getElementById('2405.11826v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.11826v3-abstract-full" style="display: none;"> The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic ray and gamma-ray showers. This information is used for physical analysis in gamma-ray astronomy and cosmic ray physics. To ensure the reliability of the LHAASO-KM2A data, a three-level quality control system has been established. It is used to monitor the status of detector units, stability of reconstructed parameters and the performance of the array based on observations of the Crab Nebula and Moon shadow. This paper will introduce the control system and its application on the LHAASO-KM2A data collected from August 2021 to July 2023. During this period, the pointing and angular resolution of the array were stable. From the observations of the Moon shadow and Crab Nebula, the results achieved using the two methods are consistent with each other. According to the observation of the Crab Nebula at energies from 25 TeV to 100 TeV, the time averaged pointing errors are estimated to be $-0.003^{\circ} \pm 0.005^{\circ}$ and $0.001^{\circ} \pm 0.006^{\circ}$ in the R.A. and Dec directions, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11826v3-abstract-full').style.display = 'none'; document.getElementById('2405.11826v3-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">15 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.07691">arXiv:2405.07691</a> <span> [<a href="https://arxiv.org/pdf/2405.07691">pdf</a>, <a href="https://arxiv.org/format/2405.07691">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Discovery of Very-high-energy Gamma-ray Emissions from the Low Luminosity AGN NGC 4278 by LHAASO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 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="2405.07691v1-abstract-short" style="display: inline;"> The first source catalog of Large High Altitude Air Shower Observatory reported the detection of a very-high-energy gamma ray source, 1LHAASO J1219+2915. In this paper a further detailed study of the spectral and temporal behavior of this point-like source have been carried. The best-fit position of the TeV source ($\rm{RA}=185.05^{\circ}\pm0.04^{\circ}$, $\rm{Dec}=29.25^{\circ}\pm0.03^{\circ}$) i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07691v1-abstract-full').style.display = 'inline'; document.getElementById('2405.07691v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.07691v1-abstract-full" style="display: none;"> The first source catalog of Large High Altitude Air Shower Observatory reported the detection of a very-high-energy gamma ray source, 1LHAASO J1219+2915. In this paper a further detailed study of the spectral and temporal behavior of this point-like source have been carried. The best-fit position of the TeV source ($\rm{RA}=185.05^{\circ}\pm0.04^{\circ}$, $\rm{Dec}=29.25^{\circ}\pm0.03^{\circ}$) is compatible with NGC 4278 within $\sim0.03$ degree. Variation analysis shows an indication of the variability at a few months level in the TeV band, which is consistent with low frequency observations. Based on these observations, we report the detection of TeV $纬$-ray emissions from this low-luminosity AGN NGC 4278. The observations by LHAASO-WCDA during active period has a significance level of 8.8\,$蟽$ with best-fit photon spectral index $\varGamma=2.56\pm0.14$ and a flux $f_{1-10\,\rm{TeV}}=(7.0\pm1.1_{\rm{sta}}\pm0.35_{\rm{syst}})\times10^{-13}\,\rm{photons\,cm^{-2}\,s^{-1}}$, or approximately $5\%$ of the Crab Nebula. The discovery of VHE from NGC 4278 indicates that the compact, weak radio jet can efficiently accelerate particles and emit TeV photons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07691v1-abstract-full').style.display = 'none'; document.getElementById('2405.07691v1-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 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">11 pages, 5 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/2404.18563">arXiv:2404.18563</a> <span> [<a href="https://arxiv.org/pdf/2404.18563">pdf</a>, <a href="https://arxiv.org/format/2404.18563">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Cool matter distribution in inner solar corona from 2023 total solar eclipse observation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Qu%2C+Z+Q">Z. Q. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+H">H. Su</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+Y">Y. Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Z. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R+Y">R. Y. Zhou</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="2404.18563v1-abstract-short" style="display: inline;"> Solar corona has been judged to consist of free electrons and highly ionized ions with extremely high temperature as a widely accepted knowledge. This view is changed by our eclipse observations. Distributions of cool matter represented by neutral iron atoms in hot inner solar corona are presented via derived global maps of solar Fraunhofer(F-) and Emission(E-) coronae, compared with those of cont… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18563v1-abstract-full').style.display = 'inline'; document.getElementById('2404.18563v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18563v1-abstract-full" style="display: none;"> Solar corona has been judged to consist of free electrons and highly ionized ions with extremely high temperature as a widely accepted knowledge. This view is changed by our eclipse observations. Distributions of cool matter represented by neutral iron atoms in hot inner solar corona are presented via derived global maps of solar Fraunhofer(F-) and Emission(E-) coronae, compared with those of continuum(Kontinuierlich, K-) corona formed by free electrons. The maps are obtained from simultaneous observations of dual filtering bands centered respectively at 659.4nm and 660.1nm, performed from twin telescopes during the total solar eclipse on April 20, 2023 at Com town of East Timor, assisted for judgement via spectral images obtained by a portable spectrograph. They show respectively presences of these neutral iron atoms yielding 659.3nm and 659.4nm lines in both the quiet sun and active regions. The distribution of the cool matter in form of line depression forms an inner F-corona, different from that of the cool matter in form of line enhancement. Both the distributions show a crucial difference from that of the free electrons represented by the K-corona map. It is also found that intensities of the F-corona and the E-corona induced by these neutral atoms are only small fractions of the K-corona, and the diffusion can be seen clearly in all these maps. They uncover also that the coronal heating resources do not distribute pervasively but likely form a thermodynamic griddle where minor photospheric neutral atoms can escape from the heating into the corona globally. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18563v1-abstract-full').style.display = 'none'; document.getElementById('2404.18563v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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/2404.07283">arXiv:2404.07283</a> <span> [<a href="https://arxiv.org/pdf/2404.07283">pdf</a>, <a href="https://arxiv.org/format/2404.07283">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 between Shapefit compression and Full-Modelling method with PyBird for DESI 2024 and beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lai%2C+Y">Y. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Maus%2C+M">M. Maus</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=Noriega%2C+H+E">H. E. Noriega</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Solano%2C+S">S. Ram铆rez-Solano</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=Aviles%2C+A">A. Aviles</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+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=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=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=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=Landriau%2C+M">M. Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">M. Manera</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="2404.07283v5-abstract-short" style="display: inline;"> DESI aims to provide one of the tightest constraints on cosmological parameters by analysing the clustering of more than thirty million galaxies. However, obtaining such constraints requires special care in validating the methodology and efforts to reduce the computational time required through data compression and emulation techniques. In this work, we perform a rigorous validation of the PyBird… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07283v5-abstract-full').style.display = 'inline'; document.getElementById('2404.07283v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07283v5-abstract-full" style="display: none;"> DESI aims to provide one of the tightest constraints on cosmological parameters by analysing the clustering of more than thirty million galaxies. However, obtaining such constraints requires special care in validating the methodology and efforts to reduce the computational time required through data compression and emulation techniques. In this work, we perform a rigorous validation of the PyBird power spectrum modelling code with both a traditional emulated Full-Modelling approach and the model-independent ShapeFit compression approach. By using cubic box simulations that accurately reproduce the clustering and precision of the DESI survey, we find that the cosmological constraints from ShapeFit and Full-Modelling are consistent with each other at the $\sim0.5蟽$ level for the $螞$CDM model. Both ShapeFit and Full-Modelling are also consistent with the true $螞$CDM simulation cosmology down to a scale of $k_{\mathrm{max}} = 0.20 h\mathrm{Mpc}^{-1}$ even after including the hexadecapole. For extended models such as the wCDM and the oCDM models, we find that including the hexadecapole can significantly improve the constraints and reduce the modelling errors with the same $k_{\mathrm{max}}$. While their discrepancies between the constraints from ShapeFit and Full-Modelling are more significant than $螞$CDM, they remain consistent within $0.7蟽$. Lastly, we also show that the constraints on cosmological parameters with the correlation function evaluated from PyBird down to $s_{\mathrm{min}} = 30 h^{-1} \mathrm{Mpc}$ are unbiased and consistent with the constraints from the power spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07283v5-abstract-full').style.display = 'none'; document.getElementById('2404.07283v5-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 September, 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 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars (In prep). 51 pages, 21 figures, and 12 tables. 2nd revised version for 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/2404.07272">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/2404.04801">arXiv:2404.04801</a> <span> [<a href="https://arxiv.org/pdf/2404.04801">pdf</a>, <a href="https://arxiv.org/ps/2404.04801">ps</a>, <a href="https://arxiv.org/format/2404.04801">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s41605-024-00467-8">10.1007/s41605-024-00467-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LHAASO-KM2A detector simulation using Geant4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (254 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.04801v1-abstract-short" style="display: inline;"> KM2A is one of the main sub-arrays of LHAASO, working on gamma ray astronomy and cosmic ray physics at energies above 10 TeV. Detector simulation is the important foundation for estimating detector performance and data analysis. It is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units (>6000) with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04801v1-abstract-full').style.display = 'inline'; document.getElementById('2404.04801v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04801v1-abstract-full" style="display: none;"> KM2A is one of the main sub-arrays of LHAASO, working on gamma ray astronomy and cosmic ray physics at energies above 10 TeV. Detector simulation is the important foundation for estimating detector performance and data analysis. It is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units (>6000) with large altitude difference (30 m) and huge coverage (1.3 km^2). In this paper, the design of the KM2A simulation code G4KM2A based on Geant4 is introduced. The process of G4KM2A is optimized mainly in memory consumption to avoid memory overffow. Some simpliffcations are used to signiffcantly speed up the execution of G4KM2A. The running time is reduced by at least 30 times compared to full detector simulation. The particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented, which show good agreement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04801v1-abstract-full').style.display = 'none'; document.getElementById('2404.04801v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.04248">arXiv:2404.04248</a> <span> [<a href="https://arxiv.org/pdf/2404.04248">pdf</a>, <a href="https://arxiv.org/format/2404.04248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/10.3847/2041-8213/ad5beb">10.3847/2041-8213/ad5beb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Gravitational Waves from the Coalescence of a $2.5\text{-}4.5~M_\odot$ Compact Object and a Neutron Star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%C3%A7ay%2C+S">S. Ak莽ay</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a> , et al. (1771 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="2404.04248v3-abstract-short" style="display: inline;"> We report the observation of a coalescing compact binary with component masses $2.5\text{-}4.5~M_\odot$ and $1.2\text{-}2.0~M_\odot$ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO-Virgo-KAGRA detector network on 2023 May 29 by the LIGO Livingston Observatory. The primary component of the so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04248v3-abstract-full').style.display = 'inline'; document.getElementById('2404.04248v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04248v3-abstract-full" style="display: none;"> We report the observation of a coalescing compact binary with component masses $2.5\text{-}4.5~M_\odot$ and $1.2\text{-}2.0~M_\odot$ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO-Virgo-KAGRA detector network on 2023 May 29 by the LIGO Livingston Observatory. The primary component of the source has a mass less than $5~M_\odot$ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of $55^{+127}_{-47}~\text{Gpc}^{-3}\,\text{yr}^{-1}$ for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star-black hole merger, GW230529_181500-like sources constitute about 60% of the total merger rate inferred for neutron star-black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star-black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04248v3-abstract-full').style.display = 'none'; document.getElementById('2404.04248v3-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 5 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages (10 pages author list, 13 pages main text, 1 page acknowledgements, 13 pages appendices, 8 pages bibliography), 17 figures, 16 tables. Update to match version published in The Astrophysical Journal Letters. Data products available from https://zenodo.org/records/10845779</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2300352 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 970, L34 (2024) </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/2404.03005">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/2404.03004">arXiv:2404.03004</a> <span> [<a href="https://arxiv.org/pdf/2404.03004">pdf</a>, <a href="https://arxiv.org/format/2404.03004">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Validation of the DESI 2024 Ly$伪$ forest BAO analysis using synthetic datasets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cuceu%2C+A">Andrei Cuceu</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Alcantar%2C+H+K">Hiram K. Herrera-Alcantar</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+C">Calum Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</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=Gonzalez-Morales%2C+A+X">Alma X. Gonzalez-Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</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=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</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=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=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=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.03004v2-abstract-short" style="display: inline;"> The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$伪$ (Ly$伪$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 202… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03004v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03004v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03004v2-abstract-full" style="display: none;"> The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$伪$ (Ly$伪$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 2024 Ly$伪$ forest BAO measurement. The synthetic data sets are based on Gaussian random fields using the log-normal approximation. We produce realistic synthetic DESI spectra that include all major contaminants affecting the Ly$伪$ forest. The synthetic data sets span a redshift range $1.8<z<3.8$, and are analysed using the same framework and pipeline used for the DESI 2024 Ly$伪$ forest BAO measurement. To measure BAO, we use both the Ly$伪$ auto-correlation and its cross-correlation with quasar positions. We use the mean of correlation functions from the set of DESI DR1 realizations to show that our model is able to recover unbiased measurements of the BAO position. We also fit each mock individually and study the population of BAO fits in order to validate BAO uncertainties and test our method for estimating the covariance matrix of the Ly$伪$ forest correlation functions. Finally, we discuss the implications of our results and identify the needs for the next generation of Ly$伪$ forest synthetic data sets, with the top priority being to simulate the effect of BAO broadening due to non-linear evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03004v2-abstract-full').style.display = 'none'; document.getElementById('2404.03004v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Supporting publication of DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03002">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/2403.10010">arXiv:2403.10010</a> <span> [<a href="https://arxiv.org/pdf/2403.10010">pdf</a>, <a href="https://arxiv.org/format/2403.10010">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.132.131002">10.1103/PhysRevLett.132.131002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of All-Particle Energy Spectrum and Mean Logarithmic Mass of Cosmic Rays from 0.3 to 30 PeV with LHAASO-KM2A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LHAASO+Collaboration"> The LHAASO Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu%2C+A">A. Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a> , et al. (256 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="2403.10010v2-abstract-short" style="display: inline;"> We present the measurements of all-particle energy spectrum and mean logarithmic mass of cosmic rays in the energy range of 0.3-30 PeV using data collected from LHAASO-KM2A between September 2021 and December 2022, which is based on a nearly composition-independent energy reconstruction method, achieving unprecedented accuracy. Our analysis reveals the position of the knee at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10010v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10010v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10010v2-abstract-full" style="display: none;"> We present the measurements of all-particle energy spectrum and mean logarithmic mass of cosmic rays in the energy range of 0.3-30 PeV using data collected from LHAASO-KM2A between September 2021 and December 2022, which is based on a nearly composition-independent energy reconstruction method, achieving unprecedented accuracy. Our analysis reveals the position of the knee at $3.67 \pm 0.05 \pm 0.15$ PeV. Below the knee, the spectral index is found to be -$2.7413 \pm 0.0004 \pm 0.0050$, while above the knee, it is -$3.128 \pm 0.005 \pm 0.027$, with the sharpness of the transition measured with a statistical error of 2%. The mean logarithmic mass of cosmic rays is almost heavier than helium in the whole measured energy range. It decreases from 1.7 at 0.3 PeV to 1.3 at 3 PeV, representing a 24% decline following a power law with an index of -$0.1200 \pm 0.0003 \pm 0.0341$. This is equivalent to an increase in abundance of light components. Above the knee, the mean logarithmic mass exhibits a power law trend towards heavier components, which is reversal to the behavior observed in the all-particle energy spectrum. Additionally, the knee position and the change in power-law index are approximately the same. These findings suggest that the knee observed in the all-particle spectrum corresponds to the knee of the light component, rather than the medium-heavy components. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10010v2-abstract-full').style.display = 'none'; document.getElementById('2403.10010v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">8 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physical Review Letters 132, 131002 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.03004">arXiv:2403.03004</a> <span> [<a href="https://arxiv.org/pdf/2403.03004">pdf</a>, <a href="https://arxiv.org/format/2403.03004">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Ultralight vector dark matter search using data from the KAGRA O3GK run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adamcewicz%2C+C">C. Adamcewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a> , et al. (1778 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="2403.03004v1-abstract-short" style="display: inline;"> Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we prese… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03004v1-abstract-full').style.display = 'inline'; document.getElementById('2403.03004v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.03004v1-abstract-full" style="display: none;"> Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for $U(1)_{B-L}$ gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the $U(1)_{B-L}$ gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03004v1-abstract-full').style.display = 'none'; document.getElementById('2403.03004v1-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 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">20 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2300250 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.17099">arXiv:2402.17099</a> <span> [<a href="https://arxiv.org/pdf/2402.17099">pdf</a>, <a href="https://arxiv.org/format/2402.17099">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202347312">10.1051/0004-6361/202347312 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fermi-LAT view of the changing-look blazar OQ 334 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ren%2C+S+S">S. S. Ren</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R+X">R. X. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y+G">Y. G. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kang%2C+S+J">S. J. Kang</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q">Q. Wu</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="2402.17099v1-abstract-short" style="display: inline;"> Context.Unusually, there are still certain characteristics of the changing-look (CL) active galactic nuclei (AGNs) that remain undetected.Consequently,the trigger mechanism behind the CL phenomenon observed in partial AGNs remains unknown.Aims.We explore the light curve and spectral energy distribution (SED) of the CL blazar OQ 334 as obtained by Fermi-LAT. Methods. By examining the variability of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17099v1-abstract-full').style.display = 'inline'; document.getElementById('2402.17099v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.17099v1-abstract-full" style="display: none;"> Context.Unusually, there are still certain characteristics of the changing-look (CL) active galactic nuclei (AGNs) that remain undetected.Consequently,the trigger mechanism behind the CL phenomenon observed in partial AGNs remains unknown.Aims.We explore the light curve and spectral energy distribution (SED) of the CL blazar OQ 334 as obtained by Fermi-LAT. Methods. By examining the variability of the equivalent width (EW), we categorise the Fermi-LAT light curves of OQ 334 during the epoch of MJD 54628-58677 into seven distinct epochs, including the flat spectrum radio quasar (FSRQ) state, the transition state, and the BL Lac state. We obtained both a Fermi-LAT SED and a multi-wavelength SED for each of these distinct epochs. Results. The source exhibits a transformation from a quiescent state to a highly active state, as evidenced by the variability of the EW. The multi-wavelength SEDs display a prominent external Compton characteristic, even though the Fermi-LAT SED reveals both a FSRQ and a BL Lac state across the seven different epochs. To gain further insights, we employed a leptonic model that takes into account the soft photon fields originating from both synchrotron radiation and the external environment. By simulating the multi-wavelength SEDs for each epoch, we uncover the following results. Firstly, the energy density of the external photon fields evolves in an oscillatory manner over the seven different epochs. Also, the energy density of the external photon fields in the BL Lac state is lower than that in the FSRQ state.Conclusions. These findings suggest that the CL blazar represents a unique phase in the blazar sequence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17099v1-abstract-full').style.display = 'none'; document.getElementById('2402.17099v1-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 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">Accepted for publication in A&A. 12 pages, 5 figures, 4 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 685, A140 (2024) </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/2401.11970">arXiv:2401.11970</a> <span> [<a href="https://arxiv.org/pdf/2401.11970">pdf</a>, <a href="https://arxiv.org/format/2401.11970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1674-4527/ad06f2">10.1088/1674-4527/ad06f2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Correcting the Contamination of Second-order Spectra: Improving H伪 Measurements in Reverberation Mapping Campaigns </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xi%2C+W">Wen-Zhe Xi</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+K">Kai-Xing Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Hai-Cheng Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Sha-Sha Li</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+J">Jin-Ming Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rui-Lei Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">Hong-Tao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jian-Guo 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="2401.11970v1-abstract-short" style="display: inline;"> Long-term spectroscopic monitoring campaigns on active galactic nuclei (AGNs) provide a wealth of information about its interior structure and kinematics. However, a number of the observations suffer from the contamination of second-order spectra (SOS) which will introduce some undesirable uncertainties at the red side of the spectra. In this paper, we test the effect of SOS and propose a method t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11970v1-abstract-full').style.display = 'inline'; document.getElementById('2401.11970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11970v1-abstract-full" style="display: none;"> Long-term spectroscopic monitoring campaigns on active galactic nuclei (AGNs) provide a wealth of information about its interior structure and kinematics. However, a number of the observations suffer from the contamination of second-order spectra (SOS) which will introduce some undesirable uncertainties at the red side of the spectra. In this paper, we test the effect of SOS and propose a method to correct it in the time domain spectroscopic data using the simultaneously observed comparison stars. Based on the reverberation mapping (RM) data of NGC 5548 in 2019, one of the most intensively monitored AGNs by the Lijiang 2.4 m telescope, we find that the scientific object, comparison star, and spectrophotometric standard star can jointly introduce up to similar to 30% SOS for Grism 14. This irregular but smooth SOS significantly affects the flux density and profile of the emission line, while having little effect on the light curve. After applying our method to each spectrum, we find that the SOS can be corrected effectively. The deviation between corrected and intrinsic spectra is similar to 2%, and the impact of SOS on time lag is very minor. This method makes it possible to obtain the H alpha RM measurements from archival data provided that the spectral shape of the AGN under investigation does not have a large change. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11970v1-abstract-full').style.display = 'none'; document.getElementById('2401.11970v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res.Astron.Astrophys.23(2023)125021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.11794">arXiv:2401.11794</a> <span> [<a href="https://arxiv.org/pdf/2401.11794">pdf</a>, <a href="https://arxiv.org/format/2401.11794">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Exploring the Impact of Dissipation Coefficient in Warm Higgs Inflation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+W">Wei Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xue-Wen Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Ruiyu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Jiu-Jiang Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+X">Xin-Rui Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zi-Han Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Qin%2C+T">Tong Qin</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="2401.11794v1-abstract-short" style="display: inline;"> In this study, we conducted a detailed analysis of the core parameter of Warm Higgs Inflation (WHI) $-$ the dissipation coefficient ($Q$). As a crucial parameter in the warm inflation process, $Q$ exerts profound influences on the entire evolutionary process. By meticulously deriving the relationships between various quantities and $Q$, we successfully circumvented the common preconceptions regard… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11794v1-abstract-full').style.display = 'inline'; document.getElementById('2401.11794v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11794v1-abstract-full" style="display: none;"> In this study, we conducted a detailed analysis of the core parameter of Warm Higgs Inflation (WHI) $-$ the dissipation coefficient ($Q$). As a crucial parameter in the warm inflation process, $Q$ exerts profound influences on the entire evolutionary process. By meticulously deriving the relationships between various quantities and $Q$, we successfully circumvented the common preconceptions regarding strong and weak dissipation, laying the foundation for a more accurate exploration of their interconnections. Taking into account the constraints imposed by Cosmic Microwave Background, we observed that the dissipation coefficient $Q$ remains at extremely low levels throughout the entire warm inflation process, i.e., $Q \ll 1$. This observation indicates that WHI falls under the category of weakly dissipative warm inflation. Despite being weakly dissipative, $Q$ still plays a crucial role in the evolution of temperature, energy, and other quantities, highlighting its significance and non-negligibility. We delved deeper into the impact of the primordial power spectrum on the dissipation coefficient $Q$ during the warm inflation process, discovering that the dependency is not significant. Consequently, this naturally leads to the unobtrusive dependence of the gravitational wave power spectrum on $Q$. Finally, we found that gravitational waves generated by WHI hold the potential for verification in future observational experiments, especially through the SKA100 experiment. These findings provide a theoretical support for a more profound understanding of the early evolution of the universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11794v1-abstract-full').style.display = 'none'; document.getElementById('2401.11794v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 5 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/2310.17082">arXiv:2310.17082</a> <span> [<a href="https://arxiv.org/pdf/2310.17082">pdf</a>, <a href="https://arxiv.org/ps/2310.17082">ps</a>, <a href="https://arxiv.org/format/2310.17082">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Does or did the supernova remnant Cassiopeia A operate as a PeVatron? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 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="2310.17082v1-abstract-short" style="display: inline;"> For decades, supernova remnants (SNRs) have been considered the prime sources of Galactic Cosmic rays (CRs). But whether SNRs can accelerate CR protons to PeV energies and thus dominate CR flux up to the knee is currently under intensive theoretical and phenomenological debate. The direct test of the ability of SNRs to operate as CR PeVatrons can be provided by ultrahigh-energy (UHE;… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17082v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17082v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17082v1-abstract-full" style="display: none;"> For decades, supernova remnants (SNRs) have been considered the prime sources of Galactic Cosmic rays (CRs). But whether SNRs can accelerate CR protons to PeV energies and thus dominate CR flux up to the knee is currently under intensive theoretical and phenomenological debate. The direct test of the ability of SNRs to operate as CR PeVatrons can be provided by ultrahigh-energy (UHE; $E_纬\geq 100$~TeV) $纬$-rays. In this context, the historical SNR Cassiopeia A (Cas A) is considered one of the most promising target for UHE observations. This paper presents the observation of Cas A and its vicinity by the LHAASO KM2A detector. The exceptional sensitivity of LHAASO KM2A in the UHE band, combined with the young age of Cas A, enabled us to derive stringent model-independent limits on the energy budget of UHE protons and nuclei accelerated by Cas A at any epoch after the explosion. The results challenge the prevailing paradigm that Cas A-type SNRs are major suppliers of PeV CRs in the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17082v1-abstract-full').style.display = 'none'; document.getElementById('2310.17082v1-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, 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">11 pages, 3 figures, Accepted by the APJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12458">arXiv:2310.12458</a> <span> [<a href="https://arxiv.org/pdf/2310.12458">pdf</a>, <a href="https://arxiv.org/format/2310.12458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Confirmation of a Sub-Saturn-size transiting exoplanet orbiting a G dwarf: TOI-1194 b and a very low mass companion star: TOI-1251 B from TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jia-Qi Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+X">Xiao-Jun Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+J">Jie Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kellermann%2C+H">Hanna Kellermann</a>, <a href="/search/astro-ph?searchtype=author&query=Riffeser%2C+A">Arno Riffeser</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Liang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Bieryla%2C+A">Allyson Bieryla</a>, <a href="/search/astro-ph?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+S+B">Steve B. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Furlan%2C+E">Elise Furlan</a>, <a href="/search/astro-ph?searchtype=author&query=Girardin%2C+E">Eric Girardin</a>, <a href="/search/astro-ph?searchtype=author&query=Gregorio%2C+J">Joao Gregorio</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+E">Eric Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Murgas%2C+F">Felipe Murgas</a>, <a href="/search/astro-ph?searchtype=author&query=Yilmaz%2C+M">Mesut Yilmaz</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+S">Sam Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+X">Xing Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Ruo-Yu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Grupp%2C+F">Frank Grupp</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hui-Juan 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="2310.12458v2-abstract-short" style="display: inline;"> We report the confirmation of a sub-Saturn-size exoplanet, TOI-1194 b with a mass about $0.456_{-0.051}^{+0.055}$ $M_{J}$, and a very low mass companion star with a mass of about $96.5\pm1.5$ $M_J$, TOI-1251 B. Exoplanet candidates provided by the Transiting Exoplanet Survey Satellite (TESS) are suitable for further follow-up observations by ground-based telescopes with small and medium apertures.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12458v2-abstract-full').style.display = 'inline'; document.getElementById('2310.12458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12458v2-abstract-full" style="display: none;"> We report the confirmation of a sub-Saturn-size exoplanet, TOI-1194 b with a mass about $0.456_{-0.051}^{+0.055}$ $M_{J}$, and a very low mass companion star with a mass of about $96.5\pm1.5$ $M_J$, TOI-1251 B. Exoplanet candidates provided by the Transiting Exoplanet Survey Satellite (TESS) are suitable for further follow-up observations by ground-based telescopes with small and medium apertures. The analysis is performed based on data from several telescopes worldwide, including telescopes in the Sino-German multiband photometric campaign, which aimed at confirming TESS Objects of Interest (TOIs) using ground-based small-aperture and medium-aperture telescopes, especially for long-period targets. TOI-1194 b is confirmed based on the consistent periodic transits depths from the multiband photometric data. We measure an orbital period of $2.310644\pm0.000001$ d, and radius is $0.767_{-0.041}^{+0.045}$ $R_J$, and amplitude of RV curve is $69.4_{-7.3}^{+7.9}$ m/s. TOI-1251 B is confirmed based on the multiband photometric and high-resolution spectroscopic data, whose orbiting period is $5.963054_{-0.000001}^{+0.000002}$ d, the radius is $0.947_{-0.033}^{+0.035}$ $R_J$, and amplitude of RV curve is $9849_{-40}^{+42}$ m/s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12458v2-abstract-full').style.display = 'none'; document.getElementById('2310.12458v2-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> 20 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 8 figures, Accepted by RAA on Oct. 18th, 2023</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Zhou%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Zhou%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Zhou%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Zhou%2C+R&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Zhou%2C+R&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" 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