Mona El Morsy, Thayne Currie, Masayuki Kuzuhara, Jeffrey Chilcote, Olivier Guyon, Taylor L. Tobin, Timothy Brandt, Qier An, Kyohoon Anh, Danielle Bovie, Vincent Deo, Tyler Groff, Ziying Gu, Markus Janson, Nemanja Jovanovic, Yiting Li, Kellen Lawson, Julien Lozi, Miles Lucas, Christian Marois, Naoshi Murakami, Eric Nielsen, Barnaby Norris, Nour Skaf, Motohide Tamura, William Thompson, Taichi Uyama, Sebastien Vievard
We describe the motivation, design, and early results for our 42-night, 125 star Subaru/SCExAO direct imaging survey for planets around accelerating stars. Unlike prior large surveys, ours focuses only on stars showing evidence for an astrometric acceleration plausibly due to the dynamical pull of an unseen planet or brown dwarf. Our program is motivated by results from a recent pilot program that found the first planet jointly discovered from direct imaging and astrometry and resulted in a planet and brown dwarf discovery rate substantially higher than previous unbiased surveys like GPIES. The first preliminary results from our program reveal multiple new companions; discovered planets and brown dwarfs can be further characterized with follow-up data, including higher-resolution spectra. Finally, we describe the critical role this program plays in supporting the Roman Space Telescope Coronagraphic Instrument, providing a currently-missing list of targets suitable for the CGI technological demonstration without which the CGI tech demo risks failure.
{"title":"Design, scientific goals, and performance of the SCExAO survey for planets around accelerating stars","authors":"Mona El Morsy, Thayne Currie, Masayuki Kuzuhara, Jeffrey Chilcote, Olivier Guyon, Taylor L. Tobin, Timothy Brandt, Qier An, Kyohoon Anh, Danielle Bovie, Vincent Deo, Tyler Groff, Ziying Gu, Markus Janson, Nemanja Jovanovic, Yiting Li, Kellen Lawson, Julien Lozi, Miles Lucas, Christian Marois, Naoshi Murakami, Eric Nielsen, Barnaby Norris, Nour Skaf, Motohide Tamura, William Thompson, Taichi Uyama, Sebastien Vievard","doi":"arxiv-2409.06773","DOIUrl":"https://doi.org/arxiv-2409.06773","url":null,"abstract":"We describe the motivation, design, and early results for our 42-night, 125\u0000star Subaru/SCExAO direct imaging survey for planets around accelerating stars.\u0000Unlike prior large surveys, ours focuses only on stars showing evidence for an\u0000astrometric acceleration plausibly due to the dynamical pull of an unseen\u0000planet or brown dwarf. Our program is motivated by results from a recent pilot\u0000program that found the first planet jointly discovered from direct imaging and\u0000astrometry and resulted in a planet and brown dwarf discovery rate\u0000substantially higher than previous unbiased surveys like GPIES. The first\u0000preliminary results from our program reveal multiple new companions; discovered\u0000planets and brown dwarfs can be further characterized with follow-up data,\u0000including higher-resolution spectra. Finally, we describe the critical role\u0000this program plays in supporting the Roman Space Telescope Coronagraphic\u0000Instrument, providing a currently-missing list of targets suitable for the CGI\u0000technological demonstration without which the CGI tech demo risks failure.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217338","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}
Dieder Van den Broeck, Uzair Abdul Latif, Stijn Buitink, Krijn de Vries, Tim Huege
An ongoing challenge for radio-based detectors of high-energy cosmic particles is the accurate description of radio signal propagation in natural non-uniform media. For radio signals originating from extensive air showers, the current state of the art simulations often implicitly assume straight-line signal propagation. This while the refraction due to a non-uniform atmosphere is expected to have an effect on the received signal and associated reconstruction that is currently not completely understood for the most inclined geometries. Here, we present a study regarding the validity of assuming straight-line signal propagation when simulating radio emission associated with very inclined air shower geometries. To this end, the calculation of the electric field based on the end-point formalism used in CoREAS was improved by use of tabulated ray tracing data. We find that including ray curvature effects into the end-point formalism calculation introduces changes of up to a few percent in fluence for frequencies up to 1.2 GHz and zenith angles up to 88{deg}.
{"title":"Validation of straight-line signal propagation for radio signal of very inclined cosmic ray air showers","authors":"Dieder Van den Broeck, Uzair Abdul Latif, Stijn Buitink, Krijn de Vries, Tim Huege","doi":"arxiv-2409.06388","DOIUrl":"https://doi.org/arxiv-2409.06388","url":null,"abstract":"An ongoing challenge for radio-based detectors of high-energy cosmic\u0000particles is the accurate description of radio signal propagation in natural\u0000non-uniform media. For radio signals originating from extensive air showers,\u0000the current state of the art simulations often implicitly assume straight-line\u0000signal propagation. This while the refraction due to a non-uniform atmosphere\u0000is expected to have an effect on the received signal and associated\u0000reconstruction that is currently not completely understood for the most\u0000inclined geometries. Here, we present a study regarding the validity of\u0000assuming straight-line signal propagation when simulating radio emission\u0000associated with very inclined air shower geometries. To this end, the\u0000calculation of the electric field based on the end-point formalism used in\u0000CoREAS was improved by use of tabulated ray tracing data. We find that\u0000including ray curvature effects into the end-point formalism calculation\u0000introduces changes of up to a few percent in fluence for frequencies up to 1.2\u0000GHz and zenith angles up to 88{deg}.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217344","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}
Benjamin Schwab, Adrian Zink, Davide Depaoli, Jim Hinton, Gang Liu, Akira Okumura, Duncan Ross, Johannes Schäfer, Harm Schoorlemmer, Hiro Tajima, Justin Vandenbroucke, Richard White, Jason John Watson, Justus Zorn, Stefan Funk
We have developed a new set of Application-Specific Integrated Circuits (ASICs) of the TARGET family (CTC and CT5TEA), designed for the readout of signals from photosensors in cameras of Imaging Atmospheric Cherenkov Telescopes (IACTs) for ground-based gamma-ray astronomy. We present the performance and design details. Both ASICs feature 16 channels, with CTC being a Switched-Capacitor Array (SCA) sampler at 0.5 to 1 GSa/s with a 16,384 sample deep storage buffer, including the functionality to digitize full waveforms at arbitrary times. CT5TEA is its companion trigger ASIC (though may be used on its own), which provides trigger information for the analog sum of four (and 16) adjacent channels. Since sampling and triggering takes place in two separate ASICs, the noise due to interference from the SCA is suppressed, and allows a minimal trigger threshold of $leq$ 2.5 mV (0.74 photo electrons (p.e.)) with a trigger noise of $leq$ 0.5 mV (0.15 p.e.). For CTC, a maximal input voltage range from $-$0.5 V up to 1.7 V is achieved with an effective bit range of $>$ 11.6 bits and a baseline noise of 0.7 mV. The cross-talk improved to $leq$ 1% over the whole $-$3 dB bandwidth of 220 MHz and even down to 0.2% for 1.5 V pulses of 10 ns width. Not only is the performance presented, but a temperature-stable calibration routine for pulse mode operation is introduced and validated. The resolution is found to be $sim$ 2.5% at 33.7 mV (10 p.e.) and $leq$ 0.3% at 337 mV (100 p.e.) with an integrated non-linearity of $<$ 1.6 mV. Developed for the Small-Sized Telescope (SST) and Schwarzschild-Couder Telescope (SCT) cameras of the Cherenkov Telescope Array Observatory (CTAO), CTC and CT5TEA are deployed for both prototypes and shall be integrated into the final versions.
{"title":"CTC and CT5TEA: an advanced multi-channel digitizer and trigger ASIC for imaging atmospheric Cherenkov telescopes","authors":"Benjamin Schwab, Adrian Zink, Davide Depaoli, Jim Hinton, Gang Liu, Akira Okumura, Duncan Ross, Johannes Schäfer, Harm Schoorlemmer, Hiro Tajima, Justin Vandenbroucke, Richard White, Jason John Watson, Justus Zorn, Stefan Funk","doi":"arxiv-2409.06435","DOIUrl":"https://doi.org/arxiv-2409.06435","url":null,"abstract":"We have developed a new set of Application-Specific Integrated Circuits\u0000(ASICs) of the TARGET family (CTC and CT5TEA), designed for the readout of\u0000signals from photosensors in cameras of Imaging Atmospheric Cherenkov\u0000Telescopes (IACTs) for ground-based gamma-ray astronomy. We present the\u0000performance and design details. Both ASICs feature 16 channels, with CTC being\u0000a Switched-Capacitor Array (SCA) sampler at 0.5 to 1 GSa/s with a 16,384 sample\u0000deep storage buffer, including the functionality to digitize full waveforms at\u0000arbitrary times. CT5TEA is its companion trigger ASIC (though may be used on\u0000its own), which provides trigger information for the analog sum of four (and\u000016) adjacent channels. Since sampling and triggering takes place in two\u0000separate ASICs, the noise due to interference from the SCA is suppressed, and\u0000allows a minimal trigger threshold of $leq$ 2.5 mV (0.74 photo electrons\u0000(p.e.)) with a trigger noise of $leq$ 0.5 mV (0.15 p.e.). For CTC, a maximal\u0000input voltage range from $-$0.5 V up to 1.7 V is achieved with an effective bit\u0000range of $>$ 11.6 bits and a baseline noise of 0.7 mV. The cross-talk improved\u0000to $leq$ 1% over the whole $-$3 dB bandwidth of 220 MHz and even down to 0.2%\u0000for 1.5 V pulses of 10 ns width. Not only is the performance presented, but a\u0000temperature-stable calibration routine for pulse mode operation is introduced\u0000and validated. The resolution is found to be $sim$ 2.5% at 33.7 mV (10 p.e.)\u0000and $leq$ 0.3% at 337 mV (100 p.e.) with an integrated non-linearity of $<$\u00001.6 mV. Developed for the Small-Sized Telescope (SST) and Schwarzschild-Couder\u0000Telescope (SCT) cameras of the Cherenkov Telescope Array Observatory (CTAO),\u0000CTC and CT5TEA are deployed for both prototypes and shall be integrated into\u0000the final versions.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"25 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217340","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}
Simon Dupourqué, Didier Barret, Camille M. Diez, Sébastien Guillot, Erwan Quintin
Context. Inferring spectral parameters from X-ray data is one of the cornerstones of high-energy astrophysics, and is achieved using software stacks that have been developed over the last twenty years and more. However, as models get more complex and spectra reach higher resolutions, these established software solutions become more feature-heavy, difficult to maintain and less efficient. Aims. We present jaxspec, a Python package for performing this task quickly and robustly in a fully Bayesian framework. Based on the JAX ecosystem, jaxspec allows the generation of differentiable likelihood functions compilable on core or graphical process units (resp. CPU and GPU), enabling the use of robust algorithms for Bayesian inference. Methods. We demonstrate the effectiveness of jaxspec samplers, in particular the No U-Turn Sampler, using a composite model and comparing what we obtain with the existing frameworks. We also demonstrate its ability to process high-resolution spectroscopy data and using original methods, by reproducing the results of the Hitomi collaboration on the Perseus cluster, while solving the inference problem using variational inference on a GPU. Results. We obtain identical results when compared to other softwares and approaches, meaning that jaxspec provides reliable results while being $sim 10$ times faster than existing alternatives. In addition, we show that variational inference can produce convincing results even on high-resolution data in less than 10 minutes on a GPU. Conclusions. With this package, we aim to pursue the goal of opening up X-ray spectroscopy to the existing ecosystem of machine learning and Bayesian inference, enabling researchers to apply new methods to solve increasingly complex problems in the best possible way. Our long-term ambition is the scientific exploitation of the data from the newAthena X-ray Integral Field Unit (X-IFU).
背景从 X 射线数据中推断光谱参数是高能天体物理学的基石之一，它是利用过去二十多年来开发的软件堆栈实现的。然而，随着模型越来越复杂，光谱分辨率越来越高，这些成熟的软件解决方案变得功能繁多、难以维护且效率低下。我们的目标我们介绍了 jaxspec，这是一个 Python 软件包，用于在完全贝叶斯框架内快速、稳健地完成这项任务。基于 JAX 生态系统，jaxspec 允许生成可在核心或图形处理单元（CPU 和 GPU）上编译的可微分似然函数，从而能够使用贝叶斯推断的稳健算法。方法。我们使用一个复合模型演示了 jaxspec 采样器的有效性，特别是 No U-Turn 采样器，并将我们获得的结果与现有框架进行了比较。我们还展示了它处理高分辨率光谱数据和使用原创方法的能力，重现了英仙座星团上 Hitomi 合作的结果，同时在 GPU 上使用变分推理解决了推理问题。结果。与其他软件和方法相比，我们获得了相同的结果，这意味着jaxspec在提供可靠结果的同时，速度比现有替代方法快10倍。此外，我们还证明了变分推理即使在高分辨率数据上也能产生令人信服的结果，而且在 GPU 上的时间还不到 10 分钟。结论。通过这个软件包，我们的目标是向现有的机器学习和贝叶斯推理生态系统开放 X 射线光谱学，使研究人员能够应用新方法以最佳方式解决日益复杂的问题。我们的长远目标是对新的雅典娜 X 射线积分场装置（X-IFU）的数据进行科学利用。
{"title":"jaxspec : a fast and robust Python library for X-ray spectral fitting","authors":"Simon Dupourqué, Didier Barret, Camille M. Diez, Sébastien Guillot, Erwan Quintin","doi":"arxiv-2409.05757","DOIUrl":"https://doi.org/arxiv-2409.05757","url":null,"abstract":"Context. Inferring spectral parameters from X-ray data is one of the\u0000cornerstones of high-energy astrophysics, and is achieved using software stacks\u0000that have been developed over the last twenty years and more. However, as\u0000models get more complex and spectra reach higher resolutions, these established\u0000software solutions become more feature-heavy, difficult to maintain and less\u0000efficient. Aims. We present jaxspec, a Python package for performing this task\u0000quickly and robustly in a fully Bayesian framework. Based on the JAX ecosystem,\u0000jaxspec allows the generation of differentiable likelihood functions compilable\u0000on core or graphical process units (resp. CPU and GPU), enabling the use of\u0000robust algorithms for Bayesian inference. Methods. We demonstrate the\u0000effectiveness of jaxspec samplers, in particular the No U-Turn Sampler, using a\u0000composite model and comparing what we obtain with the existing frameworks. We\u0000also demonstrate its ability to process high-resolution spectroscopy data and\u0000using original methods, by reproducing the results of the Hitomi collaboration\u0000on the Perseus cluster, while solving the inference problem using variational\u0000inference on a GPU. Results. We obtain identical results when compared to other\u0000softwares and approaches, meaning that jaxspec provides reliable results while\u0000being $sim 10$ times faster than existing alternatives. In addition, we show\u0000that variational inference can produce convincing results even on\u0000high-resolution data in less than 10 minutes on a GPU. Conclusions. With this\u0000package, we aim to pursue the goal of opening up X-ray spectroscopy to the\u0000existing ecosystem of machine learning and Bayesian inference, enabling\u0000researchers to apply new methods to solve increasingly complex problems in the\u0000best possible way. Our long-term ambition is the scientific exploitation of the\u0000data from the newAthena X-ray Integral Field Unit (X-IFU).","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217516","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}
Directly imaging Earth-like exoplanets within habitable zones is challenging because faint signals can be obscured by exozodiacal dust, analogous to our solar system's zodiacal dust. This dust scatters starlight, creating a bright background noise. This paper introduces Toy Coronagraph, a Python package designed to quantify the impact of this dust on exoplanet detection. It takes circularly symmetric disk images point spread functions (PSFs), and exoplanet orbital parameters as input, generating key metrics like contrast curves, signal-to-noise ratios, and dynamic visualizations of exoplanet motion under the dust background. The package also provides tools for generating vortex coronagraph PSFs and includes example disk images. Toy Coronagraph empowers researchers to understand exozodiacal dust, develop mitigation strategies, and optimize future telescope designs and mission time, ultimately advancing the search for potentially habitable worlds. Future work will focus on handling non-circularly symmetric inputs, incorporating realistic noise models, and estimating exoplanet yield rates for future space telescope missions.
对宜居带内的类地行星进行直接成像具有挑战性，因为微弱的信号会被黄道外尘埃（类似于太阳系的黄道尘埃）所遮挡。这些尘埃会散射星光，产生明亮的背景噪声。本文介绍的 Toy Coronagraph 是一个 Python 软件包，用于量化这些尘埃对系外行星探测的影响。它将圆盘对称图像点扩散函数（PSF）和系外行星轨道参数作为输入，生成对比曲线、信噪比和系外行星在尘埃背景下运动的动态可视化等关键指标。该软件包还提供了生成涡旋摄谱仪 PSF 的工具，并包含磁盘图像示例。Toy Coronagraph 使研究人员有能力了解黄道外尘埃，制定减缓策略，优化未来的望远镜设计和任务时间，最终推动对潜在宜居世界的研究。未来的工作将侧重于处理非圆对称输入、纳入现实的噪声模型以及为未来的太空望远镜任务估算系外行星产出率。
{"title":"Unveiling habitable planets: Toy coronagraph tackles the exozodiacal dust challenge","authors":"Yu-Chia Lin","doi":"arxiv-2409.05797","DOIUrl":"https://doi.org/arxiv-2409.05797","url":null,"abstract":"Directly imaging Earth-like exoplanets within habitable zones is challenging\u0000because faint signals can be obscured by exozodiacal dust, analogous to our\u0000solar system's zodiacal dust. This dust scatters starlight, creating a bright\u0000background noise. This paper introduces Toy Coronagraph, a Python package\u0000designed to quantify the impact of this dust on exoplanet detection. It takes\u0000circularly symmetric disk images point spread functions (PSFs), and exoplanet\u0000orbital parameters as input, generating key metrics like contrast curves,\u0000signal-to-noise ratios, and dynamic visualizations of exoplanet motion under\u0000the dust background. The package also provides tools for generating vortex\u0000coronagraph PSFs and includes example disk images. Toy Coronagraph empowers\u0000researchers to understand exozodiacal dust, develop mitigation strategies, and\u0000optimize future telescope designs and mission time, ultimately advancing the\u0000search for potentially habitable worlds. Future work will focus on handling\u0000non-circularly symmetric inputs, incorporating realistic noise models, and\u0000estimating exoplanet yield rates for future space telescope missions.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"65 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217390","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}
This contribution summarizes the main activities and objectives of the outreach project Astroaccesible, whose main aim is to carry the teaching and diffusion of astronomy among all kinds of collectives, focusing on blind and visually impaired (BVI) people. This project is led by a blind astronomer and aims to use a variety of resources based on different sensory channels, avoiding limiting the transmission of concepts to visual perception. This principle favors inclusion and benefits everyone, as the information is not presented using just one channel. This strategy is especially convenient for the nowadays typical data acquisition, where a variety of sources of information, not solely based on the collection of different spectral domains of electromagnetic radiation, is used. Moreover, the study of new multi-messenger astronomy could be much better understood using a multi-messenger teaching approach, favoring inclusion, motivation, and creativity.
{"title":"Astroaccesible: A multi-messenger outreach for a multi-messenger science","authors":"Enrique Pérez-Montero","doi":"arxiv-2409.05505","DOIUrl":"https://doi.org/arxiv-2409.05505","url":null,"abstract":"This contribution summarizes the main activities and objectives of the\u0000outreach project Astroaccesible, whose main aim is to carry the teaching and\u0000diffusion of astronomy among all kinds of collectives, focusing on blind and\u0000visually impaired (BVI) people. This project is led by a blind astronomer and\u0000aims to use a variety of resources based on different sensory channels,\u0000avoiding limiting the transmission of concepts to visual perception. This\u0000principle favors inclusion and benefits everyone, as the information is not\u0000presented using just one channel. This strategy is especially convenient for\u0000the nowadays typical data acquisition, where a variety of sources of\u0000information, not solely based on the collection of different spectral domains\u0000of electromagnetic radiation, is used. Moreover, the study of new\u0000multi-messenger astronomy could be much better understood using a\u0000multi-messenger teaching approach, favoring inclusion, motivation, and\u0000creativity.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217395","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}
Sarah Steiger, Laurent Pueyo, Emiel H. Por, Pin Chen, Rémi Soummer, Raphaël Pourcelot, Iva Laginja, Vanessa P. Bailey
One of the primary science goals of the Habitable Worlds Observatory (HWO) as defined by the Astro2020 decadal survey is the imaging of the first Earth-like planet around a Sun-like star. A key technology gap towards reaching this goal are the development of ultra-low-noise photon counting detectors capable of measuring the incredibly low count rates coming from these planets which are at contrasts of $sim 1 times 10^{-10}$. Superconducting energy-resolving detectors (ERDs) are a promising technology for this purpose as, despite their technological challenges, needing to be cooled below their superconducting transition temperature ($< 1mathrm{K}$), they have essentially zero read noise, dark current, or clock-induced charge, and can get the wavelength of each incident photon without the use of additional throughput-reducing filters or gratings that spread light over many pixels. The use of these detectors on HWO will not only impact the science of the mission by decreasing the required exposure times for exo-Earth detection and characterization, but also in a wavefront sensing and control context when used for starlight suppression to generate a dark zone. We show simulated results using both an EMCCD and an ERD to ``dig a dark zone'' demonstrating that ERDs can achieve the same final contrast as an EMCCD in about half of the total time. We also perform a simple case study using an exposure time calculator tool called the Error Budget Software (EBS) to determine the required integration times to detect water for HWO targets of interest using both EMCCDs and ERDs. This shows that once a dark zone is achieved, using an ERD can decrease these exposure times by factors of 1.5--2 depending on the specific host star properties.
{"title":"Simulated performance of energy-resolving detectors towards exoplanet imaging with the Habitable Worlds Observatory","authors":"Sarah Steiger, Laurent Pueyo, Emiel H. Por, Pin Chen, Rémi Soummer, Raphaël Pourcelot, Iva Laginja, Vanessa P. Bailey","doi":"arxiv-2409.05987","DOIUrl":"https://doi.org/arxiv-2409.05987","url":null,"abstract":"One of the primary science goals of the Habitable Worlds Observatory (HWO) as\u0000defined by the Astro2020 decadal survey is the imaging of the first Earth-like\u0000planet around a Sun-like star. A key technology gap towards reaching this goal\u0000are the development of ultra-low-noise photon counting detectors capable of\u0000measuring the incredibly low count rates coming from these planets which are at\u0000contrasts of $sim 1 times 10^{-10}$. Superconducting energy-resolving\u0000detectors (ERDs) are a promising technology for this purpose as, despite their\u0000technological challenges, needing to be cooled below their superconducting\u0000transition temperature ($< 1mathrm{K}$), they have essentially zero read\u0000noise, dark current, or clock-induced charge, and can get the wavelength of\u0000each incident photon without the use of additional throughput-reducing filters\u0000or gratings that spread light over many pixels. The use of these detectors on\u0000HWO will not only impact the science of the mission by decreasing the required\u0000exposure times for exo-Earth detection and characterization, but also in a\u0000wavefront sensing and control context when used for starlight suppression to\u0000generate a dark zone. We show simulated results using both an EMCCD and an ERD\u0000to ``dig a dark zone'' demonstrating that ERDs can achieve the same final\u0000contrast as an EMCCD in about half of the total time. We also perform a simple\u0000case study using an exposure time calculator tool called the Error Budget\u0000Software (EBS) to determine the required integration times to detect water for\u0000HWO targets of interest using both EMCCDs and ERDs. This shows that once a dark\u0000zone is achieved, using an ERD can decrease these exposure times by factors of\u00001.5--2 depending on the specific host star properties.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"59 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217341","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}
Magnetohydrodynamic (MHD) turbulence plays a critical role in many key astrophysical processes such as star formation, acceleration of cosmic rays, and heat conduction. However, its properties are still poorly understood. We explore how to extract the intermittency of compressible MHD turbulence from the synthetic and real observations. The three statistical methods, namely the probability distribution function, kurtosis, and scaling exponent of the multi-order structure function, are used to reveal the intermittency of MHD turbulence. Our numerical results demonstrate that: (1) the synchrotron polarization intensity statistics can be used to probe the intermittency of magnetic turbulence, by which we can distinguish different turbulence regimes; (2) the intermittency of MHD turbulence is dominated by the slow mode in the sub-Alfv{'e}nic turbulence regime; (3) the Galactic interstellar medium (ISM) at the low latitude region corresponds to the sub-Alfv'enic and supersonic turbulence regime. We have successfully measured the intermittency of the Galactic ISM from the synthetic and realistic observations.
{"title":"Exploring the intermittency of magnetohydrodynamic turbulence by synchrotron polarization radiation","authors":"Ru-Yue WangXiangtan Univ., Jian-Fu Zhang, Fang Lu, Fu-Yuan Xiang","doi":"arxiv-2409.05739","DOIUrl":"https://doi.org/arxiv-2409.05739","url":null,"abstract":"Magnetohydrodynamic (MHD) turbulence plays a critical role in many key\u0000astrophysical processes such as star formation, acceleration of cosmic rays,\u0000and heat conduction. However, its properties are still poorly understood. We\u0000explore how to extract the intermittency of compressible MHD turbulence from\u0000the synthetic and real observations. The three statistical methods, namely the\u0000probability distribution function, kurtosis, and scaling exponent of the\u0000multi-order structure function, are used to reveal the intermittency of MHD\u0000turbulence. Our numerical results demonstrate that: (1) the synchrotron\u0000polarization intensity statistics can be used to probe the intermittency of\u0000magnetic turbulence, by which we can distinguish different turbulence regimes;\u0000(2) the intermittency of MHD turbulence is dominated by the slow mode in the\u0000sub-Alfv{'e}nic turbulence regime; (3) the Galactic interstellar medium (ISM)\u0000at the low latitude region corresponds to the sub-Alfv'enic and supersonic\u0000turbulence regime. We have successfully measured the intermittency of the\u0000Galactic ISM from the synthetic and realistic observations.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217486","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}
Lisa Altinier, Élodie Choquet, Arthur Vigan, Nicolás Godoy, Alexis Lau
The Roman Coronagraph Instrument will be the first space facility equipped with deformable mirrors (DMs). These will lead to reach a contrast of $10^{-8}$ or better in a dark hole between $3-9 lambda/D$. Post-processing techniques play an important role in increasing the contrast limits. Our work investigates how DMs can be used to calibrate the instrument response to controlled wavefront error maps and to improve the post-processing performance. To this goal, we are developing a simulation pipeline, CAPyBARA, that includes both a propagation model of the Coronagraph and a post-processing module and produces starlight subtracted images of a science target. This pipeline will allow us to investigate alternative observing strategies and test their performance for the Roman Coronagraph. Here we present the first version of the simulator: it currently reproduces the optical propagation, which consists in the hybrid Lyot coronagraph optical structure and dark-hole digging technique (Electric Field Conjugation coupled with $beta$-bumping), the environment (quasi-static aberration) and the post-processing. With it, we mimic a Coronagraph Instrument observing sequence, which consists in first acquiring reference star data before slewing to the scientific target, and we investigate how the evolution of quasi-static aberrations deteriorate the contrast limit in the dark hole. We simulate a science target with planets at high contrast with their star and we perform a first post-processing analysis with classical subtraction techniques. Here we present the CAPyBARA simulator, as well as some first results. The next step will be to generate PSF libraries by injecting pre-calibrated probes on the DMs (in open loop) during the reference star acquisition and compute a PCA model. Later, we will compare the performance gain obtained with the modulated-DM reference library over standard approaches (RDI).
{"title":"ESCAPE project. CAPyBARA: a Roman Coronagraph simulator for post-processing methods development","authors":"Lisa Altinier, Élodie Choquet, Arthur Vigan, Nicolás Godoy, Alexis Lau","doi":"arxiv-2409.05781","DOIUrl":"https://doi.org/arxiv-2409.05781","url":null,"abstract":"The Roman Coronagraph Instrument will be the first space facility equipped\u0000with deformable mirrors (DMs). These will lead to reach a contrast of $10^{-8}$\u0000or better in a dark hole between $3-9 lambda/D$. Post-processing techniques\u0000play an important role in increasing the contrast limits. Our work investigates\u0000how DMs can be used to calibrate the instrument response to controlled\u0000wavefront error maps and to improve the post-processing performance. To this\u0000goal, we are developing a simulation pipeline, CAPyBARA, that includes both a\u0000propagation model of the Coronagraph and a post-processing module and produces\u0000starlight subtracted images of a science target. This pipeline will allow us to\u0000investigate alternative observing strategies and test their performance for the\u0000Roman Coronagraph. Here we present the first version of the simulator: it\u0000currently reproduces the optical propagation, which consists in the hybrid Lyot\u0000coronagraph optical structure and dark-hole digging technique (Electric Field\u0000Conjugation coupled with $beta$-bumping), the environment (quasi-static\u0000aberration) and the post-processing. With it, we mimic a Coronagraph Instrument\u0000observing sequence, which consists in first acquiring reference star data\u0000before slewing to the scientific target, and we investigate how the evolution\u0000of quasi-static aberrations deteriorate the contrast limit in the dark hole. We\u0000simulate a science target with planets at high contrast with their star and we\u0000perform a first post-processing analysis with classical subtraction techniques.\u0000Here we present the CAPyBARA simulator, as well as some first results. The next\u0000step will be to generate PSF libraries by injecting pre-calibrated probes on\u0000the DMs (in open loop) during the reference star acquisition and compute a PCA\u0000model. Later, we will compare the performance gain obtained with the\u0000modulated-DM reference library over standard approaches (RDI).","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217391","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}
Davide Vaccaro, Jan van der Kuur, Paul van der Hulst, Tobias Vos, Martin de Wit, Luciano Gottardi, Kevin Ravensberg, Emanuele Taralli, Joseph Adams, Simon Bandler, Douglas Bennet, James Chervenak, Bertrand Doriese, Malcolm Durkin, Jonathan Gard, Carl Reintsema, Kazuhiro Sakai, Steven Smith, Joel Ullom, Nicholas Wakeham, Jan-Willem den Herder, Brian jackson, Pourya Khosropanah, Jian-Rong Gao, Peter Roelfsema, Aurora Simionescu
The X-ray Integral Field Unit (X-IFU) is an instrument of ESA's future NewAthena space observatory, with the goal to provide high-energy resolution ($<$ 4 eV at X-ray energies up to 7 keV) and high-spatial resolution (9") spectroscopic imaging over the X-ray energy range from 200 eV to 12 keV, by means of an array of about 1500 transition-edge sensors (TES) read out via SQUID time-division multiplexing (TDM). In 2022, to aid in the transfer of TDM readout technology from the laboratory toward flight hardware, our team commissioned a new TDM-based laboratory test-bed at SRON. This setup hosts an array of $75times 75 mu$m$^2$ TESs that are read out via 2-column $times$ 32-row TDM. A system component that is critical to high-performance operation is the wiring harness that connects the room-temperature electronics to the cryogenic readout componentry. In November 2023, we implemented a re-designed flex harness, which in the SRON test-bed has a length close to what is envisioned for the X-IFU flight harness. We report here on our characterization of the TDM system with the new flex harness, which allowed the system to achieve a co-added energy resolution at a level of 2.7~eV FWHM at 6~keV via 32-row readout. In addition, we provide an outlook on the upcoming integration of TDM readout into the X-IFU Focal-Plane Assembly Development Model.
{"title":"System performance of a cryogenic test-bed for the time-division multiplexing readout for NewAthena X-IFU","authors":"Davide Vaccaro, Jan van der Kuur, Paul van der Hulst, Tobias Vos, Martin de Wit, Luciano Gottardi, Kevin Ravensberg, Emanuele Taralli, Joseph Adams, Simon Bandler, Douglas Bennet, James Chervenak, Bertrand Doriese, Malcolm Durkin, Jonathan Gard, Carl Reintsema, Kazuhiro Sakai, Steven Smith, Joel Ullom, Nicholas Wakeham, Jan-Willem den Herder, Brian jackson, Pourya Khosropanah, Jian-Rong Gao, Peter Roelfsema, Aurora Simionescu","doi":"arxiv-2409.05643","DOIUrl":"https://doi.org/arxiv-2409.05643","url":null,"abstract":"The X-ray Integral Field Unit (X-IFU) is an instrument of ESA's future\u0000NewAthena space observatory, with the goal to provide high-energy resolution\u0000($<$ 4 eV at X-ray energies up to 7 keV) and high-spatial resolution (9\")\u0000spectroscopic imaging over the X-ray energy range from 200 eV to 12 keV, by\u0000means of an array of about 1500 transition-edge sensors (TES) read out via\u0000SQUID time-division multiplexing (TDM). In 2022, to aid in the transfer of TDM\u0000readout technology from the laboratory toward flight hardware, our team\u0000commissioned a new TDM-based laboratory test-bed at SRON. This setup hosts an\u0000array of $75times 75 mu$m$^2$ TESs that are read out via 2-column $times$\u000032-row TDM. A system component that is critical to high-performance operation\u0000is the wiring harness that connects the room-temperature electronics to the\u0000cryogenic readout componentry. In November 2023, we implemented a re-designed\u0000flex harness, which in the SRON test-bed has a length close to what is\u0000envisioned for the X-IFU flight harness. We report here on our characterization\u0000of the TDM system with the new flex harness, which allowed the system to\u0000achieve a co-added energy resolution at a level of 2.7~eV FWHM at 6~keV via\u000032-row readout. In addition, we provide an outlook on the upcoming integration\u0000of TDM readout into the X-IFU Focal-Plane Assembly Development Model.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217394","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}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：