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start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.07970">arXiv:2411.07970</a> <span> [<a href="https://arxiv.org/pdf/2411.07970">pdf</a>, <a href="https://arxiv.org/format/2411.07970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> MUltiplexed Survey Telescope: Perspectives for Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zhao%2C+C">Cheng Zhao</a>, <a href="/search/?searchtype=author&query=Huang%2C+S">Song Huang</a>, <a href="/search/?searchtype=author&query=He%2C+M">Mengfan He</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Liu%2C+Y">Yu Liu</a>, <a href="/search/?searchtype=author&query=Renard%2C+P">Pablo Renard</a>, <a href="/search/?searchtype=author&query=Tang%2C+Y">Yunyi Tang</a>, <a href="/search/?searchtype=author&query=Verdier%2C+A">Aurelien Verdier</a>, <a href="/search/?searchtype=author&query=Xu%2C+W">Wenshuo Xu</a>, <a href="/search/?searchtype=author&query=Yang%2C+X">Xiaorui Yang</a>, <a href="/search/?searchtype=author&query=Yu%2C+J">Jiaxi Yu</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Yao Zhang</a>, <a href="/search/?searchtype=author&query=Zhao%2C+S">Siyi Zhao</a>, <a href="/search/?searchtype=author&query=Zhou%2C+X">Xingchen Zhou</a>, <a href="/search/?searchtype=author&query=He%2C+S">Shengyu He</a>, <a href="/search/?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/?searchtype=author&query=Li%2C+J">Jiayi Li</a>, <a href="/search/?searchtype=author&query=Li%2C+Z">Zhuoyang Li</a>, <a href="/search/?searchtype=author&query=Wang%2C+W">Wen-Ting Wang</a>, <a href="/search/?searchtype=author&query=Xianyu%2C+Z">Zhong-Zhi Xianyu</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Yidian Zhang</a>, <a href="/search/?searchtype=author&query=Gsponer%2C+R">Rafaela Gsponer</a>, <a href="/search/?searchtype=author&query=Li%2C+X">Xiao-Dong Li</a>, <a href="/search/?searchtype=author&query=Rocher%2C+A">Antoine Rocher</a>, <a href="/search/?searchtype=author&query=Zou%2C+S">Siwei Zou</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="2411.07970v2-abstract-short" style="display: inline;"> The MUltiplexed Survey Telescope (MUST) is a 6.5-meter telescope under development. Dedicated to highly-multiplexed, wide-field spectroscopic surveys, MUST observes over 20,000 targets simultaneously using 6.2-mm pitch positioning robots within a ~5 deg2 field of view. MUST aims to carry out the first Stage-V spectroscopic survey in the 2030s to map the 3D Universe with over 100 million galaxies a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07970v2-abstract-full').style.display = 'inline'; document.getElementById('2411.07970v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07970v2-abstract-full" style="display: none;"> The MUltiplexed Survey Telescope (MUST) is a 6.5-meter telescope under development. Dedicated to highly-multiplexed, wide-field spectroscopic surveys, MUST observes over 20,000 targets simultaneously using 6.2-mm pitch positioning robots within a ~5 deg2 field of view. MUST aims to carry out the first Stage-V spectroscopic survey in the 2030s to map the 3D Universe with over 100 million galaxies and quasars, spanning from the nearby Universe to redshift z~5.5, corresponding to around 1 billion years after the Big Bang. To cover this extensive redshift range, we present an initial conceptual target selection algorithm for different types of galaxies, from local bright galaxies, luminous red galaxies, and emission line galaxies to high-redshift (2 < z < 5.5) Lyman-break galaxies. Using Fisher forecasts, we demonstrate that MUST can address fundamental questions in cosmology, including the nature of dark energy, test of gravity theories, and investigations into primordial physics. This is the first paper in the series of science white papers for MUST, with subsequent developments focusing on additional scientific cases such as galaxy and quasar evolution, Milky Way physics, and dynamic phenomena in the time-domain Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07970v2-abstract-full').style.display = 'none'; document.getElementById('2411.07970v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">To be submitted to SCPMA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.19390">arXiv:2410.19390</a> <span> [<a href="https://arxiv.org/pdf/2410.19390">pdf</a>, <a href="https://arxiv.org/format/2410.19390">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</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/10.1051/0004-6361/202449113">10.1051/0004-6361/202449113 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLAP. I. Resolving miscalibration for deep learning-based galaxy photometric redshift estimation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lin%2C+Q">Qiufan Lin</a>, <a href="/search/?searchtype=author&query=Ruan%2C+H">Hengxin Ruan</a>, <a href="/search/?searchtype=author&query=Fouchez%2C+D">Dominique Fouchez</a>, <a href="/search/?searchtype=author&query=Chen%2C+S">Shupei Chen</a>, <a href="/search/?searchtype=author&query=Li%2C+R">Rui Li</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/?searchtype=author&query=Ting%2C+Y">Yuan-Sen Ting</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W">Wei 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="2410.19390v1-abstract-short" style="display: inline;"> Obtaining well-calibrated photometric redshift probability densities for galaxies without a spectroscopic measurement remains a challenge. Deep learning discriminative models, typically fed with multi-band galaxy images, can produce outputs that mimic probability densities and achieve state-of-the-art accuracy. However, such models may be affected by miscalibration that would result in discrepanci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19390v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19390v1-abstract-full" style="display: none;"> Obtaining well-calibrated photometric redshift probability densities for galaxies without a spectroscopic measurement remains a challenge. Deep learning discriminative models, typically fed with multi-band galaxy images, can produce outputs that mimic probability densities and achieve state-of-the-art accuracy. However, such models may be affected by miscalibration that would result in discrepancies between the model outputs and the actual distributions of true redshifts. Our work develops a novel method called the Contrastive Learning and Adaptive KNN for Photometric Redshift (CLAP) that resolves this issue. It leverages supervised contrastive learning (SCL) and k-nearest neighbours (KNN) to construct and calibrate raw probability density estimates, and implements a refitting procedure to resume end-to-end discriminative models ready to produce final estimates for large-scale imaging data. The harmonic mean is adopted to combine an ensemble of estimates from multiple realisations for improving accuracy. Our experiments demonstrate that CLAP takes advantage of both deep learning and KNN, outperforming benchmark methods on the calibration of probability density estimates and retaining high accuracy and computational efficiency. With reference to CLAP, we point out that miscalibration is particularly sensitive to the method-induced excessive correlations among data instances in addition to the unaccounted-for epistemic uncertainties. Reducing the uncertainties may not guarantee the removal of miscalibration due to the presence of such excessive correlations, yet this is a problem for conventional deep learning methods rather than CLAP. These discussions underscore the robustness of CLAP for obtaining photometric redshift probability densities required by astrophysical and cosmological applications. This is the first paper in our series on CLAP. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19390v1-abstract-full').style.display = 'none'; document.getElementById('2410.19390v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 + 6 pages, 9 + 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/2409.11613">arXiv:2409.11613</a> <span> [<a href="https://arxiv.org/pdf/2409.11613">pdf</a>, <a href="https://arxiv.org/format/2409.11613">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"> Reionization relics in the cross-correlation between the Ly$伪$ forest and 21 cm intensity mapping in the post-reionization era </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Morales-Guti%C3%A9rrez%2C+C">Catalina Morales-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Yao Zhang</a>, <a href="/search/?searchtype=author&query=Long%2C+H">Heyang Long</a>, <a href="/search/?searchtype=author&query=Mao%2C+Y">Yi Mao</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="2409.11613v1-abstract-short" style="display: inline;"> The tumultuous effects of ultraviolet photons that source cosmic reionization, the subsequent compression and shock-heating of low-density regions, and the modulation of baryons in shallow potential wells induced by the passage of ionization fronts, collectively introduce perturbations to the evolution of the intergalactic medium in the post-reionization era. These enduring fluctuations persist de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.11613v1-abstract-full').style.display = 'inline'; document.getElementById('2409.11613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.11613v1-abstract-full" style="display: none;"> The tumultuous effects of ultraviolet photons that source cosmic reionization, the subsequent compression and shock-heating of low-density regions, and the modulation of baryons in shallow potential wells induced by the passage of ionization fronts, collectively introduce perturbations to the evolution of the intergalactic medium in the post-reionization era. These enduring fluctuations persist deep into the post-reionization era, casting a challenge upon precision cosmology endeavors targeting tracers in this cosmic era. Simultaneously, these relics from reionization also present a unique opportunity to glean insights into the astrophysics that govern the epoch of reionization. In this work, we propose a first study of the cross-correlation of \lya forest and 21 cm intensity mapping, accounting for the repercussions of inhomogeneous reionization in the post-reionization era. We investigate the ability of SKA $\times$ DESI-like, SKA $\times$ MUST-like, and PUMA $\times$ MUST-like instrumental setups to achieve a high signal-to-noise ratio (SNR) in the redshift range $3.5 \leq z \leq 4$. Moreover, we assess how alterations in integration time, survey area, and reionization scenarios impact the SNR. Furthermore, we forecast the cross-correlation's potential to constrain cosmological parameters under varying assumptions: considering or disregarding reionization relics, marginalizing over reionization astrophysics, and assuming perfect knowledge of reionization. Notably, our findings underscore the remarkable capability of a futuristic PUMA $\times$ MUST-like setup, with a modest 100-hour integration time over a 100 sq. deg. survey, to constrain the ionization efficiency error to $蟽_味= 3.42 $. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.11613v1-abstract-full').style.display = 'none'; document.getElementById('2409.11613v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Comments welcome! (16 pages, 10 figures)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18775">arXiv:2406.18775</a> <span> [<a href="https://arxiv.org/pdf/2406.18775">pdf</a>, <a href="https://arxiv.org/format/2406.18775">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Probing the cosmic web in Ly$伪$ emission over large scales: an Intensity Mapping forecast for DECaLS/BASS and DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Renard%2C+P">Pablo Renard</a>, <a href="/search/?searchtype=author&query=Spinoso%2C+D">Daniele Spinoso</a>, <a href="/search/?searchtype=author&query=Sun%2C+Z">Zechang Sun</a>, <a href="/search/?searchtype=author&query=Zou%2C+H">Hu Zou</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Cai%2C+Z">Zheng Cai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.18775v1-abstract-short" style="display: inline;"> Being the most prominent HI line, Ly$伪$ permeates the cosmic web in emission. Despite its potential as a cosmological probe, its detection on large scales remains elusive. We present a new methodology to perform Ly$伪$ intensity mapping with broad-band optical images, by cross-correlating them with Ly$伪$ forest data using a custom one-parameter estimator. We also develop an analytical large-scale L… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18775v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18775v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18775v1-abstract-full" style="display: none;"> Being the most prominent HI line, Ly$伪$ permeates the cosmic web in emission. Despite its potential as a cosmological probe, its detection on large scales remains elusive. We present a new methodology to perform Ly$伪$ intensity mapping with broad-band optical images, by cross-correlating them with Ly$伪$ forest data using a custom one-parameter estimator. We also develop an analytical large-scale Ly$伪$ emission model with two parameters (average luminosity $\langle L_{\rm Ly伪} \rangle$ and bias $b_{\rm e}$) that respects observational constraints from QSO luminosity functions. We compute a forecast for DECaLS/BASS $g$-band images cross-correlated with DESI Ly$伪$ forest data, setting guidelines for reducing images into Ly$伪$ intensity maps. Given the transversal scales of our cross-correlation (26.4 arcmin, $\sim$33 cMpc/h), our study effectively integrates Ly$伪$ emission over all the cosmic volume inside the DESI footprint at $2.2 < z < 3.4$ (the $g$-band Ly$伪$ redshift range). Over the parameter space ($\langle L_{\rm Ly伪} \rangle$, $b_{\rm e}$) sampled by our forecast, we find a 3$蟽$ of large-scale structure in Ly$伪$ likely, with a probability of detection of 23.95\% for DESI-DECaLS/BASS, and 54.93\% for a hypothetical DESI phase II with twice as much Ly$伪$ QSOs. Without a detection, we derive upper bounds on $\langle L_{\rm Ly伪} \rangle$ competitive with optimistic literature estimates ($2.3 \pm 1 \cdot 10^{\rm 41}$ erg/s/cMpc$^3$ for DESI, and $\sim$35\% lower for its hypothetical phase II). Extrapolation to the DESI-Rubin overlap shows that a detection of large-scale structure with Ly$伪$ intensity mapping using next-generation imaging surveys is certain. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18775v1-abstract-full').style.display = 'none'; document.getElementById('2406.18775v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">26 pages, 24 figures, submitted to MNRAS. Comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13680">arXiv:2405.13680</a> <span> [<a href="https://arxiv.org/pdf/2405.13680">pdf</a>, <a href="https://arxiv.org/format/2405.13680">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"> Five parameters are all you need (in $螞$CDM) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Li%2C+Y">Yin Li</a>, <a href="/search/?searchtype=author&query=Cranmer%2C+M">Miles Cranmer</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13680v2-abstract-short" style="display: inline;"> The standard cosmological model, with its six independent parameters, successfully describes our observable Universe. One of these parameters, the optical depth to reionization $蟿_\mathrm{reio}$, represents the scatterings that Cosmic Microwave Background (CMB) photons will experience after decoupling from the primordial plasma as the intergalactic medium transitions from neutral to ionized.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13680v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13680v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13680v2-abstract-full" style="display: none;"> The standard cosmological model, with its six independent parameters, successfully describes our observable Universe. One of these parameters, the optical depth to reionization $蟿_\mathrm{reio}$, represents the scatterings that Cosmic Microwave Background (CMB) photons will experience after decoupling from the primordial plasma as the intergalactic medium transitions from neutral to ionized. $蟿_\mathrm{reio}$ depends on the neutral hydrogen fraction $x_\mathrm{HI}$, which, in turn, should theoretically depend on cosmology. We present a novel method to establish the missing link between cosmology and reionization timeline using symbolic regression. We discover the timeline has a universal shape well described by the Gompertz mortality law, applicable to any cosmology within our simulated data. Unlike the conventional tanh prescription, our model is asymmetric in time and a good fit to astrophysical constraints on $x_\mathrm{HI}$. By combining CMB with astrophysical data and marginalizing over astrophysics, we treat $蟿_\mathrm{reio}$ as a derived parameter, tightening its constraint to $<3\%$. This approach reduces the error on the amplitude of the primordial fluctuations by a factor of 2.3 compared to Planck's PR3 constraint and provides a commanding constraint on the ionization efficiency $味_\mathrm{UV} = 26.9^{+2.1}_{-2.5}$. We expect further improvements in the near term as reionization constraints increase and our understanding of reionization advances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13680v2-abstract-full').style.display = 'none'; document.getElementById('2405.13680v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Correctly accounting for ionization efficiency enables us to place leading constraints by combining our universal asymmetric reionization model with CMB and damping wing constraints on $x_\mathrm{HI}$. By marginalizing over $味_\mathrm{UV}$, we achieve powerful constraints on $A_\mathrm{s}$ and $蟿_\mathrm{reio}$, with uncertainties around 3% for the former</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.09737">arXiv:2405.09737</a> <span> [<a href="https://arxiv.org/pdf/2405.09737">pdf</a>, <a href="https://arxiv.org/format/2405.09737">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 Lyman Alpha Forest BAL Masking Strategy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=Ennesser%2C+L">L. Ennesser</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+Belsunce%2C+R">R. de Belsunce</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/?searchtype=author&query=Lambert%2C+A">A. Lambert</a>, <a href="/search/?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a>, <a href="/search/?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/?searchtype=author&query=Meisner%2C+A">A. Meisner</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.09737v2-abstract-short" style="display: inline;"> Broad absorption line quasars (BALs) exhibit blueshifted absorption relative to a number of their prominent broad emission features. These absorption features can contribute to quasar redshift errors and add absorption to the Lyman-alpha (LyA) forest that is unrelated to large-scale structure. We present a detailed analysis of the impact of BALs on the Baryon Acoustic Oscillation (BAO) results wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09737v2-abstract-full').style.display = 'inline'; document.getElementById('2405.09737v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.09737v2-abstract-full" style="display: none;"> Broad absorption line quasars (BALs) exhibit blueshifted absorption relative to a number of their prominent broad emission features. These absorption features can contribute to quasar redshift errors and add absorption to the Lyman-alpha (LyA) forest that is unrelated to large-scale structure. We present a detailed analysis of the impact of BALs on the Baryon Acoustic Oscillation (BAO) results with the LyA forest from the first year of data from the Dark Energy Spectroscopic Instrument (DESI). The baseline strategy for the first year analysis is to mask all pixels associated with all BAL absorption features that fall within the wavelength region used to measure the forest. We explore a range of alternate masking strategies and demonstrate that these changes have minimal impact on the BAO measurements with both DESI data and synthetic data. This includes when we mask the BAL features associated with emission lines outside of the forest region to minimize their contribution to redshift errors. We identify differences in the properties of BALs in the synthetic datasets relative to the observational data, as well as use the synthetic observations to characterize the completeness of the BAL identification algorithm, and demonstrate that incompleteness and differences in the BALs between real and synthetic data also do not impact the BAO results for the LyA forest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09737v2-abstract-full').style.display = 'none'; document.getElementById('2405.09737v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">32 pages, 8 figures, accepted by JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03003">arXiv:2404.03003</a> <span> [<a href="https://arxiv.org/pdf/2404.03003">pdf</a>, <a href="https://arxiv.org/format/2404.03003">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Characterization of contaminants in the Lyman-alpha forest auto-correlation with DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Guti%C3%A9rrez%2C+A">A. Mu帽oz-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Pieri%2C+M">M. Pieri</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C. Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">M. Walther</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a> , et al. (39 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.03003v4-abstract-short" style="display: inline;"> Baryon Acoustic Oscillations can be measured with sub-percent precision above redshift two with the Lyman-alpha forest auto-correlation and its cross-correlation with quasar positions. This is one of the key goals of the Dark Energy Spectroscopic Instrument (DESI) which started its main survey in May 2021. We present in this paper a study of the contaminants to the lyman-alpha forest which are mai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03003v4-abstract-full').style.display = 'inline'; document.getElementById('2404.03003v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03003v4-abstract-full" style="display: none;"> Baryon Acoustic Oscillations can be measured with sub-percent precision above redshift two with the Lyman-alpha forest auto-correlation and its cross-correlation with quasar positions. This is one of the key goals of the Dark Energy Spectroscopic Instrument (DESI) which started its main survey in May 2021. We present in this paper a study of the contaminants to the lyman-alpha forest which are mainly caused by correlated signals introduced by the spectroscopic data processing pipeline as well as astrophysical contaminants due to foreground absorption in the intergalactic medium. Notably, an excess signal caused by the sky background subtraction noise is present in the lyman-alpha auto-correlation in the first line-of-sight separation bin. We use synthetic data to isolate this contribution, we also characterize the effect of spectro-photometric calibration noise, and propose a simple model to account for both effects in the analysis of the lyman-alpha forest. We then measure the auto-correlation of the quasar flux transmission fraction of low redshift quasars, where there is no lyman-alpha forest absorption but only its contaminants. We demonstrate that we can interpret the data with a two-component model: data processing noise and triply ionized Silicon and Carbon auto-correlations. This result can be used to improve the modeling of the lyman-alpha auto-correlation function measured with DESI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03003v4-abstract-full').style.display = 'none'; document.getElementById('2404.03003v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18009">arXiv:2402.18009</a> <span> [<a href="https://arxiv.org/pdf/2402.18009">pdf</a>, <a href="https://arxiv.org/format/2402.18009">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Impact of Systematic Redshift Errors on the Cross-correlation of the Lyman-$伪$ Forest with Quasars at Small Scales Using DESI Early Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bault%2C+A">Abby Bault</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">Allyson Brodzeller</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Filbert%2C+S">S. Filbert</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">C. Gordon</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.18009v2-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) will measure millions of quasar spectra by the end of its 5 year survey. Quasar redshift errors impact the shape of the Lyman-$伪$ forest correlation functions, which can affect cosmological analyses and therefore cosmological interpretations. Using data from the DESI Early Data Release and the first two months of the main survey, we measure the syste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18009v2-abstract-full').style.display = 'inline'; document.getElementById('2402.18009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18009v2-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) will measure millions of quasar spectra by the end of its 5 year survey. Quasar redshift errors impact the shape of the Lyman-$伪$ forest correlation functions, which can affect cosmological analyses and therefore cosmological interpretations. Using data from the DESI Early Data Release and the first two months of the main survey, we measure the systematic redshift error from an offset in the cross-correlation of the Lyman-$伪$ forest with quasars. We find evidence for a redshift dependent bias causing redshifts to be underestimated with increasing redshift, stemming from improper modeling of the Lyman-$伪$ optical depth in the templates used for redshift estimation. New templates were derived for the DESI Year 1 quasar sample at $z > 1.6$ and we found the redshift dependent bias, $螖r_\parallel$, increased from $-1.94 \pm 0.15$ $h^{-1}$ Mpc to $-0.08 \pm 0.04$ $h^{-1}$ Mpc ($-205 \pm 15~\text{km s}^{-1}$ to $-9.0 \pm 4.0~\text{km s}^{-1}$). These new templates will be used to provide redshifts for the DESI Year 1 quasar sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18009v2-abstract-full').style.display = 'none'; document.getElementById('2402.18009v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 9 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.00303">arXiv:2401.00303</a> <span> [<a href="https://arxiv.org/pdf/2401.00303">pdf</a>, <a href="https://arxiv.org/format/2401.00303">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Synthetic spectra for Lyman-$伪$ forest analysis in the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">Hiram K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Guti%C3%A9rrez%2C+A">Andrea Mu帽oz-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">Ting Tan</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Morales%2C+A+X">Alma X. Gonz谩lez-Morales</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+L+%C3%81">L. 脕. Garc铆a</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">C. Gordon</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Goff%2C+J+M+L">J. M. Le Goff</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Niz%2C+G">G. Niz</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C. Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">M. Walther</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.00303v2-abstract-short" style="display: inline;"> Synthetic data sets are used in cosmology to test analysis procedures, to verify that systematic errors are well understood and to demonstrate that measurements are unbiased. In this work we describe the methods used to generate synthetic datasets of Lyman-$伪$ quasar spectra aimed for studies with the Dark Energy Spectroscopic Instrument (DESI). In particular, we focus on demonstrating that our si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00303v2-abstract-full').style.display = 'inline'; document.getElementById('2401.00303v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.00303v2-abstract-full" style="display: none;"> Synthetic data sets are used in cosmology to test analysis procedures, to verify that systematic errors are well understood and to demonstrate that measurements are unbiased. In this work we describe the methods used to generate synthetic datasets of Lyman-$伪$ quasar spectra aimed for studies with the Dark Energy Spectroscopic Instrument (DESI). In particular, we focus on demonstrating that our simulations reproduces important features of real samples, making them suitable to test the analysis methods to be used in DESI and to place limits on systematic effects on measurements of Baryon Acoustic Oscillations (BAO). We present a set of mocks that reproduce the statistical properties of the DESI early data set with good agreement. Additionally, we use full survey synthetic data to forecast the BAO scale constraining power with DESI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00303v2-abstract-full').style.display = 'none'; document.getElementById('2401.00303v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 17 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03434">arXiv:2309.03434</a> <span> [<a href="https://arxiv.org/pdf/2309.03434">pdf</a>, <a href="https://arxiv.org/format/2309.03434">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Broad Absorption Line Quasars in the Dark Energy Spectroscopic Instrument Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Filbert%2C+S">S. Filbert</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">P. Martini</a>, <a href="/search/?searchtype=author&query=Seebaluck%2C+K">K. Seebaluck</a>, <a href="/search/?searchtype=author&query=Ennesser%2C+L">L. Ennesser</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">I. P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C. Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">C. Ravoux</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">T. Tan</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.03434v2-abstract-short" style="display: inline;"> Broad absorption line (BAL) quasars are characterized by gas clouds that absorb flux at the wavelength of common quasar spectral features, although blueshifted by velocities that can exceed 0.1c. BAL features are interesting as signatures of significant feedback, yet they can also compromise cosmological studies with quasars by distorting the shape of the most prominent quasar emission lines, impa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03434v2-abstract-full').style.display = 'inline'; document.getElementById('2309.03434v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03434v2-abstract-full" style="display: none;"> Broad absorption line (BAL) quasars are characterized by gas clouds that absorb flux at the wavelength of common quasar spectral features, although blueshifted by velocities that can exceed 0.1c. BAL features are interesting as signatures of significant feedback, yet they can also compromise cosmological studies with quasars by distorting the shape of the most prominent quasar emission lines, impacting redshift accuracy and measurements of the matter density distribution traced by the Lyman-alpha forest. We present a catalog of BAL quasars discovered in the Dark Energy Spectroscopic Instrument (DESI) survey Early Data Release, which were observed as part of DESI Survey Validation, as well as the first two months of the main survey. We describe our method to automatically identify BAL quasars in DESI data, the quantities we measure for each BAL, and investigate the completeness and purity of this method with mock DESI observations. We mask the wavelengths of the BAL features and re-evaluate each BAL quasar redshift, finding new redshifts which are 243 km/s smaller on average for the BAL quasar sample. These new, more accurate redshifts are important to obtain the best measurements of quasar clustering, especially at small scales. Finally, we present some spectra of rarer classes of BALs that illustrate the potential of DESI data to identify such populations for further study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03434v2-abstract-full').style.display = 'none'; document.getElementById('2309.03434v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.10950">arXiv:2308.10950</a> <span> [<a href="https://arxiv.org/pdf/2308.10950">pdf</a>, <a href="https://arxiv.org/format/2308.10950">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> 3D Correlations in the Lyman-$伪$ Forest from Early DESI Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gordon%2C+C">Calum Gordon</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">Andrei Cuceu</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">Jon谩s Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Morales%2C+A+X">Alma Xochitl Gonz谩lez-Morales</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a>, <a href="/search/?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/?searchtype=author&query=Guy%2C+J">J. Guy</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Kirkby%2C+D">D. Kirkby</a>, <a href="/search/?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.10950v1-abstract-short" style="display: inline;"> We present the first measurements of Lyman-$伪$ (Ly$伪$) forest correlations using early data from the Dark Energy Spectroscopic Instrument (DESI). We measure the auto-correlation of Ly$伪$ absorption using 88,509 quasars at $z>2$, and its cross-correlation with quasars using a further 147,899 tracer quasars at $z\gtrsim1.77$. Then, we fit these correlations using a 13-parameter model based on linear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10950v1-abstract-full').style.display = 'inline'; document.getElementById('2308.10950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.10950v1-abstract-full" style="display: none;"> We present the first measurements of Lyman-$伪$ (Ly$伪$) forest correlations using early data from the Dark Energy Spectroscopic Instrument (DESI). We measure the auto-correlation of Ly$伪$ absorption using 88,509 quasars at $z>2$, and its cross-correlation with quasars using a further 147,899 tracer quasars at $z\gtrsim1.77$. Then, we fit these correlations using a 13-parameter model based on linear perturbation theory and find that it provides a good description of the data across a broad range of scales. We detect the BAO peak with a signal-to-noise ratio of $3.8蟽$, and show that our measurements of the auto- and cross-correlations are fully-consistent with previous measurements by the Extended Baryon Oscillation Spectroscopic Survey (eBOSS). Even though we only use here a small fraction of the final DESI dataset, our uncertainties are only a factor of 1.7 larger than those from the final eBOSS measurement. We validate the existing analysis methods of Ly$伪$ correlations in preparation for making a robust measurement of the BAO scale with the first year of DESI data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10950v1-abstract-full').style.display = 'none'; document.getElementById('2308.10950v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.10598">arXiv:2307.10598</a> <span> [<a href="https://arxiv.org/pdf/2307.10598">pdf</a>, <a href="https://arxiv.org/format/2307.10598">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae751">10.1093/mnras/stae751 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The long-lasting effect of X-ray preheating in the post-reionization intergalactic medium </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Yao Zhang</a>, <a href="/search/?searchtype=author&query=Mao%2C+Y">Yi Mao</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="2307.10598v2-abstract-short" style="display: inline;"> X-ray photons can penetrate deep into the intergalactic medium (IGM), leading to preheating of the IGM prior to cosmic reionization. X-ray preheating wipes out some of the small-scale structures that would otherwise be present prior to the passage of an ionization front. Accurate modeling of the small-scale structure is vital to the post-reionization IGM since the small-scale structure is ultimate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10598v2-abstract-full').style.display = 'inline'; document.getElementById('2307.10598v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10598v2-abstract-full" style="display: none;"> X-ray photons can penetrate deep into the intergalactic medium (IGM), leading to preheating of the IGM prior to cosmic reionization. X-ray preheating wipes out some of the small-scale structures that would otherwise be present prior to the passage of an ionization front. Accurate modeling of the small-scale structure is vital to the post-reionization IGM since the small-scale structure is ultimately the dominant source of long-lasting relics from hydrogen reionization. However, the precise impact of X-ray preheating in the fossils from hydrogen reionization is highly uncertain. In this work, we explore and establish for the first time, the long-lasting impact of X-ray preheating in the post-reionization IGM via hydrodynamic simulations with high-mass resolution. We find that the addition of X-ray preheating astrophysics leads to an overall lesser impact of the effect of inhomogeneous reionization in the Lyman-$伪$ forest -- depending on specific X-ray prescription -- at low redshifts ($z \sim 2$) with respect to a model with no X-ray preheating. However, at high redshifts ($z \sim 4$), our results indicate a strengthening of the relics of reionization in the Lyman-$伪$ forest because the IGM becomes more transparent compared to the scenario with no preheating. Thus, the absence of X-ray preheating in Lyman-$伪$ modeling can lead to a biased inference of cosmological parameters. Nevertheless, optimistically, the inclusion of X-ray preheating emerges as a promising novel avenue to probe the astrophysics of cosmic dawn. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10598v2-abstract-full').style.display = 'none'; document.getElementById('2307.10598v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Updated to match accepted version for publication, 19 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 2024, vol. 529, pp.3666-3683 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.11784">arXiv:2306.11784</a> <span> [<a href="https://arxiv.org/pdf/2306.11784">pdf</a>, <a href="https://arxiv.org/format/2306.11784">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"> NANCY: Next-generation All-sky Near-infrared Community surveY </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Han%2C+J+J">Jiwon Jesse Han</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/?searchtype=author&query=Price-Whelan%2C+A+M">Adrian M. Price-Whelan</a>, <a href="/search/?searchtype=author&query=Najita%2C+J">Joan Najita</a>, <a href="/search/?searchtype=author&query=Schlafly%2C+E+F">Edward F. Schlafly</a>, <a href="/search/?searchtype=author&query=Saydjari%2C+A">Andrew Saydjari</a>, <a href="/search/?searchtype=author&query=Wechsler%2C+R+H">Risa H. Wechsler</a>, <a href="/search/?searchtype=author&query=Bonaca%2C+A">Ana Bonaca</a>, <a href="/search/?searchtype=author&query=Schlegel%2C+D+J">David J Schlegel</a>, <a href="/search/?searchtype=author&query=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/?searchtype=author&query=Raichoor%2C+A">Anand Raichoor</a>, <a href="/search/?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/?searchtype=author&query=Kollmeier%2C+J+A">Juna A. Kollmeier</a>, <a href="/search/?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/?searchtype=author&query=Goodman%2C+A">Alyssa Goodman</a>, <a href="/search/?searchtype=author&query=Finkbeiner%2C+D">Douglas Finkbeiner</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">Abhijeet Anand</a>, <a href="/search/?searchtype=author&query=Ashby%2C+M">Matthew Ashby</a>, <a href="/search/?searchtype=author&query=Bahr-Kalus%2C+B">Benedict Bahr-Kalus</a>, <a href="/search/?searchtype=author&query=Beaton%2C+R">Rachel Beaton</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">Jayashree Behera</a>, <a href="/search/?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/?searchtype=author&query=Bellm%2C+E+C">Eric C Bellm</a> , et al. (184 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.11784v1-abstract-short" style="display: inline;"> The Nancy Grace Roman Space Telescope is capable of delivering an unprecedented all-sky, high-spatial resolution, multi-epoch infrared map to the astronomical community. This opportunity arises in the midst of numerous ground- and space-based surveys that will provide extensive spectroscopy and imaging together covering the entire sky (such as Rubin/LSST, Euclid, UNIONS, SPHEREx, DESI, SDSS-V, GAL… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11784v1-abstract-full').style.display = 'inline'; document.getElementById('2306.11784v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.11784v1-abstract-full" style="display: none;"> The Nancy Grace Roman Space Telescope is capable of delivering an unprecedented all-sky, high-spatial resolution, multi-epoch infrared map to the astronomical community. This opportunity arises in the midst of numerous ground- and space-based surveys that will provide extensive spectroscopy and imaging together covering the entire sky (such as Rubin/LSST, Euclid, UNIONS, SPHEREx, DESI, SDSS-V, GALAH, 4MOST, WEAVE, MOONS, PFS, UVEX, NEO Surveyor, etc.). Roman can uniquely provide uniform high-spatial-resolution (~0.1 arcsec) imaging over the entire sky, vastly expanding the science reach and precision of all of these near-term and future surveys. This imaging will not only enhance other surveys, but also facilitate completely new science. By imaging the full sky over two epochs, Roman can measure the proper motions for stars across the entire Milky Way, probing 100 times fainter than Gaia out to the very edge of the Galaxy. Here, we propose NANCY: a completely public, all-sky survey that will create a high-value legacy dataset benefiting innumerable ongoing and forthcoming studies of the universe. NANCY is a pure expression of Roman's potential: it images the entire sky, at high spatial resolution, in a broad infrared bandpass that collects as many photons as possible. The majority of all ongoing astronomical surveys would benefit from incorporating observations of NANCY into their analyses, whether these surveys focus on nearby stars, the Milky Way, near-field cosmology, or the broader universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11784v1-abstract-full').style.display = 'none'; document.getElementById('2306.11784v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to the call for white papers for the Roman Core Community Survey (June 16th, 2023), and to the Bulletin of the AAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06312">arXiv:2306.06312</a> <span> [<a href="https://arxiv.org/pdf/2306.06312">pdf</a>, <a href="https://arxiv.org/format/2306.06312">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Lyman-$伪$ forest catalog from the Dark Energy Spectroscopic Instrument Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ram%C3%ADrez-P%C3%A9rez%2C+C">C茅sar Ram铆rez-P茅rez</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-R%C3%A0fols%2C+I">Ignasi P茅rez-R脿fols</a>, <a href="/search/?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/?searchtype=author&query=Karim%2C+M+A">M. Abdul Karim</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/?searchtype=author&query=Cabayol-Garcia%2C+L">L. Cabayol-Garcia</a>, <a href="/search/?searchtype=author&query=Cai%2C+Z">Z. Cai</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">S. Chabanier</a>, <a href="/search/?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/?searchtype=author&query=de+la+Cruz%2C+R">R. de la Cruz</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/?searchtype=author&query=Gonzalez-Morales%2C+A+X">A. X. Gonzalez-Morales</a>, <a href="/search/?searchtype=author&query=Gordon%2C+C">C. Gordon</a>, <a href="/search/?searchtype=author&query=Herrera-Alcantar%2C+H+K">H. K. Herrera-Alcantar</a>, <a href="/search/?searchtype=author&query=Ir%C5%A1i%C4%8D%2C+V">V. Ir拧i膷</a>, <a href="/search/?searchtype=author&query=Ishak%2C+M">M. Ishak</a>, <a href="/search/?searchtype=author&query=Kara%C3%A7ayl%C4%B1%2C+N+G">N. G. Kara莽ayl谋</a>, <a href="/search/?searchtype=author&query=Luki%C4%87%2C+Z">Zarija Luki膰</a>, <a href="/search/?searchtype=author&query=Manser%2C+C+J">C. J. Manser</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">P. Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.06312v6-abstract-short" style="display: inline;"> We present and validate the catalog of Lyman-$伪$ forest fluctuations for 3D analyses using the Early Data Release (EDR) from the Dark Energy Spectroscopic Instrument (DESI) survey. We used 88,511 quasars collected from DESI Survey Validation (SV) data and the first two months of the main survey (M2). We present several improvements to the method used to extract the Lyman-$伪$ absorption fluctuation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06312v6-abstract-full').style.display = 'inline'; document.getElementById('2306.06312v6-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06312v6-abstract-full" style="display: none;"> We present and validate the catalog of Lyman-$伪$ forest fluctuations for 3D analyses using the Early Data Release (EDR) from the Dark Energy Spectroscopic Instrument (DESI) survey. We used 88,511 quasars collected from DESI Survey Validation (SV) data and the first two months of the main survey (M2). We present several improvements to the method used to extract the Lyman-$伪$ absorption fluctuations performed in previous analyses from the Sloan Digital Sky Survey (SDSS). In particular, we modify the weighting scheme and show that it can improve the precision of the correlation function measurement by more than 20%. This catalog can be downloaded from https://data.desi.lbl.gov/public/edr/vac/edr/lya/fuji/v0.3 and it will be used in the near future for the first DESI measurements of the 3D correlations in the Lyman-$伪$ forest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06312v6-abstract-full').style.display = 'none'; document.getElementById('2306.06312v6-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06308">arXiv:2306.06308</a> <span> [<a href="https://arxiv.org/pdf/2306.06308">pdf</a>, <a href="https://arxiv.org/format/2306.06308">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ad3217">10.3847/1538-3881/ad3217 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Data Release of the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (244 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.06308v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06308v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06308v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'none'; document.getElementById('2306.06308v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages, 7 figures, 17 tables, accepted for publication in the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ 168 58 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06307">arXiv:2306.06307</a> <span> [<a href="https://arxiv.org/pdf/2306.06307">pdf</a>, <a href="https://arxiv.org/format/2306.06307">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5281/zenodo.7858207">10.5281/zenodo.7858207 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (239 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.06307v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06307v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06307v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg$^2$ using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg$^2$ program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval $z<1.1$, 0.39% over the redshift interval $1.1<z<1.9$, and 0.46% over the redshift interval $1.9<z<3.5$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'none'; document.getElementById('2306.06307v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 18 figures, accepted by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.02385">arXiv:2210.02385</a> <span> [<a href="https://arxiv.org/pdf/2210.02385">pdf</a>, <a href="https://arxiv.org/format/2210.02385">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 of inhomogeneous reionization on post-reionization 21 cm intensity mapping measurement of cosmological parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Long%2C+H">Heyang Long</a>, <a href="/search/?searchtype=author&query=Morales-Guti%C3%A9rrez%2C+C">Catalina Morales-Guti茅rrez</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Hirata%2C+C+M">Christopher M. Hirata</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="2210.02385v2-abstract-short" style="display: inline;"> 21 cm intensity mapping (IM) has the potential to be a strong and unique probe of cosmology from redshift of order unity to redshift potentially as high as 30. For post-reionization 21 cm observations, the signal is modulated by the thermal and dynamical reaction of gas in the galaxies to the passage of ionization fronts during the Epoch of Reionization. In this work, we investigate the impact of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02385v2-abstract-full').style.display = 'inline'; document.getElementById('2210.02385v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.02385v2-abstract-full" style="display: none;"> 21 cm intensity mapping (IM) has the potential to be a strong and unique probe of cosmology from redshift of order unity to redshift potentially as high as 30. For post-reionization 21 cm observations, the signal is modulated by the thermal and dynamical reaction of gas in the galaxies to the passage of ionization fronts during the Epoch of Reionization. In this work, we investigate the impact of inhomogeneous reionization on the post-reionization 21 cm power spectrum and the induced shifts of cosmological parameters at redshifts $3.5 \lesssim z \lesssim 5.5$. We make use of hydrodynamics simulations that could resolve small-scale baryonic structure evolution to quantify HI abundance fluctuation, while semi-numerical large box 21cmFAST simulations capable of displaying inhomogeneous reionization process are deployed to track the inhomogeneous evolution of reionization bubbles. We discussed the prospects of capturing this effect in two post-reionization 21 cm intensity mapping experiments: SKA1-LOW and PUMA. We find the inhomogeneous reionization effect could impact the HI power spectrum up to tens of percent level and shift cosmological parameters estimation from sub-percent to tens percent in the observation of future post-reionization 21 cm intensity mapping experiments such as PUMA, while SKA1-LOW is likely to miss this effect at the redshifts of interest given the considered configuration. In particular, the shift is up to 0.0206 in the spectral index $n_s$ and 0.0192 eV in the sum of the neutrino masses $\sum m_谓$ depending on the reionization model and the observational parameters. We discuss strategies to mitigate and separate these biases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02385v2-abstract-full').style.display = 'none'; document.getElementById('2210.02385v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 9 figures. Published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.09005">arXiv:2207.09005</a> <span> [<a href="https://arxiv.org/pdf/2207.09005">pdf</a>, <a href="https://arxiv.org/format/2207.09005">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad437">10.1093/mnras/stad437 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Separating the memory of reionization from cosmology in the Ly$伪$ forest power spectrum at the post-reionization era </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Liu%2C+Y">Yuchen Liu</a>, <a href="/search/?searchtype=author&query=Mao%2C+Y">Yi Mao</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="2207.09005v2-abstract-short" style="display: inline;"> It has been recently shown that the astrophysics of reionization can be extracted from the Ly$伪$ forest power spectrum by marginalizing the memory of reionization over cosmological information. This impact of cosmic reionization on the Ly$伪$ forest power spectrum can survive cosmological time scales because cosmic reionization, which is inhomogeneous, and subsequent shocks from denser regions can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09005v2-abstract-full').style.display = 'inline'; document.getElementById('2207.09005v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.09005v2-abstract-full" style="display: none;"> It has been recently shown that the astrophysics of reionization can be extracted from the Ly$伪$ forest power spectrum by marginalizing the memory of reionization over cosmological information. This impact of cosmic reionization on the Ly$伪$ forest power spectrum can survive cosmological time scales because cosmic reionization, which is inhomogeneous, and subsequent shocks from denser regions can heat the gas in low-density regions to $\sim 3\times10^4$ K and compress it to mean-density. Current approach of marginalization over the memory of reionization, however, is not only model-dependent, based on the assumption of a specific reionization model, but also computationally expensive. Here we propose a simple analytical template for the impact of cosmic reionization, thereby treating it as a broadband systematic to be marginalized over for Bayesian inference of cosmological information from the Ly$伪$ forest in a model-independent manner. This template performs remarkably well with an error of $\leq 6 \%$ at large scales $k \approx 0.19$ Mpc$^{-1}$ where the effect of the memory of reionization is important, and reproduces the broadband effect of the memory of reionization in the Ly$伪$ forest correlation function, as well as the expected bias of cosmological parameters due to this systematic. The template can successfully recover the morphology of forecast errors in cosmological parameter space as expected when assuming a specific reionization model for marginalization purposes, with a slight overestimation of tens of per cent for the forecast errors on the cosmological parameters. We further propose a similar template for this systematic on the Ly$伪$ forest 1D power spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09005v2-abstract-full').style.display = 'none'; document.getElementById('2207.09005v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated to match accepted version for publication, 14 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 2023, vol. 520, pp.4853-4866 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.10939">arXiv:2205.10939</a> <span> [<a href="https://arxiv.org/pdf/2205.10939">pdf</a>, <a href="https://arxiv.org/format/2205.10939">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac882b">10.3847/1538-3881/ac882b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abareshi%2C+B">B. Abareshi</a>, <a href="/search/?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/?searchtype=author&query=Ameel%2C+J">J. Ameel</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/?searchtype=author&query=Aviles%2C+A">Alejandro Aviles</a>, <a href="/search/?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/?searchtype=author&query=Benavides%2C+B">B. Benavides</a>, <a href="/search/?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besuner%2C+R">R. Besuner</a>, <a href="/search/?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a> , et al. (242 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.10939v1-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'inline'; document.getElementById('2205.10939v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.10939v1-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt脜 > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'none'; document.getElementById('2205.10939v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">78 pages, 32 figures, submitted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07491">arXiv:2203.07491</a> <span> [<a href="https://arxiv.org/pdf/2203.07491">pdf</a>, <a href="https://arxiv.org/ps/2203.07491">ps</a>, <a href="https://arxiv.org/format/2203.07491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Snowmass2021 Cosmic Frontier White Paper: Prospects for obtaining Dark Matter Constraints with DESI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Valluri%2C+M">Monica Valluri</a>, <a href="/search/?searchtype=author&query=Chabanier%2C+S">Solene Chabanier</a>, <a href="/search/?searchtype=author&query=Irsic%2C+V">Vid Irsic</a>, <a href="/search/?searchtype=author&query=Armengaud%2C+E">Eric Armengaud</a>, <a href="/search/?searchtype=author&query=Walther%2C+M">Michael Walther</a>, <a href="/search/?searchtype=author&query=Rockosi%2C+C">Connie Rockosi</a>, <a href="/search/?searchtype=author&query=Sanchez-Conde%2C+M+A">Miguel A. Sanchez-Conde</a>, <a href="/search/?searchtype=author&query=Silva%2C+L+B+e">Leandro Beraldo e Silva</a>, <a href="/search/?searchtype=author&query=Cooper%2C+A+P">Andrew P. Cooper</a>, <a href="/search/?searchtype=author&query=Darragh-Ford%2C+E">Elise Darragh-Ford</a>, <a href="/search/?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/?searchtype=author&query=Deason%2C+A+J">Alis J. Deason</a>, <a href="/search/?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/?searchtype=author&query=Garzilli%2C+A">Antonella Garzilli</a>, <a href="/search/?searchtype=author&query=Li%2C+T">Ting Li</a>, <a href="/search/?searchtype=author&query=Lukic%2C+Z">Zarija Lukic</a>, <a href="/search/?searchtype=author&query=Manser%2C+C+J">Christopher J. Manser</a>, <a href="/search/?searchtype=author&query=Palanque-Delabrouille%2C+N">Nathalie Palanque-Delabrouille</a>, <a href="/search/?searchtype=author&query=Ravoux%2C+C">Corentin Ravoux</a>, <a href="/search/?searchtype=author&query=Tan%2C+T">Ting Tan</a>, <a href="/search/?searchtype=author&query=Wang%2C+W">Wenting Wang</a>, <a href="/search/?searchtype=author&query=Wechsler%2C+R">Risa Wechsler</a>, <a href="/search/?searchtype=author&query=Carrillo%2C+A">Andreia Carrillo</a>, <a href="/search/?searchtype=author&query=Dey%2C+A">Arjun Dey</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07491v2-abstract-short" style="display: inline;"> Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on thei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07491v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07491v2-abstract-full" style="display: none;"> Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on their properties can ONLY be arrived at using astrophysical observations. The Dark Energy Spectroscopic Instrument (DESI) is currently one of the most powerful instruments for wide-field surveys. The synergy of DESI with ESA's Gaia satellite and future observing facilities will yield datasets of unprecedented size and coverage that will enable constraints on DM over a wide range of physical and mass scales and across redshifts. DESI will obtain spectra of the Lyman-alpha forest out to z~5 by detecting about 1 million QSO spectra that will put constraints on clustering of the low-density intergalactic gas and DM halos at high redshift. DESI will obtain radial velocities of 10 million stars in the Milky Way (MW) and Local Group satellites enabling us to constrain their global DM distributions, as well as the DM distribution on smaller scales. The paradigm of cosmological structure formation has been extensively tested with simulations. However, the majority of simulations to date have focused on collisionless CDM. Simulations with alternatives to CDM have recently been gaining ground but are still in their infancy. While there are numerous publicly available large-box and zoom-in simulations in the LCDM framework, there are no comparable publicly available WDM, SIDM, FDM simulations. DOE support for a public simulation suite will enable a more cohesive community effort to compare observations from DESI (and other surveys) with numerical predictions and will greatly impact DM science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07491v2-abstract-full').style.display = 'none'; document.getElementById('2203.07491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contributed white paper to Snowmass 2021, CF03; minor revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14492">arXiv:2106.14492</a> <span> [<a href="https://arxiv.org/pdf/2106.14492">pdf</a>, <a href="https://arxiv.org/format/2106.14492">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab2569">10.1093/mnras/stab2569 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extracting the astrophysics of reionization from the Ly$伪$ forest power spectrum: a first forecast </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Mao%2C+Y">Yi Mao</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14492v2-abstract-short" style="display: inline;"> The impact of cosmic reionization on the Ly$伪$ forest power spectrum has recently been shown to be significant even at low redshifts ($z \sim 2$). This memory of reionization survives cosmological time scales because high-entropy mean-density gas is heated to $\sim 3\times10^4$ K by reionization, which is inhomogeneous, and subsequent shocks from denser regions. In the near future, the first measu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14492v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14492v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14492v2-abstract-full" style="display: none;"> The impact of cosmic reionization on the Ly$伪$ forest power spectrum has recently been shown to be significant even at low redshifts ($z \sim 2$). This memory of reionization survives cosmological time scales because high-entropy mean-density gas is heated to $\sim 3\times10^4$ K by reionization, which is inhomogeneous, and subsequent shocks from denser regions. In the near future, the first measurements of the Ly$伪$ forest 3D power spectrum will be very likely achieved by upcoming observational efforts such as the Dark Energy Spectroscopic Instrument (DESI). In addition to abundant cosmological information, these observations have the potential to extract the astrophysics of reionization from the Ly$伪$ forest. We forecast, for the first time, the accuracy with which the measurements of Ly$伪$ forest 3D power spectrum can place constraints on the reionization parameters with DESI. Specifically, we demonstrate that the constraints on the ionization efficiency, $味$, and the threshold mass for haloes that host ionizing sources, $m_{\rm turn}$, will have the $1蟽$ error at the level of $味= 25.0 \pm 11.6$ and $\log_{10} (m_{\rm turn}/{\rm M}_\odot) = 8.7^{+0.36}_{-0.70}$, respectively. The Ly$伪$ forest 3D power spectrum will thus provide an independent probe of reionization, probably even earlier in detection with DESI, with a sensitivity only slightly worse than the upcoming 21 cm power spectrum measurement with the Hydrogen Epoch of Reionization Array (HERA), i.e.\ $蟽_{\rm DESI} / 蟽_{\rm HERA} \approx 1.5$ for $味$ and $蟽_{\rm DESI}/蟽_{\rm HERA} \approx 2.0$ for $\log_{10}(m_{\rm turn} / $M$_\odot)$. Nevertheless, the Ly$伪$ forest constraint will be improved about three times tighter than the current constraint from reionization observations with high-z galaxy priors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14492v2-abstract-full').style.display = 'none'; document.getElementById('2106.14492v2-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated to match accepted version for publication. 19 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.10077">arXiv:2003.10077</a> <span> [<a href="https://arxiv.org/pdf/2003.10077">pdf</a>, <a href="https://arxiv.org/format/2003.10077">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2918">10.1093/mnras/staa2918 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ly$伪$ forest power spectrum as an emerging window into the epoch of reionization and cosmic dawn </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Mao%2C+Y">Yi Mao</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="2003.10077v2-abstract-short" style="display: inline;"> Conventional wisdom was that thermal relics from the epoch of reionization (EOR) would vanish swiftly. Recently, however, it was shown that these relics can survive to lower redshifts ($z \sim 2$) than previously thought, due to gas at mean density being heated to $T \sim 3 \times 10^4$ K by reionization, which is inhomogeneous, and shocks. Given the high sensitivities of upcoming Ly$伪$ forest sur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.10077v2-abstract-full').style.display = 'inline'; document.getElementById('2003.10077v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.10077v2-abstract-full" style="display: none;"> Conventional wisdom was that thermal relics from the epoch of reionization (EOR) would vanish swiftly. Recently, however, it was shown that these relics can survive to lower redshifts ($z \sim 2$) than previously thought, due to gas at mean density being heated to $T \sim 3 \times 10^4$ K by reionization, which is inhomogeneous, and shocks. Given the high sensitivities of upcoming Ly$伪$ forest surveys, this effect will be a novel broadband systematic for cosmological application. From the astrophysical point of view, however, the imprint of inhomogeneous reionization can shed light on the EOR and cosmic dawn. We utilize a hybrid method -- which includes two different simulation codes capable of handling the huge dynamical range -- to show the impact of patchy reionization on the Ly$伪$ forest and its dependence on different astrophysical scenarios. We found statistically significant deviations in the 1D Ly$伪$ power spectrum at $k = 0.14$ cMpc$^{-1}$ that range from $\sim 1\%$ at $z = 2$ up to almost $\sim 20\%$ at $z = 4$. The deviations in the 3D Ly$伪$ power spectrum, at the same wavenumber, are large and range from a few per cent at $z = 2$ up to $\sim 50\%$ at $z = 4$, although these deviations ignore the effect of He II reionization and AGN feedback at $z<4$. By exploiting different $k$-dependence of power spectrum among various astrophysical scenarios, the effect of patchy reionization on the Ly$伪$ forest power spectrum can open a new window into cosmic reionization and possibly cosmic dawn. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.10077v2-abstract-full').style.display = 'none'; document.getElementById('2003.10077v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated to match accepted version for publication. 13 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, Volume 499, Issue 2, pp.1640-1651 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.02504">arXiv:1910.02504</a> <span> [<a href="https://arxiv.org/pdf/1910.02504">pdf</a>, <a href="https://arxiv.org/format/1910.02504">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab67c6">10.3847/1538-4357/ab67c6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detecting Magnetic Fields in Exoplanets with Spectropolarimetry of the Helium Line at 1083 nm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Oklop%C4%8Di%C4%87%2C+A">Antonija Oklop膷i膰</a>, <a href="/search/?searchtype=author&query=Silva%2C+M">Makana Silva</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Hirata%2C+C+M">Christopher M. Hirata</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="1910.02504v2-abstract-short" style="display: inline;"> The magnetic fields of the solar system planets provide valuable insights into the planets' interiors and can have dramatic consequences for the evolution of their atmospheres and interaction with the solar wind. However, we have little direct knowledge of magnetic fields in exoplanets. Here we present a method for detecting magnetic fields in the atmospheres of close-in exoplanets based on spectr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.02504v2-abstract-full').style.display = 'inline'; document.getElementById('1910.02504v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.02504v2-abstract-full" style="display: none;"> The magnetic fields of the solar system planets provide valuable insights into the planets' interiors and can have dramatic consequences for the evolution of their atmospheres and interaction with the solar wind. However, we have little direct knowledge of magnetic fields in exoplanets. Here we present a method for detecting magnetic fields in the atmospheres of close-in exoplanets based on spectropolarimetric transit observations at the wavelength of the helium line at 1083 nm. This methodology has been successfully applied before for exploring magnetic fields in solar coronal filaments. Strong absorption signatures (transit depths on the order of a few percent) in the 1083 nm line have recently been observed for several close-in exoplanets. We show that in the conditions in these escaping atmospheres, metastable helium atoms should be optically pumped by the starlight and, for field strengths more than a few $\times 10^{-4}$ G, should align with the magnetic field. This results in linearly polarized absorption at 1083 nm that traces the field direction (the Hanle effect), which we explore by both analytic computation and with the Hazel numerical code. The linear polarization $\sqrt{Q^2+U^2}/I$ ranges from $\sim 10^{-3}$ in optimistic cases down to a few $\times 10^{-5}$ for particularly unfavorable cases, with very weak dependence on field strength. The line-of-sight component of the field results in a slight circular polarization (the Zeeman effect), also reaching $V/I\sim {\rm few}\times 10^{-5}(B_\parallel/10\,{\rm G})$. We discuss the detectability of these signals with current (SPIRou) and future (extremely large telescope) high-resolution infrared spectropolarimeters, and we briefly comment on possible sources of astrophysical contamination. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.02504v2-abstract-full').style.display = 'none'; document.getElementById('1910.02504v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">published in The Astrophysical Journal on February 14, 2020; updated to match the published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 890, 88 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.05950">arXiv:1906.05950</a> <span> [<a href="https://arxiv.org/pdf/1906.05950">pdf</a>, <a href="https://arxiv.org/format/1906.05950">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2019/08/031">10.1088/1475-7516/2019/08/031 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Revisiting constraints on asteroid-mass primordial black holes as dark matter candidates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Fang%2C+X">Xiao Fang</a>, <a href="/search/?searchtype=author&query=Vasquez%2C+G">Gabriel Vasquez</a>, <a href="/search/?searchtype=author&query=Silva%2C+M">Makana Silva</a>, <a href="/search/?searchtype=author&query=Hirata%2C+C+M">Christopher M. Hirata</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1906.05950v2-abstract-short" style="display: inline;"> As the only dark matter candidate that does not invoke a new particle that survives to the present day, primordial black holes (PBHs) have drawn increasing attention recently. Up to now, various observations have strongly constrained most of the mass range for PBHs, leaving only small windows where PBHs could make up a substantial fraction of the dark matter. Here we revisit the PBH constraints fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05950v2-abstract-full').style.display = 'inline'; document.getElementById('1906.05950v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.05950v2-abstract-full" style="display: none;"> As the only dark matter candidate that does not invoke a new particle that survives to the present day, primordial black holes (PBHs) have drawn increasing attention recently. Up to now, various observations have strongly constrained most of the mass range for PBHs, leaving only small windows where PBHs could make up a substantial fraction of the dark matter. Here we revisit the PBH constraints for the asteroid-mass window, i.e., the mass range $3.5\times 10^{-17}M_\odot < m_{\mathrm{PBH}} < 4\times 10^{-12}M_\odot$. We revisit 3 categories of constraints. (1) For optical microlensing, we analyze the finite source size and diffractive effects and discuss the scaling relations between the event rate, $m_{\mathrm{PBH}}$ and the event duration. We argue that it will be difficult to push the existing optical microlensing constraints to much lower m$_{\mathrm{PBH}}$. (2) For dynamical capture of PBHs in stars, we derive a general result on the capture rate based on phase space arguments. We argue that survival of stars does not constrain PBHs, but that disruption of stars by captured PBHs should occur and that the asteroid-mass PBH hypothesis could be constrained if we can work out the observational signature of this process. (3) For destruction of white dwarfs by PBHs that pass through the white dwarf without getting gravitationally captured, but which produce a shock that ignites carbon fusion, we perform a 1+1D hydrodynamic simulation to explore the post-shock temperature and relevant timescales, and again we find this constraint to be ineffective. In summary, we find that the asteroid-mass window remains open for PBHs to account for all the dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05950v2-abstract-full').style.display = 'none'; document.getElementById('1906.05950v2-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated to match accepted version for publication. 43 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP08(2019)031 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.02892">arXiv:1902.02892</a> <span> [<a href="https://arxiv.org/pdf/1902.02892">pdf</a>, <a href="https://arxiv.org/format/1902.02892">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz1388">10.1093/mnras/stz1388 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of inhomogeneous reionization on the Lyman-伪 forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Hirata%2C+C+M">Christopher M. Hirata</a>, <a href="/search/?searchtype=author&query=Martini%2C+P">Paul Martini</a>, <a href="/search/?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</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="1902.02892v2-abstract-short" style="display: inline;"> The \lya forest at high redshifts is a powerful probe of reionization. Modeling and observing this imprint comes with significant technical challenges: inhomogeneous reionization must be taken into account while simultaneously being able to resolve the web-like small-scale structure prior to reionization. In this work we quantify the impact of inhomogeneous reionization on the \lya forest at lower… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.02892v2-abstract-full').style.display = 'inline'; document.getElementById('1902.02892v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.02892v2-abstract-full" style="display: none;"> The \lya forest at high redshifts is a powerful probe of reionization. Modeling and observing this imprint comes with significant technical challenges: inhomogeneous reionization must be taken into account while simultaneously being able to resolve the web-like small-scale structure prior to reionization. In this work we quantify the impact of inhomogeneous reionization on the \lya forest at lower redshifts ($2 < z < 4$), where upcoming surveys such as DESI will enable precision measurements of the flux power spectrum. We use both small box simulations capable of handling the small-scale structure of the \lya forest and semi-numerical large box simulations capable of representing the effects of inhomogeneous reionization. We find that inhomogeneous reionization could produce a measurable effect on the \lya forest power spectrum. The deviation in the 3D power spectrum at $z_{\rm obs} = 4$ and $k = 0.14 \ \rm{Mpc}^{-1}$ ranges from $19 - 36\%$, with a larger effect for later reionization. The corrections decrease to $2.0 - 4.1\%$ by $z_{\rm obs} = 2$. The impact on the 1D power spectrum is smaller, and ranges from $3.3 - 6.5\%$ at $z_{\rm obs}=4$ to $0.35 - 0.75\%$ at $z_{\rm obs}=2$, values which are comparable to the statistical uncertainties in current and upcoming surveys. Furthermore, we study how can this systematic be constrained with the help of the quadrupole of the 21 cm power spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.02892v2-abstract-full').style.display = 'none'; document.getElementById('1902.02892v2-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">New version matches the accepted version for publication. 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/1803.04505">arXiv:1803.04505</a> <span> [<a href="https://arxiv.org/pdf/1803.04505">pdf</a>, <a href="https://arxiv.org/format/1803.04505">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2018/08/040">10.1088/1475-7516/2018/08/040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring circular polarization in the CMB due to conventional sources of cosmic birefringence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Hirata%2C+C+M">Christopher M. Hirata</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="1803.04505v2-abstract-short" style="display: inline;"> The circular polarization of the cosmic microwave background (CMB) is usually taken to be zero since it is not generated by Thomson scattering. Here we explore the actual level of circular polarization in the CMB generated by conventional cosmological sources of birefringence. We consider two classes of mechanisms for birefringence. One is alignment of the matter to produce an anisotropic suscepti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.04505v2-abstract-full').style.display = 'inline'; document.getElementById('1803.04505v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.04505v2-abstract-full" style="display: none;"> The circular polarization of the cosmic microwave background (CMB) is usually taken to be zero since it is not generated by Thomson scattering. Here we explore the actual level of circular polarization in the CMB generated by conventional cosmological sources of birefringence. We consider two classes of mechanisms for birefringence. One is alignment of the matter to produce an anisotropic susceptibility tensor: the hydrogen spins can be aligned either by density perturbations or CMB anisotropies themselves. The other is anisotropy of the radiation field coupled to the non-linear response of the medium to electromagnetic fields: this can occur either via photon-photon scattering (non-linear response of the vacuum); atomic hyperpolarizability (non-linear response of neutral atoms); or plasma delay (non-linear response of free electrons). The strongest effect comes from photon-photon scattering from recombination at a level of $\sim 10^{-14}$ K. Our results are consistent with a negligible circular polarization of the CMB in comparison with the linear polarization or the sensitivity of current and near-term experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.04505v2-abstract-full').style.display = 'none'; document.getElementById('1803.04505v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </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">New version matches the accepted version for publication. 45 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP08(2018)040 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.00102">arXiv:1609.00102</a> <span> [<a href="https://arxiv.org/pdf/1609.00102">pdf</a>, <a href="https://arxiv.org/ps/1609.00102">ps</a>, <a href="https://arxiv.org/format/1609.00102">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Approximate Kerr-Newman-like Metric with Quadrupole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Frutos-Alfaro%2C+F">Francisco Frutos-Alfaro</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</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="1609.00102v1-abstract-short" style="display: inline;"> The Kerr metric is known to present issues when trying to find an interior solution. In this work we continue in our efforts to construct a more realistic exterior metric for astrophysical objects. A new approximate metric representing the spacetime of a charged, rotating and slightly-deformed body is obtained by perturbing the Kerr-Newman metric to include the mass-quadrupole and quadrupole-quadr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00102v1-abstract-full').style.display = 'inline'; document.getElementById('1609.00102v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.00102v1-abstract-full" style="display: none;"> The Kerr metric is known to present issues when trying to find an interior solution. In this work we continue in our efforts to construct a more realistic exterior metric for astrophysical objects. A new approximate metric representing the spacetime of a charged, rotating and slightly-deformed body is obtained by perturbing the Kerr-Newman metric to include the mass-quadrupole and quadrupole-quadrupole orders. It has a simple form, because is Kerr-Newman-like. Its post-linear form without charge coincides with post-linear quadrupole-quadrupole metrics already found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00102v1-abstract-full').style.display = 'none'; document.getElementById('1609.00102v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.2899">arXiv:1405.2899</a> <span> [<a href="https://arxiv.org/pdf/1405.2899">pdf</a>, <a href="https://arxiv.org/ps/1405.2899">ps</a>, <a href="https://arxiv.org/format/1405.2899">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.15517/rmta.v22i2.20833">10.15517/rmta.v22i2.20833 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Slowly rotating Curzon-Chazy Metric </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Frutos-Alfaro%2C+F">Francisco Frutos-Alfaro</a>, <a href="/search/?searchtype=author&query=Gutierrez-Chaves%2C+C">Carlos Gutierrez-Chaves</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="1405.2899v3-abstract-short" style="display: inline;"> A new rotation version of the Curzon-Chazy metric is found. This new metric was obtained by means of a perturbation method, in order to include slow rotation. The solution is then proved to fulfill the Einstein field equations using a REDUCE program. Furthermore, the applications of this new solution are discussed. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.2899v3-abstract-full" style="display: none;"> A new rotation version of the Curzon-Chazy metric is found. This new metric was obtained by means of a perturbation method, in order to include slow rotation. The solution is then proved to fulfill the Einstein field equations using a REDUCE program. Furthermore, the applications of this new solution are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.2899v3-abstract-full').style.display = 'none'; document.getElementById('1405.2899v3-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Revista de Matem谩tica: Teor铆a y Aplicaciones, 22 (2): 265-274, 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.1776">arXiv:1405.1776</a> <span> [<a href="https://arxiv.org/pdf/1405.1776">pdf</a>, <a href="https://arxiv.org/ps/1405.1776">ps</a>, <a href="https://arxiv.org/format/1405.1776">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> </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/10.4236/ijaa.2015.51001">10.4236/ijaa.2015.51001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Approximate Metric for a Rotating Deformed Mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Frutos-Alfaro%2C+F">Francisco Frutos-Alfaro</a>, <a href="/search/?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/?searchtype=author&query=Araya-Arguedas%2C+M">Miguel Araya-Arguedas</a>, <a href="/search/?searchtype=author&query=Bonatti-Gonzalez%2C+J">Javier Bonatti-Gonzalez</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="1405.1776v3-abstract-short" style="display: inline;"> A new Kerr-like metric with quadrupole moment is obtained by means of perturbing the Kerr spacetime. The form of this new metric is simple as the Kerr metric. By comparison with the exterior Hartle-Thorne metric, it is shown that it could be matched to an interior solution. This approximate metric may represent the spacetime of a real astrophysical object with any Kerr rotation parameter a and sli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.1776v3-abstract-full').style.display = 'inline'; document.getElementById('1405.1776v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.1776v3-abstract-full" style="display: none;"> A new Kerr-like metric with quadrupole moment is obtained by means of perturbing the Kerr spacetime. The form of this new metric is simple as the Kerr metric. By comparison with the exterior Hartle-Thorne metric, it is shown that it could be matched to an interior solution. This approximate metric may represent the spacetime of a real astrophysical object with any Kerr rotation parameter a and slightly deformed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.1776v3-abstract-full').style.display = 'none'; document.getElementById('1405.1776v3-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </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">arXiv admin note: substantial text overlap with arXiv:1401.0866</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> International Journal of Astronomy and Astrophysics, 5(1):1-10, 2015 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 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