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Measuring the global 21-cm signal with the MWA-II: improved characterisation of lunar-reflected radio frequency interference 用MWA-II测量全球21厘米信号:改进月球反射射频干扰的特性
3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-08 DOI: 10.1017/pasa.2023.57
Himanshu Tiwari, Benjamin McKinley, Cathryn M. Trott, Nithyanandan Thyagarajan
Abstract Radio interferometers can potentially detect the sky-averaged signal from the Cosmic Dawn (CD) and the Epoch of Reionisation (EoR) by studying the Moon as a thermal block to the foreground sky. The first step is to mitigate the Earth-based RFI reflections (Earthshine) from the Moon, which significantly contaminate the FM band ≈ 88 – 110 MHz, crucial to CD-EoR science. We analysed MWA phase-I data from 72 – 180 MHz at 40 kHz resolution to understand the nature of Earthshine over three observing nights. We took two approaches to correct the Earthshine component from the Moon. In the first method, we mitigated the Earthshine using the flux density of the two components from the data, while in the second method, we used simulated flux density based on an FM catalogue to mitigate the Earthshine. Using these methods, we were able to recover the expected Galactic foreground temperature of the patch of sky obscured by the Moon. We performed a joint analysis of the Galactic foregrounds and the Moon’s intrinsic temperature ( T Moon ) while assuming that the Moon has a constant thermal temperature throughout three epochs. We found T Moon to be at 184.4±2.6 K and 173.8±2.5 K using the first and the second methods, respectively, and the best-fit values of the Galactic spectral index ( α ) to be within the 5% uncertainty level when compared with the global sky models. Compared with our previous work, these results improved constraints on the Galactic spectral index and the Moon’s intrinsic temperature. We also simulated the Earthshine atMWA between November and December 2023 to find suitable observing times less affected by the Earthshine. Such observing windows act as Earthshine avoidance and can be used to perform future global CD-EoR experiments using the Moon with the MWA.
无线电干涉仪可以通过研究月球作为前景天空的热块来探测来自宇宙黎明(CD)和再电离时代(EoR)的天空平均信号。第一步是减轻来自月球的地球RFI反射(地球光),这会严重污染FM频段≈88 - 110 MHz,这对CD-EoR科学至关重要。我们以40 kHz的分辨率分析了72 - 180 MHz的MWA第一阶段数据,以了解三个观测夜晚地球发光的性质。我们用了两种方法来修正月球上的地球光分量。在第一种方法中,我们使用数据中两个分量的通量密度来减轻地球辐射,而在第二种方法中,我们使用基于FM目录的模拟通量密度来减轻地球辐射。使用这些方法,我们能够恢复被月球遮挡的天空中预期的银河系前景温度。我们对银河前景和月球的固有温度(T月亮)进行了联合分析,同时假设月球在三个时期具有恒定的热温度。我们用第一种方法和第二种方法分别得到了T Moon的184.4±2.6 K和173.8±2.5 K,银河系光谱指数(α)的最佳拟合值与全球天空模型相比,不确定度在5%以内。与我们之前的工作相比,这些结果改善了对银河系光谱指数和月球固有温度的限制。我们还模拟了2023年11月至12月的地球辐射atMWA,以寻找受地球辐射影响较小的合适观测时间。这样的观测窗口起到了避免地球辐射的作用,可以用来在未来利用带MWA的月球进行全球CD-EoR实验。
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引用次数: 0
Inviscid protostellar disc ring formation and high density ring edges due to the ejection and subsequent infall of material onto a protostellar disc 无粘性原恒星盘环的形成和高密度环的边缘,这是由于物质的喷射和随后落入原恒星盘
3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-06 DOI: 10.1017/pasa.2023.55
Kurt Liffman
Abstract Discs of gas and dust are ubiquitous around protostars. Hypothetical viscous interactions within the disc are thought to cause the gas and dust to accrete onto the star. Turbulence within the disc is theorised to be the source of this disc viscosity. However, observed protostellar disc turbulence often appears to be small and not always conducive to disc accretion. In addition, theories for disc and planet evolution have difficulty in explaining the observed disc rings/gaps which form much earlier than expected. Protostellar accretion discs are observed to contain significant quantities of dust and pebbles. Observations also show that some of this material is ejected from near the protostar, where it travels to the outer regions of the disc. Such solid infalling material has a relatively small amount of angular momentum compared to the material in the disc. This infalling material lowers the angular momentum of the disc and should drive a radial flow towards the protostar. We show that the local radial accretion speed of the disc is proportional to the mass rate of infalling material onto the disc. Higher rates of infall onto the disc implies higher radial accretion disc speeds. As such, regions with high rates of infall of gas, dust, and pebbles onto the disc will produce gaps on relatively short timescales in the disc, while regions associated with relative low rates of infalling material will produce disc rings. As such, the inner edge of a disc gap will tend to have a higher surface density, which may enhance the probability of planet formation. In addition, the outer edge of a disc gap will act as a dust trap and may also become a site for planet formation. For the early Solar System, such a process may have collected O16-poor forsterite dust from the inner regions of the protosolar disc and O16-rich CAIs and AOAs from the inner edge regions of the protosolar disc, thereby constructing a region favourable to the formation of prechondritic planetesimals.
气体和尘埃盘在原恒星周围无处不在。假设圆盘内的粘性相互作用被认为是导致气体和尘埃吸积到恒星上的原因。理论上,圆盘内的湍流是圆盘粘度的来源。然而,观测到的原恒星盘湍流通常看起来很小,并不总是有利于盘的吸积。此外,关于盘和行星演化的理论很难解释观测到的盘环/间隙形成的时间比预期的要早得多。原恒星吸积盘被观察到含有大量的尘埃和鹅卵石。观测还表明,其中一些物质是从原恒星附近喷射出来的,在那里它向圆盘的外部区域移动。与圆盘内的物质相比,这种固体物质的角动量相对较小。这些流入的物质降低了圆盘的角动量,应该会推动径向流流向原恒星。我们证明了盘的局部径向吸积速度与进入盘的物质的质量率成正比。更高的流入率意味着更高的径向吸积盘速度。因此,气体、尘埃和鹅卵石流入盘的速率高的区域将在相对较短的时间尺度上在盘上产生间隙,而与相对较低的物质流入率相关的区域将产生盘环。因此,圆盘间隙的内缘将倾向于具有更高的表面密度,这可能会增加行星形成的可能性。此外,圆盘间隙的外缘将充当尘埃收集器,也可能成为行星形成的地点。对于早期太阳系,这一过程可能从原太阳盘的内部区域收集了缺乏o16的forsterite尘埃,从原太阳盘的内缘区域收集了富含o16的cai和aoa,从而构建了一个有利于形成预球粒状星子的区域。
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引用次数: 0
Dynamical aspects of Galactic habitability in N-body simulations n体模拟中银河系可居住性的动力学方面
3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-11-06 DOI: 10.1017/pasa.2023.54
A. Mitrašinović, B. Vukotić, M. Micic, M. M. Ćirković
Abstract Recent studies of Galactic evolution revealed that the dynamics of the stellar component might be one of the key factors when considering galactic habitability. We run an N-body simulation model of the Milky Way, which we evolve for 10 Gyr, to study the secular evolution of stellar orbits and the resulting galactic habitability-related properties, i.e., the density of the stellar component and close stellar encounters. The results indicate that radial migrations are not negligible, even in a simple axisymmetric model with mild levels of dynamical heating, and that the net outward diffusion of the stellar component can populate galactic outskirts with habitable systems. Habitable environment is also likely even at sub-Solar galactocentric radii, because the rate of close encounters should not significantly degrade habitability. Stars that evolve from non-circular to stable nearly-circular orbits typically migrate outwards, settling down in a broad Solar neighborhood. The region between R ≈ 3 kpc and R ≈ 12 kpc represents the zone of radial mixing, which can blur the boundaries of the Galactic Habitable Zone, as it has been conventionally understood. The present-day stable population of the stars in the Solar neighborhood originates from this radial mixing zone, with most of the stars coming from the inner regions. The Solar system can be considered as a typical Milky Way habitable system because it migrated outwards from the metal-rich inner regions of the Disk and has a circular orbit in the present epoch. We conclude that the boundaries of the Galactic Habitable Zone cannot be sharply confined for a given epoch because of the mixing caused by the stellar migrations and secular evolution of stellar orbits.
最近对星系演化的研究表明,恒星成分的动力学可能是考虑星系宜居性的关键因素之一。我们运行了一个银河系的n体模拟模型,我们对其进行了10 Gyr的演化,以研究恒星轨道的长期演化以及由此产生的星系可居住性相关属性,即恒星成分的密度和近距离恒星相遇。结果表明,即使在具有轻度动态加热水平的简单轴对称模型中,径向迁移也是不可忽略的,并且恒星成分的净向外扩散可以使星系外围充满可居住系统。即使在亚太阳星系中心半径处,也可能存在宜居环境,因为近距离接触的频率不应显著降低宜居性。从非圆形轨道演变成稳定的近圆形轨道的恒星通常会向外迁移,在广阔的太阳附近定居下来。R≈3 kpc和R≈12 kpc之间的区域代表了径向混合区,它可以模糊银河系宜居带的边界,就像传统理解的那样。今天太阳附近稳定的恒星数量起源于这个径向混合带,大多数恒星来自内部区域。太阳系可以被认为是一个典型的银河系宜居系统,因为它从盘内富含金属的区域向外迁移,并且在现在的时代有一个圆形的轨道。我们得出的结论是,由于恒星迁移和恒星轨道的长期演化造成的混合,银河系宜居带的边界在给定的时代不可能被严格限制。
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引用次数: 0
Modelling repetition in zDM: a single population of repeating fast radio bursts can explain CHIME data zDM中的重复建模:一个重复的快速射电暴的单一种群可以解释CHIME数据
3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-26 DOI: 10.1017/pasa.2023.51
C.W. James
Abstract Regardless of whether or not all fast radio bursts (FRBs) repeat, those that do form a population with a distribution of rates. This work considers a power-law model of this population, with rate distribution Φ r ∼ R γ r between R min and R max . The zDM code is used to model the probability of detecting this population as either apparently once-off or repeat events as a function of redshift, z , and dispersion measure, DM. I demonstrate that in the nearby Universe, repeating sources can contribute significantly to the total burst rate. This causes an apparent deficit in the total number of observed sources (once-off and repeaters) relative to the distant Universe that will cause a bias in FRB population models. Thus instruments with long exposure times should explicitly take repetition into account when fitting the FRB population. I then fit data from The Canadian Hydrogen Intensity Mapping Experiment (CHIME). The relative number of repeat and apparently once-off FRBs, and their DM, declination, and burst rate distributions, can be well-explained by 50–100% of CHIME single FRBs being due to repeaters, with R max > 0.75 day –1 above 10 39 erg, and This result is surprisingly consistent with follow-up studies of FRBs detected by the Australian Square Kilometre Array Pathfinder (ASKAP). Thus the evidence suggests that CHIME and ASKAP view the same repeating FRB population, which is responsible not just for repeating FRBs, but the majority of apparently once-off bursts. For greater quantitative accuracy, non-Poissonian arrival times, second-order effects in the CHIME response, and a simultaneous fit to the total FRB population parameters, should be treated in more detail in future studies.
不管所有的快速射电暴(frb)是否都会重复,那些重复的射电暴会形成一个具有频率分布的种群。这项工作考虑了这个群体的幂律模型,其速率分布Φ r ~ r γ r在r min和r max之间。zDM代码用于模拟探测到这个群体的概率,作为红移,z和色散测量DM的函数,要么是明显的一次性事件,要么是重复事件。我证明了在附近的宇宙中,重复源可以显著地贡献总爆发率。这导致观测到的源(一次性和重复)的总数相对于遥远的宇宙明显不足,这将导致快速射电暴人口模型的偏差。因此,长曝光时间的仪器在拟合FRB种群时应明确考虑重复。然后,我拟合了加拿大氢强度测绘实验(CHIME)的数据。重复和明显一次性快速射电暴的相对数量,以及它们的DM、衰减和突发率分布,可以很好地解释为50-100%的CHIME单次快速射电暴是由重复器引起的,其中R max >这一结果与澳大利亚平方公里阵列探路者(ASKAP)探测到的快速射电暴的后续研究惊人地一致。因此,证据表明CHIME和ASKAP观测到的是相同的重复FRB群,这不仅是重复FRB的原因,也是大多数明显的一次性爆发的原因。为了获得更高的定量准确性,在未来的研究中应该更详细地处理非泊松到达时间、CHIME响应的二阶效应以及与FRB总体参数的同时拟合。
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引用次数: 0
Radio Galaxy Zoo: Tagging Radio Subjects using Text 无线电银河动物园:使用文本标记无线电主题
3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-16 DOI: 10.1017/pasa.2023.50
Dawei Chen, Vinay Kerai, Matthew J. Alger, O. Ivy Wong, Cheng Soon Ong
Abstract RadioTalk is a communication platform that enabled members of the Radio Galaxy Zoo (RGZ) citizen science project to engage in discussion threads and provide further descriptions of the radio subjects they were observing in the form of tags and comments. It contains a wealth of auxiliary information which is useful for the morphology identification of complex and extended radio sources. In this paper, we present this new dataset, and for the first time in radio astronomy, we combine text and images to automatically classify radio galaxies using a multi-modal learning approach. We found incorporating text features improved classification performance which demonstrates that text annotations are rare but valuable sources of information for classifying astronomical sources, and suggests the importance of exploiting multi-modal information in future citizen science projects. We also discovered over 10,000 new radio sources beyond the RGZ-DR1 catalogue in this dataset.
RadioTalk是一个交流平台,它使Radio Galaxy Zoo (RGZ)公民科学项目的成员能够参与讨论线程,并以标签和评论的形式提供他们所观察到的无线电主题的进一步描述。它包含了丰富的辅助信息,这是有用的形态识别复杂和扩展的射电源。在本文中,我们展示了这个新的数据集,并且在射电天文学中首次使用多模态学习方法将文本和图像结合起来自动分类射电星系。我们发现结合文本特征可以提高分类性能,这表明文本注释是对天文来源分类的罕见但有价值的信息来源,并表明在未来的公民科学项目中利用多模态信息的重要性。我们还在这个数据集中发现了超过10,000个新的射电源,超出了RGZ-DR1目录。
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引用次数: 0
The Dawes Review 11: From young to old: The evolutionary path of Pulsar Wind Nebulae – CORRIGENDUM 道斯评论11:从年轻到年老:脉冲星风星云的演化路径-勘误表
IF 6.3 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-31 DOI: 10.1017/pasa.2023.41
B. Olmi, N. Bucciantini
11
11
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引用次数: 0
The Mopra Southern Galactic Plane CO Survey – data release 4– complete survey 莫普拉南银河面CO测量-数据发布4 -完整的测量
IF 6.3 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-22 DOI: 10.1017/pasa.2023.44
K. Cubuk, M. Burton, C. Braiding, G. Wong, G. Rowell, N. Maxted, D. Eden, R. Z. E. Alsaberi, R. Blackwell, R. Enokiya, K. Feijen, M. Filipović, M. Freeman, S. Fujita, M. Ghavam, B. Gunay, B. Indermuehle, K. Hayashi, M. Kohno, T. Nagaya, A. Nishimura, K. Okawa, D. Rebolledo, D. Romano, H. Sano, C. Snoswell, N. Tothill, K. Tsuge, F. Voisin, Y. Yamane, S. Yoshiike
Abstract We present observations of the Mopra carbon monoxide (CO) survey of the Southern Galactic Plane, covering Galactic longitudes spanning $l = 250^{circ}$ ( $-110^{circ}$ ) to $l = 355^{circ}$ ( $-5^{circ}$ ), with a latitudinal coverage of at least $|b|<1^circ$ , totalling an area of $>$ 210 deg $^{2}$ . These data have been taken at 0.6 arcmin spatial resolution and 0.1 km s $^{-1}$ spectral resolution, providing an unprecedented view of the molecular gas clouds of the Southern Galactic Plane in the 109–115 GHz $J = 1-0$ transitions of $^{12}$ CO, $^{13}$ CO, C $^{18}$ O, and C $^{17}$ O.
摘要:本文介绍了南银面Mopra一氧化碳巡天的观测结果,覆盖了$l = 250^{circ}$ ($-110^{circ}$)至$l = 355^{circ}$ ($-5^{circ}$)的银河经度,纬度覆盖至少$|b|$ 210°$^{2}$。这些数据以0.6弧分空间分辨率和0.1 km s $^{-1}$光谱分辨率拍摄,提供了前所未有的在109-115 GHz $J = 1-0$跃迁$^{12}$ CO, $^{13}$ CO, $ $^{18}$ O和C $ $^{17}$ O的南银面分子气体云的视图。
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引用次数: 0
A novel approach for variable star classification based on imbalanced learning 一种基于不平衡学习的变星分类新方法
IF 6.3 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-09 DOI: 10.1017/pasa.2023.35
Jingyi Zhang, Yanxia Zhang, Zihan Kang, Changhua Li, Yihan Tao, Yongheng Zhao, Xue-bing Wu
Abstract The advent of time-domain sky surveys has generated a vast amount of light variation data, enabling astronomers to investigate variable stars with large-scale samples. However, this also poses new opportunities and challenges for the time-domain research. In this paper, we focus on the classification of variable stars from the Catalina Surveys Data Release 2 and propose an imbalanced learning classifier based on Self-paced Ensemble (SPE) method. Compared with the work of Hosenie et al. (2020), our approach significantly enhances the classification Recall of Blazhko RR Lyrae stars from 12% to 85%, mixed-mode RR Lyrae variables from 29% to 64%, detached binaries from 68% to 97%, and LPV from 87% to 99%. SPE demonstrates a rather good performance on most of the variable classes except RRab, RRc, and contact and semi-detached binary. Moreover, the results suggest that SPE tends to target the minority classes of objects, while Random Forest is more effective in finding the majority classes. To balance the overall classification accuracy, we construct a Voting Classifier that combines the strengths of SPE and Random Forest. The results show that the Voting Classifier can achieve a balanced performance across all classes with minimal loss of accuracy. In summary, the SPE algorithm and Voting Classifier are superior to traditional machine learning methods and can be well applied to classify the periodic variable stars. This paper contributes to the current research on imbalanced learning in astronomy and can also be extended to the time-domain data of other larger sky survey projects (LSST, etc.).
时域巡天的出现产生了大量的光变化数据,使天文学家能够用大尺度的样本来研究变星。然而,这也给时域研究带来了新的机遇和挑战。本文以Catalina survey Data Release 2中的变星分类为研究对象,提出了一种基于自同步集成(self -pace Ensemble, SPE)方法的不平衡学习分类器。与Hosenie et al.(2020)的工作相比,我们的方法显著提高了Blazhko RR Lyrae恒星的分类召回率,从12%提高到85%,混合模式RR Lyrae变量从29%提高到64%,分离双星从68%提高到97%,LPV从87%提高到99%。SPE在除RRab、RRc以及接触和半分离二进制之外的大多数变量类上都表现出相当好的性能。此外,结果表明SPE倾向于针对对象的少数类,而随机森林在寻找多数类方面更有效。为了平衡整体分类精度,我们构建了一个结合SPE和随机森林优势的投票分类器。结果表明,投票分类器可以在最小的准确性损失的情况下实现所有类的平衡性能。综上所述,SPE算法和投票分类器优于传统的机器学习方法,可以很好地应用于周期变星的分类。本文对当前天文学中不平衡学习的研究有一定的贡献,也可以推广到其他大型巡天项目(LSST等)的时域数据。
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引用次数: 0
Evolved galaxies in high-density environments across 2.0 ≤ z < 4.2 using the ZFOURGE survey 通过ZFOURGE调查,在2.0≤z < 4.2的高密度环境中进化的星系
IF 6.3 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-09 DOI: 10.1017/pasa.2023.42
Georgia R. Hartzenberg, M. Cowley, A. Hopkins, R. Allen
Abstract To explore the role environment plays in influencing galaxy evolution at high redshifts, we study $2.0leq z<4.2$ environments using the FourStar Galaxy Evolution (ZFOURGE) survey. Using galaxies from the COSMOS legacy field with ${rm log(M_{*}/M_{odot})}geq9.5$ , we use a seventh nearest neighbour density estimator to quantify galaxy environment, dividing this into bins of low-, intermediate-, and high-density. We discover new high-density environment candidates across $2.0leq z<2.4$ and $3.1leq z<4.2$ . We analyse the quiescent fraction, stellar mass and specific star formation rate (sSFR) of our galaxies to understand how these vary with redshift and environment. Our results reveal that, across $2.0leq z<2.4$ , the high-density environments are the most significant regions, which consist of elevated quiescent fractions, ${rm log(M_{*}/M_{odot})}geq10.2$ massive galaxies and suppressed star formation activity. At $3.1leq z<4.2$ , we find that high-density regions consist of elevated stellar masses but require more complete samples of quiescent and sSFR data to study the effects of environment in more detail at these higher redshifts. Overall, our results suggest that well-evolved, passive galaxies are already in place in high-density environments at $zsim2.4$ , and that the Butcher–Oemler effect and SFR-density relation may not reverse towards higher redshifts as previously thought.
为了探索环境在高红移星系演化中的作用,我们利用四星星系演化(ZFOURGE)调查研究了$2.0leq z<4.2$环境。使用来自COSMOS遗留场的星系与${rm log(M_{*}/M_{odot})}geq9.5$,我们使用第七近邻密度估计器来量化星系环境,将其分为低,中,高密度的箱子。我们在$2.0leq z<2.4$和$3.1leq z<4.2$上发现了新的高密度候选环境。我们分析了我们星系的静止部分、恒星质量和特定恒星形成率(sSFR),以了解它们如何随着红移和环境而变化。我们的研究结果表明,在$2.0leq z<2.4$中,高密度环境是最重要的区域,其中包括升高的静态部分,${rm log(M_{*}/M_{odot})}geq10.2$大质量星系和抑制的恒星形成活动。在$3.1leq z<4.2$上,我们发现高密度区域由高质量恒星组成,但需要更完整的静态和sSFR数据样本来更详细地研究环境对这些高红移的影响。总的来说,我们的结果表明,进化良好的被动星系已经在$zsim2.4$的高密度环境中存在,并且布彻-欧姆勒效应和sr -密度关系可能不会像之前认为的那样向更高的红移方向逆转。
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引用次数: 0
Statistical analysis of kicked black holes from TNG300 simulation TNG300模拟中被踢黑洞的统计分析
IF 6.3 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-09 DOI: 10.1017/pasa.2023.45
M. Smole, M. Micic
Abstract Asymmetric emission of gravitational waves during mergers of black holes (BHs) produces a recoil kick, which can set a newly formed BH on a bound orbit around the centre of its host galaxy, or even completely eject it. To study this population of recoiling BHs we extract properties of galaxies with merging BHs from Illustris TNG300 simulation and then employ both analytical and numerical techniques to model unresolved process of BH recoil. This comparative analysis between analytical and numerical models shows that, on cosmological scales, numerically modelled recoiling BHs have a higher escape probability and predict a greater number of offset active galactic nuclei (AGN). BH escaped probability $>$ 40% is expected in 25 $%$ of merger remnants in numerical models, compared to 8 $%$ in analytical models. At the same time, the predicted number of offset AGN at separations ${>}5$ kpc changes from 58 $%$ for numerical models to 3 $%$ for analytical models. Since BH ejections in major merger remnants occur in non-virialised systems, static analytical models cannot provide an accurate description. Thus we argue that numerical models should be used to estimate the expected number density of escaped BHs and offset AGN.
在黑洞合并过程中,不对称的引力波发射会产生反冲,这可以使新形成的黑洞在围绕其宿主星系中心的束缚轨道上运行,甚至完全将其弹出。为了研究这一反冲黑洞群,我们从Illustris TNG300模拟中提取合并黑洞的星系特性,然后采用解析和数值方法对黑洞反冲的未解析过程进行建模。分析模型和数值模型之间的对比分析表明,在宇宙学尺度上,数值模拟的反冲黑洞具有更高的逃逸概率,并预测了更多的偏移活动星系核(AGN)。在数值模型中,25 %的合并残留物中黑洞逃逸概率> 40%,而在分析模型中为8 %。同时,在分离值${>}5$ kpc处,预测的偏移AGN数从数值模型的58 $%$变为解析模型的3 $%$。由于主要合并残余物中的黑洞喷射发生在非病毒化系统中,静态分析模型无法提供准确的描述。因此,我们认为应该使用数值模型来估计逃逸黑洞和偏移AGN的期望数量密度。
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引用次数: 0
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