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II.

核心文献

2 篇

0108-20 补录

优先级 85　·　任务方法　·　Einstein Probe　·　时域天文学　·　数据处理

AstroFlow: A customizable workflow management system for astronomical data production and case study of EP-WXT

AstroFlow：天文数据生产可定制工作流管理系统及 EP-WXT 案例研究

Zhang Zhen, Xu Yunfei, Liu Yuan et al.

原文摘要Abstract

In the era of time-domain astronomy, automated and efficient data processing is a crucial factor in ensuring astronomical scientific output. With the international collaboration trend in large-scale sky survey projects, data processing algorithms developed through multi-institutional collaboration face challenges in system integration, scheduling capability, extensibility, and traceability. In this work, we employ containerized execution modules to resolve dependency issues in multi-institutional software integration, implement complex workflow orchestration through message queue control modules, including cyclic dependencies, dynamic parallel relationships, and resource/priority-based scheduling. The system also non-intrusively implements the International Virtual Observatory Alliance (IVOA) provenance data model through aspect injection mechanisms, ensuring traceability and reproducibility of data products. In Einstein Probe (EP) data processing, the system has processed over 20,000 general observations, 170,000 FXT observations, and 21,000 VHF and Beidou alerts, supported over 300 agile algorithm updates, and detected more than 17,000 sources and nearly 200 transient events. The system demonstrates excellent generality and portability, smoothly migrating from the single-module LEIA to the 12-module EP, and supporting data fusion for new payload FXT and multiple data transmission links. This workflow management system provides a flexible, extensible, and standardized data processing framework for future large-scale astronomical observation projects, effectively addressing key issues such as multi-institutional collaboration, complex workflow orchestration, and scientific data reproducibility.

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AI 综述 AI-generated · 以原文为准

亮点

通过容器化执行模块和消息队列控制模块解决多机构软件集成、循环/动态并行调度与资源优先级调度问题，并以切面注入非侵入式实现 IVOA 溯源；在爱因斯坦探针中处理逾 2 万常规观测、17 万 FXT 观测和 2.1 万警报，发现 1.7 万余个源、近 200 个暂现事件。

脉络与展望

该工作承接时域天文学与虚拟天文台对自动化数据处理、溯源和标准化的需求，将容器化和消息队列引入天文数据流水线，使多机构算法集成不再受依赖冲突制约。相比传统单体或定制流水线，AstroFlow 通过切面注入实现 IVOA 溯源模型而无侵入，兼顾产品可追溯与复现。在爱因斯坦探针从 LEIA 到 EP 的迁移中，系统展示从单模块扩展到 12 模块、并接入 FXT 及多条数传链路的通用性。未来这类工作流框架有望成为大型巡天和时域项目的通用底座，进一步结合云原生调度、事件驱动分析和自动化暂现源筛选，提升多载荷、多信使数据融合的科学产出效率。

刊出 2026-02-04 · 收录 2026-08-20

ADS:2026A&C....5501073Z ↗DOI ↗

优先级 75　·　TDE　·　宇宙学与基础物理应用

Tidal Disruption Event Rates across Cosmic Time: Forecasts for LSST, Roman, and JWST and Their Constraints on the Supermassive Black Hole Mass Function

宇宙时间尺度上的潮汐瓦解事件率：对 LSST、Roman 和 JWST 的预测及其对超大质量黑洞质量函数的约束

Mitchell Karmen (Johns Hopkins University), Suvi Gezari (University of Maryland), Colin Norman (Johns Hopkins University), et al.

原文摘要Abstract

Measuring the mass distribution of supermassive black holes (SMBHs) over cosmic time remains particularly challenging for the low-mass (M∙ ≲ 108 M⊙) population at z > 1. This population is also the most sensitive to SMBH seeding and early growth models. In this work, we construct a semiempirical model for the redshift evolution of the tidal disruption event (TDE) rate under multiple SMBH mass function prescriptions, and show that the observed redshift-dependent rate of TDEs is very sensitive to the SMBH mass function and its evolution with redshift. We further incorporate galaxy-scale processes that evolve with redshift—namely, increasing galaxy nuclear stellar densities, enhanced galaxy─galaxy merger rates, dust obscuration, and a possible top-heavy initial mass function at early cosmic times—and quantify their combined impact on the TDE rate. We find that including these effects generally results in a volumetric TDE rate that increases with redshift until a maximum near cosmic noon, before declining at higher redshift, where SMBHs that can disrupt stars become increasingly scarce. We forecast TDE rates in the Rubin Legacy Survey of Space and Time (LSST) and the Roman High Latitude Time Domain Survey, alongside expectations for serendipitous TDE rates in the JWST COSMOS-Web survey. Finally, we provide a methodology for using a flux-limited survey of TDEs in LSST to directly constrain the redshift evolution of the SMBH mass function.

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AI 综述 AI-generated · 以原文为准

亮点

首次系统性地将星系核密度、合并率、尘埃消光及 IMF 演化等红移依赖的星系过程纳入 TDE 率计算；揭示不同 SMBH 质量函数模型在 z>1 的 TDE 率差异可达一个量级，并给出利用 LSST 年探测总数与中值红移直接约束 BHMF 斜率的前景。

脉络与展望

该工作以本地 TDE 光度函数（Yao+ 2023）为起点，结合对比鲜明的 SMBH 质量函数模型（Shankar+ 2009 半经验模型与 Genel+ 2014 Illustris 模拟），并进一步引入星系核密度、合并率及尘埃消光等随红移演化的效应，构建了半经验 TDE 红移演化率模型。相较于早期仅依赖 BHMF 的预测（如 Kochanek 2016），本文发现星系尺度过程在 z∼2 宇宙正午前后显著增强 TDE 率，且不同 BHMF 模型在 z>1 的预测差异可达一个量级。展望未来，LSST 年探测数千 TDE 的流量限制样本，配合 Roman 和 JWST 的高红移覆盖，将能够通过总探测数和样本中值红移直接约束低质量端 SMBH 质量函数的红移演化，为 SMBH 种籽与增长研究提供全新观测窗口。

预印本 2026-02-04 · 接收 2026-06-05 · 刊出 2026-07-14 · 收录 2026-07-22

ADS:2026ApJ..1006...20K ↗arXiv:2602.04947 ↗DOI ↗

0308-20 补录

优先级 70　·　引力波电磁对应体　·　多信使触发与联合　·　高能暂现天体

McFACTS. IV. Electromagnetic Counterparts to AGN-disk-embedded Binary Black Hole Mergers

McFACTS. IV. AGN盘内双黑洞并合的电磁对应体

Emily McPike, Rosalba Perna, K. E. Saavik Ford et al.

原文摘要Abstract

The accretion disks of active galactic nuclei (AGNs) are promising environments for producing binary black hole (BBH) mergers, which have been detected via gravitational waves (GWs) with the LIGO−Virgo−KAGRA (LVK) GW detector network. BBH mergers embedded in AGN disks are unique among GW formation channels in their generic ability to produce electromagnetic (EM) counterparts, via interactions between the merger remnant and the surrounding disk gas (though these are not always observable). While such mergers represent valuable multimessenger sources, the lack of predictive statistical models in existing literature currently limits our ability to select possible EM counterparts with GW detections in archival data and in real time using time-domain surveys such as the Zwicky Transient Facility or LSST. Here we employ the Monte Carlo For AGN Channel Testing and Simulation code (McFACTS, https://www.github.com/mcfacts/mcfacts) to predict the bolometric luminosities of jets and shocks associated with LVK-detectable BBH merger remnants in AGN disks. McFACTS predicts the distribution of GW observables for an underlying black hole population and disk model. In this work we present a new capability that simultaneously generates the distribution of bolometric EM luminosities corresponding to these predicted GW detections. Our results are consistent with current observational surveys and indicate that (i) migration in dense, Sirko─Goodman-like disks preferentially produces EM counterparts from high-mass (<inline-formula> <mml:math><mml:mi>M</mml:mi><mml:mo>≳</mml:mo><mml:mn>40</mml:mn><mml:mspace></mml:mspace><mml:msub><mml:mi>M</mml:mi><mml:mo>⊙</mml:mo></mml:msub></mml:math> </inline-formula>), high-spin remnants across multiple merger generations and (ii) lower chirp mass mergers are more likely to contribute observable counterparts and with shorter emission breakout times in less dense, Thompson─Quataert─Murray-like disks.

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AI 综述 AI-generated · 以原文为准

亮点

首次在 McFACTS 框架中同时生成引力波可探测事件对应的电磁热光度分布；发现密盘（Sirko–Goodman 类）利于高质量、高自旋残余的多代并合电磁对应体，而稀盘（Thompson–Quataert–Murray 类）中低啁啾质量并合更易产生短突破时标的可观测对应体。

脉络与展望

AGN 吸积盘是双黑洞并合的重要可能场所，并合残余与盘气体相互作用使其具有产生电磁对应体的独特潜力；但此前研究多为单事件或半解析估计，缺少可随 LVK 探测同步给出的统计预测。本文在 McFACTS 蒙特卡洛框架内新增电磁热光度生成能力，在给定黑洞族群和盘模型下同时输出引力波可观测量与对应体热光度分布。结果显示盘密度与并合代数对可观测对应体性质有显著区分：Sirko–Goodman 类致密盘偏向大质量、高自旋残余的多代并合，Thompson–Quataert–Murray 类较稀盘则更利于低啁啾质量并合且突破时标更短。这一统计先验可为 ZTF/LSST 等时域巡天的回溯筛选和实时多信使证认提供支撑，未来可进一步耦合巡天深度、谱能量分布和盘外流模型。

预印本 2026-02-04 · 接收 2026-06-25 · 刊出 2026-08-11 · 收录 2026-08-20

ADS:2026ApJ..1007..105M ↗arXiv:2602.04135 ↗DOI ↗

0408-20 补录

优先级 65　·　引力波电磁对应体　·　多信使触发与联合

Intermediate-mass Black Hole Formation from Hierarchical Mergers in Galactic Nuclei

星系核中通过层级并合形成中等质量黑洞

✉ A. Newton (Loyola University Chicago; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University), S. C. Rose (Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University), F. Kıroğlu (Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University) et al.

原文摘要Abstract

Dense stellar environments such as nuclear star clusters (NSCs) can dynamically assemble gravitational wave (GW) sources. We consider a population of single stellar mass black holes (BHs) in the inner 0.1 pc of an NSC surrounding a 4 × 106 M⊙ supermassive black hole (SMBH). Using a semianalytic model, we account for direct collisions between BHs and stars and GW capture between BHs. We explore the effect of the initial BH mass and spin distributions on their final properties and the production of GW sources. Specifically, we consider upper and lower limits for the BH initial mass distribution, and we account for the possibility that a subset of our initial population are the merger products of primordial BH binaries. We find that ∼500 M⊙ intermediate mass black holes (IMBHs) can form for our upper limit mass distribution, while our lower limit mass distribution forms none. Most IMBHs ≳200 M⊙ eventually sink towards the center of the cluster and merge with the SMBH. We also find successive BH─star collisions can produce low-spinning BHs with χ ≲ 0.2. Our results have implications for LIGO-Virgo-KAGRA sources. We find that the overall merger rate depends primarily on the initial BH mass distribution and is ≳10−9 yr−1 per Milky Way─like galaxy for our range of initial conditions. However, primordial binaries can change the number of GW mergers with second and higher generation progenitor BHs by nearly an order of magnitude.

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AI 综述 AI-generated · 以原文为准

亮点

在同一半解析框架中同时纳入黑洞-恒星碰撞和黑洞-黑洞引力波俘获；高质量上限初始条件可形成约500太阳质量中等质量黑洞，且多数大于200太阳质量者最终沉入中央超大质量黑洞，连续恒星碰撞会压低自旋。

脉络与展望

既往对核星团中单黑洞引力波俘获的研究给出了约10^-9 yr^-1量级的并合率，但未细分并合世代与质量/自旋性质 O'Leary+ 2009；Rose 等人的半解析模型建立了黑洞-恒星碰撞与质量增长的框架 Rose+ 2022；Hoang 等人则提供了由 EKL 机制诱发的银心原初双星并合条件，构成本文初始质量与自旋分布的上限 Hoang+ 2018。本文在 Rose 等模型中加入黑洞-黑洞引力波俘获并纳入原初双星并合产物，发现初始质量范围是决定 IMBH 能否形成及并合率的主要因素，且多数 >200 M⊙ 的 IMBH 会沉入 SMBH 成为 EMRI。这表明核星团环境中的层级并合与恒星碰撞可共同把恒星质量黑洞推向中等质量区间，未来需要在更大初始条件空间、双星-单星散射及可变恒星/黑洞密度背景中检验 Liu & Lai 2025。

预印本 2026-02-04 · 接收 2026-06-22 · 刊出 2026-07-24 · 收录 2026-08-20

ADS:2026ApJ..1006..184N ↗arXiv:2602.04176 ↗DOI ↗

边缘相关 2 篇 · 低相关性展开＋

优先级 10　·　引力波电磁对应体　·　多信使触发与联合08-20 补录

Impact of higher-order modes on eccentricity measurement in binary black hole gravitational waves

Tang, Honglue, Yang, Jinzhao, Wang, Baoxiang, et al.

原文摘要Abstract

We investigate the systematic biases in measuring orbital eccentricity for binary black hole (BBH) mergers that arise when higher-order modes (HOMs) of gravitational waves are neglected in waveform modeling. Using Bayesian inference with the state-of-the-art eccentric, spin-aligned, higher-mode effective-one-body model SEOBNRv5EHM, we reanalyze six previously suggested eccentric gravitational-wave events—GW190521, GW190620, GW190701, GW191109, GW200129, and GW200208_222617. Comparing results with its dominant-mode-only counterpart SEOBNRv5E, we find no statistically significant HOM-induced bias in eccentricity for any of these events, including GW190521, whose eccentricity has been debated in the literature. To explore representative parameter regimes vulnerable to HOM omission, we perform a broad zero-noise injection campaign varying detector-frame total mass, mass ratio, eccentricity, inclination, and network SNR. We find that significant systematic biases (<inline-formula><mml:math><mml:msub><mml:mi>∆</mml:mi><mml:mi>e</mml:mi></mml:msub><mml:mo>/</mml:mo><mml:mi>σ</mml:mi><mml:mo>></mml:mo><mml:mn>1</mml:mn></mml:math></inline-formula>) arise predominantly in systems with relatively high total mass (<inline-formula><mml:math><mml:msup><mml:mi>M</mml:mi><mml:mi>det</mml:mi></mml:msup><mml:mo>≳</mml:mo><mml:mn>120</mml:mn><mml:msub><mml:mi>M</mml:mi><mml:mo>⊙</mml:mo></mml:msub></mml:math></inline-formula>), highly asymmetric mass ratios (<inline-formula><mml:math><mml:mi>q</mml:mi><mml:mo>≳</mml:mo><mml:mn>4</mml:mn></mml:math></inline-formula>), large inclinations (<inline-formula><mml:math><mml:msub><mml:mi>θ</mml:mi><mml:mi>JN</mml:mi></mml:msub><mml:mo>≳</mml:mo><mml:mn>3</mml:mn><mml:mn>0</mml:mn><mml:mi>°</mml:mi></mml:math></inline-formula>), and high SNRs (<inline-formula><mml:math><mml:msubsup><mml:mi>ρ</mml:mi><mml:mi>mf</mml:mi><mml:mi>N</mml:mi></mml:msubsup><mml:mo>≍</mml:mo><mml:mn>50</mml:mn></mml:math></inline-formula>). Notably, for quasicircular BBHs with approximately <inline-formula><mml:math><mml:msup><mml:mi>M</mml:mi><mml:mi>det</mml:mi></mml:msup><mml:mo>≳</mml:mo><mml:mn>140</mml:mn><mml:msub><mml:mi>M</mml:mi><mml:mo>⊙</mml:mo></mml:msub></mml:math></inline-formula>, our results suggest that neglecting HOMs may lead to strong false-positive evidence for nonzero eccentricity. By contrast, for lower-mass systems (<inline-formula><mml:math><mml:msup><mml:mi>M</mml:mi><mml:mi>det</mml:mi></mml:msup><mml:mo>∼</mml:mo><mml:mn>100</mml:mn><mml:msub><mml:mi>M</mml:mi><mml:mo>⊙</mml:mo></mml:msub></mml:math></inline-formula>), HOM exclusion produces negligible eccentricity biases. Our results demonstrate that although current eccentric candidates are not impacted by HOM omission, future eccentricity measurements—particularly for relatively massive, asymmetric, or edge-on systems—require HOM-inclusive waveforms to avoid substantial systematic errors.

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高阶模式对双黑洞引力波偏心率测量的影响　·　该研究通过贝叶斯推断和注入实验，发现忽略高阶模式不会显著影响当前候选事件的偏心率测量，但在高质量、高不对称、高倾角和高信噪比系统中会导致系统性偏差，甚至可能对近圆双黑洞产生虚假的偏心率信号。

预印本 2026-02-04 · 刊出 2026-08-10 · 收录 2026-08-20

ADS:2026PhRvD.114d4027T ↗arXiv:2602.04642 ↗DOI ↗

优先级 007-27 补录

The EXoplanet Climate Infrared TElescope (EXCITE): A balloon-borne mission to measure spectroscopic phase curves of transiting hot Jupiters

Rehm, T. D., Altermatt, C., Bernard, L., et al.

原文摘要Abstract

The EXoplanet Climate Infrared TElescope (EXCITE) is a balloon-borne mission dedicated to measuring spectroscopic phase curves of hot Jupiter-type exoplanets. Phase curve measurements can be used to characterize an exoplanet's longitude-dependent atmospheric composition and energy circulation patterns. EXCITE carries a 0.5 m primary mirror and a moderate resolution diffraction-limited spectrograph with spectral coverage from 0.8 to 3.5 μm. EXCITE is designed to fly from a long-duration balloon. EXCITE will observe through the peak of a target's spectral energy distribution and through spectral signatures of hydrogen and carbon-containing molecules. In this paper, we present the science goals of EXCITE, detail the as-built instrument, and discuss its performance during a 2024 engineering flight from Fort Sumner, New Mexico.

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系外行星气候红外望远镜（EXCITE）：一项测量凌星热木星光谱相位曲线的球载任务　·　本文介绍了EXCITE球载望远镜的科学目标、仪器设计及2024年工程飞行性能，用于测量热木星的光谱相位曲线。

预印本 2026-02-04 · 刊出 2026-07-20 · 收录 2026-07-27

ADS:2026RScI...97g4504R ↗arXiv:2602.04840 ↗DOI ↗