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class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li><span class="pagination-ellipsis">…</span></li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.11328">arXiv:2502.11328</a> <span> [<a href="https://arxiv.org/pdf/2502.11328">pdf</a>, <a href="https://arxiv.org/format/2502.11328">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Progress of the TianQin project </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Luo%2C+J">Jun Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+S">Shaojun Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y">Yan-Zheng Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+L">Lin Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Dang%2C+H">Hao Dang</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Q">Qijia Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Duan%2C+H">Hui-Zong Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+Y">Yuanbo Du</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+L">Lei Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+X">Xinju Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Yong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Gou%2C+X">Xingyu Gou</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+C">Changlei Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+W">Wei Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+B">Bin Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+H">Heran Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+M">Ming Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y">Yi-Ming Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+F+P">Fa Peng Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+D">Defeng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+X">Xin Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+Y">Yuan-Ze Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+E">En-Kun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Hongyin Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a> , et al. (76 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="2502.11328v1-abstract-short" style="display: inline;"> TianQin is a future space-based gravitational wave observatory targeting the frequency window of $10^{-4}$ Hz $\sim 1$ Hz. A large variety of gravitational wave sources are expected in this frequency band, including the merger of massive black hole binaries, the inspiral of extreme/intermediate mass ratio systems, stellar-mass black hole binaries, Galactic compact binaries, and so on. TianQin will… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11328v1-abstract-full').style.display = 'inline'; document.getElementById('2502.11328v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.11328v1-abstract-full" style="display: none;"> TianQin is a future space-based gravitational wave observatory targeting the frequency window of $10^{-4}$ Hz $\sim 1$ Hz. A large variety of gravitational wave sources are expected in this frequency band, including the merger of massive black hole binaries, the inspiral of extreme/intermediate mass ratio systems, stellar-mass black hole binaries, Galactic compact binaries, and so on. TianQin will consist of three Earth orbiting satellites on nearly identical orbits with orbital radii of about $10^5$ km. The satellites will form a normal triangle constellation whose plane is nearly perpendicular to the ecliptic plane. The TianQin project has been progressing smoothly following the ``0123" technology roadmap. In step ``0", the TianQin laser ranging station has been constructed and it has successfully ranged to all the five retro-reflectors on the Moon. In step ``1", the drag-free control technology has been tested and demonstrated using the TianQin-1 satellite. In step ``2", the inter-satellite laser interferometry technology will be tested using the pair of TianQin-2 satellites. The TianQin-2 mission has been officially approved and the satellites will be launched around 2026. In step ``3", i.e., the TianQin-3 mission, three identical satellites will be launched around 2035 to form the space-based gravitational wave detector, TianQin, and to start gravitational wave detection in space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11328v1-abstract-full').style.display = 'none'; document.getElementById('2502.11328v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages, 3 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/2502.06950">arXiv:2502.06950</a> <span> [<a href="https://arxiv.org/pdf/2502.06950">pdf</a>, <a href="https://arxiv.org/format/2502.06950">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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Cryoscope: A Cryogenic Infrared Survey Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M+M">Mansi M. Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Earley%2C+N">Nicholas Earley</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Roger Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Guillot%2C+T">Tristan Guillot</a>, <a href="/search/astro-ph?searchtype=author&query=Travouillon%2C+T">Tony Travouillon</a>, <a href="/search/astro-ph?searchtype=author&query=Fucik%2C+J">Jason Fucik</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+L">Lyu Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Greffe%2C+T">Timothee Greffe</a>, <a href="/search/astro-ph?searchtype=author&query=Agabi%2C+A">Abdelkrim Agabi</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">Michael C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Triaud%2C+A+H+M+J">Amaury H. M. J. Triaud</a>, <a href="/search/astro-ph?searchtype=author&query=Tinyanont%2C+S">Samaporn Tinyanont</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">Sarah Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Bendjoya%2C+P">Philippe Bendjoya</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattarai%2C+R">Rohan Bhattarai</a>, <a href="/search/astro-ph?searchtype=author&query=Bertz%2C+R">Rob Bertz</a>, <a href="/search/astro-ph?searchtype=author&query=Brugger%2C+J">James Brugger</a>, <a href="/search/astro-ph?searchtype=author&query=Burdanov%2C+A">Artem Burdanov</a>, <a href="/search/astro-ph?searchtype=author&query=Caiazzo%2C+I">Ilaria Caiazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">Luca Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+J">Jeff Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=De%2C+K">Kishalay De</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+R">Richard Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Deloupy%2C+V">Vincent Deloupy</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="2502.06950v1-abstract-short" style="display: inline;"> We present Cryoscope -- a new 50 sq. deg field-of-view, 1.2 m aperture, K-dark survey telescope to be located at Dome C, Antarctica. Cryoscope has an innovative optical-thermal design wherein the entire telescope is cryogenically cooled. Cryoscope also explores new detector technology to cost-effectively tile the full focal plane. Leveraging the dark Antarctic sky and minimizing telescope thermal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.06950v1-abstract-full').style.display = 'inline'; document.getElementById('2502.06950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.06950v1-abstract-full" style="display: none;"> We present Cryoscope -- a new 50 sq. deg field-of-view, 1.2 m aperture, K-dark survey telescope to be located at Dome C, Antarctica. Cryoscope has an innovative optical-thermal design wherein the entire telescope is cryogenically cooled. Cryoscope also explores new detector technology to cost-effectively tile the full focal plane. Leveraging the dark Antarctic sky and minimizing telescope thermal emission, Cryoscope achieves unprecedented deep, wide, fast and red observations, matching and exceeding volumetric survey speeds from the Ultraviolet Explorer, Vera Rubin Observatory, and Nancy Grace Roman Space Telescope. By providing coverage beyond wavelengths of 2 $渭$m, we aim to create the most comprehensive dynamic movie of the most obscured reaches of the Universe. Cryoscope will be a dedicated discovery engine for electromagnetic emission from coalescing compact binaries, Earth-like exoplanets orbiting cold stars, and multiple facets of time-domain, stellar and solar system science. In this paper, we describe the scientific drivers and technical innovations for this new discovery engine operating in the K-dark passband, why we choose to deploy it in Antarctica, and the status of a fifth-scale prototype designed as a Pathfinder to retire technological risks prior to full-scale implementation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.06950v1-abstract-full').style.display = 'none'; document.getElementById('2502.06950v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 20 figures, 4 tables; submitted to PASP on 2025-02-09</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.05805">arXiv:2502.05805</a> <span> [<a href="https://arxiv.org/pdf/2502.05805">pdf</a>, <a href="https://arxiv.org/format/2502.05805">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SUPERCOLD-CGM survey: II. [\ion{C}{1}]$(1-0)$ emission and the physical conditions of cold gas in Enormous Ly$伪$ nebulae at $z\,\sim\,2$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jianan Li</a>, <a href="/search/astro-ph?searchtype=author&query=Emonts%2C+B+H+C">Bjorn H. C. Emonts</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jianrui Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+R">Ran Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Villar-Mart%C3%ADn%2C+M">Montserrat Villar-Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Battaia%2C+F+A">Fabrizio Arrigoni Battaia</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Yunjing Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+I">Ilsang Yoon</a>, <a href="/search/astro-ph?searchtype=author&query=Lehnert%2C+M+D">Matthew D. Lehnert</a>, <a href="/search/astro-ph?searchtype=author&query=Massingill%2C+K">Kyle Massingill</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">Craig Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">Jason X Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Lacy%2C+M">Mark Lacy</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">Brian Mason</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="2502.05805v1-abstract-short" style="display: inline;"> We report ALMA and ACA observations of atomic carbon ([\ion{C}{1}]$(1-0)$) and dust continuum in 10 Enormous Ly$伪$ Nebulae hosting ultra-luminous Type-I QSOs at $z=2.2-2.5$, as part of the SUrvey of Protocluster ELANe Revealing CO/CI in the Ly$伪$ Detected CGM (SUPERCOLD-CGM). We detect [\ion{C}{1}]$(1-0)$ and dust in all ten QSOs and five companion galaxies. We find that the QSOs and companions ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05805v1-abstract-full').style.display = 'inline'; document.getElementById('2502.05805v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.05805v1-abstract-full" style="display: none;"> We report ALMA and ACA observations of atomic carbon ([\ion{C}{1}]$(1-0)$) and dust continuum in 10 Enormous Ly$伪$ Nebulae hosting ultra-luminous Type-I QSOs at $z=2.2-2.5$, as part of the SUrvey of Protocluster ELANe Revealing CO/CI in the Ly$伪$ Detected CGM (SUPERCOLD-CGM). We detect [\ion{C}{1}]$(1-0)$ and dust in all ten QSOs and five companion galaxies. We find that the QSOs and companions have higher gas densities and more intense radiation fields than Luminous Infrared galaxies and high-$z$ main sequence galaxies, with the highest values found in the QSOs. By comparing molecular gas masses derived from [\ion{C}{1}]$(1-0)$, CO(4$-$3) and dust continuum, we find that the QSOs and companions display a similar low CO conversion factor of $伪_{\rm CO}$\,$\sim$\,0.8 $\rm M_{\sun}$${[\rm K\,km/s\,pc^2]}^{-1}$. After tapering our data to low resolution, the [\ion{C}{1}]$(1-0)$ flux increases for nine QSOs, hinting at the possibility of [\ion{C}{1}]$(1-0)$ in the circum-galactic medium (CGM) on a scale of 16$-$40 kpc. However, the [\ion{C}{1}]$(1-0)$ sensitivity is too low to confirm this for individual targets, except for a tentative (2.7$蟽$) CGM detection in Q0050+0051{} with M$_{\rm H_2}$\,=\, ($1.0 - 2.8$)$\times 10^{10}$ $\rm M_{\sun}$. The 3$蟽$ mass limits of molecular CGM for the remaining QSO fields are ($0.2-1.4$)\,$\times$\,10$^{10}$ $\rm M_{\sun}$. This translates into a baryon fraction of $<$0.4-3$\% $ in the molecular CGM relative to the total baryonic halo mass. Our sample also includes a radio-detected AGN, Q1416+2649{}, which shows [\ion{C}{1}]$(1-0)$ and CO(4$-$3) luminosities an order of magnitude fainter for its far-infrared luminosity than other QSOs in our sample, possibly due to a lower molecular gas mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05805v1-abstract-full').style.display = 'none'; document.getElementById('2502.05805v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </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">27 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.12621">arXiv:2501.12621</a> <span> [<a href="https://arxiv.org/pdf/2501.12621">pdf</a>, <a href="https://arxiv.org/format/2501.12621">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"> DarkAI: Reconstructing the density, velocity and tidal field of dark matter from DESI-like bright galaxy sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+F">Feng Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Zitong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Y">Yizhou Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+C">Chengliang Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">Jiaxin Han</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Huiyuan Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Youcai Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+W">Wensheng Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yirong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiao-dong Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.12621v1-abstract-short" style="display: inline;"> Reconstructing the dark matter density, velocity, and tidal (MTV) fields from galaxy surveys is essential for advancing our understanding of the large-scale structure of the Universe. In this work, we present a machine learning-based framework using a UNet convolutional neural network to reconstruct the MTV fields from mock samples of the DESI bright galaxy survey within the redshift range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.12621v1-abstract-full').style.display = 'inline'; document.getElementById('2501.12621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.12621v1-abstract-full" style="display: none;"> Reconstructing the dark matter density, velocity, and tidal (MTV) fields from galaxy surveys is essential for advancing our understanding of the large-scale structure of the Universe. In this work, we present a machine learning-based framework using a UNet convolutional neural network to reconstruct the MTV fields from mock samples of the DESI bright galaxy survey within the redshift range $0.1 < z < 0.4$. Our approach accounts for realistic observational effects, including geometric selection, flux-limited data, and redshift space distortion (RSD) effects, thereby improving the fidelity of the reconstructed fields. Testing on mock galaxy catalogs generated from the Jiutian N-body simulation, our method achieves significant accuracy level. The reconstructed density field exhibits strong consistency with the true field, effectively eliminating most RSD effects and achieving a cross-correlation power spectrum coefficient greater than 0.985 on scales with $k < 0.1 \, h \, \mathrm{Mpc}^{-1}$. The velocity field reconstruction accurately captures large-scale coherent flows and small-scale turbulent features, exhibiting slopes of the grid-to-grid relationship close to unity and a scatter below $\sim$100 $\mathrm{km} \, \mathrm{s}^{-1}$. Additionally, the tidal field is reconstructed without bias, successfully recovering the features of the large-scale cosmic web, including clusters, filaments, sheets, and voids. Our results confirm that the proposed framework effectively captures the large-scale distribution and dynamics of dark matter while addressing key systematic challenges. These advancements provide a reliable and robust tool for analyzing current and future galaxy surveys, paving the way for new insights into cosmic structure formation and evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.12621v1-abstract-full').style.display = 'none'; document.getElementById('2501.12621v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 15 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/2501.10622">arXiv:2501.10622</a> <span> [<a href="https://arxiv.org/pdf/2501.10622">pdf</a>, <a href="https://arxiv.org/format/2501.10622">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"> CWTHF: Identifying Dark Matter Halos with Continuous Wavelet Transform </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Minxing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+P">Ping He</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="2501.10622v1-abstract-short" style="display: inline;"> Cosmological simulations are an important method for investigating the evolution of the Universe. In order to gain further insight into the processes of structure formation, it is necessary to identify isolated bound objects within the simulations, namely, the dark matter halos. The continuous wavelet transform (CWT) is an effective tool used as a halo finder due to its ability to extract clusteri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10622v1-abstract-full').style.display = 'inline'; document.getElementById('2501.10622v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10622v1-abstract-full" style="display: none;"> Cosmological simulations are an important method for investigating the evolution of the Universe. In order to gain further insight into the processes of structure formation, it is necessary to identify isolated bound objects within the simulations, namely, the dark matter halos. The continuous wavelet transform (CWT) is an effective tool used as a halo finder due to its ability to extract clustering information from the input data. In this study, we introduce CWTHF (Continuous Wavelet Transform Halo Finder), the first wavelet-based, MPI-parallelized halo finder, marking a novel approach in the field of cosmology. We calculate the CWT from the cloud-in-cell (CIC) grid and segment the grid based on the local CWT maxima. We then investigate the effects of the parameters that influence our program and identify the default settings. A comparison with the conventional friends-of-friends (FOF) method demonstrates the viability of CWT for halo finding. Although the actual performance is not faster than FOF, the linear time complexity of $\mathcal{O}(N)$ of our identification scheme indicates its significant potential for future optimization and application. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10622v1-abstract-full').style.display = 'none'; document.getElementById('2501.10622v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 15 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.10571">arXiv:2501.10571</a> <span> [<a href="https://arxiv.org/pdf/2501.10571">pdf</a>, <a href="https://arxiv.org/format/2501.10571">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> <p class="title is-5 mathjax"> Near-circular orbits for planets around M/K-type stars with Earth-like sizes and instellations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kipping%2C+D">David Kipping</a>, <a href="/search/astro-ph?searchtype=author&query=Solano-Oropeza%2C+D">Diana Solano-Oropeza</a>, <a href="/search/astro-ph?searchtype=author&query=Yahalomi%2C+D+A">Daniel A. Yahalomi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Madison Li</a>, <a href="/search/astro-ph?searchtype=author&query=Poddar%2C+A">Avishi Poddar</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">Xunhe 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="2501.10571v1-abstract-short" style="display: inline;"> Recent advances have enabled the discovery of a population of potentially Earth-like planets, yet their orbital eccentricity, which governs their climate and provides clues about their origin and dynamical history, is still largely unconstrained. We identify a sample of 17 transiting exoplanets around late-type stars with similar radii and irradiation to that of Earth and use the "photoeccentric e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10571v1-abstract-full').style.display = 'inline'; document.getElementById('2501.10571v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10571v1-abstract-full" style="display: none;"> Recent advances have enabled the discovery of a population of potentially Earth-like planets, yet their orbital eccentricity, which governs their climate and provides clues about their origin and dynamical history, is still largely unconstrained. We identify a sample of 17 transiting exoplanets around late-type stars with similar radii and irradiation to that of Earth and use the "photoeccentric effect" - which exploits transit durations - to infer their eccentricity distribution via hierarchical Bayesian modelling. Our analysis establishes that these worlds further resemble Earth in that their eccentricities are nearly circular (mean eccentricity $=0.060_{-0.028}^{+0.040}$ and $\leq0.15$), with the exception of one outlier of moderate eccentricity. The results hint at a subset population of dynamically warmer Earths, but this requires a larger sample to statistically confirm. The planets in our sample are thus largely subject to minimal eccentricity-induced seasonal variability and are consistent with emerging via smooth disk migration rather than violent planet-planet scattering. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10571v1-abstract-full').style.display = 'none'; document.getElementById('2501.10571v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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 appear in Nature Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.09580">arXiv:2501.09580</a> <span> [<a href="https://arxiv.org/pdf/2501.09580">pdf</a>, <a href="https://arxiv.org/format/2501.09580">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> An Intermediate-mass Black Hole Lurking in A Galactic Halo Caught Alive during Outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+C+-">C. -C. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D+-">D. -Y. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+N">N. Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+L+-">L. -X. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+H+-">H. -Q. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+J+-">J. -Z. Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C+-">C. -W. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+P">P. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T+-">T. -G. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+H+-">H. -Y. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">W. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+C">C. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Shu%2C+X+-">X. -W. Shu</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+R+-">R. -F. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y+-">Y. -L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+S+-">S. -X. Wen</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q+-">Q. -Y. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y+-">Y. -B. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Thomsen%2C+L+L">L. L. Thomsen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -J. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W+-">W. -J. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Coleiro%2C+A">A. Coleiro</a>, <a href="/search/astro-ph?searchtype=author&query=Eyles-Ferris%2C+R">R. Eyles-Ferris</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+X">X. Fang</a> , et al. (116 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="2501.09580v1-abstract-short" style="display: inline;"> Stellar-mass and supermassive black holes abound in the Universe, whereas intermediate-mass black holes (IMBHs) of ~10^2-10^5 solar masses in between are largely missing observationally, with few cases found only. Here we report the real-time discovery of a long-duration X-ray transient, EP240222a, accompanied by an optical flare with prominent H and He emission lines revealed by prompt follow-up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09580v1-abstract-full').style.display = 'inline'; document.getElementById('2501.09580v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.09580v1-abstract-full" style="display: none;"> Stellar-mass and supermassive black holes abound in the Universe, whereas intermediate-mass black holes (IMBHs) of ~10^2-10^5 solar masses in between are largely missing observationally, with few cases found only. Here we report the real-time discovery of a long-duration X-ray transient, EP240222a, accompanied by an optical flare with prominent H and He emission lines revealed by prompt follow-up observations. Its observed properties evidence an IMBH located unambiguously in the halo of a nearby galaxy and flaring by tidally disrupting a star -- the only confirmed off-nucleus IMBH-tidal disruption event so far. This work demonstrates the potential of sensitive time-domain X-ray surveys, complemented by timely multi-wavelength follow-ups, in probing IMBHs, their environments, demographics, origins and connections to stellar-mass and supermassive black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09580v1-abstract-full').style.display = 'none'; document.getElementById('2501.09580v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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">64 pages, 15 figures, submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.08503">arXiv:2501.08503</a> <span> [<a href="https://arxiv.org/pdf/2501.08503">pdf</a>, <a href="https://arxiv.org/format/2501.08503">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmological distance forecasts for the CSST Galaxy Survey using BAO peaks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+F">Feng Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Tian%2C+J">Jieyi Tian</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Zhejie Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Y">Yizhou Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Saulder%2C+C">Christoph Saulder</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiaoping Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yanming Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Zitong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhan%2C+H">Hu Zhan</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiaolei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+H">Hong Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Gong%2C+Y">Yan Gong</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+Y">Yunkun Han</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C">Cheng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Sui%2C+J">Jipeng Sui</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+R">Run Wen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+G">Gong-Bo Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+H">Hu Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+P">Pengjie Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+X">Xianzhong Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xingchen Zhou</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.08503v1-abstract-short" style="display: inline;"> The measurement of cosmological distances using baryon acoustic oscillations (BAO) is crucial for studying the universe's expansion. The Chinese Space Station Telescope (CSST) galaxy redshift survey, with its vast volume and sky coverage, provides an opportunity to address key challenges in cosmology. However, redshift uncertainties in galaxy surveys can degrade both angular and radial distance es… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.08503v1-abstract-full').style.display = 'inline'; document.getElementById('2501.08503v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.08503v1-abstract-full" style="display: none;"> The measurement of cosmological distances using baryon acoustic oscillations (BAO) is crucial for studying the universe's expansion. The Chinese Space Station Telescope (CSST) galaxy redshift survey, with its vast volume and sky coverage, provides an opportunity to address key challenges in cosmology. However, redshift uncertainties in galaxy surveys can degrade both angular and radial distance estimates. In this study, we forecast the precision of BAO distance measurements using mock CSST galaxy samples, applying a two-point correlation function (2PCF) wedge approach to mitigate redshift errors. We simulate redshift uncertainties of $蟽_0 = 0.003$ and $蟽_0 = 0.006$, representative of expected CSST errors, and examine their effects on the BAO peak and distance scaling factors, $伪_\perp$ and $伪_\parallel$, across redshift bins within $0.0 < z \leqslant 1.0$. The wedge 2PCF method proves more effective in detecting the BAO peak compared to the monopole 2PCF, particularly for $蟽_0 = 0.006$. Constraints on the BAO peaks show that $伪_\perp$ is well constrained around 1.0, regardless of $蟽_0$, with precision between 1% and 3% across redshift bins. In contrast, $伪_\parallel$ measurements are more sensitive to increases in $蟽_0$. For $蟽_0 = 0.003$, the results remain close to the fiducial value, with uncertainties ranging between 4% and 9%; for $蟽_0 = 0.006$, significant deviations from the fiducial value are observed. We also study the ability to measure parameters $(惟_m, H_0r_\mathrm{d})$ using distance measurements, proving robust constraints as a cosmological probe under CSST-like redshift uncertainties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.08503v1-abstract-full').style.display = 'none'; document.getElementById('2501.08503v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 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/2501.03337">arXiv:2501.03337</a> <span> [<a href="https://arxiv.org/pdf/2501.03337">pdf</a>, <a href="https://arxiv.org/format/2501.03337">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Multi-Wavelength Analysis of AT 2023sva: a Luminous Orphan Afterglow With Evidence for a Structured Jet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Srinivasaragavan%2C+G+P">Gokul P. Srinivasaragavan</a>, <a href="/search/astro-ph?searchtype=author&query=Perley%2C+D+A">Daniel A. Perley</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+A+Y+Q">Anna Y. Q. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connor%2C+B">Brendan O'Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Postigo%2C+A+d+U">Antonio de Ugarte Postigo</a>, <a href="/search/astro-ph?searchtype=author&query=Sarin%2C+N">Nikhil Sarin</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Sollerman%2C+J">Jesper Sollerman</a>, <a href="/search/astro-ph?searchtype=author&query=Rhodes%2C+L">Lauren Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+D+A">David A. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Svinkin%2C+D+S">Dmitry S. Svinkin</a>, <a href="/search/astro-ph?searchtype=author&query=Bhalerao%2C+V">Varun Bhalerao</a>, <a href="/search/astro-ph?searchtype=author&query=Waratkar%2C+G">Gaurav Waratkar</a>, <a href="/search/astro-ph?searchtype=author&query=Nayana%2C+A+J">A. J. Nayana</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+M+C">M. Coleman Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Malesani%2C+D+B">Daniele B. Malesani</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+G">Geoffrey Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=Srijan%2C+S">Suryansh Srijan</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">Eric C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Titterington%2C+D+J">David J. Titterington</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+M+B">Maria B. Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Purdum%2C+J">Josiah Purdum</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+T">Tom谩s Ahumada</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.03337v1-abstract-short" style="display: inline;"> We present multi-wavelength analysis of ZTF23abelseb (AT 2023sva), an optically discovered fast-fading ($螖m_r = 2.2$ mag in $螖t = 0.74 $ days), luminous ($M_r \sim -30.0$ mag) and red ($g-r = 0.50$ mag) transient at $z = 2.28$ with accompanying luminous radio emission. AT 2023sva does not possess a $纬$-ray burst (GRB) counterpart to an isotropic equivalent energy limit of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03337v1-abstract-full').style.display = 'inline'; document.getElementById('2501.03337v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.03337v1-abstract-full" style="display: none;"> We present multi-wavelength analysis of ZTF23abelseb (AT 2023sva), an optically discovered fast-fading ($螖m_r = 2.2$ mag in $螖t = 0.74 $ days), luminous ($M_r \sim -30.0$ mag) and red ($g-r = 0.50$ mag) transient at $z = 2.28$ with accompanying luminous radio emission. AT 2023sva does not possess a $纬$-ray burst (GRB) counterpart to an isotropic equivalent energy limit of $E_{\rm{纬, \, iso}} < 1.6 \times 10^{52}$ erg, determined through searching $纬$-ray satellite archives between the last non-detection and first detection, making it the sixth example of an optically-discovered afterglow with a redshift measurement and no detected GRB counterpart. We analyze AT 2023sva's optical, radio, and X-ray observations to characterize the source. From radio analyses, we find the clear presence of strong interstellar scintillation (ISS) 72 days after the initial explosion, allowing us to place constraints on the source's angular size and bulk Lorentz factor. When comparing the source sizes derived from ISS of orphan events to those of the classical GRB population, we find orphan events have statistically smaller source sizes. We also utilize Bayesian techniques to model the multi-wavelength afterglow. Within this framework, we find evidence that AT 2023sva possesses a shallow power-law structured jet viewed slightly off-axis ($胃_{\rm{v}} = 0.07 \pm 0.02$) just outside of the jet's core opening angle ($胃_{\rm{c}} = 0.06 \pm 0.02$). We determine this is likely the reason for the lack of a detected GRB counterpart, but also investigate other scenarios. AT 2023sva's evidence for possessing a structured jet stresses the importance of broadening orphan afterglow search strategies to a diverse range of GRB jet angular energy profiles, to maximize the return of future optical surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03337v1-abstract-full').style.display = 'none'; document.getElementById('2501.03337v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 14 Figures, Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.00986">arXiv:2501.00986</a> <span> [<a href="https://arxiv.org/pdf/2501.00986">pdf</a>, <a href="https://arxiv.org/format/2501.00986">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Photometric Objects Around Cosmic Webs (PAC). VII. Disentangling Mass and Environment Quenching with the Aid of Galaxy-halo Connection in Simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y">Yun Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+K">Kun Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+D">Donghai Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y+P">Y. P. Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">Hongyu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+X">Xiaolin Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.00986v1-abstract-short" style="display: inline;"> Star formation quenching in galaxies is a critical process in galaxy formation. It is widely believed that the quenching process is dominated by the mass of galaxies and/or their environment. In Paper V, we addressed the challenge to disentangle the effects of mass and environment by employing the PAC method, which combines spectroscopic and deep photometric surveys. This approach enabled us to me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.00986v1-abstract-full').style.display = 'inline'; document.getElementById('2501.00986v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.00986v1-abstract-full" style="display: none;"> Star formation quenching in galaxies is a critical process in galaxy formation. It is widely believed that the quenching process is dominated by the mass of galaxies and/or their environment. In Paper V, we addressed the challenge to disentangle the effects of mass and environment by employing the PAC method, which combines spectroscopic and deep photometric surveys. This approach enabled us to measure the excess surface density of blue and red galaxies around massive central galaxies down to $10^{9.0}M_{\odot}$. However, it is not straightforward to completely separate the two effects.To address this issue, in this paper, we derive the average quenched fraction of central (isolated) galaxies, $\bar{f}_{\mathrm{q}}^{\mathrm{cen}}(M_{*})$, by combining the 3D quenched fraction distribution $f^{\mathrm{sat}}_{\mathrm{q}}(r; M_{*,\mathrm{cen}}, M_{*,\mathrm{sat}})$, reconstructed from the $\bar{n}_2w_{\mathrm{p}}(r_{\mathrm{p}})$ measurements, with the stellar mass-halo mass relation in N-body simulations from Paper IV, and the observed total quenched fraction, $\bar{f}_{\mathrm{q}}^{\mathrm{all}}(M_{*})$. Using $f^{\mathrm{sat}}_{\mathrm{q}}(r;M_{*,\mathrm{cen}},M_{*,\mathrm{sat}})$, $\bar{f}_{\mathrm{q}}^{\mathrm{cen}}(M_{*})$, and the galaxy-halo connection, we assign a quenched probability to each (sub)halo in the simulation, enabling a comprehensive study of galaxy quenching. We find that the mass-quenched fraction increases from 0.3 to 0.87 across the stellar mass range $[10^{9.5}, 10^{11.0}]M_{\odot}$, while the environmental quenched fraction decreases from 0.17 to 0.03. The mass effect dominates galaxy quenching across the entire stellar mass range we studied. Moreover, more massive host halos are more effective at quenching their satellite galaxies, while satellite stellar mass has minimal influence on environmental quenching. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.00986v1-abstract-full').style.display = 'none'; document.getElementById('2501.00986v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ. Abstract abridged for arxiv. 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/2412.17611">arXiv:2412.17611</a> <span> [<a href="https://arxiv.org/pdf/2412.17611">pdf</a>, <a href="https://arxiv.org/format/2412.17611">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Superoutbursts and Positive Superhumps Occurred During the Standstill of a Z Cam-type Dwarf Nova </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qin-Mei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+P">Ping Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.17611v2-abstract-short" style="display: inline;"> Dwarf novae are semi-detached binaries, where a white dwarf accretes material from a cool main-sequence companion via an accretion disk, and are known for their intermittent outbursts, making them key systems for studying accretion physics. The accumulation of large survey datasets has challenged traditional models, which assumed that the disk remains hot and cannot produce superoutbursts during t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17611v2-abstract-full').style.display = 'inline'; document.getElementById('2412.17611v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.17611v2-abstract-full" style="display: none;"> Dwarf novae are semi-detached binaries, where a white dwarf accretes material from a cool main-sequence companion via an accretion disk, and are known for their intermittent outbursts, making them key systems for studying accretion physics. The accumulation of large survey datasets has challenged traditional models, which assumed that the disk remains hot and cannot produce superoutbursts during the standstill of Z Cam-type dwarf nova and that superoutbursts require a mass ratio of q = M_2/M_1 < 0.25 - 0.33. Here we report the detection of superoutbursts and positive superhumps (PSHs) during a standstill in the Z Cam-type star AT Cnc with a mass ratio larger than 0.33. Notably, the PSHs evolve gradually before the superoutburst begins, suggesting that an eccentric, precessing disk forms first, with the superoutburst occurring as the disk radius continues to expand. These findings provide the first detailed observational evidence of superoutbursts and PSHs occurring during standstill, offering important new insights into the classification of dwarf novae and the underlying mechanisms of outbursts <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17611v2-abstract-full').style.display = 'none'; document.getElementById('2412.17611v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 8 figures and 2 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/2412.08809">arXiv:2412.08809</a> <span> [<a href="https://arxiv.org/pdf/2412.08809">pdf</a>, <a href="https://arxiv.org/format/2412.08809">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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applications">stat.AP</span> </div> </div> <p class="title is-5 mathjax"> DAmodel: Hierarchical Bayesian Modelling of DA White Dwarfs for Spectrophotometric Calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyd%2C+B+M">Benjamin M. Boyd</a>, <a href="/search/astro-ph?searchtype=author&query=Narayan%2C+G">Gautham Narayan</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K+S">Kaisey S. Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Grayling%2C+M">Matthew Grayling</a>, <a href="/search/astro-ph?searchtype=author&query=Berres%2C+A">Aidan Berres</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mai Li</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">Tim Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">Thomas Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlin%2C+R+C">Ralph C. Bohlin</a>, <a href="/search/astro-ph?searchtype=author&query=Calamida%2C+A">Annalisa Calamida</a>, <a href="/search/astro-ph?searchtype=author&query=Holberg%2C+J+B">Jay B. Holberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hubeny%2C+I">Ivan Hubeny</a>, <a href="/search/astro-ph?searchtype=author&query=Mackenty%2C+J+W">John W. Mackenty</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Sabbi%2C+E">Elena Sabbi</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C+W">Christopher W. Stubbs</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="2412.08809v1-abstract-short" style="display: inline;"> We use hierarchical Bayesian modelling to calibrate a network of 32 all-sky faint DA white dwarf (DA WD) spectrophotometric standards ($16.5 < V < 19.5$) alongside the three CALSPEC standards, from 912 脜 to 32 $渭$m. The framework is the first of its kind to jointly infer photometric zeropoints and WD parameters ($\log g$, $T_{\text{eff}}$, $A_V$, $R_V$) by simultaneously modelling both photometric… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08809v1-abstract-full').style.display = 'inline'; document.getElementById('2412.08809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.08809v1-abstract-full" style="display: none;"> We use hierarchical Bayesian modelling to calibrate a network of 32 all-sky faint DA white dwarf (DA WD) spectrophotometric standards ($16.5 < V < 19.5$) alongside the three CALSPEC standards, from 912 脜 to 32 $渭$m. The framework is the first of its kind to jointly infer photometric zeropoints and WD parameters ($\log g$, $T_{\text{eff}}$, $A_V$, $R_V$) by simultaneously modelling both photometric and spectroscopic data. We model panchromatic HST/WFC3 UVIS and IR fluxes, HST/STIS UV spectroscopy and ground-based optical spectroscopy to sub-percent precision. Photometric residuals for the sample are the lowest yet yielding $<0.004$ mag RMS on average from the UV to the NIR, achieved by jointly inferring time-dependent changes in system sensitivity and WFC3/IR count-rate nonlinearity. Our GPU-accelerated implementation enables efficient sampling via Hamiltonian Monte Carlo, critical for exploring the high-dimensional posterior space. The hierarchical nature of the model enables population analysis of intrinsic WD and dust parameters. Inferred SEDs from this model will be essential for calibrating the James Webb Space Telescope as well as next-generation surveys, including Vera Rubin Observatory's Legacy Survey of Space and Time, and the Nancy Grace Roman Space Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08809v1-abstract-full').style.display = 'none'; document.getElementById('2412.08809v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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, 24 figures, 5 tables, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.06894">arXiv:2412.06894</a> <span> [<a href="https://arxiv.org/pdf/2412.06894">pdf</a>, <a href="https://arxiv.org/format/2412.06894">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">Roberto Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Colina%2C+L">Luis Colina</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">Eiichi Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Khusanova%2C+Y">Yana Khusanova</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zihao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">Xiaojing Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+R+A">Romain A. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Pudoka%2C+M+A">Maria A. Pudoka</a>, <a href="/search/astro-ph?searchtype=author&query=Rieke%2C+G+H">George H. Rieke</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Tee%2C+W+L">Wei Leong Tee</a>, <a href="/search/astro-ph?searchtype=author&query=Venemans%2C+B">Bram Venemans</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.06894v1-abstract-short" style="display: inline;"> We present a stringent measurement of the dust-obscured star-formation rate density (SFRD) at $z=4-6$ from the ASPIRE JWST Cycle-1 medium and ALMA Cycle-9 large program. We obtained JWST/NIRCam grism spectroscopy and ALMA 1.2-mm continuum map along 25 independent quasar sightlines, covering a total survey area of $\sim$35 arcmin$^2$ where we search for dusty star-forming galaxies (DSFGs) at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.06894v1-abstract-full').style.display = 'inline'; document.getElementById('2412.06894v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.06894v1-abstract-full" style="display: none;"> We present a stringent measurement of the dust-obscured star-formation rate density (SFRD) at $z=4-6$ from the ASPIRE JWST Cycle-1 medium and ALMA Cycle-9 large program. We obtained JWST/NIRCam grism spectroscopy and ALMA 1.2-mm continuum map along 25 independent quasar sightlines, covering a total survey area of $\sim$35 arcmin$^2$ where we search for dusty star-forming galaxies (DSFGs) at $z = 0 - 7$. We identify eight DSFGs in seven fields at $z=4-6$ through the detection of H$伪$ or [O III] $位$5008 lines, including fainter lines such as H$尾$, [O III] $位$4960, [N II] $位$6585, [S II] $位位$6718,6733 for six sources. With this spectroscopically complete DSFG sample at $z=4-6$ and negligible impact from cosmic variance (shot noise), we measure the infrared luminosity function (IRLF) down to $L_\mathrm{IR} \sim 2\times10^{11}$ $L_\odot$. We find flattening of IRLF at $z=4-6$ towards the faint end (power-law slope $伪= 0.59_{-0.45}^{+0.39}$). We determine the dust-obscured cosmic SFRD at this epoch as $\log[蟻_\mathrm{SFR,IR} / (\mathrm{M}_\odot\,\mathrm{yr}^{-1}\,\mathrm{Mpc}^{-3})] = -1.52_{-0.13}^{+0.14}$. This is significantly higher than previous determination using ALMA data in the Hubble Ultra Deep Field, which is void of DSFGs at $z=4-6$ because of strong cosmic variance (shot noise). We conclude that the majority ($66\pm7$%) of cosmic star formation at $z \sim 5$ is still obscured by dust. We also discuss the uncertainty of SFRD propagated from far-IR spectral energy distribution and IRLF at the bright end, which will need to be resolved with future ALMA and JWST observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.06894v1-abstract-full').style.display = 'none'; document.getElementById('2412.06894v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">27 pages, 13 figures, 3 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05542">arXiv:2412.05542</a> <span> [<a href="https://arxiv.org/pdf/2412.05542">pdf</a>, <a href="https://arxiv.org/format/2412.05542">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> <span class="tag is-small is-grey 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="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> </div> </div> <p class="title is-5 mathjax"> 113 km absolute ranging with nanometer precision </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yan-Wei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Lian%2C+M">Meng-Zhe Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">Jin-Jian Han</a>, <a href="/search/astro-ph?searchtype=author&query=Zeng%2C+T">Ting Zeng</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+G">Guo-Dong Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Sheng%2C+Y">Yi Sheng</a>, <a href="/search/astro-ph?searchtype=author&query=Esamdin%2C+A">Ali Esamdin</a>, <a href="/search/astro-ph?searchtype=author&query=Hou%2C+L">Lei Hou</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Q">Qi Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+J">Jian-Yu Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Jia%2C+J">Jian-Jun Jia</a>, <a href="/search/astro-ph?searchtype=author&query=Ren%2C+J">Ji-Gang Ren</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+C">Cheng-Zhi Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Q">Qiang Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+H">Hai-Feng Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+J">Jian-Wei Pan</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="2412.05542v1-abstract-short" style="display: inline;"> Accurate long-distance ranging is crucial for diverse applications, including satellite formation flying, very-long-baseline interferometry, gravitational-wave observatory, geographical research, etc. The integration of the time-of-flight mesurement with phase interference in dual-comb method enables high-precision ranging with a rapid update rate and an extended ambiguity range. Pioneering experi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05542v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05542v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05542v1-abstract-full" style="display: none;"> Accurate long-distance ranging is crucial for diverse applications, including satellite formation flying, very-long-baseline interferometry, gravitational-wave observatory, geographical research, etc. The integration of the time-of-flight mesurement with phase interference in dual-comb method enables high-precision ranging with a rapid update rate and an extended ambiguity range. Pioneering experiments have demonstrated unprecedented precision in ranging, achieving 5 nm @ 60 ms for 1.1 m and 200 nm @ 0.5 s for 25 m. However, long-distance ranging remains technically challenging due to high transmission loss and noise. In this letter, we propose a two-way dual-comb ranging (TWDCR) approach that enables successful ranging over a distance of 113 kilometers. We employ air dispersion analysis and synthetic repetition rate technique to extend the ambiguity range of the inherently noisy channel beyond 100 km. The achieved ranging precision is 11.5 $渭$m @ 1.3 ms, 681 nm @ 1 s, and 82 nm @ 21 s, as confirmed through a comparative analysis of two independent systems. The advanced long-distance ranging technology is expected to have immediate implications for space research initiatives, such as the space telescope array and the satellite gravimetry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05542v1-abstract-full').style.display = 'none'; document.getElementById('2412.05542v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">21 pages, 5 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.00331">arXiv:2412.00331</a> <span> [<a href="https://arxiv.org/pdf/2412.00331">pdf</a>, <a href="https://arxiv.org/format/2412.00331">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xu%2C+X">Xin Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+K">Kai Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+F">Fei Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+Q">Qian-Xue Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yi-Fan Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+X">Xin-Yu Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jing-Yi Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+X">Xing Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+G">Guo-You Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+C">Cheng-Yu Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mu-Zi-Mei Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.00331v1-abstract-short" style="display: inline;"> We performed photometric and spectroscopic studies of three large amplitude contact binaries, NSVS 2418361, ATLAS J057.1170+31.2384 and NSVS 7377875. The amplitudes of three systems' light curves are more than 0.7 magnitude. We analyzed the light curves using Wilson-Devinney code to yield physical parameters. The photometric solutions suggested that NSVS 7377875 belongs to an A-subtype contact bin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00331v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00331v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00331v1-abstract-full" style="display: none;"> We performed photometric and spectroscopic studies of three large amplitude contact binaries, NSVS 2418361, ATLAS J057.1170+31.2384 and NSVS 7377875. The amplitudes of three systems' light curves are more than 0.7 magnitude. We analyzed the light curves using Wilson-Devinney code to yield physical parameters. The photometric solutions suggested that NSVS 7377875 belongs to an A-subtype contact binary, while the others are classified as W-subtype ones. Furthermore, the mass ratio of NSVS 7377875 is higher than 0.72, so it belongs to H-subtype contact binaries. Since their light curves have unequal height at two maxima which is called O'Connell effect, a dark spot on the primary component for each target was required to get a better fit of light curves. The orbital period investigation shows that the period of NSVS 2418361 is increasing, indicating a mass transfer from the less massive component to the more massive one, while the other targets exhibit no long-term variation. Our spectral subtraction analysis of LAMOST spectra revealed excess emissions in the $H_伪$ line, indicating chromospheric activity in all the three targets. The Gaia distance was applied to estimate the absolute parameters of the three targets, and we obtained their evolutionary state. The relationships between the energy transfer parameter of 76 H-subtype contact binaries and their bolometric luminosity ratios, as well as their contact degree, were presented. We discovered that H-subtype systems have less efficient energy transfer rate, which is corresponding to the conclusion proposed by Csizmadia \& Klagyivik. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00331v1-abstract-full').style.display = 'none'; document.getElementById('2412.00331v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">21 pages, 10 figures, 12 tables, 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/2411.09753">arXiv:2411.09753</a> <span> [<a href="https://arxiv.org/pdf/2411.09753">pdf</a>, <a href="https://arxiv.org/format/2411.09753">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The democratic detrender: Ensemble-Based Removal of the Nuisance Signal in Stellar Time-Series Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yahalomi%2C+D+A">Daniel A. Yahalomi</a>, <a href="/search/astro-ph?searchtype=author&query=Kipping%2C+D">David Kipping</a>, <a href="/search/astro-ph?searchtype=author&query=Solano-Oropeza%2C+D">Diana Solano-Oropeza</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Madison Li</a>, <a href="/search/astro-ph?searchtype=author&query=Poddar%2C+A">Avishi Poddar</a>, <a href="/search/astro-ph?searchtype=author&query=Xunhe"> Xunhe</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang"> Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Abaakil%2C+Y">Yassine Abaakil</a>, <a href="/search/astro-ph?searchtype=author&query=Cassese%2C+B">Benjamin Cassese</a>, <a href="/search/astro-ph?searchtype=author&query=Teachey%2C+A">Alex Teachey</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+J">Jiajing Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Sundai%2C+F">Farai Sundai</a>, <a href="/search/astro-ph?searchtype=author&query=Valaskovic%2C+L">Lila Valaskovic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.09753v1-abstract-short" style="display: inline;"> Accurate, precise, and computationally efficient removal of unwanted activity that exists as a combination of periodic, quasi-periodic, and non-periodic systematic trends in time-series photometric data is a critical step in exoplanet transit analysis. Throughout the years, many different modeling methods have been used for this process, often called "detrending." However, there is no community-wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09753v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09753v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09753v1-abstract-full" style="display: none;"> Accurate, precise, and computationally efficient removal of unwanted activity that exists as a combination of periodic, quasi-periodic, and non-periodic systematic trends in time-series photometric data is a critical step in exoplanet transit analysis. Throughout the years, many different modeling methods have been used for this process, often called "detrending." However, there is no community-wide consensus regarding the favored approach. In order to mitigate model dependency, we present an ensemble-based approach to detrending via community-of-models and the $\texttt{democratic detrender}$: a modular and scalable open-source coding package that implements ensemble detrending. The $\texttt{democratic detrender}$ allows users to select from a number of packaged detrending methods (including cosine filtering, Gaussian processes, and polynomial fits) or provide their own set of detrended light curves via methods of their choosing. The $\texttt{democratic detrender}$ then combines the resulting individually detrended light curves into a single method marginalized (via median selection) light curve. Additionally, the $\texttt{democratic detrender}$ inflates the uncertainties of each time-series data point using information from the median absolute deviation between the individually detrended light curve, propagating information into the final detrended light curve about the added uncertainty due to the correctness of the underlying models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09753v1-abstract-full').style.display = 'none'; document.getElementById('2411.09753v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">15 pages, 10 figures, submitted to ApJS. For source code, documentation, and tutorials, see https://github.com/dyahalomi/democratic_detrender</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.07973">arXiv:2411.07973</a> <span> [<a href="https://arxiv.org/pdf/2411.07973">pdf</a>, <a href="https://arxiv.org/format/2411.07973">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The Nature of Optical Afterglows Without Gamma-ray Bursts: Identification of AT2023lcr and Multiwavelength Modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M+L">Maggie L. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+A+Y+Q">Anna Y. Q. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+G">Geoffrey Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=Perley%2C+D+A">Daniel A. Perley</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+G+P">Gavin P. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Nayana%2C+A+J">A. J. Nayana</a>, <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</a>, <a href="/search/astro-ph?searchtype=author&query=Anupama%2C+G+C">G. C. Anupama</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">Eric C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+E">Edo Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Caiazzo%2C+I">Ilaria Caiazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+M+W">Michael W. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=El-Badry%2C+K">Kareem El-Badry</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+J">Matthew J. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M">Mansi Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Keating%2C+G+K">Garrett K. Keating</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">S. R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+H">Harsh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Masci%2C+F+J">Frank J. Masci</a>, <a href="/search/astro-ph?searchtype=author&query=Perley%2C+R+A">Richard A. Perley</a>, <a href="/search/astro-ph?searchtype=author&query=Purdum%2C+J">Josiah Purdum</a>, <a href="/search/astro-ph?searchtype=author&query=Rao%2C+R">Ramprasad Rao</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="2411.07973v1-abstract-short" style="display: inline;"> In the past few years, the improved sensitivity and cadence of wide-field optical surveys have enabled the discovery of several afterglows without associated detected gamma-ray bursts (GRBs). We present the identification, observations, and multiwavelength modeling of a recent such afterglow (AT2023lcr), and model three literature events (AT2020blt, AT2021any, and AT2021lfa) in a consistent fashio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07973v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07973v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07973v1-abstract-full" style="display: none;"> In the past few years, the improved sensitivity and cadence of wide-field optical surveys have enabled the discovery of several afterglows without associated detected gamma-ray bursts (GRBs). We present the identification, observations, and multiwavelength modeling of a recent such afterglow (AT2023lcr), and model three literature events (AT2020blt, AT2021any, and AT2021lfa) in a consistent fashion. For each event, we consider the following possibilities as to why a GRB was not observed: 1) the jet was off-axis; 2) the jet had a low initial Lorentz factor; and 3) the afterglow was the result of an on-axis classical GRB (on-axis jet with physical parameters typical of the GRB population), but the emission was undetected by gamma-ray satellites. We estimate all physical parameters using afterglowpy and Markov Chain Monte Carlo methods from emcee. We find that AT2023lcr, AT2020blt, and AT2021any are consistent with on-axis classical GRBs, and AT2021lfa is consistent with both on-axis low Lorentz factor ($螕_0 \approx 5 - 13$) and off-axis ($胃_\text{obs}=2胃_\text{jet}$) high Lorentz factor ($螕_0 \approx 100$) jets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07973v1-abstract-full').style.display = 'none'; document.getElementById('2411.07973v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 18 figures, 20 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.03592">arXiv:2411.03592</a> <span> [<a href="https://arxiv.org/pdf/2411.03592">pdf</a>, <a href="https://arxiv.org/format/2411.03592">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Evolutionary states and triplicity of four massive semi-detached binaries with long-term decreasing orbital periods in the LMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Liao%2C+W">Wen-Ping Liao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+e">er-gang Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+L">Lin-Feng Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+W">Wen-Xu Lin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.03592v1-abstract-short" style="display: inline;"> The massive semi-detached binary with a long-term decreasing orbital period may involve a rapid mass-transfer phase in Case A, and thus they are good astrophysical laboratories for investigating the evolution of massive binary stars. In this work, by using the long-term observational light curves from the OGLE project and other data in the low-metallicity LMC, four semi-detached massive binaries w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03592v1-abstract-full').style.display = 'inline'; document.getElementById('2411.03592v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.03592v1-abstract-full" style="display: none;"> The massive semi-detached binary with a long-term decreasing orbital period may involve a rapid mass-transfer phase in Case A, and thus they are good astrophysical laboratories for investigating the evolution of massive binary stars. In this work, by using the long-term observational light curves from the OGLE project and other data in the low-metallicity LMC, four semi-detached massive binaries with long-term decreases in the orbital periods are detected from 165 EB-type close binaries. It is found that the more massive component in S07798 is filling its Roche lobe where the period decrease is caused by mass transfer from the primary to the secondary. However, the other three (S03065, S12631, S16873) are semi-detached binaries with a lobe-filling secondary where the mass transfer between the components should cause the period to increase if the angular momentum is conservative. The long-term period decreases in these three systems may be caused by the angular momentum loss. Additionally, the orbital periods of three systems (S03065, S07798, S16873) are detected to show cyclic variation with periods shorter than 11 years, which can be plausibly explained by the presence of close-in third bodies in these massive binaries. Based on all of these results, it is suggested that the detected four semi-detached binaries almost have multiplicity. The companion stars are crucial for the origin and evolution of these massive close binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03592v1-abstract-full').style.display = 'none'; document.getElementById('2411.03592v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.21617">arXiv:2410.21617</a> <span> [<a href="https://arxiv.org/pdf/2410.21617">pdf</a>, <a href="https://arxiv.org/format/2410.21617">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11433-024-2524-4">10.1007/s11433-024-2524-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Einstein Probe discovery of EP240408a: a peculiar X-ray transient with an intermediate timescale </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W">Wenda Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Weimin Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+Z">Zhixing Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yong Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+A">Arne Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zhiming Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+H">Huaqing Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zelati%2C+F+C">Francesco Coti Zelati</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+L">Lixin Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+J">Jingwei Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Jia%2C+S">Shumei Jia</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+C">Chichuan Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dongyue Li</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+R">Rongfeng Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Shu%2C+X">Xinwen Shu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+S">Shengli Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+X">Xiaojin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xiaofeng Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+L">Lei Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+C">Chen Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shuang-Nan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yonghe Zhang</a> , et al. (115 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.21617v1-abstract-short" style="display: inline;"> We report the discovery of a peculiar X-ray transient, EP240408a, by Einstein Probe (EP) and follow-up studies made with EP, Swift, NICER, GROND, ATCA and other ground-based multi-wavelength telescopes. The new transient was first detected with Wide-field X-ray Telescope (WXT) on board EP on April 8th, 2024, manifested in an intense yet brief X-ray flare lasting for 12 seconds. The flare reached a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21617v1-abstract-full').style.display = 'inline'; document.getElementById('2410.21617v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.21617v1-abstract-full" style="display: none;"> We report the discovery of a peculiar X-ray transient, EP240408a, by Einstein Probe (EP) and follow-up studies made with EP, Swift, NICER, GROND, ATCA and other ground-based multi-wavelength telescopes. The new transient was first detected with Wide-field X-ray Telescope (WXT) on board EP on April 8th, 2024, manifested in an intense yet brief X-ray flare lasting for 12 seconds. The flare reached a peak flux of 3.9x10^(-9) erg/cm2/s in 0.5-4 keV, about 300 times brighter than the underlying X-ray emission detected throughout the observation. Rapid and more precise follow-up observations by EP/FXT, Swift and NICER confirmed the finding of this new transient. Its X-ray spectrum is non-thermal in 0.5-10 keV, with a power-law photon index varying within 1.8-2.5. The X-ray light curve shows a plateau lasting for about 4 days, followed by a steep decay till becoming undetectable about 10 days after the initial detection. Based on its temporal property and constraints from previous EP observations, an unusual timescale in the range of 7-23 days is found for EP240408a, which is intermediate between the commonly found fast and long-term transients. No counterparts have been found in optical and near-infrared, with the earliest observation at 17 hours after the initial X-ray detection, suggestive of intrinsically weak emission in these bands. We demonstrate that the remarkable properties of EP240408a are inconsistent with any of the transient types known so far, by comparison with, in particular, jetted tidal disruption events, gamma-ray bursts, X-ray binaries and fast blue optical transients. The nature of EP240408a thus remains an enigma. We suggest that EP240408a may represent a new type of transients with intermediate timescales of the order of about 10 days. The detection and follow-ups of more of such objects are essential for revealing their origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21617v1-abstract-full').style.display = 'none'; document.getElementById('2410.21617v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 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">25 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> published in SCIENCE CHINA Physics, Mechanics & Astronomy(SCPMA) (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.19388">arXiv:2410.19388</a> <span> [<a href="https://arxiv.org/pdf/2410.19388">pdf</a>, <a href="https://arxiv.org/format/2410.19388">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmological forecast for the weak gravitational lensing and galaxy clustering joint analysis in the CSST photometric survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xiong%2C+Q">Qi Xiong</a>, <a href="/search/astro-ph?searchtype=author&query=Gong%2C+Y">Yan Gong</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xingchen Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H">Hengjie Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+F">Furen Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Ziwei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ibitoye%2C+A">Ayodeji Ibitoye</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xuelei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+Z">Zuhui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Q">Qi Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yun Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Pei%2C+W">Wenxiang Pei</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="2410.19388v1-abstract-short" style="display: inline;"> We explore the joint weak lensing and galaxy clustering analysis from the photometric survey operated by the China Space Station Telescope (CSST), and study the strength of the cosmological constraints. We employ a high-resolution JiuTian-1G simulation to construct a partial-sky light cone to $z=3$ covering 100 deg$^2$, and obtain the CSST galaxy mock samples based on an improved semi-analytical m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19388v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19388v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19388v1-abstract-full" style="display: none;"> We explore the joint weak lensing and galaxy clustering analysis from the photometric survey operated by the China Space Station Telescope (CSST), and study the strength of the cosmological constraints. We employ a high-resolution JiuTian-1G simulation to construct a partial-sky light cone to $z=3$ covering 100 deg$^2$, and obtain the CSST galaxy mock samples based on an improved semi-analytical model. We perform a multi-lens-plane algorithm to generate corresponding synthetic weak lensing maps and catalogs. Then we generate the mock data based on these catalogs considering the instrumental and observational effects of the CSST, and use the Markov Chain Monte Carlo (MCMC) method to perform the constraints. The covariance matrix includes non-Gaussian contributions and super-sample covariance terms, and the systematics from intrinsic alignments, galaxy bias, photometric redshift uncertainties, shear calibration, and non-linear effects are considered in the analysis. We find that, for the joint analysis of the CSST weak lensing and galaxy clustering surveys, the cosmological parameters can be constrained to a few percent or even less than one percent level. This indicates the CSST photometric survey is powerful for exploring the Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19388v1-abstract-full').style.display = 'none'; document.getElementById('2410.19388v1-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">17 pages, 12 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.16086">arXiv:2410.16086</a> <span> [<a href="https://arxiv.org/pdf/2410.16086">pdf</a>, <a href="https://arxiv.org/format/2410.16086">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Enhanced $S$-factor for the $^{14}$N$(p,纬)^{15}$O reaction and its impact on the solar composition problem </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+J">J. Su</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y+P">Y. P. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+L+Y">L. Y. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+J+J">J. J. He</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">S. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Z+L">Z. L. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+S">S. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+L+Y">L. Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">H. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L+H">L. H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+X+Z">X. Z. Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Y+T">Y. T. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Qin%2C+Z+W">Z. W. Qin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+F+C">F. C. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Sheng%2C+Y+D">Y. D. Sheng</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y+J">Y. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+Y+L">Y. L. Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X+Y">X. Y. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+J+Y">J. Y. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+Y+C">Y. C. Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y+Q">Y. Q. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.16086v1-abstract-short" style="display: inline;"> The solar composition problem has puzzled astrophysicists for more than 20 years. Recent measurements of carbon-nitrogen-oxygen (CNO) neutrinos by the Borexino experiment show a $\sim2蟽$ tension with the "low-metallicity" determinations. $^{14}$N$(p,纬)^{15}$O, the slowest reaction in the CNO cycle, plays a crucial role in the standard solar model (SSM) calculations of CNO neutrino fluxes. Here we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16086v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16086v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16086v1-abstract-full" style="display: none;"> The solar composition problem has puzzled astrophysicists for more than 20 years. Recent measurements of carbon-nitrogen-oxygen (CNO) neutrinos by the Borexino experiment show a $\sim2蟽$ tension with the "low-metallicity" determinations. $^{14}$N$(p,纬)^{15}$O, the slowest reaction in the CNO cycle, plays a crucial role in the standard solar model (SSM) calculations of CNO neutrino fluxes. Here we report a direct measurement of the $^{14}$N$(p,纬)^{15}$O reaction, in which $S$-factors for all transitions were simultaneously determined in the energy range of $E_p=110-260$ keV for the first time. Our results resolve previous discrepancies in the ground-state transition, yielding a zero-energy $S$-factor $S_{114}(0) = 1.92\pm0.08$ keV b which is 14% higher than the $1.68\pm0.14$ keV b recommended in Solar Fusion III (SF-III). With our $S_{114}$ values, the SSM B23-GS98, and the latest global analysis of solar neutrino measurements, the C and N photospheric abundance determined by the Borexino experiment is updated to $N_{\mathrm{CN}}=({4.45}^{+0.69}_{-0.61})\times10^{-4}$. This new $N_{\mathrm{CN}}$ value agrees well with latest "high-metallicity" composition, however, is also consistent with the "low-metallicity" determination within $\sim 1蟽$ C.L., indicating that the solar metallicity problem remains an open question. In addition, the significant reduction in the uncertainty of $S_{114}$ paves the way for the precise determination of the CN abundance in future large-volume solar neutrino measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16086v1-abstract-full').style.display = 'none'; document.getElementById('2410.16086v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.10993">arXiv:2410.10993</a> <span> [<a href="https://arxiv.org/pdf/2410.10993">pdf</a>, <a href="https://arxiv.org/format/2410.10993">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202452610">10.1051/0004-6361/202452610 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct high-resolution observation of feedback and chemical enrichment in the circumgalactic medium at redshift z ~ 2.8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peng%2C+B">Bo Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Battaia%2C+F+A">Fabrizio Arrigoni Battaia</a>, <a href="/search/astro-ph?searchtype=author&query=Vishwas%2C+A">Amit Vishwas</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Iani%2C+E">Edoardo Iani</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ferkinhoff%2C+C">Carl Ferkinhoff</a>, <a href="/search/astro-ph?searchtype=author&query=Stacey%2C+G">Gordon Stacey</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Ivison%2C+R">Rob Ivison</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="2410.10993v2-abstract-short" style="display: inline;"> The circumgalactic medium (CGM) plays a vital role in galaxy evolution, however, studying the emission from CGM is challenging due to its low surface brightness and the complexities involved in interpreting resonant lines such as Ly$伪$. The near-infrared coverage, unprecedented sensitivity, and high spatial resolution of JWST enable us to study the optical strong lines associated with the extended… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10993v2-abstract-full').style.display = 'inline'; document.getElementById('2410.10993v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10993v2-abstract-full" style="display: none;"> The circumgalactic medium (CGM) plays a vital role in galaxy evolution, however, studying the emission from CGM is challenging due to its low surface brightness and the complexities involved in interpreting resonant lines such as Ly$伪$. The near-infrared coverage, unprecedented sensitivity, and high spatial resolution of JWST enable us to study the optical strong lines associated with the extended Ly$伪$ "nebulae" at redshifts of 2--3. These lines serve as diagnostic tools to infer the physical conditions in the CGM gas reservoir of these systems. In deep medium-band images taken by the JWST, we serendipitously discovered the [O III] emission from the CGM around a massive interacting galaxy system at a redshift z~2.8, known to be embedded in a bright extended (100 kpc) Ly$伪$ "nebula." This is the first time that the [O III] lines have been detected from a Ly$伪$ "nebula." The JWST images reveal that the CGM gas actually resides in narrow (~ 2.5 kpc) filamentary structures with strong [O III] emission, tracing the same extent as the Ly$伪$ emission. An analysis of the [O III] suggests that the emitting CGM is fully ionized and is energetically dominated by mechanical heating. We also find that the density and pressure are higher than those commonly predicted by simulations of the CGM. We conclude that the observed CGM emission originates from the gas expelled by the episodic feedback processes, cooling down and enriching the CGM, while traveling a distance of at least 60 kpc. These observations demonstrate how intensive feedback processes shape gas distribution and properties in the CGM around massive halos. While access to such deep, high-resolution imaging opens up a new discovery space for investigating the CGM, it also challenges numerical simulations with respect to explaining and reproducing the exquisitely complex structures revealed by the observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10993v2-abstract-full').style.display = 'none'; document.getElementById('2410.10993v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures, 1 table, accepted by A&A Letter</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, L1 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.03827">arXiv:2410.03827</a> <span> [<a href="https://arxiv.org/pdf/2410.03827">pdf</a>, <a href="https://arxiv.org/format/2410.03827">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Quasar-Anchored Protocluster at z=6.6 in the ASPIRE Survey: II. An Environmental Analysis of Galaxy Properties in an Overdense Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Bosman%2C+S+E+I">Sarah E. I. Bosman</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+T">Tiago Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Habouzit%2C+M">Melanie Habouzit</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">Federica Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">Alessandro Lupi</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">Chiara Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pudoka%2C+M">Maria Pudoka</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ruiz%2C+S">Sofia Rojas-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Tee%2C+W+L">Wei Leong Tee</a>, <a href="/search/astro-ph?searchtype=author&query=Trebitsch%2C+M">Maxime Trebitsch</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haowen Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhuang%2C+M">Ming-Yang Zhuang</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+S">Siwei Zou</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="2410.03827v1-abstract-short" style="display: inline;"> We present paper II comprising a 35 arcmin$^2$ JWST/NIRCam imaging and wide-field slitless spectroscopy mosaic centered on J0305$-$3150, a luminous quasar at $z=6.61$. The F356W grism data reveals 124 [OIII]+H$尾$ emitters at $5.3<z<7$, 53 of which constitute a protocluster spanning (10 cMpc)$^2$ across $6.5<z<6.8$. We find no evidence of any broad-line AGN in individual galaxies or stacking, repor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03827v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03827v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03827v1-abstract-full" style="display: none;"> We present paper II comprising a 35 arcmin$^2$ JWST/NIRCam imaging and wide-field slitless spectroscopy mosaic centered on J0305$-$3150, a luminous quasar at $z=6.61$. The F356W grism data reveals 124 [OIII]+H$尾$ emitters at $5.3<z<7$, 53 of which constitute a protocluster spanning (10 cMpc)$^2$ across $6.5<z<6.8$. We find no evidence of any broad-line AGN in individual galaxies or stacking, reporting a median H$尾$ FWHM of 585 $\pm$ 152 km s$^{-1}$; however, the mass-excitation diagram and ``little red dot" color and compactness criteria suggest that there are a few AGN candidates on the outskirts of the protocluster. We fit the spectral energy distributions (SEDs) of the [OIII] emitters with Prospector and Bagpipes, and find that none of the SED-derived properties (stellar mass, age, or star formation rate) correlates with proximity to the quasar. While there is no correlation between galaxy age and local galaxy density, we find modest correlations between local galaxy density with increasing stellar mass, decreasing 10-to-100 Myr star formation rate ratios and decreasing nebular line equivalent widths. We further find that the protocluster galaxies are consistent with being more massive, older, and hosting higher star formation rates than the field sample at the 3$蟽$ level, distributed in a filamentary structure which supports inside-out formation of the protocluster. There is modest evidence that galaxy evolution proceeds differently as a function of the density of local environment within protoclusters during the epoch of reionization, and the central quasar has little effect on the galaxy properties of the surrounding structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03827v1-abstract-full').style.display = 'none'; document.getElementById('2410.03827v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">accepted to ApJ. 24 pages, 13 figures. Paper I by Champagne+24a is also available on arxiv today</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.03826">arXiv:2410.03826</a> <span> [<a href="https://arxiv.org/pdf/2410.03826">pdf</a>, <a href="https://arxiv.org/format/2410.03826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Quasar-Anchored Protocluster at z=6.6 in the ASPIRE Survey: I. Properties of [OIII] Emitters in a 10 Mpc Overdensity Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haowen Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Bosman%2C+S+E+I">Sarah E. I. Bosman</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+T">Tiago Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Eilers%2C+A">Anna-Christina Eilers</a>, <a href="/search/astro-ph?searchtype=author&query=Endsley%2C+R">Ryan Endsley</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">Xiaojing Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">Federica Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">Alessandro Lupi</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">Chiara Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pudoka%2C+M">Maria Pudoka</a>, <a href="/search/astro-ph?searchtype=author&query=Protu%C5%A1ov%C3%A0%2C+K">Klaudia Protu拧ov脿</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ruiz%2C+S">Sofia Rojas-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Tee%2C+W+L">Wei Leong Tee</a>, <a href="/search/astro-ph?searchtype=author&query=Trebitsch%2C+M">Maxime Trebitsch</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.03826v1-abstract-short" style="display: inline;"> ASPIRE (A SPectroscopic survey of bIased halos in the Reionization Era) is a quasar legacy survey primarily using JWST to target a sample of 25 $z>6$ quasars with NIRCam slitless spectroscopy and imaging. The first study in this series found evidence of a strong overdensity of galaxies around J0305-3150, a luminous quasar at $z=6.61$, within a single NIRCam pointing obtained in JWST Cycle 1. Here,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03826v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03826v1-abstract-full" style="display: none;"> ASPIRE (A SPectroscopic survey of bIased halos in the Reionization Era) is a quasar legacy survey primarily using JWST to target a sample of 25 $z>6$ quasars with NIRCam slitless spectroscopy and imaging. The first study in this series found evidence of a strong overdensity of galaxies around J0305-3150, a luminous quasar at $z=6.61$, within a single NIRCam pointing obtained in JWST Cycle 1. Here, we present the first results of a JWST Cycle 2 mosaic that covers 35 arcmin$^2$ with NIRCam imaging/WFSS of the same field to investigate the spatial extent of the putative protocluster. The F356W grism data targets [OIII]+H$尾$ at $5.3<z<7$ and reveals a population of 124 line emitters down to a flux limit of 1.2$\times$10$^{-18}$ erg s$^{-1}$ cm$^{-2}$. Fifty-three of these galaxies lie at $6.5<z<6.8$ spanning 10 cMpc on the sky, corresponding to an overdensity within a 2500 cMpc$^3$ volume of 12.5 $\pm$ 2.6, anchored by the quasar. Comparing to the [OIII] luminosity function from the Emission line galaxies and Intergalactic Gas in the Epoch of Reionization (EIGER) project, we find a dearth of faint [OIII] emitters at log(L/erg s$^{-1}$) $<$ 42.3, which we suggest is consistent with either bursty star formation causing galaxies to scatter around the grism detection limit or modest suppression from quasar feedback. While we find a strong filamentary overdensity of [OIII] emitters consistent with a protocluster, we suggest that we could be insensitive to a population of older, more massive Lyman-break galaxies with weak nebular emission on scales $>10$ cMpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03826v1-abstract-full').style.display = 'none'; document.getElementById('2410.03826v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">submitted to ApJ june 2024. 18 pages, 7 figures. companion paper II by Champagne+24b is also available on arXiv today</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.02315">arXiv:2410.02315</a> <span> [<a href="https://arxiv.org/pdf/2410.02315">pdf</a>, <a href="https://arxiv.org/format/2410.02315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Extragalactic fast X-ray transient from a weak relativistic jet associated with a Type Ic-BL supernova </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">H. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+W+-">W. -X. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+L+-">L. -D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">H. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X+-">X. -F. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">W. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">A. V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+D">D. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">T. An</a>, <a href="/search/astro-ph?searchtype=author&query=Ai%2C+S">S. Ai</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+T+G">T. G. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y+-">Y. -Q. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+C+-">C. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q+-">Q. -Y. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X+-">X. -F. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Y. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B+-">B. -B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W+-">W. -K. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+T">T. Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+Z+-">Z. -G. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Delaunay%2C+J">J. Delaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Elias-Rosa%2C+N">N. Elias-Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Benetti%2C+S">S. Benetti</a> , et al. (140 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.02315v1-abstract-short" style="display: inline;"> Massive stars end their life as core-collapse supernovae, amongst which some extremes are Type Ic broad-lined supernovae associated with long-duration gamma-ray bursts (LGRBs) having powerful relativistic jets. Their less-extreme brethren make unsuccessful jets that are choked inside the stars, appearing as X-ray flashes or low-luminosity GRBs. On the other hand, there exists a population of extra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02315v1-abstract-full').style.display = 'inline'; document.getElementById('2410.02315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.02315v1-abstract-full" style="display: none;"> Massive stars end their life as core-collapse supernovae, amongst which some extremes are Type Ic broad-lined supernovae associated with long-duration gamma-ray bursts (LGRBs) having powerful relativistic jets. Their less-extreme brethren make unsuccessful jets that are choked inside the stars, appearing as X-ray flashes or low-luminosity GRBs. On the other hand, there exists a population of extragalactic fast X-ray transients (EFXTs) with timescales ranging from seconds to thousands of seconds, whose origins remain obscure. Known sources that contribute to the observed EFXT population include the softer analogs of LGRBs, shock breakouts of supernovae, or unsuccessful jets. Here, we report the discovery of the bright X-ray transient EP240414a detected by the Einstein Probe (EP), which is associated with the Type Ic supernova SN 2024gsa at a redshift of 0.401. The X-ray emission evolution is characterised by a very soft energy spectrum peaking at < 1.3 keV, which makes it distinct from known LGRBs, X-ray flashes, or low-luminosity GRBs. Follow-up observations at optical and radio bands revealed the existence of a weak relativistic jet that interacts with an extended shell surrounding the progenitor star. Located on the outskirts of a massive galaxy, this event reveals a new population of explosions of Wolf-Rayet stars characterised by a less powerful engine that drives a successful but weak jet, possibly owing to a progenitor star with a smaller core angular momentum than in traditional LGRB progenitors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02315v1-abstract-full').style.display = 'none'; document.getElementById('2410.02315v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 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">43 pages, 9 figures, 4 tables, submitted. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01886">arXiv:2410.01886</a> <span> [<a href="https://arxiv.org/pdf/2410.01886">pdf</a>, <a href="https://arxiv.org/format/2410.01886">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Nonparametric Morphological Analysis of H$伪$ Emission in Bright Dwarfs Using the Merian Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mintz%2C+A">Abby Mintz</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Kado-Fong%2C+E">Erin Kado-Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Danieli%2C+S">Shany Danieli</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jiaxuan Li</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+Y">Yifei Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Leauthaud%2C+A">Alexie Leauthaud</a>, <a href="/search/astro-ph?searchtype=author&query=Baldassare%2C+V">Vivienne Baldassare</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+S">Song Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Peter%2C+A+H+G">Annika H. G. Peter</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+J">Joy Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y">Yue Pan</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="2410.01886v1-abstract-short" style="display: inline;"> Using medium-band imaging from the newly released Merian Survey, we conduct a nonparametric morphological analysis of H$伪$ emission maps and stellar continua for a sample of galaxies with $8\lesssim\log (M_\star/M_\odot) < 10.3$ at $0.064<z<0.1$. We present a novel method for estimating the stellar continuum emission through the Merian Survey's N708 medium-band filter, which we use to measure H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01886v1-abstract-full').style.display = 'inline'; document.getElementById('2410.01886v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01886v1-abstract-full" style="display: none;"> Using medium-band imaging from the newly released Merian Survey, we conduct a nonparametric morphological analysis of H$伪$ emission maps and stellar continua for a sample of galaxies with $8\lesssim\log (M_\star/M_\odot) < 10.3$ at $0.064<z<0.1$. We present a novel method for estimating the stellar continuum emission through the Merian Survey's N708 medium-band filter, which we use to measure H$伪$ emission and produce H$伪$ maps for our sample of galaxies with seven-band Merian photometry and available spectroscopy. We measure nonparametric morphological statistics for the H$伪$ and stellar continuum images, explore how the morphology of the H$伪$ differs from the continuum, and investigate how the parameters evolve with the galaxies' physical properties. In agreement with previous results for more massive galaxies, we find that the asymmetry of the stellar continuum increases with specific star formation rate (SSFR) and we extend the trend to lower masses, also showing that it holds for the asymmetry of the H$伪$ emission. We find that the lowest-mass galaxies with the highest SSFR have H$伪$ emission that is consistently heterogeneous and compact, while the less active galaxies in this mass range have H$伪$ emission that appears diffuse. At higher masses, our data do not span a sufficient range in SSFR to evaluate whether similar trends apply. We conclude that high SSFRs in low-mass galaxies likely result from dynamical instabilities that compress a galaxy's molecular gas to a dense region near the center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01886v1-abstract-full').style.display = 'none'; document.getElementById('2410.01886v1-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, 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">33 pages, 15 figures, 2 tables. Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01884">arXiv:2410.01884</a> <span> [<a href="https://arxiv.org/pdf/2410.01884">pdf</a>, <a href="https://arxiv.org/format/2410.01884">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Merian: A Wide-Field Imaging Survey of Dwarf Galaxies at z~0.06-0.10 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Danieli%2C+S">Shany Danieli</a>, <a href="/search/astro-ph?searchtype=author&query=Kado-Fong%2C+E">Erin Kado-Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+S">Song Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+Y">Yifei Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T+S">Ting S Li</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Leauthaud%2C+A">Alexie Leauthaud</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Mintz%2C+A">Abby Mintz</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">Xiaojing Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jiaxuan Li</a>, <a href="/search/astro-ph?searchtype=author&query=Baldassare%2C+V">Vivienne Baldassare</a>, <a href="/search/astro-ph?searchtype=author&query=Banerjee%2C+A">Arka Banerjee</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+J">Joy Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Blanco%2C+D">Diana Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+A">Alyson Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xinjun Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz%2C+A">Akaxia Cruz</a>, <a href="/search/astro-ph?searchtype=author&query=Geda%2C+R">Robel Geda</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+R">Runquan Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+S">Sean Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kannawadi%2C+A">Arun Kannawadi</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S+Y">Stacy Y. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.01884v2-abstract-short" style="display: inline;"> We present the Merian Survey, an optical imaging survey optimized for studying the physical properties of bright star-forming dwarf galaxies. Merian is carried out with two medium-band filters ($N708$ and $N540$, centered at $708$ and $540$ nm), custom-built for the Dark Energy Camera (DECam) on the Blanco telescope. Merian covers $\sim 750\,\mathrm{deg}^2$ of equatorial fields, overlapping with t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01884v2-abstract-full').style.display = 'inline'; document.getElementById('2410.01884v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01884v2-abstract-full" style="display: none;"> We present the Merian Survey, an optical imaging survey optimized for studying the physical properties of bright star-forming dwarf galaxies. Merian is carried out with two medium-band filters ($N708$ and $N540$, centered at $708$ and $540$ nm), custom-built for the Dark Energy Camera (DECam) on the Blanco telescope. Merian covers $\sim 750\,\mathrm{deg}^2$ of equatorial fields, overlapping with the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) wide, deep, and ultra-deep fields. When combined with the HSC-SSP imaging data ($grizy$), the new Merian DECam medium-band imaging allows for photometric redshift measurements via the detection of H$\rm伪$ and [OIII] line emission flux excess in the $N708$ and $N540$ filters, respectively, at $0.06<z<0.10$. We present an overview of the survey design, observations taken to date, data reduction using the LSST Science Pipelines, including aperture-matched photometry for accurate galaxy colors, and a description of the data included in the first data release (DR1). The key science goals of Merian include: probing the dark matter halos of dwarf galaxies out to their virial radii using high signal-to-noise weak lensing profile measurements, decoupling the effects of baryonic processes from dark matter, and understanding the role of black holes in dwarf galaxy evolution. This rich dataset will also offer unique opportunities for studying extremely metal-poor galaxies via their strong [OIII] emission and H$\rm伪$ lines, as well as [OIII] emitters at $z\sim 0.4$, and Ly$\rm伪$ emitters at $z\sim 3.3$ and $z\sim 4.8$. Merian showcases the power of utilizing narrow and medium-band filters alongside broad-band filters for sky imaging, demonstrating their synergistic capacity to unveil astrophysical insights across diverse astrophysical phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01884v2-abstract-full').style.display = 'none'; document.getElementById('2410.01884v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 13 figures, 2 tables. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01318">arXiv:2410.01318</a> <span> [<a href="https://arxiv.org/pdf/2410.01318">pdf</a>, <a href="https://arxiv.org/format/2410.01318">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [OIII] Emitters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Kakiichi%2C+K">Koki Kakiichi</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+R+A">Romain A. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+G+D">George D. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+S">Siwei Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">Valentina D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Yue%2C+M">Minghao Yue</a>, <a href="/search/astro-ph?searchtype=author&query=Bosman%2C+S+E+I">Sarah E. I. Bosman</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Eilers%2C+A">Anna-Christina Eilers</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zihao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Pudoka%2C+M">Maria Pudoka</a>, <a href="/search/astro-ph?searchtype=author&query=Satyavolu%2C+S">Sindhu Satyavolu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Tee%2C+W+L">Wei Leong Tee</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Yunjing Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.01318v1-abstract-short" style="display: inline;"> Understanding when and how reionization happened is crucial for studying the early structure formation and the properties of first galaxies in the Universe. At $z>5.5$, the observed IGM optical depth shows a significant scatter, indicating an inhomogeneous reionization process. However, the nature of the inhomogeneous reionization remains debated. ASPIRE is a JWST Cycle 1 program that has spectros… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01318v1-abstract-full').style.display = 'inline'; document.getElementById('2410.01318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01318v1-abstract-full" style="display: none;"> Understanding when and how reionization happened is crucial for studying the early structure formation and the properties of first galaxies in the Universe. At $z>5.5$, the observed IGM optical depth shows a significant scatter, indicating an inhomogeneous reionization process. However, the nature of the inhomogeneous reionization remains debated. ASPIRE is a JWST Cycle 1 program that has spectroscopically identified $>400$ [OIII] emitters in 25 quasar fields at $z>6.5$. Combined with deep ground-based optical spectroscopy of ASPIRE quasars, ASPIRE program provides the current largest sample for IGM-galaxy connection studies during cosmic reionization. We present the first results of IGM effective optical depth measurements around [OIII] emitters using 14 ASPIRE quasar fields. We find the IGM transmission is tightly related with reionization-era galaxies to the extent that significant excess of Ly$伪$ transmission exists around [OIII] emitters. We measure the stacked IGM effective optical depth of IGM patches associated with [OIII] emitters and find they reach the same IGM effective optical depth at least dz~0.1 ahead of those IGM patches where no [OIII] emitters are detected, supporting earlier reionization around [OIII] emitters. Our results indicate an enhancement in IGM Ly$伪$ transmission around [OIII] emitters at scales beyond 25 $h^{-1}$ cMpc, consistent with the predicted topology of reionization from fluctuating UV background (UVB) models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01318v1-abstract-full').style.display = 'none'; document.getElementById('2410.01318v1-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, 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">27 pages, 19 figures, 1 table, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.13189">arXiv:2409.13189</a> <span> [<a href="https://arxiv.org/pdf/2409.13189">pdf</a>, <a href="https://arxiv.org/format/2409.13189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Fast Outflow in the Host Galaxy of the Luminous z $=$ 7.5 Quasar J1007$+$2115 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Barth%2C+A+J">Aaron J. Barth</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+T">Tiago Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">Roberto Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Eilers%2C+A">Anna-Christina Eilers</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">Federica Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Farina%2C+E+P">Emanuele Paolo Farina</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">Alessandro Lupi</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Zhiwei Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Pudoka%2C+M">Maria Pudoka</a>, <a href="/search/astro-ph?searchtype=author&query=Zhuang%2C+M">Ming-Yang Zhuang</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Huan Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Tee%2C+W+L">Wei Leong Tee</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.13189v1-abstract-short" style="display: inline;"> James Webb Space Telescope opens a new window to directly probe luminous quasars powered by billion solar mass black holes in the epoch of reionization and their co-evolution with massive galaxies with unprecedented details. In this paper, we report the first results from the deep NIRSpec integral field spectroscopy study of a quasar at $z = 7.5$. We obtain a bolometric luminosity of $\sim$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13189v1-abstract-full').style.display = 'inline'; document.getElementById('2409.13189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.13189v1-abstract-full" style="display: none;"> James Webb Space Telescope opens a new window to directly probe luminous quasars powered by billion solar mass black holes in the epoch of reionization and their co-evolution with massive galaxies with unprecedented details. In this paper, we report the first results from the deep NIRSpec integral field spectroscopy study of a quasar at $z = 7.5$. We obtain a bolometric luminosity of $\sim$$1.8\times10^{47}$ erg s$^{-1}$ and a black hole mass of $\sim$0.7--2.5$\times10^{9}$ M$_{\odot}$ based on H$尾$ emission line from the quasar spectrum. We discover $\sim$2 kpc scale, highly blueshifted ($\sim$$-$870 km/s) and broad ($\sim$1400 km/s) [O III] line emission after the quasar PSF has been subtracted. Such line emission most likely originates from a fast, quasar-driven outflow, the earliest one on galactic-scale known so far. The dynamical properties of this outflow fall within the typical ranges of quasar-driven outflows at lower redshift, and the outflow may be fast enough to reach the circumgalactic medium. Combining both the extended and nuclear outflow together, the mass outflow rate, $\sim$300 M$_{\odot}$yr, is $\sim$60%--380% of the star formation rate of the quasar host galaxy, suggesting that the outflow may expel a significant amount of gas from the inner region of the galaxy. The kinetic energy outflow rate, $\sim$3.6$\times10^{44}$ erg s$^{-1}$, is $\sim$0.2% of the quasar bolometric luminosity, which is comparable to the minimum value required for negative feedback based on simulation predictions. The dynamical timescale of the extended outflow is $\sim$1.7 Myr, consistent with the typical quasar lifetime in this era. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13189v1-abstract-full').style.display = 'none'; document.getElementById('2409.13189v1-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> 19 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03011">arXiv:2409.03011</a> <span> [<a href="https://arxiv.org/pdf/2409.03011">pdf</a>, <a href="https://arxiv.org/format/2409.03011">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad8446">10.3847/1538-4357/ad8446 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New IW And-Type Star: Karachurin 12 with Tilted Disks and Diverse cycles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qin-Mei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+P">Ping Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.03011v2-abstract-short" style="display: inline;"> The IW And-type phenomenon in cataclysmic variables presents a significant challenge to the accretion disk instability model. Using photometric data from the All-Sky Automated Survey for Supernovae, the Zwicky Transient Facility, and the Transiting Exoplanet Survey Satellite, we identify Karachurin 12 as a new non-eclipsing IW And-type object with a cycle period of 35.69(3) days. We also report fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03011v2-abstract-full').style.display = 'inline'; document.getElementById('2409.03011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03011v2-abstract-full" style="display: none;"> The IW And-type phenomenon in cataclysmic variables presents a significant challenge to the accretion disk instability model. Using photometric data from the All-Sky Automated Survey for Supernovae, the Zwicky Transient Facility, and the Transiting Exoplanet Survey Satellite, we identify Karachurin 12 as a new non-eclipsing IW And-type object with a cycle period of 35.69(3) days. We also report for the first time that Karachurin 12 is a negative superhump (NSH) system featuring a precessing tilted disks, with precession, orbital, and NSH periods of 4.9588(2) days, 0.3168895(13) days, and 0.2979861(8) days, respectively. Our analysis, using dips as index and NSHs as probe, reveals diverse cycle patterns in Karachurin 12, with NSH amplitude varying throughout the cycle. These findings offer new insights for studying tilted disks and the IW And-type phenomenon. The mass-transfer burst model has difficulty explaining the observed variations in NSH amplitude, especially given the uncertainty surrounding the origin of the mass transfer burst. Meanwhile, the tilted thermally unstable disk model indicates a possible connection to the IW And-type phenomenon, but it also struggles to account for the detailed variations in Karachurin 12. Therefore, a wider range of factors must be considered to fully understand the complex changes in Karachurin 12. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03011v2-abstract-full').style.display = 'none'; document.getElementById('2409.03011v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">20 pages, 9 figures and 3 tables, accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02480">arXiv:2409.02480</a> <span> [<a href="https://arxiv.org/pdf/2409.02480">pdf</a>, <a href="https://arxiv.org/format/2409.02480">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div 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/ad631a">10.3847/1538-4357/ad631a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A brown dwarf orbiting around the planetary-nebula central binary KV Vel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S+-">S. -B. Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L+-">L. -Y. Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F+-">F. -X. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+L+-">L. -J. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+Z+-">Z. -T. Han</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+J+-">J. -J. He</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+L">L. Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+L+-">L. -F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q+-">Q. -B. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M+-">M. -Y. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H+-">H. -T. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+F+-">F. -Z. Yan</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="2409.02480v1-abstract-short" style="display: inline;"> KV Vel is a non-eclipsing short-period (P = 0.3571 days) close binary containing a very hot subdwarf primary (77000 K) and a cool low-mass secondary star (3400 K) that is located at the center of the planetary nebula DS 1. The changes in the orbital period of the close binary were analyzed based on 262 new times of light maximum together with those compiled from the literature. It is discovered th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02480v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02480v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02480v1-abstract-full" style="display: none;"> KV Vel is a non-eclipsing short-period (P = 0.3571 days) close binary containing a very hot subdwarf primary (77000 K) and a cool low-mass secondary star (3400 K) that is located at the center of the planetary nebula DS 1. The changes in the orbital period of the close binary were analyzed based on 262 new times of light maximum together with those compiled from the literature. It is discovered that the O-C curve shows a small-amplitude (0.0034 days) cyclic period variation with a period of 29.55 years. The explanation by the solar-type magnetic activity cycles of the cool component is ruled out because the required energies are much larger than the total radiant energy of this component in a whole cycle. Therefore, the cyclic variation was plausibly explained as the light-travel time effect via the presence of a tertiary component, which is supported by the periodic changes of the O-C curve and the rather symmetric and stable light curves obtained by TESS. The mass of the tertiary companion is determined to be M_3sini' = 0.060(7) M_sun. If the third body is coplanar with the central binary (i.e., i' = 62.5掳), the mass of the tertiary component is computed as M_3 ~ 0.068 M\sun, and thus it would be below the stable hydrogen-burning limit and is a brown dwarf. The orbital separation is shorter than 9.35 astronomical units (AU). KV Vel together with its surrounding planetary nebula and the brown-dwarf companion may be formed through the common-envelope evolution after the primary filled its Roche lobe during the early asymptotic giant branch stage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02480v1-abstract-full').style.display = 'none'; document.getElementById('2409.02480v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.01098">arXiv:2409.01098</a> <span> [<a href="https://arxiv.org/pdf/2409.01098">pdf</a>, <a href="https://arxiv.org/format/2409.01098">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"> Forecasts on Anisotropic Cosmic Birefringence Constraints for CMB Experiment in the Northern Hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhong%2C+Y">Yiwei Zhong</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Si-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingzhe Li</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+W">Wenjuan Fang</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="2409.01098v1-abstract-short" style="display: inline;"> The study of cosmic birefringence through Cosmic Microwave Background (CMB) experiments is a key research area in cosmology and particle physics, providing a critical test for Lorentz and CPT symmetries. This paper focuses on an upcoming CMB experiment in the mid-latitude of the Northern Hemisphere, and investigates the potential to detect anisotropies in cosmic birefringence. Applying a quadratic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.01098v1-abstract-full').style.display = 'inline'; document.getElementById('2409.01098v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.01098v1-abstract-full" style="display: none;"> The study of cosmic birefringence through Cosmic Microwave Background (CMB) experiments is a key research area in cosmology and particle physics, providing a critical test for Lorentz and CPT symmetries. This paper focuses on an upcoming CMB experiment in the mid-latitude of the Northern Hemisphere, and investigates the potential to detect anisotropies in cosmic birefringence. Applying a quadratic estimator on simulated polarization data, we reconstruct the power spectrum of anisotropic cosmic birefringence successfully and estimate constraints on the amplitude of the spectrum, $A_{\mathrm{CB}}$, assuming scale invariance. The forecast is based on a wide-scan observation strategy during winter, yielding an effective sky coverage of approximately 23.6%. We consider two noise scenarios corresponding to the short-term and long-term phases of the experiment. Our results show that with a small aperture telescope operating at 95/150GHz, the $2蟽$ upper bound for $A_{\mathrm{CB}}$ can reach 0.017 under the low noise scenario when adopting the method of merging multi-frequency data in map domain, and merging multi-frequency data in spectrum domain tightens the limit by about 10%.A large-aperture telescope with the same bands is found to be more effective, tightening the $2蟽$ upper limit to 0.0062. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.01098v1-abstract-full').style.display = 'none'; document.getElementById('2409.01098v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">18 pages, 2 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/2408.08589">arXiv:2408.08589</a> <span> [<a href="https://arxiv.org/pdf/2408.08589">pdf</a>, <a href="https://arxiv.org/format/2408.08589">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yingxiao Song</a>, <a href="/search/astro-ph?searchtype=author&query=Xiong%2C+Q">Qi Xiong</a>, <a href="/search/astro-ph?searchtype=author&query=Gong%2C+Y">Yan Gong</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+F">Furen Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+K+C">Kwan Chuen Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xuelei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Q">Qi Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+G">Guoliang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yun Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+Y">Yu Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Pei%2C+W">Wenxiang Pei</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+C">Chengliang Wei</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.08589v2-abstract-short" style="display: inline;"> The void power spectrum is related to the clustering of low-density regions in the large-scale structure (LSS) of the Universe, and can be used as an effective cosmological probe to extract the information of the LSS. We generate the galaxy mock catalogs from Jiutian simulation, and identify voids using the watershed algorithm for studying the cosmological constraint strength of the China Space St… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.08589v2-abstract-full').style.display = 'inline'; document.getElementById('2408.08589v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.08589v2-abstract-full" style="display: none;"> The void power spectrum is related to the clustering of low-density regions in the large-scale structure (LSS) of the Universe, and can be used as an effective cosmological probe to extract the information of the LSS. We generate the galaxy mock catalogs from Jiutian simulation, and identify voids using the watershed algorithm for studying the cosmological constraint strength of the China Space Station Telescope (CSST) spectroscopic survey. The galaxy and void auto power spectra and void-galaxy cross power spectra at $z=0.3$, 0.6, and 0.9 are derived from the mock catalogs. To fit the full power spectra, we propose to use the void average effective radius at a given redshift to simplify the theoretical model, and adopt the Markov Chain Monte Carlo (MCMC) technique to implement the constraints on the cosmological and void parameters. The systematical parameters, such as galaxy and void biases, and noise terms in the power spectra are also included in the fitting process. We find that our theoretical model can correctly extract the cosmological information from the galaxy and void power spectra, which demonstrates its feasibility and effectivity. The joint constraint accuracy of the cosmological parameters can be improved by $\sim20\%$ compared to that from the galaxy power spectrum only. The fitting results of the void density profile and systematical parameters are also well constrained and consistent with the expectation. This indicates that the void clustering measurement can be an effective complement to the galaxy clustering probe, especially for the next generation galaxy surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.08589v2-abstract-full').style.display = 'none'; document.getElementById('2408.08589v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 5 figures, 2 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.07761">arXiv:2408.07761</a> <span> [<a href="https://arxiv.org/pdf/2408.07761">pdf</a>, <a href="https://arxiv.org/format/2408.07761">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The effects of the carbon-to-oxygen ratio on the condensate compositions around Solar-like stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shakespeare%2C+C+J">Cody J. Shakespeare</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min Li</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+S">Shichun Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+Z">Zhaohuan Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Steffen%2C+J+H">Jason H. Steffen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.07761v1-abstract-short" style="display: inline;"> The initial stellar carbon-to-oxygen (C/O) ratio can have a large impact on the resulting condensed species present in the protoplanetary disk and, hence, the composition of the bodies and planets that form. The observed C/O ratios of stars can vary from 0.1-2. We use a sequential dust condensation model to examine the impact of the C/O ratio on the composition of solids around a Solar-like star.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07761v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07761v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07761v1-abstract-full" style="display: none;"> The initial stellar carbon-to-oxygen (C/O) ratio can have a large impact on the resulting condensed species present in the protoplanetary disk and, hence, the composition of the bodies and planets that form. The observed C/O ratios of stars can vary from 0.1-2. We use a sequential dust condensation model to examine the impact of the C/O ratio on the composition of solids around a Solar-like star. We utilize this model in a focused examination of the impact of varying the initial stellar C/O ratio to isolate the effects of the C/O ratio in the context of Solar-like stars. We describe three different system types in our findings. The Solar system falls into the silicate-dominant, low C/O ratio systems which end at a stellar C/O ratio somewhere between 0.52 and 0.6. At C/O ratios between about 0.6 and 0.9, we have intermediate systems. Intermediate systems show a decrease in silicates while carbides begin to become significant. Carbide-dominant systems begin around a C/O ratio of 0.9. Carbide-dominant systems exhibit high carbide surface densities at inner radii with comparable levels of carbides and silicates at outer radii. Our models show that changes between C/O=0.8 and C/O=1 are more significant than previous studies, that carbon can exceed 80% of the condensed mass, and that carbon condensation can be significant at radii up to 6 AU. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07761v1-abstract-full').style.display = 'none'; document.getElementById('2408.07761v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.07102">arXiv:2408.07102</a> <span> [<a href="https://arxiv.org/pdf/2408.07102">pdf</a>, <a href="https://arxiv.org/format/2408.07102">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Anisotropic Circumgalactic Medium of Sub-L$^*$ Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Huanian Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Miao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.07102v1-abstract-short" style="display: inline;"> Using stacked emission line flux measurements of cool circumgalactic gas (CGM) in lower-mass galaxies ($10^{9.0} \le M_*/M_\odot \le 10^{10.2} $), we measure the dependence of the emission characteristics on orientation relative to the disk plane as a function of radius and compare to that we found previously for massive ($M_* > 10^{10.4} M_\odot$) early-type galaxies. Although the line ratios (th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07102v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07102v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07102v1-abstract-full" style="display: none;"> Using stacked emission line flux measurements of cool circumgalactic gas (CGM) in lower-mass galaxies ($10^{9.0} \le M_*/M_\odot \le 10^{10.2} $), we measure the dependence of the emission characteristics on orientation relative to the disk plane as a function of radius and compare to that we found previously for massive ($M_* > 10^{10.4} M_\odot$) early-type galaxies. Although the line ratios (the lower [N II]/H$伪$ and [O III]/H$尾$) suggest an overall softer ionizing source than in the more massive galaxies, consistent with previous findings, we find the same ionization hardening signature (a higher [N II]/H$伪$ ratio in the inner polar region) along the polar direction at small radii that we found for the more massive galaxies. The line ratio in the inner polar bin is distinct from that measured for the inner planar bin with 99.99% confidence and with $>$ 99.9% confidence we conclude that it lies outside the star formation regime. The effective hardening of the ionization of the CGM along the polar axis, at small radii, could either indicate relic effects of AGN activity or shock ionization. In either case, this signature appears to be ubiquitous across the stellar mass range we are able to explore with our spectral stacking technique and currently available archival data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07102v1-abstract-full').style.display = 'none'; document.getElementById('2408.07102v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in ApJ, 8 pages. arXiv admin note: text overlap with arXiv:2210.10043</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.01019">arXiv:2408.01019</a> <span> [<a href="https://arxiv.org/pdf/2408.01019">pdf</a>, <a href="https://arxiv.org/format/2408.01019">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+A">Ai-Ying Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Liao%2C+W">Wen-Ping Liao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+E">Er-Gang Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+X">Xiang-Dong Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.01019v1-abstract-short" style="display: inline;"> Heartbeat stars (HBSs) with tidally excited oscillations (TEOs) are ideal astrophysical laboratories for studying the internal properties of the systems. In this paper, five new HBSs exhibiting TEOs are discovered using TESS photometric data. The orbital parameters are derived using a corrected version of Kumar et al.'s model based on the Markov Chain Monte Carlo (MCMC) method. The TEOs in these o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01019v1-abstract-full').style.display = 'inline'; document.getElementById('2408.01019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.01019v1-abstract-full" style="display: none;"> Heartbeat stars (HBSs) with tidally excited oscillations (TEOs) are ideal astrophysical laboratories for studying the internal properties of the systems. In this paper, five new HBSs exhibiting TEOs are discovered using TESS photometric data. The orbital parameters are derived using a corrected version of Kumar et al.'s model based on the Markov Chain Monte Carlo (MCMC) method. The TEOs in these objects are examined, and their pulsation phases and modes are identified. The pulsation phases of the TEOs in TIC 266809405, TIC 266894805, and TIC 412881444 are consistent with the dominant $l=2$, $m=0$, or $\pm2$ spherical harmonic. For TIC 11619404, although the TEO phase is close to the $m=+2$ mode, the $m = 0$ mode cannot be excluded because of the low inclination in this system. The TEO phase in TIC 447927324 shows a large deviation ($>2蟽$) from the adiabatic expectations, suggesting that it is expected to be a traveling wave rather than a standing wave. In addition, these TEOs occur at relatively low orbital harmonics, and we cautiously suggest that this may be an observational bias. These objects are valuable sources for studying the structure and evolution of eccentricity orbit binaries and extending the TESS HBS catalog with TEOs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01019v1-abstract-full').style.display = 'none'; document.getElementById('2408.01019v1-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">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9pages, 5figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.18621">arXiv:2407.18621</a> <span> [<a href="https://arxiv.org/pdf/2407.18621">pdf</a>, <a href="https://arxiv.org/format/2407.18621">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div 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/stae2057">10.1093/mnras/stae2057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Twenty-three New Heartbeat Star Systems Discovered Based on TESS Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+A">Ai-Ying Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Liao%2C+W">Wen-Ping Liao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+E">Er-Gang Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+X">Xiang-Dong Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.18621v2-abstract-short" style="display: inline;"> Heartbeat stars (HBSs) are ideal astrophysical laboratories to study the formation and evolution of binary stars in eccentric orbits and the internal structural changes of their components under strong tidal action. We discover 23 new HBSs based on TESS photometric data. The orbital parameters, including orbital period, eccentricity, orbital inclination, argument of periastron, and epoch of perias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18621v2-abstract-full').style.display = 'inline'; document.getElementById('2407.18621v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.18621v2-abstract-full" style="display: none;"> Heartbeat stars (HBSs) are ideal astrophysical laboratories to study the formation and evolution of binary stars in eccentric orbits and the internal structural changes of their components under strong tidal action. We discover 23 new HBSs based on TESS photometric data. The orbital parameters, including orbital period, eccentricity, orbital inclination, argument of periastron, and epoch of periastron passage of these HBSs are derived by using a corrected version of Kumar et al.'s model based on the Markov Chain Monte Carlo (MCMC) method. The preliminary results show that these HBSs have orbital periods in the range from 2.7 to 20 days and eccentricities in the range from 0.08 to 0.70. The eccentricity-period relation of these objects shows a positive correlation between eccentricity and period, and also shows the existence of orbital circularization. The Hertzsprung-Russell diagram shows that the HBSs are not all located in a particular area. The distribution of the derived parameters suggests a selection bias within the TESS survey towards massive HBSs with shorter orbital periods, higher temperatures and luminosities. These objects are a very useful source to study the structure and evolution of eccentricity orbit binaries and to extend the TESS HBS catalog. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18621v2-abstract-full').style.display = 'none'; document.getElementById('2407.18621v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 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/2407.17570">arXiv:2407.17570</a> <span> [<a href="https://arxiv.org/pdf/2407.17570">pdf</a>, <a href="https://arxiv.org/format/2407.17570">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Broad-line AGN at $z=4-5$ revealed by JWST/NIRCam WFSS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">Xiaojing Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">Feige Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Volonteri%2C+M">Marta Volonteri</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jinyi Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Barth%2C+A">Aaron Barth</a>, <a href="/search/astro-ph?searchtype=author&query=Eilers%2C+A">Anna-Christina Eilers</a>, <a href="/search/astro-ph?searchtype=author&query=Farina%2C+E+P">Emanuele Paolo Farina</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+W">Weizhe Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+X">Xiangyu Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jun%2C+H+D">Hyunsung D. Jun</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">Alessandro Lupi</a>, <a href="/search/astro-ph?searchtype=author&query=Kakiichi%2C+K">Koki Kakiichi</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">Chiara Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Onoue%2C+M">Masafusa Onoue</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Zhiwei Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Pizzati%2C+E">Elia Pizzati</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ruiz%2C+S">Sof铆a Rojas-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Schindler%2C+J">Jan-Torge Schindler</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.17570v1-abstract-short" style="display: inline;"> Low-luminosity AGNs with low-mass black holes (BHs) in the early universe are fundamental to understanding the BH growth and their co-evolution with the host galaxies. Utilizing JWST NIRCam Wide Field Slitless Spectroscopy (WFSS), we perform a systematic search for broad-line ${\rm H伪}$ emitters (BHAEs) at $z\approx 4-5$ in 25 fields of the ASPIRE (A SPectroscopic survey of biased halos In the Rei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17570v1-abstract-full').style.display = 'inline'; document.getElementById('2407.17570v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.17570v1-abstract-full" style="display: none;"> Low-luminosity AGNs with low-mass black holes (BHs) in the early universe are fundamental to understanding the BH growth and their co-evolution with the host galaxies. Utilizing JWST NIRCam Wide Field Slitless Spectroscopy (WFSS), we perform a systematic search for broad-line ${\rm H伪}$ emitters (BHAEs) at $z\approx 4-5$ in 25 fields of the ASPIRE (A SPectroscopic survey of biased halos In the Reionization Era) project, covering a total area of 275 arcmin$^2$. We identify 16 BHAEs with FWHM of the broad components spanning from $\sim$ 1000 km s$^{-1}$ to 3000 km s$^{-1}$. Assuming the broad linewidths arise due to Doppler broadening around BHs, the implied BH masses range from $10^7$ to $10^{8}~M_\odot$, with broad ${\rm H伪}$-converted bolometric luminosity of $10^{44.5}-10^{45.5}$ erg s$^{-1}$ and Eddington ratios of $0.07-0.47$. The spatially extended structure of the F200W stacked image may trace the stellar light from the host galaxies. The ${\rm H伪}$ luminosity function indicates an increasing AGN fraction towards the higher ${\rm H伪}$ luminosities. We find possible evidence for clustering of BHAEs: two sources are at the same redshift with a projected separation of 519 kpc; one BHAE appears as a composite system residing in an overdense region with three close companion ${\rm H伪}$ emitters. Three BHAEs exhibit blueshifted absorption troughs indicative of the presence of high-column-density gas. We find the broad-line and photometrically selected BHAE samples exhibit different distributions in the optical continuum slopes, which can be attributed to their different selection methods. The ASPIRE broad-line ${\rm H伪}$ sample provides a good database for future studies of faint AGN populations at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17570v1-abstract-full').style.display = 'none'; document.getElementById('2407.17570v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 13 figures, 4 tables. Accepted by the ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.10892">arXiv:2407.10892</a> <span> [<a href="https://arxiv.org/pdf/2407.10892">pdf</a>, <a href="https://arxiv.org/format/2407.10892">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> First Indication of Solar $^8$B Neutrino Flux through Coherent Elastic Neutrino-Nucleus Scattering in PandaX-4T </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=PandaX+Collaboration"> PandaX Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bo%2C+Z">Zihao Bo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xun Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yunhua Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Z">Zhaokan Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+X">Xiangyi Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+Y">Yingjie Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+D">Deqing Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Z">Zhixing Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Geng%2C+L">Lisheng Geng</a>, <a href="/search/astro-ph?searchtype=author&query=Giboni%2C+K">Karl Giboni</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+X">Xunan Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+X">Xuyuan Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Z">Zichao Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Chencheng Han</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+K">Ke Han</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+C">Changda He</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+J">Jinrong He</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+D">Di Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+H">Houqi Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+J">Junting Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Hou%2C+R">Ruquan Hou</a>, <a href="/search/astro-ph?searchtype=author&query=Hou%2C+Y">Yu Hou</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+X">Xiangdong Ji</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.10892v3-abstract-short" style="display: inline;"> The PandaX-4T liquid xenon detector at the China Jinping Underground Laboratory is used to measure the solar $^8$B neutrino flux by detecting neutrinos through coherent scattering with xenon nuclei. Data samples requiring the coincidence of scintillation and ionization signals (paired), as well as unpaired ionization-only signals (US2), are selected with energy threshold of approximately 1.1 keV (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10892v3-abstract-full').style.display = 'inline'; document.getElementById('2407.10892v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10892v3-abstract-full" style="display: none;"> The PandaX-4T liquid xenon detector at the China Jinping Underground Laboratory is used to measure the solar $^8$B neutrino flux by detecting neutrinos through coherent scattering with xenon nuclei. Data samples requiring the coincidence of scintillation and ionization signals (paired), as well as unpaired ionization-only signals (US2), are selected with energy threshold of approximately 1.1 keV (0.33 keV) nuclear recoil energy. Combining the commissioning run and the first science run of PandaX-4T, a total exposure of 1.20 and 1.04 tonne$\cdot$year are collected for the paired and US2, respectively. After unblinding, 3 and 332 events are observed with an expectation of 2.8$\pm$0.5 and 251$\pm$32 background events, for the paired and US2 data, respectively. A combined analysis yields a best-fit $^8$B neutrino signal of 3.5 (75) events from the paired (US2) data sample, with $\sim$37\% uncertainty, and the background-only hypothesis is disfavored at 2.64$蟽$ significance. This gives a solar $^8$B neutrino flux of ($8.4\pm3.1$)$\times$10$^6$ cm$^{-2}$s$^{-1}$, consistent with the standard solar model prediction. It is also the first indication of solar $^8$B neutrino ``fog'' in a dark matter direct detection experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10892v3-abstract-full').style.display = 'none'; document.getElementById('2407.10892v3-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Physical Review Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04913">arXiv:2407.04913</a> <span> [<a href="https://arxiv.org/pdf/2407.04913">pdf</a>, <a href="https://arxiv.org/format/2407.04913">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div 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/ad6f05">10.3847/1538-4357/ad6f05 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tilted Disk Precession and Negative Superhumps in HS 2325+8205: A Multi-Window Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qin-Mei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+P">Ping Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04913v2-abstract-short" style="display: inline;"> Tilted disk precession exists in different objects. Negative superhumps (NSHs) in cataclysmic variable stars (CVs) are believed to arise from the interaction between the reverse precession of a tilted disk and the streams from the secondary star.Utilizing TESS photometry, we present a comprehensive investigation into the tilted disk precession and NSHs in the dwarf nova (DN) HS 2325+8205, employin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04913v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04913v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04913v2-abstract-full" style="display: none;"> Tilted disk precession exists in different objects. Negative superhumps (NSHs) in cataclysmic variable stars (CVs) are believed to arise from the interaction between the reverse precession of a tilted disk and the streams from the secondary star.Utilizing TESS photometry, we present a comprehensive investigation into the tilted disk precession and NSHs in the dwarf nova (DN) HS 2325+8205, employing eclipse minima, eclipse depths, NSH frequencies, and NSH amplitudes and the correlation between them as the windows. We identified NSHs with a period of 0.185671(17) days in HS 2325+8205. The NSH frequency exhibits variability with a period of 3.943(9) days, akin to the tilted disk precession period validated in novae-like stars (NLs, SDSS J0812) and intermediate polars (IPs, TV Col).The O-C of eclipse minima were similarly found to vary cyclically in period 4.135(5) days, characterized by a faster rise than fall. Furthermore, the NSH amplitude exhibits complex and diverse variations, which may be linked to changes in the disk radius, mass transfer rate, and the apparent area of the hot spot. For the first time in DNe, we observe bi-periodic variations in eclipse depth (P1= 4.131(4) d and P2= 2.065(2) d ~ Pprec/2), resembling those seen in IPs, suggesting that variations with P2 are not attributable to an accretion curtain, as previously suspected. Moreover, NSH amplitude and eclipse depth decrease with increasing NSH frequency, while NSH amplitude correlates positively with eclipse depth.These complex variations observed across multiple observational windows provide substantial evidence for understanding of tilted disk precession and NSHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04913v2-abstract-full').style.display = 'none'; document.getElementById('2407.04913v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 figures and 3 tables; accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18169">arXiv:2406.18169</a> <span> [<a href="https://arxiv.org/pdf/2406.18169">pdf</a>, <a href="https://arxiv.org/ps/2406.18169">ps</a>, <a href="https://arxiv.org/format/2406.18169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Timing and Scintillation Studies of Pulsars in Globular Cluster M3 (NGC 5272) with FAST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+B">Baoda Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+L">Li-yun Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Yao%2C+J">Jumei Yao</a>, <a href="/search/astro-ph?searchtype=author&query=Yin%2C+D">Dejiang Yin</a>, <a href="/search/astro-ph?searchtype=author&query=Eatough%2C+R+P">Ralph P. Eatough</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Minghui Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yifeng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lian%2C+Y">Yujie Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y">Yu Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+Y">Yinfeng Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yaowei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">Xingnan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+T">Tianhao Su</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Yuxiao Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">Kuo Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+L">Lei Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Zhichen Pan</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="2406.18169v1-abstract-short" style="display: inline;"> We present the phase-connected timing solutions of all the five pulsars in globular cluster (GC) M3 (NGC 5272), namely PSRs M3A to F (PSRs J1342+2822A to F), with the exception of PSR M3C, from FAST archival data. In these timing solutions, those of PSRs M3E, and F are obtained for the first time. We find that PSRs M3E and F have low mass companions, and are in circular orbits with periods of 7.1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18169v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18169v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18169v1-abstract-full" style="display: none;"> We present the phase-connected timing solutions of all the five pulsars in globular cluster (GC) M3 (NGC 5272), namely PSRs M3A to F (PSRs J1342+2822A to F), with the exception of PSR M3C, from FAST archival data. In these timing solutions, those of PSRs M3E, and F are obtained for the first time. We find that PSRs M3E and F have low mass companions, and are in circular orbits with periods of 7.1 and 3.0 days, respectively. For PSR M3C, we have not detected it in all the 41 observations. We found no X-ray counterparts for these pulsars in archival Chandra images in the band of 0.2-20 keV. We noticed that the pulsars in M3 seem to be native. From the Auto-Correlation Function (ACF) analysis of the M3A's and M3B's dynamic spectra, the scintillation timescale ranges from $7.0\pm0.3$ min to $60.0\pm0.6$ min, and the scintillation bandwidth ranges from $4.6\pm0.2$ MHz to $57.1\pm1.1$ MHz. The measured scintillation bandwidths from the dynamic spectra indicate strong scintillation, and the scattering medium is anisotropic. From the secondary spectra, we captured a scintillation arc only for PSR M3B with a curvature of $649\pm23 {\rm m}^{-1} {\rm mHz}^{-2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18169v1-abstract-full').style.display = 'none'; document.getElementById('2406.18169v1-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">14 pages, 4 figures, accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.00476">arXiv:2406.00476</a> <span> [<a href="https://arxiv.org/pdf/2406.00476">pdf</a>, <a href="https://arxiv.org/format/2406.00476">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Revisiting Energy Distribution and Formation Rate of CHIME Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+K+J">K. J. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+X+F">X. F. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Rodin%2C+A+E">A. E. Rodin</a>, <a href="/search/astro-ph?searchtype=author&query=Fedorova%2C+V+A">V. A. Fedorova</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Y+F">Y. F. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">D. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+P">P. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q+M">Q. M. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+C">C. Du</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+F">F. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+B">Z. B. 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="2406.00476v1-abstract-short" style="display: inline;"> Using a large sample of fast radio bursts (FRBs) from the first CHIME/FRB catalog, we apply the Lynden-Bell's c$^-$ method to study their energy function and formation rate evolutions with redshift. It is found with the non-parametric Kendell's $蟿$ statistics that the FRB energy strongly evolves with the cosmological redshift as $E(z)\propto(1 + z)^{5.23}$. After removing the redshift dependence,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00476v1-abstract-full').style.display = 'inline'; document.getElementById('2406.00476v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.00476v1-abstract-full" style="display: none;"> Using a large sample of fast radio bursts (FRBs) from the first CHIME/FRB catalog, we apply the Lynden-Bell's c$^-$ method to study their energy function and formation rate evolutions with redshift. It is found with the non-parametric Kendell's $蟿$ statistics that the FRB energy strongly evolves with the cosmological redshift as $E(z)\propto(1 + z)^{5.23}$. After removing the redshift dependence, the local energy distribution can be described by a broken power-law form of $唯(E_{0})\propto E_{0}^{-0.38}$ for the low-energy segment and $唯(E_{0})\propto E_{0}^{-2.01}$ for the high-energy segment with a dividing line of $\sim2.1\times10^{40} \rm erg$. Interestingly, we find that the formation rate of CHIME FRBs also evolves with redshift as $蟻(z)\propto(1+z)^{-4.73\pm0.08}$. The local formation rate $蟻(0)$ of the CHIME FRBs is constrained to be about $ 1.25\times 10^4\rm{\,Gpc^{-3}yr^{-1}}$ that is comparable with some previous estimations. In addition, we notice the formation rate not only exceeds the star formation rate at the lower redshifts but also always declines with the increase of redshift, which does not match the star formation history at all. Consequently, we suggest that most FRBs could originate from the older stellar populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00476v1-abstract-full').style.display = 'none'; document.getElementById('2406.00476v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.18228">arXiv:2405.18228</a> <span> [<a href="https://arxiv.org/pdf/2405.18228">pdf</a>, <a href="https://arxiv.org/format/2405.18228">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad534e">10.3847/2041-8213/ad534e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FAST Discovery of Eight Isolated Millisecond Pulsars in NGC 6517 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yin%2C+D">Dejiang Yin</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+L">Li-yun Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+L">Lei Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Eatough%2C+R+P">Ralph P. Eatough</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+B">Baoda Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lorimer%2C+D+R">Duncan R. Lorimer</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+Y">Yinfeng Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yaowei Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">Xingnan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Minghui Li</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+T">Tianhao Su</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Yuxiao Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y">Yu Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Lian%2C+Y">Yujie Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+Z">Zhen Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Zhichen Pan</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="2405.18228v1-abstract-short" style="display: inline;"> We present the discovery of 8 isolated millisecond pulsars in Globular Cluster (GC) NGC 6517 using the Five-Hundred-meter Aperture Spherical radio Telescope (FAST). The spin periods of those pulsars (namely PSR J1801-0857K to R, or, NGC 6517K to R) are all shorter than 10 ms. With these discoveries, NGC 6517 is currently the GC with the most known pulsars in the FAST sky. The largest difference in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18228v1-abstract-full').style.display = 'inline'; document.getElementById('2405.18228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18228v1-abstract-full" style="display: none;"> We present the discovery of 8 isolated millisecond pulsars in Globular Cluster (GC) NGC 6517 using the Five-Hundred-meter Aperture Spherical radio Telescope (FAST). The spin periods of those pulsars (namely PSR J1801-0857K to R, or, NGC 6517K to R) are all shorter than 10 ms. With these discoveries, NGC 6517 is currently the GC with the most known pulsars in the FAST sky. The largest difference in dispersion measure of the pulsars in NGC 6517 is 11.2 cm$^{-3}$ pc, the second among all GCs. The fraction of isolated pulsars in this GC (16 of 17, 94$\%$) is consistent with previous studies indicating an overabundance of isolated pulsars in the densest GCs, especially in those undergoing cluster core collapse. Considering the FAST GC pulsar discoveries, we modeled the GC pulsar population using the empirical Bayesian method described by Turk and Lorimer with the recent counts. Using this approach, we find that the expected number of potential pulsars in GCs seems to be correlated with the central escape velocity, hence, the GCs Liller 1, NGC 6441, M54 (NGC 6715), and $蠅$-Cen (NGC 5139) are expected to host the largest numbers of pulsars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18228v1-abstract-full').style.display = 'none'; document.getElementById('2405.18228v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 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">21 pages, 2 figures, accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.16484">arXiv:2405.16484</a> <span> [<a href="https://arxiv.org/pdf/2405.16484">pdf</a>, <a href="https://arxiv.org/format/2405.16484">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div 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/ad6156">10.3847/1538-4357/ad6156 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Accurate Measurement of the Lensing Magnification by BOSS CMASS Galaxies and Its Implications for Cosmology and Dark Matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xu%2C+K">Kun Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y+P">Y. P. Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">Hongyu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+X">Xiaolin Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Ming Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.16484v3-abstract-short" style="display: inline;"> Magnification serves as an independent and complementary gravitational lensing measurement to shear. We develop a novel method to achieve an accurate and robust magnification measurement around BOSS CMASS galaxies across physical scales of $0.016h^{-1}{\rm Mpc} < r_{\rm p} < 10h^{-1}{\rm Mpc}$. We first measure the excess total flux density $未M$ of the source galaxies in deep DECaLS photometric ca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16484v3-abstract-full').style.display = 'inline'; document.getElementById('2405.16484v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.16484v3-abstract-full" style="display: none;"> Magnification serves as an independent and complementary gravitational lensing measurement to shear. We develop a novel method to achieve an accurate and robust magnification measurement around BOSS CMASS galaxies across physical scales of $0.016h^{-1}{\rm Mpc} < r_{\rm p} < 10h^{-1}{\rm Mpc}$. We first measure the excess total flux density $未M$ of the source galaxies in deep DECaLS photometric catalog that are lensed by CMASS galaxies. We convert $未M$ to magnification $渭$ by establishing the $未渭-未M$ relation using a deeper photometric sample. By comparing magnification measurements in three optical bands ($grz$), we constrain the dust attenuation curve and its radial distribution, discovering a steep attenuation curve in the circumgalactic medium of CMASS galaxies. We further compare dust-corrected magnification measurements to model predictions from high-resolution dark matter-only (DMO) simulations in WMAP and Planck cosmologies, as well as the hydrodynamic simulation \texttt{TNG300-1}, using precise galaxy-halo connections from the Photometric objects Around Cosmic webs method and the accurate ray-tracing algorithm \texttt{P3MLens}. For $r_{\rm p} > 70h^{-1}$ kpc, our magnification measurements are in good agreement with both WMAP and Planck cosmologies, resulting in an estimation of the matter fluctuation amplitude of $S_8=0.816\pm0.024$. However, at $r_{\rm p} < 70h^{-1}$ kpc, we observe an excess magnification signal, which is higher than the DMO model in Planck cosmology at $2.8蟽$ and would be exacerbated if significant baryon feedback is included. Implications of the potential small scale discrepancy for the nature of dark matter and for the processes governing galaxy formation are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16484v3-abstract-full').style.display = 'none'; document.getElementById('2405.16484v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 19 figures. Main results in Figure 9 (dust) and Figure 18 (matter). Published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 973, 2024, Number 2 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13113">arXiv:2405.13113</a> <span> [<a href="https://arxiv.org/pdf/2405.13113">pdf</a>, <a href="https://arxiv.org/format/2405.13113">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <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"> MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Ly$伪$ Nebulae at Cosmic Noon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haibin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+Y">Yongming Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Kashikawa%2C+N">Nobunari Kashikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+K">Ke Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">J. Xavier Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Emonts%2C+B+H+C">Bjorn H. C. Emonts</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Yunjing Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shiwu Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+S+D">Sean D. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Yue%2C+M">Minghao Yue</a>, <a href="/search/astro-ph?searchtype=author&query=Battaia%2C+F+A">Fabrizio Arrigoni Battaia</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalupo%2C+S">Sebastiano Cantalupo</a>, <a href="/search/astro-ph?searchtype=author&query=Hennawi%2C+J+F">Joseph F. Hennawi</a>, <a href="/search/astro-ph?searchtype=author&query=Kikuta%2C+S">Satoshi Kikuta</a>, <a href="/search/astro-ph?searchtype=author&query=Ning%2C+Y">Yuanhang Ning</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">Masami Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Shimakawa%2C+R">Rhythm Shimakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Ben Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Weichen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Z">Zheng Zheng</a> , et al. (1 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="2405.13113v2-abstract-short" style="display: inline;"> Circumgalactic Lyman-alpha (Ly$伪$) nebulae are gaseous halos around galaxies exhibiting luminous extended Ly$伪$ emission. This work investigates Ly$伪$ nebulae from deep imaging of $\sim12~\mathrm{deg}^2$ sky, targeted by the MAMMOTH-Subaru survey. Utilizing the wide-field capability of Hyper Suprime-Cam (HSC), we present one of the largest blind Ly$伪$ nebula selections, including QSO nebulae, Ly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13113v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13113v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13113v2-abstract-full" style="display: none;"> Circumgalactic Lyman-alpha (Ly$伪$) nebulae are gaseous halos around galaxies exhibiting luminous extended Ly$伪$ emission. This work investigates Ly$伪$ nebulae from deep imaging of $\sim12~\mathrm{deg}^2$ sky, targeted by the MAMMOTH-Subaru survey. Utilizing the wide-field capability of Hyper Suprime-Cam (HSC), we present one of the largest blind Ly$伪$ nebula selections, including QSO nebulae, Ly$伪$ blobs, and radio galaxy nebulae down to typical $2蟽$ Ly$伪$ surface brightness of $(5-10)\times10^{-18}\mathrm{~erg~s^{-1}~cm^{-2}~arcsec^{-2}}$. The sample contains 117 nebulae with Ly$伪$ sizes of 40 - 400 kpc, and the most gigantic one spans about 365 kpc, referred to as the Ivory Nebula. Combining multiwavelength data, we investigate diverse nebula populations and associated galaxies. We find a small fraction of Ly$伪$ nebulae have QSOs ($\sim7\%$), luminous infrared galaxies ($\sim1\%$), and radio galaxies ($\sim 2\%$). Remarkably, among the 28 enormous Ly$伪$ nebulae (ELANe) exceeding 100 kpc, about 80\% are associated with UV-faint galaxies ($M_\mathrm{UV} > -22$), categorized as Type II ELANe. We underscore that Type II ELANe constitute the majority but remain largely hidden in current galaxy and QSO surveys. Dusty starburst and obscured AGN activity are proposed to explain the nature of Type II ELANe. The SED of stacking all Ly$伪$ nebulae also reveals signs of massive dusty star-forming galaxies with obscured AGNs. We propose a model to explain the dusty nature where the diverse populations of Ly$伪$ nebulae capture massive galaxies at different evolutionary stages undergoing violent assembling. Ly$伪$ nebulae provide critical insights into the formation and evolution of today's massive cluster galaxies at cosmic noon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13113v2-abstract-full').style.display = 'none'; document.getElementById('2405.13113v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJS after minor revision; 26 pages, 10 figures, 3 tables,</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.11826">arXiv:2405.11826</a> <span> [<a href="https://arxiv.org/pdf/2405.11826">pdf</a>, <a href="https://arxiv.org/format/2405.11826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Data quality control system and long-term performance monitor of the LHAASO-KM2A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bian%2C+W">W. Bian</a>, <a href="/search/astro-ph?searchtype=author&query=Bukevich%2C+A+V">A. V. Bukevich</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H+X">H. X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a> , et al. (263 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.11826v3-abstract-short" style="display: inline;"> The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic ray and gamma-ray showers. This information is used for physical analysis in gamma-ray astronomy and cosmic ray physics. To… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11826v3-abstract-full').style.display = 'inline'; document.getElementById('2405.11826v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.11826v3-abstract-full" style="display: none;"> The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic ray and gamma-ray showers. This information is used for physical analysis in gamma-ray astronomy and cosmic ray physics. To ensure the reliability of the LHAASO-KM2A data, a three-level quality control system has been established. It is used to monitor the status of detector units, stability of reconstructed parameters and the performance of the array based on observations of the Crab Nebula and Moon shadow. This paper will introduce the control system and its application on the LHAASO-KM2A data collected from August 2021 to July 2023. During this period, the pointing and angular resolution of the array were stable. From the observations of the Moon shadow and Crab Nebula, the results achieved using the two methods are consistent with each other. According to the observation of the Crab Nebula at energies from 25 TeV to 100 TeV, the time averaged pointing errors are estimated to be $-0.003^{\circ} \pm 0.005^{\circ}$ and $0.001^{\circ} \pm 0.006^{\circ}$ in the R.A. and Dec directions, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11826v3-abstract-full').style.display = 'none'; document.getElementById('2405.11826v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.01801">arXiv:2405.01801</a> <span> [<a href="https://arxiv.org/pdf/2405.01801">pdf</a>, <a href="https://arxiv.org/format/2405.01801">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div 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/pasj/psae103">10.1093/pasj/psae103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KIC 7914906: An Eclipsing Heartbeat Star with Tidally Excited Oscillations and Gamma Doradus/Delta Scuti Hybrid Pulsations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Min-Yu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+S">Sheng-Bang Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Ying Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+L">Liang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liao%2C+W">Wen-Ping Liao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+E">Er-Gang Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+X">Xiang-Dong Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Fu-Xing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Q">Qi-Bin Sun</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="2405.01801v3-abstract-short" style="display: inline;"> We present the eclipsing Heartbeat Star KIC 9704906 with tidally excited oscillations (TEOs) and gamma Doradus/delta Scuti hybrid pulsations. The derived parameters show that it has an orbital period of $P$=8.7529108(1) days, a high eccentricity of $e$=0.467(3), and a high inclination of $i$=78$^{\circ}$.81(6). The mass ratio $q$=0.981(5), the relative radii (radius divided by semi-major axis)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01801v3-abstract-full').style.display = 'inline'; document.getElementById('2405.01801v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.01801v3-abstract-full" style="display: none;"> We present the eclipsing Heartbeat Star KIC 9704906 with tidally excited oscillations (TEOs) and gamma Doradus/delta Scuti hybrid pulsations. The derived parameters show that it has an orbital period of $P$=8.7529108(1) days, a high eccentricity of $e$=0.467(3), and a high inclination of $i$=78$^{\circ}$.81(6). The mass ratio $q$=0.981(5), the relative radii (radius divided by semi-major axis) $r_1$=0.0639(2), and $r_2$=0.0715(4) indicate that the secondary component has a less mass and a larger radius, and may have evolved off the main sequence. The eight derived TEO candidates, $n$ = 3, 4, 5, 6, 7, 12, 40, and 44 harmonics, are consistent with or close to the dominant spherical harmonic $l=2$, $m=0$, or $\pm2$, assuming that the spin and orbital axes are aligned, and the pulsations are adiabatic and standing waves. We also identify ten independent frequency candidates, but one of them, $\mathit{f_{7}}$, is more like a modulation of a quasi-periodic signal and the orbits. According to the g-mode frequencies, we find that the rotation period of one component is 11.52(29) days. Although the masses and radii cannot be further constrained due to the lack of sufficient high-precision spectra, the fascinating phenomena in the Fourier spectra are evident and valuable in this system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01801v3-abstract-full').style.display = 'none'; document.getElementById('2405.01801v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.00920">arXiv:2405.00920</a> <span> [<a href="https://arxiv.org/pdf/2405.00920">pdf</a>, <a href="https://arxiv.org/format/2405.00920">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad65d1">10.3847/1538-4357/ad65d1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identifying Halos in Cosmological Simulations with Continuous Wavelet Analysis: The 2D Case </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Minxing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+P">Ping He</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="2405.00920v3-abstract-short" style="display: inline;"> Continuous wavelet analysis is gaining popularity in science and engineering for its ability to analyze data across spatial and scale domains simultaneously. In this study, we introduce a wavelet-based method to identify halos and assess its feasibility in two-dimensional (2D) scenarios. We begin with the generation of four pseudo-2D datasets from the SIMBA dark matter simulation by compressing th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00920v3-abstract-full').style.display = 'inline'; document.getElementById('2405.00920v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.00920v3-abstract-full" style="display: none;"> Continuous wavelet analysis is gaining popularity in science and engineering for its ability to analyze data across spatial and scale domains simultaneously. In this study, we introduce a wavelet-based method to identify halos and assess its feasibility in two-dimensional (2D) scenarios. We begin with the generation of four pseudo-2D datasets from the SIMBA dark matter simulation by compressing thin slices of three-dimensional (3D) data into 2D. We then calculate the continuous wavelet transform (CWT) directly from the particle distributions, identify local maxima that represent actual halos, and segment the CWT to delineate halo boundaries. A comparison with the traditional friends-of-friends (FOF) method shows that our CWT-identified halos, while contain slightly fewer particles, have smoother boundaries and are more compact in dense regions. In contrast, the CWT method can link particles over greater distances to form halos in sparse regions due to its spatial segmentation scheme. The spatial distribution and halo power spectrum of both CWT and FOF halos demonstrate substantial consistency, validating the 2D applicability of CWT for halo detection. Our identification scheme operates with a linear time complexity of $\mathcal{O}(N)$, suggesting its suitability for analyzing significantly larger datasets in the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00920v3-abstract-full').style.display = 'none'; document.getElementById('2405.00920v3-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> 19 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">19 pages, 13 figures, 2 table, comments welcome, accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ (2024), 973, 39 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16425">arXiv:2404.16425</a> <span> [<a href="https://arxiv.org/pdf/2404.16425">pdf</a>, <a href="https://arxiv.org/format/2404.16425">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Soft X-ray prompt emission from a high-redshift gamma-ray burst EP240315a </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">H. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+D">D. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Svinkin%2C+D+S">D. S. Svinkin</a>, <a href="/search/astro-ph?searchtype=author&query=Delaunay%2C+J">J. Delaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Tanvir%2C+N+R">N. R. Tanvir</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">H. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+C">C. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Y. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X+-">X. -F. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">W. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+J">J. An</a>, <a href="/search/astro-ph?searchtype=author&query=Bruni%2C+G">G. Bruni</a>, <a href="/search/astro-ph?searchtype=author&query=Frederiks%2C+D+D">D. D. Frederiks</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirlanda%2C+G">G. Ghirlanda</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+J+-">J. -W. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+A">A. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C+-">C. -K. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J+-">J. -D. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Malesani%2C+D+B">D. B. Malesani</a>, <a href="/search/astro-ph?searchtype=author&query=Piro%2C+L">L. Piro</a>, <a href="/search/astro-ph?searchtype=author&query=Raman%2C+G">G. Raman</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+R">R. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Troja%2C+E">E. Troja</a> , et al. (170 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="2404.16425v1-abstract-short" style="display: inline;"> Long gamma-ray bursts (GRBs) are believed to originate from core collapse of massive stars. High-redshift GRBs can probe the star formation and reionization history of the early universe, but their detection remains rare. Here we report the detection of a GRB triggered in the 0.5--4 keV band by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated as EP240315a,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16425v1-abstract-full').style.display = 'inline'; document.getElementById('2404.16425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16425v1-abstract-full" style="display: none;"> Long gamma-ray bursts (GRBs) are believed to originate from core collapse of massive stars. High-redshift GRBs can probe the star formation and reionization history of the early universe, but their detection remains rare. Here we report the detection of a GRB triggered in the 0.5--4 keV band by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated as EP240315a, whose bright peak was also detected by the Swift Burst Alert Telescope and Konus-Wind through off-line analyses. At a redshift of $z=4.859$, EP240315a showed a much longer and more complicated light curve in the soft X-ray band than in gamma-rays. Benefiting from a large field-of-view ($\sim$3600 deg$^2$) and a high sensitivity, EP-WXT captured the earlier engine activation and extended late engine activity through a continuous detection. With a peak X-ray flux at the faint end of previously known high-$z$ GRBs, the detection of EP240315a demonstrates the great potential for EP to study the early universe via GRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16425v1-abstract-full').style.display = 'none'; document.getElementById('2404.16425v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 8 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/2404.15963">arXiv:2404.15963</a> <span> [<a href="https://arxiv.org/pdf/2404.15963">pdf</a>, <a href="https://arxiv.org/format/2404.15963">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmic Himalayas: The Highest Quasar Density Peak Identified in a 10,000 deg$^2$ Sky with Spatial Discrepancies between Galaxies, Quasars, and IGM HI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liang%2C+Y">Yongming Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">Masami Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+D">Dongsheng Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Kashikawa%2C+N">Nobunari Kashikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalupo%2C+S">Sebastiano Cantalupo</a>, <a href="/search/astro-ph?searchtype=author&query=Nagamine%2C+K">Kentaro Nagamine</a>, <a href="/search/astro-ph?searchtype=author&query=Yajima%2C+H">Hidenobu Yajima</a>, <a href="/search/astro-ph?searchtype=author&query=Kirihara%2C+T">Takanobu Kirihara</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haibin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+M">Mingyu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Shimakawa%2C+R">Rhythm Shimakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+K">Kei Ito</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+M">Masayuki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Harikane%2C+Y">Yuichi Harikane</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">J. Xavier Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Travascio%2C+A">Andrea Travascio</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Weichen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">Martin Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Fabbiano%2C+G">Giuseppina Fabbiano</a>, <a href="/search/astro-ph?searchtype=author&query=Arita%2C+J">Junya Arita</a>, <a href="/search/astro-ph?searchtype=author&query=Onoue%2C+M">Masafusa Onoue</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">John D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+D">Dongdong Shi</a> , et al. (5 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="2404.15963v1-abstract-short" style="display: inline;"> We report the identification of a quasar overdensity in the BOSSJ0210 field, dubbed Cosmic Himalayas, consisting of 11 quasars at $z=2.16-2.20$, the densest overdensity of quasars ($17蟽$) in the $\sim$10,000 deg$^2$ of the Sloan Digital Sky Survey. We present the spatial distributions of galaxies and quasars and an HI absorption map of the intergalactic medium (IGM). On the map of 465 galaxies sel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.15963v1-abstract-full').style.display = 'inline'; document.getElementById('2404.15963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.15963v1-abstract-full" style="display: none;"> We report the identification of a quasar overdensity in the BOSSJ0210 field, dubbed Cosmic Himalayas, consisting of 11 quasars at $z=2.16-2.20$, the densest overdensity of quasars ($17蟽$) in the $\sim$10,000 deg$^2$ of the Sloan Digital Sky Survey. We present the spatial distributions of galaxies and quasars and an HI absorption map of the intergalactic medium (IGM). On the map of 465 galaxies selected from the MAMMOTH-Subaru survey, we find two galaxy density peaks that do not fall on the quasar overdensity but instead exist at the northwest and southeast sides, approximately 25 $h^{-1}$ comoving-Mpc apart from the quasar overdensity. With a spatial resolution of 15 $h^{-1}$ comoving Mpc in projection, we produce a three-dimensional HI tomography map by the IGM Ly$伪$ forest in the spectra of 23 SDSS/eBOSS quasars behind the quasar overdensity. Surprisingly, the quasar overdensity coincides with neither an absorption peak nor a transmission peak of IGM HI but lies near the border separating opaque and transparent volumes, with the more luminous quasars located in an environment with lesser IGM HI. Hence remarkably, the overdensity region traced by the 11 quasars, albeit all in coherently active states, has no clear coincidence with peaks of galaxies or HI absorption densities. Current physical scenarios with mixtures of HI overdensities and quasar photoionization cannot fully interpret the emergence of Cosmic Himalayas, suggesting this peculiar structure is an excellent laboratory to unveil the interplay between galaxies, quasars, and the IGM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.15963v1-abstract-full').style.display = 'none'; document.getElementById('2404.15963v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures, submitted to ApJ, comments are welcome</span> </p> </li> </ol> <nav class="pagination is-small 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