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AstroYOLO: A hybrid CNN–Transformer deep-learning object-detection model for blue horizontal-branch stars AstroYOLO:一种针对蓝色水平分支恒星的CNN-Transformer混合深度学习目标检测模型
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-27 DOI: 10.1093/pasj/psad071
Yuchen He, Jingjing Wu, Wenyu Wang, Bin Jiang, Yanxia Zhang
Abstract Blue horizontal-branch stars (BHBs) are ideal tracers for studying the Milky Way (MW) due to their bright and nearly constant magnitude. However, an incomplete screen of BHBs from a survey would result in bias of estimation of the structure or mass of the MW. With surveys of large sky telescopes like the Sloan Digital Sky Survey (SDSS), it is possible to obtain a complete sample. Thus, detecting BHBs from massive photometric images quickly and effectually is necessary. The current acquisition methods of BHBs are mainly based on manual or semi-automatic modes. Therefore, novel approaches are required to replace manual or traditional machine-learning detection. The mainstream deep-learning-based object-detection methods are often vanilla convolutional neural networks whose ability to extract global features is limited by the receptive field of the convolution operator. Recently, a new Transformer-based method has benefited from the global receptive field advantage brought by the self-attention mechanism, exceeded the vanilla convolution model in many tasks, and achieved excellent results. Therefore, this paper proposes a hybrid convolution and Transformer model called AstroYOLO to take advantage of the convolution in local feature representation and Transformer’s easier discovery of long-distance feature dependences. We conduct a comparative experiment on the 4799 SDSS DR16 photometric image dataset. The experimental results show that our model achieves 99.25% AP@50, 93.79% AP@75, and 64.45% AP@95 on the test dataset, outperforming the YOLOv3 and YOLOv4 object-detection models. In addition, we test on larger cutout images based on the same resolution. Our model can reach 99.02% AP@50, 92.00% AP@75, and 61.96% AP@95 respectively, still better than YOLOv3 and YOLOv4. These results also suggest that an appropriate size for cutout images is necessary for the performance and computation of object detection. Compared with the previous models, our model has achieved satisfactory object-detection results and can effectively improve the accuracy of BHB detection.
蓝色水平分支恒星(BHBs)由于其明亮和几乎恒定的星等而成为研究银河系(MW)的理想示踪剂。然而,调查中对BHBs的不完整筛选会导致对MW结构或质量的估计存在偏差。通过像斯隆数字巡天(SDSS)这样的大型天文望远镜的巡天,有可能获得一个完整的样本。因此,快速有效地从海量测光图像中检测BHBs是必要的。目前bhb的采集方法主要是手动或半自动模式。因此,需要新的方法来取代人工或传统的机器学习检测。主流的基于深度学习的目标检测方法通常是普通的卷积神经网络,其提取全局特征的能力受到卷积算子接受域的限制。近年来,一种新的基于transformer的方法利用自注意机制带来的全局感受场优势,在许多任务中超越了普通卷积模型,并取得了优异的效果。因此,本文提出了一种混合卷积和Transformer模型,称为astrroyolo,以利用卷积在局部特征表示和Transformer更容易发现长距离特征依赖的优势。我们在4799 SDSS DR16光度图像数据集上进行了对比实验。实验结果表明,该模型在测试数据集上的准确率分别达到99.25% AP@50、93.79% AP@75和64.45% AP@95,优于YOLOv3和YOLOv4的目标检测模型。此外,我们在相同分辨率的基础上测试了更大的剪切图像。我们的模型分别可以达到99.02% AP@50、92.00% AP@75和61.96% AP@95,仍然优于YOLOv3和YOLOv4。这些结果还表明,适当的切割图像尺寸对于目标检测的性能和计算是必要的。与以往的模型相比,我们的模型取得了令人满意的目标检测结果,可以有效地提高BHB检测的精度。
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引用次数: 0
Transonic galactic wind model including stellar feedbacks and application to outflows in high/low-z galaxies 包含恒星反馈的跨音速星系风模型及其在高/低z星系外流中的应用
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-20 DOI: 10.1093/pasj/psad065
Asuka Igarashi, Masao Mori, Shin-ya Nitta
Abstract Galactic winds play a crucial role in the ejection of the interstellar medium (ISM) into intergalactic space. This study presents a model that classifies possible transonic solutions of galactic winds in the gravitational potential of the dark matter halo and stellar component under spherically symmetric and steady assumptions. Our model includes injections of mass and energy resulting from supernova feedback along a flow line. The mass flux in galactic winds is a critical factor in determining the acceleration process of the flow and revealing the impact of galactic winds on galaxy evolution. We apply the transonic galactic wind model to the observed outflow velocities of star-forming galaxies to estimate the mass flux. Dividing the mass flux by the star formation rate (SFR) yields the mass loading rate (and mass loading factor), which indicates the entrainment effect of the ISM by the hot gas flow. Our results demonstrate that the mass loading rate is inversely correlated with galaxy mass and SFR. In less massive galaxies (stellar mass ∼107−8 M⊙), the mass loading rate exceeds unity, indicating effective ejection of the ISM into intergalactic space. However, in massive galaxies (stellar mass ∼1010−11 M⊙), the mass loading rate falls below unity, meaning that the mass flux cannot exceed the injected mass by supernovae, thus resulting in ineffective ejection of the ISM.
星系风在星际介质(ISM)喷射到星系间空间中起着至关重要的作用。本研究提出了一个模型,在球对称和稳定的假设下,对暗物质晕和恒星成分的引力势中星系风的可能跨音速解进行分类。我们的模型包括由超新星沿着流线反馈产生的质量和能量的注入。星系风中的质量通量是决定星系风加速过程和揭示星系风对星系演化影响的关键因素。我们将跨音速星系风模型应用于观测到的恒星形成星系的流出速度来估计质量通量。用质量通量除以恒星形成速率(SFR)得到质量加载率(和质量加载因子),它表示热气流对ISM的夹带效应。我们的结果表明,质量加载率与星系质量和SFR呈负相关。在质量较小的星系(恒星质量~ 107−8 M⊙),质量加载率超过1,表明ISM有效地弹射到星系间空间。然而,在大质量星系(恒星质量~ 1010−11 M⊙)中,质量加载率低于1,这意味着质量通量不能超过超新星注入的质量,从而导致ISM的无效喷射。
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引用次数: 0
A comparative study of three modes of s-process nucleosynthesis in extremely metal-poor AGB stars 极贫金属AGB星s过程核合成三种模式的比较研究
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-18 DOI: 10.1093/pasj/psad062
Shimako Yamada, Takuma Suda, Yutaka Komiya, Masayuki Aikawa, Masayuki Y Fujimoto
Carbon-enhanced metal-poor (CEMP) stars in the Galactic halo have a wide range of neutron-capture element abundance patterns. To identify their origin, we investigated three modes of $s$-process nucleosynthesis that have been proposed to operate in extremely metal-poor (EMP) Asymptotic Giant Branch (AGB) stars: the convective 13C burning, which occurs when hydrogen is engulfed by the helium flash convection in low-mass AGB stars, the convective 22Ne burning, which occurs in the helium flash convection of intermediate-mass AGB stars, and the radiative 13C burning, which occurs in the $^{13}$C pocket that is formed during the inter-pulse periods. We show that the production of $s$-process elements per iron seed ($s$-process efficiency) does not depend on metallicity below $[{rm Fe}/{rm H}]=-2$, because 16O in the helium zone dominates the neutron poison. The convective 13C mode can produce a variety of $s$-process efficiencies for Sr, Ba and Pb, including the maxima observed among CEMP stars. The 22Ne mode only produce the lowest end of $s$-process efficiencies among CEMP models. We show that the combination of these two modes can explain the full range of observed enrichment of $s$-process elements in CEMP stars. In contrast, the 13C pocket mode can hardly explain the high level of enrichment observed in some CEMP stars, even if considering star-to-star variations of the mass of the 13C pocket. These results provide a basis for discussing the binary mass transfer origin of CEMP stars and their subgroups.
银晕中的碳增强贫金属(CEMP)恒星具有广泛的中子捕获元素丰度模式。为了确定它们的起源,我们研究了三种被提出在极贫金属(EMP)渐近巨星分支(AGB)恒星中运行的$s$过程核合成模式:低质量AGB恒星中氢被氦闪对流吞没时发生的对流13C燃烧,中质量AGB恒星中氦闪对流中发生的对流22Ne燃烧,以及在脉冲间隔期间形成的$^{13}$C口袋中发生的辐射13C燃烧。我们发现,每颗铁种子产生的$ $ $过程元素($ $ $过程效率)并不取决于$[{rm Fe}/{rm H}]=-2$以下的金属丰度,因为氦区的16O主导了中子中毒。对流13C模式可以产生Sr, Ba和Pb的各种$s$过程效率,包括在CEMP恒星中观测到的最大值。在CEMP模型中,22Ne模式只能产生最低端的$ 5 $流程效率。我们表明,这两种模式的结合可以解释在CEMP恒星中观测到的$s$过程元素富集的全部范围。相比之下,即使考虑到13C口袋质量的恒星间变化,13C口袋模式也很难解释在一些CEMP恒星中观察到的高富集水平。这些结果为讨论CEMP恒星及其亚群的二元传质起源提供了基础。
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引用次数: 0
Spectral analysis of the Galactic supernova remnant Kesteven 69 with Suzaku 银河系超新星遗迹Kesteven 69与Suzaku的光谱分析
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-09 DOI: 10.1093/pasj/psad068
Shigeo Yamauchi, Thomas G Pannuti
Abstract The results of a Suzaku observation of the supernova remnant (SNR) Kesteven 69 = G21.8−0.6 are presented. To estimate the sky background precisely, we conducted a simultaneous fit of the source region spectrum with the background region spectrum and found that the SNR spectrum is well represented by a two-component ionizing plasma model composed of a low-temperature plasma at kTe = 0.80 ± 0.11 keV and a high-temperature plasma at kTe = 1.5 ± 0.4 keV. The existence of a low-ionized Fe K line at 6.49 ± 0.07 keV was confirmed. The center energy of the line is consistent with those of type Ia SNRs.
摘要介绍了超新星遗迹(SNR) Kesteven 69 = G21.8−0.6的Suzaku观测结果。为了准确估计天空背景,我们将源区光谱与背景区光谱进行了同步拟合,发现由低温等离子体(kTe = 0.80±0.11 keV)和高温等离子体(kTe = 1.5±0.4 keV)组成的双组分电离等离子体模型可以很好地代表信噪比谱。证实了在6.49±0.07 keV下存在低电离Fe - K线。该线的中心能量与Ia型信噪比一致。
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引用次数: 0
Investigating the magnetic field of the quiet Sun internetwork 研究宁静太阳网络的磁场
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-03 DOI: 10.1093/pasj/psad067
Mohamed Sedik, Abdelrazek M K Shaltout, Yuanyong Deng, Kiyoshi Ichimoto
Abstract We analyze the magnetism of the quiet Sun internetwork (IN) using high-spatial-resolution data obtained by the spectropolarimeter (SP) of the Solar Optical Telescope aboard the Hinode satellite near the disk center of the Sun. The SP data were inverted using the Stokes Inversion based on Response functions (SIR) inversion code with a single-component atmosphere with depth dependent in the solar photosphere, assuming gradients in physical parameters along the line of sight (LOS). To avoid the effect of noise, only pixels with Stokes U and/or Q signals above 4.5 times the noise level are considered. The inversion results show that the magnetic field of the IN has mainly hG field strength and the inclination distribution is quasi-isotropic at the solar surface. The field strength decreases with height and becomes predominantly horizontal at the upper layers. At the mid photosphere, the distributions of field strength and inclination are consistent with those derived by Milne–Eddington inversion. The mean transverse and longitudinal flux densities are 66 Mx cm−2 and 13 Mx cm−2 at log τ = −1.0; we also study the ratio between the transverse and longitudinal components in the IN region as a function of depth in the photosphere, finding that the ratio is almost 2.7 in the deep layer, increasing to 5.1 in the upper layer. The mean field strength is greater than 100 G in the upper photosphere, which is consistent with the results based on the Hanle effect. We present the LOS velocity probability distribution function for IN at different optical depths, where its distribution is mainly associated with upflow velocities of VLOS = 1.2 and 0.6 km s−1 in the deeper and upper layers, respectively. In addition, there exists a reliable inversion analysis, which is obvious from the comparison between the observed and calculated area asymmetries in both Fe i lines of Hinode SP data.
摘要利用太阳光学望远镜的偏振光谱仪(SP)获得的高空间分辨率数据,分析了安静太阳网络(IN)的磁性。SP数据的反演采用基于响应函数(SIR)反演代码的Stokes反演,反演条件为单组分大气,大气深度依赖于太阳光球层,假设物理参数沿视线(LOS)方向存在梯度。为了避免噪声的影响,只考虑Stokes U和/或Q信号高于噪声水平4.5倍的像素。反演结果表明,太阳磁场以hG场强为主,太阳表面的倾角分布呈准各向同性。场强随高度的增加而减小,在上层以水平场强为主。在光球中部,场强和倾斜度的分布与Milne-Eddington反演结果一致。在log τ = - 1.0时,平均横向通量密度为66 Mx cm−2,纵向通量密度为13 Mx cm−2;我们还研究了in区域的横向分量与纵向分量之比和光球深度的关系,发现该比值在深层几乎为2.7,在上层增加到5.1。上层光球的平均场强大于100 G,这与基于汉勒效应的结果一致。我们给出了不同光学深度下IN的LOS速度概率分布函数,其分布主要与深部和上层VLOS分别为1.2和0.6 km s−1的上流速度有关。此外,从Hinode SP数据的两条Fe - i线的观测和计算面积不对称的对比中可以明显看出,存在可靠的反演分析。
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引用次数: 0
FLASHING: Project overview 闪灯:项目概述
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-10-03 DOI: 10.1093/pasj/psad064
Hiroshi Imai, Yuhki Hamae, Kei Amada, Keisuke Nakashima, Ka-Yiu Shum, Rina Kasai, José F Gómez, Lucero Uscanga, Daniel Tafoya, Gabor Orosz, Ross A Burns
Abstract This paper describes an overview of the FLASHING (Finest Legacy Acquisitions of SiO-/H2O-maser Ignitions by the Nobeyama Generation) project promoted using the 45 m telescope of Nobeyama Radio Observatory, which aims to intensively monitor H2O (at 22 GHz) and SiO (at 43 GHz) masers associated with so-called “water fountain” sources. Here we show scientific results based on the data taken in the first five seasons of FLASHING, from 2018 December to 2023 April. We show the evolution of the H2O maser spectra, discovering new spectral components that break the record of the jet’s top speed and/or systematic velocity drifts in the spectrum indicating acceleration or deceleration of the maser gas clumps. For the 43 GHz SiO maser emission, we newly detect it in one source and find that it is no longer present in another source. This implies that the jets from these water fountains can be accelerated or decelerated, and show how circumstellar envelopes are destroyed.
摘要:本文概述了利用Nobeyama射电天文台45米望远镜推进的闪光灯(Nobeyama Generation of SiO-/H2O脉泽点火的最佳遗留收购)项目,该项目旨在集中监测H2O (22 GHz)和SiO (43 GHz)脉泽,这些脉泽与所谓的“喷泉”源有关。在这里,我们展示了基于flash前五个季节(2018年12月至2023年4月)数据的科学结果。我们展示了H2O脉泽光谱的演变,发现了新的光谱成分,这些成分打破了射流的最高速度和/或光谱中系统速度漂移的记录,表明了脉泽气体团块的加速或减速。对于43 GHz SiO脉泽发射,我们在一个源中新检测到它,发现它在另一个源中不再存在。这意味着这些喷泉的射流可以加速或减速,并显示了星周包层是如何被破坏的。
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引用次数: 0
AGN number fraction in galaxy groups and clusters at z &lt; 1.4 from the Subaru Hyper Suprime-Cam survey z &lt星系群和星系团的AGN数分数;1.4来自Subaru Hyper prime- cam调查
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-09-29 DOI: 10.1093/pasj/psad066
Aoi Hashiguchi, Yoshiki Toba, Naomi Ota, Masamune Oguri, Nobuhiro Okabe, Yoshihiro Ueda, Masatoshi Imanishi, Satoshi Yamada, Tomotsugu Goto, Shuhei Koyama, Kianhong Lee, Ikuyuki Mitsuishi, Tohru Nagao, Atsushi J Nishizawa, Akatoki Noboriguchi, Taira Oogi, Koki Sakuta, Malte Schramm, Mio Shibata, Yuichi Terashima, Takuji Yamashita, Anri Yanagawa, Anje Yoshimoto
Abstract One of the key questions on active galactic nuclei (AGN) in galaxy clusters is how AGN could affect the formation and evolution of member galaxies and galaxy clusters in the history of the Universe. To address this issue, we investigate the dependence of AGN number fraction (fAGN) on cluster redshift (zcl) and distance from the cluster center (R$/$R200). We focus on more than 27000 galaxy groups and clusters at 0.1 &lt; zcl &lt; 1.4 with more than 1 million member galaxies selected from the Subaru Hyper Suprime-Cam. By combining various AGN selection methods based on infrared (IR), radio, and X-ray data, we identify 2688 AGN. We find that (i) fAGN increases with zcl and (ii) fAGN decreases with R$/$R200. The main contributors to the rapid increase of fAGN towards high-z and cluster center are IR- and radio-selected AGN, respectively. These results indicate that the emergence of the AGN population depends on the environment and redshift, and galaxy groups and clusters at high z play an important role in AGN evolution. We also find that cluster–cluster mergers may not drive AGN activity in at least the cluster center, while we have tentative evidence that cluster–cluster mergers could enhance AGN activity in the outskirts of (particularly massive) galaxy clusters.
星系团活动星系核(AGN)在宇宙历史中如何影响成员星系和星系团的形成和演化是研究活动星系核的关键问题之一。为了解决这个问题,我们研究了AGN数分数(fAGN)与簇红移(zcl)和到簇中心的距离(R$/$R200)的关系。我们关注的是超过27000个0.1 <的星系团和星团;zcl, lt;140多万个成员星系从斯巴鲁超级超级相机中选择。通过结合各种基于红外、无线电和x射线数据的AGN选择方法,我们确定了2688 AGN。我们发现(i) fAGN随zcl的增加而增加,(ii) fAGN随R$/$R200的增加而减小。导致AGN向高z和簇中心快速增加的主要因素分别是红外选择AGN和无线电选择AGN。这些结果表明,AGN群体的出现取决于环境和红移,高z星系群和星系团在AGN的演化中起着重要作用。我们还发现,至少在星团中心,星团-星团合并可能不会推动AGN的活动,而我们有初步证据表明,星团-星团合并可以增强(特别是大质量)星团外围的AGN活动。
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引用次数: 0
Relationship of peak fluxes of solar radio bursts and X-ray class of solar flares: Application to early great solar flares 太阳射电暴峰值通量与太阳耀斑x射线等级的关系:早期大太阳耀斑的应用
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-09-29 DOI: 10.1093/pasj/psad058
Keitarou Matsumoto, Satoshi Masuda, Masumi Shimojo, Hisashi Hayakawa
Abstract Large solar flares occasionally trigger significant space-weather disturbances that affect the technological infrastructures of modern civilization, and therefore require further investigation. Although these solar flares have been monitored by satellite observations since the 1970s, large solar flares occur only infrequently and restrict systematic statistical research owing to data limitations. However, Toyokawa Observatory has operated solar radio observations at low frequencies (at 3.75 and 9.4 GHz) since 1951 and captured the early great flares as solar radio bursts. To estimate the magnitudes of flares that occurred before the start of solar X-ray (SXR) observations with the Geostationary Operational Environmental Satellite (GOES) satellites, we show the relationship between microwave fluxes at 3.75 and 9.4 GHz and X-ray fluxes of flares that occurred after 1988. In total, we explored 341 solar flares observed with the Nobeyama Radio Polarimeters and Toyokawa Observatory from 1988–2014 and compared them with the SXR observations recorded by the GOES satellites. The correlation coefficient was approximately 0.7. Therefore, the GOES X-ray class can be estimated from the peak flux at 3.75 and 9.4 GHz with a large variance and an error of factor of 3 (1σ). Thus, for the first time, we quantitatively estimated the light curves of two early solar flares observed in 1956 February by the Toyokawa solar radio observations using the relationship between SXR thermal radiation and microwave nonthermal radiation (Neupert, 1968, ApJ, 153, 59).
大型太阳耀斑偶尔会引发重大的空间天气干扰,影响现代文明的技术基础设施,因此需要进一步研究。虽然这些太阳耀斑自1970年代以来一直通过卫星观测进行监测,但由于数据的限制,大型太阳耀斑很少发生,并限制了系统的统计研究。然而,自1951年以来,东川天文台一直在低频率(3.75 GHz和9.4 GHz)上进行太阳射电观测,并捕捉到了早期的太阳射电爆发大耀斑。为了估计在地球同步运行环境卫星(GOES)开始太阳x射线(SXR)观测之前发生的耀斑的大小,我们展示了3.75和9.4 GHz的微波通量与1988年后发生的耀斑的x射线通量之间的关系。我们研究了Nobeyama射电偏振计和Toyokawa天文台在1988-2014年间观测到的341个太阳耀斑,并将它们与GOES卫星记录的SXR观测结果进行了比较。相关系数约为0.7。因此,从3.75 GHz和9.4 GHz的峰值通量可以估计出GOES的x射线类别,方差较大,误差为3 (1σ)。因此,我们首次利用SXR热辐射和微波非热辐射之间的关系,定量估计了1956年2月Toyokawa太阳射电观测观测到的两个早期太阳耀斑的光曲线(Neupert, 1968, ApJ, 153,59)。
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引用次数: 1
Solar eclipses observed worldwide in the first half of the 15th century and ΔT determined from multiply observed eclipses 15世纪上半叶在世界范围内观测到的日食,ΔT通过多次观测日食而确定
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-09-26 DOI: 10.1093/pasj/psad036
Kiyotaka Tanikawa, Mitsuru Sôma, Ockie Simmonds, Kiyomi Iwahashi
Abstract The main purpose of the present paper is to list all the solar eclipses which took place in the first half of the 15th century, to list all the available records of observation of these eclipses, and, by using the multiply observed or contemporaneously observed solar eclipses, to determine ΔT for a few periods of the first half of the 15th century. We make the table using solar eclipse records from East Asia (China, Korea, and Japan), India, West Asia, and Europe, though the table is not perfect because the compilation of records is not complete in some of the relevant areas. We evaluate the reliability of the Chinese records of solar eclipses. The Chinese official history book, the Mingshi, records visible eclipses, while it does not record invisible eclipses. A simple analysis shows that the reliability of the book is $97%$. The marginally observable eclipses in China are useful for us to determine ΔT. We briefly consider the Māori eclipse observed in 1409. We extract the multiply observed eclipses and check whether these are useful for determining the value of ΔT. Finally, with newly added records of solar eclipses, we re-determine the value range of ΔT during the years 1431–1433 (see Tanikawa et al. 2019, in Proc. 5th Symposium on Historical Astronomical Records and Modern Science), and add a new ΔT in the year 1445.
本文的主要目的是列出15世纪上半叶发生的所有日食,列出所有可获得的日食观测记录,并利用多次观测或同时观测的日食来确定15世纪上半叶的几个时期的ΔT。我们使用东亚(中国、韩国和日本)、印度、西亚和欧洲的日食记录制作了这个表,尽管由于一些相关地区的记录汇编不完整,这个表并不完善。我们评估了中国日食记录的可靠性。中国的官方史书《明史》记载了可见的日食,而没有记载不可见的日食。简单的分析表明,这本书的可靠性为97%。在中国边际观测到的日食对我们确定ΔT很有用。我们简单地考虑一下1409年观测到的Māori日食。我们提取多次观测到的日食,并检查它们是否有助于确定ΔT的值。最后,通过新增加的日食记录,我们重新确定了ΔT在1431-1433年间的值范围(见Tanikawa et al. 2019, Proc. 5th Symposium on Historical Astronomical records and Modern Science),并在1445年增加了一个新的ΔT。
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引用次数: 0
Galaxy Cruise: Deep Insights into Interacting Galaxies in the Local Universe 银河巡航:深入了解当地宇宙中相互作用的星系
4区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2023-09-26 DOI: 10.1093/pasj/psad055
Masayuki Tanaka, Michitaro Koike, Sei’ichiro Naito, Junko Shibata, Kumiko Usuda-Sato, Hitoshi Yamaoka, Makoto Ando, Kei Ito, Umi Kobayashi, Yutaro Kofuji, Atsuki Kuwata, Suzuka Nakano, Rhythm Shimakawa, Ken-ichi Tadaki, Suguru Takebayashi, Chie Tsuchiya, Tomofumi Umemoto, Connor Bottrell
Abstract We present the first results from GALAXY CRUISE, a community (or citizen) science project based on data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). The current paradigm of galaxy evolution suggests that galaxies grow hierarchically via mergers, but our observational understanding of the role of mergers is still limited. The data from HSC-SSP are ideally suited to improve our understanding with improved identifications of interacting galaxies thanks to the superb depth and image quality of HSC-SSP. We launched a community science project, GALAXY CRUISE, in 2019 and have collected over two million independent classifications of 20686 galaxies at z &lt; 0.2. We first characterize the accuracy of the participants’ classifications and demonstrate that it surpasses previous studies based on shallower imaging data. We then investigate various aspects of interacting galaxies in detail. We show that there is a clear sign of enhanced activities of super-massive black holes and star formation in interacting galaxies compared to those in isolated galaxies. The enhancement seems particularly strong for galaxies undergoing violent mergers. We also show that the mass growth rate inferred from our results is roughly consistent with the observed evolution of the stellar mass function. The second season of GALAXY CRUISE is currently underway and we conclude with future prospects. We make the morphological classification catalog used in this paper publicly available at the GALAXY CRUISE website, which will be particularly useful for machine-learning applications.
我们提出了银河巡航的第一个结果,银河巡航是一个社区(或公民)科学项目,基于超级超级凸轮斯巴鲁战略计划(HSC-SSP)的数据。目前的星系演化范式表明,星系通过合并分层增长,但我们对合并作用的观测理解仍然有限。来自HSC-SSP的数据非常适合提高我们对相互作用星系的认识,这要归功于HSC-SSP的极好的深度和图像质量。我们在2019年启动了一个社区科学项目,银河巡航,并收集了20686个星系的200多万份独立分类。0.2. 我们首先描述了参与者分类的准确性,并证明它超越了以前基于较浅成像数据的研究。然后我们详细研究相互作用星系的各个方面。我们表明,与孤立星系相比,相互作用星系中超大质量黑洞和恒星形成活动增强的明显迹象。在经历剧烈合并的星系中,这种增强似乎特别强烈。我们还表明,从我们的结果推断出的质量增长率与观测到的恒星质量函数的演化大致一致。银河邮轮第二季目前正在进行中,我们展望未来。我们在GALAXY CRUISE网站上公开了本文中使用的形态分类目录,这对机器学习应用特别有用。
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引用次数: 0
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Publications of the Astronomical Society of Japan
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