Science Organizing Committeeon behalf of Workshop Participants, :, George Helou, Ewine van Dishoeck, Jonas Zmuidzinas, Alberto Bolatto, Ilse Cleeves, Daniel Dale, Kentaro Motohara, Pat Roche, Linda Tacconi
This Report summarizes findings and recommendations from the Kavli-IAU workshop on "Probing the Universe from far-infrared to millimeter wavelengths: future facilities and their synergies" which took place from 26 to 28 March 2024 in Pasadena, CA, USA. The workshop aimed to define the needs and potential synergies for different facilities at wavelengths from 30 {mu}m to a few cm in the post-2030 era, considering both financial and programmatic limitations and exploring how to maximize the scientific insights from the data they will yield in the coming decades. This wavelength range provides unique probes of relatively cool, dense interstellar material central to studying the physics and chemistry of nascent stars, proton-planetary disks, and young forming exoplanets. On larger scales, these facilities probe dust and dense gas in galaxies and around highly obscured accreting supermassive black holes and are thus essential for characterizing feedback processes and galaxy evolution out to the highest redshifts. Solar system and time domain studies are also addressed. The main recommendations include the need for ALMA to develop an ALMA2040 vision; for ngVLA to maintain its momentum and schedule and further develop international partnerships; for far-IR astronomy to pursue a space-based observatory with urgency; and for large aperture, wide field millimeter/submillimeter telescopes to continue studies to mature science and technology.
{"title":"Report of the Kavli-IAU Workshop on Global Coordination, \"Probing the Universe from far-infrared to millimeter wavelengths: future facilities and their synergies\"","authors":"Science Organizing Committeeon behalf of Workshop Participants, :, George Helou, Ewine van Dishoeck, Jonas Zmuidzinas, Alberto Bolatto, Ilse Cleeves, Daniel Dale, Kentaro Motohara, Pat Roche, Linda Tacconi","doi":"arxiv-2409.07570","DOIUrl":"https://doi.org/arxiv-2409.07570","url":null,"abstract":"This Report summarizes findings and recommendations from the Kavli-IAU\u0000workshop on \"Probing the Universe from far-infrared to millimeter wavelengths:\u0000future facilities and their synergies\" which took place from 26 to 28 March\u00002024 in Pasadena, CA, USA. The workshop aimed to define the needs and potential\u0000synergies for different facilities at wavelengths from 30 {mu}m to a few cm in\u0000the post-2030 era, considering both financial and programmatic limitations and\u0000exploring how to maximize the scientific insights from the data they will yield\u0000in the coming decades. This wavelength range provides unique probes of relatively cool, dense\u0000interstellar material central to studying the physics and chemistry of nascent\u0000stars, proton-planetary disks, and young forming exoplanets. On larger scales,\u0000these facilities probe dust and dense gas in galaxies and around highly\u0000obscured accreting supermassive black holes and are thus essential for\u0000characterizing feedback processes and galaxy evolution out to the highest\u0000redshifts. Solar system and time domain studies are also addressed. The main recommendations include the need for ALMA to develop an ALMA2040\u0000vision; for ngVLA to maintain its momentum and schedule and further develop\u0000international partnerships; for far-IR astronomy to pursue a space-based\u0000observatory with urgency; and for large aperture, wide field\u0000millimeter/submillimeter telescopes to continue studies to mature science and\u0000technology.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217313","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Extending geodetic and astrometric Very Long Baseline Interferometry (VLBI) observations from traditional centimeter wavebands to millimeter wavebands offers numerous scientific potentials and benefits. However, it was considered quite challenging due to various factors, including the increased effects of atmospheric opacity and turbulence at millimeter wavelengths. Here, we present the results of the first geodetic-mode VLBI experiment, simultaneously observing 82 sources at 22/43/88/132 GHz (K/Q/W/D bands) using the Korean VLBI Network (KVN). We introduced the frequency phase transfer (FPT) method to geodetic VLBI analysis, an approach for calibrating atmospheric phase fluctuations at higher frequencies by transferring phase solutions from lower frequencies. With a 2-minute scan, FPT improved the signal-to-noise ratio (SNR) of most fringes, some by over 100%, thereby enhancing the detection rate of weak sources at millimeter wavebands. Additionally, FPT reduced systematic errors in group delay and delay rate, with the weighted root-mean-squares (WRMS) of the post-fitting residuals decreasing from 25.0 ps to 20.5 ps at the W band and from 39.3 ps to 27.6 ps at the D band. There were no notable differences observed in calibrating atmospheric phase fluctuations at the K band (WRMS = 12.4 ps) and Q band (WRMS = 11.8 ps) with the KVN baselines. This experiment demonstrated that the millimeter waveband can be used for geodetic and astrometric applications with high precision.
{"title":"A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz","authors":"Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang","doi":"arxiv-2409.07309","DOIUrl":"https://doi.org/arxiv-2409.07309","url":null,"abstract":"Extending geodetic and astrometric Very Long Baseline Interferometry (VLBI)\u0000observations from traditional centimeter wavebands to millimeter wavebands\u0000offers numerous scientific potentials and benefits. However, it was considered\u0000quite challenging due to various factors, including the increased effects of\u0000atmospheric opacity and turbulence at millimeter wavelengths. Here, we present\u0000the results of the first geodetic-mode VLBI experiment, simultaneously\u0000observing 82 sources at 22/43/88/132 GHz (K/Q/W/D bands) using the Korean VLBI\u0000Network (KVN). We introduced the frequency phase transfer (FPT) method to\u0000geodetic VLBI analysis, an approach for calibrating atmospheric phase\u0000fluctuations at higher frequencies by transferring phase solutions from lower\u0000frequencies. With a 2-minute scan, FPT improved the signal-to-noise ratio (SNR)\u0000of most fringes, some by over 100%, thereby enhancing the detection rate of\u0000weak sources at millimeter wavebands. Additionally, FPT reduced systematic\u0000errors in group delay and delay rate, with the weighted root-mean-squares\u0000(WRMS) of the post-fitting residuals decreasing from 25.0 ps to 20.5 ps at the\u0000W band and from 39.3 ps to 27.6 ps at the D band. There were no notable\u0000differences observed in calibrating atmospheric phase fluctuations at the K\u0000band (WRMS = 12.4 ps) and Q band (WRMS = 11.8 ps) with the KVN baselines. This\u0000experiment demonstrated that the millimeter waveband can be used for geodetic\u0000and astrometric applications with high precision.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217314","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, Mary N. Parenteau, Vincent Kofman
Telescope missions are currently being designed which will make direct imaging of habitable exoplanets possible in the near future, and studies are needed to quantify the detectability of biosignature features in the planet's reflectance spectrum. We simulated the detectability of a NIR-absorbing surface biosignature feature with simulated observations of the nearby exoplanet Proxima Centauri b. We modeled a biosignature spectral feature with a reflectance spectrum based on an anoxygenic photosynthetic bacterial species that has strong absorption at 1 um, which could make it well suited for life on an M-dwarf hosted planet. We modeled the distribution of this organism across the planet's surface based on climate states from a 3D General Circulation Model (GCM), which were Archean and Proterozoic-like exo-Earth analogues. We included the GCM runs' prognostically simulated water clouds and added organic haze into the Archean-like atmospheres. We simulated observations of these Proxima Centauri b scenarios with the LUVOIR-A and B telescope concepts, with LUVOIR-B serving as a proxy to the planned Habitable Worlds Observatory (HWO). We calculated integration times necessary to detect the biosignature, and found that it would be detectable on Proxima Centauri b if the organism is moderately abundant (greater than a 1-4% global surface area coverage), as long as the atmosphere is transmitting in the wavelength range under consideration. Small amounts of methane, clouds, and haze do not greatly impede detectability. We found preliminary evidence that such a biosignature would be detectable on exoplanets within 15 pc, but further investigations are needed to corroborate this.
目前正在设计的望远镜任务将在不久的将来实现对宜居系外行星的直接成像，因此需要对行星反射光谱中生物特征的可探测性进行量化研究。我们模拟了近红外吸收表面生物特征的可探测性，并对附近的系外行星半人马座比邻星b进行了模拟观测。我们模拟了一个生物特征光谱，其反射光谱是基于一种含氧光合细菌，该细菌在1微米处有很强的吸收能力，这可能使其非常适合在M矮星寄居的行星上生存。我们根据三维大气环流模型（GCM）的气候状态，模拟了这种生物在行星表面的分布，这些气候状态是类似于阿歇纪和新生代的外地球类似物。我们将 GCM 运行的预言模拟水云包括在内，并在类阿歇安大气中添加了有机霾。我们计算了探测生物特征所需的积分时间，发现只要大气层在所考虑的波长范围内透射，如果生物适度丰富（大于全球表面积的1-4%），就能在比邻星b上探测到生物特征。少量的甲烷、云层和雾霾不会严重影响探测能力。我们发现有初步证据表明，在 15 pc 范围内的系外行星上可以探测到这种生物特征，但还需要进一步的研究来证实这一点。
{"title":"Detectability Simulations of a NIR Surface Biosignature on Proxima Centauri b with Future Space Observatories","authors":"Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, Mary N. Parenteau, Vincent Kofman","doi":"arxiv-2409.07289","DOIUrl":"https://doi.org/arxiv-2409.07289","url":null,"abstract":"Telescope missions are currently being designed which will make direct\u0000imaging of habitable exoplanets possible in the near future, and studies are\u0000needed to quantify the detectability of biosignature features in the planet's\u0000reflectance spectrum. We simulated the detectability of a NIR-absorbing surface\u0000biosignature feature with simulated observations of the nearby exoplanet\u0000Proxima Centauri b. We modeled a biosignature spectral feature with a\u0000reflectance spectrum based on an anoxygenic photosynthetic bacterial species\u0000that has strong absorption at 1 um, which could make it well suited for life on\u0000an M-dwarf hosted planet. We modeled the distribution of this organism across\u0000the planet's surface based on climate states from a 3D General Circulation\u0000Model (GCM), which were Archean and Proterozoic-like exo-Earth analogues. We\u0000included the GCM runs' prognostically simulated water clouds and added organic\u0000haze into the Archean-like atmospheres. We simulated observations of these\u0000Proxima Centauri b scenarios with the LUVOIR-A and B telescope concepts, with\u0000LUVOIR-B serving as a proxy to the planned Habitable Worlds Observatory (HWO).\u0000We calculated integration times necessary to detect the biosignature, and found\u0000that it would be detectable on Proxima Centauri b if the organism is moderately\u0000abundant (greater than a 1-4% global surface area coverage), as long as the\u0000atmosphere is transmitting in the wavelength range under consideration. Small\u0000amounts of methane, clouds, and haze do not greatly impede detectability. We\u0000found preliminary evidence that such a biosignature would be detectable on\u0000exoplanets within 15 pc, but further investigations are needed to corroborate\u0000this.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217337","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Victoria Bollo, Martin Zwaan, Celine Peroux, Aleksandra Hamanowicz, Jianhang Chen, Simon Weng, Rob J. Ivison, Andrew Biggs
The ALMACAL survey is based on a database of reprocessed ALMA calibration scans suitable for scientific analysis, observed as part of regular PI observations. We present all the data accumulated from the start of ALMA operations until May 2022 for 1047 calibrator fields across the southern sky spanning ALMA Bands 3 to 10 (~ 84 - 950 GHz), so-called ALMACAL-22. Encompassing over 1000 square arcmin and accumulating over 2000 hours of integration time, ALMACAL is not only one of the largest ALMA surveys to date, but it continues to grow with each new scientific observation. We outline the methods for processing and imaging a subset of the highest-quality data ('pruned sample'). Using deconvolution techniques within the visibility data (uv plane), we created data cubes as the final product for further scientific analysis. We describe the properties and shortcomings of ALMACAL and compare its area and sensitivity with other sub-millimetre surveys. Notably, ALMACAL overcomes limitations of previous sub-millimetre surveys, such as small sky coverage and the effects of cosmic variance. Moreover, we discuss the improvements introduced by the latest version of this dataset that will enhance our understanding of dusty star-forming galaxies, extragalactic absorption lines, active galactic nucleus physics, and ultimately the evolution of molecular gas.
ALMACAL 勘测基于一个适合科学分析的 ALMA 校准扫描再处理数据库，该数据库是定期 PI 观测的一部分。我们展示了从 ALMA 开始运行到 2022 年 5 月期间积累的所有数据，这些数据来自横跨 ALMA 频段 3 到 10（~ 84 - 950 GHz）的南部天空的 1047 个定标场，即 ALMACAL-22。ALMACAL 不仅是迄今为止最大的 ALMA 勘测之一，而且随着每一次新的科学观测而持续增长。我们概述了处理最高质量数据子集（"剪枝样本"）并对其成像的方法。利用可见度数据（紫外平面）的解卷积技术，我们创建了数据立方体，作为进一步科学分析的最终产品。我们描述了 ALMACAL 的特性和不足，并将其面积和灵敏度与其他亚毫米巡天进行了比较。值得注意的是，ALMACAL 克服了以往亚毫米巡天的局限性，如天空覆盖范围小和宇宙方差的影响。此外，我们还讨论了该数据集最新版本所带来的改进，这些改进将增强我们对尘埃星形成星系、银河系外吸收线、活动星系核物理学以及最终对分子气体演化的理解。
{"title":"ALMACAL XII. Data characterisation and products","authors":"Victoria Bollo, Martin Zwaan, Celine Peroux, Aleksandra Hamanowicz, Jianhang Chen, Simon Weng, Rob J. Ivison, Andrew Biggs","doi":"arxiv-2409.07166","DOIUrl":"https://doi.org/arxiv-2409.07166","url":null,"abstract":"The ALMACAL survey is based on a database of reprocessed ALMA calibration\u0000scans suitable for scientific analysis, observed as part of regular PI\u0000observations. We present all the data accumulated from the start of ALMA\u0000operations until May 2022 for 1047 calibrator fields across the southern sky\u0000spanning ALMA Bands 3 to 10 (~ 84 - 950 GHz), so-called ALMACAL-22.\u0000Encompassing over 1000 square arcmin and accumulating over 2000 hours of\u0000integration time, ALMACAL is not only one of the largest ALMA surveys to date,\u0000but it continues to grow with each new scientific observation. We outline the\u0000methods for processing and imaging a subset of the highest-quality data\u0000('pruned sample'). Using deconvolution techniques within the visibility data\u0000(uv plane), we created data cubes as the final product for further scientific\u0000analysis. We describe the properties and shortcomings of ALMACAL and compare\u0000its area and sensitivity with other sub-millimetre surveys. Notably, ALMACAL\u0000overcomes limitations of previous sub-millimetre surveys, such as small sky\u0000coverage and the effects of cosmic variance. Moreover, we discuss the\u0000improvements introduced by the latest version of this dataset that will enhance\u0000our understanding of dusty star-forming galaxies, extragalactic absorption\u0000lines, active galactic nucleus physics, and ultimately the evolution of\u0000molecular gas.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217343","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ismael Mendoza, Andrii Torchylo, Thomas Sainrat, Axel Guinot, Alexandre Boucaud, Maxime Paillasa, Camille Avestruz, Prakruth Adari, Eric Aubourg, Biswajit Biswas, James Buchanan, Patricia Burchat, Cyrille Doux, Remy Joseph, Sowmya Kamath, Alex I. Malz, Grant Merz, Hironao Miyatake, Cécile Roucelle, Tianqing Zhang, the LSST Dark Energy Science Collaboration
We present an open source Python library for simulating overlapping (i.e., blended) images of galaxies and performing self-consistent comparisons of detection and deblending algorithms based on a suite of metrics. The package, named Blending Toolkit (BTK), serves as a modular, flexible, easy-to-install, and simple-to-use interface for exploring and analyzing systematic effects related to blended galaxies in cosmological surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time (LSST). BTK has three main components: (1) a set of modules that perform fast image simulations of blended galaxies, using the open source image simulation package GalSim; (2) a module that standardizes the inputs and outputs of existing deblending algorithms; (3) a library of deblending metrics commonly defined in the galaxy deblending literature. In combination, these modules allow researchers to explore the impacts of galaxy blending in cosmological surveys. Additionally, BTK provides researchers who are developing a new deblending algorithm a framework to evaluate algorithm performance and make principled comparisons with existing deblenders. BTK includes a suite of tutorials and comprehensive documentation. The source code is publicly available on GitHub at https://github.com/LSSTDESC/BlendingToolKit.
{"title":"The Blending ToolKit: A simulation framework for evaluation of galaxy detection and deblending","authors":"Ismael Mendoza, Andrii Torchylo, Thomas Sainrat, Axel Guinot, Alexandre Boucaud, Maxime Paillasa, Camille Avestruz, Prakruth Adari, Eric Aubourg, Biswajit Biswas, James Buchanan, Patricia Burchat, Cyrille Doux, Remy Joseph, Sowmya Kamath, Alex I. Malz, Grant Merz, Hironao Miyatake, Cécile Roucelle, Tianqing Zhang, the LSST Dark Energy Science Collaboration","doi":"arxiv-2409.06986","DOIUrl":"https://doi.org/arxiv-2409.06986","url":null,"abstract":"We present an open source Python library for simulating overlapping (i.e.,\u0000blended) images of galaxies and performing self-consistent comparisons of\u0000detection and deblending algorithms based on a suite of metrics. The package,\u0000named Blending Toolkit (BTK), serves as a modular, flexible, easy-to-install,\u0000and simple-to-use interface for exploring and analyzing systematic effects\u0000related to blended galaxies in cosmological surveys such as the Vera Rubin\u0000Observatory Legacy Survey of Space and Time (LSST). BTK has three main\u0000components: (1) a set of modules that perform fast image simulations of blended\u0000galaxies, using the open source image simulation package GalSim; (2) a module\u0000that standardizes the inputs and outputs of existing deblending algorithms; (3)\u0000a library of deblending metrics commonly defined in the galaxy deblending\u0000literature. In combination, these modules allow researchers to explore the\u0000impacts of galaxy blending in cosmological surveys. Additionally, BTK provides\u0000researchers who are developing a new deblending algorithm a framework to\u0000evaluate algorithm performance and make principled comparisons with existing\u0000deblenders. BTK includes a suite of tutorials and comprehensive documentation.\u0000The source code is publicly available on GitHub at\u0000https://github.com/LSSTDESC/BlendingToolKit.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"59 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217518","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pawan Girifor the ARA Collaboration, Ilya Kravchenkofor the ARA Collaboration, Patrick Allisonfor the ARA Collaboration, Amy L. Connollyfor the ARA Collaboration
The Askaryan Radio Array (ARA) experiment aims to detect ultra-high-energy cosmic neutrinos (>10 PeV) using radio detection techniques. To enhance ARA's capabilities, a new RFSoC-based DAQ, ARA-Next, is in the early stages of development. This advanced system will facilitate the creation of sophisticated triggers, including a novel multi-trigger approach, similar to those used in collider experiments. Our approach involves crafting and implementing innovative triggers for ARA's new DAQ, such as identifying double pulses from potential in-ice neutrino interactions, utilizing templates for atmospheric cosmic ray signals, optimizing triggers for astrophysical neutrino sources, correlating special events between ARA and IceCube, and discerning anthropogenic events using directional information. These trigger designs aim to lower thresholds and enhance ARA's detector sensitivity. Overall, this upgrade will not only enhance ARA's capabilities but also contribute to the technological advancements necessary for future experiments of this nature.
阿斯卡良射电阵列（ARA）实验旨在利用射电探测技术探测超高能中微子（>10 PeV）。为了增强 ARA 的能力，一种基于 RFSoC 的新型 DAQ ARA-Next 正在早期开发阶段。这个先进的系统将有助于创建复杂的触发器，包括一种新颖的多触发方法，类似于在对撞机实验中使用的方法。我们的方法包括为 ARA 的新 DAQ 设计和实施创新触发器，例如识别来自潜在冰内中微子相互作用的双脉冲、利用大气宇宙射线信号模板、优化天体物理中微子源触发器、关联 ARA 和冰立方之间的特殊事件，以及利用方向信息辨别人类活动事件。这些触发器设计旨在降低阈值并提高 ARA 探测器的灵敏度。总之，这次升级不仅将增强 ARA 的能力，而且还将促进未来此类实验所需的技术进步。
{"title":"ARA-Next: a new DAQ and trigger architecture for the Askaryan Radio Array","authors":"Pawan Girifor the ARA Collaboration, Ilya Kravchenkofor the ARA Collaboration, Patrick Allisonfor the ARA Collaboration, Amy L. Connollyfor the ARA Collaboration","doi":"arxiv-2409.07634","DOIUrl":"https://doi.org/arxiv-2409.07634","url":null,"abstract":"The Askaryan Radio Array (ARA) experiment aims to detect ultra-high-energy\u0000cosmic neutrinos (>10 PeV) using radio detection techniques. To enhance ARA's\u0000capabilities, a new RFSoC-based DAQ, ARA-Next, is in the early stages of\u0000development. This advanced system will facilitate the creation of sophisticated\u0000triggers, including a novel multi-trigger approach, similar to those used in\u0000collider experiments. Our approach involves crafting and implementing\u0000innovative triggers for ARA's new DAQ, such as identifying double pulses from\u0000potential in-ice neutrino interactions, utilizing templates for atmospheric\u0000cosmic ray signals, optimizing triggers for astrophysical neutrino sources,\u0000correlating special events between ARA and IceCube, and discerning\u0000anthropogenic events using directional information. These trigger designs aim\u0000to lower thresholds and enhance ARA's detector sensitivity. Overall, this\u0000upgrade will not only enhance ARA's capabilities but also contribute to the\u0000technological advancements necessary for future experiments of this nature.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"43 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217312","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Vievard Sébastien, Lallement Manon, Leon-Saval Sergio, Guyon Olivier, Jovanovic Nemanja, Huby Elsa, Lacour Sylvestre, Lozi Julien, Deo Vincent, Ahn Kyohoon, Lucas Miles, Sallum Steph, Norris Barnaby, Betters Chris, Amezcua-Correa Rodrygo, Yerolatsitis Stephanos, Fitzgerald Michael, Lin Jon, Kim Yoo Jung, Gatkine Pradip, Kotani Takayuki, Tamura Motohide, Currie Thayne, Kenchington Harry-Dean, Martin Guillermo, Perrin Guy
Photonic lanterns are waveguide devices enabling high throughput single mode spectroscopy and high angular resolution. We aim to present the first on-sky demonstration of a photonic lantern (PL) operating in visible light, to measure its throughput and assess its potential for high-resolution spectroscopy of compact objects. We used the SCExAO instrument (a double stage extreme AO system installed at the Subaru telescope) and FIRST mid-resolution spectrograph (R 3000) to test the visible capabilities of the PL on internal source and on-sky observations. The best averaged coupling efficiency over the PL field of view was measured at 51% +/- 10% with a peak at 80%. We also investigate the relationship between coupling efficiency and the Strehl ratio for a PL, comparing them with those of a single-mode fiber (SMF). Findings show that in the AO regime, a PL offers better coupling efficiency performance than a SMF, especially in the presence of low spatial frequency aberrations. We observed Ikiiki (alpha Leo - mR = 1.37) and `Aua (alpha Ori - mR = -1.17) at a frame rate of 200 Hz. Under median seeing conditions (about 1 arcsec measured in H band) and large tip/tilt residuals (over 20 mas), we estimated an average light coupling efficiency of 14.5% +/- 7.4%, with a maximum of 42.8% at 680 nm. We were able to reconstruct both star's spectra, containing various absorption lines. The successful demonstration of this device opens new possibilities in terms of high throughput single-mode fiber-fed spectroscopy in the Visible. The demonstrated on-sky coupling efficiency performance would not have been achievable with a single SMF injection setup under similar conditions, partly because the residual tip/tilt alone exceeded the field of view of a visible SMF (18 mas at 700 nm). Thus emphasizing the enhanced resilience of PL technology to such atmospheric disturbances. The additional
{"title":"Spectroscopy using a visible photonic lantern at the Subaru telescope: Laboratory characterization and first on-sky demonstration on Ikiiki (α Leo) and `Aua (α Ori)","authors":"Vievard Sébastien, Lallement Manon, Leon-Saval Sergio, Guyon Olivier, Jovanovic Nemanja, Huby Elsa, Lacour Sylvestre, Lozi Julien, Deo Vincent, Ahn Kyohoon, Lucas Miles, Sallum Steph, Norris Barnaby, Betters Chris, Amezcua-Correa Rodrygo, Yerolatsitis Stephanos, Fitzgerald Michael, Lin Jon, Kim Yoo Jung, Gatkine Pradip, Kotani Takayuki, Tamura Motohide, Currie Thayne, Kenchington Harry-Dean, Martin Guillermo, Perrin Guy","doi":"arxiv-2409.06958","DOIUrl":"https://doi.org/arxiv-2409.06958","url":null,"abstract":"Photonic lanterns are waveguide devices enabling high throughput single mode\u0000spectroscopy and high angular resolution. We aim to present the first on-sky\u0000demonstration of a photonic lantern (PL) operating in visible light, to measure\u0000its throughput and assess its potential for high-resolution spectroscopy of\u0000compact objects. We used the SCExAO instrument (a double stage extreme AO\u0000system installed at the Subaru telescope) and FIRST mid-resolution spectrograph\u0000(R 3000) to test the visible capabilities of the PL on internal source and\u0000on-sky observations. The best averaged coupling efficiency over the PL field of\u0000view was measured at 51% +/- 10% with a peak at 80%. We also investigate the\u0000relationship between coupling efficiency and the Strehl ratio for a PL,\u0000comparing them with those of a single-mode fiber (SMF). Findings show that in\u0000the AO regime, a PL offers better coupling efficiency performance than a SMF,\u0000especially in the presence of low spatial frequency aberrations. We observed\u0000Ikiiki (alpha Leo - mR = 1.37) and `Aua (alpha Ori - mR = -1.17) at a frame\u0000rate of 200 Hz. Under median seeing conditions (about 1 arcsec measured in H\u0000band) and large tip/tilt residuals (over 20 mas), we estimated an average light\u0000coupling efficiency of 14.5% +/- 7.4%, with a maximum of 42.8% at 680 nm. We\u0000were able to reconstruct both star's spectra, containing various absorption\u0000lines. The successful demonstration of this device opens new possibilities in\u0000terms of high throughput single-mode fiber-fed spectroscopy in the Visible. The\u0000demonstrated on-sky coupling efficiency performance would not have been\u0000achievable with a single SMF injection setup under similar conditions, partly\u0000because the residual tip/tilt alone exceeded the field of view of a visible SMF\u0000(18 mas at 700 nm). Thus emphasizing the enhanced resilience of PL technology\u0000to such atmospheric disturbances. The additional","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"181 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217315","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Matteo Battisti, Johannes Eser, Angela Olinto, Giuseppe Osteria
The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) is a proposed dual-satellite mission to observe Ultra-High-Energy Cosmic Rays (UHECRs), increasing the statistics at the highest energies, and Very-High-Energy Neutrinos (VHENs), following multi-messenger alerts of astrophysical transient events throughout the universe such as gamma-ray bursts and gravitational wave events. POEMMA-Balloon with Radio (PBR) is a scaled-down version of the POEMMA design, adapted to be flown as a payload on one of NASA's sub-orbital Super Pressure Balloons (SPBs) circling over the Southern Ocean for up to 100 days after a launch from Wanaka, New Zealand. This overview will provide a summary of the mission with its science goals, the instruments, and the current status of PBR.
{"title":"POEMMA-Balloon with Radio: a balloon-born multi-messenger multi-detector observatory","authors":"Matteo Battisti, Johannes Eser, Angela Olinto, Giuseppe Osteria","doi":"arxiv-2409.06753","DOIUrl":"https://doi.org/arxiv-2409.06753","url":null,"abstract":"The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) is a proposed\u0000dual-satellite mission to observe Ultra-High-Energy Cosmic Rays (UHECRs),\u0000increasing the statistics at the highest energies, and Very-High-Energy\u0000Neutrinos (VHENs), following multi-messenger alerts of astrophysical transient\u0000events throughout the universe such as gamma-ray bursts and gravitational wave\u0000events. POEMMA-Balloon with Radio (PBR) is a scaled-down version of the POEMMA\u0000design, adapted to be flown as a payload on one of NASA's sub-orbital Super\u0000Pressure Balloons (SPBs) circling over the Southern Ocean for up to 100 days\u0000after a launch from Wanaka, New Zealand. This overview will provide a summary\u0000of the mission with its science goals, the instruments, and the current status\u0000of PBR.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"95 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
F. BufanoINAF-Osservatorio Astrofisico di Catania, Italy, C. BordiuINAF-Osservatorio Astrofisico di Catania, Italy, T. CecconelloINAF-Osservatorio Astrofisico di Catania, Italy, M. MunariINAF-Osservatorio Astrofisico di Catania, Italy, A. HopkinsSchool of Mathematical and Physical Sciences, Australia, A. IngallineraINAF-Osservatorio Astrofisico di Catania, Italy, P. LetoINAF-Osservatorio Astrofisico di Catania, Italy, S. LoruINAF-Osservatorio Astrofisico di Catania, Italy, S. RiggiINAF-Osservatorio Astrofisico di Catania, Italy, E. SciaccaINAF-Osservatorio Astrofisico di Catania, Italy, G. VizzariUniversita degli Studi di Milano-Bicocca, Italy, A. De MarcoInstitute of Space Sciences and Astronomy, Malta, C. S. BuemiINAF-Osservatorio Astrofisico di Catania, Italy, F. CavallaroINAF-Osservatorio Astrofisico di Catania, Italy, C. TrigilioINAF-Osservatorio Astrofisico di Catania, Italy, G. UmanaINAF-Osservatorio Astrofisico di Catania, Italy
Supernova remnants (SNRs) carry vast amounts of mechanical and radiative energy that heavily influence the structural, dynamical, and chemical evolution of galaxies. To this day, more than 300 SNRs have been discovered in the Milky Way, exhibiting a wide variety of observational features. However, existing classification schemes are mainly based on their radio morphology. In this work, we introduce a novel unsupervised deep learning pipeline to analyse a representative subsample of the Galactic SNR population ($sim$ 50% of the total) with the aim of finding a connection between their multi-wavelength features and their physical properties. The pipeline involves two stages: (1) a representation learning stage, consisting of a convolutional autoencoder that feeds on imagery from infrared and radio continuum surveys (WISE 22$mu$m, Hi-GAL 70 $mu$m and SMGPS 30 cm) and produces a compact representation in a lower-dimensionality latent space; and (2) a clustering stage that seeks meaningful clusters in the latent space that can be linked to the physical properties of the SNRs and their surroundings. Our results suggest that this approach, when combined with an intermediate uniform manifold approximation and projection (UMAP) reprojection of the autoencoded embeddings into a more clusterable manifold, enables us to find reliable clusters. Despite a large number of sources being classified as outliers, most clusters relate to the presence of distinctive features, such as the distribution of infrared emission, the presence of radio shells and pulsar wind nebulae, and the existence of dust filaments.
{"title":"Sifting the debris: Patterns in the SNR population with unsupervised ML methods","authors":"F. BufanoINAF-Osservatorio Astrofisico di Catania, Italy, C. BordiuINAF-Osservatorio Astrofisico di Catania, Italy, T. CecconelloINAF-Osservatorio Astrofisico di Catania, Italy, M. MunariINAF-Osservatorio Astrofisico di Catania, Italy, A. HopkinsSchool of Mathematical and Physical Sciences, Australia, A. IngallineraINAF-Osservatorio Astrofisico di Catania, Italy, P. LetoINAF-Osservatorio Astrofisico di Catania, Italy, S. LoruINAF-Osservatorio Astrofisico di Catania, Italy, S. RiggiINAF-Osservatorio Astrofisico di Catania, Italy, E. SciaccaINAF-Osservatorio Astrofisico di Catania, Italy, G. VizzariUniversita degli Studi di Milano-Bicocca, Italy, A. De MarcoInstitute of Space Sciences and Astronomy, Malta, C. S. BuemiINAF-Osservatorio Astrofisico di Catania, Italy, F. CavallaroINAF-Osservatorio Astrofisico di Catania, Italy, C. TrigilioINAF-Osservatorio Astrofisico di Catania, Italy, G. UmanaINAF-Osservatorio Astrofisico di Catania, Italy","doi":"arxiv-2409.06383","DOIUrl":"https://doi.org/arxiv-2409.06383","url":null,"abstract":"Supernova remnants (SNRs) carry vast amounts of mechanical and radiative\u0000energy that heavily influence the structural, dynamical, and chemical evolution\u0000of galaxies. To this day, more than 300 SNRs have been discovered in the Milky\u0000Way, exhibiting a wide variety of observational features. However, existing\u0000classification schemes are mainly based on their radio morphology. In this\u0000work, we introduce a novel unsupervised deep learning pipeline to analyse a\u0000representative subsample of the Galactic SNR population ($sim$ 50% of the\u0000total) with the aim of finding a connection between their multi-wavelength\u0000features and their physical properties. The pipeline involves two stages: (1) a\u0000representation learning stage, consisting of a convolutional autoencoder that\u0000feeds on imagery from infrared and radio continuum surveys (WISE 22$mu$m,\u0000Hi-GAL 70 $mu$m and SMGPS 30 cm) and produces a compact representation in a\u0000lower-dimensionality latent space; and (2) a clustering stage that seeks\u0000meaningful clusters in the latent space that can be linked to the physical\u0000properties of the SNRs and their surroundings. Our results suggest that this\u0000approach, when combined with an intermediate uniform manifold approximation and\u0000projection (UMAP) reprojection of the autoencoded embeddings into a more\u0000clusterable manifold, enables us to find reliable clusters. Despite a large\u0000number of sources being classified as outliers, most clusters relate to the\u0000presence of distinctive features, such as the distribution of infrared\u0000emission, the presence of radio shells and pulsar wind nebulae, and the\u0000existence of dust filaments.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217346","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Xikai Shan, Guoliang Li, Xuechun Chen, Wen Zhao, Bin Hu, Shude Mao
The gravitational lensing wave effect generated by a microlensing field embedded in a lens galaxy is an inevitable phenomenon in strong lensed gravitational waves (SLGWs). This effect presents both challenges and opportunities for the detection and application of SLGWs. However, investigating this wave effect requires computing a complete diffraction integral over each microlens in the field. This is extremely time-consuming due to the large number of microlenses. Therefore, simply adding all the microlenses is impractical. Additionally, the complexity of the time delay surface makes the lens plane resolution a crucial factor in controlling numerical errors. In this paper, we propose a trapezoid approximation-based adaptive hierarchical tree algorithm to meet the challenges of calculation speed and precision. We find that this algorithm accelerates the calculation by four orders of magnitude compared to the simple adding method and is one order of magnitude faster than the fixed hierarchical tree algorithm proposed for electromagnetic microlensing. More importantly, our algorithm ensures controllable numerical errors, increasing confidence in the results. Together with our previous work, this paper addresses all numerical issues, including integral convergence, precision, and computational time. Finally, we conducted a population study on the microlensing wave effect of SLGWs using this algorithm and found that the microlensing wave effect cannot be ignored, especially for Type II SLGWs due to their intrinsic geometric structures and their typical intersection with a denser microlensing field. Statistically, more than 33% (11%) of SLGWs have a mismatch larger than 1% (3%) compared to the unlensed waveform. Additionally, we found that the mismatch between signal pairs in a doubly imaged GW is generally larger than 10^{-3}, and 61% (25%) of signal pairs have a mismatch larger than 1% (3%).
{"title":"Wave effect of gravitational waves intersected with a microlens field II: an adaptive hierarchical tree algorithm and population study","authors":"Xikai Shan, Guoliang Li, Xuechun Chen, Wen Zhao, Bin Hu, Shude Mao","doi":"arxiv-2409.06747","DOIUrl":"https://doi.org/arxiv-2409.06747","url":null,"abstract":"The gravitational lensing wave effect generated by a microlensing field\u0000embedded in a lens galaxy is an inevitable phenomenon in strong lensed\u0000gravitational waves (SLGWs). This effect presents both challenges and\u0000opportunities for the detection and application of SLGWs. However,\u0000investigating this wave effect requires computing a complete diffraction\u0000integral over each microlens in the field. This is extremely time-consuming due\u0000to the large number of microlenses. Therefore, simply adding all the\u0000microlenses is impractical. Additionally, the complexity of the time delay\u0000surface makes the lens plane resolution a crucial factor in controlling\u0000numerical errors. In this paper, we propose a trapezoid approximation-based\u0000adaptive hierarchical tree algorithm to meet the challenges of calculation\u0000speed and precision. We find that this algorithm accelerates the calculation by\u0000four orders of magnitude compared to the simple adding method and is one order\u0000of magnitude faster than the fixed hierarchical tree algorithm proposed for\u0000electromagnetic microlensing. More importantly, our algorithm ensures\u0000controllable numerical errors, increasing confidence in the results. Together\u0000with our previous work, this paper addresses all numerical issues, including\u0000integral convergence, precision, and computational time. Finally, we conducted\u0000a population study on the microlensing wave effect of SLGWs using this\u0000algorithm and found that the microlensing wave effect cannot be ignored,\u0000especially for Type II SLGWs due to their intrinsic geometric structures and\u0000their typical intersection with a denser microlensing field. Statistically,\u0000more than 33% (11%) of SLGWs have a mismatch larger than 1% (3%) compared to\u0000the unlensed waveform. Additionally, we found that the mismatch between signal\u0000pairs in a doubly imaged GW is generally larger than 10^{-3}, and 61% (25%) of\u0000signal pairs have a mismatch larger than 1% (3%).","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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