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MeV astrophysical spectroscopic surveyor (MASS): a compton telescope mission concept MeV天体物理光谱勘测器(MASS):康普顿望远镜任务概念
IF 2.7 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-02-24 DOI: 10.1007/s10686-024-09920-4
Jiahuan Zhu, Xutao Zheng, Hua Feng, Ming Zeng, Chien-You Huang, Jr-Yue Hsiang, Hsiang-Kuang Chang, Hong Li, Hao Chang, Xiaofan Pan, Ge Ma, Qiong Wu, Yulan Li, Xuening Bai, Mingyu Ge, Long Ji, Jian Li, Yangping Shen, Wei Wang, Xilu Wang, Binbin Zhang, Jin Zhang

We propose a future mission concept, the MeV Astrophysical Spectroscopic Surveyor (MASS), which is a large area Compton telescope using 3D position sensitive cadmium zinc telluride (CZT) detectors optimized for emission line detection. The payload consists of two layers of CZT detectors in a misaligned chessboard layout, with a total geometric area of 4096 cm(^2) for on-axis observations. The detectors can be operated at room-temperature with an energy resolution of 0.6% at 0.662 MeV. The in-orbit background is estimated with a mass model. At energies around 1 MeV, a line sensitivity of about (10^{-5}) photons cm(^{-2}) s(^{-1}) can be obtained with a 1 Ms observation. The main science objectives of MASS include nucleosynthesis in astrophysics and high energy astrophysics related to compact objects and transient sources. The payload CZT detectors weigh roughly 40 kg, suggesting that it can be integrated into a micro- or mini-satellite. We have constructed a pathfinder, named as MASS-Cube, to have a direct test of the technique with 4 detector units in space in the near future.

摘要 我们提出了一个未来任务概念--MeV 天体光谱勘测器(MASS),这是一个大面积康普顿望远镜,使用三维位置敏感的碲锌镉(CZT)探测器,优化了发射线探测。有效载荷由两层棋盘式错位布局的碲锌镉探测器组成,轴上观测的总几何面积为 4096 厘米(^2)。探测器可在室温下运行,0.662MeV时的能量分辨率为0.6%。在轨本底是用质量模型估算的。在 1 MeV 左右的能量下,1 Ms 的观测可获得约 (10^{-5}) 光子 cm (^{-2}) s (^{-1}) 的线灵敏度。MASS的主要科学目标包括天体物理学中的核合成以及与紧凑天体和瞬变源有关的高能天体物理学。有效载荷 CZT 探测器重约 40 千克,这表明它可以集成到微型或小型卫星中。我们已经建造了一个名为 MASS-Cube 的探路者,以便在不久的将来在太空中用 4 个探测器单元对该技术进行直接测试。
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引用次数: 0
Simulation studies for the first pathfinder of the CATCH space mission CATCH 空间飞行任务第一个探路者的模拟研究
IF 2.7 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-02-24 DOI: 10.1007/s10686-024-09924-0
Yiming Huang, Juan Zhang, Lian Tao, Zhengwei Li, Donghua Zhao, Qian-Qing Yin, Xiangyang Wen, Jingyu Xiao, Chen Zhang, Shuang-Nan Zhang, Shaolin Xiong, Qingcui Bu, Jirong Cang, Dezhi Cao, Wen Chen, Siran Ding, Min Gao, Yang Gao, Shujin Hou, Liping Jia, Ge Jin, Dalin Li, Jinsong Li, Panping Li, Yajun Li, Xiaojing Liu, Ruican Ma, Xingyu Pan, Liqiang Qi, Jinhui Rao, Xianfei Sun, Qingwen Tang, Ruijing Tang, Yusa Wang, Yibo Xu, Sheng Yang, Yanji Yang, Yong Yang, Xuan Zhang, Yueting Zhang, Heng Zhou, Kang Zhao, Qingchang Zhao, Shujie Zhao, Zijian Zhao

The Chasing All Transients Constellation Hunters (CATCH) space mission is an intelligent constellation consisting of 126 micro-satellites in three types (A, B, and C), designed for X-ray observation with the objective of studying the dynamic universe. Currently, we are actively developing the first Pathfinder (CATCH-1) for the CATCH mission, specifically for type-A satellites. CATCH-1 is equipped with Micro Pore Optics (MPO) and a 4-pixel Silicon Drift Detector (SDD) array. To assess its scientific performance, including the effective area of the optical system, on-orbit background, and telescope sensitivity, we employ the Monte Carlo software Geant4 for simulation in this study. The MPO optics exhibit an effective area of 41 cm(^2) at the focal spot for 1 keV X-rays, while the entire telescope system achieves an effective area of 29 cm(^2) at 1 keV when taking into account the SDD detector’s detection efficiency. The primary contribution to the background is found to be from the Cosmic X-ray Background. Assuming a 625 km orbit with an inclination of (29^circ ), the total background for CATCH-1 is estimated to be (8.13times 10^{-2}) counts s(^{-1}) in the energy range of 0.5–4 keV. Based on the background within the central detector and assuming a Crab-like source spectrum, the estimated ideal sensitivity could achieve (1.9times 10^{-12}) erg cm(^{-2}) s(^{-1}) for an exposure of 10(^4) s in the energy band of 0.5–4 keV. Furthermore, after simulating the background caused by low-energy charged particles near the geomagnetic equator, we have determined that there is no need to install a magnetic deflector.

摘要 "追逐所有瞬变星座猎手"(CATCH)空间任务是一个智能星座,由 126 颗微型卫星组成,分为 A、B 和 C 三种类型,设计用于 X 射线观测,目的是研究动态宇宙。目前,我们正在积极开发 CATCH 任务的第一个探路者(CATCH-1),专门用于 A 型卫星。CATCH-1 配备了微孔光学器件(MPO)和 4 像素硅漂移探测器(SDD)阵列。为了评估其科学性能,包括光学系统的有效面积、在轨背景和望远镜灵敏度,我们在本研究中使用蒙特卡洛软件 Geant4 进行了模拟。对于 1 keV X 射线,MPO 光学系统的焦斑有效面积为 41 厘米,而考虑到 SDD 探测器的探测效率,整个望远镜系统在 1 keV 时的有效面积为 29 厘米。对背景的主要贡献来自宇宙 X 射线背景。假定CATCH-1的轨道为625公里,倾角为(29^circ),那么在0.5-4 keV的能量范围内,CATCH-1的总背景估计为(8.13times 10^{-2}) counts s(^{-1}) 。根据中央探测器内的本底,并假定有一个类似于螃蟹的源光谱,在0.5-4 keV的能段内曝光10 (^4) s,估计理想的灵敏度可以达到 (1.9 次 10^{-12}) erg cm (^{-2}) s (^{-1}) 。此外,在模拟了地磁赤道附近低能量带电粒子造成的背景之后,我们确定没有必要安装磁偏转器。
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引用次数: 0
A mission to nature’s telescope for high-resolution imaging of an exoplanet 为系外行星提供高分辨率成像的大自然望远镜任务
IF 2.7 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-02-13 DOI: 10.1007/s10686-024-09919-x
Louis D. Friedman, Darren Garber, Slava G. Turyshev, Henry Helvajian, Thomas Heinshiemer, John McVey, Artur R. Davoyan

The solar gravitational lens (SGL) provides a factor of (10^{11}) amplification for viewing distant point sources beyond our solar system. As such, it may be used for resolved imaging of extended sources, such as exoplanets, not possible otherwise. To use the SGL, a spacecraft carrying a modest telescope and a coronagraph must reach the SGLs focal region, that begins at (sim )550 astronomical units (AU) from the Sun and is oriented outward along the line connecting the distant object and the Sun. No spacecraft has ever reached even a half of that distance; and to do so within a reasonable mission lifetime (e.g., less than 25 years) and affordable cost requires a new type of mission design, using solar sails and microsats ((<100) kg). The payoff is high – using the SGL is the only practical way we can ever get a high-resolution, multi-pixel image of an Earth-like exoplanet, one that we identify as potentially habitable. This paper describes a novel mission design starting with a rideshare launch from the Earth, spiraling in toward the Sun, and then flying around it to achieve solar system exit speeds of over 20 AU/year. A new sailcraft design is used to make possible high area to mass ratio for the sailcraft. The mission design enables other fast solar system missions, starting with a proposed very low cost technology demonstration mission (TDM) to prove the functionality and operation of the microsat-solar sail design and then, building on the TDM, missions to explore distant regions of the solar system, and those to study Kuiper Belt objects (KBOs) and the recently discovered interstellar objects (ISOs) are also possible.

太阳引力透镜(SGL)为观测太阳系以外的遥远点源提供了一个(10^{11})放大系数。因此,它可以用来对系外行星等扩展源进行分辨成像,这是其他方法无法实现的。要使用SGL,携带适中望远镜和日冕仪的航天器必须到达SGL的焦点区域,该区域从距离太阳550天文单位(AU)处开始,沿着遥远天体和太阳的连接线向外定向。从来没有航天器到达过这个距离的一半;要在合理的飞行任务寿命(例如少于25年)和可承受的成本范围内到达这个距离,需要一种新型的飞行任务设计,使用太阳帆和微型卫星(100千克)。这样做的回报是很高的--使用太阳帆是我们获得类地系外行星的高分辨率、多像素图像的唯一实用方法,而这颗类地系外行星是我们认定可能适合居住的。本文介绍了一种新颖的任务设计,首先从地球发射,螺旋式飞向太阳,然后绕太阳飞行,以达到太阳系出口速度超过 20 AU/年。新的帆船设计使帆船的高面积质量比成为可能。该飞行任务的设计使其他快速太阳系飞行任务成为可能,首先是一个拟议的低成本技术演示飞行任务(TDM),以证明微型卫星-太阳帆设计的功能和运行,然后在TDM的基础上,探索太阳系遥远区域的飞行任务,以及研究柯伊伯带天体(KBOs)和最近发现的星际天体(ISOs)的飞行任务也成为可能。
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引用次数: 0
Searching for long faint astronomical high energy transients: a data driven approach 寻找长时间微弱的天文高能瞬变:数据驱动的方法
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-22 DOI: 10.1007/s10686-023-09915-7
Riccardo Crupi, Giuseppe Dilillo, Elisabetta Bissaldi, Kester Ward, Fabrizio Fiore, Andrea Vacchi

HERMES Pathfinder is an in-orbit demonstration consisting of a constellation of six 3U nano-satellites hosting simple but innovative detectors for the monitoring of cosmic high-energy transients. The main objective of HERMES Pathfinder is to prove that accurate position of high-energy cosmic transients can be obtained using miniaturized hardware. The transient position is obtained by studying the delay time of arrival of the signal to different detectors hosted by nano-satellites on low-Earth orbits. In this context, we need to develop novel tools to fully exploit the future scientific data output of HERMES Pathfinder. In this paper, we introduce a new framework to assess the background count rate of a spaceborne, high energy detector; a key step towards the identification of faint astrophysical transients. We employ a neural network to estimate the background lightcurves on different timescales. Subsequently, we employ a fast change-point and anomaly detection technique called Poisson-FOCuS to identify observation segments where statistically significant excesses in the observed count rate relative to the background estimate exist. We test the new software on archival data from the NASA Fermi Gamma-ray Burst Monitor (GBM), which has a collecting area and background level of the same order of magnitude to those of HERMES Pathfinder. The neural network performances are discussed and analyzed over period of both high and low solar activity. We were able to confirm events in the Fermi-GBM catalog, both solar flares and gamma-ray bursts, and found events, not present in Fermi-GBM database, that could be attributed to solar flares, terrestrial gamma-ray flashes, gamma-ray bursts and galactic X-ray flashes. Seven of these are selected and further analyzed, providing an estimate of localisation and a tentative classification.

HERMES Pathfinder是一个在轨演示,由6颗3U纳米卫星组成,这些卫星承载着简单但创新的探测器,用于监测宇宙高能瞬变。HERMES探路者的主要目标是证明使用小型化硬件可以获得高能宇宙瞬变的精确位置。通过研究信号到达低地球轨道纳米卫星不同探测器的延迟时间,得到了瞬态位置。在此背景下,我们需要开发新的工具来充分利用HERMES探路者未来的科学数据输出。本文提出了一种评估星载高能探测器背景计数率的新框架;这是识别微弱天体物理瞬变的关键一步。我们使用神经网络来估计不同时间尺度上的背景光曲线。随后,我们采用一种称为泊松焦点的快速变化点和异常检测技术来识别观测到的计数率相对于背景估计存在统计上显著过剩的观测段。我们在美国宇航局费米伽马射线暴监测仪(GBM)的档案数据上测试了新软件,它的收集面积和背景水平与赫尔墨斯探路者的相同数量级。讨论和分析了神经网络在太阳活动高峰和低谷时期的性能。我们能够确认Fermi-GBM目录中的事件,太阳耀斑和伽马射线暴,并发现Fermi-GBM数据库中没有的事件,可以归因于太阳耀斑,地球伽马射线闪光,伽马射线暴和银河系x射线闪光。选择其中的七个并进一步分析,提供本地化的估计和初步分类。
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引用次数: 0
Digital archival spectral data for Seyfert galaxies and their use in conjunction with modern FAI spectral data 塞弗特星系的数字档案光谱数据及其与现代FAI光谱数据的结合使用
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-22 DOI: 10.1007/s10686-023-09916-6
Saule Shomshekova, Lyudmila Kondratyeva, Chingis Omarov, Ildana Izmailova, Adel Umirbayeva, Svetlana Moshkina

The paper presents a methodology for the digitization and processing of our own spectral data archive and the results of comparing the obtained data with those of modern observations. An Epson Perfection V850 Pro scanner with optional SilverFast8 software was used to scan photographic films. More than 2,000 archive spectra of Seyfert galaxies obtained in 1970–1990 with the AZT-8 telescope have been scanned to date (resolution 2400 dpi). The work describes the reduction of distortion for the scanned spectra using the program code, created in Python. Our code has been registered on the web service “GitHub” and a link to the code is given in the work. The results of digitization and subsequent spectra processing are presented in the example of the Seyfert galaxy Mrk 3. For the absolute calibration of the early spectra (Jan. 25, 1976) the radiation fluxes in the emission lines of [SII] were used. The lines were measured on the modern spectrogram obtained in 2023 on telescope AZT-8 (Mar. 14, 2023)

本文介绍了我国自己的光谱数据档案的数字化和处理方法,并将所获得的数据与现代观测数据进行了比较。使用爱普生perfect V850 Pro扫描仪和可选的SilverFast8软件扫描摄影胶片。迄今为止,AZT-8望远镜在1970-1990年间获得了2000多个塞弗特星系的存档光谱(分辨率2400 dpi)。该工作描述了使用Python创建的程序代码减少扫描光谱的失真。我们的代码已经在web服务“GitHub”上注册,并且在工作中给出了代码的链接。以塞弗特星系Mrk 3为例,给出了数字化和后续光谱处理的结果。对早期光谱(1976年1月25日)的绝对定标,采用了[SII]发射谱线的辐射通量。这些线是在2023年用AZT-8望远镜(2023年3月14日)获得的现代谱图上测量的。
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引用次数: 0
Relativistic particle measurement in jupiter’s magnetosphere with Pix.PAN 用Pix测量木星磁层中的相对论粒子。锅
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-18 DOI: 10.1007/s10686-023-09918-4
Johannes Hulsman, Xin Wu, Philipp Azzarello, Benedikt Bergmann, Michael Campbell, George Clark, Franck Cadoux, Tomoya Ilzawa, Peter Kollmann, Xavi Llopart, Quentin Nénon, Mercedes Paniccia, Elias Roussos, Petr Smolyanskiy, Daniil Sukhonos, Pierre Alexandre Thonet

Pix.PAN is a compact cylindrical magnetic spectrometer, intended to provide excellent high energy particle measurements under high rate and hostile operating conditions in space. Its principal design is composed of two Halbach-array magnetic sectors and six Timepix4-based tracking layers; the latest hybrid silicon pixel detector readout ASIC designed. Due to Pix.PAN’s compact and relatively simple design, it has the potential to be used for space missions exploring with measurements of unprecedented precision, high energy particles in radiation belts and the heliophere (solar energetic particles, anomalous and galactic cosmic rays). In this white paper, we discuss the design and expected performance of Pix.PAN for COMPASS (Comprehensive Observations of Magnetospheric Particle Acceleration, Sources, and Sinks), a mission concept submitted to NASA’s Call “B.16 Heliophysics Mission Concept Studies (HMCS)” in 2021 that targets the extreme high energy particle environment of Jupiter’s inner radiation belts. We also discuss PixPAN’s operational conditions and interface requirements. The conceptual design shows that is possible to achieve an energy resolution of<12% for electrons in the range of 10 MeV-1 GeV and<35% for protons between (sim )200 MeV to a few GeV. Due to the timestamp precision of Timepix4, a time resolution (on an instrument level) of about 100 ps can be achieved for time-of-flight measurements. In the most intense radiation environments of the COMPASS mission, Pix.PAN is expected to have a maximum hit rate of 44(frac{text {MHz}}{text {cm}^2}) which is below the design limit of 360(frac{text {MHz}}{text {cm}^2}) of Timepix4. Finally, a sensor design is proposed which allows the instrument to operate with a power budget of 20W without the loss of scientific performance.

Pix。PAN是一种紧凑的圆柱形磁谱仪,旨在在高速率和恶劣的空间操作条件下提供出色的高能粒子测量。其主要设计由两个哈尔巴赫阵列磁扇区和六个基于timepix4的跟踪层组成;最新设计的混合硅像素检测器读出专用集成电路。由于Pix。PAN的紧凑和相对简单的设计,它有潜力用于空间任务,探索前所未有的精度,辐射带和日球层的高能粒子(太阳高能粒子,异常和银河宇宙射线)。在本白皮书中,我们讨论了Pix的设计和预期性能。PAN for COMPASS(磁层粒子加速、源和汇的综合观测),这是一个提交给NASA B.16的任务概念太阳物理任务概念研究(HMCS)”,目标是木星内部辐射带的极端高能粒子环境。讨论了PixPAN的运行条件和接口要求。概念设计表明,可以实现12的能量分辨率% for electrons in the range of 10 MeV-1 GeV and<35% for protons between (sim )200 MeV to a few GeV. Due to the timestamp precision of Timepix4, a time resolution (on an instrument level) of about 100 ps can be achieved for time-of-flight measurements. In the most intense radiation environments of the COMPASS mission, Pix.PAN is expected to have a maximum hit rate of 44(frac{text {MHz}}{text {cm}^2}) which is below the design limit of 360(frac{text {MHz}}{text {cm}^2}) of Timepix4. Finally, a sensor design is proposed which allows the instrument to operate with a power budget of 20W without the loss of scientific performance.
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引用次数: 0
The measurement and modeling of gravitational deformation for large radio telescope based on wavefront perturbation method 基于波前扰动法的大型射电望远镜引力变形测量与建模
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-13 DOI: 10.1007/s10686-023-09917-5
Jinqing Wang, Zheng Lou, Yongbin Jiang, Zhengxiong Sun, Linfeng Yu, Weiye Zhong, Yongchen Jiang, Rongbin Zhao, Li Fu, Qian Ye, Shengcai Shi, Qinghui Liu, Yingxi Zuo

In this paper, the wavefront perturbation method based on power detection of radio sources is used to measure the surface error of the Tianma radio telescope. By measuring the surface errors at different elevation angles, a surface compensation model to correct gravitational deformation is established. Observation results shows that the efficiency reduction caused by the gravitational deformation can be effectively compensated by loading this model on the active surface, especially at high and low elevations. A dual-beam calibration scheme is further used to remove atmospheric background fluctuations, which significantly improves data quality at lower elevations. The form and order of the perturbation modes and data processing are optimized to improve measurement accuracy. This paper presents the first attempt to apply the wavefront perturbation method to large radio telescopes and demonstrates its capacity and effectiveness in telescope runtime surface measurement and maintenance.

本文采用基于射电源功率检测的波前扰动方法来测量天马射电望远镜的表面误差。通过测量不同仰角下的表面误差,建立了修正引力变形的表面补偿模型。观测结果表明,通过在有源面上加载该模型,可以有效补偿重力形变导致的效率降低,尤其是在高海拔和低海拔地区。双波束校准方案进一步用于消除大气背景波动,从而显著提高了低海拔地区的数据质量。对扰动模式的形式和顺序以及数据处理进行了优化,以提高测量精度。本文首次尝试将波前扰动方法应用于大型射电望远镜,并展示了该方法在望远镜运行表面测量和维护方面的能力和有效性。
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引用次数: 0
Analytical fitting of (gamma )–ray photopeaks in germanium cross strip detectors 锗交叉带探测器中的(γ)射线光峰的分析拟合
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-24 DOI: 10.1007/s10686-023-09914-8
Steven E. Boggs, Sean N. Pike

In an ideal germanium detector, fully-absorbed monoenergetic (gamma )–rays will appear in the measured spectrum as a narrow peak, broadened into a Gaussian of width determined only by the statistical properties of charge cloud generation and the electronic noise of the readout electronics. Multielectrode detectors complicate this picture. Broadening of the charge clouds as they drift through the detector will lead to charge sharing between neighboring electrodes and, inevitably, low-energy tails on the photopeak spectra. We simulate charge sharing in our germanium cross strip detectors in order to reproduce the low-energy tails due to charge sharing. Our goal is to utilize these simulated spectra to develop an analytical fit (shape function) for the spectral lines that provides a robust and high-quality fit to the spectral profile, reliably reproduces the interaction energy, noise width, and the number of counts in both the true photopeak and the low-energy tail, and minimizes the number of additional parameters. Accurate modeling of the detailed line profiles is crucial for both calibration of the detectors as well as scientific interpretation of measured spectra.

在一个理想的锗探测器中,完全吸收的单能(γ)射线在测量光谱中将显示为一个窄峰,其宽度仅由电荷云产生的统计特性和读出电子设备的电子噪声决定。多电极探测器使情况更加复杂。电荷云在探测器中漂移时会变宽,这将导致相邻电极之间的电荷共享,不可避免地会在光电峰光谱上出现低能尾。我们模拟了锗交叉带探测器中的电荷共享,以重现电荷共享导致的低能尾迹。我们的目标是利用这些模拟光谱来开发光谱线的分析拟合(形状函数),它能对光谱剖面进行稳健而高质量的拟合,可靠地再现真实光峰和低能尾的相互作用能量、噪声宽度和计数数量,并最大限度地减少附加参数的数量。精确的详细线剖面建模对于探测器的校准和测量光谱的科学解释都至关重要。
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引用次数: 0
Storage optimisation and distributed architecture for time series reconstruction of massive astronomical catalogues 海量天文目录时间序列重建的存储优化和分布式架构
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-09-28 DOI: 10.1007/s10686-023-09913-9
Qing Zhao, Le Sun, Mengxiang Zhang, Chengkui Zhang, Chenzhou Cui, Dongwei Fan

Time series reconstruction of astronomical catalogues is an important part of data archiving and a basis for time-domain astronomical analysis in the era of time-domain astronomy. As the field of view and sampling frequency of various time-domain telescopes increase, the amount of data to be processed becomes larger and larger. How to optimize the spatial and temporal efficiency of this process with the aid of computer technology becomes a hot issue. To address the problem of spatial efficiency, in this paper, we propose a time series data compression algorithm based on the negative database and dynamic programming, and on this basis, we design a multi-level storage and access query architecture for hot data and non-hot data, which greatly compresses the storage space of data while ensuring the query efficiency. To address the issue of time efficiency, this paper proposes a spatio-temporal data partitioning and layout algorithm suitable for distributed architecture, whose nested round-robin strategy has a wide range of load balancing effects on different spatial locations, temporal locations, and different ranges of temporal data queries, which can effectively ensure the execution efficiency of the distributed system. Experimental results show that the proposed optimization algorithm can keep the system at a low load skewness level of about 4% and save about 83% of storage space.

在时域天文学时代,天文目录的时间序列重建是数据存档的重要组成部分,也是时域天文分析的基础。随着各种时域望远镜视场和采样频率的提高,需要处理的数据量也越来越大。如何借助计算机技术优化这一处理过程的空间和时间效率成为一个热点问题。针对空间效率问题,本文提出了一种基于负数据库和动态编程的时间序列数据压缩算法,并在此基础上设计了热数据和非热数据的多级存储和访问查询架构,在保证查询效率的同时极大地压缩了数据的存储空间。针对时间效率问题,本文提出了一种适合分布式架构的时空数据分区与布局算法,其嵌套轮循策略对不同空间位置、不同时间位置、不同范围的时空数据查询具有大范围的负载均衡效果,能有效保证分布式系统的执行效率。实验结果表明,所提出的优化算法能使系统保持在约 4% 的低负载倾斜度水平,并节省约 83% 的存储空间。
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引用次数: 0
A near-UV reconnaissance of metal-poor massive stars 贫金属大质量恒星的近紫外侦察
IF 3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-09-26 DOI: 10.1007/s10686-023-09912-w
Chris Evans, Wagner Marcolino, Jean-Claude Bouret, Miriam Garcia

We use synthetic model spectra to investigate the potential of near-ultraviolet (3000-4050 Å) observations of massive O-type stars. We highlight the He I (lambda )3188 and He II (lambda )3203 pair as a potential temperature diagnostic in this range, supported by estimates of gravity using the high Balmer series lines. The near-ultraviolet also contains important metallic lines for determinations of chemical abundances (oxygen in particular) and estimates of projected rotational velocities for O-type spectra. Using the model spectra we present performance estimates for observations of extragalactic massive stars with the Cassegrain U-Band Efficient Spectrograph (CUBES) now in construction for the Very Large Telescope. The high efficiency of CUBES will open-up exciting new possibilities in the study of massive stars in external galaxies. For instance, CUBES will provide new insights into the physical properties of O-type stars, including oxygen abundances, in metal-poor irregular galaxies at (sim )1 Mpc from integrations of just 2-3 hrs. Moreover, CUBES will bring quantitative spectroscopy of more distant targets within reach for the first time, such as the O-type star (V (sim ) 21.5 mag) in Leo P (at 1.6 Mpc) in only half a night of observations.

我们使用合成模型光谱来研究大质量O型星的近紫外(3000-4050 Å)观测潜力。我们强调He I ((lambda)3188和He II ((lambda)3203)线对是这一范围内潜在的温度诊断线,并利用高巴尔默系列线对重力的估算提供支持。近紫外光谱还包含重要的金属线,用于确定化学丰度(尤其是氧)和估计 O 型光谱的预计旋转速度。利用模型光谱,我们提出了使用正在为甚大望远镜建造的卡塞格伦 U 波段高效摄谱仪(CUBES)观测河外大质量恒星的性能估算。CUBES 的高效率将为研究河外星系中的大质量恒星提供令人兴奋的新可能性。例如,CUBES将提供对O型恒星物理性质的新见解,包括氧丰度,这些恒星位于(sim )1 Mpc的贫金属不规则星系中,其积分时间仅为2-3小时。此外,CUBES还将首次对更遥远的目标进行定量光谱分析,比如狮子座P(1.6 Mpc)中的O型星(V (sim ) 21.5 mag),只需要半个晚上的观测。
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Experimental Astronomy
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