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is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=200" 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/2502.20138">arXiv:2502.20138</a> <span> [<a href="https://arxiv.org/pdf/2502.20138">pdf</a>, <a href="https://arxiv.org/format/2502.20138">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Fundamental Physics and Cosmology with TianQin </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=An%2C+H">Haipeng An</a>, <a href="/search/astro-ph?searchtype=author&query=Bian%2C+L">Ligong Bian</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+R">Rong-Gen Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhoujian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+W">Wenbiao Han</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+J">Jianhua He</a>, <a href="/search/astro-ph?searchtype=author&query=Hendry%2C+M+A">Martin A. Hendry</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+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=Huang%2C+S">Shun-Jia Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S+P">Sang Pyo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+E">En-Kun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yu-Xiao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Milyukov%2C+V">Vadim Milyukov</a>, <a href="/search/astro-ph?searchtype=author&query=Pi%2C+S">Shi Pi</a>, <a href="/search/astro-ph?searchtype=author&query=Postnov%2C+K">Konstantin Postnov</a>, <a href="/search/astro-ph?searchtype=author&query=Sasaki%2C+M">Misao Sasaki</a>, <a href="/search/astro-ph?searchtype=author&query=Shao%2C+C">Cheng-Gang Shao</a>, <a href="/search/astro-ph?searchtype=author&query=Shao%2C+L">Lijing Shao</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+C">Changfu Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+S">Shuo Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+A">Anzhong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+P">Pan-Pan Wang</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="2502.20138v1-abstract-short" style="display: inline;"> The exploration of the surrounding world and the universe is an important theme in the legacy of humankind. The detection of gravitational waves is adding a new dimension to this grand effort. What are the fundamental physical laws governing the dynamics of the universe? What is the fundamental composition of the universe? How has the universe evolved in the past and how will it evolve in the futu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.20138v1-abstract-full').style.display = 'inline'; document.getElementById('2502.20138v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.20138v1-abstract-full" style="display: none;"> The exploration of the surrounding world and the universe is an important theme in the legacy of humankind. The detection of gravitational waves is adding a new dimension to this grand effort. What are the fundamental physical laws governing the dynamics of the universe? What is the fundamental composition of the universe? How has the universe evolved in the past and how will it evolve in the future? These are the basic questions that press for answers. The space-based gravitational wave detector TianQin will tune in to gravitational waves in the millihertz frequency range ($10^{-4} \sim 1$ Hz, to be specific), opening a new gravitational wave spectrum window to explore many of the previously hidden sectors of the universe. TianQin will discover many astrophysical systems, populating the universe at different redshifts: some will be of new types that have never been detected before, some will have very high signal-to-noise ratios, and some will have very high parameter estimation precision. The plethora of information collected will bring us to new fronts on which to search for the breaking points of general relativity, the possible violation of established physical laws, the signature of possible new gravitational physics and new fundamental fields, and to improve our knowledge on the expansion history of the universe. In this white paper, we highlight the advances that TianQin can bring to fundamental physics and cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.20138v1-abstract-full').style.display = 'none'; document.getElementById('2502.20138v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">113 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.19776">arXiv:2502.19776</a> <span> [<a href="https://arxiv.org/pdf/2502.19776">pdf</a>, <a href="https://arxiv.org/format/2502.19776">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"> Probing the PeV Region in the Astrophysical Neutrino Spectrum using $谓_渭$ from the Southern Sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (404 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="2502.19776v1-abstract-short" style="display: inline;"> IceCube has observed a diffuse astrophysical neutrino flux over the energy region from a few TeV to a few PeV. At PeV energies, the spectral shape is not yet well measured due to the low statistics of the data. This analysis probes the gap between 1 PeV and 10 PeV by using high-energy downgoing muon neutrinos. To reject the large atmospheric muon background, two complementary techniques are combin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19776v1-abstract-full').style.display = 'inline'; document.getElementById('2502.19776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.19776v1-abstract-full" style="display: none;"> IceCube has observed a diffuse astrophysical neutrino flux over the energy region from a few TeV to a few PeV. At PeV energies, the spectral shape is not yet well measured due to the low statistics of the data. This analysis probes the gap between 1 PeV and 10 PeV by using high-energy downgoing muon neutrinos. To reject the large atmospheric muon background, two complementary techniques are combined. The first technique selects events with high stochasticity to reject atmospheric muon bundles whose stochastic energy losses are smoothed due to high muon multiplicity. The second technique vetoes atmospheric muons with the IceTop surface array. Using 9 years of data, we found two neutrino candidate events in the signal region, consistent with expectation from background, each with relatively high signal probabilities. A joint maximum likelihood estimation is performed using this sample and an independent 9.5-year sample of tracks to measure the neutrino spectrum. A likelihood ratio test is done to compare the single power-law (SPL) vs. SPL+cutoff hypothesis; the SPL+cutoff model is not significantly better than the SPL. High-energy astrophysical objects from four source catalogs are also checked around the direction of the two events. No significant coincidence was found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19776v1-abstract-full').style.display = 'none'; document.getElementById('2502.19776v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.18790">arXiv:2502.18790</a> <span> [<a href="https://arxiv.org/pdf/2502.18790">pdf</a>, <a href="https://arxiv.org/format/2502.18790">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"> Delensing for Precision Cosmology: Optimizing Future CMB B-mode Surveys to Constrain r </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wen-Zheng Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yi-Ming Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Hong 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="2502.18790v1-abstract-short" style="display: inline;"> The detection of primordial B-modes, a key probe of cosmic inflation, is increasingly challenged by contamination from weak gravitational lensing B-modes induced by large-scale structure (LSS). We present a delensing pipeline designed to enhance the sensitivity to the inflationary parameter r, minimizing reliance on foreground mitigation during lensing reconstruction. Using simulations of Simons O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18790v1-abstract-full').style.display = 'inline'; document.getElementById('2502.18790v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.18790v1-abstract-full" style="display: none;"> The detection of primordial B-modes, a key probe of cosmic inflation, is increasingly challenged by contamination from weak gravitational lensing B-modes induced by large-scale structure (LSS). We present a delensing pipeline designed to enhance the sensitivity to the inflationary parameter r, minimizing reliance on foreground mitigation during lensing reconstruction. Using simulations of Simons Observatory-like CMB observations and Euclid-like LSS surveys in the Northern hemisphere, we demonstrate that excluding low-l modes (l<200) effectively mitigates foreground biases, enabling robust lensing potential reconstruction using observed CMB polarization maps. We reconstruct the lensing potential with a minimum-variance (MV) quadratic estimator (QE) applied to CMB polarization data and combine this with external LSS tracers to improve delensing efficiency. Two complementary methods, the Gradient-order template and the Inverse-lensing approach, are used to generate lensing B-mode templates, which are cross-correlated with observed B-modes. This achieves a 40 percent reduction in the uncertainty of r with CMB-only reconstruction, improving to 60 percent when incorporating external LSS tracers. We validate our results using both the Hamimeche and Lewis likelihood and a Gaussian approximation, finding consistent constraints on r. Our work establishes a streamlined framework for ground-based CMB experiments, demonstrating that synergies with LSS surveys significantly enhance sensitivity to primordial gravitational waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18790v1-abstract-full').style.display = 'none'; document.getElementById('2502.18790v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.17890">arXiv:2502.17890</a> <span> [<a href="https://arxiv.org/pdf/2502.17890">pdf</a>, <a href="https://arxiv.org/format/2502.17890">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 - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Seasonal Variations of the Atmospheric Muon Neutrino Spectrum measured with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (404 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="2502.17890v1-abstract-short" style="display: inline;"> This study presents an energy-dependent analysis of seasonal variations in the atmospheric muon neutrino spectrum, using 11.3 years of data from the IceCube Neutrino Observatory. By leveraging a novel spectral unfolding method, we explore the energy range from 125 GeV to 10 TeV for zenith angles between 90掳 to 110掳, corresponding to the Antarctic atmosphere. Our findings reveal that the seasonal v… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17890v1-abstract-full').style.display = 'inline'; document.getElementById('2502.17890v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.17890v1-abstract-full" style="display: none;"> This study presents an energy-dependent analysis of seasonal variations in the atmospheric muon neutrino spectrum, using 11.3 years of data from the IceCube Neutrino Observatory. By leveraging a novel spectral unfolding method, we explore the energy range from 125 GeV to 10 TeV for zenith angles between 90掳 to 110掳, corresponding to the Antarctic atmosphere. Our findings reveal that the seasonal variation amplitude decreases with energy reaching ($-4.6 \pm 1.1$)\% during Austral winter and increases ($+3.9 \pm 1.2$)\% during Austral summer relative to the annual average at 10TeV. While the unfolded flux exceeds the model predictions by up to 30\%, the differential measurement of seasonal variations remains unaffected. The measured seasonal variations of the muon neutrino spectrum are consistent with theoretical predictions using the MCEq code and the NRLMSISE-00 atmospheric model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17890v1-abstract-full').style.display = 'none'; document.getElementById('2502.17890v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.16807">arXiv:2502.16807</a> <span> [<a href="https://arxiv.org/pdf/2502.16807">pdf</a>, <a href="https://arxiv.org/ps/2502.16807">ps</a>, <a href="https://arxiv.org/format/2502.16807">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-025-02484-z">10.1038/s41550-025-02484-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astronomical image denoising by self-supervised deep learning and restoration processes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tie Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Quan%2C+Y">Yuhui Quan</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+Y">Yingna Su</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Y">Yang Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+S">Shu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+H">Haisheng Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Hao%2C+Q">Qi Hao</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Yulong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuxia Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yikang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+W">Wenqing Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+M">Mingde Ding</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="2502.16807v1-abstract-short" style="display: inline;"> Image denoising based on deep learning has witnessed significant advancements in recent years. However, existing deep learning methods lack quantitative control of the deviation or error on denoised images. The neural networks Self2Self is designed for denoising single-image, training on it and denoising itself, during which training is costly. In this work we explore training Self2Self on an astr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.16807v1-abstract-full').style.display = 'inline'; document.getElementById('2502.16807v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.16807v1-abstract-full" style="display: none;"> Image denoising based on deep learning has witnessed significant advancements in recent years. However, existing deep learning methods lack quantitative control of the deviation or error on denoised images. The neural networks Self2Self is designed for denoising single-image, training on it and denoising itself, during which training is costly. In this work we explore training Self2Self on an astronomical image and denoising other images of the same kind, which is suitable for quickly denoising massive images in astronomy. To address the deviation issue, the abnormal pixels whose deviation exceeds a predefined threshold are restored to their initial values. The noise reduction includes training, denoising, restoring and named TDR-method, by which the noise level of the solar magnetograms is improved from about 8 G to 2 G. Furthermore, the TDR-method is applied to galaxy images from the Hubble Space Telescope and makes weak galaxy structures become much clearer. This capability of enhancing weak signals makes the TDR-method applicable in various disciplines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.16807v1-abstract-full').style.display = 'none'; document.getElementById('2502.16807v1-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 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">Nature Astronomy online publication https://www.nature.com/articles/s41550-025-02484-z</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.15527">arXiv:2502.15527</a> <span> [<a href="https://arxiv.org/pdf/2502.15527">pdf</a>, <a href="https://arxiv.org/format/2502.15527">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"> High-redshift quasars at $z \geq 3$ -- III. Parsec-scale jet properties from VLBI observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guo%2C+S">Shaoguang Guo</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">Tao An</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuanqi Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chuanzeng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Zhijun Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Sotnikova%2C+Y">Yulia Sotnikova</a>, <a href="/search/astro-ph?searchtype=author&query=Mufakharov%2C+T">Timur Mufakharov</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+A">Ailing Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.15527v1-abstract-short" style="display: inline;"> High redshift active galactic nuclei (AGN) provide key insights into early supermassive black hole growth and cosmic evolution. This study investigates the parsec-scale properties of 86 radio-loud quasars at z $\geq$ 3 using very long baseline interferometry (VLBI) observations. Our results show predominantly compact core and core-jet morphologies, with 35\% unresolved cores, 59\% core-jet structu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15527v1-abstract-full').style.display = 'inline'; document.getElementById('2502.15527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.15527v1-abstract-full" style="display: none;"> High redshift active galactic nuclei (AGN) provide key insights into early supermassive black hole growth and cosmic evolution. This study investigates the parsec-scale properties of 86 radio-loud quasars at z $\geq$ 3 using very long baseline interferometry (VLBI) observations. Our results show predominantly compact core and core-jet morphologies, with 35\% unresolved cores, 59\% core-jet structures, and only 6\% core-double jet morphology. Brightness temperatures are generally lower than expected for highly radiative sources. The jet proper motions are surprisingly slow compared to lower-redshift samples. We observe a high fraction of young and/or confined peak-spectrum sources, providing insights into early AGN evolution in dense environments during early cosmic epochs. The observed trends may reflect genuine evolutionary changes in AGN structure over cosmic time, or selection effects favoring more compact sources at higher redshifts. These results stress the complexity of high-redshift radio-loud AGN populations and emphasize the need for multi-wavelength, high-resolution observations to fully characterize their properties and evolution through cosmic history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15527v1-abstract-full').style.display = 'none'; document.getElementById('2502.15527v1-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 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">23 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/2502.15447">arXiv:2502.15447</a> <span> [<a href="https://arxiv.org/pdf/2502.15447">pdf</a>, <a href="https://arxiv.org/format/2502.15447">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 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/10.1016/j.xinn.2025.100802">10.1016/j.xinn.2025.100802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultra-high-energy $纬$-ray emission associated with the tail of a bow-shock pulsar wind nebula </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=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=Cai%2C+C+M">C. M. Cai</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">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>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (274 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="2502.15447v2-abstract-short" style="display: inline;"> In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) $纬$-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1$蟽$ (9.4$蟽$) above 25$\,$TeV (100$\,$TeV). The source energy spectrum extended up to 300$\,$TeV, which was well fitted by a log-parabola f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15447v2-abstract-full').style.display = 'inline'; document.getElementById('2502.15447v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.15447v2-abstract-full" style="display: none;"> In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) $纬$-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1$蟽$ (9.4$蟽$) above 25$\,$TeV (100$\,$TeV). The source energy spectrum extended up to 300$\,$TeV, which was well fitted by a log-parabola function with $N0 = (1.93\pm0.23) \times 10^{-16} \rm{TeV^{-1}\,cm^{-2}\,s^{-2}}$, $伪= 2.14\pm0.27$, and $尾= 1.20\pm0.41$ at E0 = 30$\,$TeV. The associated pulsar, PSR J1740+1000, resides at a high galactic latitude and powers a bow-shock pulsar wind nebula (BSPWN) with an extended X-ray tail. The best-fit position of the gamma-ray source appeared to be shifted by $0.2^{\circ}$ with respect to the pulsar position. As the (i) currently identified pulsar halos do not demonstrate such offsets, and (ii) centroid of the gamma-ray emission is approximately located at the extension of the X-ray tail, we speculate that the UHE $纬$-ray emission may originate from re-accelerated electron/positron pairs that are advected away in the bow-shock tail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15447v2-abstract-full').style.display = 'none'; document.getElementById('2502.15447v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">Corrected spelling errors in several author names</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Innovation (2025), 100802 </p> </li> <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/2502.10037">arXiv:2502.10037</a> <span> [<a href="https://arxiv.org/pdf/2502.10037">pdf</a>, <a href="https://arxiv.org/format/2502.10037">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"> Gamma-Ray Bursts Calibrated from the Observational $H(z)$ Data in Artificial Neural Network Framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Z">Zhen Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Xiong%2C+Z">Zhiguo Xiong</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+X">Xin Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+G">Guangzhen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+N">Nan Liang</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="2502.10037v1-abstract-short" style="display: inline;"> In this paper, we calibrate the luminosity relation of gamma-ray bursts (GRBs) from an Artificial Neural Network (ANN) framework for reconstructing the Hubble parameter \unboldmath{$H(z)$} from the latest observational Hubble data (OHD) obtained with the cosmic chronometers method in a cosmology-independent way. We consider the physical relationships between the data to introduce the covariance ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.10037v1-abstract-full').style.display = 'inline'; document.getElementById('2502.10037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.10037v1-abstract-full" style="display: none;"> In this paper, we calibrate the luminosity relation of gamma-ray bursts (GRBs) from an Artificial Neural Network (ANN) framework for reconstructing the Hubble parameter \unboldmath{$H(z)$} from the latest observational Hubble data (OHD) obtained with the cosmic chronometers method in a cosmology-independent way. We consider the physical relationships between the data to introduce the covariance matrix and KL divergence of the data to construct the loss function and calibrate the Amati relation ($E_{\rm p}$--$E_{\rm iso}$) by selecting the optimal ANN model with the A219 sample and the J220 sample at low redshift. Combining the Pantheon+ sample of type Ia supernovae (SNe Ia) and Baryon acoustic oscillations (BAOs) with GRBs at high redshift in the Hubble diagram with Markov Chain Monte Carlo numerical method, we find that the $螞$CDM model is preferred over the $w$CDM and CPL models with the joint constraints by the Akaike Information Criterion (AIC) and Bayesian Information Criterion (BIC). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.10037v1-abstract-full').style.display = 'none'; document.getElementById('2502.10037v1-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 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">16 pages, 6 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/2502.09071">arXiv:2502.09071</a> <span> [<a href="https://arxiv.org/pdf/2502.09071">pdf</a>, <a href="https://arxiv.org/format/2502.09071">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"> Foreground Removal in Ground-Based CMB Observations Using a Transformer Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yan%2C+Y">Ye-Peng Yan</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=Xia%2C+J">Jun-Qing Xia</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Hong 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="2502.09071v1-abstract-short" style="display: inline;"> We present a novel method for Cosmic Microwave Background (CMB) foreground removal based on deep learning techniques. This method employs a Transformer model, referred to as \texttt{TCMB}, which is specifically designed to effectively process HEALPix-format spherical sky maps. \texttt{TCMB} represents an innovative application in CMB data analysis, as it is an image-based technique that has rarely… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09071v1-abstract-full').style.display = 'inline'; document.getElementById('2502.09071v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.09071v1-abstract-full" style="display: none;"> We present a novel method for Cosmic Microwave Background (CMB) foreground removal based on deep learning techniques. This method employs a Transformer model, referred to as \texttt{TCMB}, which is specifically designed to effectively process HEALPix-format spherical sky maps. \texttt{TCMB} represents an innovative application in CMB data analysis, as it is an image-based technique that has rarely been utilized in this field. Using simulated data with noise levels representative of current ground-based CMB polarization observations, the \texttt{TCMB} method demonstrates robust performance in removing foreground contamination. The mean absolute variance for the reconstruction of the noisy CMB Q/U map is significantly less than the CMB polarization signal. To mitigate biases caused by instrumental noise, a cross-correlation approach using two half-mission maps was employed, successfully recovering CMB EE and BB power spectra that align closely with the true values, and these results validate the effectiveness of the \texttt{TCMB} method. Compared to the previously employed convolutional neural network (CNN)-based approach, the \texttt{TCMB} method offers two significant advantages: (1) It demonstrates superior effectiveness in reconstructing CMB polarization maps, outperforming CNN-based methods. (2) It can directly process HEALPix spherical sky maps without requiring rectangular region division, a step necessary for CNN-based approaches that often introduces uncertainties such as boundary effects. This study highlights the potential of Transformer-based models as a powerful tool for CMB data analysis, offering a substantial improvement over traditional CNN-based techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09071v1-abstract-full').style.display = 'none'; document.getElementById('2502.09071v1-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 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">17 pages, 13 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/2502.07831">arXiv:2502.07831</a> <span> [<a href="https://arxiv.org/pdf/2502.07831">pdf</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> </div> </div> <p class="title is-5 mathjax"> Endurance Science Workshop 2023 Final Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Keane%2C+J+T">James Tuttle Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+B">Barbara Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Crow%2C+C">Carolyn Crow</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhagen%2C+B">Benjamin Greenhagen</a>, <a href="/search/astro-ph?searchtype=author&query=Jolliff%2C+B">Bradley Jolliff</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Shearer%2C+C">Charles Shearer</a>, <a href="/search/astro-ph?searchtype=author&query=Tikoo%2C+S">Sonia Tikoo</a>, <a href="/search/astro-ph?searchtype=author&query=Valencia%2C+S">Sarah Valencia</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="2502.07831v1-abstract-short" style="display: inline;"> Endurance is a mission concept to explore and ultimately return samples from the Moon's largest and oldest impact basin, South Pole-Aitken (SPA). SPA holds the answers to many outstanding planetary science questions, including the earliest impact bombardment of the Solar System and the evolution of the Moon's interior. Endurance would address these questions by traversing 2,000 kilometers across t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07831v1-abstract-full').style.display = 'inline'; document.getElementById('2502.07831v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.07831v1-abstract-full" style="display: none;"> Endurance is a mission concept to explore and ultimately return samples from the Moon's largest and oldest impact basin, South Pole-Aitken (SPA). SPA holds the answers to many outstanding planetary science questions, including the earliest impact bombardment of the Solar System and the evolution of the Moon's interior. Endurance would address these questions by traversing 2,000 kilometers across the lunar farside, collecting samples, and delivering those samples to Artemis astronauts for return to Earth. Endurance was identified as the highest priority strategic mission for NASA's Lunar Discovery and Program in the recent Planetary Science and Astrobiology Decadal Survey. This report summarizes the results from the first public workshop about the concept. Major findings include: (1) Endurance is an exciting concept that would address long-standing, high-priority lunar and planetary science questions, and the community is ready for it. (2) Endurance's sample science objectives are achievable, although they would require coordinated analysis techniques and numerous diverse samples. (3) Geologic context is essential for addressing Endurance's science objectives. (4) While Endurance's objectives center on sample return, Endurance's long traverse would enable a variety of additional transformative science investigations. (5) Endurance is an ambitious mission that would be enabled and enhanced by investing in developing key technologies now. (6) Endurance should strive to include more diverse perspectives in its formulation, particularly from early-career scientists and engineers who will ultimately operate the rover and analyze the samples. Endurance is early in its formulation and the next major activity will be a Science Definition Team (SDT). It is expected that this report and the findings therein may be useful input to the Endurance SDT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07831v1-abstract-full').style.display = 'none'; document.getElementById('2502.07831v1-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">58 pages, 14 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/2502.04848">arXiv:2502.04848</a> <span> [<a href="https://arxiv.org/pdf/2502.04848">pdf</a>, <a href="https://arxiv.org/format/2502.04848">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"> Broadband $纬$-ray spectrum of supernova remnant Cassiopeia A </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=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=Cai%2C+C+M">C. M. Cai</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">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>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (293 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="2502.04848v1-abstract-short" style="display: inline;"> The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of $\sim$ 2.5 $\arcmin$. Although no extension of this source has been detected in the $纬$-ray band, using more than 1000 days of LHAASO data above $\sim 0.8$ TeV, we find that its spectrum is significantly softer than those obtained with Imaging Air Cherenkov Telesc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04848v1-abstract-full').style.display = 'inline'; document.getElementById('2502.04848v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.04848v1-abstract-full" style="display: none;"> The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of $\sim$ 2.5 $\arcmin$. Although no extension of this source has been detected in the $纬$-ray band, using more than 1000 days of LHAASO data above $\sim 0.8$ TeV, we find that its spectrum is significantly softer than those obtained with Imaging Air Cherenkov Telescopes (IACTs) and its flux near $\sim 1$ TeV is about two times higher. In combination with analyses of more than 16 years of \textit{Fermi}-LAT data covering $0.1 \, \mathrm{GeV} - 1 \, \mathrm{TeV}$, we find that the spectrum above 30 GeV deviates significantly from a single power-law, and is best described by a smoothly broken power-law with a spectral index of $1.90 \pm 0.15_\mathrm{stat}$ ($3.41 \pm 0.19_\mathrm{stat}$) below (above) a break energy of $0.63 \pm 0.21_\mathrm{stat} \, \mathrm{TeV}$. Given differences in the angular resolution of LHAASO-WCDA and IACTs, TeV $纬$-ray emission detected with LHAASO may have a significant contribution from regions surrounding the SNR illuminated by particles accelerated earlier, which, however, are treated as background by IACTs. Detailed modelling can be used to constrain acceleration processes of TeV particles in the early stage of SNR evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04848v1-abstract-full').style.display = 'none'; document.getElementById('2502.04848v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.03853">arXiv:2502.03853</a> <span> [<a href="https://arxiv.org/pdf/2502.03853">pdf</a>, <a href="https://arxiv.org/format/2502.03853">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"> VERITAS and multiwavelength observations of the Blazar B3 2247+381 in response to an IceCube neutrino alert </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">Atreya Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">Colin B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">Priyadarshini Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Bartkoske%2C+J+T">J. T. Bartkoske</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">Wystan Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">James H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yu Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J">Jodi Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A">Alisha Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Duerr%2C+A">Anne Duerr</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">Manel Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Godoy%2C+M+E">Miguel E. Godoy</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">Abe Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Qi Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+J">Juniper Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">Amy Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">William Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">David Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">Olivier Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">Claire E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">Jamie Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">Thomas B. Humensky</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+W">Weidong Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+M+N">Madalyn N. Johnson</a> , et al. (473 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="2502.03853v1-abstract-short" style="display: inline;"> While the sources of the diffuse astrophysical neutrino flux detected by the IceCube Neutrino Observatory are still largely unknown, one of the promising methods used towards understanding this is investigating the potential temporal and spatial correlations between neutrino alerts and the electromagnetic radiation from blazars. We report on the multiwavelength target-of-opportunity observations o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03853v1-abstract-full').style.display = 'inline'; document.getElementById('2502.03853v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.03853v1-abstract-full" style="display: none;"> While the sources of the diffuse astrophysical neutrino flux detected by the IceCube Neutrino Observatory are still largely unknown, one of the promising methods used towards understanding this is investigating the potential temporal and spatial correlations between neutrino alerts and the electromagnetic radiation from blazars. We report on the multiwavelength target-of-opportunity observations of the blazar B3 2247+381, taken in response to an IceCube multiplet alert for a cluster of muon neutrino events compatible with the source location between May 20, 2022 and November 10, 2022. B3 2247+381 was not detected with VERITAS during this time period. The source was found to be in a low-flux state in the optical, ultraviolet and gamma-ray bands for the time interval corresponding to the neutrino event, but was detected in the hard X-ray band with NuSTAR during this period. We find the multiwavelength spectral energy distribution is well described using a simple one-zone leptonic synchrotron self-Compton radiation model. Moreover, assuming the neutrinos originate from hadronic processes within the jet, the neutrino flux would be accompanied by a photon flux from the cascade emission, and the integrated photon flux required in such a case would significantly exceed the total multiwavelength fluxes and the VERITAS upper limits presented here. The lack of flaring activity observed with VERITAS, combined with the low multiwavelength flux levels, and given the significance of the neutrino excess is at 3$蟽$ level (uncorrected for trials), makes B3 2247+381 an unlikely source of the IceCube multiplet. We conclude that the neutrino excess is likely a background fluctuation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03853v1-abstract-full').style.display = 'none'; document.getElementById('2502.03853v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 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">26 pages, 5 figures. Accepted for publication in the Astrophysical Journal (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/2502.03548">arXiv:2502.03548</a> <span> [<a href="https://arxiv.org/pdf/2502.03548">pdf</a>, <a href="https://arxiv.org/format/2502.03548">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Stellar Abundances and Galactic Evolution Survey (SAGES). II. Machine Learning-Based Stellar parameters for 21 million stars from the First Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gu%2C+H">Hongrui Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+Z">Zhou Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+G">Gang Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Y">Yang Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Wei Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+J">Jie Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+J">Jingkun Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C">Chun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yuqin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+H">Haibo Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Haining Li</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+K">Kefeng Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yihan Song</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+A">Ali Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+N">Nan Song</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yujuan Liu</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="2502.03548v1-abstract-short" style="display: inline;"> Stellar parameters for large samples of stars play a crucial role in constraining the nature of stars and stellar populations in the Galaxy. An increasing number of medium-band photometric surveys are presently used in estimating stellar parameters. In this study, we present a machine-learning approach to derive estimates of stellar parameters, including [Fe/H], logg, and Teff, based on a combinat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03548v1-abstract-full').style.display = 'inline'; document.getElementById('2502.03548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.03548v1-abstract-full" style="display: none;"> Stellar parameters for large samples of stars play a crucial role in constraining the nature of stars and stellar populations in the Galaxy. An increasing number of medium-band photometric surveys are presently used in estimating stellar parameters. In this study, we present a machine-learning approach to derive estimates of stellar parameters, including [Fe/H], logg, and Teff, based on a combination of medium-band and broad-band photometric observations. Our analysis employs data primarily sourced from the SAGE Survey , which aims to observe much of the Northern Hemisphere. We combine the $uv$-band data from SAGES DR1 with photometric and astrometric data from Gaia EDR3, and apply the random forest method to estimate stellar parameters for approximately 21 million stars. We are able to obtain precisions of 0.09 dex for [Fe/H], 0.12 dex for logg, and 70 K for Teff. Furthermore, by incorporating 2MASS and WISE infrared photometric and GALEX ultraviolet data, we are able to achieve even higher precision estimates for over 2.2 million stars. These results are applicable to both giant and dwarf stars. Building upon this mapping, we construct a foundational dataset for research on metal-poor stars, the structure of the Milky Way, and beyond. With the forthcoming release of additional bands from SAGE Survey such DDO51 and H-alpha, this versatile machine learning approach is poised to play an important role in upcoming surveys featuring expanded filter sets <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03548v1-abstract-full').style.display = 'none'; document.getElementById('2502.03548v1-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 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">Accepted by ApJS.12 pages, 12 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/2502.01963">arXiv:2502.01963</a> <span> [<a href="https://arxiv.org/pdf/2502.01963">pdf</a>, <a href="https://arxiv.org/format/2502.01963">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A search for extremely-high-energy neutrinos and first constraints on the ultra-high-energy cosmic-ray proton fraction with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (402 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="2502.01963v1-abstract-short" style="display: inline;"> We present a search for the diffuse extremely-high-energy neutrino flux using $12.6$ years of IceCube data. The non-observation of neutrinos with energies well above $10 \, \mathrm{PeV}$ constrains the all-flavor neutrino flux at $10^{18} \, \mathrm{eV}$ to a level of $E^2 桅_{谓_e + 谓_渭+ 谓_蟿} \simeq 10^{-8} \, \mathrm{GeV} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1} \, \mathrm{sr}^{-1}$, the most string… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.01963v1-abstract-full').style.display = 'inline'; document.getElementById('2502.01963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.01963v1-abstract-full" style="display: none;"> We present a search for the diffuse extremely-high-energy neutrino flux using $12.6$ years of IceCube data. The non-observation of neutrinos with energies well above $10 \, \mathrm{PeV}$ constrains the all-flavor neutrino flux at $10^{18} \, \mathrm{eV}$ to a level of $E^2 桅_{谓_e + 谓_渭+ 谓_蟿} \simeq 10^{-8} \, \mathrm{GeV} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1} \, \mathrm{sr}^{-1}$, the most stringent limit to date. Using this data, we constrain the proton fraction of ultra-high-energy cosmic rays (UHECRs) above $\simeq 30 \, \mathrm{EeV}$ to be $\lesssim 70\,$% (at $90\,$% CL) if the cosmological evolution of the sources is comparable to or stronger than the star formation rate. This result complements direct air-shower measurements by being insensitive to uncertainties associated with hadronic interaction models. It is the first such result to disfavor the ``proton-only" hypothesis for UHECRs using neutrino data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.01963v1-abstract-full').style.display = 'none'; document.getElementById('2502.01963v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.17472">arXiv:2501.17472</a> <span> [<a href="https://arxiv.org/pdf/2501.17472">pdf</a>, <a href="https://arxiv.org/format/2501.17472">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> </div> </div> <p class="title is-5 mathjax"> A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">Shao-Han Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+B">Bing-Xue Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">Jun-Qiang Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+L">LuLu Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M">Min-Xuan Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Ze-Lin Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Kong%2C+X">Xu Kong</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+H">Haibin Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+B">Bin Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Ya-Ting Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+Q">Qing-feng Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Wan%2C+Z">Zhen Wan</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+J">Jingquan Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Ji-an Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+F">Feng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+M">Ming Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">Hao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+W">Wentao Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Lou%2C+Z">Zhen Lou</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hairen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jian Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tinggui Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xue%2C+Y">Yongquan Xue</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongfei Zhang</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="2501.17472v1-abstract-short" style="display: inline;"> Wide-field surveys have markedly enhanced the discovery and study of solar system objects (SSOs). The 2.5-meter Wide Field Survey Telescope (WFST) represents the foremost facility dedicated to optical time-domain surveys in the northern hemisphere. To fully exploit WFST's capabilities for SSO detection, we have developed a heliocentric-orbiting objects processing system (HOPS) tailored for identif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.17472v1-abstract-full').style.display = 'inline'; document.getElementById('2501.17472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.17472v1-abstract-full" style="display: none;"> Wide-field surveys have markedly enhanced the discovery and study of solar system objects (SSOs). The 2.5-meter Wide Field Survey Telescope (WFST) represents the foremost facility dedicated to optical time-domain surveys in the northern hemisphere. To fully exploit WFST's capabilities for SSO detection, we have developed a heliocentric-orbiting objects processing system (HOPS) tailored for identifying these objects. This system integrates HelioLinC3D, an algorithm well suited for the WFST survey cadence, characterized by revisiting the same sky field twice on the majority of nights. In this paper, we outline the architecture and processing flow of our SSO processing system. The application of the system to the WFST pilot survey data collected between March and May 2024 demonstrates exceptional performance in terms of both temporal efficiency and completeness. A total of 658,489 observations encompassing 38,520 known asteroids have been documented, and 241 newly discovered asteroids have been assigned provisional designations. In particular, 27% of these new discoveries were achieved using merely two observations per night on three nights. The preliminary results not only illuminate the effectiveness of integrating HelioLinC3D within the SSO processing system, but also emphasize the considerable potential contributions of WFST to the field of solar system science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.17472v1-abstract-full').style.display = 'none'; document.getElementById('2501.17472v1-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 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">23 pages, 6 figures, submitted to AAS 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/2501.16440">arXiv:2501.16440</a> <span> [<a href="https://arxiv.org/pdf/2501.16440">pdf</a>, <a href="https://arxiv.org/format/2501.16440">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"> Time-Integrated Southern-Sky Neutrino Source Searches with 10 Years of IceCube Starting-Track Events at Energies Down to 1 TeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (402 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="2501.16440v1-abstract-short" style="display: inline;"> In the IceCube Neutrino Observatory, a signal of astrophysical neutrinos is obscured by backgrounds from atmospheric neutrinos and muons produced in cosmic-ray interactions. IceCube event selections used to isolate the astrophysical neutrino signal often focus on t/he morphology of the light patterns recorded by the detector. The analyses presented here use the new IceCube Enhanced Starting Track… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16440v1-abstract-full').style.display = 'inline'; document.getElementById('2501.16440v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16440v1-abstract-full" style="display: none;"> In the IceCube Neutrino Observatory, a signal of astrophysical neutrinos is obscured by backgrounds from atmospheric neutrinos and muons produced in cosmic-ray interactions. IceCube event selections used to isolate the astrophysical neutrino signal often focus on t/he morphology of the light patterns recorded by the detector. The analyses presented here use the new IceCube Enhanced Starting Track Event Selection (ESTES), which identifies events likely generated by muon neutrino interactions within the detector geometry, focusing on neutrino energies of 1-500 TeV with a median angular resolution of 1.4掳. Selecting for starting track events filters out not only the atmospheric-muon background, but also the atmospheric-neutrino background in the southern sky. This improves IceCube's muon neutrino sensitivity to southern-sky neutrino sources, especially for Galactic sources that are not expected to produce a substantial flux of neutrinos above 100 TeV. In this work, the ESTES sample was applied for the first time to searches for astrophysical sources of neutrinos, including a search for diffuse neutrino emission from the Galactic plane. No significant excesses were identified from any of the analyses; however, constraining limits are set on the hadronic emission from TeV gamma-ray Galactic plane objects and models of the diffuse Galactic plane neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16440v1-abstract-full').style.display = 'none'; document.getElementById('2501.16440v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">23 pages, 8 figures, 4 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/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/2501.09276">arXiv:2501.09276</a> <span> [<a href="https://arxiv.org/pdf/2501.09276">pdf</a>, <a href="https://arxiv.org/format/2501.09276">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for neutrino doublets and triplets using 11.4 years of IceCube data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (402 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="2501.09276v1-abstract-short" style="display: inline;"> We report a search for high-energy astrophysical neutrino multiplets, detections of multiple neutrino clusters in the same direction within 30 days, based on an analysis of 11.4 years of IceCube data. A new search method optimized for transient neutrino emission with a monthly time scale is employed, providing a higher sensitivity to neutrino fluxes. This result is sensitive to neutrino transient… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09276v1-abstract-full').style.display = 'inline'; document.getElementById('2501.09276v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.09276v1-abstract-full" style="display: none;"> We report a search for high-energy astrophysical neutrino multiplets, detections of multiple neutrino clusters in the same direction within 30 days, based on an analysis of 11.4 years of IceCube data. A new search method optimized for transient neutrino emission with a monthly time scale is employed, providing a higher sensitivity to neutrino fluxes. This result is sensitive to neutrino transient emission, reaching per-flavor flux of approximately $10^{-10}\ {\rm erg}\ {\rm cm}^{-2}\ {\rm sec}^{-1}$ from the Northern sky in the energy range $E\gtrsim 50$~TeV. The number of doublets and triplets identified in this search is compatible with the atmospheric background hypothesis, which leads us to set limits on the nature of neutrino transient sources with emission timescales of one month. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09276v1-abstract-full').style.display = 'none'; document.getElementById('2501.09276v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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/2501.07362">arXiv:2501.07362</a> <span> [<a href="https://arxiv.org/pdf/2501.07362">pdf</a>, <a href="https://arxiv.org/format/2501.07362">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/s11433-024-2600-3">10.1007/s11433-024-2600-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Science objectives of the Einstein Probe mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Weimin Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+L">Lixin Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Hua Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+C">Chichuan Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Jonker%2C+P">Peter Jonker</a>, <a href="/search/astro-ph?searchtype=author&query=Kuulkers%2C+E">Erik Kuulkers</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</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=Piro%2C+L">Luigi Piro</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+A">Arne Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J">Jeremy Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Tao%2C+L">Lian Tao</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Junfeng Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X">Xuefeng Wu</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+S">Shuangnan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ai%2C+S">Shunke Ai</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hechao Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M">Minghua Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yong Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yu-Peng Chen</a> , et al. (71 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="2501.07362v1-abstract-short" style="display: inline;"> The Einstein Probe (EP) is an interdisciplinary mission of time-domain and X-ray astronomy. Equipped with a wide-field lobster-eye X-ray focusing imager, EP will discover cosmic X-ray transients and monitor the X-ray variability of known sources in 0.5-4 keV, at a combination of detecting sensitivity and cadence that is not accessible to the previous and current wide-field monitoring missions. EP… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.07362v1-abstract-full').style.display = 'inline'; document.getElementById('2501.07362v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.07362v1-abstract-full" style="display: none;"> The Einstein Probe (EP) is an interdisciplinary mission of time-domain and X-ray astronomy. Equipped with a wide-field lobster-eye X-ray focusing imager, EP will discover cosmic X-ray transients and monitor the X-ray variability of known sources in 0.5-4 keV, at a combination of detecting sensitivity and cadence that is not accessible to the previous and current wide-field monitoring missions. EP can perform quick characterisation of transients or outbursts with a Wolter-I X-ray telescope onboard. In this paper, the science objectives of the Einstein Probe mission are presented. EP is expected to enlarge the sample of previously known or predicted but rare types of transients with a wide range of timescales. Among them, fast extragalactic transients will be surveyed systematically in soft X-rays, which include 纬-ray bursts and their variants, supernova shock breakouts, and the predicted X-ray transients associated with binary neutron star mergers. EP will detect X-ray tidal disruption events and outbursts from active galactic nuclei, possibly at an early phase of the flares for some. EP will monitor the variability and outbursts of X-rays from white dwarfs, neutron stars and black holes in our and neighbouring galaxies at flux levels fainter than those detectable by the current instruments, and is expected to discover new objects. A large sample of stellar X-ray flares will also be detected and characterised. In the era of multi-messenger astronomy, EP has the potential of detecting the possible X-ray counterparts of gravitational wave events, neutrino sources, and ultra-high energy 纬-ray and cosmic ray sources. EP is expected to help advance the studies of extreme objects/phenomena and their underlying physical processes revealed in the dynamic X-ray universe, as well as studies in other areas of X-ray astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.07362v1-abstract-full').style.display = 'none'; document.getElementById('2501.07362v1-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 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">67 pages, 24 figures, accepted for publication in SCIENCE CHINA Physics, Mechanics & 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/2501.05913">arXiv:2501.05913</a> <span> [<a href="https://arxiv.org/pdf/2501.05913">pdf</a>, <a href="https://arxiv.org/format/2501.05913">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"> Dust processing in the terrestrial planet-forming region of the PDS 70 disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dafa Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hongchi Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Haoran Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+M">Min Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+F">Fujun Du</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Perotti%2C+G">Giulia Perotti</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="2501.05913v1-abstract-short" style="display: inline;"> Dust grains in protoplanetary disks are the building blocks of planets. Investigating the dust composition and size, and their variation over time, is crucial for understanding the planet formation process. The PDS 70 disk is so far the only protoplanetary disk with concrete evidence for the presence of young planets. Mid-infrared spectra were obtained for PDS 70 by the Infrared Spectrograph (IRS)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05913v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05913v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05913v1-abstract-full" style="display: none;"> Dust grains in protoplanetary disks are the building blocks of planets. Investigating the dust composition and size, and their variation over time, is crucial for understanding the planet formation process. The PDS 70 disk is so far the only protoplanetary disk with concrete evidence for the presence of young planets. Mid-infrared spectra were obtained for PDS 70 by the Infrared Spectrograph (IRS) on the Spitzer Space Telescope (SST) and the Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) in 2007 and 2022, respectively. In this work, we investigate the dust mineralogy through a detailed decomposition of the observed mid-infrared spectra. The results show that both the dust size and crystallinity increased by a factor of about two during the two epochs of observation, indicating evident dust processing in the terrestrial planet-forming region of the PDS 70 disk. The dust size (~0.8 micron) and crystallinity (~6%) in the PDS 70 disk are similar to those of other disks, which implies that the two nascent planets, PDS 70b and PDS 70c located at radial distances of ~22AU and ~34AU, do not have a significant impact on the dust processing in the inner disk. The flux densities at wavelengths longer than ~16 micron measured by JWST/MIRI are only ~60% of those obtained by Spitzer/IRS. Based on self-consistent radiative transfer modeling, we found that such a strong variability in mid-infrared fluxes can be produced by adjustments to the dust density distribution and structure of the inner disk probably induced by planet-disk interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05913v1-abstract-full').style.display = 'none'; document.getElementById('2501.05913v1-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 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">12 pages, 5 figures, accepted for publication in SCIENCE CHINA Physics, Mechanics & 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/2501.05116">arXiv:2501.05116</a> <span> [<a href="https://arxiv.org/pdf/2501.05116">pdf</a>, <a href="https://arxiv.org/format/2501.05116">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"> Conditioning of the solar corona due to large flares </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thalmann%2C+J+K">Julia K. Thalmann</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+M">Manu Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Veronig%2C+A+M">Astrid M. Veronig</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yang Liu</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="2501.05116v2-abstract-short" style="display: inline;"> We aim to better characterize the conditions of the solar corona, especially with respect to the occurrence of confined and eruptive flares. In this work, we model the coronal evolution around 231 large flares observed during solar cycle 24. Using Helioseismic and Magnetic Imager vector magnetic field data around each event, we employed nonlinear force-free field extrapolations to approximate the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05116v2-abstract-full').style.display = 'inline'; document.getElementById('2501.05116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05116v2-abstract-full" style="display: none;"> We aim to better characterize the conditions of the solar corona, especially with respect to the occurrence of confined and eruptive flares. In this work, we model the coronal evolution around 231 large flares observed during solar cycle 24. Using Helioseismic and Magnetic Imager vector magnetic field data around each event, we employed nonlinear force-free field extrapolations to approximate the coronal energy and helicity budgets of the solar source regions. A superposed epoch analysis and dynamical time warping applied to the time series of selected photospheric and coronal quantities were used to pin down the characteristics of the pre- and postflare time evolution, as well as to assess flare-related changes. During the 24 hours leading up to a major flare, the total magnetic energy and unsigned magnetic flux were seen to evolve closely with respect to each other, irrespective of the flare type. Prior to confined flares, the free energy evolves in a way that exhibits more of a similarity with the unsigned flux than the helicity of the current-carrying field, while the opposite trend is seen prior to eruptive flares. Furthermore, the flare type can be predicted correctly in more than 90\% of major flares when combining measures of the active regions nonpotentiality and local stability. The coronal energy and helicity budgets return to preflare levels within approximately six to 12 hours after eruptive major M-class flares, while the impact of eruptive X-flares lasts considerably longer. Finally, the postflare replenishment times of more than 12 hours after eruptive X-class flares may serve as a partial explanation for the rare observation of eruptive X-class flares within a time frame of a few hours. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05116v2-abstract-full').style.display = 'none'; document.getElementById('2501.05116v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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, 13 figures, 3 tables; accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.04295">arXiv:2501.04295</a> <span> [<a href="https://arxiv.org/pdf/2501.04295">pdf</a>, <a href="https://arxiv.org/format/2501.04295">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"> LAMOST Reveals Long-lived Protoplanetary Disks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xiao-Long Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+M">Min Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+M">Miao-Miao Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">Wen-Yuan Cui</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="2501.04295v1-abstract-short" style="display: inline;"> While both observations and theories demonstrate that protoplanetary disks are not expected to live much longer than $\sim$10 Myr, several examples of prolonged disks have been observed in the past. In this work, we perform a systematic search for aged YSOs still surrounded by protoplanetary disks in the M star catalog from the LAMOST archive. We identify 14 sources older than 10 Myr, still surrou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04295v1-abstract-full').style.display = 'inline'; document.getElementById('2501.04295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04295v1-abstract-full" style="display: none;"> While both observations and theories demonstrate that protoplanetary disks are not expected to live much longer than $\sim$10 Myr, several examples of prolonged disks have been observed in the past. In this work, we perform a systematic search for aged YSOs still surrounded by protoplanetary disks in the M star catalog from the LAMOST archive. We identify 14 sources older than 10 Myr, still surrounded by protoplanetary disks and with ongoing accretion activities, significantly improving the census of the category known as the Peter Pan disks. The stellar parameters, variability and accretion properties of these objects, as well as their spatial distribution, are investigated. Nearly all of these objects are distributed far away from nearby associations and star forming regions, but show evidence of being members of open clusters. Investigating the correlation between mass accretion rates and stellar masses, we find these long-lived disks accrete at systematically lower levels, compared to their younger counterparts with similar stellar masses. Studying the evolution of mass accretion rates with stellar ages, we find these aged disks follow similar trend as young ones. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04295v1-abstract-full').style.display = 'none'; document.getElementById('2501.04295v1-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 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">24 pages, 12 figures, 2 tables, Accepted for publication in 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/2412.18463">arXiv:2412.18463</a> <span> [<a href="https://arxiv.org/pdf/2412.18463">pdf</a>, <a href="https://arxiv.org/format/2412.18463">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Detection of an Orphan X-ray Flare from a Blazar Candidate EP240709a with Einstein Probe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+M">Mingjun Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yijia Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xue%2C+R">Rui Xue</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D">David Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+D+A">D. Andrew Howell</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+W">Wenxiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Monageng%2C+I">Itumeleng Monageng</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Haiwu Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+N">Ning-Chen Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Tinyanont%2C+S">Samaporn Tinyanont</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lingzhi Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Weimin Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+J">Jie An</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+M">Moira Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Anutarawiramkul%2C+R">Rungrit Anutarawiramkul</a>, <a href="/search/astro-ph?searchtype=author&query=Butpan%2C+P">Pathompong Butpan</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+H">Huaqing Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+C">Cui-Yuan Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+L">Lixin Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+J">Joseph Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Hua Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S">Shaoyu Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Z">Zhen Guo</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.18463v1-abstract-short" style="display: inline;"> Blazars are often observed to flare across multiple wavelengths. Orphan flares from blazars have been only detected a few times, providing an opportunity to understand the structure of the jet in the accreting system. We report a remarkable orphan X-ray flare from a blazar candidate EP240709a, detected by Einstein Probe (EP) in July 2024. The multi-band spectral properties and variability support… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18463v1-abstract-full').style.display = 'inline'; document.getElementById('2412.18463v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.18463v1-abstract-full" style="display: none;"> Blazars are often observed to flare across multiple wavelengths. Orphan flares from blazars have been only detected a few times, providing an opportunity to understand the structure of the jet in the accreting system. We report a remarkable orphan X-ray flare from a blazar candidate EP240709a, detected by Einstein Probe (EP) in July 2024. The multi-band spectral properties and variability support EP240709a as a high-energy peaked BL Lacertae-type object. The flux in 0.5-10 keV increases by at least 28 times to the value of low state in 2020, with non-detection of remarkable flaring in other bands during the same period. EP240709a exhibits the harder-when-brighter tendency in the X-ray band during the orphan flare, while its infrared-optical spectra are featureless. We employ one-zone and two-zone leptonic synchrotron self-Compton models to perform the spectral energy distribution fitting. Detecting this rare orphan flare shows the potential of EP in discovering peculiar activities from AGN in high-cadence X-ray sky surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18463v1-abstract-full').style.display = 'none'; document.getElementById('2412.18463v1-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 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">14 pages, 4 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.18301">arXiv:2412.18301</a> <span> [<a href="https://arxiv.org/pdf/2412.18301">pdf</a>, <a href="https://arxiv.org/format/2412.18301">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Position reconstruction using deep learning for the HERD PSD beam test </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yu%2C+L">Longkun Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+C">Chenxing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+D">Dongya Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yaqing Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+W">Wenxi Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Zhigang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+B">Bing Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Qiao%2C+R">Rui Qiao</a>, <a href="/search/astro-ph?searchtype=author&query=Gong%2C+K">Ke Gong</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jing Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Shuai Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yongye 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="2412.18301v2-abstract-short" style="display: inline;"> The High Energy cosmic-Radiation Detection (HERD) facility is a dedicated high energy astronomy and particle physics experiment planned to be installed on the Chinese space station, aiming to detect high-energy cosmic rays (GeV $\sim$ PeV) and high-energy gamma rays ($>$ 500 MeV). The Plastic Scintillator Detector (PSD) is one of the sub-detectors of HERD, with its main function of providing real-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18301v2-abstract-full').style.display = 'inline'; document.getElementById('2412.18301v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.18301v2-abstract-full" style="display: none;"> The High Energy cosmic-Radiation Detection (HERD) facility is a dedicated high energy astronomy and particle physics experiment planned to be installed on the Chinese space station, aiming to detect high-energy cosmic rays (GeV $\sim$ PeV) and high-energy gamma rays ($>$ 500 MeV). The Plastic Scintillator Detector (PSD) is one of the sub-detectors of HERD, with its main function of providing real-time anti-conincidence signals for gamma-ray detection and the secondary function of measuring the charge of cosmic-rays. In 2023, a prototype of PSD was developed and tested at CERN PS&SPS. In this paper, we investigate the position response of the PSD using two reconstruction algorithms: the classic dual-readout ratio and the deep learning method (KAN & MLP neural network). With the latter, we achieved a position resolution of 2 mm (1$蟽$), which is significantly better than the classic method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18301v2-abstract-full').style.display = 'none'; document.getElementById('2412.18301v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.17624">arXiv:2412.17624</a> <span> [<a href="https://arxiv.org/pdf/2412.17624">pdf</a>, <a href="https://arxiv.org/ps/2412.17624">ps</a>, <a href="https://arxiv.org/format/2412.17624">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Axion effects on quark matter and quark-matter cores in massive hybrid stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">He Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yu-Heng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Yong-Hang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Ju%2C+M">Min Ju</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X">Xu-Hao Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">Hong-Ming Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Chu%2C+P">Peng-Cheng Chu</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="2412.17624v1-abstract-short" style="display: inline;"> Using a three-flavor Nambu--Jona-Lasinio model to describe the charge-parity violating effects through axion field, we investigate the axion effects on quark matter and quark-matter cores in massive hybrid stars. The properties of quark matter vary with the scaled axion field $a/f_a$ in a periodic manner, with a period of $2蟺$. Within the range from 0 to $蟺$, axion field decrease the baryon chemic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17624v1-abstract-full').style.display = 'inline'; document.getElementById('2412.17624v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.17624v1-abstract-full" style="display: none;"> Using a three-flavor Nambu--Jona-Lasinio model to describe the charge-parity violating effects through axion field, we investigate the axion effects on quark matter and quark-matter cores in massive hybrid stars. The properties of quark matter vary with the scaled axion field $a/f_a$ in a periodic manner, with a period of $2蟺$. Within the range from 0 to $蟺$, axion field decrease the baryon chemical potential of the first-order phase transition, leading to an increase in normalized pressure and stiffening of the quark matter equation of state. The effect of axions on hybrid star matter that includes the hadron-quark phase transition is contrary to expectations. The axion field shifts the onset of the hadron-quark mixed phase to lower densities but slightly softens the equation of state of the mixed phase matter, which also results in a slight decrease in the maximum mass and corresponding radius of the hybrid stars. However, we also find that the lowering of the onset of the mixed phase significantly increases the radius and mass of the quark-matter core in the hybrid star. Therefore, our results indicate with axion effects, a sizable quark-matter core can appear in $2M_{\odot}$ massive neutron stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17624v1-abstract-full').style.display = 'none'; document.getElementById('2412.17624v1-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 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">7 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/2412.11460">arXiv:2412.11460</a> <span> [<a href="https://arxiv.org/pdf/2412.11460">pdf</a>, <a href="https://arxiv.org/format/2412.11460">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 - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Observation of a spectral hardening in cosmic ray boron spectrum with the DAMPE space mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DAMPE+Collaboration"> DAMPE Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Alemanno%2C+F">F. Alemanno</a>, <a href="/search/astro-ph?searchtype=author&query=Altomare%2C+C">C. Altomare</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F+C+T">F. C. T. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+P">P. Bernardini</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=Boutin%2C+H">H. Boutin</a>, <a href="/search/astro-ph?searchtype=author&query=Cagnoli%2C+I">I. Cagnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M+S">M. S. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Casilli%2C+E">E. Casilli</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzani%2C+E">E. Catanzani</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+D+Y">D. Y. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+J+L">J. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+F">Z. F. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+X">Z. X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Coppin%2C+P">P. Coppin</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+M+Y">M. Y. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+T+S">T. S. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Y+X">Y. X. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=De+Mitri%2C+I">I. De Mitri</a>, <a href="/search/astro-ph?searchtype=author&query=de+Palma%2C+F">F. de Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giovanni%2C+A">A. Di Giovanni</a> , et al. (121 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="2412.11460v2-abstract-short" style="display: inline;"> Secondary cosmic ray fluxes are important probes of the propagation and interaction of high-energy particles in the Galaxy. Recent measurements of primary and secondary cosmic ray nuclei have revealed unexpected spectral features that demand a deeper understanding. In this work we report the direct measurement of the cosmic ray boron spectrum from 10 GeV/n to 8 TeV/n with eight years of data colle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11460v2-abstract-full').style.display = 'inline'; document.getElementById('2412.11460v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.11460v2-abstract-full" style="display: none;"> Secondary cosmic ray fluxes are important probes of the propagation and interaction of high-energy particles in the Galaxy. Recent measurements of primary and secondary cosmic ray nuclei have revealed unexpected spectral features that demand a deeper understanding. In this work we report the direct measurement of the cosmic ray boron spectrum from 10 GeV/n to 8 TeV/n with eight years of data collected by the Dark Matter Particle Explorer (DAMPE) mission. The measured spectrum shows an evident hardening at $182\pm24$ GeV/n with a spectral power index of $纬_1 = 3.02 \pm 0.01$ before the break and an index change of $螖纬= 0.31 \pm 0.05$ after the break. A simple power law model is disfavored at a confidence level of 8$蟽$. Compared with the hardenings measured in the DAMPE proton and helium spectra, the secondary boron spectrum hardens roughly twice as much as these primaries, which is consistent with a propagation related mechanism to interpret the spectral hardenings of cosmic rays observed at hundreds of GeV/n. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11460v2-abstract-full').style.display = 'none'; document.getElementById('2412.11460v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">10 pages, 10 figures, submitted to PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.09956">arXiv:2412.09956</a> <span> [<a href="https://arxiv.org/pdf/2412.09956">pdf</a>, <a href="https://arxiv.org/format/2412.09956">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Exploring the anisotropic gravitational wave background from all-sky mock gravitational wave event catalogues </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhencheng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+Z">Zhen Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yun Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xi-Long Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+L">Liang Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yun Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+T">Tengpeng Xu</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="2412.09956v1-abstract-short" style="display: inline;"> Anisotropic stochastic gravitational wave background (SGWB) serves as a potential probe of the large-scale structure (LSS) of the universe. In this work, we explore the anisotropic SGWB from local ($z < \sim 0.085$) merging stellar mass compact binaries, specifically focusing on merging stellar binary black holes, merging neutron-star-black-hole binaries, and merging binary neutron stars. The anal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09956v1-abstract-full').style.display = 'inline'; document.getElementById('2412.09956v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.09956v1-abstract-full" style="display: none;"> Anisotropic stochastic gravitational wave background (SGWB) serves as a potential probe of the large-scale structure (LSS) of the universe. In this work, we explore the anisotropic SGWB from local ($z < \sim 0.085$) merging stellar mass compact binaries, specifically focusing on merging stellar binary black holes, merging neutron-star-black-hole binaries, and merging binary neutron stars. The analysis employs seven all-sky mock lightcone gravitational wave event catalogues, which are derived from the Millennium simulation combined with a semi-analytic model of galaxy formation and a binary population synthesis model. We calculate the angular power spectra $\mathrm{C}_\ell$ at multipole moments $\ell$, expressed as $\text{log}_{10} [\ell(\ell+1)\mathrm{C}_\ell/(2蟺)]$, based on the skymaps of the overdensity $未_\mathrm{GW}$ in the anisotropic SGWB. The spectra for all three source types exhibit an approximately linear increase with $\text{log}_{10} \ell$ at higher $\ell$ (e.g., $\ell > \sim 30 - 300$) in seven catalogues, with a characteristic slope of $\sim 2$. The spectra of seven catalogues exhibit considerable variations, arising from fluctuations in spatial distribution, primarily in the radial distribution, of nearby sources (e.g., $< 50$ Mpc/h). After subtracting these nearby sources, the variations become much smaller and the spectra for the three source types become closely aligned (within discrepancies of a factor of $\sim 2$ across $\ell = 1 - 1000$ for all catalogues). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09956v1-abstract-full').style.display = 'none'; document.getElementById('2412.09956v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 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">11 pages 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.08390">arXiv:2412.08390</a> <span> [<a href="https://arxiv.org/pdf/2412.08390">pdf</a>, <a href="https://arxiv.org/format/2412.08390">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/10.1051/0004-6361/202449477">10.1051/0004-6361/202449477 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational studies on S-bearing molecules in massive star forming regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Luo%2C+R">R. Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+Z">J. Z. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">X. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Quan%2C+D+H">D. H. Quan</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+X+J">X. J. Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Gou%2C+Q">Q. Gou</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y+Q">Y. Q. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Y+N">Y. N. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+S+Q">S. Q. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Ou%2C+C">C. Ou</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y+J">Y. J. Liu</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="2412.08390v1-abstract-short" style="display: inline;"> Aims. We present observational results of H$_{2}$S 1$_{10}$-1$_{01}$, H$_{2}$$^{34}$S 1$_{10}$-1$_{01}$, H$_{2}$CS 5$_{14}$-4$_{14}$, HCS$^{+}$ 4-3, SiO 4-3, HC$_{3}$N 19-18 and C$^{18}$O 1-0 toward a sample of 51 late-stage massive star-forming regions, to study relationships among H$_{2}$S, H$_{2}$CS, HCS$^{+}$ and SiO in hot cores. Chemical connections of these S-bearing molecules are discussed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08390v1-abstract-full').style.display = 'inline'; document.getElementById('2412.08390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.08390v1-abstract-full" style="display: none;"> Aims. We present observational results of H$_{2}$S 1$_{10}$-1$_{01}$, H$_{2}$$^{34}$S 1$_{10}$-1$_{01}$, H$_{2}$CS 5$_{14}$-4$_{14}$, HCS$^{+}$ 4-3, SiO 4-3, HC$_{3}$N 19-18 and C$^{18}$O 1-0 toward a sample of 51 late-stage massive star-forming regions, to study relationships among H$_{2}$S, H$_{2}$CS, HCS$^{+}$ and SiO in hot cores. Chemical connections of these S-bearing molecules are discussed based on the relations between relative abundances in sources. Results. H$_{2}$S 1$_{10}$-1$_{01}$, H$_{2}$$^{34}$S 1$_{10}$-1$_{01}$, H$_{2}$CS 5$_{14}$-4$_{14}$, HCS$^{+}$ 4-3 and HC$_{3}$N 19-18 were detected in 50 of the 51 sources, while SiO 4-3 was detected in 46 sources. C$^{18}$O 1-0 was detected in all sources. The Pearson correlation coefficients between H$_{2}$CS and HCS$^+$ normalized by H$_{2}$ and H$_{2}$S are 0.94 and 0.87, respectively, and a tight linear relationship is found between them with slope of 1.00 and 1.09, while they are 0.77 and 0.98 between H$_2$S and H$_2$CS, respectively, and 0.76 and 0.97 between H$_2$S and HCS$^+$. The values of full width at half maxima (FWHM) of them in each source are similar to each other, which indicate that they can trace similar regions. Comparing the observed abundance with model results, there is one possible time (2-3$\times$10$^{5}$ yr) for each source in the model. The abundances of these molecules increase with the increment of SiO abundance in these sources, which implies that shock chemistry may be important for them. Conclusions. Close abundance relation of H$_2$S, H$_2$CS and HCS$^+$ molecules and similar line widths in observational results indicate that these three molecules could be chemically linked, with HCS$^+$ and H$_2$CS the most correlated. The comparison of the observational results with chemical models shows that the abundances can be reproduced for almost all the sources at a specific time. The observational results, including abundances in these sources need to be considered in further modeling H$_{2}$S, H$_{2}$CS and HCS$^{+}$ in hot cores with shock chemistry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08390v1-abstract-full').style.display = 'none'; document.getElementById('2412.08390v1-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">15 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 691, A359 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05046">arXiv:2412.05046</a> <span> [<a href="https://arxiv.org/pdf/2412.05046">pdf</a>, <a href="https://arxiv.org/format/2412.05046">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"> Observation of Cosmic-Ray Anisotropy in the Southern Hemisphere with Twelve Years of Data Collected by the IceCube Neutrino Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+T">T. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (413 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="2412.05046v1-abstract-short" style="display: inline;"> We analyzed the 7.92$\times 10^{11}$ cosmic-ray-induced muon events collected by the IceCube Neutrino Observatory from May 13, 2011, when the fully constructed experiment started to take data, to May 12, 2023. This dataset provides an up-to-date cosmic-ray arrival direction distribution in the Southern Hemisphere with unprecedented statistical accuracy covering more than a full period length of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05046v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05046v1-abstract-full" style="display: none;"> We analyzed the 7.92$\times 10^{11}$ cosmic-ray-induced muon events collected by the IceCube Neutrino Observatory from May 13, 2011, when the fully constructed experiment started to take data, to May 12, 2023. This dataset provides an up-to-date cosmic-ray arrival direction distribution in the Southern Hemisphere with unprecedented statistical accuracy covering more than a full period length of a solar cycle. Improvements in Monte Carlo event simulation and better handling of year-to-year differences in data processing significantly reduce systematic uncertainties below the level of statistical fluctuations compared to the previously published results. We confirm the observation of a change in the angular structure of the cosmic-ray anisotropy between 10 TeV and 1 PeV, more specifically in the 100-300 TeV energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05046v1-abstract-full').style.display = 'none'; document.getElementById('2412.05046v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.03316">arXiv:2412.03316</a> <span> [<a href="https://arxiv.org/pdf/2412.03316">pdf</a>, <a href="https://arxiv.org/format/2412.03316">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"> First Detection of Radio Emission from the Intermediate Mass Black Hole in POX 52: Deep Multi-Band Observations with ATCA and VLA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Q">Qi Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+H">Hengxiao Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+M">Minfeng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Stevens%2C+J">Jamie Stevens</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+P+G">Philip G. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yongjun Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Zuo%2C+W">Wenwen Zuo</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jingbo Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jun Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Lira%2C+P">Paulina Lira</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">Tao An</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+R">Renzhi Su</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuanqi Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yijun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+N">Ning Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+P">Pengfei Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+M">Ming 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="2412.03316v2-abstract-short" style="display: inline;"> We present the first multi-band centimeter detection of POX 52, a nearby dwarf galaxy believed to habor a robust intermediate mass black hole (IMBH). We conducted the deep observations using the Australia Telescope Compact Array (ATCA), spanning frequencies from 4.5 to 10 GHz, as well as the sensitive observations from the Karl G. Jansky Very Large Array (VLA) operating in its most extended A-conf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03316v2-abstract-full').style.display = 'inline'; document.getElementById('2412.03316v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.03316v2-abstract-full" style="display: none;"> We present the first multi-band centimeter detection of POX 52, a nearby dwarf galaxy believed to habor a robust intermediate mass black hole (IMBH). We conducted the deep observations using the Australia Telescope Compact Array (ATCA), spanning frequencies from 4.5 to 10 GHz, as well as the sensitive observations from the Karl G. Jansky Very Large Array (VLA) operating in its most extended A-configuration at S band (2--4 GHz) and C band (4--8 GHz). In the ATCA observations, the source shows a compact morphology, with only one direction marginally resolved. The higher resolution of the VLA allowed us to slightly resolve the source, fitting it well with a two-dimensional Gaussian model. The detected radio emission confirms the presence of Active Galactic Nucleus (AGN) activity, indicating either a low-power jet or AGN-driven winds/outflows. Our dual-epoch observations with ATCA and VLA, together with previous non-detection flux density upper limits, reveal radio emission variability spanning two decades. In addition, we find that POX 52 aligns well with the low-mass extension of the fundamental plane for high-accretion, radio-quiet massive AGNs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03316v2-abstract-full').style.display = 'none'; document.getElementById('2412.03316v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">11 pages, 3 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/2412.02409">arXiv:2412.02409</a> <span> [<a href="https://arxiv.org/pdf/2412.02409">pdf</a>, <a href="https://arxiv.org/format/2412.02409">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348581">10.1051/0004-6361/202348581 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The classification of real and bogus transients using active learning and semi-supervised learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yating Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+L">Lulu Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+L">Lei Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">Junqiang Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+Y">Yan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Zelin Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+J">Jiazheng Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Haochen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Kong%2C+X">Xu Kong</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="2412.02409v2-abstract-short" style="display: inline;"> Deep-learning-based methods have been favored in astrophysics owing to their adaptability and remarkable performance and have been applied to the task of the classification of real and bogus transients. Different from most existing approaches which necessitate massive yet expensive annotated data, We aim to leverage training samples with only 1000 labels available to discover real sources that var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02409v2-abstract-full').style.display = 'inline'; document.getElementById('2412.02409v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.02409v2-abstract-full" style="display: none;"> Deep-learning-based methods have been favored in astrophysics owing to their adaptability and remarkable performance and have been applied to the task of the classification of real and bogus transients. Different from most existing approaches which necessitate massive yet expensive annotated data, We aim to leverage training samples with only 1000 labels available to discover real sources that vary in brightness over time in the early stage of the WFST 6-year survey. Methods. We present a novel deep-learning method that combines active learning and semi-supervised learning to construct a competitive real/bogus classifier. Our method incorporates an active learning stage, where we actively select the most informative or uncertain samples for annotation. This stage aims to achieve higher model performance by leveraging fewer labeled samples, thus reducing annotation costs and improving the overall learning process efficiency. Furthermore, our approach involves a semi-supervised learning stage that exploits the unlabeled data to enhance the model's performance and achieve superior results compared to using only the limited labeled data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02409v2-abstract-full').style.display = 'none'; document.getElementById('2412.02409v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">Journal ref:</span> A&A 693, A105 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.02232">arXiv:2412.02232</a> <span> [<a href="https://arxiv.org/pdf/2412.02232">pdf</a>, <a href="https://arxiv.org/format/2412.02232">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Searches for signatures of ultra-light axion dark matter in polarimetry data of the European Pulsar Timing Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Porayko%2C+N+K">N. K. Porayko</a>, <a href="/search/astro-ph?searchtype=author&query=Usynina%2C+P">P. Usynina</a>, <a href="/search/astro-ph?searchtype=author&query=Terol-Calvo%2C+J">J. Terol-Calvo</a>, <a href="/search/astro-ph?searchtype=author&query=Camalich%2C+J+M">J. Martin Camalich</a>, <a href="/search/astro-ph?searchtype=author&query=Shaifullah%2C+G+M">G. M. Shaifullah</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+A">A. Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Blas%2C+D">D. Blas</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</a>, <a href="/search/astro-ph?searchtype=author&query=Peel%2C+M">M. Peel</a>, <a href="/search/astro-ph?searchtype=author&query=Tiburzi%2C+C">C. Tiburzi</a>, <a href="/search/astro-ph?searchtype=author&query=Postnov%2C+K">K. Postnov</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Barausse%2C+E">E. Barausse</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+C">C. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a> , et al. (52 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="2412.02232v1-abstract-short" style="display: inline;"> Ultra-light axion-like particles (ALPs) can be a viable solution to the dark matter problem. The scalar field associated with ALPs, coupled to the electromagnetic field, acts as an active birefringent medium, altering the polarisation properties of light through which it propagates. In particular, oscillations of the axionic field induce monochromatic variations of the plane of linearly polarised… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02232v1-abstract-full').style.display = 'inline'; document.getElementById('2412.02232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.02232v1-abstract-full" style="display: none;"> Ultra-light axion-like particles (ALPs) can be a viable solution to the dark matter problem. The scalar field associated with ALPs, coupled to the electromagnetic field, acts as an active birefringent medium, altering the polarisation properties of light through which it propagates. In particular, oscillations of the axionic field induce monochromatic variations of the plane of linearly polarised radiation of astrophysical signals. The radio emission of millisecond pulsars provides an excellent tool to search for such manifestations, given their high fractional linear polarisation and negligible fluctuations of their polarisation properties. We have searched for the evidence of ALPs in the polarimetry measurements of pulsars collected and preprocessed for the European Pulsar Timing Array (EPTA) campaign. Focusing on the twelve brightest sources in linear polarisation, we searched for an astrophysical signal from axions using both frequentist and Bayesian statistical frameworks. For the frequentist analysis, which uses Lomb-Scargle periodograms at its core, no statistically significant signal has been found. The model used for the Bayesian analysis has been adjusted to accommodate multiple deterministic systematics that may be present in the data. A statistically significant signal has been found in the dataset of multiple pulsars with common frequency between $10^{-8}$ Hz and $2\times10^{-8}$ Hz, which can most likely be explained by the residual Faraday rotation in the terrestrial ionosphere. Strong bounds on the coupling constant $g_{a纬}$, in the same ballpark as other searches, have been obtained in the mass range between $6\times10^{-24}$ eV and $5\times10^{-21}$ eV. We conclude by discussing problems that can limit the sensitivity of our search for ultra-light axions in the polarimetry data of pulsars, and possible ways to resolve them. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02232v1-abstract-full').style.display = 'none'; document.getElementById('2412.02232v1-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 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">24 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/2412.02095">arXiv:2412.02095</a> <span> [<a href="https://arxiv.org/pdf/2412.02095">pdf</a>, <a href="https://arxiv.org/format/2412.02095">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"> The Terminator Region Atmosphere of the hot Jupiter WASP-77Ab with ESPRESSO/VLT observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+Z">Zewen Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Wei Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Guo Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+Y">Yaqing Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhai%2C+M">Meng Zhai</a>, <a href="/search/astro-ph?searchtype=author&query=Rojo%2C+P">Patricio Rojo</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yujuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+G">Gang Zhao</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="2412.02095v1-abstract-short" style="display: inline;"> Atmospheric studies are essential for elucidating the formation history, evolutionary processes, and atmospheric dynamics of exoplanets. High-resolution transmission spectroscopy offers the advantage of detecting subtle variations in stellar spectral profiles, thereby enabling the identification of the sources of observed signals. In this study, we present the transmission spectra of the exoplanet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02095v1-abstract-full').style.display = 'inline'; document.getElementById('2412.02095v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.02095v1-abstract-full" style="display: none;"> Atmospheric studies are essential for elucidating the formation history, evolutionary processes, and atmospheric dynamics of exoplanets. High-resolution transmission spectroscopy offers the advantage of detecting subtle variations in stellar spectral profiles, thereby enabling the identification of the sources of observed signals. In this study, we present the transmission spectra of the exoplanet WASP-77Ab, a hot Jupiter with a 1.36-day orbital period around a G8 host star with $V=11.29$ mag. These observations were conducted using the high-resolution spectrograph ESPRESSO at the Very Large Telescope over three transit events. We analyze the Rossiter-McLaughlin effect for WASP-77A and determine a projected spin-orbit angle of ${位= 16.131^{\circ}}^{+2.106}_{-2.324}$, indicating that the planet's orbit is nearly aligned. Following the generation of transmission spectra for the three nights, we model and correct for center-to-limb variation and the Rossiter-McLaughlin effects. In the residual transmission spectra, we detect H$伪$, H$尾$ and CaII H with a significance exceeding 3.5$蟽$. After applying 0.1-0.5 脜 masks to the cores of these lines to mitigate stellar contamination, all them still shows visible absorptions although not significant, suggesting at least partial planet contribution to them. Therefore, we are yet unable to confirm or reject the planetary origin of these spectral signals based on the current data set. Further investigation of WASP-77Ab's atmosphere, particularly in areas beyond the terminator region, is essential to illuminate the planet's two-dimensional atmospheric structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02095v1-abstract-full').style.display = 'none'; document.getElementById('2412.02095v1-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 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">Accepted for publication in MNRAS. 13 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.01699">arXiv:2412.01699</a> <span> [<a href="https://arxiv.org/pdf/2412.01699">pdf</a>, <a href="https://arxiv.org/format/2412.01699">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Uncovering the Effects of Array Mutual Coupling in 21-cm Experiments with the SKA-Low Radio Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Hara%2C+O+S+D">Oscar S. D. O'Hara</a>, <a href="/search/astro-ph?searchtype=author&query=Gueuning%2C+Q">Quentin Gueuning</a>, <a href="/search/astro-ph?searchtype=author&query=Acedo%2C+E+d+L">Eloy de Lera Acedo</a>, <a href="/search/astro-ph?searchtype=author&query=Dulwich%2C+F">Fred Dulwich</a>, <a href="/search/astro-ph?searchtype=author&query=Cumner%2C+J">John Cumner</a>, <a href="/search/astro-ph?searchtype=author&query=Anstey%2C+D">Dominic Anstey</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">Anthony Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Fialkov%2C+A">Anastasia Fialkov</a>, <a href="/search/astro-ph?searchtype=author&query=Dhandha%2C+J">Jiten Dhandha</a>, <a href="/search/astro-ph?searchtype=author&query=Faulkner%2C+A">Andrew Faulkner</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yuchen Liu</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="2412.01699v2-abstract-short" style="display: inline;"> We investigate the impact of Mutual Coupling (MC) between antennas on the time-delay power spectrum response of the core of the SKA-Low radio telescope. Using two in-house tools - Fast Array Simulation Tool (FAST) (a fast full-wave electromagnetic solver) and OSKAR (a GPU-accelerated radio telescope simulator) - we simulate station beams and compute visibilities for various array layouts (regular,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01699v2-abstract-full').style.display = 'inline'; document.getElementById('2412.01699v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01699v2-abstract-full" style="display: none;"> We investigate the impact of Mutual Coupling (MC) between antennas on the time-delay power spectrum response of the core of the SKA-Low radio telescope. Using two in-house tools - Fast Array Simulation Tool (FAST) (a fast full-wave electromagnetic solver) and OSKAR (a GPU-accelerated radio telescope simulator) - we simulate station beams and compute visibilities for various array layouts (regular, sunflower, and random). Simulations are conducted in an Epoch of Reionisation subband between 120-150~MHz, with a fine frequency resolution of 100~kHz, enabling the investigation of longer delays. Our results show that MC effects significantly increase foreground leakage into longer delays, especially for regular station layouts. For 21-cm science, foreground spill-over into the 21-cm window extends beyond $k_{\parallel} \sim 2$~h$^{-1}$Mpc for all station layouts and across all $k_{\perp}$ modes, completely obscuring the detection window. We find that attempting to remove the foreground contribution from the visibilities using an approximated beam model, based on the average embedded element pattern or interpolating the embedded element patterns from a coarse channel rate of 781~kHz, results in residuals around 1% ($\sim 10^{11}~\mathrm{mK}^2$h$^{-3}\mathrm{Mpc}^3$) which is still around 7 orders of magnitude brighter than the expected level of the EoR signal ($\sim 10^{4}~\mathrm{mK}^2$h$^{-3}\mathrm{Mpc}^3$). We also find that station beam models with at least 4-5 significant digits in the far-field pattern and high spectral resolution are needed for effective foreground removal. Our research provides critical insights into the role of MC in SKA-Low experiments and highlights the computational challenges of fully integrating array patterns that account for MC effects into processing pipelines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01699v2-abstract-full').style.display = 'none'; document.getElementById('2412.01699v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">18 pages, 17 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/2412.00960">arXiv:2412.00960</a> <span> [<a href="https://arxiv.org/pdf/2412.00960">pdf</a>, <a href="https://arxiv.org/format/2412.00960">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/10.1093/mnras/stae2676">10.1093/mnras/stae2676 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Broadband study of the Be X-ray binary RX J0520.5-6932 during its outburst in 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H+N">H. N. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Vasilopoulos%2C+G">G. Vasilopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Jenke%2C+P+A">P. A. Jenke</a>, <a href="/search/astro-ph?searchtype=author&query=Karaferias%2C+A+S">A. S. Karaferias</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+R">R. Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Beri%2C+A">A. Beri</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+L">L. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+C">C. Jin</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+Y+J">Y. J. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+C+Y">C. Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+X+P">X. P. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W+D">W. D. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+C">C. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+Z+X">Z. X. Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H+Y">H. Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+H+Q">H. Q. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H+W">H. W. 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="2412.00960v1-abstract-short" style="display: inline;"> A new giant outburst of the Be X-ray binary RX J0520.5-6932 was detected and subsequently observed with several space-borne and ground-based instruments. This study presents a comprehensive analysis of the optical and X-ray data, focusing on the spectral and timing characteristics of selected X-ray observations. A joint fit of spectra from simultaneous observations performed by the X-ray telescope… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00960v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00960v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00960v1-abstract-full" style="display: none;"> A new giant outburst of the Be X-ray binary RX J0520.5-6932 was detected and subsequently observed with several space-borne and ground-based instruments. This study presents a comprehensive analysis of the optical and X-ray data, focusing on the spectral and timing characteristics of selected X-ray observations. A joint fit of spectra from simultaneous observations performed by the X-ray telescope (XRT) on the Neil Gehrels Swift Observatory (Swift) and Nuclear Spectroscopic Telescope ARray (NuSTAR) provides broadband parameter constraints, including a cyclotron resonant scattering feature (CRSF) at 32.2(+0.8/-0.7) keV with no significant energy change since 2014, and a weaker Fe line. Independent spectral analyses of observations by the Lobster Eye Imager for Astronomy (LEIA), Einstein Probe (EP), Swift-XRT, and NuSTAR demonstrate the consistency of parameters across different bands. Luminosity variations during the current outburst were tracked. The light curve of the Optical Gravitational Lensing Experiment (OGLE) aligns with the X-ray data in both 2014 and 2024. Spin evolution over 10 years is studied after adding Fermi Gamma-ray Burst Monitor (GBM) data, improving the orbital parameters, with an estimated orbital period of 24.39 days, slightly differing from OGLE data. Despite intrinsic spin-up during outbursts, a spin-down of ~0.04s over 10.3 years is suggested. For the new outburst, the pulse profiles indicate a complicated energy-dependent shape, with decreases around 15 keV and 25 keV in the pulsed fraction, a first for an extragalactic source. Phase-resolved NuSTAR data indicate variations in parameters such as flux, photon index, and CRSF energy with rotation phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00960v1-abstract-full').style.display = 'none'; document.getElementById('2412.00960v1-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 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, 15 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.18769">arXiv:2411.18769</a> <span> [<a href="https://arxiv.org/pdf/2411.18769">pdf</a>, <a href="https://arxiv.org/format/2411.18769">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> DeepDISC-photoz: Deep Learning-Based Photometric Redshift Estimation for Rubin LSST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merz%2C+G">Grant Merz</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+X">Xin Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+S">Samuel Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Malz%2C+A+I">Alex I. Malz</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+T">Tianqing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Branton%2C+D">Doug Branton</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Colin J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Delucchi%2C+M">Melissa Delucchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ejjagiri%2C+Y+S">Yaswant Sai Ejjagiri</a>, <a href="/search/astro-ph?searchtype=author&query=Kubica%2C+J">Jeremy Kubica</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yichen Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lynn%2C+O">Olivia Lynn</a>, <a href="/search/astro-ph?searchtype=author&query=Oldag%2C+D">Drew Oldag</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+L+D+E+S">The LSST Dark Energy Science Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.18769v1-abstract-short" style="display: inline;"> Photometric redshifts will be a key data product for the Rubin Observatory Legacy Survey of Space and Time (LSST) as well as for future ground and space-based surveys. The need for photometric redshifts, or photo-zs, arises from sparse spectroscopic coverage of observed galaxies. LSST is expected to observe billions of objects, making it crucial to have a photo-z estimator that is accurate and eff… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18769v1-abstract-full').style.display = 'inline'; document.getElementById('2411.18769v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.18769v1-abstract-full" style="display: none;"> Photometric redshifts will be a key data product for the Rubin Observatory Legacy Survey of Space and Time (LSST) as well as for future ground and space-based surveys. The need for photometric redshifts, or photo-zs, arises from sparse spectroscopic coverage of observed galaxies. LSST is expected to observe billions of objects, making it crucial to have a photo-z estimator that is accurate and efficient. To that end, we present DeepDISC photo-z, a photo-z estimator that is an extension of the DeepDISC framework. The base DeepDISC network simultaneously detects, segments, and classifies objects in multi-band coadded images. We introduce photo-z capabilities to DeepDISC by adding a redshift estimation Region of Interest head, which produces a photo-z probability distribution function for each detected object. On simulated LSST images, DeepDISC photo-z outperforms traditional catalog-based estimators, in both point estimate and probabilistic metrics. We validate DeepDISC by examining dependencies on systematics including galactic extinction, blending and PSF effects. We also examine the impact of the data quality and the size of the training set and model. We find that the biggest factor in DeepDISC photo-z quality is the signal-to-noise of the imaging data, and see a reduction in photo-z scatter approximately proportional to the image data signal-to-noise. Our code is fully public and integrated in the RAIL photo-z package for ease of use and comparison to other codes at https://github.com/LSSTDESC/rail_deepdisc <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18769v1-abstract-full').style.display = 'none'; document.getElementById('2411.18769v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 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/2411.16980">arXiv:2411.16980</a> <span> [<a href="https://arxiv.org/pdf/2411.16980">pdf</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/10.3847/1538-4365/ad746a">10.3847/1538-4365/ad746a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the Behavior and Spatiotemporal Variations of Green Line Emission in the Solar Corona </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oloketuyi%2C+J">Jacob Oloketuyi</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+L">Linhua Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Elmhamdi%2C+A">Abouazza Elmhamdi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+F">Fengrong Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Ibitoye%2C+A">Ayodeji Ibitoye</a>, <a href="/search/astro-ph?searchtype=author&query=Omole%2C+O">Opeyemi Omole</a>, <a href="/search/astro-ph?searchtype=author&query=Sha%2C+F">Feiyang Sha</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Q">Qiang Liu</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="2411.16980v1-abstract-short" style="display: inline;"> Understanding coronal structure and dynamics can be facilitated by analyzing green-line emission, which enables the investigation of diverse coronal structures such as coronal loops, streamers, coronal holes, and various eruptions in the solar atmosphere. In this study, we investigated the spatiotemporal behaviors of green-line emissions in both low and high latitudes across nine solar cycles, ran… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16980v1-abstract-full').style.display = 'inline'; document.getElementById('2411.16980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16980v1-abstract-full" style="display: none;"> Understanding coronal structure and dynamics can be facilitated by analyzing green-line emission, which enables the investigation of diverse coronal structures such as coronal loops, streamers, coronal holes, and various eruptions in the solar atmosphere. In this study, we investigated the spatiotemporal behaviors of green-line emissions in both low and high latitudes across nine solar cycles, ranging from cycle 17 to the current cycle 25, using the Modified Homogeneous Data Set (MHDS). We employed methodologies such as cross-correlation, power spectral density (PSD), and wavelet transform techniques for this analysis. We found distinct behaviors in green line energy across various latitudinal distributions in the solar atmosphere. The trends observed at higher latitudes differ from those at lower latitudes. The emission behaviors show a close association with other solar phenomena like solar flares, sunspots, and coronal mass ejections (CMEs) throughout the solar cycles. The observed variations exhibit harmonic periods. The emission activity is significantly higher in the low latitudes, accounting for over 70 percent of the emissions, while the higher latitudes contribute less than 30 percent. The emissions exhibit asymmetric behavior between the northern and southern hemispheres, leading to a 44-year cycle of solar hemispheric dominance shifts. Various factors, such as Alfv茅n waves, solar magnetic fields, sunspots, differential rotation, and reconnection events, influence the observed differences in behavior between lower and higher latitudes, suggesting the existence of potential underlying phenomena contributing to deviations in properties, intensity, temporal dynamics, and spatiotemporal lifetime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16980v1-abstract-full').style.display = 'none'; document.getElementById('2411.16980v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures, 6 ables, Published in the Astrophysical Journal Supplement Series, 275:3 (21pp), 2024 November</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.15739">arXiv:2411.15739</a> <span> [<a href="https://arxiv.org/pdf/2411.15739">pdf</a>, <a href="https://arxiv.org/format/2411.15739">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A 44-minute periodic radio transient in a supernova remnant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Di Li</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+M">Mao Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+L">Lin Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+J">Jingye Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Lv%2C+X">Xuning Lv</a>, <a href="/search/astro-ph?searchtype=author&query=Tsai%2C+C">Chao-Wei Tsai</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+P">Pei Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">WeiWei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+L">Li Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%2C+A">Ailan Lan</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+R">Renxin Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">Xianglei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Meng%2C+L">Lingqi Meng</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jian Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiangdong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+P">Ping Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Haoran Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Xue%2C+M">Mengyao Xue</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">Jiguang Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Miao%2C+C">Chenchen Miao</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Weiyang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Niu%2C+J">Jiarui Niu</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+Z">Ziyao Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+Q">Qiuyang Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Y">Yi Feng</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="2411.15739v1-abstract-short" style="display: inline;"> Long-period radio transients (LPTs) are a newly discovered class of radio emitters with yet incomprehensibly long rotation periods, ranging from minutes to hours. The astrophysical nature of their isolated counterparts remains undetermined. We report a new LPT, DART J1832-0911 (2656.23 $\pm$ 0.15 s period), the first evidence associating such objects to supernova remnants (SNRs). Its dispersion me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.15739v1-abstract-full').style.display = 'inline'; document.getElementById('2411.15739v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.15739v1-abstract-full" style="display: none;"> Long-period radio transients (LPTs) are a newly discovered class of radio emitters with yet incomprehensibly long rotation periods, ranging from minutes to hours. The astrophysical nature of their isolated counterparts remains undetermined. We report a new LPT, DART J1832-0911 (2656.23 $\pm$ 0.15 s period), the first evidence associating such objects to supernova remnants (SNRs). Its dispersion measure distance aligns well with the distance of the SNR, confirming its origin from a supernova explosion. The source displays either phase-locked circularly polarized emission or nearly 100% linear polarization in radio bands. No detectable optical counterpart was found, even with a 10 m class telescope. The J1832-0911's SNR association, stable, highly polarized emission, and abnormally long period strongly favor its origin from a young neutron star, whose spin has been braked, possibly by interaction with supernova's fallback materials. This discovery provides critical insights into the nature of ultra-long period transients and their evolutionary link to stellar remnants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.15739v1-abstract-full').style.display = 'none'; document.getElementById('2411.15739v1-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 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">36 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/2411.13891">arXiv:2411.13891</a> <span> [<a href="https://arxiv.org/pdf/2411.13891">pdf</a>, <a href="https://arxiv.org/format/2411.13891">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> UPdec-Webb: A Dataset for Coaddition of JWST NIRCam Images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lei Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Shan%2C+H">Huanyuan Shan</a>, <a href="/search/astro-ph?searchtype=author&query=Nie%2C+L">Lin Nie</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C">Cheng Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Fang-Ting Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Q">Qifan Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+G">Guoliang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+Y">Yushan Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Dezi Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+M">Min Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+N">Nan Li</a>, <a href="/search/astro-ph?searchtype=author&query=Jia%2C+P">Peng Jia</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">Ran Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+F">Fengshan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Shu%2C+Y">Yiping Shu</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+C">Chang Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+C">Cheng-Liang Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">Han Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">Wen-Wen Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">Li-Yan Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Kang%2C+X">Xi Kang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.13891v1-abstract-short" style="display: inline;"> We present the application of the image coaddition algorithm, Up-sampling and PSF Deconvolution Coaddition (UPDC), for stacking multiple exposure images captured by the James Webb Space Telescope (JWST) Near-Infrared Camera (NIRCam). By addressing the point spread function (PSF) effect, UPDC provides visually enhanced and sharper images. Furthermore, the anti-aliasing and super-resolution capabili… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13891v1-abstract-full').style.display = 'inline'; document.getElementById('2411.13891v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13891v1-abstract-full" style="display: none;"> We present the application of the image coaddition algorithm, Up-sampling and PSF Deconvolution Coaddition (UPDC), for stacking multiple exposure images captured by the James Webb Space Telescope (JWST) Near-Infrared Camera (NIRCam). By addressing the point spread function (PSF) effect, UPDC provides visually enhanced and sharper images. Furthermore, the anti-aliasing and super-resolution capabilities of UPDC make it easier to deblend sources overlapped on images, yielding a higher accuracy of aperture photometry. We apply this algorithm to the SMACS J0723 imaging data. Comparative analysis with the Drizzle algorithm demonstrates significant improvements in detecting faint sources, achieving accurate photometry, and effectively deblending (super-resolution) closely packed sources. {As a result, we have newly detected a pair of close binary stars that were previously unresolvable in the original exposures or the Drizzled image.} These improvements significantly benefit various scientific projects conducted by JWST. The resulting dataset, named "UPdec-Webb", can be accessible through the official website of the Chinese Virtual Observatory (ChinaVO). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13891v1-abstract-full').style.display = 'none'; document.getElementById('2411.13891v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">21 pages, 18 figures, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.11905">arXiv:2411.11905</a> <span> [<a href="https://arxiv.org/pdf/2411.11905">pdf</a>, <a href="https://arxiv.org/format/2411.11905">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Revisit of discrete energy bands in Galilean moon's footprint tails: remote signals of particle absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+F">Fan Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Xuzhi-Zhou"> Xuzhi-Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Ying Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+Y">Yi-Xin Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Yin%2C+Z">Ze-Fan Yin</a>, <a href="/search/astro-ph?searchtype=author&query=Hao%2C+Y">Yi-Xin Hao</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Z">Zhi-Yang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+M">Michel Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+J">Jiu-Tong Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+D">Dong-Wen He</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Y">Ya-Ze Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">Shan Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yue%2C+C">Chao Yue</a>, <a href="/search/astro-ph?searchtype=author&query=Zong%2C+Q">Qiu-Gang Zong</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="2411.11905v1-abstract-short" style="display: inline;"> Recent observations from the Juno spacecraft during its transit over flux tubes of the Galilean moons have identified sharp enhancements of particle fluxes at discrete energies. These banded structures have been suspected to originate from a bounce resonance between particles and standing Alfven waves generated by the moon-magnetospheric interaction. Here, we show that predictions from the above h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11905v1-abstract-full').style.display = 'inline'; document.getElementById('2411.11905v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.11905v1-abstract-full" style="display: none;"> Recent observations from the Juno spacecraft during its transit over flux tubes of the Galilean moons have identified sharp enhancements of particle fluxes at discrete energies. These banded structures have been suspected to originate from a bounce resonance between particles and standing Alfven waves generated by the moon-magnetospheric interaction. Here, we show that predictions from the above hypothesis are inconsistent with the observations, and propose an alternative interpretation that the banded structures are remote signals of particle absorption at the moons. In this scenario, whether a particle would encounter the moon before reaching Juno depends on the number of bounce cycles it experiences within a fixed section of drift motion determined by moon-spacecraft longitudinal separation. Therefore, the absorption bands are expected to appear at discrete, equally-spaced velocities consistent with the observations. This finding improves our understanding of moon-plasma interactions and provides a potential way to evaluate the Jovian magnetospheric models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11905v1-abstract-full').style.display = 'none'; document.getElementById('2411.11905v1-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 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, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.07970">arXiv:2411.07970</a> <span> [<a href="https://arxiv.org/pdf/2411.07970">pdf</a>, <a href="https://arxiv.org/format/2411.07970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> MUltiplexed Survey Telescope: Perspectives for Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+C">Cheng Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+S">Song Huang</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+M">Mengfan He</a>, <a href="/search/astro-ph?searchtype=author&query=Montero-Camacho%2C+P">Paulo Montero-Camacho</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Renard%2C+P">Pablo Renard</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+Y">Yunyi Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Verdier%2C+A">Aurelien Verdier</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+W">Wenshuo Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaorui Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+J">Jiaxi Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yao Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+S">Siyi Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xingchen Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+S">Shengyu He</a>, <a href="/search/astro-ph?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jiayi Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhuoyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Wen-Ting Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xianyu%2C+Z">Zhong-Zhi Xianyu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yidian Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Gsponer%2C+R">Rafaela Gsponer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiao-Dong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Rocher%2C+A">Antoine Rocher</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+S">Siwei Zou</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07970v2-abstract-short" style="display: inline;"> The MUltiplexed Survey Telescope (MUST) is a 6.5-meter telescope under development. Dedicated to highly-multiplexed, wide-field spectroscopic surveys, MUST observes over 20,000 targets simultaneously using 6.2-mm pitch positioning robots within a ~5 deg2 field of view. MUST aims to carry out the first Stage-V spectroscopic survey in the 2030s to map the 3D Universe with over 100 million galaxies a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07970v2-abstract-full').style.display = 'inline'; document.getElementById('2411.07970v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07970v2-abstract-full" style="display: none;"> The MUltiplexed Survey Telescope (MUST) is a 6.5-meter telescope under development. Dedicated to highly-multiplexed, wide-field spectroscopic surveys, MUST observes over 20,000 targets simultaneously using 6.2-mm pitch positioning robots within a ~5 deg2 field of view. MUST aims to carry out the first Stage-V spectroscopic survey in the 2030s to map the 3D Universe with over 100 million galaxies and quasars, spanning from the nearby Universe to redshift z~5.5, corresponding to around 1 billion years after the Big Bang. To cover this extensive redshift range, we present an initial conceptual target selection algorithm for different types of galaxies, from local bright galaxies, luminous red galaxies, and emission line galaxies to high-redshift (2 < z < 5.5) Lyman-break galaxies. Using Fisher forecasts, we demonstrate that MUST can address fundamental questions in cosmology, including the nature of dark energy, test of gravity theories, and investigations into primordial physics. This is the first paper in the series of science white papers for MUST, with subsequent developments focusing on additional scientific cases such as galaxy and quasar evolution, Milky Way physics, and dynamic phenomena in the time-domain Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07970v2-abstract-full').style.display = 'none'; document.getElementById('2411.07970v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To be submitted to SCPMA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.04749">arXiv:2411.04749</a> <span> [<a href="https://arxiv.org/pdf/2411.04749">pdf</a>, <a href="https://arxiv.org/format/2411.04749">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 - Phenomenology">hep-ph</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="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Berry phase in axion physics: implications for detection, SM global structure, and generalized symmetries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Qing-Hong Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Ge%2C+S">Shuailiang Ge</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yandong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jun-Chen Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.04749v1-abstract-short" style="display: inline;"> We investigate the Berry phase arising from axion-gauge-boson and axion-fermion interactions. The effective Hamiltonians in these two systems are shown to share the same form, enabling a unified description of the Berry phase. This approach offers a new perspective on certain axion experiments, including photon birefringence and storage-ring experiments. Additionally, we conceptually propose a nov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04749v1-abstract-full').style.display = 'inline'; document.getElementById('2411.04749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.04749v1-abstract-full" style="display: none;"> We investigate the Berry phase arising from axion-gauge-boson and axion-fermion interactions. The effective Hamiltonians in these two systems are shown to share the same form, enabling a unified description of the Berry phase. This approach offers a new perspective on certain axion experiments, including photon birefringence and storage-ring experiments. Additionally, we conceptually propose a novel photon-ring experiment for axion detection. Furthermore, we demonstrate that measuring the axion-induced Berry phase provides a unique way for probing the global structure of the Standard Model (SM) gauge group and axion-related generalized symmetries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04749v1-abstract-full').style.display = 'none'; document.getElementById('2411.04749v1-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 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">9 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/2411.01215">arXiv:2411.01215</a> <span> [<a href="https://arxiv.org/pdf/2411.01215">pdf</a>, <a href="https://arxiv.org/format/2411.01215">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Detection of two TeV gamma-ray outbursts from NGC 1275 by LHAASO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T+L">T. L. Chen</a> , et al. (254 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.01215v2-abstract-short" style="display: inline;"> The Water Cherenkov Detector Array (WCDA) is one of the components of Large High Altitude Air Shower Observatory (LHAASO) and can monitor any sources over two-thirds of the sky for up to 7 hours per day with >98\% duty cycle. In this work, we report the detection of two outbursts of the Fanaroff-Riley I radio galaxy NGC 1275 that were detected by LHAASO-WCDA between November 2022 and January 2023… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01215v2-abstract-full').style.display = 'inline'; document.getElementById('2411.01215v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.01215v2-abstract-full" style="display: none;"> The Water Cherenkov Detector Array (WCDA) is one of the components of Large High Altitude Air Shower Observatory (LHAASO) and can monitor any sources over two-thirds of the sky for up to 7 hours per day with >98\% duty cycle. In this work, we report the detection of two outbursts of the Fanaroff-Riley I radio galaxy NGC 1275 that were detected by LHAASO-WCDA between November 2022 and January 2023 with statistical significance of 5.2~$蟽$ and 8.3~$蟽$. The observed spectral energy distribution in the range from 500 GeV to 3 TeV is fitted by a power-law with a best-fit spectral index of $伪=-3.37\pm0.52$ and $-3.35\pm0.29$, respectively. The outburst flux above 0.5~TeV was ($4.55\pm 4.21)\times~10^{-11}~\rm cm^{-2}~s^{-1}$ and ($3.45\pm 1.78)\times~10^{-11}~\rm cm^{-2}~s^{-1}$, corresponding to 60\%, 45\% of Crab Nebula flux. Variation analysis reveals the variability time-scale of days at the TeV energy band. A simple test by one-zone synchrotron self-Compton model reproduces the data in the gamma-ray band well. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01215v2-abstract-full').style.display = 'none'; document.getElementById('2411.01215v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 8 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.00277">arXiv:2411.00277</a> <span> [<a href="https://arxiv.org/pdf/2411.00277">pdf</a>, <a href="https://arxiv.org/format/2411.00277">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451981">10.1051/0004-6361/202451981 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust mass in protoplanetary disks with porous dust opacities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Roussel%2C+H">H茅l猫ne Roussel</a>, <a href="/search/astro-ph?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+M">Min Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Kirchschlager%2C+F">Florian Kirchschlager</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Haifeng Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+F">Fujun Du</a>, <a href="/search/astro-ph?searchtype=author&query=Flock%2C+M">Mario Flock</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hongchi Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.00277v1-abstract-short" style="display: inline;"> ALMA surveys have suggested that protoplanetary disks are not massive enough to form the known exoplanet population, under the assumption that the millimeter continuum emission is optically thin. In this work, we investigate how the mass determination is influenced when the porosity of dust grains is considered in radiative transfer models. The results show that disks with porous dust opacities yi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00277v1-abstract-full').style.display = 'inline'; document.getElementById('2411.00277v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.00277v1-abstract-full" style="display: none;"> ALMA surveys have suggested that protoplanetary disks are not massive enough to form the known exoplanet population, under the assumption that the millimeter continuum emission is optically thin. In this work, we investigate how the mass determination is influenced when the porosity of dust grains is considered in radiative transfer models. The results show that disks with porous dust opacities yield similar dust temperature, but systematically lower millimeter fluxes compared to disks incorporating compact dust grains. Moreover, we recalibrate the relation between dust temperature and stellar luminosity for a wide range of stellar parameters, and calculate the dust masses of a large sample of disks using the traditionally analytic approach. The median dust mass from our calculation is about 6 times higher than the literature result, and this is mostly driven by the different opacities of porous and compact grains. A comparison of the cumulative distribution function between disk dust masses and exoplanet masses show that the median exoplanet mass is about 2 times lower than the median dust mass, if grains are porous, and there are no exoplanetary systems with masses higher than the most massive disks. Our analysis suggests that adopting porous dust opacities may alleviate the mass budget problem for planet formation. As an example illustrating the combined effects of optical depth and porous dust opacities on the mass estimation, we conduct new IRAM/NIKA-2 observations toward the IRAS 04370+2559 disk and perform a detailed radiative transfer modeling of the spectral energy distribution. The best-fit dust mass is roughly 100 times higher than the value from the traditionally analytic calculation. Future spatially resolved observations at various wavelengths are required to better constrain the dust mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00277v1-abstract-full').style.display = 'none'; document.getElementById('2411.00277v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A148 (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/2410.17999">arXiv:2410.17999</a> <span> [<a href="https://arxiv.org/pdf/2410.17999">pdf</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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> LEIA discovery of the longest-lasting and most energetic stellar X-ray flare ever detected </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mao%2C+X">Xuan Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">He-Yang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">Song Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+Z">Zhixing Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Weimin Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+H">Huaqing Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Haiwu Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dongyue Li</a>, <a href="/search/astro-ph?searchtype=author&query=Favata%2C+F">Fabio Favata</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+T">Tuo Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jujia Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+X">Xinlin Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Wan%2C+J">Jing Wan</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zhiming Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">Alberto J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+Y">Yanfeng Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+L">Licai Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+X">Xu Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+K">Kaifan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+C">Chichuan Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Lei%2C+Y">Yajuan Lei</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">Huali Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+J">Jun Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H">Huaqiu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+M">Mingjun Liu</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17999v2-abstract-short" style="display: inline;"> The Lobster Eye Imager for Astronomy (LEIA) detected a new X-ray transient on 2022 November 7, identified as a superflare event occurring on a nearby K-type giant star HD 251108. The flux increase was also detected in follow-up observations at X-ray, UV and optical wavelengths. The flare lasted for about 40 days in soft X-ray observations, reaching a peak luminosity of ~1.1 * 10^34 erg/s in 0.5-4.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17999v2-abstract-full').style.display = 'inline'; document.getElementById('2410.17999v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17999v2-abstract-full" style="display: none;"> The Lobster Eye Imager for Astronomy (LEIA) detected a new X-ray transient on 2022 November 7, identified as a superflare event occurring on a nearby K-type giant star HD 251108. The flux increase was also detected in follow-up observations at X-ray, UV and optical wavelengths. The flare lasted for about 40 days in soft X-ray observations, reaching a peak luminosity of ~1.1 * 10^34 erg/s in 0.5-4.0 keV, which is roughly 60 times the quiescent luminosity. Optical brightening was observed for only one night. The X-ray light curve is well described by a double fast rise and exponential decay model, attributed to the cooling process of a loop arcade structure formed subsequent to the initial large loop with a half-length of ~1.9 * 10^12 cm. Time-resolved X-ray spectra were fitted by a four-temperature apec model (with three components being the quiescent background), showing significant evolution of plasma temperature and emission measure over time. The estimated energy released in the LEIA band is ~3 * 10^39 erg, suggesting that this is likely the most energetic X-ray stellar flare with the longest duration detected to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17999v2-abstract-full').style.display = 'none'; document.getElementById('2410.17999v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">published in ApJ, 15 pages, 7 figures, 8 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/2410.16816">arXiv:2410.16816</a> <span> [<a href="https://arxiv.org/pdf/2410.16816">pdf</a>, <a href="https://arxiv.org/format/2410.16816">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"> An Extreme Radio Fluctuation of Pulsar B1929$+$10 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Zhengli Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+S">Shunshun Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">Jiguang Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yulan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+X">Xun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Jinchen Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+E">Enwei Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Weiyang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+H">Heng Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+R">Renxin Xu</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="2410.16816v1-abstract-short" style="display: inline;"> We report the detection of an extreme flux decrease accompanied by clear dispersion measure (DM) and rotation measure (RM) variations for pulsar B1929+10 during the 110-minute radio observation with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The radio flux decreases by 2 to 3 orders of magnitude within a rapid time scale of about 20 minutes. Meanwhile, the variations of DM a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16816v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16816v1-abstract-full" style="display: none;"> We report the detection of an extreme flux decrease accompanied by clear dispersion measure (DM) and rotation measure (RM) variations for pulsar B1929+10 during the 110-minute radio observation with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The radio flux decreases by 2 to 3 orders of magnitude within a rapid time scale of about 20 minutes. Meanwhile, the variations of DM and RM are approximately 0.05 pc cm$^{-3}$ and 0.7 rad m$^{-2}$, respectively. Frequency-dependent analysis of DM indicates an extremely weak chromatic DM feature, which does not notably affect the radiative behavior detected. Moreover, the pulsar timing analysis shows an additional time delay from 100 $渭$s to 400 $渭$s in the event. These results are speculated to be due to the eclipse and bend for the radio emission of pulsar B1929+10 by a highly dense outflow from the pulsar. This not only impacts the intrinsic radio emission feature but also affects the pulsar timing behavior. Nevertheless, a plasma lens effect lasting around 20 minutes could also be responsible for the event. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16816v1-abstract-full').style.display = 'none'; document.getElementById('2410.16816v1-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 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">13 pages, 6 figures. Accepted for publication in ApJL</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Liu%2C+Y&start=200" 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