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<button class="button is-small 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=Kumar%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a 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href="/search/astro-ph?searchtype=author&query=Nandi%2C+A">Anuj Nandi</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+S">Swapnil Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Jaiswal%2C+B">Bhavesh Jaiswal</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+A">Anand Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Verma%2C+S">Smrati Verma</a>, <a href="/search/astro-ph?searchtype=author&query=Palawat%2C+R">Reenu Palawat</a>, <a href="/search/astro-ph?searchtype=author&query=T.%2C+R+B">Ravishankar B. T.</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+B">Brajpal Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+A">Anurag Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+P">Priyanka Das</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+S">Supratik Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Verma%2C+S">Supriya Verma</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+W+R">Waghmare Rahul Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=R.%2C+Y+P+K">Yogesh Prasad K. R.</a>, <a href="/search/astro-ph?searchtype=author&query=Raha%2C+B">Bijoy Raha</a>, <a href="/search/astro-ph?searchtype=author&query=Mendhekar%2C+B">Bhavesh Mendhekar</a>, <a href="/search/astro-ph?searchtype=author&query=K.%2C+S+R">Sathyanaryana Raju K.</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+S+R+K">Srinivasa Rao Kondapi V.</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sumit Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+M+K">Mukund Kumar Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatia%2C+V">Vinti Bhatia</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+N">Nidhi Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Yenni%2C+G+R">Govinda Rao Yenni</a>, <a href="/search/astro-ph?searchtype=author&query=Satya%2C+N+K">Neeraj Kumar Satya</a>, <a href="/search/astro-ph?searchtype=author&query=Raghavendra%2C+V">Venkata Raghavendra</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.07416v1-abstract-short" style="display: inline;"> SHAPE (Spectro-polarimetry of HAbitable Planet Earth) is an experiment onboard the Chandrayaan-3 Mission, designed to study the spectro-polarimetric signatures of the habitable planet Earth in the near-infrared (NIR) wavelength range (1.0 - 1.7 $渭$m). The spectro-polarimeter is the only scientific payload (experimental in nature) on the Propulsion Module (PM) of the Chandrayaan-3 mission. The inst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07416v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07416v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07416v1-abstract-full" style="display: none;"> SHAPE (Spectro-polarimetry of HAbitable Planet Earth) is an experiment onboard the Chandrayaan-3 Mission, designed to study the spectro-polarimetric signatures of the habitable planet Earth in the near-infrared (NIR) wavelength range (1.0 - 1.7 $渭$m). The spectro-polarimeter is the only scientific payload (experimental in nature) on the Propulsion Module (PM) of the Chandrayaan-3 mission. The instrument is a compact and lightweight spectro-polarimeter with an Acousto-Optic Tunable Filter (AOTF) at its core. The AOTF operates in the frequency range of 80 MHz to 135 MHz with a power of 0.5 - 2.0 Watts. The two output beams (e-beam and o-beam) from the AOTF are focused onto two InGaAs detectors (pixelated, 1D linear array) with the help of focusing optics. The primary (aperture) optics, with a diameter of $\sim$2 mm, collects the NIR light for input to the AOTF, defining the field of view (FOV) of 2.6$^\circ$. The payload has a mass of 4.8 kg and operates at a power of 25 Watts. This manuscript highlights some of the ground-based results, including the post-launch initial performance of the payload while orbiting around the Moon to observe Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07416v1-abstract-full').style.display = 'none'; document.getElementById('2412.07416v1-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 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 Journal of Aerospace Sciences and Technologies</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.06914">arXiv:2412.06914</a> <span> [<a href="https://arxiv.org/pdf/2412.06914">pdf</a>, <a href="https://arxiv.org/format/2412.06914">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 Multiwavelength Autopsy of the Interacting IIn Supernova 2020ywx: Tracing its Progenitor Mass-Loss History for 100 Years before Death </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baer-Way%2C+R">Raphael Baer-Way</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Modjaz%2C+M">Maryam Modjaz</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sahana Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Pellegrino%2C+C">Craig Pellegrino</a>, <a href="/search/astro-ph?searchtype=author&query=Chevalier%2C+R">Roger Chevalier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+A">Adrian Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Sarangi%2C+A">Arkaprabha Sarangi</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+N">Nathan Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Maeda%2C+K">Keiichi Maeda</a>, <a href="/search/astro-ph?searchtype=author&query=Nayana%2C+A+J">A. J. Nayana</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+J+E">Jennifer E. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">Iair Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+K+A">K. Azalee Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+T+G">Thomas G. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Yize Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Dwarkadas%2C+V">Vikram Dwarkadas</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+J+R">Joseph R. Farah</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=Hiramatsu%2C+D">Daichi Hiramatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Hosseinzadeh%2C+G">Griffin Hosseinzadeh</a>, <a href="/search/astro-ph?searchtype=author&query=McCully%2C+C">Curtis McCully</a>, <a href="/search/astro-ph?searchtype=author&query=Meza%2C+N">Nicolas Meza</a>, <a href="/search/astro-ph?searchtype=author&query=Newsome%2C+M">Megan Newsome</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.06914v1-abstract-short" style="display: inline;"> While the subclass of interacting supernovae with narrow hydrogen emission lines (SNe IIn) consists of some of the longest-lasting and brightest SNe ever discovered, their progenitors are still not well understood. Investigating SNe IIn as they emit across the electromagnetic spectrum is the most robust way to understand the progenitor evolution before the explosion. This work presents X-Ray, opti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.06914v1-abstract-full').style.display = 'inline'; document.getElementById('2412.06914v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.06914v1-abstract-full" style="display: none;"> While the subclass of interacting supernovae with narrow hydrogen emission lines (SNe IIn) consists of some of the longest-lasting and brightest SNe ever discovered, their progenitors are still not well understood. Investigating SNe IIn as they emit across the electromagnetic spectrum is the most robust way to understand the progenitor evolution before the explosion. This work presents X-Ray, optical, infrared, and radio observations of the strongly interacting Type IIn SN 2020ywx covering a period $>1200$ days after discovery. Through multiwavelength modeling, we find that the progenitor of 2020ywx was losing mass at $\sim10^{-2}$--$10^{-3} \mathrm{\,M_{\odot}\,yr^{-1}}$ for at least 100 yr pre-explosion using the circumstellar medium (CSM) speed of $120$ km/s measured from our optical and NIR spectra. Despite the similar magnitude of mass-loss measured in different wavelength ranges, we find discrepancies between the X-ray and optical/radio-derived mass-loss evolution, which suggest asymmetries in the CSM. Furthermore, we find evidence for dust formation due to the combination of a growing blueshift in optical emission lines and near-infrared continuum emission which we fit with blackbodies at $\sim$ 1000 K. Based on the observed elevated mass loss over more than 100 years and the configuration of the CSM inferred from the multiwavelength observations, we invoke binary interaction as the most plausible mechanism to explain the overall mass-loss evolution. SN 2020ywx is thus a case that may support the growing observational consensus that SNe IIn mass loss is explained by binary interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.06914v1-abstract-full').style.display = 'none'; document.getElementById('2412.06914v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ, 31 pages, 19 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.01893">arXiv:2412.01893</a> <span> [<a href="https://arxiv.org/pdf/2412.01893">pdf</a>, <a href="https://arxiv.org/format/2412.01893">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"> Performance of Photometric Template Fitting for Ultra-High Redshift Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Clausen%2C+T">Thorbj酶rn Clausen</a>, <a href="/search/astro-ph?searchtype=author&query=Steinhardt%2C+C+L">Charles L. Steinhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Shao%2C+A">Arden Shao</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+G+S">Gaurav Senthil Kumar</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="2412.01893v1-abstract-short" style="display: inline;"> JWST has allowed the discovery of a significant population of galaxies at z > 10. Our understanding of the astrophysical properties of these ultra-high redshift galaxies relies on fitting templates, developed using astrophysical models representing our current understanding of high-redshift galaxies. In this work, the highest confidence recent JWST spectroscopic observations are used to evaluate t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01893v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01893v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01893v1-abstract-full" style="display: none;"> JWST has allowed the discovery of a significant population of galaxies at z > 10. Our understanding of the astrophysical properties of these ultra-high redshift galaxies relies on fitting templates, developed using astrophysical models representing our current understanding of high-redshift galaxies. In this work, the highest confidence recent JWST spectroscopic observations are used to evaluate the performance of several high-redshift templates based on two tests: (1) comparing photometric redshifts against spectroscopic redshifts; and (2) comparing the reconstructed spectral energy distributions against observed SEDs. Strict sample selection and error-propagation by bootstrapping is employed to make results robust towards future JWST systematics mitigation. It is shown that some templates perform adequately at high redshift prediction, given a sample selection by observational filters and depth. Other templates work better for SED fitting, but a few objects remain unrepresented in their spectra. We conclude that although templates are usable, models are not yet able to reliably extract astrophysical properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01893v1-abstract-full').style.display = 'none'; document.getElementById('2412.01893v1-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">16 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/2411.11970">arXiv:2411.11970</a> <span> [<a href="https://arxiv.org/pdf/2411.11970">pdf</a>, <a href="https://arxiv.org/format/2411.11970">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Shadows of generalised Hayward spacetimes : in vacuum and with plasma </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gera%2C+S">Suvikranth Gera</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Saurabh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+P+D">Poulami Dutta Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Chakrabarti%2C+S">Sayan Chakrabarti</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="2411.11970v1-abstract-short" style="display: inline;"> The Hayward regular BH solution attempted to resolve the curvature singularity issue by entering the domain of non-singular spacetimes. Recently, Dutta Roy and Kar (Phys. Rev. D 106, 044028) expanded this solution to encompass a broader range of spacetimes. These spacetimes are constructed based on the Damour-Solodukhin prescription, which involves introducing different metric parameters in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11970v1-abstract-full').style.display = 'inline'; document.getElementById('2411.11970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.11970v1-abstract-full" style="display: none;"> The Hayward regular BH solution attempted to resolve the curvature singularity issue by entering the domain of non-singular spacetimes. Recently, Dutta Roy and Kar (Phys. Rev. D 106, 044028) expanded this solution to encompass a broader range of spacetimes. These spacetimes are constructed based on the Damour-Solodukhin prescription, which involves introducing different metric parameters in the $g_{tt}$ and $g_{rr}$ components of the original Hayward line element, and are characterized by two parameters ($蟽, 魏$). This generalization gives rise to both known and novel regular/singular BHs as well as various types of wormhole spacetimes. In this work, we explore the spacetimes that emerge for different values of ($蟽, 魏$) from the generalized Hayward metric, particularly focusing on their shadows in vacuum and when surrounded by plasma. Intriguingly, we observe the presence of both photon and anti-photon spheres for certain regular spacetimes. Our study highlights the differences in the shadows of different types of regular spacetime compared to those of the singular BH derived from the generalized Hayward metric and also sheds light on the impact of plasma on the shadow radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11970v1-abstract-full').style.display = 'none'; document.getElementById('2411.11970v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 15 figures and 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.01165">arXiv:2411.01165</a> <span> [<a href="https://arxiv.org/pdf/2411.01165">pdf</a>, <a href="https://arxiv.org/format/2411.01165">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> On The Influence Of The Solar Wind On The Propagation Of Earth-impacting Coronal Mass Ejections </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sandeep Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Srivastava%2C+N">Nandita Srivastava</a>, <a href="/search/astro-ph?searchtype=author&query=Gopalswamy%2C+N">Nat Gopalswamy</a>, <a href="/search/astro-ph?searchtype=author&query=Dash%2C+A">Ashutosh Dash</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="2411.01165v1-abstract-short" style="display: inline;"> Coronal Mass Ejections (CMEs) are subject to changes in their direction of propagation, tilt, and other properties as they interact with the variable solar wind. We investigated the heliospheric propagation of 15 Earth-impacting CMEs observed during April 2010 to August 2018 in the field of view (FOV) of the Heliospheric Imager (HI) onboard the STEREO. About half of the 15 events followed self-sim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01165v1-abstract-full').style.display = 'inline'; document.getElementById('2411.01165v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.01165v1-abstract-full" style="display: none;"> Coronal Mass Ejections (CMEs) are subject to changes in their direction of propagation, tilt, and other properties as they interact with the variable solar wind. We investigated the heliospheric propagation of 15 Earth-impacting CMEs observed during April 2010 to August 2018 in the field of view (FOV) of the Heliospheric Imager (HI) onboard the STEREO. About half of the 15 events followed self-similar expansion up to 40 $R_\odot$. The remaining events showed deflection either in latitude, longitude, or a tilt change. Only two events showed significant rotation in the HI1 FOV. We also use toroidal and cylindrical flux rope fitting on the in situ observations of interplanetary magnetic field (IMF) and solar wind parameters to estimate the tilt at L1 for these two events. Although the sample size is small, this study suggests that CME rotation is not very common in the heliosphere. We attributed the observed deflections and rotations of CMEs to a combination of factors, including their interaction with the ambient solar wind and the influence of the ambient magnetic field. These findings contribute to our understanding of the complex dynamics involved in CME propagation and highlight the need for comprehensive modeling and observational studies to improve space weather prediction. In particular, HI observations help us to connect observations near the Sun and near Earth, improving our understanding of how CMEs move through the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.01165v1-abstract-full').style.display = 'none'; document.getElementById('2411.01165v1-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 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">Accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.17291">arXiv:2410.17291</a> <span> [<a href="https://arxiv.org/pdf/2410.17291">pdf</a>, <a href="https://arxiv.org/format/2410.17291">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <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"> Towards a Complete Treatment of Scalar-induced Gravitational Waves with Early Matter Domination </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Tai%2C+H">Hanwen Tai</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lian-Tao Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17291v1-abstract-short" style="display: inline;"> Large curvature perturbations can source an observable amount of stochastic gravitational wave background (SGWB). We consider several scenarios where small-scale curvature perturbations are naturally enhanced due to the presence of additional spectator fields during inflation. The same spectator fields can lead to a period of early matter domination (EMD) after inflation. We compute the inflationa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17291v1-abstract-full').style.display = 'inline'; document.getElementById('2410.17291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17291v1-abstract-full" style="display: none;"> Large curvature perturbations can source an observable amount of stochastic gravitational wave background (SGWB). We consider several scenarios where small-scale curvature perturbations are naturally enhanced due to the presence of additional spectator fields during inflation. The same spectator fields can lead to a period of early matter domination (EMD) after inflation. We compute the inflationary spectrum of curvature perturbation and determine its evolution at later times, taking into account both the onset and the end of the EMD epoch, and also the impact of relative velocity perturbation between matter and radiation. The feature that the same field is responsible for both enhanced perturbations and the EMD era, leads to a predictive framework within which the full frequency dependence of SGWB can be computed. The SGWB can be observed in several detectors, including those focused on the nano-Hz regime. Our numerical framework can also be used to study other non-standard cosmological histories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17291v1-abstract-full').style.display = 'none'; document.getElementById('2410.17291v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 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/2409.17765">arXiv:2409.17765</a> <span> [<a href="https://arxiv.org/pdf/2409.17765">pdf</a>, <a href="https://arxiv.org/format/2409.17765">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="High Energy Astrophysical Phenomena">astro-ph.HE</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"> Eccentric extreme mass-ratio inspirals: A gateway to probe quantum gravity effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zi%2C+T">Tieguang Zi</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shailesh Kumar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.17765v1-abstract-short" style="display: inline;"> We examine a loop quantum gravity (LQG) inspired rotating black hole, treating it as a central supermassive black hole (SMBH) in an extreme mass-ratio inspiral (EMRI) system, where an inspiralling object exhibits eccentric motion around the SMBH. With the orbital dynamics, we derive analytical expressions for the rate of change of orbital energy and angular momentum, as well as orbital evolution,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17765v1-abstract-full').style.display = 'inline'; document.getElementById('2409.17765v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.17765v1-abstract-full" style="display: none;"> We examine a loop quantum gravity (LQG) inspired rotating black hole, treating it as a central supermassive black hole (SMBH) in an extreme mass-ratio inspiral (EMRI) system, where an inspiralling object exhibits eccentric motion around the SMBH. With the orbital dynamics, we derive analytical expressions for the rate of change of orbital energy and angular momentum, as well as orbital evolution, and subsequently generate the gravitational waveforms. To evaluate the difference between EMR waveforms emitted from the Kerr black hole and a spinning black hole in LQG, we compute the dephasing and mismatch using the Laser Interferometer Space Antenna (LISA) observation. Our result indicates that LISA can distinguish the modified effect of LQG with a parameter as small as $2\times10^{-6}$. The constraint on a parameter in LQG using the Fisher information matrix can be obtained within a fraction error of $10^{-6}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17765v1-abstract-full').style.display = 'none'; document.getElementById('2409.17765v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 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/2409.13391">arXiv:2409.13391</a> <span> [<a href="https://arxiv.org/pdf/2409.13391">pdf</a>, <a href="https://arxiv.org/format/2409.13391">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"> Prompt and afterglow analysis of the Fermi-LAT detected GRB 230812B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ror%2C+A+K">Amit K. Ror</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Aryan%2C+A">A. Aryan</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sudhir Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.13391v1-abstract-short" style="display: inline;"> Prompt emission of GRB 230812B stands out as one of the most luminous events observed by both the Fermi-GBM and LAT. Prompt emission spectral analysis (both time-integrated and resolved) of this burst supports an additional thermal component together with a non-thermal, indicating the hybrid jet composition. The spectral parameters alpha, Ep, and kT of the best-fit Band+Blackbody model show a tack… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13391v1-abstract-full').style.display = 'inline'; document.getElementById('2409.13391v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.13391v1-abstract-full" style="display: none;"> Prompt emission of GRB 230812B stands out as one of the most luminous events observed by both the Fermi-GBM and LAT. Prompt emission spectral analysis (both time-integrated and resolved) of this burst supports an additional thermal component together with a non-thermal, indicating the hybrid jet composition. The spectral parameters alpha, Ep, and kT of the best-fit Band+Blackbody model show a tacking behaviour with the intensity. Further, the low energy afterglow emission is consistent with the synchrotron emission from the external forward shock in the ISM medium. LAT detected very high energy emission (VHE) deviating from the synchrotron mechanism, possibly originating from the Lorentz boosting of prompt emission photons by accelerated electrons in the external shock via Inverse Compton (IC) or Synchrotron Self Compton (SSC) emission mechanisms. The comparison of the prompt and afterglow emission properties of this burst revealed that, unlike the bright prompt emission, the afterglow of GRB 230812B is fainter than the other SN-detected bright bursts (GRB 130427A and GRB 171010A) at a similar redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13391v1-abstract-full').style.display = 'none'; document.getElementById('2409.13391v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures and the revised version after addressing the referee's comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.04762">arXiv:2409.04762</a> <span> [<a href="https://arxiv.org/pdf/2409.04762">pdf</a>, <a href="https://arxiv.org/format/2409.04762">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"> Multi-epoch UV $-$ X-ray spectral study of NGC 4151 with AstroSat </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shrabani Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Dewangan%2C+G+C">G. C. Dewangan</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Papadakis%2C+I+E">I. E. Papadakis</a>, <a href="/search/astro-ph?searchtype=author&query=Mithun%2C+N+P+S">N. P. S. Mithun</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+K+P">K. P. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+D">D. Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Zdziarski%2C+A+A">A. A. Zdziarski</a>, <a href="/search/astro-ph?searchtype=author&query=Stewart%2C+G+C">G. C. Stewart</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+S">S. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.04762v1-abstract-short" style="display: inline;"> We present a multi-wavelength spectral study of NGC 4151 based on five epochs of simultaneous AstroSat observations in the near ultra-violet (NUV) to hard X-ray band ($\sim 0.005-80$ keV) during $2017 - 2018$. We derived the intrinsic accretion disk continuum after correcting for internal and Galactic extinction, contributions from broad and narrow line regions, and emission from the host galaxy.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04762v1-abstract-full').style.display = 'inline'; document.getElementById('2409.04762v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.04762v1-abstract-full" style="display: none;"> We present a multi-wavelength spectral study of NGC 4151 based on five epochs of simultaneous AstroSat observations in the near ultra-violet (NUV) to hard X-ray band ($\sim 0.005-80$ keV) during $2017 - 2018$. We derived the intrinsic accretion disk continuum after correcting for internal and Galactic extinction, contributions from broad and narrow line regions, and emission from the host galaxy. We found a bluer continuum at brighter UV flux possibly due to variations in the accretion disk continuum or the UV reddening. We estimated the intrinsic reddening, $E(B-V) \sim 0.4$, using high-resolution HST/STIS spectrum acquired in March 2000. We used thermal Comptonization, neutral and ionized absorption, and X-ray reflection to model the X-ray spectra. We obtained the X-ray absorbing neutral column varying between $N_H \sim 1.2-3.4 \times 10^{23} cm^{-2}$, which are $\sim 100$ times larger than that estimated from UV extinction, assuming the Galactic dust-to-gas ratio. To reconcile this discrepancy, we propose two plausible configurations of the obscurer: (a) a two-zone obscurer consisting of dust-free and dusty regions, divided by the sublimation radius, or (b) a two-phase obscurer consisting of clumpy, dense clouds embedded in a low-density medium, resulting in a scenario where a few dense clouds obscure the compact X-ray source substantially, while the bulk of UV emission arising from the extended accretion disk passes through the low-density medium. Furthermore, we find a positive correlation between X-ray absorption column and $NUV-FUV$ color and UV flux, indicative of enhanced winds possibly driven by the 'bluer-when-brighter' UV continuum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04762v1-abstract-full').style.display = 'none'; document.getElementById('2409.04762v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 22 figures, 6 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.15824">arXiv:2408.15824</a> <span> [<a href="https://arxiv.org/pdf/2408.15824">pdf</a>, <a href="https://arxiv.org/format/2408.15824">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/10.33232/001c.124930">10.33232/001c.124930 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Nature of the C IV-bearing Circumgalactic Medium at z~1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suyash Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hsiao-Wen Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+Z">Zhijie Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+M+C">Mandy C. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Zahedy%2C+F+S">Fakhri S. Zahedy</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+S+D">Sean D. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Muzahid%2C+S">Sowgat Muzahid</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalupo%2C+S">Sebastiano Cantalupo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.15824v2-abstract-short" style="display: inline;"> This paper presents a detailed study of the physical properties of seven C IV absorbers identified at z_abs = 0.68-1.28 along the line of sight toward QSO PG 1522+101 (z_QSO = 1.330). The study leverages high-quality QSO spectra from HST COS and STIS, and Keck HIRES to resolve component structures and to constrain the gas density and elemental abundances of individual components. Under the assumpt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.15824v2-abstract-full').style.display = 'inline'; document.getElementById('2408.15824v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.15824v2-abstract-full" style="display: none;"> This paper presents a detailed study of the physical properties of seven C IV absorbers identified at z_abs = 0.68-1.28 along the line of sight toward QSO PG 1522+101 (z_QSO = 1.330). The study leverages high-quality QSO spectra from HST COS and STIS, and Keck HIRES to resolve component structures and to constrain the gas density and elemental abundances of individual components. Under the assumption of photoionization equilibrium (PIE), five of the 12 C IV components require a mixture of high- and low-density phases to fully explain the observed relative abundances between low-, intermediate-, and high-ionization species. In addition, galaxy surveys carried out using VLT MUSE and Magellan LDSS3C are utilized to characterize the galaxy environments. The results of this analysis are summarized as follows: (1) no luminous galaxies (> 0.1 L*) are found within 100 kpc in projected distance from the C IV absorbers; (2) the C IV selection preferentially targets high-metallicity (near solar) and chemically-evolved gas (~ solar [C/O] elemental abundances) in galaxy halos; (3) the observed narrow line widths of individual C IV components, places a stringent limit on the gas temperature (< 5e4 K) and supports a photoionization origin; (4) additional local ionizing sources beyond the UV ionizing background may be necessary for at least one absorber based on the observed deficit of He I relative to H I; and (5) a PIE assumption may not apply when the gas metallicity exceeds the solar value and the component line width implies a warmer temperature than expected from PIE models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.15824v2-abstract-full').style.display = 'none'; document.getElementById('2408.15824v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 16 figures, accepted to The Open Journal of Astrophysics with revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.12403">arXiv:2408.12403</a> <span> [<a href="https://arxiv.org/pdf/2408.12403">pdf</a>, <a href="https://arxiv.org/format/2408.12403">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.123508">10.1103/PhysRevD.110.123508 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quantifying the $S_8$ tension and evidence for interacting dark energy from redshift-space distortion measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sabogal%2C+M+A">Miguel A. Sabogal</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+E">Emanuelly Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Nunes%2C+R+C">Rafael C. Nunes</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Giar%C3%A8%2C+W">William Giar猫</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.12403v2-abstract-short" style="display: inline;"> In recent years, Cosmic Microwave Background (CMB) observations, Weak Lensing surveys, and $f蟽_8(z)$ measurements from Redshift-Space Distortions (RSD) have revealed a significant ($\sim$3$-$5$蟽$) discrepancy in the inferred value of the matter clustering parameter $S_8$. In this work, we investigate the implications of RSD for a cosmological framework postulating an interaction between Dark Energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12403v2-abstract-full').style.display = 'inline'; document.getElementById('2408.12403v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.12403v2-abstract-full" style="display: none;"> In recent years, Cosmic Microwave Background (CMB) observations, Weak Lensing surveys, and $f蟽_8(z)$ measurements from Redshift-Space Distortions (RSD) have revealed a significant ($\sim$3$-$5$蟽$) discrepancy in the inferred value of the matter clustering parameter $S_8$. In this work, we investigate the implications of RSD for a cosmological framework postulating an interaction between Dark Energy (DE) and Dark Matter (DM). We explore scenarios where DM can transfer energy-momentum to DE or vice versa. The energy-momentum flow is characterized by the strength and the sign of the coupling parameter $尉$. Our baseline analysis combines RSD measurements with the latest data from Baryon Acoustic Oscillations (BAO) observed by DESI, Type Ia Supernovae from the PantheonPlus sample, and CMB data from Planck. We demonstrate that RSD measurements provide significant additional information imposing new and strong upper bounds on possible interaction in the dark sector. Models with $尉> 0$ can effectively alleviate the tension in $S_8$, presenting them as compelling alternatives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12403v2-abstract-full').style.display = 'none'; document.getElementById('2408.12403v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures. Comments welcome and appreciated</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 123508 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.16518">arXiv:2407.16518</a> <span> [<a href="https://arxiv.org/pdf/2407.16518">pdf</a>, <a href="https://arxiv.org/format/2407.16518">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="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 - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> An indirect search for dark matter with a combined analysis of dwarf spheroidal galaxies from VERITAS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. 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=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Duerr%2C+A">A. Duerr</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+G+M">G. M. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">C. E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">J. Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">T. B. Humensky</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+W">W. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+M+N">M. N. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">P. Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Kertzman%2C+M">M. Kertzman</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.16518v2-abstract-short" style="display: inline;"> Understanding the nature and identity of dark matter is a key goal in the physics community. In the case that TeV-scale dark matter particles decay or annihilate into standard model particles, very-high-energy (VHE) gamma rays (greater than 100 GeV) will be present in the final state. The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is an imaging atmospheric Cherenkov telescop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16518v2-abstract-full').style.display = 'inline'; document.getElementById('2407.16518v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16518v2-abstract-full" style="display: none;"> Understanding the nature and identity of dark matter is a key goal in the physics community. In the case that TeV-scale dark matter particles decay or annihilate into standard model particles, very-high-energy (VHE) gamma rays (greater than 100 GeV) will be present in the final state. The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is an imaging atmospheric Cherenkov telescope array that can indirectly detect VHE gamma rays in an energy range of 100 GeV to > 30 TeV. Dwarf spheroidal galaxies (dSphs) are ideal candidates in the search for dark matter due to their high dark matter content, high mass-to-light ratios, and their low gamma-ray fluxes from astrophysical processes. This study uses a legacy data set of 638 hours collected on 17 dSphs, built over 11 years with an observing strategy optimized according to the dark matter content of the targets. The study addresses a broad dark matter particle mass range, extending from 200 GeV to 30 PeV. In the absence of a detection, we set the upper limits on the dark matter velocity-weighted annihilation cross section. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16518v2-abstract-full').style.display = 'none'; document.getElementById('2407.16518v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 7 figures, 3 tables, accepted in PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.11848">arXiv:2407.11848</a> <span> [<a href="https://arxiv.org/pdf/2407.11848">pdf</a>, <a href="https://arxiv.org/format/2407.11848">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"> A multi-wavelength study to decipher the 2017 flare of the blazar OJ 287 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. 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=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+J+P">J. P. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+M">M. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+J">J. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+G">G. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">C. E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+J">J. Hoang</a> , et al. (49 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.11848v3-abstract-short" style="display: inline;"> In February 2017, the blazar OJ~287 underwent a period of intense multiwavelength activity. It reached a new historic peak in the soft X-ray (0.3-10 keV) band, as measured by Swift-XRT. This event coincides with a very-high-energy (VHE) $纬$-ray outburst that led VERITAS to detect emission above 100 GeV, with a detection significance of $10蟽$ (from 2016 December 9 to 2017 March 31). The time-averag… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11848v3-abstract-full').style.display = 'inline'; document.getElementById('2407.11848v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.11848v3-abstract-full" style="display: none;"> In February 2017, the blazar OJ~287 underwent a period of intense multiwavelength activity. It reached a new historic peak in the soft X-ray (0.3-10 keV) band, as measured by Swift-XRT. This event coincides with a very-high-energy (VHE) $纬$-ray outburst that led VERITAS to detect emission above 100 GeV, with a detection significance of $10蟽$ (from 2016 December 9 to 2017 March 31). The time-averaged VHE $纬$-ray spectrum was consistent with a soft power law ($螕= -3.81 \pm 0.26$) and an integral flux corresponding to $\sim2.4\%$ that of the Crab Nebula above the same energy. Contemporaneous data from multiple instruments across the electromagnetic spectrum reveal complex flaring behavior, primarily in the soft X-ray and VHE bands. To investigate the possible origin of such an event, our study focuses on three distinct activity states: before, during, and after the February 2017 peak. The spectral energy distributions during these periods suggest the presence of at least two non-thermal emission zones, with the more compact one responsible for the observed flare. Broadband modeling results and observations of a new radio knot in the jet of OJ~287 in 2017 are consistent with a flare originating from a strong recollimation shock outside the radio core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11848v3-abstract-full').style.display = 'none'; document.getElementById('2407.11848v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 7 figures, accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.03789">arXiv:2407.03789</a> <span> [<a href="https://arxiv.org/pdf/2407.03789">pdf</a>, <a href="https://arxiv.org/format/2407.03789">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="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Preliminary results of the Single Event Effect testing for the ULTRASAT sensors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berlea%2C+V+D">Vlad Dumitru Berlea</a>, <a href="/search/astro-ph?searchtype=author&query=Asif%2C+A">Arooj Asif</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M+F">Merlin F. Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+J+M+H">Juan Maria Haces Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shashank Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Porelli%2C+A">Andrea Porelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Simone%2C+N">Nicola de Simone</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+J">Jason Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Worm%2C+S">Steven Worm</a>, <a href="/search/astro-ph?searchtype=author&query=Zappon%2C+F">Francesco Zappon</a>, <a href="/search/astro-ph?searchtype=author&query=Birman%2C+A">Adi Birman</a>, <a href="/search/astro-ph?searchtype=author&query=Alfassi%2C+S">Shay Alfassi</a>, <a href="/search/astro-ph?searchtype=author&query=Feningstein%2C+A">Amos Feningstein</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">Eli Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+U">Udi Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Liran%2C+T">Tuvia Liran</a>, <a href="/search/astro-ph?searchtype=author&query=Lapid%2C+O">Ofer Lapid</a>, <a href="/search/astro-ph?searchtype=author&query=Algranatti%2C+V+M">Viktor M. Algranatti</a>, <a href="/search/astro-ph?searchtype=author&query=Schvartzvald%2C+Y">Yossi Schvartzvald</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.03789v1-abstract-short" style="display: inline;"> ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is plan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03789v1-abstract-full').style.display = 'inline'; document.getElementById('2407.03789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.03789v1-abstract-full" style="display: none;"> ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is planned for launch in 2026 in collaboration with the Israeli Space Agency and NASA. DESY will provide the UV camera, composed by the detector assembly located in the telescope focal plane and the remote electronics unit. The camera is composed out of four back-metallized CMOS Image Sensors (CIS) manufactured in the 4T, dual gain Tower process. As part of the radiation qualification of the camera, Single Event Effect (SEE) testing has been performed by irradiating the sensor with heavy ions at the RADEF, Jyvaskyla facility. Preliminary results of both Single Event Upset (SEU) and Single Event Latch-up (SEL) occurrence rate in the sensor are presented. Additionally, an in-orbit SEE rate simulation has been performed in order to gain preliminary knowledge about the expected effect of SEE on the mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03789v1-abstract-full').style.display = 'none'; document.getElementById('2407.03789v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18496">arXiv:2406.18496</a> <span> [<a href="https://arxiv.org/pdf/2406.18496">pdf</a>, <a href="https://arxiv.org/format/2406.18496">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <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"> $螞_{\rm s}$CDM cosmology: Alleviating major cosmological tensions by predicting standard neutrino properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yadav%2C+A">Anita Yadav</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Kibris%2C+C">Cihad Kibris</a>, <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.18496v1-abstract-short" style="display: inline;"> We investigate a two-parameter extension of the $螞_{\rm s}$CDM model by allowing variations in the effective number of neutrino species $N_{\rm eff}$ and their total mass $\sum m_谓$. Our motivation is twofold: (i) to examine whether $螞_{\rm s}$CDM retains its success in fitting the data and addressing major cosmological tensions, without suggesting a need for a deviation from the standard model of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18496v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18496v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18496v1-abstract-full" style="display: none;"> We investigate a two-parameter extension of the $螞_{\rm s}$CDM model by allowing variations in the effective number of neutrino species $N_{\rm eff}$ and their total mass $\sum m_谓$. Our motivation is twofold: (i) to examine whether $螞_{\rm s}$CDM retains its success in fitting the data and addressing major cosmological tensions, without suggesting a need for a deviation from the standard model of particle physics, and (ii) to determine whether the data indicate new physics that could potentially address cosmological tensions, either in the post-recombination universe through the late-time mirror AdS-dS transition, or in the pre-recombination universe through modifications in the standard values of $N_{\rm eff}$ and $\sum m_谓$, or both. Within the extended $螞_{\rm s}$CDM model, referred to as $螞_{\rm s}$CDM+$N_{\rm eff}$+$\sum m_{\rm 谓}$, we find no significant tension when considering the Planck-alone analysis. We observe that incorporating BAO data limits the further success of the $螞_{\rm s}$CDM extension. However, the weakly model-dependent BAOtr data, along with Planck and Planck+PP\&SH0ES, favor $H_0\sim 73\,{\rm km\, s^{-1}\, Mpc^{-1}}$. In cases where BAOtr dataset is used, the mirror AdS-dS transition is very effective in providing enhanced $H_0$ values, and thus the model requires no significant deviation from the standard value of $N_{\rm eff} = 3.044$. Both the $H_0$ and $S_8$ tensions are effectively addressed, with some compromise in the case of the Planck+BAO dataset. Finally, the upper bounds obtained on $\sum m_谓\lesssim 0.5$~eV are fully compatible with neutrino oscillation experiments. Our findings provide evidence that late-time physics beyond $螞$CDM, such as $螞_{\rm s}$CDM, without altering the standard pre-recombination universe, can suffice to alleviate the major cosmological tensions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18496v1-abstract-full').style.display = 'none'; document.getElementById('2406.18496v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 6 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/2406.16646">arXiv:2406.16646</a> <span> [<a href="https://arxiv.org/pdf/2406.16646">pdf</a>, <a href="https://arxiv.org/format/2406.16646">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="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/10.1051/0004-6361/202450584">10.1051/0004-6361/202450584 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISTA Variables in the V铆a L谩ctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+S">S. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Baravalle%2C+L">L. Baravalle</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+N">A. N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Duplancic%2C+F">F. Duplancic</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+M">M. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Luna%2C+A">A. Luna</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+M+G">M. G. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J+B">J. B. Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+L">J. L. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Albino%2C+P+H+C">P. H. C. Albino</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. V. Alonso</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="2406.16646v1-abstract-short" style="display: inline;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16646v1-abstract-full" style="display: none;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in $JHK_{\rm s}$ filters from $2016-2023$. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. VVVX took $\sim 2000$ hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. VVVX provides a deep $JHK_{\rm s}$ catalogue of $\gtrsim 1.5\times10^9$ point sources, as well as a $K_{\rm s}$ band catalogue of $\sim 10^7$ variable sources. Within the existing VVV area, we produced a $5D$ map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'none'; document.getElementById('2406.16646v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures (+ appendix). Accepted for publication in Astronomy and Astrophysics in section 14: Catalogs and data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, 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/2406.07526">arXiv:2406.07526</a> <span> [<a href="https://arxiv.org/pdf/2406.07526">pdf</a>, <a href="https://arxiv.org/format/2406.07526">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.103527">10.1103/PhysRevD.110.103527 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmological constraints on $螞_{\rm s}$CDM scenario in a type II minimally modified gravity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+%C3%96">脰zg眉r Akarsu</a>, <a href="/search/astro-ph?searchtype=author&query=De+Felice%2C+A">Antonio De Felice</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Nunes%2C+R+C">Rafael C. Nunes</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%96z%C3%BClker%2C+E">Emre 脰z眉lker</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+J+A">J. Alberto Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Yadav%2C+A">Anita Yadav</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.07526v2-abstract-short" style="display: inline;"> The idea of a rapid sign-switching cosmological constant (mirror AdS-dS transition) in the late universe at $z\sim1.7$, known as the $螞_{\rm s}$CDM model, has significantly improved the fit to observational data and provides a promising scenario for alleviating major cosmological tensions, such as the $H_0$ and $S_8$ tensions. However, in the absence of a fully predictive model, implementing this… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07526v2-abstract-full').style.display = 'inline'; document.getElementById('2406.07526v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07526v2-abstract-full" style="display: none;"> The idea of a rapid sign-switching cosmological constant (mirror AdS-dS transition) in the late universe at $z\sim1.7$, known as the $螞_{\rm s}$CDM model, has significantly improved the fit to observational data and provides a promising scenario for alleviating major cosmological tensions, such as the $H_0$ and $S_8$ tensions. However, in the absence of a fully predictive model, implementing this fit required conjecturing that the dynamics of the linear perturbations are governed by general relativity. Recent work embedding the $螞_{\rm s}$CDM model with the Lagrangian of a type II minimally modified gravity known as VCDM has propelled $螞_{\rm s}$CDM to a fully predictive model, removing the uncertainty related to the aforementioned assumption; we call this new model $螞_{\rm s}$VCDM. In this work, we demonstrate that not only does $螞_{\rm s}$CDM fit the data better than the standard $螞$CDM model, but the new model, $螞_{\rm s}$VCDM, performs even better in alleviating cosmological tensions while also providing a better fit to the data, including CMB, BAO, SNe Ia, and cosmic shear measurements. Our findings highlight the $螞_{\rm s}$CDM framework, particularly the $螞_{\rm s}$VCDM model, as a compelling alternative to the standard $螞$CDM model, especially by successfully alleviating the $H_0$ tension. Additionally, these models predict higher values for $蟽_8$, indicating enhanced structuring, albeit with lower present-day matter density parameter values and consequently reduced $S_8$ values, alleviating the $S_8$ tension as well. This demonstrates that the data are well fit by a combination of background and linear perturbations, both having dynamics differing from those of $螞$CDM. This paves the way for further exploration of new ways for embedding the sign-switching cosmological constant into other models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07526v2-abstract-full').style.display = 'none'; document.getElementById('2406.07526v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 6 figures, 2 tables; matches the version published in Physical Review D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> YITP-24-57 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 103527 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.06328">arXiv:2406.06328</a> <span> [<a href="https://arxiv.org/pdf/2406.06328">pdf</a>, <a href="https://arxiv.org/format/2406.06328">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="Plasma Physics">physics.plasm-ph</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"> Exploring the generation and annihilation of three dimensional nulls through MHD simulations in initially chaotic magnetic field devoid of nulls </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maurya%2C+Y+K">Yogesh Kumar Maurya</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+R">Ramit Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Pontin%2C+D+I">David I. Pontin</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sanjay Kumar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.06328v1-abstract-short" style="display: inline;"> Three-dimensional (3D) magnetic nulls are abundant in the solar atmosphere, as been firmly established through contemporary observations. They are established to be important magnetic structures in, for example, jets and circular ribbon flares. While simulations and extrapolations support this, the mechanisms behind 3D null generation remain an open question. Recent magnetohydrodynamics (MHD) simu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06328v1-abstract-full').style.display = 'inline'; document.getElementById('2406.06328v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06328v1-abstract-full" style="display: none;"> Three-dimensional (3D) magnetic nulls are abundant in the solar atmosphere, as been firmly established through contemporary observations. They are established to be important magnetic structures in, for example, jets and circular ribbon flares. While simulations and extrapolations support this, the mechanisms behind 3D null generation remain an open question. Recent magnetohydrodynamics (MHD) simulations propose that magnetic reconnection is responsible for both generating and annihilating 3D nulls, a novel concept. However, these simulations began with initial magnetic fields already supporting pre-existing nulls, raising the question of whether magnetic reconnection can create nulls in fields initially devoid of them. Previously, this question was briefly explored in a simulation with an initial chaotic magnetic field. However, the study failed to precisely identify locations, topological degrees, and natures (spiral or radial) of nulls, and it approximated magnetic reconnection without fully tracking field line in time. In this paper these findings are revisited in light of recent advancements and tools used to locate and trace nulls, along with the tracing of field lines, through which the concept of generation/annihilation of 3D nulls from chaotic fields is established in a precise manner. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06328v1-abstract-full').style.display = 'none'; document.getElementById('2406.06328v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01220">arXiv:2406.01220</a> <span> [<a href="https://arxiv.org/pdf/2406.01220">pdf</a>, <a href="https://arxiv.org/format/2406.01220">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"> Exploring Origin of Ultra-Long Gamma-ray Bursts: Lessons from GRB 221009A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ror%2C+A+K">Amit Kumar Ror</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+R">Rahul Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Aryan%2C+A">Amar Aryan</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">Shashi Bhushan Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sudhir Kumar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.01220v1-abstract-short" style="display: inline;"> The brightest Gamma-ray burst (GRB) ever, GRB 221009A, displays ultra-long GRB (ULGRB) characteristics, with a prompt emission duration exceeding 1000 s. To constrain the origin and central engine of this unique burst, we analyze its prompt and afterglow characteristics and compare them to the established set of similar GRBs. To achieve this, we statistically examine a nearly complete sample of Sw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01220v1-abstract-full').style.display = 'inline'; document.getElementById('2406.01220v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.01220v1-abstract-full" style="display: none;"> The brightest Gamma-ray burst (GRB) ever, GRB 221009A, displays ultra-long GRB (ULGRB) characteristics, with a prompt emission duration exceeding 1000 s. To constrain the origin and central engine of this unique burst, we analyze its prompt and afterglow characteristics and compare them to the established set of similar GRBs. To achieve this, we statistically examine a nearly complete sample of Swift-detected GRBs with measured redshifts. Categorizing the sample to Bronze, Silver, and Gold by fitting a Gaussian function to the log-normal of T$_{90}$ duration distribution and considering three sub-samples respectively to 1, 2, and 3 times of the standard deviation to the mean value. GRB 221009A falls into the Gold sub-sample. Our analysis of prompt emission and afterglow characteristics aims to identify trends between the three burst groups. Notably, the Gold sub-sample (a higher likelihood of being ULGRB candidates) suggests a collapsar scenario with a hyper-accreting black hole as a potential central engine, while a few GRBs (GRB 060218, GRB 091024A, and GRB 100316D) in our Gold sub-sample favor a magnetar. Late-time near-IR (NIR) observations from 3.6m Devasthal Optical Telescope (DOT) rule out the presence of any bright supernova associated with GRB 221009A in the Gold sub-sample. To further constrain the physical properties of ULGRB progenitors, we employ the tool MESA to simulate the evolution of low-metallicity massive stars with different initial rotations. The outcomes suggest that rotating ($惟\geq 0.2\,惟_{\rm c}$) massive stars could potentially be the progenitors of ULGRBs within the considered parameters and initial inputs to MESA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01220v1-abstract-full').style.display = 'none'; document.getElementById('2406.01220v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Astrophysical Journal: 39 pages, 19 Figures and 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/2405.18508">arXiv:2405.18508</a> <span> [<a href="https://arxiv.org/pdf/2405.18508">pdf</a>, <a href="https://arxiv.org/format/2405.18508">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/10/047">10.1088/1475-7516/2024/10/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring waveforms with non-GR deviations for extreme mass-ratio inspirals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shailesh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+R+K">Rishabh Kumar Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Chowdhuri%2C+A">Abhishek Chowdhuri</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+A">Arpan Bhattacharyya</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.18508v2-abstract-short" style="display: inline;"> The fundamental process of detecting and examining the polarization modes of gravitational waves plays a pivotal role in enhancing our grasp on the precise mechanisms behind their generation. A thorough investigation is essential for delving deeper into the essence of gravitational waves and rigorously evaluating and validating the range of modified gravity theories. In this line of interest, a ge… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18508v2-abstract-full').style.display = 'inline'; document.getElementById('2405.18508v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18508v2-abstract-full" style="display: none;"> The fundamental process of detecting and examining the polarization modes of gravitational waves plays a pivotal role in enhancing our grasp on the precise mechanisms behind their generation. A thorough investigation is essential for delving deeper into the essence of gravitational waves and rigorously evaluating and validating the range of modified gravity theories. In this line of interest, a general description of black holes in theories beyond general relativity can serve a meaningful purpose where distinct deviation parameters can be mapped to solutions representing distinct theories. Employing a refined version of the deformed Kerr geometry, which is free from pathological behaviours such as unphysical divergences in the metric, we explore an extreme mass-ratio inspiral system, wherein a stellar-mass object perturbs a supermassive black hole. We compute the effects of deformation parameters on the rate of change of orbital energy and angular momentum, orbital evolution and phase dynamics with leading order post-Newtonian corrections. With the waveform analysis, we assess the plausibility of detecting deviations from general relativity through observations facilitated by the Laser Interferometer Space Antenna (LISA), simultaneously constraining the extent of these deviations. Therefore, this analysis provides an understanding while highlighting the essential role of observations in advancing gravitational phenomena beyond general relativity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18508v2-abstract-full').style.display = 'none'; document.getElementById('2405.18508v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 5 Figures, Texts modified, Version to appear in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2024) 047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.15027">arXiv:2405.15027</a> <span> [<a href="https://arxiv.org/pdf/2405.15027">pdf</a>, <a href="https://arxiv.org/ps/2405.15027">ps</a>, <a href="https://arxiv.org/format/2405.15027">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"> 1991T-like Supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">M. A. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">Christopher R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+C">Carlos Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">P. Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">S. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">Nidia Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Uddin%2C+S+A">Syed A. Uddin</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Freedman%2C+W+L">Wendy L. Freedman</a>, <a href="/search/astro-ph?searchtype=author&query=Krisciunas%2C+K">Kevin Krisciunas</a>, <a href="/search/astro-ph?searchtype=author&query=Persson%2C+S+E">S. E. Persson</a>, <a href="/search/astro-ph?searchtype=author&query=Piro%2C+A+L">Anthony L. Piro</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M">Maximilian Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">Nicholas B. Suntzeff</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+S">Sudeshna Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Kirshner%2C+R+P">R. P. Kirshner</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">J. Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Marion%2C+G+H">G. H. Marion</a>, <a href="/search/astro-ph?searchtype=author&query=Polin%2C+A">Abigail Polin</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.15027v1-abstract-short" style="display: inline;"> Understanding the nature of the luminous 1991T-like supernovae is of great importance to supernova cosmology as they are likely to have been more common in the early universe. In this paper we explore the observational properties of 1991T-like supernovae to study their relationship to other luminous, slow-declining Type~Ia supernovae (SNe Ia). From the spectroscopic and photometric criteria define… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15027v1-abstract-full').style.display = 'inline'; document.getElementById('2405.15027v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.15027v1-abstract-full" style="display: none;"> Understanding the nature of the luminous 1991T-like supernovae is of great importance to supernova cosmology as they are likely to have been more common in the early universe. In this paper we explore the observational properties of 1991T-like supernovae to study their relationship to other luminous, slow-declining Type~Ia supernovae (SNe Ia). From the spectroscopic and photometric criteria defined in Phillips et al. (1992), we identify 17 1991T-like supernovae from the literature. Combining these objects with ten 1991T-like supernovae from the Carnegie Supernova Project-II, the spectra, light curves, and colors of these events, along with their host galaxy properties, are examined in detail. We conclude that 1991T-like supernovae are closely related in essentially all of their UV, optical, and near-infrared properties -- as well as their host galaxy parameters -- to the slow-declining subset of Branch core-normal supernovae and to the intermediate 1999aa-like events, forming a continuum of luminous SNe Ia. The overriding difference between these three subgroups appears to be the extent to which $^{56}$Ni mixes into the ejecta, producing the pre-maximum spectra dominated by Fe III absorption, the broader UV light curves, and the higher luminosities that characterize the 1991T-like events. Nevertheless, the association of 1991T-like SNe with the rare Type Ia CSM supernovae would seem to run counter to this hypothesis, in which case 1991T-like events may form a separate subclass of SNe Ia, possibly arising from single-degenerate progenitor systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15027v1-abstract-full').style.display = 'none'; document.getElementById('2405.15027v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2405.09607">arXiv:2405.09607</a> <span> [<a href="https://arxiv.org/pdf/2405.09607">pdf</a>, <a href="https://arxiv.org/format/2405.09607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Probing Dark Matter Isocurvature with Primordial Non-Gaussianity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Geller%2C+M">Michael Geller</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lian-Tao 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="2405.09607v1-abstract-short" style="display: inline;"> Multiple fields can become dynamical during the inflationary epoch. We consider an example where a light field acquires isocurvature fluctuations during inflation and contributes to the dark matter abundance at late times. Interactions between the light field and the adiabatic sector contribute to mixed adiabatic-isocurvature non-Gaussianity (NG). We show the resulting form of NG has a different k… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09607v1-abstract-full').style.display = 'inline'; document.getElementById('2405.09607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.09607v1-abstract-full" style="display: none;"> Multiple fields can become dynamical during the inflationary epoch. We consider an example where a light field acquires isocurvature fluctuations during inflation and contributes to the dark matter abundance at late times. Interactions between the light field and the adiabatic sector contribute to mixed adiabatic-isocurvature non-Gaussianity (NG). We show the resulting form of NG has a different kinematic dependence than the 'local shape' commonly considered, and highlight the parameter space where a dedicated search is expected to significantly improve the current $\textit{Planck}$ sensitivity. We interpret our results in the context of the QCD axion and illustrate how the proposed NG searches can improve upon the existing searches for isocurvature power spectrum and bispectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09607v1-abstract-full').style.display = 'none'; document.getElementById('2405.09607v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 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/2405.03738">arXiv:2405.03738</a> <span> [<a href="https://arxiv.org/pdf/2405.03738">pdf</a>, <a href="https://arxiv.org/format/2405.03738">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey 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="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Too Hot to Handle: Searching for Inflationary Particle Production in Planck Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Philcox%2C+O+H+E">Oliver H. E. Philcox</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.03738v1-abstract-short" style="display: inline;"> Non-adiabatic production of massive particles is a generic feature of many inflationary mechanisms. If sufficiently massive, these particles can leave features in the cosmic microwave background (CMB) that are not well-captured by traditional correlation function analyses. We consider a scenario in which particle production occurs only in a narrow time-interval during inflation, eventually leading… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03738v1-abstract-full').style.display = 'inline'; document.getElementById('2405.03738v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03738v1-abstract-full" style="display: none;"> Non-adiabatic production of massive particles is a generic feature of many inflationary mechanisms. If sufficiently massive, these particles can leave features in the cosmic microwave background (CMB) that are not well-captured by traditional correlation function analyses. We consider a scenario in which particle production occurs only in a narrow time-interval during inflation, eventually leading to CMB hot- or coldspots with characteristic shapes and sizes. Searching for such features in CMB data is analogous to searching for late-Universe hot- or coldspots, such as those due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Exploiting this data-analysis parallel, we perform a search for particle-production hotspots in the Planck PR4 temperature dataset, which we implement via a matched-filter analysis. Our pipeline is validated on synthetic observations and found to yield unbiased constraints on sufficiently large hotspots across $\approx 60\%$ of the sky. After removing point sources and tSZ clusters, we find no evidence for new physics and place novel bounds on the coupling between the inflaton and massive particles. These bounds are strongest for larger hotspots, produced early in inflation, whilst sensitivity to smaller hotspots is limited by noise and beam effects. Through such methods we can constrain particles with masses $\mathcal{O}(100)$ times larger than the inflationary Hubble scale, which represents possibly the highest energies ever directly probed with observational data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03738v1-abstract-full').style.display = 'none'; document.getElementById('2405.03738v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 figures, submitted to Phys. Rev. D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.19208">arXiv:2404.19208</a> <span> [<a href="https://arxiv.org/pdf/2404.19208">pdf</a>, <a href="https://arxiv.org/format/2404.19208">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"> Optical Spectroscopy of Type Ia Supernovae by the Carnegie Supernova Projects I and II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">N. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Folatelli%2C+G">G. Folatelli</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M+D">M. D. Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Hamuy%2C+M">M. Hamuy</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">N. B. Suntzeff</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Taddia%2C+F">F. Taddia</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">C. R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">P. Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+C">C. Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">J. Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Piro%2C+A+L">A. L. Piro</a>, <a href="/search/astro-ph?searchtype=author&query=Anais%2C+J">J. Anais</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Burrow%2C+A">A. Burrow</a>, <a href="/search/astro-ph?searchtype=author&query=Busta%2C+L">L. Busta</a>, <a href="/search/astro-ph?searchtype=author&query=Campillay%2C+A">A. Campillay</a>, <a href="/search/astro-ph?searchtype=author&query=Castell%C3%B3n%2C+S">S. Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Corco%2C+C">C. Corco</a>, <a href="/search/astro-ph?searchtype=author&query=Diamond%2C+T">T. Diamond</a>, <a href="/search/astro-ph?searchtype=author&query=Freedman%2C+W+L">W. L. Freedman</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+C">C. Gonz谩lez</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.19208v2-abstract-short" style="display: inline;"> We present the second and final release of optical spectroscopy of Type Ia Supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of the CSP-I, and 234 spectra of 127 SNe Ia obtained during the CSP-II. We also present 216 optical spectra of 46 historical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19208v2-abstract-full').style.display = 'inline'; document.getElementById('2404.19208v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.19208v2-abstract-full" style="display: none;"> We present the second and final release of optical spectroscopy of Type Ia Supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of the CSP-I, and 234 spectra of 127 SNe Ia obtained during the CSP-II. We also present 216 optical spectra of 46 historical SNe Ia, including 53 spectra of 30 SNe Ia observed by the Cal谩n/Tololo Supernova Survey. We combine these observations with previously published CSP data and publicly-available spectra to compile a large sample of measurements of spectroscopic parameters at maximum light, consisting of pseudo-equivalent widths and expansion velocities of selected features, for 232 CSP and historical SNe Ia (including more than 1000 spectra). Finally, we review some of the strongest correlations between spectroscopic and photometric properties of SNe Ia. Specifically, we define two samples: one consisting of SNe Ia discovered by targeted searches (most of them CSP-I objects) and the other composed of SNe Ia discovered by untargeted searches, which includes most of the CSP-II objects. The analysed correlations are similar for both samples. We find a larger incidence of SNe Ia belonging to the Cool (CL)and Broad Line (BL) Branch subtypes among the events discovered by targeted searches, Shallow Silicon (SS) SNe Ia are present with similar frequencies in both samples, while Core Normal (CN) SNe Ia are more frequent in untargeted searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19208v2-abstract-full').style.display = 'none'; document.getElementById('2404.19208v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">59 pages, 16 figures, accepted for publication in The Astrophysical Journal. May 7, 2024: LaTex file updated: corrected one missing comma and an extraneous space in Table 2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17623">arXiv:2404.17623</a> <span> [<a href="https://arxiv.org/pdf/2404.17623">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Broadband Multi-wavelength Properties of M87 during the 2018 EHT Campaign including a Very High Energy Flaring Episode </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Algaba%2C+J+C">J. C. Algaba</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Cheong%2C+W+Y">W. Y. Cheong</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Y+Z">Y. Z. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A+D">A. D. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+N+M">N. M. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Goddi%2C+C">C. Goddi</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Hada%2C+K">K. Hada</a>, <a href="/search/astro-ph?searchtype=author&query=Haggard%2C+D">D. Haggard</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S">S. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Kaur%2C+A">A. Kaur</a>, <a href="/search/astro-ph?searchtype=author&query=Kawashima%2C+T">T. Kawashima</a>, <a href="/search/astro-ph?searchtype=author&query=Kerby%2C+S">S. Kerby</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+Y">J. Y. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kino%2C+M">M. Kino</a>, <a href="/search/astro-ph?searchtype=author&query=Kravchenko%2C+E+V">E. V. Kravchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+S+S">S. S. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+R+S">R. S. Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Markoff%2C+S">S. Markoff</a>, <a href="/search/astro-ph?searchtype=author&query=Michail%2C+J">J. Michail</a>, <a href="/search/astro-ph?searchtype=author&query=Neilsen%2C+J">J. Neilsen</a> , et al. (721 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.17623v3-abstract-short" style="display: inline;"> The nearby elliptical galaxy M87 contains one of the only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. The goal of this extensive MWL campaign was to better understand the physi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17623v3-abstract-full').style.display = 'inline'; document.getElementById('2404.17623v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17623v3-abstract-full" style="display: none;"> The nearby elliptical galaxy M87 contains one of the only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87*, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity. The MWL campaign took place in April 2018, overlapping with the EHT M87* observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high energy (VHE) gamma-rays, as well as details of the individual observations and light curves. We also conduct phenomenological modelling to investigate the basic source properties. We present the first VHE gamma-ray flare from M87 detected since 2010. The flux above 350 GeV has more than doubled within a period of about 36 hours. We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE gamma-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and emphasises the need for combined image and spectral modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17623v3-abstract-full').style.display = 'none'; document.getElementById('2404.17623v3-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">46 pages, 23 figures, accepted by Astronomy & Astrophysics on August. 29, 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17043">arXiv:2404.17043</a> <span> [<a href="https://arxiv.org/pdf/2404.17043">pdf</a>, <a href="https://arxiv.org/format/2404.17043">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A JWST Medium Resolution MIRI Spectrum and Models of the Type Ia supernova 2021aefx at +415 d </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">P. Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Shahbandeh%2C+M">M. Shahbandeh</a>, <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J+M">J. M. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Medler%2C+K">K. Medler</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">M. A. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Fereidouni%2C+E">E. Fereidouni</a>, <a href="/search/astro-ph?searchtype=author&query=Mera%2C+T">T. Mera</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+J">J. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Baade%2C+D">D. Baade</a>, <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+K+A">K. A. Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">P. J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">C. R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Burrow%2C+A">A. Burrow</a>, <a href="/search/astro-ph?searchtype=author&query=Cikota%2C+A">A. Cikota</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">T. de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">A. Do</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Y. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Dominguez%2C+I">I. Dominguez</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+O">O. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Krisciunas%2C+K">K. Krisciunas</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.17043v2-abstract-short" style="display: inline;"> We present a JWST MIRI/MRS spectrum (5-27 $\mathrm渭$m) of the Type Ia supernova (SN Ia), SN 2021aefx at $+415$ days past $B$-band maximum. The spectrum, which was obtained during the iron-dominated nebular phase, has been analyzed in combination with previous JWST observations of SN 2021aefx, to provide the first JWST time series analysis of an SN Ia. We find the temporal evolution of the [Co III]… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17043v2-abstract-full').style.display = 'inline'; document.getElementById('2404.17043v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17043v2-abstract-full" style="display: none;"> We present a JWST MIRI/MRS spectrum (5-27 $\mathrm渭$m) of the Type Ia supernova (SN Ia), SN 2021aefx at $+415$ days past $B$-band maximum. The spectrum, which was obtained during the iron-dominated nebular phase, has been analyzed in combination with previous JWST observations of SN 2021aefx, to provide the first JWST time series analysis of an SN Ia. We find the temporal evolution of the [Co III] 11.888 $\mathrm渭$m feature directly traces the decay of $^{56}$Co. The spectra, line profiles, and their evolution are analyzed with off-center delayed-detonation models. Best fits were obtained with White Dwarf (WD) central densities of $蟻_c=0.9-1.1\times 10^9$g cm$^{-3}$, a WD mass of M$_{\mathrm{WD}}$=1.33-1.35M$_\odot$, a WD magnetic field of $\approx10^6$G, and an off-center deflagration-to-detonation transition at $\approx$ 0.5 $M_\odot$ seen opposite to the line of sight of the observer (-30). The inner electron capture core is dominated by energy deposition from $纬$-rays whereas a broader region is dominated by positron deposition, placing SN 2021aefx at +415 d in the transitional phase of the evolution to the positron-dominated regime. The formerly `flat-tilted' profile at 9 $\mathrm渭$m now has significant contribution from [Ni IV], [Fe II], and [Fe III] and less from [Ar III], which alters the shape of the feature as positrons excite mostly the low-velocity Ar. Overall, the strength of the stable Ni features in the spectrum is dominated by positron transport rather than the Ni mass. Based on multi-dimensional models, our analysis is consistent with a single-spot, close-to-central ignition with an indication for a pre-existing turbulent velocity field, and excludes a multiple-spot, off-center ignition. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17043v2-abstract-full').style.display = 'none'; document.getElementById('2404.17043v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2404.13303">arXiv:2404.13303</a> <span> [<a href="https://arxiv.org/pdf/2404.13303">pdf</a>, <a href="https://arxiv.org/format/2404.13303">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"> Insights on the Optical and Infrared Nature of MAXI J0709-159: Implications for High-Mass X-ray Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+S">Suman Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Mathew%2C+B">Blesson Mathew</a>, <a href="/search/astro-ph?searchtype=author&query=Banerjee%2C+G">Gourav Banerjee</a>, <a href="/search/astro-ph?searchtype=author&query=G%2C+S">Sindhu G</a>, <a href="/search/astro-ph?searchtype=author&query=Muneer%2C+S">S. Muneer</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S+P">S. Pramod Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+S">Santosh Joshi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.13303v1-abstract-short" style="display: inline;"> In our previous study (Bhattacharyya et al., 2022), HD~54786, the optical counterpart of the MAXI J0709-159 system, was identified to be an evolved star, departing from the main sequence, based on comparisons with non-X-ray binary systems. In this paper, using color-magnitude diagram (CMD) analysis for High-Mass X-ray Binaries (HMXBs) and statistical t-tests, we found evidence supporting HD 54786'… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13303v1-abstract-full').style.display = 'inline'; document.getElementById('2404.13303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.13303v1-abstract-full" style="display: none;"> In our previous study (Bhattacharyya et al., 2022), HD~54786, the optical counterpart of the MAXI J0709-159 system, was identified to be an evolved star, departing from the main sequence, based on comparisons with non-X-ray binary systems. In this paper, using color-magnitude diagram (CMD) analysis for High-Mass X-ray Binaries (HMXBs) and statistical t-tests, we found evidence supporting HD 54786's potential membership in both Be/X-ray binaries (BeXRBs) and supergaint X-ray binaries (SgXBs) populations of HMXBs. Hence, our study points towards dual optical characteristics of HD~54786, as an X-ray binary star and also belonging to a distinct evolutionary phase from BeXRB towards SgXB. Our further analysis suggests that MAXI J0709-159, associated with HD 54786, exhibits low-level activity during the current epoch and possesses a limited amount of circumstellar material. Although similarities with the previously studied BeXRB system LSI +61$^{\circ}$ 235 (Coe et al., 1994) are noted, continued monitoring and data collection are essential to fully comprehend the complexities of MAXI J0709-159 and its evolutionary trajectory within the realm of HMXBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13303v1-abstract-full').style.display = 'none'; document.getElementById('2404.13303v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 2 figures, accepted in the Bulletin of Li猫ge Royal Society of Sciences (Proceedings paper for the 3rd BINA Workshop held at ARIES, India)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.12439">arXiv:2403.12439</a> <span> [<a href="https://arxiv.org/pdf/2403.12439">pdf</a>, <a href="https://arxiv.org/format/2403.12439">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</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.dark.2024.101472">10.1016/j.dark.2024.101472 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational signatures of Rotating compact objects in Plasma space-time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Saurabh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Uniyal%2C+A">Akhil Uniyal</a>, <a href="/search/astro-ph?searchtype=author&query=Chakrabarti%2C+S">Sayan Chakrabarti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.12439v2-abstract-short" style="display: inline;"> We have investigated the characteristics of shadows cast by the Kerr black hole in the presence of plasma and compared them to those of a rotating wormhole in a uniform plasma space-time for an observer at infinity. Interestingly, for the same uniform plasma density, the apparent shadow size of the rotating wormhole is always greater than that of the Kerr black hole. To further distinguish the two… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12439v2-abstract-full').style.display = 'inline'; document.getElementById('2403.12439v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.12439v2-abstract-full" style="display: none;"> We have investigated the characteristics of shadows cast by the Kerr black hole in the presence of plasma and compared them to those of a rotating wormhole in a uniform plasma space-time for an observer at infinity. Interestingly, for the same uniform plasma density, the apparent shadow size of the rotating wormhole is always greater than that of the Kerr black hole. To further distinguish the two compact objects we studied the deflection angle and did a comparative study in the presence of the uniform and non-uniform plasma profiles. The goal of this whole exercise is to deepen our understanding of the observational phenomena of these astrophysical objects. The analysis reveals the importance of specific plasma distribution profiles, the impact of plasma on the shadow diameter, and the behavior of deflection angles in different plasma scenarios. We have calculated constraints on the plasma parameters by considering observational data and employing analytical formulations. Our work therefore provides valuable insights into the behavior of light rays near compact objects in plasma space-time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12439v2-abstract-full').style.display = 'none'; document.getElementById('2403.12439v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Dark Univ. 44 (2024) 101472 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.07373">arXiv:2403.07373</a> <span> [<a href="https://arxiv.org/pdf/2403.07373">pdf</a>, <a href="https://arxiv.org/format/2403.07373">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="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/10.1007/s10686-024-09922-2">10.1007/s10686-024-09922-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of VELC detectors on-board Aditya-L1 mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mishra%2C+S">Shalabh Mishra</a>, <a href="/search/astro-ph?searchtype=author&query=Raja%2C+K+S">K. Sasikumar Raja</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+S+K+V">Sanal Krishnan V U</a>, <a href="/search/astro-ph?searchtype=author&query=Narra%2C+V+S">Venkata Suresh Narra</a>, <a href="/search/astro-ph?searchtype=author&query=S%2C+B+H">Bhavana Hegde S</a>, <a href="/search/astro-ph?searchtype=author&query=D.%2C+U">Utkarsha D.</a>, <a href="/search/astro-ph?searchtype=author&query=Priyal%2C+M">Muthu Priyal V</a>, <a href="/search/astro-ph?searchtype=author&query=S%2C+P+K">Pawan Kumar S</a>, <a href="/search/astro-ph?searchtype=author&query=V%2C+N">Natarajan V</a>, <a href="/search/astro-ph?searchtype=author&query=B%2C+R+P">Raghavendra Prasad B</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+J">Jagdev Singh</a>, <a href="/search/astro-ph?searchtype=author&query=P%2C+U+K">Umesh Kamath P</a>, <a href="/search/astro-ph?searchtype=author&query=S%2C+K">Kathiravan S</a>, <a href="/search/astro-ph?searchtype=author&query=T%2C+V">Vishnu T</a>, <a href="/search/astro-ph?searchtype=author&query=Suresha"> Suresha</a>, <a href="/search/astro-ph?searchtype=author&query=P%2C+S">Savarimuthu P</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+J+H">Jalshri H Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Kumaran%2C+R">Rajiv Kumaran</a>, <a href="/search/astro-ph?searchtype=author&query=Sagar%2C+S">Shiv Sagar</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sumit Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Bamrah%2C+I+S">Inderjeet Singh Bamrah</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">Amit Kumar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.07373v1-abstract-short" style="display: inline;"> Aditya-L1 is the first Indian space mission to explore the Sun and solar atmosphere with seven multi-wavelength payloads, with Visible Emission Line Coronagraph (VELC) being the prime payload. It is an internally occulted coronagraph with four channels to image the Sun at 5000 脜~ in the field of view 1.05 - 3 \rsun, and to pursue spectroscopy at 5303 脜, 7892 脜~ and 10747 脜~ channels in the FOV (1.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07373v1-abstract-full').style.display = 'inline'; document.getElementById('2403.07373v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.07373v1-abstract-full" style="display: none;"> Aditya-L1 is the first Indian space mission to explore the Sun and solar atmosphere with seven multi-wavelength payloads, with Visible Emission Line Coronagraph (VELC) being the prime payload. It is an internally occulted coronagraph with four channels to image the Sun at 5000 脜~ in the field of view 1.05 - 3 \rsun, and to pursue spectroscopy at 5303 脜, 7892 脜~ and 10747 脜~ channels in the FOV (1.05 - 1.5 \rsun). In addition, spectropolarimetry is planned at 10747 脜~ channel. Therefore, VELC has three sCMOS detectors and one InGaAs detector. In this article, we aim to describe the technical details and specifications of the detectors achieved by way of thermo-vacuum calibration at the CREST campus of the Indian Institute of Astrophysics, Bangalore, India. Furthermore, we report the estimated conversion gain, full-well capacity, and readout noise at different temperatures. Based on the numbers, it is thus concluded that it is essential to operate the sCMOS detectors and InGaAs detectors at $-5^{\circ}$ and $-17^{\circ}$ C, respectively, at the spacecraft level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07373v1-abstract-full').style.display = 'none'; document.getElementById('2403.07373v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Experimental Astronomy; 13 Pages, 5 Figures and 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/2402.07716">arXiv:2402.07716</a> <span> [<a href="https://arxiv.org/pdf/2402.07716">pdf</a>, <a href="https://arxiv.org/format/2402.07716">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <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"> $螞_{\rm s}$CDM cosmology from a type-II minimally modified gravity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/astro-ph?searchtype=author&query=De+Felice%2C+A">Antonio De Felice</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Nunes%2C+R+C">Rafael C. Nunes</a>, <a href="/search/astro-ph?searchtype=author&query=Ozulker%2C+E">Emre Ozulker</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+J+A">J. Alberto Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Yadav%2C+A">Anita Yadav</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.07716v1-abstract-short" style="display: inline;"> We have successfully integrated $螞_{\rm s}$CDM, a promising model for alleviating cosmological tensions, into a theoretical framework by endowing it with a specific Lagrangian from the VCDM model, a type-II minimally modified gravity. In this theory, we demonstrate that an auxiliary scalar field with a linear potential induces an effective cosmological constant, enabling the realization of an abru… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07716v1-abstract-full').style.display = 'inline'; document.getElementById('2402.07716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07716v1-abstract-full" style="display: none;"> We have successfully integrated $螞_{\rm s}$CDM, a promising model for alleviating cosmological tensions, into a theoretical framework by endowing it with a specific Lagrangian from the VCDM model, a type-II minimally modified gravity. In this theory, we demonstrate that an auxiliary scalar field with a linear potential induces an effective cosmological constant, enabling the realization of an abrupt mirror AdS-dS transition in the late universe through a piecewise linear potential. To eliminate the sudden singularity in this setup and ensure stable transitions, we smooth out this potential. Realized within the VCDM theory, the $螞_{\rm s}$CDM model facilitates two types of rapid smooth mirror AdS-dS transitions: (i) the agitated transition, associated with a smooth jump in the potential, where $螞_{\rm s}$, and consequently $H$, exhibits a bump around the transition's midpoint; and (ii) the quiescent transition, associated with a smooth change in the slope of the potential, where $螞_{\rm s}$ transitions gracefully. These transitions are likely to leave distinct imprints on the background and perturbation dynamics, potentially allowing the observational data to distinguish between them. This novel theoretical framework propels $螞_{\rm s}$CDM into a fully predictive model capable of exploring the evolution of the Universe including the late-time AdS-dS transition epoch, and extends the applicability of the model. We believe further research is crucial in establishing $螞_{\rm s}$CDM as a leading candidate or guide for a new concordance cosmological model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07716v1-abstract-full').style.display = 'none'; document.getElementById('2402.07716v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages (including appendices), 4 figures, and no tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> YITP-24-18 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.02476">arXiv:2402.02476</a> <span> [<a href="https://arxiv.org/pdf/2402.02476">pdf</a>, <a href="https://arxiv.org/format/2402.02476">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"> Constraints on Triton atmospheric evolution from occultations: 1989-2022 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sicardy%2C+B">B. Sicardy</a>, <a href="/search/astro-ph?searchtype=author&query=Tej%2C+A">A. Tej</a>, <a href="/search/astro-ph?searchtype=author&query=Gomes-Junior%2C+A+R">A. R. Gomes-Junior</a>, <a href="/search/astro-ph?searchtype=author&query=Romanov%2C+F+D">F. D. Romanov</a>, <a href="/search/astro-ph?searchtype=author&query=Bertrand%2C+T">T. Bertrand</a>, <a href="/search/astro-ph?searchtype=author&query=Ashok%2C+N+M">N. M. Ashok</a>, <a href="/search/astro-ph?searchtype=author&query=Lellouch%2C+E">E. Lellouch</a>, <a href="/search/astro-ph?searchtype=author&query=Morgado%2C+B+E">B. E. Morgado</a>, <a href="/search/astro-ph?searchtype=author&query=Assafin%2C+M">M. Assafin</a>, <a href="/search/astro-ph?searchtype=author&query=Desmars%2C+J">J. Desmars</a>, <a href="/search/astro-ph?searchtype=author&query=Camargo%2C+J+I+B">J. I. B. Camargo</a>, <a href="/search/astro-ph?searchtype=author&query=Kilic%2C+Y">Y. Kilic</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+J+L">J. L. Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Vieira-Martins%2C+R">R. Vieira-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Braga-Ribas%2C+F">F. Braga-Ribas</a>, <a href="/search/astro-ph?searchtype=author&query=Ninan%2C+J+P">J. P. Ninan</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatt%2C+B+C">B. C. Bhatt</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S+P">S. Pramod Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Swain%2C+V">V. Swain</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+S">S. Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">A. Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Ojha%2C+D+K">D. K. Ojha</a>, <a href="/search/astro-ph?searchtype=author&query=Pawar%2C+G">G. Pawar</a>, <a href="/search/astro-ph?searchtype=author&query=Deshmukh%2C+S">S. Deshmukh</a>, <a href="/search/astro-ph?searchtype=author&query=Deshpande%2C+A">A. Deshpande</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="2402.02476v1-abstract-short" style="display: inline;"> Context - Around the year 2000, Triton's south pole experienced an extreme summer solstice that occurs every about 650 years, when the subsolar latitude reached about 50掳. Bracketing this epoch, a few occultations probed Triton's atmosphere in 1989, 1995, 1997, 2008 and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of Triton's atmospheric pre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.02476v1-abstract-full').style.display = 'inline'; document.getElementById('2402.02476v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.02476v1-abstract-full" style="display: none;"> Context - Around the year 2000, Triton's south pole experienced an extreme summer solstice that occurs every about 650 years, when the subsolar latitude reached about 50掳. Bracketing this epoch, a few occultations probed Triton's atmosphere in 1989, 1995, 1997, 2008 and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of Triton's atmospheric pressure which is presented here. Aims- The goal is to constrain the Volatile Transport Models (VTMs) of Triton's atmosphere that is basically in vapor pressure equilibrium with the nitrogen ice at its surface. Methods - Fits to the occultation light curves yield Triton's atmospheric pressure at the reference radius 1400 km, from which the surface pressure is induced. Results - The fits provide a pressure p_1400= 1.211 +/- 0.039 microbar at radius 1400 km (47 km altitude), from which a surface pressure of p_surf= 14.54 +/- 0.47 microbar is induced (1-sigma error bars). To within error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p_1400 = 1.18 +/- 0.03 microbar and p_surf= 14.1 +/- 0.4 microbar, respectively. Based on recent models of Triton's volatile cycles, the overall evolution over the last 30 years of the surface pressure is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton could explain the relatively constant pressure between 2017 and 2022. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.02476v1-abstract-full').style.display = 'none'; document.getElementById('2402.02476v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.14474">arXiv:2401.14474</a> <span> [<a href="https://arxiv.org/pdf/2401.14474">pdf</a>, <a href="https://arxiv.org/format/2401.14474">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> JWST NIRSpec+MIRI Observations of the nearby Type IIP supernova 2022acko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shahbandeh%2C+M">M. Shahbandeh</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">P. Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+O">O. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Mera%2C+T">T. Mera</a>, <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J">J. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M+D">M. D. Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B">B. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D">D. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Morrison%2C+J">J. Morrison</a>, <a href="/search/astro-ph?searchtype=author&query=Pauly%2C+T">T. Pauly</a>, <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J">J. Pierel</a>, <a href="/search/astro-ph?searchtype=author&query=Medler%2C+K">K. Medler</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+J">J. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Baade%2C+D">D. Baade</a>, <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+A">A. Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P">P. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C">C. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Burrow%2C+A">A. Burrow</a>, <a href="/search/astro-ph?searchtype=author&query=Cikota%2C+A">A. Cikota</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+D">D. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+S">S. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">T. de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">A. Do</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.14474v1-abstract-short" style="display: inline;"> We present JWST spectral and photometric observations of the Type IIP supernova (SN) 2022acko at ~50 days past explosion. These data are the first JWST spectral observations of a core-collapse SN. We identify ~30 different H I features, other features associated with products produced from the CNO cycle, and s-process elements such as Sc II and Ba II. By combining the JWST spectra with ground-base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14474v1-abstract-full').style.display = 'inline'; document.getElementById('2401.14474v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.14474v1-abstract-full" style="display: none;"> We present JWST spectral and photometric observations of the Type IIP supernova (SN) 2022acko at ~50 days past explosion. These data are the first JWST spectral observations of a core-collapse SN. We identify ~30 different H I features, other features associated with products produced from the CNO cycle, and s-process elements such as Sc II and Ba II. By combining the JWST spectra with ground-based optical and NIR spectra, we construct a full Spectral Energy Distribution from 0.4 to 25 microns and find that the JWST spectra are fully consistent with the simultaneous JWST photometry. The data lack signatures of CO formation and we estimate a limit on the CO mass of < 10^{-8} solar mass. We demonstrate how the CO fundamental band limits can be used to probe underlying physics during stellar evolution, explosion, and the environment. The observations indicate little mixing between the H envelope and C/O core in the ejecta and show no evidence of dust. The data presented here set a critical baseline for future JWST observations, where possible molecular and dust formation may be seen. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14474v1-abstract-full').style.display = 'none'; document.getElementById('2401.14474v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.13187">arXiv:2401.13187</a> <span> [<a href="https://arxiv.org/pdf/2401.13187">pdf</a>, <a href="https://arxiv.org/format/2401.13187">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad2e97">10.3847/2041-8213/ad2e97 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effects of type Ia supernovae absolute magnitude priors on the Hubble constant value </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yun Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Ratra%2C+B">Bharat Ratra</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="2401.13187v2-abstract-short" style="display: inline;"> We systematically explore the influence of the prior of the peak absolute magnitude ($M$) of type Ia supernovae (SNe Ia) on the measurement of the Hubble constant ($H_0$) from SNe Ia observations. We consider five different data-motivated $M$ priors, representing varying levels of dispersion, and assume the spatially-flat $螞$CDM cosmological model. Different $M$ priors lead to relative changes in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13187v2-abstract-full').style.display = 'inline'; document.getElementById('2401.13187v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13187v2-abstract-full" style="display: none;"> We systematically explore the influence of the prior of the peak absolute magnitude ($M$) of type Ia supernovae (SNe Ia) on the measurement of the Hubble constant ($H_0$) from SNe Ia observations. We consider five different data-motivated $M$ priors, representing varying levels of dispersion, and assume the spatially-flat $螞$CDM cosmological model. Different $M$ priors lead to relative changes in the mean values of $H_0$ from 2% to 7%. Loose priors on $M$ yield $H_0$ estimates consistent with both the Planck 2018 result and the SH0ES result at the 68% confidence level. We also examine the potential impact of peculiar velocity subtraction on the value of $H_0$, and show that it is insignificant for the SNe Ia observations with redshift $z > 0.01$ used in our analyses. We also repeat the analysis in the cosmography model and find very similar results. This suggests that our results are robust and model independent. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13187v2-abstract-full').style.display = 'none'; document.getElementById('2401.13187v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 1 figure, 1 table; Accepted for Publication in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 2024, 964, L4 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.10976">arXiv:2401.10976</a> <span> [<a href="https://arxiv.org/pdf/2401.10976">pdf</a>, <a href="https://arxiv.org/format/2401.10976">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 - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> An Effective Cosmological Collider </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Craig%2C+N">Nathaniel Craig</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=McCune%2C+A">Amara McCune</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.10976v1-abstract-short" style="display: inline;"> Effective field theories (EFTs) of heavy particles coupled to the inflaton are rife with operator redundancies, frequently obscured by sensitivity to both boundary terms and field redefinitions. We initiate a systematic study of these redundancies by establishing a minimal operator basis for an archetypal example, the abelian gauge-Higgs-inflaton EFT. Working up to dimension 9, we show that certai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.10976v1-abstract-full').style.display = 'inline'; document.getElementById('2401.10976v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.10976v1-abstract-full" style="display: none;"> Effective field theories (EFTs) of heavy particles coupled to the inflaton are rife with operator redundancies, frequently obscured by sensitivity to both boundary terms and field redefinitions. We initiate a systematic study of these redundancies by establishing a minimal operator basis for an archetypal example, the abelian gauge-Higgs-inflaton EFT. Working up to dimension 9, we show that certain low-dimensional operators are entirely redundant and identify new non-redundant operators with potentially interesting cosmological collider signals. Our methods generalize straightforwardly to other EFTs of heavy particles coupled to the inflaton. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.10976v1-abstract-full').style.display = 'none'; document.getElementById('2401.10976v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 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/2401.08288">arXiv:2401.08288</a> <span> [<a href="https://arxiv.org/pdf/2401.08288">pdf</a>, <a href="https://arxiv.org/format/2401.08288">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/06/001">10.1088/1475-7516/2024/06/001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Finding origins of CMB anomalies in the inflationary quantum fluctuations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+K+S">K. Sravan Kumar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.08288v3-abstract-short" style="display: inline;"> In this paper, we present compelling evidence for the parity asymmetry (a discrete symmetry that is separate from isotropy) in the Cosmic Microwave Background (CMB) map, measured through two-point temperature correlations. This parity asymmetric CMB challenges our understanding of the quantum physics of the early Universe rather than LCDM ($螞$ Cold-Dark-Matter). We commence by conducting a compreh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08288v3-abstract-full').style.display = 'inline'; document.getElementById('2401.08288v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.08288v3-abstract-full" style="display: none;"> In this paper, we present compelling evidence for the parity asymmetry (a discrete symmetry that is separate from isotropy) in the Cosmic Microwave Background (CMB) map, measured through two-point temperature correlations. This parity asymmetric CMB challenges our understanding of the quantum physics of the early Universe rather than LCDM ($螞$ Cold-Dark-Matter). We commence by conducting a comprehensive analysis of the Planck CMB, focusing on the distribution of power in low-multipoles and temperature anticorrelations at parity conjugate points in position space. We find tension with the near scale-invariant power-law power spectrum of Standard Inflation (SI), with p-values of the order $\mathcal{O}\left( 10^{-4}-10^{-3} \right)$. Alternatively, we explore the framework of direct-sum inflation (DSI), where a quantum fluctuation arises as a direct-sum of two components evolving forward and backward in time at parity conjugate points in physical space. We found that DSI is consistent with data on parity asymmetry, the absence of power at $胃>60^{\circ}$, and power suppression at low-even-multipoles, which are major data anomalies in the SI. Furthermore, we discover that the parameters characterizing the hemispherical power asymmetry anomaly become statistically insignificant when the large SI quadrupole amplitude is reduced to align with the data. DSI explains this low quadrupole with a p-value of $3.5\%$, 39 times higher than SI. Combining statistics from parameters measuring parity and low-$\ell$ angular power spectrum, we find that DSI is 50-650 times more probable than SI. In summary, our investigation suggests that CMB temperature fluctuations exhibit homogeneity and isotropy but parity-asymmetric consistent with predictions of DSI. This observation provides tantalizing evidence for the quantum mechanical nature of gravity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08288v3-abstract-full').style.display = 'none'; document.getElementById('2401.08288v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">63 pages, 22 figures, minor typos corrected. Matches with the version in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP06(2024)001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.05490">arXiv:2401.05490</a> <span> [<a href="https://arxiv.org/pdf/2401.05490">pdf</a>, <a href="https://arxiv.org/format/2401.05490">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Discovery and Follow-up of ASASSN-23bd (AT 2023clx): The Lowest Redshift and Least Luminous Tidal Disruption Event To Date </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hoogendam%2C+W+B">W. B. Hoogendam</a>, <a href="/search/astro-ph?searchtype=author&query=Hinkle%2C+J+T">J. T. Hinkle</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">K. Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Kochanek%2C+C+S">C. S. Kochanek</a>, <a href="/search/astro-ph?searchtype=author&query=Stanek%2C+K+Z">K. Z. Stanek</a>, <a href="/search/astro-ph?searchtype=author&query=Maksym%2C+W+P">W. P. Maksym</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">M. A. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M+E">M. E. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">N. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">C. R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Hey%2C+D">D. Hey</a>, <a href="/search/astro-ph?searchtype=author&query=Holoien%2C+T+W+-">T. W. -S. Holoien</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">J. L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M">M. Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">A. Do</a>, <a href="/search/astro-ph?searchtype=author&query=Polin%2C+A">A. Polin</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">P. J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J+M">J. M. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+L">L. Ferrari</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">S. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">J. Lu</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="2401.05490v1-abstract-short" style="display: inline;"> We report the All-Sky Automated Survey for SuperNovae discovery of the tidal disruption event (TDE) ASASSN-23bd (AT 2023clx) in NGC 3799, a LINER galaxy with no evidence of strong AGN activity over the past decade. With a redshift of $z = 0.01107$ and a peak UV/optical luminosity of $(5.4\pm0.4)\times10^{42}$ erg s$^{-1}$, ASASSN-23bd is the lowest-redshift and least-luminous TDE discovered to dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05490v1-abstract-full').style.display = 'inline'; document.getElementById('2401.05490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.05490v1-abstract-full" style="display: none;"> We report the All-Sky Automated Survey for SuperNovae discovery of the tidal disruption event (TDE) ASASSN-23bd (AT 2023clx) in NGC 3799, a LINER galaxy with no evidence of strong AGN activity over the past decade. With a redshift of $z = 0.01107$ and a peak UV/optical luminosity of $(5.4\pm0.4)\times10^{42}$ erg s$^{-1}$, ASASSN-23bd is the lowest-redshift and least-luminous TDE discovered to date. Spectroscopically, ASASSN-23bd shows H$伪$ and He I emission throughout its spectral time series, and the UV spectrum shows nitrogen lines without the strong carbon and magnesium lines typically seen for AGN. Fits to the rising ASAS-SN light curve show that ASASSN-23bd started to brighten on MJD 59988$^{+1}_{-1}$, $\sim$9 days before discovery, with a nearly linear rise in flux, peaking in the $g$ band on MJD $60000^{+3}_{-3}$. Scaling relations and TDE light curve modelling find a black hole mass of $\sim$10$^6$ $M_\odot$, which is on the lower end of supermassive black hole masses. ASASSN-23bd is a dim X-ray source, with an upper limit of $L_{0.3-10\,\mathrm{keV}} < 1.0\times10^{40}$ erg s$^{-1}$ from stacking all \emph{Swift} observations prior to MJD 60061, but with soft ($\sim 0.1$ keV) thermal emission with a luminosity of $L_{0.3-2 \,\mathrm{keV}}\sim4\times10^{39}$ erg s$^{-1}$ in \emph{XMM-Newton} observations on MJD 60095. The rapid $(t < 15$ days) light curve rise, low UV/optical luminosity, and a luminosity decline over 40 days of $螖L_{40}\approx-0.7$ make ASASSN-23bd one of the dimmest TDEs to date and a member of the growing ``Low Luminosity and Fast'' class of TDEs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05490v1-abstract-full').style.display = 'none'; document.getElementById('2401.05490v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 13 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08425">arXiv:2312.08425</a> <span> [<a href="https://arxiv.org/pdf/2312.08425">pdf</a>, <a href="https://arxiv.org/format/2312.08425">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 - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> The Cosmological Dynamics of String Theory Axion Strings </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Benabou%2C+J+N">Joshua N. Benabou</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+Q">Quentin Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Buschmann%2C+M">Malte Buschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Safdi%2C+B+R">Benjamin R. Safdi</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="2312.08425v1-abstract-short" style="display: inline;"> The quantum chromodynamics (QCD) axion may solve the strong CP problem and explain the dark matter (DM) abundance of our Universe. The axion was originally proposed to arise as the pseudo-Nambu Goldstone boson of global $\mathrm{U}(1)_{\rm PQ}$ Peccei-Quinn (PQ) symmetry breaking, but axions also arise generically in string theory as zero modes of higher-dimensional gauge fields. In this work we s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08425v1-abstract-full').style.display = 'inline'; document.getElementById('2312.08425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08425v1-abstract-full" style="display: none;"> The quantum chromodynamics (QCD) axion may solve the strong CP problem and explain the dark matter (DM) abundance of our Universe. The axion was originally proposed to arise as the pseudo-Nambu Goldstone boson of global $\mathrm{U}(1)_{\rm PQ}$ Peccei-Quinn (PQ) symmetry breaking, but axions also arise generically in string theory as zero modes of higher-dimensional gauge fields. In this work we show that string theory axions behave fundamentally differently from field theory axions in the early Universe. Field theory axions may form axion strings if the PQ phase transition takes place after inflation. In contrast, we show that string theory axions do not generically form axion strings. In special inflationary paradigms, such as D-brane inflation, string theory axion strings may form; however, their tension is parametrically larger than that of field theory axion strings. We then show that such QCD axion strings overproduce the DM abundance for all allowed QCD axion masses and are thus ruled out, except in scenarios with large warping. A loop-hole to this conclusion arises in the axiverse, where an axion string could be composed of multiple different axion mass eigenstates; a heavier eigenstate could collapse the network earlier, allowing for the QCD axion to produce the correct DM abundance and also generating observable gravitational wave signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08425v1-abstract-full').style.display = 'none'; document.getElementById('2312.08425v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 6 figures, video abstract at https://youtu.be/LnN9W9Vkxt4</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07774">arXiv:2312.07774</a> <span>  </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 contributions to the 38th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. 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=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Duerr%2C+A">A. Duerr</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+G+M">G. M. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">C. E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+J">J. Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">J. Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+Z">Z. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">T. B. Humensky</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+W">W. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+M+N">M. N. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kertzman%2C+M">M. Kertzman</a> , et al. (39 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.07774v1-abstract-short" style="display: inline;"> Compilation of papers presented by the VERITAS Collaboration at the 38th International Cosmic Ray Conference (ICRC), held July 26 through August 3, 2023 in Nagoya, Japan. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07774v1-abstract-full" style="display: none;"> Compilation of papers presented by the VERITAS Collaboration at the 38th International Cosmic Ray Conference (ICRC), held July 26 through August 3, 2023 in Nagoya, Japan. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07774v1-abstract-full').style.display = 'none'; document.getElementById('2312.07774v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">html page. ICRC 2023, Nagoya, Japan</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.16222">arXiv:2311.16222</a> <span> [<a href="https://arxiv.org/pdf/2311.16222">pdf</a>, <a href="https://arxiv.org/format/2311.16222">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> </div> </div> <p class="title is-5 mathjax"> Finite Bubble Statistics Constrain Late Cosmological Phase Transitions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Elor%2C+G">Gilly Elor</a>, <a href="/search/astro-ph?searchtype=author&query=Jinno%2C+R">Ryusuke Jinno</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Soubhik Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=McGehee%2C+R">Robert McGehee</a>, <a href="/search/astro-ph?searchtype=author&query=Tsai%2C+Y">Yuhsin Tsai</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="2311.16222v1-abstract-short" style="display: inline;"> We consider first order cosmological phase transitions (PT) happening at late times, below Standard Model (SM) temperatures $T_{\rm PT} \lesssim$ GeV. The inherently stochastic nature of bubble nucleation and the finite number of bubbles associated with a late-time PT lead to superhorizon fluctuations in the PT completion time. We compute how such fluctuations eventually source curvature fluctuati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16222v1-abstract-full').style.display = 'inline'; document.getElementById('2311.16222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.16222v1-abstract-full" style="display: none;"> We consider first order cosmological phase transitions (PT) happening at late times, below Standard Model (SM) temperatures $T_{\rm PT} \lesssim$ GeV. The inherently stochastic nature of bubble nucleation and the finite number of bubbles associated with a late-time PT lead to superhorizon fluctuations in the PT completion time. We compute how such fluctuations eventually source curvature fluctuations with universal properties, independent of the microphysics of the PT dynamics. Using Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) measurements, we constrain the energy released in a dark-sector PT. For 0.1 eV $\lesssim T_{\rm PT} \lesssim$ keV this constraint is stronger than both the current bound from additional neutrino species $螖N_{\rm eff}$, and in some cases, even CMB-S4 projections. Future measurements of CMB spectral distortions and pulsar timing arrays will also provide competitive sensitivity for keV $\lesssim T_{\rm PT} \lesssim$ GeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16222v1-abstract-full').style.display = 'none'; document.getElementById('2311.16222v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5+7 pages, 2+5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FTPI-MINN-23-20, UTWI-39-2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.10530">arXiv:2311.10530</a> <span> [<a href="https://arxiv.org/pdf/2311.10530">pdf</a>, <a href="https://arxiv.org/format/2311.10530">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/04/013">10.1088/1475-7516/2024/04/013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational bounds on extended minimal theories of massive gravity: New limits on the graviton mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Felice%2C+A">Antonio De Felice</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Mukohyama%2C+S">Shinji Mukohyama</a>, <a href="/search/astro-ph?searchtype=author&query=Nunes%2C+R+C">Rafael C. Nunes</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="2311.10530v1-abstract-short" style="display: inline;"> In this work, we derive for the first time observational constraints on the extended Minimal Theory of Massive Gravity (eMTMG) framework in light of Planck-CMB data, geometrical measurements from Baryon Acoustic Oscillation (BAO), Type Ia supernovae from the recent Pantheon+ samples, and also using the auto and cross-correlations cosmic shear measurements from KIDS-1000 survey. Given the great fre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10530v1-abstract-full').style.display = 'inline'; document.getElementById('2311.10530v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.10530v1-abstract-full" style="display: none;"> In this work, we derive for the first time observational constraints on the extended Minimal Theory of Massive Gravity (eMTMG) framework in light of Planck-CMB data, geometrical measurements from Baryon Acoustic Oscillation (BAO), Type Ia supernovae from the recent Pantheon+ samples, and also using the auto and cross-correlations cosmic shear measurements from KIDS-1000 survey. Given the great freedom of dynamics choice for the theory, we consider an observationally motivated subclass in which the background evolution of the Universe goes through a transition from a (positive or negative) value of the effective cosmological constant to another value. From the statistical point of view, we did not find evidence of such a transition, i.e. deviation from the standard $螞$CDM behavior, and from the joint analysis using Planck + BAO + Pantheon+ data, we constrain the graviton mass to $< 6.6 \times 10^{-34}$ eV at 95% CL. We use KIDS-1000 survey data to constrain the evolution of the scalar perturbations of the model and its limits for the growth of structure predicted by the eMTMG scenario. In this case, we find small evidence at 95% CL for a non-zero graviton mass. We interpret and discuss these results in light of the current tension on the $S_8$ parameter. We conclude that, within the subclass considered, the current data are only able to impose upper bounds on the eMTMG dynamics. Given its potentialities beyond the subclass, eMTMG can be classified as a good candidate for modified gravity, serving as a framework in which observational data can effectively constrain (or confirm) the graviton mass and deviations from the standard $螞$CDM behavior. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10530v1-abstract-full').style.display = 'none'; document.getElementById('2311.10530v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, uses REVTeX, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> YITP-23-144, IPMU23-0043 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP04(2024)013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.05983">arXiv:2311.05983</a> <span> [<a href="https://arxiv.org/pdf/2311.05983">pdf</a>, <a href="https://arxiv.org/format/2311.05983">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/04/001">10.1088/1475-7516/2024/04/001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects of detecting deviations to Kerr geometry with radiation reaction effects in EMRIs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chowdhuri%2C+A">Abhishek Chowdhuri</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+A">Arpan Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shailesh Kumar</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="2311.05983v2-abstract-short" style="display: inline;"> Direct detection of gravitational waves and binary black hole mergers have proven to be remarkable investigations of general relativity. In order to have a definitive answer as to whether the black hole spacetime under test is the Kerr or non-Kerr, one requires accurate mapping of the metric. Since EMRIs are perfect candidates for space-based detectors, Laser Interferometer Space Antenna (LISA) ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05983v2-abstract-full').style.display = 'inline'; document.getElementById('2311.05983v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.05983v2-abstract-full" style="display: none;"> Direct detection of gravitational waves and binary black hole mergers have proven to be remarkable investigations of general relativity. In order to have a definitive answer as to whether the black hole spacetime under test is the Kerr or non-Kerr, one requires accurate mapping of the metric. Since EMRIs are perfect candidates for space-based detectors, Laser Interferometer Space Antenna (LISA) observations will serve a crucial purpose in mapping the spacetime metric. In this article, we consider such a study with the Johannsen spacetime that captures the deviations from the Kerr black hole and further discuss their detection prospects. We analytically derive the leading order post-Newtonian corrections in the average loss of energy and angular momentum fluxes generated by a stellar-mass object exhibiting eccentric equatorial motion in the Johannsen background. We further obtain the orbital evolution of the inspiralling object within the adiabatic approximation and estimate the orbital phase. We lastly provide the possible detectability of deviations from the Kerr black hole by estimating gravitational wave dephasing and highlight the crucial role of LISA observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05983v2-abstract-full').style.display = 'none'; document.getElementById('2311.05983v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Improved PN analysis, comments in light of LIGO-VIRGO GWTC-3 observations are added, analysis regarding possible upper bounds on the deviation parameters from LISA observations is added, Version to appear in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 04 (2024) 001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04952">arXiv:2311.04952</a> <span> [<a href="https://arxiv.org/pdf/2311.04952">pdf</a>, <a href="https://arxiv.org/format/2311.04952">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The High Energy X-ray Probe (HEX-P): Supernova remnants, pulsar wind nebulae, and nuclear astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+S">Stephen Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+H">Hongjun An</a>, <a href="/search/astro-ph?searchtype=author&query=Abdelmaguid%2C+M">Moaz Abdelmaguid</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+J">Jason Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C+L">Chris L. Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/astro-ph?searchtype=author&query=Nynka%2C+M">Melania Nynka</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+J">Jaegeun Park</a>, <a href="/search/astro-ph?searchtype=author&query=Terada%2C+Y">Yukikatsu Terada</a>, <a href="/search/astro-ph?searchtype=author&query=Woo%2C+J">Jooyun Woo</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">Aya Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">Priyadarshini Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Diesing%2C+R">Rebecca Diesing</a>, <a href="/search/astro-ph?searchtype=author&query=Eagle%2C+J">Jordan Eagle</a>, <a href="/search/astro-ph?searchtype=author&query=Gabici%2C+S">Stefano Gabici</a>, <a href="/search/astro-ph?searchtype=author&query=Gelfand%2C+J">Joseph Gelfand</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">Javier Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chanho Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sajan Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Mac+Intyre%2C+B">Brydyn Mac Intyre</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K">Kristin Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Manconi%2C+S">Silvia Manconi</a>, <a href="/search/astro-ph?searchtype=author&query=Motogami%2C+Y">Yugo Motogami</a>, <a href="/search/astro-ph?searchtype=author&query=Ohsumi%2C+H">Hayato Ohsumi</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04952v1-abstract-short" style="display: inline;"> HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging ($<10"$ full width at half maximum) and broad spectral coverage (0.2--80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. HEX-P is ideally suited to address important p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04952v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04952v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04952v1-abstract-full" style="display: none;"> HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging ($<10"$ full width at half maximum) and broad spectral coverage (0.2--80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. HEX-P is ideally suited to address important problems in the physics and astrophysics of supernova remnants (SNRs) and pulsar-wind nebulae (PWNe). For shell SNRs, HEX-P can greatly improve our understanding via more accurate spectral characterization and localization of non-thermal X-ray emission from both non-thermal-dominated SNRs and those containing both thermal and non-thermal components, and can discover previously unknown non-thermal components in SNRs. Multi-epoch HEX-P observations of several young SNRs (e.g., Cas A and Tycho) are expected to detect year-scale variabilities of X-ray filaments and knots, thus enabling us to determine fundamental parameters related to diffusive shock acceleration, such as local magnetic field strengths and maximum electron energies. For PWNe, HEX-P will provide spatially-resolved, broadband X-ray spectral data separately from their pulsar emission, allowing us to study how particle acceleration, cooling, and propagation operate in different evolution stages of PWNe. HEX-P is also poised to make unique and significant contributions to nuclear astrophysics of Galactic radioactive sources by improving detections of, or limits on, $^{44}$Ti in the youngest SNRs and by potentially discovering rare nuclear lines as evidence of double neutron star mergers. Throughout the paper, we present simulations of each class of objects, demonstrating the power of both the imaging and spectral capabilities of HEX-P to advance our knowledge of SNRs, PWNe, and nuclear astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04952v1-abstract-full').style.display = 'none'; document.getElementById('2311.04952v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 15 figures; part of a suite of papers describing the HEX-P hard X-ray mission concept</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04851">arXiv:2311.04851</a> <span> [<a href="https://arxiv.org/pdf/2311.04851">pdf</a>, <a href="https://arxiv.org/format/2311.04851">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The High Energy X-ray Probe (HEX-P): Galactic PeVatrons, star clusters, superbubbles, microquasar jets, and gamma-ray binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+S">Stephen Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+H">Hongjun An</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">Aya Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/astro-ph?searchtype=author&query=Tsuji%2C+N">Naomi Tsuji</a>, <a href="/search/astro-ph?searchtype=author&query=Abdelmaguid%2C+M">Moaz Abdelmaguid</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+J">Jason Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">Priyadarshini Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">Silvia Celli</a>, <a href="/search/astro-ph?searchtype=author&query=Diesing%2C+R">Rebecca Diesing</a>, <a href="/search/astro-ph?searchtype=author&query=Eagle%2C+J">Jordan Eagle</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C+L">Chris L. Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Gabici%2C+S">Stefano Gabici</a>, <a href="/search/astro-ph?searchtype=author&query=Gelfand%2C+J">Joseph Gelfand</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">Javier Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chanho Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sajan Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsova%2C+E">Ekaterina Kuznetsova</a>, <a href="/search/astro-ph?searchtype=author&query=Mac+Intyre%2C+B">Brydyn Mac Intyre</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K">Kristin Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Manconi%2C+S">Silvia Manconi</a>, <a href="/search/astro-ph?searchtype=author&query=Motogami%2C+Y">Yugo Motogami</a>, <a href="/search/astro-ph?searchtype=author&query=Ohsumi%2C+H">Hayato Ohsumi</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="2311.04851v1-abstract-short" style="display: inline;"> HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging (<10" FWHM) and broad spectral coverage (0.2-80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. With the recent discoveries of over 40 ultra-high-energy gamma-ray sour… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04851v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04851v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04851v1-abstract-full" style="display: none;"> HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging (<10" FWHM) and broad spectral coverage (0.2-80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. With the recent discoveries of over 40 ultra-high-energy gamma-ray sources (detected above 100 TeV) and neutrino emission in the Galactic Plane, we have entered a new era of multi-messenger astrophysics facing the exciting reality of Galactic PeVatrons. In the next decade, as more Galactic PeVatrons and TeV gamma-ray sources are expected to be discovered, the identification of their acceleration and emission mechanisms will be the most pressing issue in both particle and high-energy astrophysics. In this paper, along with its companion papers (Reynolds et al. 2023, Mori et al. 2023), we will present that HEX-P is uniquely suited to address important problems in various cosmic-ray accelerators, including Galactic PeVatrons, through investigating synchrotron X-ray emission of TeV-PeV electrons produced by both leptonic and hadronic processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04851v1-abstract-full').style.display = 'none'; document.getElementById('2311.04851v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 12 figures, submitted to FrASS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03473">arXiv:2311.03473</a> <span> [<a href="https://arxiv.org/pdf/2311.03473">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad4702">10.3847/1538-4357/ad4702 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Type Ia Supernova Progenitor Properties and Their Host Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+S">Sudeshna Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Sadler%2C+B">Benjamin Sadler</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">Peter Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E">Eric Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">C. R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Diamond%2C+T">T. Diamond</a>, <a href="/search/astro-ph?searchtype=author&query=Dominguez%2C+I">I. Dominguez</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Uddin%2C+S+A">S. A. Uddin</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Krisciunas%2C+K">K. Krisciunas</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">S. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Mera%2C+T+B">T. B. Mera</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">N. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+M+C">M. C. Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M+D">M. D. Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+N">N. N. Suntzeff</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="2311.03473v3-abstract-short" style="display: inline;"> We present an eigenfunction method to analyze 161 visual light curves (LCs) of Type Ia supernovae (SNe Ia) obtained by the Carnegie Supernova Project to characterize their diversity and host-galaxy correlations. The eigenfunctions are based on the delayed-detonation scenario using three parameters: the LC stretch being determined by the amount of deflagration-burning governing the 56Ni production,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03473v3-abstract-full').style.display = 'inline'; document.getElementById('2311.03473v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03473v3-abstract-full" style="display: none;"> We present an eigenfunction method to analyze 161 visual light curves (LCs) of Type Ia supernovae (SNe Ia) obtained by the Carnegie Supernova Project to characterize their diversity and host-galaxy correlations. The eigenfunctions are based on the delayed-detonation scenario using three parameters: the LC stretch being determined by the amount of deflagration-burning governing the 56Ni production, the main-sequence mass M_MS of the progenitor white dwarf controlling the explosion energy, and its central density rho_c shifting the 56Ni distribution. Our analysis tool (SPAT) extracts the parameters from observations and projects them into physical space using their allowed ranges M_MS < 8 M_sun, rho_c < 7-8x10^9g/cc. The residuals between fits and individual LC-points are ~ 1-3% for ~ 92% of objects. We find two distinct M_MS groups corresponding to a fast (~ 40-65 Myrs) and a slow(~ 200-500 Myrs) stellar evolution. Most underluminous SNe Ia have hosts with low star formation but high M_MS, suggesting slow evolution times of the progenitor system. 91T-likes SNe show very similar LCs and high M_MS and are correlated to star formation regions, making them potentially important tracers of star formation in the early Universe out to z = 4-11. Some 6% outliers with `non-physical' parameters can be attributed to superluminous SNe Ia and subluminous SNe Ia with hosts of active star formation. For deciphering the SNe Ia diversity and high-precision SNe Ia cosmology, the importance is shown for LCs covering out to ~ 60 days past maximum. Finally, our method and results are discussed within the framework of multiple explosion scenarios, and in light of upcoming surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03473v3-abstract-full').style.display = 'none'; document.getElementById('2311.03473v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 22 figures, 6 tables in main text, 2 tables in appendix. This work has been published in the ApJ journal and is in partial fulfillment of the PhD thesis of the first author</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal (2024), Volume 969, Number 2, 80 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.02754">arXiv:2311.02754</a> <span> [<a href="https://arxiv.org/pdf/2311.02754">pdf</a>, <a href="https://arxiv.org/format/2311.02754">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Revisiting primordial black holes formation from preheating instabilities: the case of Starobinsky inflation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=del-Corral%2C+D">Daniel del-Corral</a>, <a href="/search/astro-ph?searchtype=author&query=Gondolo%2C+P">Paolo Gondolo</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+K+S">K. Sravan Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Marto%2C+J">Jo茫o Marto</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="2311.02754v2-abstract-short" style="display: inline;"> In recent years, the formation of primordial black holes (PBH) in the early universe inflationary cosmology has garnered significant attention. One plausible scenario for primordial black hole (PBH) formation arises during the preheating stage following inflation. Notably, this scenario does not necessitate any ad-hoc fine-tuning of the scalar field potential. This paper focuses on the growth of p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02754v2-abstract-full').style.display = 'inline'; document.getElementById('2311.02754v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.02754v2-abstract-full" style="display: none;"> In recent years, the formation of primordial black holes (PBH) in the early universe inflationary cosmology has garnered significant attention. One plausible scenario for primordial black hole (PBH) formation arises during the preheating stage following inflation. Notably, this scenario does not necessitate any ad-hoc fine-tuning of the scalar field potential. This paper focuses on the growth of primordial density perturbation and the consequent possibility of PBH formation in the preheating stage of the Starobinsky model for inflation. The typical mechanism for PBH formation during preheating is based on the collapse of primordial fluctuations that become super-horizon during inflation (type I) and re-enter the particle horizon in the different phases of cosmic expansion. In this work, we show that there exists a certain range of modes that remain in the sub-horizon (not exited) during inflation (type II modes) but evolve identically to type I modes if they fall into the instability band, leading to large density perturbation above the threshold and can potentially also contribute to the PBH formation. We detail the conditions determining the possible collapse of type I and/or type II modes whose wavelengths are larger than the Jeans length we derive from the effective sound speed of scalar field fluctuations. Since the preheating stage is an 'inflaton' (approximately) matter-dominated phase, we follow the framework of the critical collapse of fluctuations and compute the mass fraction using the well-known Press-Schechter and the Khlopov-Polnarev formalisms, and compare the two. Finally, we comment on the implications of our study for the investigations concerned with primordial accretion and consequent PBH contribution to the dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02754v2-abstract-full').style.display = 'none'; document.getElementById('2311.02754v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 18 figures, version with extended results and discussion</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09153">arXiv:2310.09153</a> <span> [<a href="https://arxiv.org/pdf/2310.09153">pdf</a>, <a href="https://arxiv.org/format/2310.09153">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> JWST MIRI/MRS Observations and Spectral Models of the Under-luminous Type Ia Supernova 2022xkq </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J+M">J. M. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">C. Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">P. Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">E. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Shahbandeh%2C+M">M. Shahbandeh</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+J">J. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Baade%2C+D">D. Baade</a>, <a href="/search/astro-ph?searchtype=author&query=Balangan%2C+E+F">E. F Balangan</a>, <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+K+A">K. A. Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">P. J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">C. R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Burrow%2C+A">A. Burrow</a>, <a href="/search/astro-ph?searchtype=author&query=Cikota%2C+A">A. Cikota</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">T. de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">A. Do</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Y. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Dominguez%2C+I">I. Dominguez</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+O">O. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+E+T">E. T. Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Janzen%2C+D">D. Janzen</a>, <a href="/search/astro-ph?searchtype=author&query=Jencson%2C+J+E">J. E. Jencson</a>, <a href="/search/astro-ph?searchtype=author&query=Krisciunas%2C+K">K. Krisciunas</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.09153v2-abstract-short" style="display: inline;"> We present a JWST mid-infrared spectrum of the under-luminous Type Ia Supernova (SN Ia) 2022xkq, obtained with the medium-resolution spectrometer on the Mid-Infrared Instrument (MIRI) $\sim130$ days post-explosion. We identify the first MIR lines beyond 14 $渭$m in SN Ia observations. We find features unique to under-luminous SNe Ia, including: isolated emission of stable Ni, strong blends of [Ti I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09153v2-abstract-full').style.display = 'inline'; document.getElementById('2310.09153v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09153v2-abstract-full" style="display: none;"> We present a JWST mid-infrared spectrum of the under-luminous Type Ia Supernova (SN Ia) 2022xkq, obtained with the medium-resolution spectrometer on the Mid-Infrared Instrument (MIRI) $\sim130$ days post-explosion. We identify the first MIR lines beyond 14 $渭$m in SN Ia observations. We find features unique to under-luminous SNe Ia, including: isolated emission of stable Ni, strong blends of [Ti II], and large ratios of singly ionized to doubly ionized species in both [Ar] and [Co]. Comparisons to normal-luminosity SNe Ia spectra at similar phases show a tentative trend between the width of the [Co III] 11.888 $渭$m feature and the SN light curve shape. Using non-LTE-multi-dimensional radiation hydro simulations and the observed electron capture elements we constrain the mass of the exploding white dwarf. The best-fitting model shows that SN 2022xkq is consistent with an off-center delayed-detonation explosion of a near-Chandrasekhar mass WD (M$_{\rm ej}$ $\approx 1.37$ M$_{\odot}$) of high-central density ($蟻_c \geq 2.0\times10^{9}$ g cm$^{-3}$) seen equator on, which produced M($^{56}$Ni) $= 0.324$ M$_{\odot}$ and M($^{58}$Ni) $\geq 0.06$ M$_{\odot}$. The observed line widths are consistent with the overall abundance distribution; and the narrow stable Ni lines indicate little to no mixing in the central regions, favoring central ignition of sub-sonic carbon burning followed by an off-center DDT beginning at a single point. Additional observations may further constrain the physics revealing the presence of additional species including Cr and Mn. Our work demonstrates the power of using the full coverage of MIRI in combination with detailed modeling to elucidate the physics of SNe Ia at a level not previously possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09153v2-abstract-full').style.display = 'none'; document.getElementById('2310.09153v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 18 figures, accepted to ApJ; updated to accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.04512">arXiv:2310.04512</a> <span> [<a href="https://arxiv.org/pdf/2310.04512">pdf</a>, <a href="https://arxiv.org/format/2310.04512">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 multi-wavelength investigation of PSR J2229+6114 and its pulsar wind nebula in the radio, X-ray, and gamma-ray bands </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pope%2C+I">I. Pope</a>, <a href="/search/astro-ph?searchtype=author&query=Mori%2C+K">K. Mori</a>, <a href="/search/astro-ph?searchtype=author&query=Abdelmaguid%2C+M">M. Abdelmaguid</a>, <a href="/search/astro-ph?searchtype=author&query=Gelfand%2C+J+D">J. D. Gelfand</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+S+P">S. P. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Safi-Harb%2C+S">S. Safi-Harb</a>, <a href="/search/astro-ph?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+H">H. An</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+V">VERITAS Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+G+M">G. M Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+G">G. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W+F">W. F Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.04512v1-abstract-short" style="display: inline;"> G106.3$+$2.7, commonly considered a composite supernova remnant (SNR), is characterized by a boomerang-shaped pulsar wind nebula (PWN) and two distinct ("head" & "tail") regions in the radio band. A discovery of very-high-energy (VHE) gamma-ray emission ($E_纬> 100$ GeV) followed by the recent detection of ultra-high-energy (UHE) gamma-ray emission ($E_纬> 100$ TeV) from the tail region suggests tha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04512v1-abstract-full').style.display = 'inline'; document.getElementById('2310.04512v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.04512v1-abstract-full" style="display: none;"> G106.3$+$2.7, commonly considered a composite supernova remnant (SNR), is characterized by a boomerang-shaped pulsar wind nebula (PWN) and two distinct ("head" & "tail") regions in the radio band. A discovery of very-high-energy (VHE) gamma-ray emission ($E_纬> 100$ GeV) followed by the recent detection of ultra-high-energy (UHE) gamma-ray emission ($E_纬> 100$ TeV) from the tail region suggests that G106.3$+$2.7 is a PeVatron candidate. We present a comprehensive multi-wavelength study of the Boomerang PWN (100" around PSR J2229+6114) using archival radio and Chandra data obtained from two decades ago, a new NuSTAR X-ray observation from 2020, and upper limits on gamma-ray fluxes obtained by Fermi and VERITAS observatories. The NuSTAR observation allowed us to detect a 51.67 ms spin period from the pulsar PSR J2229+6114 and the PWN emission characterized by a power-law model with $螕= 1.52\pm0.06$ up to 20 keV. Contrary to the previous radio study by Kothes et al. 2006, we prefer a much lower PWN B-field ($B\sim3$ $渭$G) and larger distance ($d \sim 8$ kpc) based on (1) the non-varying X-ray flux over the last two decades, (2) the energy-dependent X-ray PWN size resulting from synchrotron burn-off and (3) the multi-wavelength spectral energy distribution (SED) data. Our SED model suggests that the PWN is currently re-expanding after being compressed by the SNR reverse shock $\sim 1000$ years ago. In this case, the head region should be formed by GeV--TeV electrons injected earlier by the pulsar propagating into the low density environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04512v1-abstract-full').style.display = 'none'; document.getElementById('2310.04512v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.04335">arXiv:2310.04335</a> <span> [<a href="https://arxiv.org/pdf/2310.04335">pdf</a>, <a href="https://arxiv.org/format/2310.04335">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"> A detailed study of the polarisation convention of the Giant Metrewave Radio Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S+S">S. Suresh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Kudale%2C+S">Sanjay Kudale</a>, <a href="/search/astro-ph?searchtype=author&query=Kansabanik%2C+D">Devojyoti Kansabanik</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+B">Barnali Das</a>, <a href="/search/astro-ph?searchtype=author&query=Kharb%2C+P">Preeti Kharb</a>, <a href="/search/astro-ph?searchtype=author&query=Sasikumar%2C+S">Silpa Sasikumar</a>, <a href="/search/astro-ph?searchtype=author&query=Sebastian%2C+B">Biny Sebastian</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.04335v2-abstract-short" style="display: inline;"> Our work aims to investigate the polarisation convention of the Giant Metrewave Radio Telescope (GMRT) radio telescope and understand whether the telescope follows the standard IAU/IEEE convention. The GMRT antennas are prime focus antennas, i.e. the radiation falling on the antenna feed reverses its circular polarisation. If this reflection is not taken into account, it will result in a reversal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04335v2-abstract-full').style.display = 'inline'; document.getElementById('2310.04335v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.04335v2-abstract-full" style="display: none;"> Our work aims to investigate the polarisation convention of the Giant Metrewave Radio Telescope (GMRT) radio telescope and understand whether the telescope follows the standard IAU/IEEE convention. The GMRT antennas are prime focus antennas, i.e. the radiation falling on the antenna feed reverses its circular polarisation. If this reflection is not taken into account, it will result in a reversal of circular polarisation. We carried out several tests to understand the GMRT polarisation convention. The observations were carried out on several strong and highly polarised pulsars with known polarisation properties at GMRT wavelengths, mainly covering frequency bands 2, 3 and 4. In addition, we tracked the signal from the feed to the fibre optic system, and fibre optic system to the user end. We also tracked satellites of known polarisations as well as utilised right and left circularly polarised helical antennas to study the polarisation convention. Our study shows that the GMRT channels 1 and 2 are true R and L, however, GMRT being a prime focus instrument, the reflection due to the dish reverses the sense of polarisation and converts the right circular polarisation (RCP) into left circular polarisation (LCP) and vice versa. This has not been taken into account and thus the GMRT Stokes V and U signs need to be reversed to make them consistent with the IAU/IEEE convention. This objective can be achieved by reassigning channel 1 to L and channel 2 to R for all circular feeds, i.e. bands 2, 3, and 4. The study remains inconclusive for the GMRT band 5, which has linear feeds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04335v2-abstract-full').style.display = 'none'; document.getElementById('2310.04335v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">NCRA-TIFR Internal Technical Report</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.04023">arXiv:2310.04023</a> <span> [<a href="https://arxiv.org/pdf/2310.04023">pdf</a>, <a href="https://arxiv.org/format/2310.04023">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Rotation of a Stealth CME on 2012 October 5 Observed in the Inner Heliosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Sandeep Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Hegde%2C+D+V">Dinesha V. Hegde</a>, <a href="/search/astro-ph?searchtype=author&query=Srivastava%2C+N">Nandita Srivastava</a>, <a href="/search/astro-ph?searchtype=author&query=Pogorelov%2C+N+V">Nikolai V. Pogorelov</a>, <a href="/search/astro-ph?searchtype=author&query=Gopalswamy%2C+N">Nat Gopalswamy</a>, <a href="/search/astro-ph?searchtype=author&query=Yashiro%2C+S">Seiji Yashiro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.04023v1-abstract-short" style="display: inline;"> Coronal Mass Ejections (CMEs) are subject to changes in their direction of propagation, tilt, and other properties. This is because CMEs interact with the ambient solar wind and other large-scale magnetic field structures. In this work, we report on the observations of the 2012 October 5 stealth CME using coronagraphic and heliospheric images. We find clear evidence of a continuous rotation of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04023v1-abstract-full').style.display = 'inline'; document.getElementById('2310.04023v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.04023v1-abstract-full" style="display: none;"> Coronal Mass Ejections (CMEs) are subject to changes in their direction of propagation, tilt, and other properties. This is because CMEs interact with the ambient solar wind and other large-scale magnetic field structures. In this work, we report on the observations of the 2012 October 5 stealth CME using coronagraphic and heliospheric images. We find clear evidence of a continuous rotation of the CME, i.e., an increase in the tilt angle, estimated using the Graduated Cylindrical Shell (GCS) reconstruction at different heliocentric distances, up to 58 solar radii. We find a further increase in the tilt at L1 estimated from the toroidal and cylindrical flux rope fitting on the in situ observations of IMF and solar wind parameters. This study highlights the importance of observations of Heliospheric Imager (HI), onboard the Solar TErrestrial RElations Observatory (STEREO). In particular, the GCS reconstruction of CMEs in HI field-of-view promises to bridge the gap between the near-Sun and in-situ observations at the L1. The changes in the CME tilt has significant implications for the space weather impact of stealth CMEs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04023v1-abstract-full').style.display = 'none'; document.getElementById('2310.04023v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.10054">arXiv:2309.10054</a> <span> [<a href="https://arxiv.org/pdf/2309.10054">pdf</a>, <a href="https://arxiv.org/format/2309.10054">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+J">Jeniveve Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+D+J">David J. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Lundqvist%2C+P">Peter Lundqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">Llu铆s Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+J+E">Jennifer E. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+K+A">K. Azalee Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Yize Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+E">Emily Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Hosseinzadeh%2C+G">Griffin Hosseinzadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Janzen%2C+D">Daryl Janzen</a>, <a href="/search/astro-ph?searchtype=author&query=Jencson%2C+J+E">Jacob E. Jencson</a>, <a href="/search/astro-ph?searchtype=author&query=Lundquist%2C+M+J">Michael J. Lundquist</a>, <a href="/search/astro-ph?searchtype=author&query=Mehta%2C+D">Darshana Mehta</a>, <a href="/search/astro-ph?searchtype=author&query=Retamal%2C+N+M">Nicol谩s Meza Retamal</a>, <a href="/search/astro-ph?searchtype=author&query=Shrestha%2C+M">Manisha Shrestha</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+S">Stefano Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Wyatt%2C+S">Samuel Wyatt</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J+P">Joseph P. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">Chris Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+E">Eddie Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Blondin%2C+S">St茅phane Blondin</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">Christopher R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Y">Yongzhi Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Ting-Wan Chen</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.10054v2-abstract-short" style="display: inline;"> We present optical, infrared, ultraviolet, and radio observations of SN 2022xkq, an underluminous fast-declining type Ia supernova (SN Ia) in NGC 1784 ($\mathrm{D}\approx31$ Mpc), from $<1$ to 180 days after explosion. The high-cadence observations of SN 2022xkq, a photometrically transitional and spectroscopically 91bg-like SN Ia, cover the first days and weeks following explosion which are criti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10054v2-abstract-full').style.display = 'inline'; document.getElementById('2309.10054v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.10054v2-abstract-full" style="display: none;"> We present optical, infrared, ultraviolet, and radio observations of SN 2022xkq, an underluminous fast-declining type Ia supernova (SN Ia) in NGC 1784 ($\mathrm{D}\approx31$ Mpc), from $<1$ to 180 days after explosion. The high-cadence observations of SN 2022xkq, a photometrically transitional and spectroscopically 91bg-like SN Ia, cover the first days and weeks following explosion which are critical to distinguishing between explosion scenarios. The early light curve of SN 2022xkq has a red early color and exhibits a flux excess which is more prominent in redder bands; this is the first time such a feature has been seen in a transitional/91bg-like SN Ia. We also present 92 optical and 19 near-infrared (NIR) spectra, beginning 0.4 days after explosion in the optical and 2.6 days after explosion in the NIR. SN 2022xkq exhibits a long-lived C I 1.0693 $渭$m feature which persists until 5 days post-maximum. We also detect C II $位$6580 in the pre-maximum optical spectra. These lines are evidence for unburnt carbon that is difficult to reconcile with the double detonation of a sub-Chandrasekhar mass white dwarf. No existing explosion model can fully explain the photometric and spectroscopic dataset of SN 2022xkq, but the considerable breadth of the observations is ideal for furthering our understanding of the processes which produce faint SNe Ia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10054v2-abstract-full').style.display = 'none'; document.getElementById('2309.10054v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 16 figures, accepted for publication in ApJ, the figure 15 input models and synthetic spectra are now available at https://zenodo.org/record/8379254</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=Kumar%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Kumar%2C+S&start=150" class="pagination-link " aria-label="Page 4" 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