星系的天体物理学

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[1] arXiv:2508.04762 [中文pdf, pdf, html, 其他]: 标题：原恒星核心IRAS 16293E中的新生化学复杂性：复杂有机物和氘化甲醇

标题： Nascent chemical complexity in prestellar core IRAS 16293E: complex organics and deuterated methanol

Samantha Scibelli, Maria N. Drozdovskaya, Paola Caselli, Judit Ferrer Asensio, Beatrice Kulterer, Silvia Spezzano, Yuxin Lin, Yancy Shirley

评论： 18页；已接受发表于A&A

主题：星系的天体物理学 (astro-ph.GA) ; 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

预恒星核是低质量（$M$ $\leq$ 几个 M$_\odot$）恒星和行星形成早期的场所，并提供了关于复杂有机分子（COMs）初始化学条件的见解。氘化COMs追踪分子继承和/或再加工的程度，因为在原恒星系统中高氘化表明在预恒星阶段形成COMs时氘化增强。在L1689N分子云中，预恒星核IRAS 16293E位于化学丰富的IRAS 16293-2422 A和B原恒星系统的$90^{"}$东方。 IRAS 16293A、B和E在同一个诞生云内部展示了恒星形成的独特视角，它们都显示出银河系介质中最高的氘化水平之一，其D/H比值有若干个达到太阳的$10^{5}$倍。我们首次研究了最简单的COM——甲醇（CH$_3$OH）在IRAS 16293E中的氘化水平。使用亚利桑那射电天文台（ARO）的12米望远镜，我们针对CH$_2$DOH、CHD$_2$OH、$^{13}$CH$_3$OH以及几种更高复杂度的有机分子（包括乙醛，CH$_3$CHO、甲酸甲酯，HCOOCH$_3$以及二甲醚，CH$_3$OCH$_3$）在3毫米波段的有利跃迁进行观测。后续使用Yebes 40米望远镜的观测在7毫米（Q波段）中提供了额外的跃迁。我们报告了这些复合有机分子和氘化甲醇在预恒星核IRAS 16293E中的首次检测，并利用我们的观测计算激发温度、柱密度和相对丰度比。当将IRAS 16293E与A和B原恒星，以及其它预恒星核、原恒星和彗星67P/丘留莫夫-格拉西缅科进行比较时，发现相对分子比和D/H值之间存在显著相似性。我们的结果支持这样一个观点，即在原恒星阶段预恒星核坍缩和升温时，复合有机分子的化学再加工量是有限的。

Prestellar cores represent early sites of low-mass ($M$ $\leq$ few M$_\odot$) star and planet formation and provide insight into initial chemical conditions of complex organic molecules (COMs). Deuterated COMs trace the degree of molecular inheritance and/or reprocessing, as high deuteration in protostellar systems suggests COMs forming during the prestellar stage when deuteration is enhanced. Within the L1689N molecular cloud, the prestellar core IRAS 16293E sits $90^{"}$ eastward of the chemically-rich IRAS 16293-2422 A and B protostellar system. A unique view of star formation inside a common natal cloud, IRAS 16293A, B, and E all show some of the highest levels of deuteration in the ISM, with a number of D/H ratios $10^{5}$ times higher than Solar. We investigate for the first time the deuteration levels of the simplest COM, methanol (CH$_3$OH), in IRAS 16293E. Using the Arizona Radio Observatory (ARO) 12 m telescope, we target favorable transitions of CH$_2$DOH, CHD$_2$OH, $^{13}$CH$_3$OH, and several higher complexity COMs (including acetaldehyde, CH$_3$CHO, methyl formate, HCOOCH$_3$, and dimethyl ether, CH$_3$OCH$_3$) in the 3 mm band. Follow-up observations with the Yebes 40 m telescope provided additional transitions in the 7 mm (Q-band). We report the first detections of these COMs and deuterated methanol in prestellar core IRAS 16293E and use our observations to calculate excitation temperatures, column densities, and relative abundance ratios. Striking similarities are found between relative molecular ratios and D/H values when comparing IRAS 16293E to the A and B protostars, as well as to a heterogeneous sample of other prestellar cores, protostars, and the comet 67P/Churyumov-Gerasimenko. Our results support the idea that there is a limited amount of chemical reprocessing of COMs when prestellar cores collapse and heat-up during the protostellar phase.
[2] arXiv:2508.04768 [中文pdf, pdf, html, 其他]: 标题：高红移星系中恒星形成的湍流框架

标题： A Turbulent Framework for Star Formation in High-Redshift Galaxies

Guochao Sun, Claude-André Faucher-Giguère, Jonathan Stern

评论： 23页，17图；提交至AAS期刊

主题：星系的天体物理学 (astro-ph.GA)

观测显示，高红移星系的星系形成物理过程与后期时间显著不同。与像银河系这样的大型、稳定的盘状星系相反，高红移星系通常表现出团块状、扰动的形态和爆发式的恒星形成历史。低质量、爆发式星系与高质量、稳定恒星形成星系之间的差异最近已在具有分辨多相星际介质的星系形成模拟中进行了研究。这些模拟研究表明，虽然稳定的盘状星系可以很好地被建模为嵌入在独特热星系晕（CGM）中的“平衡盘”，但爆发式星系更加动态，其恒星形成发生在以暗物质晕尺度延伸的弥散主导介质中，星际介质（ISM）和CGM之间没有清晰的边界。我们开发了一个解析框架，用于建模那些无法 adequately 被建模为平衡盘的爆发式星系中的恒星形成。该框架将低质量晕中的气体近似为连续的、超音速湍流介质，具有大的密度波动。恒星形成发生在大致对数正态密度分布的高密度尾部中。这类似于分子云中湍流恒星形成的模型，但此处应用于内部CGM尺度。通过与FIRE项目中的星系形成模拟进行比较，我们表明该框架可用于理解晕中的恒星形成效率和径向分布。湍流框架明确展示了即使致密气体中的局部效率接近于1，星系平均的瞬时恒星形成效率也可能相对较低。

Observations of distant galaxies suggest that the physics of galaxy formation at high redshifts differs significantly from later times. In contrast to large, steady disk galaxies like the Milky Way, high-redshift galaxies are often characterized by clumpy, disturbed morphologies and bursty star formation histories. These differences between low-mass, bursty galaxies and higher-mass, steady star-forming galaxies have recently been studied in galaxy formation simulations with resolved multiphase ISM. These simulation studies indicate that while steady disk galaxies can be well-modeled as "equilibrium disks" embedded in a distinct, hot CGM, bursty galaxies are much more dynamic and their star formation occurs in a dispersion-dominated medium that extends to halo scales, with no clear boundary between the ISM and the CGM. We develop an analytic framework to model star formation in bursty galaxies that are not adequately modeled as equilibrium disks. The framework approximates the gas in low-mass halos as a continuous, supersonically turbulent medium with large density fluctuations. Star formation occurs locally in the high-density tail of a roughly lognormal density distribution. This is analogous to turbulent models of star formation in molecular clouds, but here applied on inner CGM scales. By comparing with galaxy formation simulations from the FIRE project, we show that this framework can be used to understand star formation efficiencies and radial profiles in halos. The turbulent framework shows explicitly how the instantaneous galaxy-averaged star formation efficiency can be relatively low even if the local efficiency in dense gas approaches unity.
[3] arXiv:2508.04778 [中文pdf, pdf, html, 其他]: 标题： JVLA和VLBA对红移约0.5的合并冷核心CHIPS 1911+4455的研究：幼年AGN和快速恒星形成BCG的射电辐射

标题： JVLA and VLBA study of the merging cool core CHIPS 1911+4455 at z~0.5: radio emission from an infant AGN and from a rapidly star-forming BCG

Francesco Ubertosi, Myriam Gitti, Pasquale Temi, Ewan O'Sullivan, Valeria Olivares, Gerrit Schellenberger, Fabrizio Brighenti, Marcello Giroletti

评论：已接受发表于《天体物理学杂志》；9页，3幅图

主题：星系的天体物理学 (astro-ph.GA)

最近对星系团的研究发现了在非冷却核心和冷却核心系统边界处的特殊案例。虽然这些物体不寻常，但它们可以帮助我们理解最大质量星系团的演化。我们研究了活动星系核（AGN）反馈在合并冷却核心星系团CHIPS 1911+4455（z = 0.485）中最明亮的星系（BCG）中的作用。我们进行了新的多频段（0.3 - 5 GHz）甚长基线阵列（VLBA）和詹斯基甚大阵列（JVLA）观测，覆盖了广泛的尺度（0.01到20 kpc）。我们的分析显示，BCG中的AGN最近苏醒，显示出对称的、长约30 pc的喷流。 AGN的开始可能与之前研究中发现的热气体增强冷却有关。在更大的尺度（10 kpc）上，向南延伸的微弱射电细丝显示出与恒星形成结的显著对齐，因此被解释为与恒星爆发BCG相关的同步辐射发射区域。推断的射电恒星形成率为100 - 155 M$_{\odot}$/yr，与光学/红外的值（140 - 190 M$_{\odot}$/yr）一致。我们的JVLA和VLBA射电研究，结合了以前的X射线/光学/毫米波研究，表明CHIPS 1911+4455代表了星系团演化的过渡阶段，其中中心星系中的AGN刚刚开始对丰富的热气体冷却作出反应。

Recent studies of galaxy clusters found peculiar cases at the boundary between non-cool core and cool core systems. While unusual, these objects can help us understand the evolution of the most massive clusters. We investigated the role of active galactic nucleus (AGN) feedback in the starburst brightest cluster galaxy (BCG) of the merging cool core cluster CHIPS 1911+4455 (z = 0.485). We conducted new multifrequency (0.3 - 5 GHz) Very Long Baseline Array (VLBA) and Jansky Very Large Array (JVLA) observations of CHIPS 1911+4455 across a wide range of scales (0.01 to 20 kpc). Our analysis reveals that the AGN in the BCG has recently awakened, showing a compact core with symmetric, ~30 pc long jets in VLBA data. The onset of the AGN may be linked to the enhanced cooling of the hot gas found in a previous study. At larger scales (10 kpc), faint radio whiskers extending to the south show a striking alignment with star-forming knots and are thus interpreted as synchrotron-emitting regions associated with the starburst BCG. The implied radio star formation rate of 100 - 155 M$_{\odot}$/yr agrees with the optical/infrared one (140 - 190 M$_{\odot}$/yr). Our JVLA and VLBA radio study, informed by previous X-ray/optical/millimeter works, indicates that CHIPS 1911+4455 represents a transitional phase in cluster evolution, where the AGN in the central galaxy has just begun to respond to copious hot gas cooling.
[4] arXiv:2508.04781 [中文pdf, pdf, html, 其他]: 标题：用LMC引起的反射运动限制银河系暗物质晕

标题： Constraining the Milky Way dark matter halo with LMC-induced reflex motion

Rashid Yaaqib, Michael Petersen, Jorge Peñarrubia

评论： 11页，6图

主题：星系的天体物理学 (astro-ph.GA)

模拟银河系晕（MW晕）因大麦云（LMC）的吸积而产生的扰动，为限制我们星系中的暗物质（DM）分布提供了新途径。一个关键的可观测量是银河系盘相对于晕由于LMC吸积引起的反冲运动，这在晕星的动力学中留下速度偶极子。在这里，我们研究偶极子如何随银河中心半径变化，并研究反冲运动信号对不同DM外晕剖面的敏感性。使用一系列截断NFW剖面（$\rho \propto r^{-\beta}$超过$r=50$kpc）的基函数展开（BFE）模拟，我们的$N$-体模型显示，(i) 反冲运动幅度随银河中心半径变化，但对外晕DM斜率不敏感，这意味着MW-LMC质量比本身并不能决定偶极子强度。 (ii) 相反，盘运动方向对外晕DM密度分布非常敏感。 (iii) LMC引力作用引起的MW晕收缩也强烈依赖于外晕DM剖面。 (iv) 我们发现了一种晕不稳定性，其振荡频率随$\beta$增加，产生了一个潜在可观察的特征——晕星平均径向速度的正弦图案。最后，使用BFE系数我们发现，更陡的截断会产生更小的偶极畸变，同时增强四极畸变。这些结果突显了仅靠反冲运动幅度对银河系外晕剖面参数的约束能力有限。

Modelling perturbations of the Milky Way (MW) halo induced by the infall of the Large Magellanic Cloud (LMC) offers new avenues to constrain the dark matter (DM) distribution in our Galaxy. A key observable is the reflex motion of the MW disc with respect to the halo induced by the LMC's infall, which imprints a velocity dipole on kinematics of halo stars. Here we investigate how the dipole varies with Galactocentric radius, and study the sensitivity of the reflex motion signal to different DM outer-halo profiles. Using a suite of basis function expansion (BFE) simulations with truncated NFW profiles ($\rho \propto r^{-\beta}$ beyond $r=50$ kpc), our $N$-body models show that (i) The reflex motion amplitude varies with Galactocentric radius but is largely insensitive to the outer DM slope, implying that the MW-LMC mass ratio alone does not set the dipole strength. (ii) In contrast, the direction of the disc motion is very sensitive to the density distribution of the outer DM halo. (iii) The contraction of the MW halo induced by the LMC's gravitational pull also depends strongly on the outer DM halo profile. (iv) We find a halo instability whose oscillation frequency increases with $\beta$ producing a potentially observable signature - a sinusoidal pattern of the mean radial velocity of halo stars. Finally, using BFE coefficients we find that steeper truncations produce smaller dipole distortions, while amplifying the quadrupole distortion. These results highlight the limited constraining power of the reflex motion amplitude alone for outer MW profile parameters.
[5] arXiv:2508.04791 [中文pdf, pdf, html, 其他]: 标题：星系的物理性质以及从$z\sim6$到$z\sim14$的紫外光度函数在COSMOS-Web中的情况

标题： Physical properties of galaxies and the UV Luminosity Function from $z\sim6$ to $z\sim14$ in COSMOS-Web

Maximilien Franco, Caitlin M. Casey, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Steven L. Finkelstein, Louise Paquereau, Andreas L. Faisst, Anton M. Koekemoer, Michaela Hirschmann, Sebastiano Cantarella, Nicole E. Drakos, Stephen M. Wilkins, Henry Joy McCracken, Jeyhan S. Kartaltepe, Claudia Maraston, Fatemeh Abedini, Mark J. Achenbach, Rafael C. Arango-Toro, Fabrizio Gentile, Ghassem Gozaliasl, Kohei Inayoshi, Darshan Kakkad, Atousa Kalantari, Ali Ahmad Khostovan, Vasily Kokorev, Erini Lambrides, Gavin Leroy, Richard Massey, Bahram Mobasher, Sophie L. Newman, Jason Rhodes, R. Michael Rich, Brant E. Robertson, David B. Sanders, Takumi S. Tanaka, Aswin P. Vijayan, John R. Weaver, Lilan Yang, Si-Yue Yu

评论： 35页，17图，提交至ApJ

主题：星系的天体物理学 (astro-ph.GA)

我们展示了在三个红移区间内从$z\sim5.5$-14 的JWST COSMOS-Web调查中的静止框架紫外线光度函数（UVLF）的测量结果。我们的样本使用HST/ACS F814W、JWST/NIRCam F115W和F150W滤镜的下落技术选择，包含总共3099个星系，覆盖从微弱（$M_{\rm UV}\sim-19$mag）到明亮（$M_{\rm UV}\sim-22.5$mag）的广泛光度范围。这些星系正在进行快速恒星形成，具有蓝色恒星种群。令人惊讶的是，它们的中位紫外线光谱斜率$\beta$在$z>8$时不演化，这表明早期时期尘埃极少，或者尘埃与恒星形成之间存在物理分离。测量的UVLF在亮端（$M_{\rm UV}<-21$mag）相比JWST之前的实测结果和演化Schechter函数的理论预测表现出过量，过量从$z\sim9$开始，并随着向$z\sim12$方向逐渐变得更加显著。我们的分析表明，重现高红移处紫外明亮星系的观测丰度需要物理过程的组合，包括提高的恒星形成效率、星系光度中的中等随机性水平以及最小的尘埃衰减。

We present measurements of the rest-frame ultraviolet luminosity function (UVLF) in three redshift bins over $z\sim5.5$-14 from the JWST COSMOS-Web survey. Our samples, selected using the dropout technique in the HST/ACS F814W, JWST/NIRCam F115W, and F150W filters, contain a total of 3099 galaxies spanning a wide luminosity range from faint ($M_{\rm UV}\sim-19$ mag) to bright ($M_{\rm UV}\sim-22.5$ mag). The galaxies are undergoing rapid star formation, with blue stellar populations. Surprisingly, their median UV spectral slope $\beta$ does not evolve at $z>8$, suggesting minimal dust, or physical separation of dust and star formation at early epochs. The measured UVLF exhibits an excess at the bright-end ($M_{\rm UV}<-21$ mag) compared to pre-JWST empirical results and theoretical predictions of an evolving Schechter function, with the excess beginning at $z\sim9$ and becoming increasingly prominent toward $z\sim12$. Our analysis suggests that reproducing the observed abundance of UV-bright galaxies at high redshift requires a combination of physical processes, including elevated star formation efficiencies, moderate levels of stochasticity in galaxy luminosities, and minimal dust attenuation.
[6] arXiv:2508.04808 [中文pdf, pdf, html, 其他]: 标题：评估半解析模型中再电离方案的准确性

标题： Evaluating the Accuracy of Reionization Prescriptions in Semi-analytic Models of the First Stars and Galaxies

Thomas Behling, Ryan Hazlett, Mihir Kulkarni, Eli Visbal

评论： 15页，5张图，准备提交给JCAP

主题：星系的天体物理学 (astro-ph.GA) ; 宇宙学与非星系天体物理学 (astro-ph.CO)

半解析模型是研究第一代恒星和星系的宝贵工具。它们的数值效率使得在大体积和红移范围内调查广泛的天体物理参数空间成为可能。在这些模型中，跟踪再电离过程是必要的，因为由于气体的光致加热，电离区域中的恒星形成会被抑制。在这里，我们通过将三种半解析再电离描述（两种之前开发的和一种新的模型）的三维电离泡分布与Renaissance流体动力学宇宙辐射转移模拟进行比较，来评估它们的准确性。我们发现，先前存在的模型能够准确确定我们在${\sim}6$共动兆秒差距模拟箱内较大泡的分布，但这些模型未能考虑致密丝状结构中的自屏蔽中性气体。因此，这些描述在一定程度上高估了受再电离反馈影响的晕中星系的比例，最多可达一个数量级（取决于晕的质量和红移）。这导致了再电离反馈对第三星族恒星和低质量金属增丰星系的不现实的强烈影响。我们新开发的模型考虑了宇宙网的密度结构，从而在发现的位于电离区域的晕的比例方面与Renaissance取得了良好的一致。

Semi-analytic models are a valuable tool to study the first stars and galaxies. Their numerical efficiency makes it possible to survey broad regions of astrophysical parameter space across large volumes and redshift ranges. Following reionization in these models is necessary since star formation is suppressed in ionized regions due to photoheating of the gas. Here we evaluate the accuracy of three semi-analytic reionization prescriptions (two previously developed and one new model) by comparing their three-dimensional distribution of ionized bubbles to the Renaissance hydrodynamical cosmological radiative transfer simulations. We find that the previously existing models accurately determine the distribution of the larger bubbles within our ${\sim}6$ comoving Mpc simulation box, but that these models fail to take into account self-shielded neutral gas in dense filaments. Thus, these prescriptions overestimate the fraction of halos in HII regions impacted by reionization feedback by up to an order of magnitude (depending on halo mass and redshift). This leads to an unrealistically large effect of reionization feedback on Pop III stars and low-mass metal-enriched galaxies. Our newly developed model takes into account the density structure of the cosmic web, leading to good agreement with Renaissance in the fraction of halos found in ionized regions.
[7] arXiv:2508.04907 [中文pdf, pdf, html, 其他]: 标题： AGN反馈模型与AGN人口统计学I：EAGLE、SIMBA和TNG100中的射电模式AGN与观测结果不一致

标题： AGN Feedback Models and AGN Demographics I: Radio-Mode AGN in EAGLE, SIMBA and TNG100 are Inconsistent with Observations

Arjun Suresh, Michael R. Blanton, Douglas Rennehan

主题：星系的天体物理学 (astro-ph.GA)

我们比较了活动星系核（AGN）在低红移时如何填充宿主星系的预测与观测结果，发现宇宙学模拟预测与观测模式之间存在显著差异。现代宇宙学模拟包含了旨在重现观测到的星系恒星质量函数的AGN反馈模型。然而，由于对AGN反馈物理机制缺乏真正的理解，这些模型在不同模拟中存在显著差异。为了区分这些模型并可能测试基本物理机制，我们对这些模型进行了独立测试。在之前的研究中，我们发现$F_{\rm AGN}$—— 拥有爱丁顿比率$\lambda > 10^{-3}$的射电AGN宿主星系的观测完整度修正比例 —— 是宿主星系恒星质量（$M_\star$）的强函数，但在固定$M_\star$的情况下几乎与宿主特定恒星形成率（sSFR）无关。在本研究中，我们通过将EAGLE、SIMBA和TNG100模拟的射电模式AGN反馈模型对$F_{\rm AGN} \left(M_\star \right)$的预测与我们的观测约束进行比较，测试了这些模型。我们发现，这些模拟中的任何一个都无法定性地再现$F_{\rm AGN}$对$M_\star$和sSFR的观测依赖关系。最后，我们发现尽管给定的TNG100模型可以进行修改以更好地再现观测到的$F_{\rm AGN}$趋势，但这种修改可能会改变其对本地恒星质量函数和恒星形成率的预测——这些是最初用于校准模拟的关键观测数据。我们的研究结果突显了迫切需要重新审视EAGLE、SIMBA、TNG100和其他类似模型中的活动星系核反馈方案。

We compare predictions of how Active Galactic Nuclei (AGN) populate host galaxies at low redshifts to observations, finding large discrepancies between cosmological simulation predictions and observed patterns. Modern cosmological simulations include AGN feedback models tuned to reproduce the observed galaxy stellar mass function. However, due to a lack of real understanding of the physics of AGN feedback, these models vary significantly across simulations. To distinguish between the models and potentially test the underlying physics, we carry out independent tests of these models. In an earlier study, we found that $F_{\rm AGN}$ -- the observed completeness-corrected fraction of galaxies hosting radio AGN with an Eddington ratio $\lambda > 10^{-3}$ -- to be a strong function of host galaxy stellar mass ($M_\star$) but nearly independent of host specific star formation rates (sSFR) at fixed $M_\star$. In this study, we test the radio mode AGN feedback models of the EAGLE, SIMBA, and TNG100 simulations by comparing their predictions of $F_{\rm AGN} \left(M_\star \right)$ to our observational constraint. We find that none of these simulations even qualitatively reproduce the observed dependencies of $F_{\rm AGN}$ on $M_\star$ and sSFR. Finally, we find that although the given TNG100 model could be modified in order to better reproduce the observed $F_{\rm AGN}$ trend, this modification would likely also change its prediction for the local stellar mass function and star formation rates -- key observations used for calibrating the simulation in the first place. Our findings highlight a pressing need to revisit the AGN feedback prescriptions in EAGLE, SIMBA, TNG100 and other similar models.
[8] arXiv:2508.04989 [中文pdf, pdf, html, 其他]: 标题：通过光学和红外观测研究演化后的富碳星云中的尘埃和多环芳烃化学

标题： Probing Dust and PAH Chemistry in Evolved Carbon-Rich Nebulae through Optical and Infrared Observations

Rahul Kumar Anand, Atul Kumar Singh, Saurabh Sharma, Brijesh Kumar, Shantanu Rastogi

主题：星系的天体物理学 (astro-ph.GA) ; 太阳与恒星天体物理学 (astro-ph.SR)

本研究提供了光学和近红外光度观测数据，以及来自ISO SWS仪器的中红外光谱数据，以检查芳香红外带（AIB）特征与富碳演化恒星光学性质之间的潜在相关性。识别此类相关性可以为低至中等质量恒星在渐近巨星分支（AGB）阶段之后的演化路径提供有价值的约束。对五个著名的富碳天体在不同后AGB或行星状星云（PN）阶段进行了U、B、V、R、I、J、H、K和L波段的光度测量：CRL 2688，PN M 2-43，NGC 7027，BD${+}$30${^\circ}$3639，以及AFGL 2132。我们的分析显示，所有五个天体都表现出显著的AIB特征；然而，它们的光谱轮廓显示出明显的差异。这些差异归因于周围星际物质的化学组成和物理条件的变化。特别是，3.28$\mu$m多环芳烃（PAH）特征在除AFGL 2132以外的所有天体中都被检测到，这表明其附近可能有不同的PAH种群或环境条件。尽管这些源具有大致相似的演化阶段，但观察到的AIB特征的多样性突显了其周围星际环境的复杂性和异质性。

This study presents optical and near-infrared photometric observations, alongside mid-infrared spectroscopic data from the ISO SWS instrument, to examine potential correlations between Aromatic Infrared Band (AIB) features and the optical properties of carbon-rich evolved stars. Identifying such correlations can provide valuable constraints on the evolutionary pathways of low- to intermediate-mass stars beyond the asymptotic giant branch (AGB) phase. Photometric measurements in the U, B, V, R, I, J, H, K, and L bands were obtained for five well-known carbon-rich objects at various post-AGB or planetary nebula (PN) stages: CRL 2688, PN M 2-43, NGC 7027, BD${+}$30${^\circ}$3639, and AFGL 2132. Our analysis reveals that all five objects exhibit prominent AIB features; however, their spectral profiles show notable variation. These differences are attributed to variations in the chemical composition and physical conditions of the surrounding circumstellar material. In particular, the 3.28$\mu$m polycyclic aromatic hydrocarbon (PAH) feature is detected in all objects except AFGL 2132, indicating a potentially distinct PAH population or environmental condition in its vicinity. Although these sources share broadly similar evolutionary stages, the observed diversity in AIB characteristics underscores the complexity and heterogeneity of their circumstellar environments.
[9] arXiv:2508.05052 [中文pdf, pdf, html, 其他]: 标题： Lyman-Alpha发射体在$3 \lesssim z < 7$之间的尺寸演化及其尺寸-质量关系，由JWST观测到的情况

标题： The Size Evolution and the Size-Mass Relation of Lyman-Alpha Emitters across $3 \lesssim z < 7$ as Observed by JWST

Qi Song, F. S. Liu, Jian Ren, Pinsong Zhao, Qifan Cui, Yubin Li, Hao Mo, Yuchong Luo, Guanghuan Wang, Nan Li, Hassen M. Yesuf, Weichen Wang, Xin Zhang, Xianmin Meng, Mingxiang Fu, Bingqing Zhang, Chenxiaoji Ling

评论： 16页，10图，2表。欢迎提出意见

主题：星系的天体物理学 (astro-ph.GA)

理解莱曼-α发射体（LAEs）的形态结构对于揭示它们的形成路径和莱曼-α$\alpha$发射的物理起源至关重要。然而，它们的大小演化和结构比例关系仍存在争议。在本研究中，我们分析了一个大样本的 876个光谱确认的LAEs在$3 \lesssim z < 7$，这些LAEs选自GOODS-S、UDS和COSMOS区域的MUSE、VANDELS和CANDELSz7调查。利用詹姆斯·韦布空间望远镜（JWST）的深度高分辨率近红外图像，我们通过二维Sérsic轮廓拟合测量了它们的静止框架紫外和光学V波段有效半径（$R_{\rm e}$）。我们的结果表明，这些LAEs通常较为紧凑，大小演化较弱，分别遵循$R_{\rm e,UV} \propto (1 + z)^{-0.91 \pm 0.10}$和$R_{\rm e,V} \propto (1 + z)^{-0.93 \pm 0.18}$。它们的紫外和光学尺寸在统计上是可比较的，表明紫外到光学的颜色梯度可以忽略不计。首次，我们在$z>3$建立了LAEs的静止框架光学尺寸-质量关系，发现其斜率与典型星系形成星系（SFGs）相当，但在给定恒星质量下尺寸稍小。这些结果为理解早期宇宙中LAEs的形成机制和结构演化提供了重要线索。

Understanding the morphological structures of Lyman-alpha emitters (LAEs) is crucial for unveiling their formation pathways and the physical origins of Ly$\alpha$ emission. However, the evolution of their sizes and structural scaling relations remains debated. In this study, we analyze a large sample of 876 spectroscopically confirmed LAEs at $3 \lesssim z < 7$, selected from the MUSE, VANDELS, and CANDELSz7 surveys in the GOODS-S, UDS, and COSMOS fields. Utilizing deep, high-resolution near-infrared images from the James Webb Space Telescope (JWST), we measure their rest-frame UV and optical V-band effective radii ($R_{\rm e}$) through two-dimensional S\'{e}rsic profile fitting. Our results show that these LAEs are generally compact with weak size evolution, following $R_{\rm e,UV} \propto (1 + z)^{-0.91 \pm 0.10}$ and $R_{\rm e,V} \propto (1 + z)^{-0.93 \pm 0.18}$, respectively. Their UV and optical sizes are statistically comparable, indicating negligible UV-to-optical color gradients. For the first time, we establish the rest-frame optical size-mass relation for LAEs at $z>3$, finding slopes comparable to typical star-forming galaxies (SFGs), but with slightly smaller sizes at a given stellar mass. These results provide important clues for understanding the formation mechanisms and structural evolution of LAEs in the early universe.
[10] arXiv:2508.05151 [中文pdf, pdf, html, 其他]: 标题：超新星遗迹碰撞的实验室模拟：对触发恒星形成的影响

标题： Laboratory Modeling of Supernova Remnants Collisions: Implications for Triggered Star Formation

Marin Fontaine, Clotilde Busschaert, Émeric Falize

评论：提交至《天体物理杂志》

主题：星系的天体物理学 (astro-ph.GA) ; 高能天体物理现象 (astro-ph.HE) ; 太阳与恒星天体物理学 (astro-ph.SR)

理论上的恒星形成模型一直低估了天文学调查中观察到的速率。恒星在巨大的分子云中形成，这些云在湍流、磁场、辐射和引力的共同影响下分裂成致密的云块。虽然其中一些云块会自发坍缩，但其他云块则需要外部触发，这种机制估计占像象鼻星云这样的区域中恒星形成率的14-25%。实验室天体物理学已成为研究此类触发过程的强大方法，特别是涉及超新星遗迹（SNRs）的过程。最近的实验，在已建立的尺度定律指导下，成功再现了SNRs的动力学及其与致密云块或其他SNRs的相互作用。在本工作中，我们使用三维辐射流体力学代码TROLL对这些实验配置进行了全面的数值研究。模拟提供了对基本物理机制的深入理解，准确再现了关键的实验现象，并为分析模型提供了有价值的比较。这项研究强调了实验室实验与数值模拟之间的强大协同作用，为实验室天体物理学的未来发展奠定了坚实的基础。此外，我们提出了一种新的实验装置，该装置为DEM L316系统中观察到的不对称碰撞提供了改进的尺度。我们的研究结果还表明，密集环境中的SNR碰撞可以降低致密云块的引力稳定性，从而促进其坍缩并可能触发恒星形成。

Theoretical models of star formation consistently underestimate the rates observed in astronomical surveys. Stars form within giant molecular clouds, which fragment into dense clumps under the combined influences of turbulence, magnetic fields, radiation and gravity. While some of these clumps collapse spontaneously, others require an external trigger, a mechanism estimated to account for 14-25% of star formation in regions such as the Elephant Trunk Nebula. Laboratory astrophysics has emerged as a powerful approach for investigating such triggering processes, particularly those involving supernova remnants (SNRs). Recent experiments, guided by well-established scaling laws, have successfully replicated the dynamics of SNRs and their interactions with dense clumps or other SNRs. In this work, we present a comprehensive numerical study of these experimental configurations using the 3D radiation-hydrodynamics code TROLL. The simulations provide enhanced insight into the underlying physical mechanisms, accurately reproduce key experimental phenomena and offer valuable comparisons with analytical models. This study underscores the strong synergy between laboratory experiments and numerical simulations, laying a robust foundation for future advancements in laboratory astrophysics. Furthermore, we propose a new experimental setup that offers improved scaling for the asymmetric collision observed in the DEM L316 system. Our findings also show that SNR collisions in dense environments can decrease the gravitational stability of dense clumps, thereby promoting their collapse and potentially triggering star formation.
[11] arXiv:2508.05296 [中文pdf, pdf, html, 其他]: 标题： DAWN. I. 使用Phantom N-Body模拟恒星团的形成和早期演化

标题： DAWN. I. Simulating the formation and early evolution of stellar clusters with Phantom N-Body

Yann Bernard, Estelle Moraux, Daniel J. Price, Frédérique Motte, Fabien Louvet, Isabelle Joncour

主题：星系的天体物理学 (astro-ph.GA) ; 天体物理学的仪器与方法 (astro-ph.IM) ; 太阳与恒星天体物理学 (astro-ph.SR)

上下文。由于年轻恒星与其周围气体之间的强耦合，以及长度和时间尺度的广泛范围，在分子云环境中模拟恒星动力学在数值上具有挑战性。目标。本文是旨在研究恒星形成区域中复杂早期恒星动力学的一系列论文的第一篇。我们提出了一种新的模拟框架，这是生成更大一组模拟的关键，从而实现统计分析。方法。来自恒星动力学领域的方法，包括正则化和减速方法（SDAR），已被添加到流体动力学代码Phantom中，以产生嵌入星团早期动力学的模拟。这通过一种新的恒星形成方案来完成，该方案以较低的数值成本初始化恒星，但以与气体分布一致的方式进行。最后，添加了H ii区扩展的方案来模拟气体去除。结果。我们运行了测试用例模拟，跟踪了从云坍缩到几百万年后的恒星团的动力学演化。我们的新数值方法通过加快计算来履行其功能。我们新实现的N体动力学从未成为瓶颈。我们的首次模拟表明，大质量恒星对恒星形成过程有显著影响，并塑造了结果星团的动力学。根据这些大质量恒星的位置及其反馈的强度，它们可以提前拆解部分云团或触发第二次云坍缩事件，优先形成低质量恒星。这种随机行为证实了进行统计研究的必要性。结论。我们的新Phantom N-Body框架实现了对星团形成和演化的高效模拟。它提供了构建嵌入星团动力学演化模型所需的统计分析。

Context. Simulating stellar dynamics in a molecular cloud environment is numerically challenging due to the strong coupling between young stars and their surrounding gas, and the large range of length and time scales. Aims. This paper is the first of a suite aimed at investigating the complex early stellar dynamics in star-forming regions. We present a new simulation framework which is the key to generating a larger set of simulations, enabling statistical analysis. Methods. Methods originating from the stellar dynamics community, including regularisation and slowdown methods (SDAR), have been added to the hydrodynamical code Phantom to produce simulations of embedded cluster early dynamics. This is completed by a novel prescription of star formation to initialise stars with a low numerical cost, but in a way that is consistent with the gas distribution. Finally, a prescription for H ii region expansion has been added to model the gas removal. Results. We have run testcase simulations following the dynamical evolution of stellar clusters from the cloud collapse to a few Myr. Our new numerical methods fulfil their function by speeding up the calculation. The N-body dynamics with our novel implementation never appear as a bottleneck. Our first simulations show that massive stars largely impact the star formation process and shape the dynamics of the resulting cluster. Depending on the position of these massive stars and the strength of their feedback, they can prematurely dismantle part of the cloud or trigger a second event of cloud collapse, preferentially forming low-mass stars. This stochastic behaviour confirms the need for statistical studies. Conclusions. Our new Phantom N-Body framework enables efficient simulation of the formation and evolution of star clusters. It enables the statistical analysis needed to build models of the dynamical evolution of embedded star clusters.
[12] arXiv:2508.05335 [中文pdf, pdf, html, 其他]: 标题： z~2-3范围内的空间分辨气相金属量与JWST/NIRISS

标题： Spatially resolved gas-phase metallicity at z~2-3 with JWST/NIRISS

Ayan Acharyya, Peter J. Watson, Benedetta Vulcani, Tommaso Treu, Kalina V. Nedkova, Andrew J. Bunker, Vihang Mehta, Hakim Atek, Andrew J. Battisti, Farhanul Hasan, Matthew J. Hayes, Mason Huberty, Tucker Jones, Nicha Leethochawalit, Yu-Heng Lin, Matthew A. Malkan, Benjamin Metha, Themiya Nanayakkara, Marc Rafelski, Zahra Sattari, Claudia Scarlata, Xin Wang, Caitlin M. Casey, Andrea Grazian, Anton M. Koekemoer, Mario Radovich, Giulia Rodighiero

评论： 15页，10图，2表。已投稿至A&A

主题：星系的天体物理学 (astro-ph.GA)

空间分辨的气相金属丰度图是理解星系化学演化的重要组成部分。我们展示了从NIRISS/WFSS观测中获得的空间分辨金属丰度图。这是首次展示多个单独星系的研究。我们对八个星系样本进行了研究——四个来自JWST-PASSAGE，四个来自GLASS-JWST ERS，从空间分辨的角度探讨电离源、金属丰度及其与恒星形成的关系。除了一个星系外，其余所有星系都在红移范围$1.9 \leq z \leq 2$内，该异常星系位于$z = 3.1$。我们的样本涵盖了恒星质量范围为$8.0 <$ \logM $< 9.5$ ，星形成率（SFR）为$0.2 <$$\log{\rm{(SFR}}$/\Msunpyr )$< 1.1$，以及整体金属量为$7.8 <$\logOH $< 9.0$ 的范围。为了解决在缺乏解析的\halpha 的情况下 SF-AGN 分界的问题，我们提出了一条新的 SF 分界线，在\textit{OHNO}参数空间中，该线基于公开可用的 MAPPINGS v5.1\hii 区域模型网格。我们展示了样本的质量-金属丰度梯度关系，该关系与恒星质量没有明显趋势，可能暗示高$z$星系尚未开始其吸积主导阶段。通过将空间解析的金属丰度与 SFR 图之间的相关性解释为星系中金属传输有效时间尺度的代理，我们发现了一个较弱的趋势，即这种时间尺度随着恒星质量的增加而增加，这意味着低质量星系中的反馈更有效。

Spatially resolved gas-phase metallicity maps are a crucial element in understanding the chemical evolution of galaxies. We present spatially resolved metallicity maps obtained from NIRISS/WFSS observations. This is the first such work presenting multiple individual galaxies. We investigate the source of ionisation, metallicity and its relation to star-formation in a spatially-resolved sense for a sample of eight galaxies -- four from JWST-PASSAGE and four from GLASS-JWST ERS. All but one galaxy are in the redshift range $1.9 \leq z \leq 2$, the outlier being at $z = 3.1$. Our sample covers a range of $8.0 <$ \logM $< 9.5$ in stellar mass, $0.2 <$ $\log{\rm{(SFR}}$/\Msunpyr) $< 1.1$ in star-formation rate (SFR) and $7.8 <$ \logOH $< 9.0$ in global metallicity. As a solution to the challenge of SF-AGN demarcation in absence of resolved \halpha, we present a new SF-demarcation line in the \textit{OHNO} parameter space based on MAPPINGS v5.1 publicly available \hii region model grids. We present the mass-metallicity gradient relation for our sample, which showed no clear trend with stellar mass, perhaps hinting at the fact that the high-$z$ galaxies have not yet started their accretion dominated phase. By interpreting the correlation between spatially resolved metallicity and SFR maps as a proxy for effective timescales of metal-transport in galaxies, we find a weak trend such that this timescale increases with stellar mass, implying a more effective feedback in lower mass galaxies.
[13] arXiv:2508.05397 [中文pdf, pdf, html, 其他]: 标题：活动星系核的金属丰度来自紫外和光学发射线-II. 重新审视$C43$金属丰度校准及其意义

标题： Metallicity of Active Galactic Nuclei from ultraviolet and optical emission lines-II. Revisiting the $C43$ metallicity calibration and its implications

O. L. Dors, C. B. Oliveira, M. V. Cardaci, G. F. Hägele, Mark Armah, R. A. Riffel, L. Ramos Vieira, G. C. Almeida, I. N. Morais, P. C. Santos

评论： 16页，10图，即将发表于MNRAS

主题：星系的天体物理学 (astro-ph.GA)

在本研究中，提出了一种新的半经验校准，将类型~2活动星系核的紫外发射线（\ion{C}{iii}]$\lambda1909$，\ion{C}{iv}$\lambda1549$ ，\ion{He}{ii}]$\lambda1640$）与其金属度（$Z$）联系起来。这种标定是通过将大量106个天体（数据来自文献）在较宽的红移范围（$0 \: \lesssim \: z \: \lesssim \: 4.0$）进行比较得出的，这些天体与采用最近通过$T_{\rm e}$方法估算得到的C/O-O/H关系的光致电离模型预测结果进行比较，该方法被认为是目前最可靠的方法。我们发现新的标定产生的$Z$值与其他标定以及通过$T_{\rm e}$方法估算的结果在不确定度为$\pm 0.1$dex范围内一致。我们还发现，活动星系核金属丰度在早期时期就已经较高，在红移范围$0 \: \lesssim \: z \: \lesssim \: 12$内没有单调演化的证据。值得注意的是，我们样本中最高的金属丰度，达到$\rm 4\: Z_{\odot}$，出现在对象位于$2 \lesssim z \lesssim 3$的位置。这个红移范围与宇宙恒星形成率历史的峰值相吻合，表明活动星系核宿主星系中恒星形成的主要时期、黑洞增长和快速金属增丰之间存在强关联。此外，我们的分析显示AGN金属丰度与射电特性（射电光谱指数或射电光度）或宿主星系恒星质量之间没有显著相关性。缺乏明确的质量-金属丰度关系，与本地AGN的研究结果一致，表明核区气体的化学演化与宿主星系的整体特性脱钩。

In this study, a new semi-empirical calibration is proposed between ultraviolet emission lines (\ion{C}{iii}]$\lambda1909$, \ion{C}{iv}$\lambda1549$, \ion{He}{ii}]$\lambda1640$) of type~2 AGNs and their metallicity ($Z$). This calibration is derived by comparing a large sample of 106 objects (data taken from the literature) located over a wide range of redshifts ($0 \: \lesssim \: z \: \lesssim \: 4.0$) with predictions from photoionization models that adopt a recent C/O-O/H relation derived via estimates using the $T_{\rm e}$ method, which is considered the most reliable method. We found that the new calibration produces $Z$ values in agreement (within an uncertainty of $\pm 0.1$ dex) with those from other calibrations and from estimates via the $T_{\rm e}$-method. We find also that AGN metallicities are already high at early epochs, with no evidence for monotonic evolution across the redshift range $0 \: \lesssim \: z \: \lesssim \: 12$. Notably, the highest metallicities in our sample, reaching up to $\rm 4\: Z_{\odot}$, are found in objects at $2 \lesssim z \lesssim 3$. This redshift range coincides with the peak of the cosmic star formation rate history, suggesting a strong connection between the major epoch of star formation, black hole growth, and rapid metal enrichment in the host galaxies of AGNs. Furthermore, our analysis reveals no significant correlation between AGN metallicity and radio properties (radio spectral index or radio luminosity) or host galaxy stellar mass. The lack of a clear mass-metallicity relation, consistent with findings for local AGNs, suggests that the chemical evolution of the nuclear gas is decoupled from the global properties of the host galaxy.
[14] arXiv:2508.05450 [中文pdf, pdf, html, 其他]: 标题： 4.7 GHz激发OH脉泽的圆偏振首次检测

标题： First detection of circular polarization in 4.7 GHz excited OH masers

Derck P Smits, Paul Fallon

评论： 16页，6图，4表，已接受发表于《天体物理杂志》

主题：星系的天体物理学 (astro-ph.GA)

我们报告了使用格林班克100米望远镜进行完整的斯托克斯测量首次在4.7 GHz激发的OH脉泽中检测到圆偏振。两个圆偏振成分之间的泽曼位移提供了这些脉泽斑点中磁场所致的测量值。三种不同的方法用于确定右圆偏振和左圆偏振成分之间的速度位移。我们发现场强为$B \sim 100$mG，使用存档的分子参数，这些参数精度有限且值不确定。讨论了使用1.7和6.0 GHz OH脉泽来估计恒星形成区域磁场的保留意见。

We report the first detection of circular polarization in 4.7 GHz excited OH masers in star-forming regions made using full Stokes measurements with the Green Bank 100m telescope. The Zeeman shift between the two circular components provides a measure of the magnetic field pervading these maser spots. Three different methods are used to determine the shift in velocity between the Right Circular Polarization and Left Circular Polarization components. We find fields with $B \sim 100$ mG using archival molecular parameters that have limited precision and uncertain values. Reservations of using 1.7 and 6.0 GHz OH masers to estimate magnetic fields in star-forming regions are discussed.
[15] arXiv:2508.05596 [中文pdf, pdf, html, 其他]: 标题：长周期变星在NGC 147和NGC 185-II中。它们的尘埃生成

标题： Long-period variable stars in NGC 147 and NGC 185-II. Their dust production

Hamidreza Mahani, Atefeh Javadi, Jacco van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh

评论：已接受发表于ApJ

主题：星系的天体物理学 (astro-ph.GA) ; 太阳与恒星天体物理学 (astro-ph.SR)

本研究对矮星系NGC 147和NGC 185中的质量损失率和尘埃生成率进行了比较分析，重点研究长周期变星（LPVs）和脉动渐近巨星分支（AGB）恒星作为尘埃反馈进入星际介质的主要指标。对于NGC 147，总质量损失率为$(9.44 \pm 3.78) \times 10^{-4} M_{sun} yr^{-1}$，LPV光度范围为$(6.20 \pm 0.25) \times 10^{2} L_\odot$到$( 7.87 \pm 0.32) \times 10^{3} L_\odot $。在NGC 185中，总质量损失率更高，为$(1.58 \pm 0.63) \times 10^{-3} M_{sun} yr^{-1}$，LPV光度范围为$ (5.68 \pm 0.23) \times 10^{2} L_\odot $到$(1.54 \pm 0.66) \times 10^{4} L_\odot$。观察到恒星光度、由于包层尘埃自消光引起的固有红化以及升高的质量损失率之间存在正相关性。此外，计算的尘埃注入率、二维尘埃分布图和观测到的尘埃质量之间的比较提供了NGC 147与仙女座星系之间存在引力相互作用的证据，这影响了系统内的尘埃分布。

This study presents a comparative analysis of mass-loss and dust-production rates in the dwarf galaxies NGC 147 and NGC 185, focusing on long-period variables (LPVs) and pulsating asymptotic giant branch (AGB) stars as primary indicators of dust feedback into the interstellar medium. For NGC 147, the total mass-loss rate is calculated as $(9.44 \pm 3.78) \times 10^{-4} M_{sun} yr^{-1}$, with LPV luminosities ranging from $(6.20 \pm 0.25) \times 10^{2} L_\odot$ to $( 7.87 \pm 0.32) \times 10^{3} L_\odot $. In NGC 185, the total mass-loss rate is higher, at $(1.58 \pm 0.63) \times 10^{-3} M_{sun} yr^{-1}$, with LPV luminosities spanning $ (5.68 \pm 0.23) \times 10^{2} L_\odot $ to $(1.54 \pm 0.66) \times 10^{4} L_\odot$. A positive correlation is observed between stellar luminosity, intrinsic reddening due to circumstellar dust self-extinction, and elevated mass-loss rates. Additionally, comparisons of calculated dust injection rates, two-dimensional dust distribution maps, and observed dust masses provide evidence for a gravitational interaction between NGC 147 and the Andromeda galaxy, which influences the dust distribution within the system.

[16] arXiv:2508.03409 (交叉列表自 physics.hist-ph) [中文pdf, pdf, html, 其他]: 标题：科内利斯·伊斯顿：银河系作为螺旋星系

标题： Cornelis Easton:The Milky Way as a spiral galaxy

Pieter C. van der Kruit (Kapteyn Astronomical Institute, University of Groningen, the Netherlands)

评论：被《天文学历史与遗产杂志》接受发表。要查看高分辨率图表的版本，请访问 www.astro.rug.nl/~vdkruit/CEaston.pdf

主题：物理的历史与哲学 (physics.hist-ph)

科内利斯·伊斯特恩（1864-1929）成为了一名记者和报纸编辑。在他职业生涯的大部分时间里，他作为一名业余天文学家活跃，并在国际天文期刊上发表了重要的论文。这涉及三个领域。第一个是绘制银河系。他于1893年出版的书籍《北半球的银河》，引起了一些关注。除了有银河系表面亮度的插图外，还包含了对结构特征的详细描述和讨论，以及对所有曾经发表过的关于银河系内容的全面、基本上完整的列表和讨论。后来他制作了一张等照度图，并使用照片来改进地图。伊斯特恩曾想到他所看到的实际上是一个螺旋星云，但此时是侧面对着我们。考虑到明亮和黑暗区域，他提出了银河系系统中螺旋结构的形式，中心位于天鹅座的方向。他在1900年和1913年发表在《天体物理学杂志》上的关于银河系理论的论文引起了广泛关注，尽管包括雅各布斯·卡普坦在内的许多天文学家仍持有一些保留意见。第三个领域涉及恒星表面密度与银河系表面亮度之间的相关性。伊斯特恩认为对于相对较亮的恒星存在这种相关性。T 有一篇伊斯特恩未能在他的出版物列表中包含的出版物，即一篇1894年发表在《自然》上的短文。仙女座星云的椭圆伴星NGC205在1874年至1889年间旋转了15度。等照度线的扭曲导致了表观旋转。1903年，卡普坦和格罗宁根大学授予伊斯特恩荣誉博士学位。

Cornelis Easton (1864-1929) became a journalist and newspaper editor. During most of his career he was active as an amateur astronomer and contributed important papers in international astronomical journals This concerned three areas. The first was mapping the Milky Way. The book, La Voie Lactee dans l'hemisphere boreal, which he published in 1893, made some impression. Since it had in addition to drawings of the surface brightness of the Milky Way, also extensive descriptions and discussions of features in the structure and a comprehensive, essentially complete, listing and discussion on everything that had ever been published on the Milky Way. Later he produce an isophotal chart and used photographs to improve the map. Easton had been struck by the idea that what he saw was actually a spiral nebula, but then seen edge-on. Considering bright and dark areas he proposed a form for the spiral in the Milky Way System with the center in the direction of the constellation Cygnus. His publications on this Theory of the Milky Way in the Astrophysical Journal in 1900 and 1913 drew much attention, although many astronomers, including Jacobus Kapteyn, kept quite some reservations. The third area concerned correlations between surface densities of stars and surface brightness of the Milky Way. Easton maintained that there was such a correlation for relatively bright stars. T There is a publication Easton failed to include in his list of his publications, namely an 1894 short article in Nature. The elliptical companion NGC205 of the Andromeda Nebula between had on in 1874 and 1889 rotated by 15 degrees. Isophote twists are responsible for the apparent rotation. In 1903 Kapteyn and the University of Groningen bestowed an honorary doctorate upon Easton.
[17] arXiv:2508.04862 (交叉列表自 astro-ph.HE) [中文pdf, pdf, html, 其他]: 标题：从人马座A分子复合体反射的X射线辐射的偏振：多个耀斑，多个源？

标题： Polarization of reflected X-ray emission from Sgr A molecular complex: multiple flares, multiple sources?

Ildar Khabibullin, Eugene Churazov, Riccardo Ferrazzoli, Philip Kaaret, Jeffery J. Kolodziejczak, Frédéric Marin, Rashid Sunyaev, Jiri Svoboda, Alexey Vikhlinin, Thibault Barnouin, Chien-Ting Chen, Enrico Costa, Laura Di Gesu, Alessandro Di Marco, Steven R. Ehlert, William Forman, Dawoon E. Kim, Ralph Kraft, W. Peter Maksym, Giorgio Matt, Juri Poutanen, Paolo Soffitta, Douglas A. Swartz, Ivan Agudo, Lucio Angelo Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolo Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovciak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel Lawrence Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgro, Patrick Slane, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf

评论： 16页，13张图。已提交至《天文学与天体物理学》；欢迎提出意见

主题：高能天体物理现象 (astro-ph.HE) ; 星系的天体物理学 (astro-ph.GA)

在我们银河系中心分子区（CMZ）的几个分子云方向上观测到的扩展X射线辐射表现出与“X射线回声”情景一致的光谱和时间特性。它假设观测到的信号是短($\delta t<$1.5 yr)且明亮($L_{\rm X}>10^{39}~{\rm erg~s^{-1}}$)的耀斑的光传播时间延迟反射，最可能是数百年前由Sgr A*产生的。该情景还预测了反射X射线连续谱的独特偏振特征，偏振矢量垂直于朝向主源的方向，偏振度（PD）由散射角决定。我们报告了2022年和2023年用成像X射线偏振探测器（IXPE）对目前反射辐射最亮的分子复合体Sgr A的两次深度观测结果。我们以更高的显著性确认了覆盖Sgr A复合体的大区域之前的偏振测量，但也揭示了其中最亮反射区域的不一致偏振模式。该区域的X射线偏振几乎垂直于Sgr A*照射时的预期方向，并且其PD比大区域小。这可能表明多个照明前沿同时在整个CMZ传播，其中其中一个的起源不是Sgr A*。主源可能与Arches恒星星团有关，或与被照射云附近的一个目前未知的源有关，这可能会降低主源所需的亮度。尽管需要IXPE进行更深入的观测才能明确区分这些情景，但高分辨率成像和微热量光谱学的结合提供了一条额外有希望的前进路径。

Extended X-ray emission observed in the direction of several molecular clouds in the Central Molecular Zone (CMZ) of our Galaxy exhibits spectral and temporal properties consistent with the `X-ray echo' scenario. It postulates that the observed signal is a light-travel-time delayed reflection of a short ($\delta t<$1.5 yr) and bright ($L_{\rm X}>10^{39}~{\rm erg~s^{-1}}$) flare, most probably produced a few hundred years ago by Sgr A*. This scenario also predicts a distinct polarization signature for the reflected X-ray continuum, with the polarization vector being perpendicular to the direction towards the primary source and polarization degree (PD) being determined by the scattering angle. We report the results of two deep observations of the currently brightest (in reflected emission) molecular complex Sgr A taken with the Imaging X-ray Polarimetry Explorer (IXPE) in 2022 and 2023. We confirm the previous polarization measurement for a large region encompassing Sgr A complex with higher significance, but also reveal an inconsistent polarization pattern for the brightest reflection region in its center. X-ray polarization from this region is almost perpendicular to the expected direction in the case of Sgr A* illumination and shows a smaller PD compared to the large region. This could indicate the simultaneous propagation of several illumination fronts throughout the CMZ, with the origin of one of them not being Sgr A*. The primary source could be associated with the Arches stellar cluster or a currently unknown source located in the closer vicinity of the illuminated cloud, potentially lowering the required luminosity of the primary source. Although significantly deeper observations with IXPE would be required to unequivocally distinguish between the scenarios, a combination of high-resolution imaging and micro-calorimetric spectroscopy offers an additional promising path forward.
[18] arXiv:2508.04958 (交叉列表自 astro-ph.HE) [中文pdf, pdf, html, 其他]: 标题： XRISM揭示了阿贝尔2029星系团中的复杂多温度结构

标题： XRISM Reveals Complex Multi-Temperature Structures in the Abell 2029 Galaxy Cluster

Arnab Sarkar, Eric Miller, Naomi Ota, Caroline Kilbourne, Brian McNamara, Ming Sun, Lorenzo Lovisari, Stefano Ettori, Dominique Eckert, Andrew Szymkowiak, Tommaso Bartalesi, Michael Loewenstein

评论： PASJ XRISM 专刊，已接受。16页，10图，五表

主题：高能天体物理现象 (astro-ph.HE) ; 宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

我们展示了$\sim$500 ks XRISM观测数据，覆盖了阿贝尔2029星系团的中心区域和两个北部区域。Resolve使我们能够区分氢-like和氦-like铁(Fe)离子的多条发射线。本研究重点是使用线比诊断方法分析阿贝尔2029的多温度结构。使用单温度碰撞电离平衡模型，我们在中心区域、内北部区域和外北部区域分别测得平均等离子体温度为6.73 keV、7.61 keV和8.14 keV，覆盖的径向范围高达700 kpc。为了进一步研究热结构，我们通过将观测到的发射线通量比与原子数据库预测进行比较，推导出激发温度和电离温度。在中心区域和内北部区域，显著偏离单温度CIE模型表明存在多相气体。激发温度和电离温度在中心区域为2.85 keV至8.5 keV，在内北部区域为4.3 keV至9.8 keV，在外北部区域为8.3 keV至10.4 keV。这些温度分布与之前观测到的A2029温度梯度基本一致。然而，Resolve检测到两个明显较冷的组分——中心区域为3.42 keV，内北部区域为$\sim$4.3 keV——可能与由于气体摆动而位移的冷却气体有关。此外，我们在阿贝尔2029的核心区域热分辨率下发现了一个2.85 keV的气体组分——这可能是我们对气体冷却理解的重要进展。我们认为这种较冷的气体是阿贝尔2029持续冷却过程的直接产物，已经冷却到目前的温度。如果这种温度结构稳定且没有加热机制，这个储库可能会进一步冷却到更低的温度并形成恒星。

We present $\sim$500 ks XRISM observations covering the central and two northern regions of the Abell 2029 galaxy cluster. Resolve enables us to distinguish multiple emission lines from hydrogen-like and helium-like iron (Fe) ions. This study focuses on the multi-temperature structure of Abell 2029 using line-ratio diagnostics. Using a single-temperature collisionally ionized equilibrium model, we measure average plasma temperatures of 6.73 keV, 7.61 keV, and 8.14 keV in the central, inner northern, and outer northern regions, respectively, spanning a radial range up to 700 kpc. To further investigate thermal structure, we derive excitation and ionization temperatures by comparing observed emission-line flux ratios with atomic database predictions. Significant deviations from the single-temperature CIE model in the central and inner northern regions indicate the presence of multi-phase gas. The excitation and ionization temperatures range from 2.85 keV to 8.5 keV in the central region, 4.3 keV to 9.8 keV in the inner northern region, and 8.3 keV to 10.4 keV in the outer northern region. These temperature distributions are largely consistent with the previously observed temperature gradient of A2029. However, Resolve detects two notably cooler components--3.42 keV in the central region and $\sim$4.3 keV in the inner northern region--likely associated with displaced cool gas due to gas sloshing. Additionally, we thermally resolve a 2.85 keV gas component at the core of A2029--potentially a significant development in our understanding of gas cooling. We propose that this cooler gas is a direct product of ongoing cooling processes in A2029, having already cooled to its present temperature. If this temperature structure is stable and no heating mechanism is present, this reservoir is likely to cool to even lower temperatures and form stars.
[19] arXiv:2508.05195 (交叉列表自 astro-ph.CO) [中文pdf, pdf, html, 其他]: 标题： CLASH-VLT：星系团速度各向异性轮廓的方差

标题： CLASH-VLT: The variance of the velocity anisotropy profiles of galaxy clusters

A. Biviano, E.A. Maraboli, L. Pizzuti, P. Rosati, A. Mercurio, G. De Lucia, C. Ragone-Figueroa, C. Grillo, G.L. Granato, M. Girardi, B. Sartoris, M. Annunziatella

评论：提交给A&A的时间是2025年5月8日。三个月后尚未收到审稿人报告

主题：宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

星系团的速度各向异性轮廓，$\beta(r)$，直接与成员星系轨道的形状相关。了解$\beta(r)$对于理解星系团的形成过程和其星系的演化过程，以及基于星系团动力学改善星系团质量的确定非常重要。我们从CLASH-VLT数据集中确定了九个红移为$0.19 \leq z \leq 0.45$的大质量星系团的$\beta(r)$，每个星系团有150到950个光谱成员，以了解不同星系团的$\beta(r)$中存在多少星系团间的差异，以及这种差异的主要驱动因素是什么。我们使用在宇宙学模拟上校准的CLUMPS算法选择光谱星系团成员。我们将MAMPOSSt代码应用于投影相空间中星系团成员的分布，以限制星系团质量轮廓，$M(r)$，使用来自之前引力透镜分析的先验信息。给定MAMPOSSt对于$M(r)$的最佳拟合解，我们随后求解Jeans方程的反演以确定$\beta(r)$，而无需对其函数形式做出假设。我们还运行DS+代码来识别子簇并描述我们簇的动力学状态。平均$\beta(r)$略微径向，各向异性从簇中心的$\beta \simeq 0.2$增加到virial半径处的$\beta \simeq 0.4$。单个簇的$\beta(r)$存在显著的方差，这不能完全由观测不确定性解释。质量较低且在给定质量下浓度较低的簇具有更多的切向$\beta(r)$。包含丰富子簇的集群具有$\beta(r)$更强烈地偏离平均值$\beta(r)$。

The velocity anisotropy profiles, $\beta(r)$, of galaxy clusters are directly related to the shape of the orbits of their member galaxies. Knowledge of $\beta(r)$ is important to understand the assembly process of clusters and the evolutionary processes of their galaxies, and to improve the determination of cluster masses based on cluster kinematics. We determine the $\beta(r)$ of nine massive clusters at redshift $0.19 \leq z \leq 0.45$ from the CLASH-VLT data set, with 150 to 950 spectroscopic members each, to understand how much cluster-to-cluster variance exists in the $\beta(r)$ of different clusters and what is the main driver of this variance. We select spectroscopic cluster members with the CLUMPS algorithm calibrated on cosmological simulations. We apply the MAMPOSSt code to the distribution of cluster members in projected phase-space to constrain the cluster mass profile, $M(r)$, using priors derived from a previous gravitational lensing analysis. Given the MAMPOSSt best-fit solution for $M(r)$, we then solve the inversion of the Jeans equation to determine $\beta(r)$ without assumptions of its functional form. We also run the DS+ code to identify subclusters and characterize the dynamical status of our clusters. The average $\beta(r)$ is slightly radial, with the anisotropy increasing from $\beta \simeq 0.2$ at the cluster center, to $\beta \simeq 0.4$ at the virial radius. There is substantial variance in the $\beta(r)$ of the individual clusters, that cannot be entirely accounted for by the observational uncertainties. Clusters of lower mass and with a low concentration per given mass have more tangential $\beta(r)$'s. Clusters hosting a rich subcluster have $\beta(r)$ deviating more strongly from the average $\beta(r)$.
[20] arXiv:2508.05233 (交叉列表自 astro-ph.SR) [中文pdf, pdf, html, 其他]: 标题： IACOB项目第十五部分。银河系O型恒星基本参数的校准更新

标题： The IACOB project XV. Updated calibrations of fundamental parameters of Galactic O-type stars

G. Holgado, S. Simón-Díaz, A. Herrero

评论： 19页，16图，已提交至《天文学与天体物理学》

主题：太阳与恒星天体物理学 (astro-ph.SR) ; 星系的天体物理学 (astro-ph.GA)

现代光谱巡天结合盖亚距离正在使对银河系O型恒星的基本参数以及各种光谱类型和光度等级的可靠估计成为可能。我们提供了更新的、统计上稳健的银河系O型恒星基本参数的实证标定，以及它们的绝对视星等（Mv）和光度修正（BC），这些基于高质量的观测数据。我们对358颗银河系O型恒星样本进行了同质分析，结合了高分辨率光谱和盖亚距离。一组234颗满足涉及视差、消光和多波段测光的严格质量标准的恒星被用于推导基本参数的实证标定。对于这些相同的恒星，通过使用推导出的关系从测量的Mv估算校准参数，使我们能够评估标定的内部一致性和预测能力。我们展示了基于光谱类型的光度等级V、III和I的基本参数的更新标定。与之前的工作相比，我们发现系统性偏移，特别是在矮星的有效温度和所有光度等级的Mv中，这些偏移会传播到推导出的量中。将Mv标定应用于整个样本，得到了半径和光度的一致估计，而光谱质量（Msp）显示出显著的分散。我们还评估了FW3414参数（来自Hβ线）作为Mv的标定器，这对于缺乏可靠光谱分类的大规模巡天很有用。排除SB1系统仅对光度等级V的Msp标定有明显影响。这些更新的实证标定为银河系O型恒星提供了一个稳健的参考，并将在大规模光谱巡天的时代支持银河系内外大质量恒星群体的研究。

Modern spectroscopic surveys combined with Gaia distances are enabling reliable estimates of fundamental parameters for hundreds of Galactic O-type stars and the full range of spectral types and luminosity classes. Here we provide updated, statistically robust empirical calibrations of the fundamental parameters of Galactic O-type stars, as well as of their absolute visual magnitudes (Mv) and bolometric corrections (BC), based on high-quality observational data. We perform a homogeneous analysis of a sample of 358 Galactic O-type stars, combining high-resolution spectroscopy and Gaia distances. A subset of 234 stars meeting strict quality criteria involving parallax, extinction, and multi-band photometry was used to derive empirical calibrations of fundamental parameters. For those same stars, calibrated parameters were estimated from their measured Mv using the derived relations, allowing us to assess the internal consistency and predictive power of the calibrations. We present updated spectral-type-based calibrations of fundamental parameters for luminosity classes V, III, and I. Compared to previous works, we find systematic shifts, particularly in effective temperature for dwarfs and in Mv across all classes, which propagate into derived quantities. Applying the Mv calibrations to the full sample yields consistent estimates of radius and luminosity, while spectroscopic mass (Msp) shows significant scatter. We also evaluate the FW3414 parameter (from the Hbeta line) as a calibrator for Mv, useful in large surveys lacking reliable spectral classification. Excluding SB1 systems has a noticeable impact only on the Msp calibration for LC V. These updated empirical calibrations offer a robust reference for Galactic O-type stars and will support studies of massive star populations in both Galactic and extragalactic contexts, particularly in the era of large spectroscopic surveys.
[21] arXiv:2508.05319 (交叉列表自 astro-ph.CO) [中文pdf, pdf, html, 其他]: 标题：星系偏置对交叉相关层析成像的影响

标题： The impact of galaxy bias on cross-correlation tomography

Sara Maleubre, Matteo Zennaro, David Alonso, Ian McCarthy, Matthieu Schaller, Joop Schaye

评论： 13页，9图

主题：宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

不同红移处星系与其他大尺度结构示踪物之间的交叉相关性可用于重建关键物理量的宇宙平均值及其在数十亿年间的演化，且精度较高。然而，对这些测量结果的正确解释必须确保它们不受所使用星系样本的聚类特性的影响。在本文中，我们探讨了不同的方案来提取分层重建测量结果，并利用FLAMINGO流体动力学模拟表明，可以构建一个与小尺度星系偏差无关的稳健估计器。我们重点关注分层重建的晕偏差加权电子压力$\langle bP_e\rangle$和恒星形成密度$\langle b\rho_{\rm SFR}\rangle$，这些量可分别通过Sunyaev-Zel'dovich和宇宙红外背景图的分层分析进行重建。我们表明，使用不同的星系样本，这些量可以在广泛的红移范围内以1-3%的精度进行重建。我们还表明，假设能够为晕质量函数、大尺度晕偏差以及被重建的物理量与晕质量之间的依赖关系构建足够可靠的模型，这些测量结果可以被准确地解释。

The cross-correlation of galaxies at different redshifts with other tracers of the large-scale structure can be used to reconstruct the cosmic mean of key physical quantities, and their evolution over billions of years, at high precision. However, a correct interpretation of these measurements must ensure that they are independent of the clustering properties of the galaxy sample used. In this paper we explore different prescriptions to extract tomographic reconstruction measurements and use the FLAMINGO hydrodynamic simulations to show that a robust estimator, independent of the small-scale galaxy bias, can be constructed. We focus on the tomographic reconstruction of the halo bias-weighted electron pressure $\langle bP_e\rangle$ and star-formation density $\langle b\rho_{\rm SFR}\rangle$, which can be reconstructed from tomographic analysis of Sunyaev-Zel'dovich and cosmic infrared background maps, respectively. We show that these quantities can be reconstructed with an accuracy of 1-3\% over a wide range of redshifts, using different galaxy samples. We also show that these measurements can be accurately interpreted using the halo model, assuming a sufficiently reliable model can be constructed for the halo mass function, large-scale halo bias, and for the dependence of the physical quantities being reconstructed on halo mass.

[22] arXiv:2408.02739 (替换) [中文pdf, pdf, html, 其他]: 标题：星际物体1I/'Oumuamua、2I/Borisov和3I/Atlas的银河轨迹

标题： Galactic Trajectories of Interstellar Objects 1I/'Oumuamua, 2I/Borisov, and 3I/Atlas

Shokhruz Kakharov, Abraham Loeb

评论： 9页，23图；于2025年7月9日提交发表至《天文学与天体物理学》

主题：星系的天体物理学 (astro-ph.GA)

The first interstellar objects, 1I/`Oumuamua, 2I/Borisov and 3I/ATLAS, were discovered over the past decade. We follow the trajectories of known interstellar objects in the gravitational potential of the Milky Way galaxy to constrain their possible origin. We perform Monte Carlo orbital integrations using 10,000 trajectory ensembles per object to properly account for measurement uncertainties in both object velocities and Solar motion parameters. We implement a Bayesian statistical framework that combines a Rayleigh-like likelihood function with star formation rate priors to infer stellar ages from the maximum vertical excursions ($z_{\text{max}}$) of orbital trajectories. The likelihood function incorporates age-dependent velocity dispersions reflecting the thin-thick disk transition and dynamical heating over galactic history. Our Monte Carlo analysis yields median $z_{\text{max}}$ values of 0.016 $\pm$ 0.002 kpc for 1I/`Oumuamua, 0.121 $\pm$ 0.010 kpc for 2I/Borisov, and 0.480 $\pm$ 0.020 kpc for 3I/ATLAS. The Bayesian age inference indicates that 1I/`Oumuamua originated from a young stellar system (1.0 Gyr, 68% CI: 0.1-4.1 Gyr), 2I/Borisov from an intermediate-age population (3.8 Gyr, 68% CI: 1.8-5.9 Gyr), and 3I/ATLAS from an old thick-disk source (9.6 Gyr, 68% CI: 7.8-10.3 Gyr). These results demonstrate clear age discrimination where smaller vertical excursions correspond to younger stellar origins.

The first interstellar objects, 1I/`Oumuamua, 2I/Borisov and 3I/ATLAS, were discovered over the past decade. We follow the trajectories of known interstellar objects in the gravitational potential of the Milky Way galaxy to constrain their possible origin. We perform Monte Carlo orbital integrations using 10,000 trajectory ensembles per object to properly account for measurement uncertainties in both object velocities and Solar motion parameters. We implement a Bayesian statistical framework that combines a Rayleigh-like likelihood function with star formation rate priors to infer stellar ages from the maximum vertical excursions ($z_{\text{max}}$) of orbital trajectories. The likelihood function incorporates age-dependent velocity dispersions reflecting the thin-thick disk transition and dynamical heating over galactic history. Our Monte Carlo analysis yields median $z_{\text{max}}$ values of 0.016 $\pm$ 0.002 kpc for 1I/`Oumuamua, 0.121 $\pm$ 0.010 kpc for 2I/Borisov, and 0.480 $\pm$ 0.020 kpc for 3I/ATLAS. The Bayesian age inference indicates that 1I/`Oumuamua originated from a young stellar system (1.0 Gyr, 68\% CI: 0.1-4.1 Gyr), 2I/Borisov from an intermediate-age population (3.8 Gyr, 68\% CI: 1.8-5.9 Gyr), and 3I/ATLAS from an old thick-disk source (9.6 Gyr, 68\% CI: 7.8-10.3 Gyr). These results demonstrate clear age discrimination where smaller vertical excursions correspond to younger stellar origins.
[23] arXiv:2503.12977 (替换) [中文pdf, pdf, html, 其他]: 标题： SISSI：分层剪切星间介质中的超新星 -- I。超新星遗迹的几何结构

标题： SISSI: Supernovae in a stratified, shearing interstellar medium -- I. The geometry of supernova remnants

Leonard E. C. Romano, Manuel Behrendt, Andreas Burkert

评论：已接受提交至《天文学与天体物理学》。18页，19幅图

主题：星系的天体物理学 (astro-ph.GA)

目标。我们介绍了SISSI（分层剪切星际介质中的超新星）模拟套件，旨在使对在复杂星际介质（ISM）中演化的超新星遗迹（SNRs）有更全面的理解，该星际介质在星系旋转、引力和湍流的影响下结构化。方法。我们利用30个超新星遗迹（SNRs）在模拟的孤立盘状星系的星际介质（ISM）中膨胀的放大模拟。该星系的星际介质被解析到最大分辨率为$\sim 12\,\text{pc}$，而在爆炸源附近实现了$\sim 0.18\, \text{pc}$的放大分辨率。我们计算了SNRs几何形状的时间演化，并将其与本地气泡的观测几何形状进行比较。结果。在演化的早期阶段，SNRs可以用现有的解析模型很好地描述。在更长的时间尺度上，大约从轨道时间尺度的百分之一开始，它们偏离球对称性，变得越来越长椭或扁椭。偏离球对称性的时标比由银河剪切变形的简单模型预期的要短，这表明仅银河剪切无法解释这些差异。然而，SNRs的次轴和主轴的对齐与该模型的预期一致，表明变形可能具有剪切相关起源。与本地气泡几何形状的比较表明，它可能比以前认为的稍年轻，但除此之外，其形态对于其年龄和大小的SNRs来说是标准的。结论。研究SNRs的几何形状可以揭示关于塑造其动力学演化的复杂相互作用的宝贵见解。未来针对银河系SNRs几何形状的研究可以利用这一见解，以获得对塑造银河系星际介质过程的更清晰的认识。

Aims. We introduce the SISSI (Supernovae In a Stratified, Shearing Interstellar medium) simulation suite, which aims to enable a more comprehensive understanding of supernova remnants (SNRs) evolving in a complex interstellar medium (ISM) structured under the influence of galactic rotation, gravity and turbulence. Methods. We utilize zoom-in simulations of 30 SNRs expanding in the ISM of a simulated isolated disk galaxy. The ISM of the galaxy is resolved down to a maximum resolution of $\sim 12\,\text{pc}$, while we achieve a zoomed-in resolution of $\sim 0.18\, \text{pc}$ in the vicinity of the explosion sources. We compute the time-evolution of the SNRs' geometry and compare it to the observed geometry of the Local Bubble. Results. During the early stages of evolution, SNRs are well described by existing analytical models. On longer timescales, starting at about a percent of the orbital timescale, they depart from spherical symmetry and become increasingly prolate or oblate. The timescale for the departure from spherical symmetry is shorter than the expectation from a simple model for the deformation by galactic shear, suggesting that galactic shear alone cannot explain these differences. Yet, the alignment of the minor- and major axis of the SNRs is in line with expectations from said model, indicating that the deformation might have a shear-related origin. A comparison with the geometry of the Local Bubble reveals that it might be slightly younger than previously believed, but otherwise has a standard morphology for a SNR of its age and size. Conclusions. Studying the geometry of SNRs can reveal valuable insights about the complex interactions shaping their dynamical evolution. Future studies targeting the geometry of Galactic SNRs may use this insight to obtain a clearer picture of the processes shaping the Galactic ISM.
[24] arXiv:2505.02917 (替换) [中文pdf, pdf, html, 其他]: 标题：通过轨道叠加方法恢复边缘朝向棒旋星系的模式速度

标题： Recovering the pattern speeds of edge-on barred galaxies via an orbit-superposition method

Yunpeng Jin, Ling Zhu, Behzad Tahmasebzadeh, Shude Mao, Glenn van de Ven, Rui Guo, Runsheng Cai

评论： 19页，15图

主题：星系的天体物理学 (astro-ph.GA)

我们开发了一种针对边缘朝向棒状星系的轨道叠加方法，并评估了其恢复棒状结构旋转速度的能力$\rm\Omega_p$。我们从Auriga模拟中选择了三个具有已知旋转速度的模拟星系（Au-18、Au-23和Au-28），并创建了类似MUSE的模拟数据集，具有边缘朝向视图（倾斜角度$\theta_{\rm T}\ge85^\circ$）和各种棒状结构的方位角角度$\varphi_{\rm T}$。对于具有侧向条纹的模拟数据集 ($\varphi_{\rm T}\ge50^\circ$)，模型恢复的旋转速度 ($\rm\Omega_p$) 在模型不确定性范围内 ($1\sigma$置信水平，$68\%$) 包含真实的旋转速度 ($\rm\Omega_T$)，在12种情况下有10种符合。在$1\sigma$置信水平内的平均模型不确定性等于$10\%$。对于具有端对端棒状结构的模拟数据集（$\varphi_{\rm T}\le30^\circ$），$\rm\Omega_p$的模型不确定性显著依赖于棒的方位角角度$\varphi_{\rm T}$，具有$\varphi_{\rm T}=10^\circ$的情况的不确定性接近$\sim30\%$。然而，通过对接收器形态施加更严格的约束（$p_{\rm bar}\le0.50$），平均不确定性降低到$14\%$，并且$\rm\Omega_p$在四种情况中的三种模型不确定性范围内仍包含$\rm\Omega_T$。对于本文中我们创建的所有模型，模型恢复的模式速度$2\sigma$ ($95\%$) 置信水平$\rm\Omega_p$始终覆盖真实值$\rm\Omega_T$。

We developed an orbit-superposition method for edge-on barred galaxies and evaluated its capability to recover the bar pattern speed $\rm\Omega_p$. We selected three simulated galaxies (Au-18, Au-23, and Au-28) with known pattern speeds from the Auriga simulations and created MUSE-like mock data sets with edge-on views (inclination angles $\theta_{\rm T}\ge85^\circ$) and various bar azimuthal angles $\varphi_{\rm T}$. For mock data sets with side-on bars ($\varphi_{\rm T}\ge50^\circ$), the model-recovered pattern speeds $\rm\Omega_p$ encompass the true pattern speeds $\rm\Omega_T$ within the model uncertainties ($1\sigma$ confidence levels, $68\%$) for 10 of 12 cases. The average model uncertainty within the $1\sigma$ confidence levels is equal to $10\%$. For mock data sets with end-on bars ($\varphi_{\rm T}\le30^\circ$), the model uncertainties of $\rm\Omega_p$ depend significantly on the bar azimuthal angles $\varphi_{\rm T}$, with the uncertainties of cases with $\varphi_{\rm T}=10^\circ$ approaching $\sim30\%$. However, by imposing a stricter constraint on the bar morphology ($p_{\rm bar}\le0.50$), the average uncertainties are reduced to $14\%$ , and $\rm\Omega_p$ still encompass $\rm\Omega_T$ within the model uncertainties for three of four cases. For all the models that we create in this paper, the $2\sigma$ ($95\%$) confidence levels of the model-recovered pattern speeds $\rm\Omega_p$ always cover the true values $\rm\Omega_T$.
[25] arXiv:2506.01159 (替换) [中文pdf, pdf, html, 其他]: 标题： H$β$线形状和半径-光度关系在2.5D FRADO中

标题： H$β$ line shape and radius-luminosity relation in 2.5D FRADO

M.H. Naddaf, M.L. Martinez-Aldama, D. Hutsemekers, D. Savic, B. Czerny

评论： 12页，11图，已接受发表于A&A

主题：星系的天体物理学 (astro-ph.GA)

具有活动星系核（AGN）的星系以宽发射线作为关键光谱特征。发射线轮廓的形状取决于称为宽线区（BLR）的空间扩展区域内离散云团的复杂动力学。 BLR内云团位置的分布，或者BLR的几何结构确实与BLR的时间滞后测量直接相关。在本文中，我们将大量基于物理的BLR云分布模拟网格与BLR云的光子通量加权发射率进行卷积，以研究光谱线轮廓的通用形状。更重要的是，我们提取相应模型的时间延迟直方图以计算BLR的大小。我们的物理模型基于这样一个假设：云团是由作用于外盘大气中尘埃上的辐射压力产生的。它只有很少的全局参数。该模型适用于BLR的低电离部分，这通过早期的模型测试得到了证明。它采用非流体动力学的单云方法来处理BLR的动力学。这样，我们模拟了云团的位置和速度分布。我们发现，线条轮廓的宽度随着黑洞质量或观测角度的增加而变宽，并随着吸积率的增加而变窄。发射线轮廓的蓝翼随着黑洞质量和吸积率的增加变得更加明显，这与外流结构的形成和增强一致。我们还发现，峰值时间延迟而不是平均延迟值更能代表观测趋势以及半径-光度关系中的散射。

Galaxies with active galactic nuclei (AGN) exhibit broad emission lines as a key spectral feature. The shape of emission-line profiles depends on the complex dynamics of discrete clouds within a spatially extended region known as the Broad Line Region (BLR). The distribution of cloud positions within BLR, or the geometry of BLR indeed, is directly linked to measurements of time lags of BLR. In this paper, we convolve a large grid of physically-based simulations of cloud distributions in BLR with photon-flux weighted emissivity of BLR clouds to investigate the generic shape of spectral line profiles. More importantly, we extract the time-delay histograms of corresponding models to calculate the size of BLR. Our physical model is based on the assumption that the clouds are launched by the radiation pressure acting on dust in the atmosphere of the outer disk. It has very few global parameters. The model is appropriate for the low ionization part of the BLR, as it was shown by earlier model tests. It uses a non-hydrodynamical single-cloud approach to the BLR dynamics. In this way we simulate the distribution of positions and velocities of the clouds. We found that the width of line profiles gets broader with black hole mass, or with viewing angle, and gets narrower with accretion rate. The blue wing of the emission line profiles becomes more pronounced with increasing black hole mass and accretion rate, consistent with the formation and intensification of an outflow structure. We also found that the peak time-delays rather than averaged delay values better represents the observational trend and also the scatter in the radius-luminosity relation.
[26] arXiv:2506.12129 (替换) [中文pdf, pdf, html, 其他]: 标题： 130亿年视角下的星系演化：通过詹姆斯韦伯太空望远镜和档案调查从本地宇宙到$z=9$的金属丰度梯度演化

标题： A 13-Billion-Year View of Galaxy Growth: Metallicity Gradient Evolution from the Local Universe to $z=9$ with JWST and Archival Surveys

Zihao Li, Zheng Cai, Xin Wang, Zhaozhou Li, Avishai Dekel, Kartick C. Sarkar, Eduardo Bañados, Fuyan Bian, Aklant K. Bhowmick, Laura Blecha, Sarah E. I. Bosman, Jaclyn B. Champagne, Xiaohui Fan, Emmet Golden-Marx, Hyunsung D. Jun, Mingyu Li, Xiaojing Lin, Weizhe Liu, Fengwu Sun, Maxime Trebitsch, Fabian Walter, Feige Wang, Yunjing Wu, Jinyi Yang, Huanian Zhang, Shiwu Zhang, Mingyang Zhuang, Siwei Zou

评论：已接受发表于ApJS。欢迎提出意见

主题：星系的天体物理学 (astro-ph.GA)

星系气体金属丰度梯度在过去四十年中已在本地和高红移宇宙中得到了广泛研究，因为它们追踪了重子循环和星系的增长。凭借JWST前所未有的空间分辨率和灵敏度，现在可以测量到红移高达$z = 9$的金属丰度及其径向梯度。在此，我们展示了一个样本，包含455个光谱确认的星系，来自红移$1.7 \lesssim z \lesssim 9$，这些星系通过深度JWST NIRCam或NIRISS宽场无狭缝光谱学（WFSS）在亚千秒差距（kpc）尺度上被空间解析。将这些新的JWST观测结果与文献中的遗留观测结果结合起来，我们观察到在红移$z > 5$时，星系中心更富含金属，表现出负的金属丰度梯度为$\sim-0.4$ dex kpc$^{-1}$。这些梯度随时间变平，在$z \approx 2$左右接近零，这与宇宙恒星形成率的峰值同时发生。在此之后，随着红移降低，梯度再次变为负值，达到$z=0$。这种演化可能反映了星系形成模式的转变：在“宇宙黎明”时期由强烈的中心恒星形成主导的内部向外增长阶段，反馈效率低且气体混合有限；在“宇宙正午”时期由于反馈驱动的风和气体吸积导致增强的气体混合；以及向现今时期缓慢演化和减少反馈的后期阶段。这些物理过程，包括气体吸积和反馈，不仅在宇宙尺度上调节恒星和星系的形成，也塑造了单个星系在宇宙时间中的演化路径。

The galaxy gas-phase metallicity gradients have been extensively studied over the past four decades, both in the local and high-redshift universe, as they trace the baryon cycle and growth of galaxies. With the unprecedented spatial resolution and sensitivity of JWST, it is now possible to measure metallicity and its radial gradients out to redshifts as high as $z = 9$. Here, we present a sample of 455 spectroscopically confirmed galaxies from redshifts $1.7 \lesssim z \lesssim 9$ that are spatially resolved on sub-kiloparsec (kpc) scales by deep JWST NIRCam or NIRISS Wide Field Slitless Spectroscopy (WFSS). Synthesizing these new JWST observations with legacy observations from the literature, we observe that at redshift $z > 5$, galaxy centers are more metal-rich, exhibiting negative metallicity gradients of $\sim-0.4$ dex kpc$^{-1}$. These gradients flatten over time, reaching near-zero around $z \approx 2$, coinciding with the peak of the cosmic star formation rate. Beyond this point, the gradients become negative again at lower redshifts approaching $z=0$. This evolution likely reflects transitions in galaxy formation modes: an inside-out growth phase dominated by intense central star formation with inefficient feedback and limited gas mixing during ``cosmic dawn", enhanced gas mixing due to feedback-driven wind and gas accretion at ``cosmic noon", and a later phase of slow evolution and reduced feedback toward the present day. These physical processes, including gas accretion and feedback, not only regulate star and galaxy formation on a cosmic scale but also shape the evolutionary pathways of individual galaxies over cosmic time.
[27] arXiv:2507.19472 (替换) [中文pdf, pdf, html, 其他]: 标题： JWST+ALMA揭示宇宙中午时期尘埃星系核心恒星质量的积累

标题： JWST+ALMA reveal the build up of stellar mass in the cores of dusty star-forming galaxies at Cosmic Noon

Sarah Bodansky, Katherine E. Whitaker, Ayesha Abdullah, Jamie Lin, Pascal A. Oesch, Alexandra Pope, Mengyuan Xiao, Alba Covelo-Paz, Sam Cutler, Carlos Garcia Diaz, Minju M. Lee, Sinclaire M. Manning, Romain A. Meyer, Desika Narayanan, Erica Nelson, Irene Shivaei, Pieter van Dokkum

评论：提交至ApJ，欢迎提出意见！17页，11图。图9相比之前版本已进行修改

主题：星系的天体物理学 (astro-ph.GA)

尘埃丰富的星系形成星系长期以来一直被认为是在大质量星系演化中星系形成阶段和静止阶段之间的缺失进化桥梁。借助JWST和ALMA的联合力量，现在可以利用在静止光学、静止近红外（NIR）和静止亚毫米波段的高分辨率成像来研究多波段形态，这些形态追踪了这一关键阶段内的恒星种群和尘埃。我们展示了JWST/NIRCam在GOODS-S中的联合分析以及由ALMA追踪的毫米波尘埃发射，针对从1.1mm GOODS-ALMA 2.0调查中选择的33个星系样本，其红移范围为$z$=1.5至$z$=5.5，并将该群体的形态与质量及红移选择的场星系形成和静止星系样本进行比较。 1.1mm选择的样本在形态上与其他同样大质量的星系形成星系不同；我们发现从1.5-4.4$\mu$m的尺寸-波长梯度更陡峭，随着波长变长，尺寸更显著地减小。尽管1.1mm选择的星系的静止-NIR表面亮度分布在内部区域比场星系形成群体更亮，但它们与静止群体非常相似。这些形态差异可能表明，尘埃丰富的星系形成星系不同于更典型的星系形成星系，它们已经在严重尘埃遮蔽的核心中积累了恒星质量，导致在静止光学波段出现扩展且不规则的形态，而在静止-NIR波段则表现出更紧凑的发射，且与尘埃共空间。如果核心已经建立，我们推测毫米波选择的星系可能会很快演变成它们的静止后代。

Dusty star-forming galaxies have long been suspected to serve as the missing evolutionary bridge between the star-forming and quiescent phases of massive galaxy evolution. With the combined power of JWST and ALMA, it is now possible to use high resolution imaging in rest-optical, rest near-infrared (NIR), and rest-submm wavelengths to study the multi-wavelength morphologies tracing both the stellar populations and dust within this key phase. We present the joint analysis of JWST/NIRCam imaging in GOODS-S and mm dust emission traced by ALMA for a sample of 33 galaxies at $z$=1.5 to $z$=5.5 selected from the 1.1mm GOODS-ALMA 2.0 survey, and compare the morphologies of this population to mass and redshift selected samples of field star-forming and quiescent galaxies. The 1.1mm-selected sample are morphologically distinct from other similarly massive star-forming galaxies; we find a steeper size-wavelength gradient from 1.5-4.4$\mu$m, with a more dramatic decrease in size towards longer wavelengths. While the rest-NIR surface brightness profiles of the 1.1mm-selected galaxies are brighter in the inner regions relative to the field star-forming population, they are remarkably similar to the quiescent population. These morphological differences could suggest that dusty star-forming galaxies, unlike more typical star-forming galaxies, have already built up stellar mass in a severely dust-obscured core, leading to extended and clumpy morphologies at rest-optical wavelengths and more compact emission in the rest-NIR that is co-spatial with dust. If the bulge is already established, we speculate that mm-selected galaxies may imminently evolve to join their quiescent descendants.
[28] arXiv:2508.03817 (替换) [中文pdf, pdf, html, 其他]: 标题：螺旋星系宿主活动星系核中的喷流准直：0313-192中的抛物线喷流轮廓

标题： Jet collimation in a spiral-hosted AGN: a parabolic jet profile in 0313-192

Seung Yeon Lee, Jae-Young Kim

评论： 13页，4图，1表，已接受发表于ApJL

主题：星系的天体物理学 (astro-ph.GA) ; 高能天体物理现象 (astro-ph.HE)

与活动星系核相关的双叶射电源（DRAGNs）通常出现在椭圆星系中，而盘状星系中的超大质量黑洞（SMBHs）很少产生强大的千秒差距尺度喷流。然而，越来越多的螺旋星系和盘状星系宿主DRAGNs挑战了这种经典的二分法。我们使用VLBA和VLA数据对这样一个源0313-192的喷流准直轮廓进行了研究，追踪了喷流形态在近五个数量级的尺度上——从$\sim$pc到$\sim100$kpc（投影）。我们发现，喷流在$\sim 610$pc（$\sim 7.9 \times 10^6$Schwarzschild半径）处表现出抛物线扩张，随后过渡到几乎圆锥形的形状，假设千秒差距尺度的辐射主要来源于喷流而不是叶状结构。这种结构演化与椭圆星系宿主的AGN非常相似，并解释了该系统中的喷流如何通过磁流体动力学准直和加速延伸到远距离。然而，这种准直断裂发生在SMBH的引力影响球之外（$\sim7.3\times10^{5} R_{S}$），并且没有检测到延伸的X射线晕或致密分子气体结构来提供必要的外部压力。因此，我们认为0313-192中的喷流约束是由非热成分的贡献所介导的，例如磁化盘风的冲压和磁场压力。这些机制可能即使在缺乏致密环境气体的情况下也能实现喷流准直。我们的结果突显了在罕见条件下盘状星系中可以产生大尺度喷流，并证明了需要将AGN喷流形成的研究所涵盖的范围超越传统模型。

Double-lobed radio sources associated with active galactic nuclei (DRAGNs) are typically found in elliptical galaxies, while supermassive black holes (SMBHs) in disk galaxies rarely produce powerful kpc-scale jets. However, the growing number of spiral- and disk-hosted DRAGNs challenges this classical dichotomy. We present a study of the jet collimation profile for one such source, 0313-192, using VLBA and VLA data, tracing the jet morphology across nearly five orders of magnitude in scale -- from $\sim$ pc to $\sim100$ kpc (projected). We find that the jet exhibits a parabolic expansion up to $\sim 610$ pc ($\sim 7.9 \times 10^6$ Schwarzschild radii), followed by a transition to a nearly conical shape, assuming kpc-scale emission primarily originates from the jet rather than the lobe. This structural evolution closely resembles those in AGNs hosted by elliptical galaxies and provides an explanation for how the jet in this system could extend to large distances by magnetohydrodynamic collimation and acceleration. However, this collimation break occurs beyond the sphere of gravitational influence of the SMBH ($\sim7.3\times10^{5} R_{S}$), and no extended X-ray halos or dense molecular gas structures are detected to provide the necessary external pressure. Therefore we suggest that jet confinement in 0313-192 is mediated by contributions from non-thermal components, such as ram and magnetic pressure from magnetized disk winds. These mechanisms may enable jet collimation even in the absence of dense ambient gas. Our results highlight how large-scale jets can arise in disk galaxies under rare conditions and demonstrate the need to broaden studies of AGN jet formation beyond traditional models.
[29] arXiv:2212.11980 (替换) [中文pdf, pdf, html, 其他]: 标题：用原初黑洞探测类轴子粒子

标题： Detecting Axion-Like Particles with Primordial Black Holes

Kaustubh Agashe, Jae Hyeok Chang, Steven J. Clark, Bhaskar Dutta, Yuhsin Tsai, Tao Xu

评论： 8页+参考文献，5图。v2：被PRD接受的版本，对图2进行了额外更正

主题：高能物理 - 现象学 (hep-ph) ; 宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

未来伽马射线实验，如e-ASTROGAM和AMEGO望远镜，如果原初黑洞（PBHs）构成暗物质的一部分或全部，就可以探测到来自原初黑洞的霍金辐射光子。 PBHs也可以类似地霍金辐射新粒子，如果这些粒子主要与标准模型（SM）部分隔离开来，这尤其有趣，因为它们可能因此更难以被探测到。这种类型的典型例子是与光子耦合非常微弱的轴子样粒子（ALPs）。我们假设由PBH产生的ALPs在到达地球之前就衰变为光子，因此这些会直接增强PBH辐射的光子。值得注意的是，我们发现由PBH产生的ALPs能量分布中的峰与霍金辐射光子的相应峰不同，这是由于自旋相关的灰体因子。因此，我们证明这个过程实际上会明显改变PBH的伽马射线谱相对于标准模型预测的结果。我们以单色的小行星质量PBH为例，说明e-ASTROGAM可以观测到PBH产生的ALP伽马射线信号（质量高达约60 MeV），并进一步将其与没有ALPs的霍金辐射区分开来。通过测量伽马射线信号，e-ASTROGAM可以探测尚未探索的ALP质量与光子耦合参数。

Future gamma-ray experiments, such as the e-ASTROGAM and AMEGO telescopes, can detect the Hawking radiation of photons from primordial black holes (PBHs) if they make up a fraction or all of dark matter. PBHs can analogously also Hawking radiate new particles, which is especially interesting if these particles are mostly secluded from the Standard Model (SM) sector, since they might therefore be less accessible otherwise. A well-motivated example of this type is axion-like particles (ALPs) with a tiny coupling to photons. We assume that the ALPs produced by PBHs decay into photons well before reaching the earth, so these will augment the photons directly radiated by the PBHs. Remarkably, we find that the peaks in the energy distributions of ALPs produced from PBHs are different than the corresponding ones for Hawking radiated photons due to the spin-dependent greybody factor. Therefore, we demonstrate that this process will in fact distinctively modify the PBHs' gamma-ray spectrum relative to the SM prediction. We use monochromatic asteroid-mass PBHs as an example to show that e-ASTROGAM can observe the PBH-produced ALP gamma-ray signal (for masses up to ~60 MeV) and further distinguish it from Hawking radiation without ALPs. By measuring the gamma-ray signals, e-ASTROGAM can thereby probe yet unexplored parameters in the ALP mass and photon coupling.
[30] arXiv:2412.08173 (替换) [中文pdf, pdf, html, 其他]: 标题： CRAFTS用于HI宇宙学：I.数据处理流程和验证测试

标题： CRAFTS for HI cosmology: I. data processing pipeline and validation tests

Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen

评论： 34页，33图，3表，发表于ApJS

期刊参考： 2025，ApJS，279，32

主题：宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

我们介绍了校准过程和源测量的验证，使用了共轭射电天文FAST调查（CRAFTS）的数据，对\HI 强度映射进行校准，由五百米口径球面射电望远镜（FAST）完成。使用70小时漂移扫描观测，采用L波段（1.05-1.45GHz）19波束接收器，我们获得了覆盖$270\,\rm deg^2$天空区域的数据。我们同时使用脉冲星后端和谱线后端对光谱时间有序数据（TOD）进行校准，然后将它们投影到HEALPix图上。我们生成了频率分辨率为30kHz、时间分辨率为1s的校准TOD，以及频率分辨率为30kHz、空间分辨率为$2.95\,\rm arcmin^2$的图数据立方体。我们检查了指向误差、噪声溢出、射频干扰（RFI）污染及其对数据质量的影响。结果表明，校准后的TOD噪声水平为$\sim$5.7mJy，图数据噪声水平为1.6mJy，在无RFI信道中与理论预测一致，偏差在5%以内。我们还通过主成分分析（PCA）验证了数据，发现去除30个模式后的残差图看起来由热噪声主导。我们在数据中识别出447个孤立的明亮连续谱源，与美国国家射电天文台-甚大天线阵天空调查（NVSS）目录匹配，TOD的相对通量误差为8.3%，图数据级别的相对通量误差为6.6%。我们还测量了90个红移为$z<0.07$的星系的\HI 发射，并与\HI -MaNGA 光谱进行比较，得出总体相对\HI 积分流量误差为16.7%。这些结果为评估使用CRAFTS进行宇宙学\HI 检测的可行性提供了重要的第一步。

We present the calibration procedures and validation of source measurement with the data of the Commensal Radio Astronomy FAST Survey (CRAFTS) for \HI intensity mapping by the Five-hundred-meter Aperture Spherical Radio Telescope (FAST). Using 70-hour drift-scan observation with the L-band (1.05-1.45GHz) 19-beam receiver, we obtain the data covering $270\,\rm deg^2$ sky area. We employ both the pulsar backend and the spectrum backend to calibrate the spectral time-ordered-data (TOD) before projecting them onto HEALPix maps. We produce calibrated TOD with frequency resolution of 30kHz and time resolution of 1s and the map data-cube with frequency resolution of 30kHz and spatial resolution of $2.95\,\rm arcmin^2$. We examine the pointing errors, noise overflow, RFI contamination and their effect on the data quality. The resulting noise level is $\sim$ 5.7mJy for the calibrated TOD and 1.6mJy for the map, consistent with the theoretical predictions within 5\% at RFI-free channels. We also validate the data by Principal Components Analysis (PCA) and find the residual map looks thermal noise dominated after removing 30 modes. We identify 447 isolated bright continuum sources in our data matching the NRAO-VLA Sky Survey (NVSS) catalog, with relative flux error of 8.3\% for TOD and 6.6\% for the map-level. We also measure the \HI emission of 90 galaxies with redshift $z<0.07$ and compare with \HI-MaNGA spectra, yielding an overall relative \HI integral flux error of 16.7\%. These results provide an important first step in assessing the feasibility of conducting cosmological \HI detection with CRAFTS.
[31] arXiv:2412.09705 (替换) [中文pdf, pdf, html, 其他]: 标题：多波段成像高α行星调查（MISHAPS）I：对半人马座47中热木星出现率的初步限制

标题： The Multiband Imaging Survey for High-Alpha PlanetS (MISHAPS) I: Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae

Alison L. Crisp (1 and 2), Jonas Klüter (1), Marz L. Newman (1), Matthew T. Penny (1), Thomas G. Beatty (3), L. Ilsedore Cleeves (4), Karen A. Collins (5), Jennifer A. Johnson (2), Marshall C. Johnson (2), Michael B. Lund (6), Clara E. Martínez-Vázquez (7), Melissa K. Ness (8 and 9), Joseph E. Rodriguez (10), Robert Siverd (11), Daniel J. Stevens (12), Steven Villanueva (13), Carl Ziegler (14) ((1) Louisiana State University, (2) The Ohio State University, (3) University of Wisconsin, (4) University of Virginia, (5) Harvard-Smithsonian Center for Astrophysics, (6) California Institute of Technology, (7) NOIRLab, (8) Columbia University, (9) Flatiron Institute, (10) Michigan State University, (11) University of Hawai'i, (12) University of Minnesota Duluth, (13) NASA Goddard Space Flight Center, (14) Stephen F. Austin State University)

评论： 39页，26图

期刊参考： AJ 170 104（2025）

主题：地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

第一代在球状星团中进行的凌日行星搜索没有发现任何检测结果，从现在来看，仅将发生率限制稍微提高到高于银河系厚盘高金属丰度区域的测量发生率。为了改进这些限制，我们介绍了在球状星团47~Tucanae中新的宽视场凌日热木星搜索的第一批结果。我们作为Multiband Imaging Survey for High-Alpha Planets (MISHAPS)的一部分对47~Tuc进行了观测。使用在CTIO的4米Blanco望远镜上用暗能量相机拍摄的24个部分和完整的夜晚观测数据，我们在星团的外区对19,930颗恒星进行了搜索。尽管我们没有发现明确的行星检测，但通过将我们的结果与Gilliland等人2000年利用哈勃望远镜对星团内部独立样本34,091颗恒星进行的行星搜索所获得的上限结合起来，我们对周期为$0.8 \leq P \leq 8.3$天和$0.5~R_{\rm Jup} \leq R_{\rm P} \leq 2.0~R_{\rm Jup}$的$f_{\rm HJ} < 0.11\%$设定了目前最强的限制，比\textit{开普勒}区域的出现率低了${\sim}$倍。我们的搜索发现了35个凌日行星候选者，但最终由于缺乏后续观测，我们能够排除每一个候选者。我们还发现了4个食双星，包括3个之前未列入目录的分离食双星。

The first generation of transiting planet searches in globular clusters yielded no detections, and in hindsight, only placed occurrence rate limits slightly higher than the measured occurrence rate in the higher-metallicity Galactic thick disk. To improve these limits, we present the first results of a new wide field search for transiting hot Jupiters in the globular cluster 47~Tucanae. We have observed 47~Tuc as part of the Multiband Imaging Survey for High-Alpha Planets (MISHAPS). Using 24 partial and full nights of observations taken with the Dark Energy Camera on the 4-m Blanco telescope at CTIO, we perform a search on 19,930 stars in the outer regions of the cluster. Though we find no clear planet detections, by combining our result with the upper limit enabled by Gilliland et al.'s 2000 Hubble search for planets around an independent sample of 34,091 stars in the inner cluster, we place the strongest limit to date on hot Jupiters with periods of $0.8 \leq P \leq 8.3$ days and $0.5~R_{\rm Jup} \leq R_{\rm P} \leq 2.0~R_{\rm Jup}$ of $f_{\rm HJ} < 0.11\%$, a factor of ${\sim}$4 below the occurrence rate in the \textit{Kepler} field. Our search found 35 transiting planet candidates, though we are ultimately able to rule out each without follow-up observations. We also found 4 eclipsing binaries, including 3 previously-uncataloged detached eclipsing binary stars.
[32] arXiv:2504.10589 (替换) [中文pdf, pdf, html, 其他]: 标题：减轻托尔-费舍尔关系中隐含倾角推断的爱丁顿和马尔姆奎斯特偏差

标题： Mitigating Eddington and Malmquist Biases in Latent-Inclination Inference of the Tully-Fisher Relation

Hai Fu

评论： ApJ已接受。Python函数和笔记本可在以下地址获取 https://github.com/fuhaiastro/TFR_biases

主题：方法论 (stat.ME) ; 星系的天体物理学 (astro-ph.GA) ; 天体物理学的仪器与方法 (astro-ph.IM)

泰利-费舍尔关系是一个重要的距离指示器，但其精确推断受到选择偏差、统计偏差和不确定的倾斜校正的挑战。本研究提出了一种贝叶斯框架，同时解决这些问题。为了消除对个别倾斜校正的需求，倾斜被当作具有已知概率分布的潜在变量处理。为了校正由于样本选择引起的距离依赖的马尔姆奎斯特偏差，模型将因变量的高斯散射、自变量的分布和观测选择函数纳入数据似然中。为了减轻由高斯散射和自变量非均匀分布引起的统计偏差——称为“一般爱丁顿偏差”，引入了两种方法：(1) 在似然计算之前对因变量应用解析偏差校正，(2) 一种双散射模型，在似然函数中考虑自变量的高斯散射。这些方法的有效性通过模拟数据集得到证明。通过在潜在变量回归分析中严格处理选择和统计偏差，这项工作提供了一种稳健的方法，用于从标准化蜡烛中获得无偏的距离估计，这对于提高哈勃常数测定的准确性至关重要。

The Tully-Fisher relation is a vital distance indicator, but its precise inference is challenged by selection bias, statistical bias, and uncertain inclination corrections. This study presents a Bayesian framework that simultaneously addresses these issues. To eliminate the need for individual inclination corrections, inclination is treated as a latent variable with a known probability distribution. To correct for the distance-dependent Malmqvist bias arising from sample selection, the model incorporates Gaussian scatter in the dependent variable, the distribution of the independent variable, and the observational selection function into the data likelihood. To mitigate the statistical bias -- termed the ``general Eddington bias'' -- caused by Gaussian scatter and the non-uniform distribution of the independent variable, two methods are introduced: (1) analytical bias corrections applied to the dependent variable before likelihood computation, and (2) a dual-scatter model that accounts for Gaussian scatter in the independent variable within the likelihood function. The effectiveness of these methods is demonstrated using simulated datasets. By rigorously addressing selection and statistical biases in a latent-variable regression analysis, this work provides a robust approach for unbiased distance estimates from standardizable candles, which is critical for improving the accuracy of Hubble constant determinations.
[33] arXiv:2505.04618 (替换) [中文pdf, pdf, html, 其他]: 标题：凝结气体-粒子混合物的线性热不稳定性，可能应用于球粒陨石和星子

标题： Linear Thermal Instability of a Condensing Gas-Particle Mixture, with Possible Application to Chondrites and Planetesimals

Kecheng Stephon Qian (Berkeley), Eugene Chiang (Berkeley)

评论：被《天体物理学杂志》接收，最终校对版本，标题已更改

主题：地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA) ; 太阳与恒星天体物理学 (astro-ph.SR)

我们研究了在光学稀薄介质中与凝聚粒子共存的热饱和气体的稳定性。这种情况可能出现在激波下游、冷凝前沿或蒸发撞击中。我们表明，气-粒子混合物会受到一种热不稳定性的影响，其中温度较低且凝聚物密度较高的区域会更快冷却并更快地凝聚。如果 runaway 凝结区域的声速穿越时间短于其冷却时间，那么它将从其高压周围环境中吸积更多的质量和粒子。对线性化扰动方程的数值积分表明，这种辐射-冷凝不稳定性可以从持续冷却的气体中产生粒子团块和空洞。如果辐射可以逃逸以冷却粒子高密度区域，热不稳定性可以帮助将小行星碰撞的蒸发碎片组合成陨石母体，并普遍形成星子。

We study the stability of a hot saturated gas coexisting with condensed particles in an optically thin medium. Such a situation may obtain downstream of a shock, at condensation fronts, or in vaporizing impacts. We show that the gas-particle mixture is subject to a thermal instability whereby a region of lower temperature and higher condensate density cools faster to condense faster. If the region of runaway condensation has a sound-crossing time shorter than its cooling time, then it accretes more mass, in gas and particles, from its higher pressure surroundings. Numerical integration of the linearized perturbation equations demonstrates that this radiation-condensation instability can create particle clumps and voids out of a secularly cooling gas. Provided radiation can escape to cool particle overdensities, thermal instability can help assemble chondrite parent bodies out of the vaporized debris of asteroid collisions, and form planetesimals generally.
[34] arXiv:2507.08111 (替换) [中文pdf, pdf, html, 其他]: 标题： 3I/ATLAS的运动学年龄及其对早期行星形成的影响

标题： The Kinematic Age of 3I/ATLAS and its Implications for Early Planet Formation

Aster G. Taylor, Darryl Z. Seligman

评论： 10页，3图。被ApJL接收

主题：地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

最近发现的第三个星际天体（3I/ATLAS）将已知的天体数量从两个增加到三个，并显著提高了关于银河系潜在天体群体的统计推断。在本文中，我们认为彗星活动很可能显著贡献于3I/ATLAS的亮度，因为假设其具有小行星反射率时推导出的核尺寸意味着每个恒星的星际天体质量是不可接受的。 3I/ATLAS相对于太阳具有较高的过剩速度$v_\infty=58$km/s，这意味着与之前的星际天体相比，3I/ATLAS相对较为古老。在这里，我们计算了由星际天体运动学所暗示的年龄后验分布，并发现假设星际天体和恒星的年龄-速度弥散关系相等，3I/ATLAS可能有$\sim3-11$Gyr 的年龄。我们还计算了宿主恒星金属丰度的分布，并发现3I/ATLAS有12%的可能性起源于一个金属丰度为$\text{[Fe/H]}\leq-0.4$的恒星。这些结果表明，星际天体的形成可能在低金属丰度和银河系早期历史中是高效的。最后，我们估算了由这三个天体所暗示的银河系历史中的星际天体形成率。随着未来更多星际天体的发现，本文提出的框架可以用于进一步优化这一计算。星际天体和恒星形成历史之间的比较将为银河系中恒星系统形成的历史提供独特的见解。

The recent discovery of the third interstellar object (3I/ATLAS) expands the known census from two to three and significantly improves statistical inferences regarding the underlying galactic population. In this paper, we argue that cometary activity likely significantly contributes to 3I/ATLAS's brightness, since the nuclear size inferred when assuming an asteroidal reflectance implies an untenable interstellar object mass per star. 3I/ATLAS exhibits a high excess velocity of $v_\infty=58$ km/s relative to the Sun, which implies that 3I/ATLAS is relatively old in comparison to previous interstellar objects. Here, we calculate the posterior distribution of ages implied by the kinematics of the interstellar objects and find that 3I/ATLAS is likely $\sim3-11$ Gyr old, assuming that the interstellar object and stellar age-velocity dispersion relations are equivalent. We also calculate the distribution of host star metallicities and find that 3I/ATLAS has a 12% chance of originating from a star with $\text{[Fe/H]}\leq-0.4$. These results show that interstellar object formation is likely efficient at low metallicities and early in the history of the Galaxy. Finally, we estimate the interstellar object formation rate throughout Galactic history implied by these three objects. As future interstellar objects are discovered, the framework presented here can be applied to further refine this calculation. Comparison between the interstellar object and stellar formation histories will provide unique insights into the history of stellar system formation in the Galaxy.
[35] arXiv:2507.22794 (替换) [中文pdf, pdf, html, 其他]: 标题： SN 2024ggi的星云阶段：没有相互作用迹象的低质量前身星

标题： The nebular phase of SN 2024ggi: a low-mass progenitor with no signs of interaction

L. Ferrari, G. Folatelli, K. Ertini, H. Kuncarayakti, T. Regna, M. C. Bersten, C. Ashall, E. Baron, C. R. Burns, L. Galbany, W. B. Hoogendam, K. Maeda, K. Medler, N. I. Morrell, B. Shappee, M. D. Stritzinger, H. Xiao

评论： 11页，7图。已提交至A&A

主题：太阳与恒星天体物理学 (astro-ph.SR) ; 星系的天体物理学 (astro-ph.GA) ; 高能天体物理现象 (astro-ph.HE)

上下文：SN 2024ggi 是在 2024 年 4 月 3 日 21:00 UT 发现的 II 型超新星（SN），位于邻近星系 NGC 3621（D $\approx6.7\pm0.d$ Mpc）。其接近性使得能够详细研究 SN 的特性及其前身星。本工作聚焦于 SN 2024ggi 在爆发后第 287 天至第 400 天期间的电离相光学演化。目标：通过研究爆发后第 287 天至第 400 天期间的电离相演化，调查前身星的特性以及抛射物可能的不对称性。方法：我们展示了在电离相期间，使用 Las Campanas 和 Gemini South 观测站获得的 SN 2024ggi 的光学测光和光谱数据。在爆发后第 287、288、360 和 396 天拍摄了四次电离相光谱，并补充了持续 $320-400$ 天的晚期时间 $uBVgri$-波段测光数据。对电离发射特征的分析用于探测抛射物的不对称性。基于 [O I] 流量和 [O I]/[Ca II] 比率，并与文献中的光谱模型进行比较，我们得出前身星质量的估计值。此外，我们从光学测光和近红外数据构建了光度曲线，以推导出合成镍的质量。结果：我们的分析表明前身星零年龄主序星质量在 $12-15 M_\odot$ 之间。晚期光度曲线与合成 $^{56}$Ni 质量为 $0.05-0.06 M_\odot$ 一致。线轮廓在观测期间仅有微小变化，表明抛射物大致对称，可能有一个富含氧的物质团块朝向观测者移动。在爆发后 400 天内未检测到任何与周围星际物质相互作用的迹象。

Context: SN 2024ggi is a Type II supernova (SN) discovered in the nearby galaxy NGC 3621 (D $\approx6.7\pm0.d$ Mpc) on 2024 April 03.21 UT. Its proximity enabled a detailed investigation of the SN's properties and its progenitor star. This work focuses on the optical evolution of SN 2024ggi at the nebular phase. Aims: We investigate the progenitor properties and possible asymmetries in the ejecta by studying the nebular phase evolution between days 287 and 400 after the explosion. Methods: We present optical photometry and spectroscopy of SN 2024ggi during the nebular phase, obtained with the Las Campanas and Gemini South Observatories. Four nebular spectra were taken at 287, 288, 360, and 396 days post-explosion, supplemented by late-time $uBVgri$-band photometry spanning $320-400$ days. The analysis of the nebular emission features is performed to probe ejecta asymmetries. Based on the [O I] flux and [O I]/[Ca II] ratio, and comparisons with spectra models from the literature, we arrive to an estimate of the progenitor mass. Additionally, we construct the bolometric light curve from optical photometry and near-infrared data to derive the synthesized nickel mass. Results: Our analysis suggests a progenitor zero-age-main-sequence mass between $12-15 M_\odot$. The late-time bolometric light curve is consistent with a synthesized $^{56}$Ni mass of $0.05-0.06 M_\odot$. The line profiles exhibit only minor changes over the observed period and suggest a roughly symmetrical ejecta, with a possible clump of oxygen-rich material moving towards the observer. No signatures of circumstellar material interaction are detected up to 400 days after the explosion.
[36] arXiv:2508.02777 (替换) [中文pdf, pdf, html, 其他]: 标题：星际天体3I/ATLAS的光谱特性来自SOAR观测

标题： Spectral Characteristics of Interstellar Object 3I/ATLAS from SOAR Observations

Thomas H. Puzia, Rohan Rahatgaonkar, Juan Pablo Carvajal, Prasanta K. Nayak, Baltasar Luco

评论： 6页，2图，已接受发表于ApJL

主题：地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA) ; 太阳与恒星天体物理学 (astro-ph.SR)

星际天体（ISOs）为了解太阳系外行星系统的构建块和条件提供了独特的见解。新发现的天体，3I/ATLAS（C/2025 N1），是在1I/'Oumuamua和2I/Borisov之后第三个已知的ISO。我们利用智利4.1米SOAR望远镜上的Goodman高通量光谱仪在7月3日夜间进行的观测，对3I进行了初步光谱表征。3I的反射光谱覆盖3700-7000{\AA }，显示出与极端海王星外天体相似的红色连续谱，弱紫外-可见光转折表明存在复杂的碳质和辐射有机物。在观测时，当3I距离太阳4.4天文单位时，我们没有检测到任何可辨别的彗星物质气体发射（CN，C$_3$，C$_2$，CO$^+$，[OI]）。这与我们的热演化模型预期一致，该模型表明一旦3I/ATLAS接近更小的太阳距离，升华驱动的活动应该开始。尽管如此，早期彗发出现但缺乏升华示踪物的矛盾情况，需要其他释放尘埃的机制，古代ISO可能在大太阳距离下经历这些机制。

Interstellar objects (ISOs) provide unique insights into the building blocks and conditions of extrasolar planetary systems. The newly discovered object, 3I/ATLAS (C/2025 N1), represents the third known ISO after 1I/'Oumuamua and 2I/Borisov. We present initial spectroscopic characterizations of 3I using observations from the Goodman High Throughput Spectrograph on the 4.1 m SOAR Telescope in Chile during the night of July 3rd. The reflectance spectrum of 3I, covering 3700-7000{\AA} reveals a red continuum, comparable to extreme trans-Neptunian objects, with a weak UV-optical turnover indicative of complex carbonaceous and irradiated organics. At the time of observation, when 3I was at a heliocentric distance of 4.4 AU, we detected no discernible gas emission from canonical cometary species (CN, C$_3$, C$_2$, CO$^+$, [OI]). This is in agreement with expectations from our thermal-evolution model, which indicates sublimation-driven activity should commence once 3I/ATLAS approaches smaller heliocentric distances. Nonetheless, the paradoxical situation of early onset coma without evidence of sublimation tracers calls for other dust-liberating mechanisms that ancient ISOs may be subjected to at large heliocentric distances.
[37] arXiv:2508.02934 (替换) [中文pdf, pdf, html, 其他]: 标题：哈勃空间望远镜对星际闯入者3I/ATLAS的观测

标题： Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS

David Jewitt, Man-To Hui, Max Mutchler, Yoonyoung Kim, Jessica Agarwal

评论： 13页，4图，2表

主题：地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

我们展示了对第三颗已知的星际闯入者3I/ATLAS的高角分辨率观测结果，来自哈勃空间望远镜。该天体在近日点前3.8天文单位明显活跃，显示出从核的面向太阳的热侧释放出尘埃，并有一个弱的、受辐射压力吹动的尾巴远离太阳。我们应用一个简单的模型来估算尘埃的质量损失率，即dM/dt = 6 sqrt(a) kg/s，其中a是以微米为单位的平均粒子大小。当1 < a < 100时，我们推断dM/dt = 6到60 kg/s。对内晕表面亮度分布的拟合将核的有效半径限制为r < 2.8公里，假设其几何反照率为0.04。相反，如果其晕由二氧化碳升华提供，则核的半径不能小于0.16公里，如果导致质量损失的分子挥发性较低，则核必须更大。

We present high angular resolution observations of the third known interstellar interloper, 3I/ATLAS, from the Hubble Space Telescope. The object is clearly active at 3.8 au pre-perihelion, showing dust emitted from the hot Sun-facing side of the nucleus and a weak, radiation pressure swept tail away from the Sun. We apply a simple model to estimate the mass loss rate in dust as dM/dt = 6 sqrt(a) kg/s, where a is the mean particle size in microns. With 1 < a < 100, we infer dM/dt = 6 to 60 kg/s. A fit to the surface brightness distribution of the inner coma limits the effective radius of the nucleus to be r < 2.8 km, assuming red geometric albedo 0.04. Conversely, the nucleus cannot be smaller than 0.16 km in radius if its coma is supplied by sublimation of carbon monoxide, and must be larger if a less volatile molecule drives the mass loss.
[38] arXiv:2508.03888 (替换) [中文pdf, pdf, html, 其他]: 标题：合成器：用于合成天文学观测的软件包

标题： Synthesizer: a Software Package for Synthetic Astronomical Observables

Christopher C. Lovell, William J. Roper, Aswin P. Vijayan, Stephen M. Wilkins, Sophie Newman, Louise Seeyave

评论：提交至《天体物理学开放期刊》。27页，17图。欢迎提出意见！请查看arXiv:2506.15811 获取配套的JOSS论文。文档可在 https://synthesizer-project.github.io/ 查看。

主题：天体物理学的仪器与方法 (astro-ph.IM) ; 宇宙学与非星系天体物理学 (astro-ph.CO) ; 星系的天体物理学 (astro-ph.GA)

我们介绍Synthesizer，这是一个快速、灵活、模块化和可扩展的平台，用于建模合成天体物理观测数据。 Synthesizer可用于多种应用，但主要设计用于从分析和数值星系形成模拟中生成模拟观测数据。这些用例包括（但不限于）星系恒星形成和金属增丰历史的分析建模，从基于粒子的模拟创建模拟图像和积分场单元观测数据，活动星系核中心区域的详细光致电离建模，以及光谱-光度拟合。我们提供了一系列可以“开箱即用”并交互使用的恒星种群合成模型、光致电离代码配置、尘埃模型和成像配置。我们邀请并鼓励社区使用、测试和开发该代码，并希望所建立的基础能够为正向和反向建模天体物理观测数据的多项任务提供一个灵活的框架。该代码可在https://synthesizer-project.github.io/公开获取。

We present Synthesizer, a fast, flexible, modular and extensible platform for modelling synthetic astrophysical observables. Synthesizer can be used for a number of applications, but is predominantly designed for generating mock observables from analytical and numerical galaxy formation simulations. These use cases include (but are not limited to) analytical modelling of the star formation and metal enrichment histories of galaxies, the creation of mock images and integral field unit observations from particle based simulations, detailed photoionisation modelling of the central regions of active galactic nuclei, and spectro-photometric fitting. We provide a number of stellar population synthesis models, photoionisation code configurations, dust models, and imaging configurations that can be used 'out-of-the-box' interactively. We invite and encourage the community to use, test and develop the code, and hope that the foundation developed will provide a flexible framework for a number of tasks in forward and inverse modelling of astrophysical observables. The code is publicly available at https://synthesizer-project.github.io/

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