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Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning 基于深度学习识别 LAMOST DR9 中的碳星
Pub Date : 2024-08-22 DOI: 10.3847/1538-4365/ad6261
YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Carbon stars play a crucial role in astronomical research and are significant for understanding stellar evolution, measuring cosmic distances, and studying galaxy kinematics. In recent years, identifying carbon stars using machine learning methods and traditional line-index methods has become a research hotspot, but there are still limitations regarding accuracy and automation. In this study, we propose to build a five-class model to identify carbon stars using spectral data from LAMOST DR9. The model achieved 99.45% precision and 91.21% recall on the carbon star testing set. We conducted independent tests using a sample of 1333 known carbon stars that were not used in the training and testing phases, and our model ultimately identified 1199 carbon stars. On this basis, we used this model to screen 11,226,252 spectra of LAMOST DR9 and identified 4383 carbon stars, including 1197 newly discovered carbon stars. To gain a more comprehensive understanding of the characteristics of the 4383 carbon stars obtained, further visual inspection of these spectra was performed to provide more detailed carbon star subtypes.
碳星在天文研究中起着至关重要的作用,对了解恒星演化、测量宇宙距离和研究星系运动学意义重大。近年来,利用机器学习方法和传统的线指数方法识别碳星已成为研究热点,但在准确性和自动化方面仍存在局限。在本研究中,我们提出利用LAMOST DR9的光谱数据建立一个五类模型来识别碳星。该模型在碳星测试集上达到了 99.45% 的精确度和 91.21% 的召回率。我们使用训练和测试阶段未使用的 1333 个已知碳星样本进行了独立测试,我们的模型最终识别出了 1199 个碳星。在此基础上,我们使用该模型筛选了 LAMOST DR9 的 11,226,252 条光谱,识别出 4383 颗碳星,其中包括 1197 颗新发现的碳星。为了更全面地了解所获得的 4383 颗碳星的特征,我们对这些光谱进行了进一步的目视检查,以提供更详细的碳星亚型。
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引用次数: 0
AstroSR: A Data Set of Galaxy Images for Astronomical Superresolution Research AstroSR:用于天文超分辨率研究的星系图像数据集
Pub Date : 2024-08-22 DOI: 10.3847/1538-4365/ad61e4
Jiawei Miao, Liangping Tu, Bin Jiang, Xiangru Li, Bo Qiu
In the past decade, various sky surveys with a wide range of wavelengths have been conducted, resulting in an explosive growth of survey data. There may be overlapping regions between different surveys, but the data quality and brightness are different. The translation of data quality between different surveys provides benefits for studying the properties of galaxies in specific regions that high-quality surveys have not yet covered. In this paper, we create a data set for analyzing the quality transformation of different surveys, AstroSR, using the galaxy images from overlapping regions from the Subaru/Hyper Suprime-Cam (HSC) and the Sloan Digital Sky Survey (SDSS). In addition, we use superresolution (SR) techniques to improve the quality of low-resolution images in the AstroSR and explore whether the proposed data set is suitable for SR. We try four representative models: EDSR, RCAN, ENLCN, and SRGAN. Finally, we compare the evaluation metrics and visual quality of the above methods. SR models trained with AstroSR successfully generate HSC-like images from SDSS images, which enhance the fine structure present in the SDSS images while retaining important morphological information and increasing the brightness and signal-to-noise. Improving the resolution of astronomical images by SR can improve the size and quality of the sky surveys. The data set proposed in this paper provides strong data support for the study of galaxy SR and opens up new research possibilities in astronomy. The data set is available online at https://github.com/jiaweimmiao/AstroSR.
在过去的十年中,人们开展了各种波长的巡天观测,巡天观测数据呈爆炸式增长。不同巡天之间可能存在重叠区域,但数据质量和亮度却各不相同。不同巡天观测之间数据质量的转换,有利于研究高质量巡天观测尚未覆盖的特定区域的星系特性。在本文中,我们利用来自Subaru/Hyper Suprime-Cam(HSC)和Sloan Digital Sky Survey(SDSS)重叠区域的星系图像,创建了一个用于分析不同巡天质量转换的数据集AstroSR。此外,我们还使用超分辨率(SR)技术来提高 AstroSR 中低分辨率图像的质量,并探索所提议的数据集是否适合 SR。我们尝试了四种具有代表性的模型:EDSR、RCAN、ENLCN 和 SRGAN。最后,我们比较了上述方法的评价指标和视觉质量。使用 AstroSR 训练的 SR 模型成功地从 SDSS 图像生成了类似 HSC 的图像,在保留重要形态信息、提高亮度和信噪比的同时,增强了 SDSS 图像中存在的精细结构。利用 SR 提高天文图像的分辨率可以改善巡天的规模和质量。本文提出的数据集为研究星系SR提供了有力的数据支持,为天文学研究开辟了新的可能性。该数据集可在 https://github.com/jiaweimmiao/AstroSR 在线查阅。
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引用次数: 0
X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4 近距离到远距离星系中的 X 射线风 (X-WING)。I. 对 z ∼ 0-4 范围内具有超快外流和暖吸收体的星系进行的遗留观测
Pub Date : 2024-08-22 DOI: 10.3847/1538-4365/ad5961
Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
As an inaugural investigation under the X-ray Winds In Nearby-to-distant Galaxies (X-WING) program, we assembled a data set comprising 132 active galactic nuclei (AGNs) spanning redshifts z ∼ 0–4 characterized by blueshifted absorption lines indicative of X-ray winds. Through an exhaustive review of previous research, we compiled the outflow parameters for 583 X-ray winds, encompassing key attributes such as outflow velocities (Vout), ionization parameters (ξ), and hydrogen column densities. By leveraging the parameters Vout and ξ, we systematically categorized the winds into three distinct groups: ultrafast outflows (UFOs), low-ionization parameter (low-IP) UFOs, and warm absorbers (WAs). Strikingly, a discernible absence of linear correlations in the outflow parameters, coupled with distributions approaching instrumental detection limits, was observed. Another notable finding was the identification of a velocity gap around Vout ∼ 10,000 km s−1. This gap was particularly evident in the winds detected via absorption lines within the ≲2 keV band, indicating disparate origins for low-IP UFOs and WAs. In cases involving Fe xxv/Fe xxvi lines, where the gap might be attributed to potential confusion between emission/absorption lines and the Fe K-edge, the possibility of UFOs and galactic-scale WAs being disconnected is considered. An examination of the outflow and dust sublimation radii revealed a distinction: UFOs appear to consist of dust-free material, whereas WAs likely comprise dusty gas. From 2024, the X-Ray Imaging and Spectroscopy Mission is poised to alleviate observational biases, providing insights into the authenticity of the identified gap, a pivotal question in comprehending AGN feedback from UFOs.
作为 "近距离到远距离星系中的 X 射线风(X-WING)"计划的首次调查,我们收集了一个数据集,其中包括 132 个活动星系核(AGN),其红移 z ∼ 0-4,其特征是蓝移吸收线表明存在 X 射线风。通过对以往研究的详尽回顾,我们汇编了 583 个 X 射线风的外流参数,包括外流速度(Vout)、电离参数(ξ)和氢柱密度等关键属性。通过利用 Vout 和 ξ 参数,我们将这些风系统地分为三类:超快外流风(UFO)、低电离参数 UFO 和暖吸收风(WAs)。令人震惊的是,外流参数中明显缺乏线性相关关系,而且其分布接近仪器探测极限。另一个值得注意的发现是在 Vout ∼ 10,000 km s-1 附近发现了一个速度差距。这种差距在通过≲2 keV波段内的吸收线探测到的风中尤为明显,表明低IP UFO和WA的起源不同。在涉及铁 xxv/Fe xxvi 线的情况下,差距可能是由于发射线/吸收线和铁 K 边之间的潜在混淆造成的,因此考虑了 UFO 和银河尺度 WAs 互不关联的可能性。对流出半径和尘埃升华半径的研究揭示了两者之间的区别:UFO似乎由无尘物质组成,而WA则可能由含尘气体组成。从 2024 年起,X 射线成像和光谱任务将缓解观测偏差,提供对已发现缺口真实性的见解,这是理解 UFO AGN 反馈的一个关键问题。
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引用次数: 0
A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys IRAS 和 SDSS 勘测中的超亮度红外星系比较研究
Pub Date : 2024-08-16 DOI: 10.3847/1538-4365/ad5d75
Shaohua Zhang, Zhijian Luo, Xiheng Shi, Chenggang Shu, Hubing Xiao, Hongyan Zhou
We present a comprehensive study of ultraluminous infrared galaxies (ULIRGs), leveraging data from the Infrared Astronomical Satellite Faint Source Catalogue and the spectroscopic catalog in the Sloan Digital Sky Survey Data Release 16. Our meticulous crossmatching technique significantly enhances the reliability of ULIRG identification, resulting in the identification of 283 reliable ULIRGs, including 102 new detections, while discarding 120 previously reported false sources. Covering a redshift range of z = 0.018–0.996, with a median redshift of z¯=0.259, our uniform sample reveals apparent interaction features in approximately 40% of ULIRGs, increasing to 92% for those with z < 0.1. Through optical spectra analysis, it is indicated that over 58% of ULIRGs host an active galactic nucleus (AGN), which is twice as high as detections based solely on infrared colors. Moreover, a pronounced excess of radio emissions associated with AGN activity results in a steeper radio–far-infrared correlation. Notably, Type I ULIRGs exhibit properties similar to those of narrow-line Seyfert 1 galaxies, with an elevated incidence rate of Mg ii broad absorption lines (16.7%), surpassing that of typical optically selected quasars by over tenfold, consistent with current evolutionary models. We anticipate that forthcoming telescopes such as the China Space Station Telescope and Leighton Chajnantor Telescope will provide deeper insights into ULIRG morphology, dust distribution, molecular gas, and AGN activity.
我们利用红外天文卫星微弱源目录和斯隆数字巡天数据第16版中的光谱目录中的数据,对超亮度红外星系(ULIRG)进行了全面研究。我们细致入微的交叉匹配技术大大提高了 ULIRG 识别的可靠性,最终识别出 283 个可靠的 ULIRG,其中包括 102 个新发现的 ULIRG,同时剔除了 120 个之前报告的虚假来源。我们的统一样本覆盖了 z = 0.018-0.996 的红移范围,中位红移为 z¯=0.259,在大约 40% 的超红外天体中发现了明显的相互作用特征,在 z < 0.1 的超红外天体中,这一比例上升到 92%。通过光学光谱分析,我们发现超过58%的超红外天体中存在活动星系核(AGN),是仅根据红外光谱探测到的活动星系核的两倍。此外,与 AGN 活动相关的射电辐射明显过剩,导致射电-远红外相关性更加陡峭。值得注意的是,I型超红外巨星表现出了与窄线赛弗1星系类似的特性,Mg ii宽吸收线的入射率很高(16.7%),比典型的光学选择类星体的入射率高出10倍以上,这与当前的演化模型是一致的。我们预计,中国空间站望远镜和莱顿-恰南托尔望远镜等即将投入使用的望远镜将为ULIRG的形态、尘埃分布、分子气体和AGN活动提供更深入的见解。
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引用次数: 0
CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network CMBFSCNN:利用卷积神经网络进行宇宙微波背景极化前景减法
Pub Date : 2024-08-14 DOI: 10.3847/1538-4365/ad5c66
Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
In our previous study, we introduced a machine learning technique, namely Cosmic Microwave Background Foreground Subtraction with Convolutional Neural Networks (CMBFSCNN), for the removal of foreground contamination in cosmic microwave background (CMB) polarization data. This method was successfully employed on actual observational data from the Planck mission. In this study, we extend our investigation by considering the CMB lensing effect in simulated data and utilizing the CMBFSCNN approach to recover the CMB lensing B-mode power spectrum from multifrequency observational maps. Our method is first applied to simulated data with the performance of the CMB-S4 experiment. We achieve reliable recovery of the noisy CMB Q (or U) maps with a mean absolute difference of 0.016 ± 0.008 μK (or 0.021 ± 0.002 μK) for the CMB-S4 experiment. To address the residual instrumental noise in the foreground-cleaned map, we employ a “half-split maps” approach, where the entire data set is divided into two segments sharing the same sky signal but having uncorrelated noise. Using cross-correlation techniques between two recovered half-split maps, we effectively reduce instrumental noise effects at the power spectrum level. As a result, we achieve precise recovery of the CMB EE and lensing B-mode power spectra. Furthermore, we also extend our pipeline to full-sky simulated data with the performance of the LiteBIRD experiment. As expected, various foregrounds are cleanly removed from the foregrounds contamination observational maps, and recovered EE and lensing B-mode power spectra exhibit excellent agreement with the true results. Finally, we discuss the dependency of our method on the foreground models.
在之前的研究中,我们介绍了一种机器学习技术,即卷积神经网络宇宙微波背景前景减法(CMBFSCNN),用于去除宇宙微波背景(CMB)极化数据中的前景污染。该方法已成功应用于普朗克任务的实际观测数据。在本研究中,我们扩展了研究范围,考虑了模拟数据中的 CMB 透镜效应,并利用 CMBFSCNN 方法从多频观测图中恢复 CMB 透镜 B 模式功率谱。我们的方法首先应用于具有 CMB-S4 实验性能的模拟数据。我们可靠地恢复了有噪声的 CMB Q(或 U)图,CMB-S4 实验的平均绝对差值为 0.016 ± 0.008 μK(或 0.021 ± 0.002 μK)。为了解决前景净化图中的残余仪器噪声问题,我们采用了 "半分割图 "方法,即将整个数据集划分为共享相同天空信号但噪声不相关的两个区段。利用两个恢复的半分割图之间的交叉相关技术,我们可以有效地减少功率谱级的仪器噪声影响。因此,我们实现了对 CMB EE 和透镜 B 模式功率谱的精确恢复。此外,我们还利用 LiteBIRD 实验的性能,将我们的管道扩展到全天空模拟数据。不出所料,各种前景都被从前景污染观测图中清除了,恢复的 EE 和 Lensing B 模式功率谱与真实结果呈现出极好的一致性。最后,我们讨论了我们的方法对前景模型的依赖性。
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引用次数: 0
Cross Observatory Coordination with tilepy: A Novel Tool for Observations of Multimessenger Transient Events 与瓦比进行跨天文台协调:观测多信使瞬变事件的新工具
Pub Date : 2024-08-12 DOI: 10.3847/1538-4365/ad5bde
Monica Seglar-Arroyo, Halim Ashkar, Mathieu de Bony de Lavergne, Fabian Schüssler
Time-domain astrophysics has leaped forward with the direct discovery of gravitational waves and the emergence of new generation instruments for multimessenger studies. The capacity of the multimessenger multiwavelength community to effectively pursue follow-up observations is hindered by the suboptimal localization of numerous transient events and the escalating volume of alerts. Thus, we have developed an effective tool to overcome the observational and technical hurdles inherent in the emerging field of multimessenger astrophysics. We present tilepy, a Python package for the automatic scheduling of follow-up observations of poorly localized transient events. It is ideally suited to tackle the challenge of complex follow-up in mid- and small-field-of-view telescope campaigns, with or without human intervention. We demonstrate the capabilities of tilepy in the realm of multiobservatory, multiwavelength campaigns, to cover the localization uncertainty region of various events ultimately aiming at pinpointing the source of the multimessenger emission. The tilepy code is publicly available on GitHub and is sufficiently flexible to be employed either automatically or in a customized manner, tailored to collaboration and individual requirements. tilepy is also accessible via a public API and through the Astro-COLIBRI platform.
随着引力波的直接发现和用于多信使研究的新一代仪器的出现,时域天体物理学突飞猛进。多信使多波长团体有效开展后续观测的能力受到众多瞬变事件定位不理想和警报数量不断增加的阻碍。因此,我们开发了一种有效的工具来克服多信使天体物理学这一新兴领域固有的观测和技术障碍。我们介绍的 tilepy 是一个 Python 软件包,用于自动安排对局部性较差的瞬变事件的跟踪观测。它非常适合在有或没有人工干预的情况下应对中视场和小视场望远镜运动中复杂的跟踪观测挑战。我们展示了tilepy在多天文台、多波长活动中的能力,以覆盖各种事件的定位不确定性区域,最终精确定位多信使发射源。tilepy代码在GitHub上公开发布,具有足够的灵活性,既可自动使用,也可根据合作和个人要求定制使用。tilepy还可通过公共应用程序接口和Astro-COLIBRI平台访问。
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引用次数: 0
An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057* 多尘紧凑遮蔽核星系 Zw 049.057* 的成像和光谱探测
Pub Date : 2024-08-11 DOI: 10.3847/1538-4365/ad55c9
J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans and M. Gorski
Zw 049.057 is a moderate-mass, dusty, early-type galaxy that hosts a powerful compact obscured nucleus (CON, LFIR,CON ≥ 1011L⊙). The resolution of the Hubble Space Telescope enabled measurements of the stellar light distribution and characterization of dust features. Zw 049.057 is inclined with a prominent three-zone disk; the R ≈ 1 kpc star-forming inner dusty disk contains molecular gas, a main disk with less dust and an older stellar population, and a newly detected outer stellar region at R > 6 kpc with circular isophotes. Previously unknown polar dust lanes are signatures of a past minor merger that could have warped the outer disk to near face-on. Dust transmission measurements provide lower limit gas mass estimates for dust features. An extended region with moderate optical depth and M ≥ 2 × 108M⊙ obscures the central 2 kpc. Optical spectra show strong interstellar Na D absorption with a constant velocity across the main disk, likely arising in this extraplanar medium. Opacity measurements of the two linear dust features, pillars, give a total mass of ≥106M⊙, flow rates of ≥2 M⊙ yr−1, and few Myr flow times. Dust pillars are associated with the CON and are visible signs of its role in driving large-scale feedback. Our assessments of feedback processes suggest gas recycling sustains the CON. However, radiation pressure driven mass loss and efficient star formation must be avoided for the active galactic nucleus to retain sufficient gas over its lifespan to produce substantial mass growth of the central black hole.
Zw 049.057 是一个中等质量、尘埃较多的早期型星系,其中有一个强大的紧密遮挡核(CON, LFIR,CON ≥ 1011L⊙)。利用哈勃太空望远镜的分辨率,可以测量恒星光分布和尘埃特征。Zw 049.057呈倾斜状,有一个突出的三区盘;R≈1 kpc的恒星形成内尘埃盘包含分子气体,主盘尘埃较少,恒星群较老,在R>6 kpc处新探测到一个外恒星区,有圆形等距线。以前未知的极地尘埃通道是过去一次小规模合并的标志,可能将外盘扭曲到接近正面。尘埃透射测量为尘埃特征提供了下限气体质量估计值。一个具有中等光学深度、M ≥ 2 × 108M⊙的扩展区域遮挡了中心的 2 kpc。光学光谱显示,主圆盘上的星际 Na D 吸收很强,速度恒定,很可能是由这种星外介质引起的。对两个线性尘柱特征的不透明度测量结果表明,尘柱的总质量≥106M⊙,流速≥2 M⊙yr-1,流动时间为几Myr。尘柱与CON有关,是其驱动大规模反馈的明显标志。我们对反馈过程的评估表明,气体循环维持着CON。然而,要使活动星系核在其生命周期内保留足够的气体,使中心黑洞的质量大幅增长,就必须避免辐射压力驱动的质量损失和有效的恒星形成。
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引用次数: 0
Se-ResNet+SVM Model: An Effective Method of Searching for Hot Subdwarfs from LAMOST Se-ResNet+SVM模型:从 LAMOST 搜寻热亚矮星的有效方法
Pub Date : 2024-08-11 DOI: 10.3847/1538-4365/ad5b61
Zhongding Cheng, Xiaoming Kong, Tianmin Wu, Aina Zhang, Bowen Liu, Yude Bu, Zhenxin Lei, Yatao Zhang, Zhenping Yi and Meng Liu
This paper presents a robust neural network approach for identifying hot subdwarfs. Our method leveraged the Squeeze-and-Excitation Residual Network to extract abstract features, which were combined with experience features to create hybrid features. These hybrid features were then classified using a support vector machine. To enhance accuracy, we employed a two-stage procedure. In the first stage, a binary classification model was constructed to distinguish hot subdwarfs, achieving a precision of 98.55% on the test set. In the second stage, a four-class classification model was employed to further refine the candidates, achieving a precision of 91.75% on the test set. Using the binary classification model, we classified 333,534 spectra from LAMOST DR8, resulting in a catalog of 3086 hot subdwarf candidates. Subsequently, the four-class classification model was applied to filter these candidates further. When applying thresholds of 0.5 and 0.9, we identified 2132 and 1247 candidates, respectively. Among these candidates, we visually inspected their spectra and identified 58 and 30 new hot subdwarfs, respectively, resulting in a precision of 82.04% and 88.21% for these discoveries. Furthermore, we evaluated the 3086 candidates obtained in the first stage and identified 168 new hot subdwarfs, achieving an overall precision of 62.54%. Lastly, we trained a Squeeze-and-Excitation regression model with mean absolute error values of 3009 K for Teff, 0.20 dex for log g, and 0.42 dex for log(nHe/nH). Using this model, we predicted the atmospheric parameters of these 168 newly discovered hot subdwarfs.
本文提出了一种用于识别热亚矮星的稳健神经网络方法。我们的方法利用挤压-激发残差网络来提取抽象特征,并将这些特征与经验特征相结合,形成混合特征。然后使用支持向量机对这些混合特征进行分类。为了提高准确性,我们采用了两阶段程序。在第一阶段,我们构建了一个二元分类模型来区分热亚战,在测试集上达到了 98.55% 的精确度。在第二阶段,我们采用了一个四级分类模型来进一步完善候选者,在测试集上达到了 91.75% 的精确度。利用二元分类模型,我们对来自 LAMOST DR8 的 333,534 条光谱进行了分类,得到了 3086 个热亚矮星候选星表。随后,我们应用四级分类模型进一步筛选这些候选者。当采用 0.5 和 0.9 的阈值时,我们分别发现了 2132 和 1247 个候选者。在这些候选者中,我们目测了它们的光谱,分别发现了 58 个和 30 个新的热亚矮星,这些发现的精确度分别为 82.04% 和 88.21%。此外,我们还对第一阶段获得的 3086 个候选者进行了评估,发现了 168 个新的热亚矮星,总体精确度达到 62.54%。最后,我们训练了一个 "挤压-激发 "回归模型,其 Teff 的平均绝对误差为 3009 K,log g 的平均绝对误差为 0.20 dex,log(nHe/nH) 的平均绝对误差为 0.42 dex。利用这个模型,我们预测了这 168 个新发现的热亚矮星的大气参数。
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引用次数: 0
p adé: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing p adé:基于帕代差分法的原行星盘湍流代码
Pub Date : 2024-08-07 DOI: 10.3847/1538-4365/ad5af3
Karim Shariff
The Padé code has been developed to treat hydrodynamic turbulence in protoplanetary disks. It solves the compressible equations of motion in cylindrical coordinates. Derivatives are computed using nondiffusive and conservative fourth-order Padé differencing, which has higher resolving power compared to both dissipative shock-capturing schemes used in most astrophysics codes, as well as nondiffusive central finite-difference schemes of the same order. The fourth-order Runge–Kutta method is used for time stepping. A previously reported error-corrected Fargo approach is used to reduce the time step constraint imposed by rapid Keplerian advection. Artificial bulk viscosity is used when shock capturing is required. Tests for correctness and scaling with respect to the number of processors are presented. Finally, efforts to improve efficiency and accuracy are suggested.
Padé 代码是为处理原行星盘中的流体动力湍流而开发的。它以圆柱坐标求解可压缩运动方程。与大多数天体物理学代码中使用的耗散冲击捕捉方案以及同阶的非扩散中央有限差分方案相比,该方案具有更高的分辨率。时间步进采用四阶 Runge-Kutta 方法。使用之前报告的误差校正 Fargo 方法来减少快速开普勒平流带来的时间步长限制。在需要捕捉冲击时,使用了人造体积粘度。对正确性和与处理器数量相关的扩展性进行了测试。最后,提出了提高效率和精度的建议。
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引用次数: 0
Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae 利用 Rubin-LSST 恢复光曲线。II.利用天琴座RR揭开银河凸起的黑暗面纱(VESTALE)
Pub Date : 2024-08-06 DOI: 10.3847/1538-4365/ad582d
M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall’Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas and R. Zanmar Sanchez
This work is part of VESTALE, a project initiated within the Legacy Survey of Space and Time (LSST) Cadence Strategy Optimization Process. Its goal is to explore the potential of Rubin-LSST observations aimed at the Galactic bulge (henceforth just “Bulge”) for studying RR Lyrae (RRL) stars. Observation and analysis of RRL stars in the Bulge are crucial for tracing the old population of the central part of our Galaxy and reconstructing its formation. Based on observations conducted with CTIO/DECam by Saha et al. toward Baade’s window, our simulations demonstrate that early Rubin-LSST observations will enable the recovery of RRL light curves (LCs) at Galactic center distances with sufficient precision. This will allow us to utilize theoretical relations from Marconi et al. to determine their distances and/or metallicity, following the REDIME algorithm introduced in Bono et al. We show how reddening and crowding affect our simulations and highlight the importance of considering these effects when deriving pulsation parameters (luminosity amplitudes, mean magnitudes) based on the LCs, especially if the goal is to explore the opposite side of the Bulge through the observation of its RRL. The simulations discussed in this investigation were conducted to support the Survey Cadence Optimization Committee’s decision to observe this important sky region since it has only recently been decided to include part of the Bulge as a target within the LSST main survey.
这项工作是VESTALE的一部分,VESTALE是在时空遗留巡天(LSST)Cadence战略优化过程中启动的一个项目。其目标是探索针对银河系凸起(以下简称 "凸起")的鲁宾-LSST观测在研究RR Lyrae(RRL)恒星方面的潜力。对隆起带中的RRL恒星进行观测和分析,对于追踪银河系中央部分的古老种群和重建其形成过程至关重要。根据Saha等人利用CTIO/DECam对Baade窗口进行的观测,我们的模拟证明早期的Rubin-LSST观测能够足够精确地恢复银河系中心距离上的RRL光变曲线(LC)。这将使我们能够利用马可尼等人的理论关系,按照 Bono 等人提出的 REDIME 算法来确定它们的距离和/或金属度。我们展示了红化和拥挤是如何影响我们的模拟的,并强调了在根据 LCs 推算脉动参数(光度振幅、平均星等)时考虑这些影响的重要性,特别是如果我们的目标是通过观测隆起的 RRL 来探索隆起的另一侧的话。本研究中讨论的模拟是为了支持巡天进度优化委员会观测这一重要天区的决定而进行的,因为最近才决定将凸起部分列为 LSST 主巡天的目标。
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